diff --git "a/Dataset/metadata-astroph.csv" "b/Dataset/metadata-astroph.csv" new file mode 100644--- /dev/null +++ "b/Dataset/metadata-astroph.csv" @@ -0,0 +1,2717 @@ +,language,creator,title,subject,keyword,identifier,description,date +0,['eng'],"['Willis, T D']",['Observations of the Isotropic Diffuse Gamma-ray Background with the EGRET Telescope'],['Astrophysics and Astronomy'],['Thesis'],['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0201515'],"[""An Isotropic Diffuse Gamma-Ray Background (IDGRB) in the spectral range 30-10,000 MeV was first reported in the early 1970's using measurements made by the SAS-2 instrument. Data recorded by the Energetic Gamma Ray Experiment Telescope (EGRET) on board the Compton Gamma Ray Observatory (CGRO) over the last 4 years are analysed in order to extract the best measurement yet made of the IDGRB. Extensive analysis of the EGRET instrumental background is presented in order to demonstrate that an uncontaminated data set can be extracted from the EGRET data. A model of the high latitude galactic diffuse foreground emission is presented and the existence of an IDGRB is confirmed. Spatial and spectral analysis of this background is presented. In addition, point source analysis at high galactic latitudes is performed to reveal the existence of a population of extragalactic sources. The characteristics of this population are examined and models of its flux distribution are reported. The question of whether the IDGRB is composed of unresolved point sources is addressed using fluctuation analysis. Finally, possible future directions for gamma ray astronomy are examined through simulations of a future gamma ray telescope: the Gamma-ray Large Area Space Telescope (GLAST). The GLAST baseline design is described and its scientific performance is evaluated. The ability of this telescope to detect 1,000-10,000 new extragalactic sources is demonstrated and the likely impact on the study of the IDGRB is considered.""]",['2002-02-01'] +1,['eng'],"['Tompkins, W F']",['Applications of Likelihood Analysis in Gamma-Ray Astrophysics'],['Astrophysics and Astronomy'],['THESIS'],['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0202141'],"['The field of gamma ray astronomy relies heavily on the statistical analysis of data. Because of the paucity of data, and the often large errors associated with detecting gamma rays, analysis and interpretation of the data require sophisticated statistical techniques. Techniques for extending the currently used maximum likelihood technique to more complicated data sets are presented. Similarly presented are methods of calculating the distribution and behavior of the maximum likelihood statistic used to measure source significance. A new method for calculating source variability is also proposed, and used to examine the sources found by the Energetic Gamma Ray Experiment Telescope (EGRET) on board the Compton Gamma Ray Observatory (CGRO). The results show that the Active Galactic Nuclei (AGN), pulsars, and unidentified sources have markedly different variability, and that the unidentified sources fall into at least two classes, differing in variability and spatial distribution. A class composed of possible Supernova Remnant associations (SNR) is distinctly more variable than the pulsars, but has a variability consistent with that of the other low latitude unidentified sources. Finally, the results of the Fall 1997 GLAST prototype beam test are presented. The results of the beam test are compared with simulated results, and found to be in remarkably good agreement.']",['2002-02-08'] +2,['eng'],"['Gordon, C']",['Adiabatic and entropy perturbations in cosmology'],['Astrophysics and Astronomy'],"['Thesis', 'Thesis']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0112523'],"['This PhD thesis presents a study of the effect and generation of non-adiabatic perturbations in Cosmology. We study adiabatic (curvature) and entropy (isocurvature) perturbations produced during a period of cosmological inflation that is driven by multiple scalar fields with an arbitrary interaction potential. A local rotation in field space is performed to separate out the adiabatic and entropy modes. The resulting field equations show explicitly how on large scales entropy perturbations can source adiabatic perturbations if the background solution follows a curved trajectory in field space, and how adiabatic perturbations cannot source entropy perturbations in the long-wavelength limit. We show why one in general expects the adiabatic and entropy perturbations to be correlated at the end of inflation. Then, we consider two-field preheating after inflation, examining conditions under which entropy perturbations can alter the large-scale curvature perturbation and showing how our new formalism has advantages in numerical stability when the background solution follows a non-trivial trajectory in field space. Then we compare the latest cosmic microwave background data with theoretical predictions including correlated adiabatic and CDM isocurvature perturbations. We find that there is a degeneracy between the amplitude of correlated isocurvature perturbations and the spectral tilt. We then study perturbations in Randall-Sundrum-type brane-world cosmologies. The density perturbations generate Weyl curvature in the bulk, which in turn backreacts on the brane via stress-energy perturbations. Bulk effects produce a non-adiabatic mode, even when the matter perturbations are adiabatic, and alter the background dynamics.']",['2001-12-24'] +3,['eng'],"['Poirier, J', ""D'Andrea, C"", 'Dunford, M']",['Secondary Muon Asymmetries at Sea Levell with Low Systematics'],['Astrophysics and Astronomy'],"['cosmic radiation, secondary radiation', 'muon, cosmic radiation', 'angular distribution, asymmetry', 'time variation', 'counters and detectors, acceptance', 'data analysis method', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109462'],"['Project GRAND has the capability of measuring the angle and identity of single tracks of secondary muons at ground level. The array is comprised of 64 stations each containing eight proportional wire planes with a 50 mm steel absorber plate placed above the bottom two planes in each station. The added steel absorber plate allows muon tracks to be separated from the less massive electrons. Over 100 billion identified muon angles have been measured. With the high statistics available, it is possible to obtain muon angular asymmetries with low systematics by subtracting west from east (and separately, south from north) angles; the subtraction eliminates most of the systematic errors while still retaining adequately small statistical errors on the differences. A preliminary analysis is performed as a function of solar time to obtain the effects on the muon rate due to effects of the sun.']",['2001-09-27'] +4,['eng'],"['Piron, F']",['TeV blazars as seen by the CAT telescope'],['Astrophysics and Astronomy'],"['talk, Lyon 2001/05/28', 'blazar', 'AGN', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109286'],"['To date, only two extragalactic objects have been firmly established as very high-energy gamma-ray sources in the Northern sky: these are the two blazars Markarian 501 and Markarian 421. This paper reviews the most striking results obtained from these sources by the CAT atmospheric Cherenkov imaging telescope, with a particular emphasis on the 1999-2000 and 2000-2001 observation campaigns of Markarian 421.']",['2001-09-28'] +5,['eng'],"['Abramo, L R', 'Woodard, R P']",['Back-Reaction Is For Real'],['Astrophysics and Astronomy'],"['relativity theory, general', 'field theory, scalar', 'inflationary universe', 'correlation function', 'perturbation theory, higher-order', 'tensor, energy-momentum']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109273'],"['We demonstrate the existence of a secular back-reaction on inflation using a simple scalar model. The model consists of a massless, minimally coupled scalar with a quartic self-interaction which is a spectator to $\\Lambda$-driven inflation. To avoid problems with coincident propagators, and to make the scalars interact more like gravitons, we impose a covariant normal ordering prescription which has the effect of removing tadpole graphs. This version of the theory exhibits a secular slowing at three loop order due to interactions between virtual infrared scalars which are ripped apart by the inflating background. The effect is quantified using an invariant observable and all orders bounds are given. We also argue that, although stochastic effects can have either sign, the slowing mechanism is superimposed upon them.']",['2001-09-28'] +6,['eng'],"['Abramo, L R', 'Woodard, R P']",['No One Loop Back_Reaction In Chaotic Inflation'],['Astrophysics and Astronomy'],"['relativity theory, general', 'inflationary universe', 'chaos', 'quantization', 'Hamiltonian formalism', 'perturbation theory, higher-order', 'radiation', 'plane wave']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109272'],"[""We use an invariant operator to study the quantum gravitational back-reaction to scalar perturbations during chaotic inflation. Our operator is the inverse covariant d'Alembertian expressed as a function of the local value of the inflaton. In the slow roll approximation this observable gives $-1/(2 H^2)$ for an arbitrary homogeneous and isotropic geometry, hence it is a good candidate for measuring the local expansion rate even when the spacetime is not perfectly homogeneous and isotropic. Corrections quadratic in the scalar creation and annihilation operators of the initial value surface are included using the slow-roll and long wavelength approximations. The result is that all terms which could produce a significant secular back-reaction cancel from the operator, before one even takes its expectation value. Although it is not relevant to the current study, we also develop a formalism for using stochastic samples to study back-reaction.""]",['2001-09-28'] +7,['eng'],"['Wang, Y', 'Lovelace, G']",['Unbiased Estimate of Dark Energy Density from Type Ia Supernova Data'],['Astrophysics and Astronomy'],"['supernova', 'dark energy', 'energy, density', 'matter, density', 'time dependence', 'quintessence', 'statistical analysis', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109233'],"['Type Ia supernovae (SNe Ia) are currently the best probes of the dark energy in the universe. To constrain the nature of dark energy in a model-independent manner, we allow the density of dark energy, $\\rho_X(z)$, to be an arbitrary function of redshift. Using simulated data from a space-based supernova pencil beam survey, we find that by optimizing the number of parameters used to parametrize the dimensionless dark energy density, $f(z)=\\rho_X(z)/\\rho_X(z=0)$, we can obtain an unbiased estimate of both f(z) and $\\Omega_m$ (assuming a flat universe and that the weak energy condition is satisfied). A plausible supernova pencil beam survey (with a square degree field of view and for an observational duration of one year) can yield about 2000 SNe Ia with $0\\le z \\le 2$. Such a survey in space would yield SN peak luminosities with a combined intrinsic and observational dispersion of $\\sigma (m_{int})=0.16$ mag. We find that for such an idealized survey, $\\Omega_m$ can be measured to 10% accuracy, and f(z) can be estimated to $\\sim$ 20% to $z \\sim 1.5$, and $\\sim$ 20-40% to $z \\sim 2$, depending on the time dependence of the true dark energy density. Dark energy densities which vary more slowly can be more accurately measured. For the anticipated SNAP mission, $\\Omega_m$ can be measured to 14% accuracy, and f(z) can be estimated to $\\sim$ 20% to $z \\sim 1.2$. Our results suggest that SNAP may gain much sensitivity to the time-dependence of f(z) and $\\Omega_m$ by devoting more observational time to the central pencil beam fields to obtain more SNe Ia at z>1.2. We also find that Monte Carlo analysis gives a more accurate estimate of the dark energy density than the maximum likelihood analysis. (abridged)']",['2001-09-28'] +8,['eng'],"['Bednarek, W']",['Extragalactic neutrino background from very young pulsars surrounded by supernova envelopes'],['Astrophysics and Astronomy'],"['supernova', 'pulsar', 'neutrino/mu, background', 'nucleus, acceleration', 'photon nucleus, interaction', 'pi, photoproduction', 'pi, decay modes', 'neutrino/mu, production', 'neutrino/mu, cosmic radiation', 'cosmic radiation, diffusion', 'cosmic radiation, flux', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109225'],"['We estimate the extragalactic muon neutrino background which is produced by hadrons injected by very young pulsars at an early phase after supernova explosion. It is assumed that hadrons are accelerated in the pulsar wind zone which is filled with thermal photons captured below the expanding supernova envelope. In collisions with those thermal photons hadrons produce pions which decay into muon neutrinos. At a later time, muon neutrinos are also produced by the hadrons in collisions with matter of the expanding envelope. We show that extragalactic neutrino background predicted by such a model should be detectable by the planned 1 km$^2$ neutrino detector if a significant part of pulsars is born with periods shorter than $\\sim 10$ ms. Since such population of pulsars is postulated by the recent models of production of extremely high energy cosmic rays, detection of neutrinos with predicted fluxes can be used as their observational test.']",['2001-09-26'] +9,['eng'],"['Lee, D S', 'Lee, W', 'Ng, K W']",['Primordial Magnetic Fields from Dark Energy'],['Astrophysics and Astronomy'],"['dark energy', 'magnetic field, production', 'field theory, scalar', 'energy, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109184'],"['Evidences indicate that the dark energy constitutes about two thirds of the critical density of the universe. If the dark energy is an evolving pseudo scalar field that couples to electromagnetism, a cosmic magnetic seed field can be produced via spinoidal instability during the formation of large-scale structures.']",['2001-09-13'] +10,['eng'],"['Aharonian, F A']",['Limits on the TeV flux of diffuse gamma rays as measured with the HEGRA air shower array'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, hadronic component', 'cosmic radiation, flux', 'flux, ratio', 'upper limit', 'showers, air', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109145'],"['Using data from the HEGRA air shower array, taken in the period from April 1998 to March 2000, upper limits on the ratio I_gamma /I_CR of the diffuse photon flux I_gamma to the hadronic cosmic ray flux I_CR are determined for the energy region 20 TeV to 100 TeV. The analysis uses a gamma-hadron discrimination which is based on differences in the development of photon- and hadron-induced air showers after the shower maximum. A method which is sensitive only to the non-isotropic component of the diffuse photon flux yields an upper limit of I_gamma /I_CR (at 54 TeV) < 2.0*10^-3 (at the 90% confidence level) for a sky region near the inner galaxy (20 degrees < galactic longitude <60 degrees and |galactic latitude|<5 degrees). A method which is sensitive to both the isotropic and the non-isotropic component yields global upper limits of I_gamma /I_CR (at 31 TeV) <1.2*10^-2 and I_gamma /I_CR (at 53 TeV) < 1.4*10^-2 (at the 90% confidence level).']",['2001-09-11'] +11,['eng'],"['Hui, L', 'Kinney, W H']",['Short Distance Physics and the Consistency Relation for Scalar and Tensor Fluctuations in the Inflationary Universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'fluctuation, scalar', 'fluctuation, tensor', 'vacuum state']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109107'],"['Recent discussions suggest the possibility that short distance physics can significantly modify the behavior of quantum fluctuations in the inflationary universe, and alter the standard large scale structure predictions. Such modifications can be viewed as due to a different choice of the vacuum state. We show that such changes generally lead to violations of the well-known consistency relation between the scalar to tensor ratio and the tensor spectral index. Vacuum effects can introduce an observable modulation to the usual predictions for the scalar and tensor power spectra.']",['2001-09-10'] +12,['eng'],"['Kirilova, Daniela P']",['Overproduction of primordial helium-4 in the presence of neutrino oscillations'],['Astrophysics and Astronomy'],"['astrophysics', 'light nucleus, production', 'helium, yield', 'neutrino, oscillation', 'neutrino/e', 'neutrino, sterile', 'neutrino, mass difference', 'neutrino, mixing angle', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109105'],"['The production of helium-4 during the cosmological nucleosynthesis in the presence of active--sterile neutrino oscillations, efficient after decoupling of electron neutrino, is analyzed. The oscillation effects on primordial nucleosynthesis, namely: neutrino spectrum distortion, depletion of electron neutrino number density and generation of neutrino-antineutrino asymmetry, are precisely taken into account. Primordially produced He-4 abundance is calculated, in a self-consistent study of the kinetics of the nucleons and the oscillating neutrinos, for the full range of parameters of the discussed oscillation model. A considerable relative increase of helium-4, up to 14% for non-resonant oscillations and up to 32% for resonant ones is registered. Cosmological constraints on oscillation parameters are discussed.']",['2001-09-07'] +13,['eng'],"['Branch, D', 'Perlmutter, S', 'Baron, E', 'Nugent, P E']","['Coping with Type Ia Supernova ""Evolution"" When Probing the Nature of the Dark Energy']",['Astrophysics and Astronomy'],"['talk, Snowmass 2001/06/30', 'supernova', 'dark energy', 'luminosity', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109070'],"['Observations of high-redshift Type Ia supernovae (SNe Ia) have provided strong evidence that the dark energy is real, and making further accurate observations of high-redshift SNe Ia is the most promising way to probe the nature of the dark energy. We discuss one of the concerns about such a project - that of coping with SN Ia evolution. We emphasize that SN Ia evolution differs in an important respect from the kind of evolution that has foiled some past projects in observational cosmology, and we outline empirical strategies that will take it into account. The supporting role of physical models of SNe Ia also is discussed. Our conclusion is that systematic errors due to SN Ia evolution will be small.']",['2001-12-14'] +14,['eng'],"['Prasanna, A R', 'Goswami, S']",['Energy deposition due to neutrino pair annhilation near rotating neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'rotational', 'neutrino antineutrino, annihilation', 'electron, pair production', 'energy', 'relativity theory, general', 'supernova', 'external field', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109058'],['General relativistic effects have been shown to increase the energy deposition rate due to the process $\\nu \\bar{\\nu} \\to e^{+}e^{-}$ in supernovae and neutron stars. In this paper we study the effect of inclusion of the rotation of the star in the general relativistic treatment. We show that inclusion of rotation results in a reduction in the heating rate as compared to the no rotation case.'],['2001-12-14'] +15,['eng'],"['Hwang, J']",['Cosmological structure problem in the ekpyrotic scenario'],['Astrophysics and Astronomy'],"['astrophysics, model', 'critical phenomena', 'potential', 'perturbation, scalar', 'perturbation, tensor', 'gravitational radiation', 'spectra, fluctuation', 'model, ekpyrotic']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109045'],"[""We address the power spectrum generated in the recently proposed ekpyrotic scenario by Khoury et al. The issue has been raised recently by Lyth who used the conventional method based on a conserved variable in the large-scale limit, and derived different results from Khoury et al. In this note we point out that the method based on the matching conditions of the joining variables gives the same answer as the one from using the conserved variables. In fact, it is known in the literature that as long as the equations hold during the transition and the large-scale condition is met both methods give the same results which is why the simpler conserved variable method is favored in the recent literature. Therefore, an exponential potential leads to a power-law expansion/contraction $a \\propto |t|^p$, and it is known that the power $p$ dictates the final power specta of both the scalar and tensor structures. If $p \\ll 1$ as one realization of the ekpyrotic scenerio suggests, the results are $n_S -1 \\simeq 2 \\simeq n_T$ and the amplitude of the scalar perturbation is supressed relative to the one of the gravitational wave by a factor $\\sqrt{p}/2$. Both results confirm Lyth's. An observation is made on the constraint on the dynamics of the seed generating stage from the requirement of scale-invariant spectrum.""]",['2001-09-05'] +16,['eng'],"['Namba, T', 'Inoue, Y', 'Moriyama, S', 'Minowa, M']",['An x-ray detector using PIN photodiodes for the axion helioscope'],['Astrophysics and Astronomy'],"['axion, solar', 'axion, search for', 'coupling, (axion 2photon)', 'magnet, superconducting', 'semiconductor, optical', 'electronics, amplifier']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109041'],"['An x-ray detector for a solar axion search was developed. The detector is operated at 60K in a cryostat of a superconducting magnet. Special care was paid to microphonic noise immunity and mechanical structure against thermal contraction. The detector consists of an array of PIN photodiodes and tailor made preamplifiers. The size of each PIN photodiode is $11\\times 11\\times 0.5\\ {\\rm mm^3}$ and 16 pieces are used for the detector. The detector consists of two parts, the front-end part being operated at a temperature of 60K and the main part in room temperature. Under these circumstances, the detector achieved 1.0 keV resolution in FWHM, 2.5 keV threshold and 6\\times 10^{-5} counts sec^{-1} keV^{-1} cm^{-2} background level.']",['2001-09-05'] +17,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Kachelriess, M', 'Ostapchenko, S']",['Extensive Air Showers from Ultra High Energy Gluinos'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, hadronic component', 'gluino, hadron', 'hadron nucleon, interaction', 'showers, air', 'gluino, search for', 'gluino, mass', 'total cross section, energy dependence', 'cross section, inelastic scattering', 'energy loss', 'energy spectrum', 'Regge poles', 'flux, glueballino', 'proposed experiment, beam dump', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109026'],"['We study the proposal that the cosmic ray primaries above the Greisen-Zatsepin-Kuzmin (GZK) cutoff are gluino-containing hadrons ($\\tilde g$-hadrons). We describe the interaction of $\\tilde g$-hadrons with nucleons in the framework of the Gribov-Regge approach using a modified version of the hadronic interaction model QGSJET for the generations of Extensive Air Showers (EAS). There are two mass windows marginally allowed for gluinos: $m_{\\tilde g}\\lsim 3$ GeV and $25\\lsim m_{\\tilde g}\\lsim 35$ GeV. Gluino-containing hadrons corresponding to the second window produce EAS very different from the observed ones. Light $\\tilde g$-hadrons corresponding to the first gluino window produce EAS similar to those initiated by protons, and only future detectors can marginally distinguish them. We propose a beam-dump accelerator experiment to search for $\\tilde g$-hadrons in this mass window. We emphasize the importance of this experiment: it can discover (or exclude) the light gluino and its role as a cosmic ray primary at ultra high energies.']",['2001-09-04'] +18,['eng'],"['Nusser, A']",['Modified Newtonian Dynamics of Large Scale Structure'],['Astrophysics and Astronomy'],"['Friedman model', 'space-time, Robertson-Walker', 'density, fluctuation', 'forces, gravitation', 'many-body problem', 'astrophysics, missing-mass', 'galaxy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109016'],"[""We examine the implications of Modified Newtonian Dynamics (MOND) on the large scale structure in a Friedmann-Robertson-Walker universe. We employ a ``Jeans swindle'' to write a MOND-type relationship between the fluctuations in the density and the gravitational force, $\\vg$. In linear Newtonian theory, $|\\vg|$ decreases with time and eventually becomes $ 10^{20}$ eV, we compute the average cascade spectra of secondary photons which enter the Earth's atmosphere, and their fluctuations around the average values. It is shown that most photons with parameters of the highest energy AGASA events should initiate cascades in the Earth's magnetosphere with high probability. We suggest that if these events are caused by photons with lower energies but these same arrival directions, than due to fluctuations of the shower development in the magnetosphere and the atmosphere, the primary energies of these events might be wrongly estimated.""]",['2001-09-04'] +20,['eng'],"['Asaoka, Y', 'Shikaze, Y', 'Abe, K', 'Anraku, K', 'Fujikawa, M', 'Fuke, H', 'Imori, M', 'Haino, S', 'Izumi, K', 'Maeno, T', 'Makida, Y', 'Matsuda, S', 'Matsui, N', 'Matsukawa, T', 'Matsumoto, H', 'Matsunaga, H', 'Mitchell, J', 'Mitsui, T', 'Moiseev, A', 'Motoki, M', 'Nishimura, J', 'Nozaki, M', 'Orito, S', 'Ormes, J F', 'Saeki, T', 'Sanuki, T', 'Sasaki, M', 'Seo, E S', 'Sonoda, T', 'Streitmatter, R', 'Suzuki, J', 'Tanaka, K', 'Tanizaki, K', 'Ueda, I', 'Wang, J Z', 'Yajima, Y', 'Yamagami, Y', 'Yamamoto, A', 'Yamamoto, Y', 'Yamato, K', 'Yoshida, T', 'Yoshimura, K']",['Measurements of Cosmic-ray Low-energy Antiproton and Proton Spectra in a Transient Period of the Solar Field Reversal'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'anti-p, cosmic radiation', 'cosmic radiation, energy spectrum', 'flux, ratio', 'time dependence', 'effect, solar', 'magnetic spectrometer, satellite', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109007'],"['The energy spectra of cosmic-ray low-energy antiprotons and protons have been measured by BESS in 1999 and 2000, during a period covering the solar field reversal. Based on these measurements, a sudden increase of the antiproton to proton flux ratio following the solar field reversal was observed as predicted by a drift model of the solar modulation.']",['2001-09-04'] +21,['eng'],"['Capone, A', 'Digaetano, T', 'Grimaldi, A', 'Habel, R', 'Presti, D L', 'Migneco, E', 'Masullo, R', 'Moro, F', 'Petruccetti, M', 'Petta, C', 'Piattelli, P', 'Randazzo, N', 'Riccobene, G', 'Salusti, E', 'Sapienza, P', 'Sedita, M', 'Trasatti, L', 'Ursella, L']",['Measurements of light transmission in deep sea with the AC9 trasmissometer'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'Cherenkov counter, water', 'deep underground detector, water', 'optics, absorption']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109005'],"['The NEMO Collaboration aims to construct an underwater Cerenkov detector in the Mediterranean Sea, able to act as a neutrino telescope. One of the main tasks of this project, which implies difficult technological challenges, is the selection of an adequate marine site. In this framework the knowledge of light transmission properties in deep seawater is extremely important. The collaboration has measured optical properties in several marine sites near the Italian coasts, at depths >3000 m, using a set-up based on a AC9, a commercial trasmissometer, manufactured by WETLabs. The results obtained for the two sites reported in this paper Alicudi and Ustica, show that deep seawater optical properties are comparable to those of the clearest waters.']",['2001-09-04'] +22,['eng'],"['Bhat, P N', 'Acharya, B S', 'Chitnis, V R', 'Da Souza, I A', 'Francis, P J', 'Gothe, K S', 'Joshi, S R', 'Majumdar, P', 'Nagesh, B K', 'Pose, M S', 'Purohit, P N', 'Rahman, M A', 'Rao, K K', 'Rao, S K', 'Sharma, S K', 'Singh, B B', 'Stanislaus, A J', 'Sudershanan, P V', 'Upadhyaya, S S', 'Murthy, B L V', 'Vishwanath, P R']",['Distributed Data Acquisition System for Pachmarhi Array of Cerenkov Telescopes'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'Cherenkov counter', 'optics, reflection', 'photoelectron, amplifier', 'data acquisition', 'programming']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0109003'],"[""Pachmarhi Array of \\v Cerenkov Telescopes (PACT) consists of a 5$\\times$5 array of \\v Cerenkov telescopes deployed over an area of 100 $m$ $\\times$ 80 $m$, in the form of a rectangular matrix. The experiment is based on atmospheric \\v Cerenkov technique using wavefront sampling technique. Each telescope consists of 7 parabolic mirrors mounted para-axially on an equatorial mount. At the focus of each mirror a fast phototube is mounted. In this experiment a large number of parameters have to be measured and recorded from each of the 175 phototubes in the shortest possible time. Further, the counting rates from each phototube as well as the analog sum of the 7 phototubes from each telescope (royal sum) need to be monitored at regular intervals during the run. In view of the complexity of the system, the entire array is divided into four smaller sectors each of which is handled by an independent field signal processing centre (FSPC) housed in a control room that collects, processes and records information from nearby six telescopes that belong to that sector. The distributed data acquisition system (DDAS) developed for the purpose consists of stand-alone sector data acquisition system (SDAS) in each of the four FSPC's and a master data acquisition system (MDAS). MDAS running in the master signal processing centre (MSPC) records data from each of the 25 telescopes. The data acquisition and monitoring PCs (SDAS and MDAS) are networked through LAN. The entire real time software for DDAS is developed in C under $linux$ environment. Most of the hardware in DDAS are designed and fabricated in-house. The design features and the performance of the entire system along with some other auxiliary systems to facilitate the entire observations will be presented.""]",['2001-09-04'] +23,['eng'],"['Takahashi, K', 'Nagataki, S']",['The anisotropy of arrival directions of the cosmic rays around $10^{18} {\\rm eV}$ and VHE neutrinos'],['Astrophysics and Astronomy'],"['cosmic radiation, anisotropy', 'photon p, exclusive reaction', 'n, photoproduction', 'n, flux', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'neutrino, flux', 'p p, inclusive reaction', 'pi, hadroproduction', 'numerical calculations', 'photon p --> n pi+', 'p p --> pi anything']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108507'],"['We show that the observed anisotropy of arrival direction of the cosmic rays around $10^{18}$eV is naturally explained by neutrons produced by collisions between ambient matter and protons which are accelerated up to $\\sim 10^{19}$eV at the Galactic center. The detection of VHE neutrinos from the Galactic center will allow us to distinguish our model and probe the composition of the CRs. As for the expected event rate for the planned 1 km$^{3}$ detectors such as ICECUBE, ANTARES and NESTOR is $\\sim$ 0.84 km$^{-2}$ year$^{-1}$. The neutrino detectability is dramatically improved when neutrino oscillation is taken into account, because tau leptons are produced due to the Earth-skimming effect. The expected event rate for Telescope Array becomes $\\sim$ 0.3 year$^{-1}$ when the Earth-skimming effect is taken into consideration. If the CRs contain substantial neutrons as in our model and the angular resolution is enough high, the acceleration region of the CRs below $\\sim 10^{19}$eV will be determined accurately, which should help our understanding on the particle acceleration.']",['2001-09-03'] +24,['eng'],"['Weekes, T C']",['VERITAS'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'Cherenkov counter, imaging', 'optics, reflection', 'photoelectron, amplifier', 'energy resolution', 'angular resolution', 'electronics', 'AGN', 'supernova', 'pulsar', 'gamma ray burst', 'neutralino, annihilation', 'astrophysics', 'black hole', 'quantum gravity', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108478'],"['The Very Energetic Radiation Imaging Telescope Array System (VERITAS) represents an important step forward in the study of extreme astrophysical processes in the universe. It combines the power of the atmospheric Cherenkov imaging technique using a large optical reflector with the power of stereoscopic observatories using arrays of separated telescopes looking at the same shower. The seven identical telescopes in VERITAS, each of aperture 10 m, will be deployed in a filled hexagonal pattern of side 80 m; each telescope will have a camera consisting of 499 pixels with a field of view of 3.5 deg VERITAS will substantially increase the catalog of very high energy (E > 100GeV) gamma-ray sources and greatly improve measurements of established sources.']",['2001-08-30'] +25,['eng'],"['Mori, M']",['GeV-TeV Gamma-ray Astronomy'],['Astrophysics and Astronomy'],"['review, experimental results', 'photon, cosmic radiation', 'cosmic radiation, energy', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'upper limit', 'pulsar', 'supernova', 'AGN', 'gamma ray burst', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108463'],"['Recent results of GeV and TeV observations of gamma-rays from the Universe are briefly reviewed. Topics include observational technique, diffuse gamma-rays, pulsars, unidentified sources, plerions, supernova remnants and AGNs.']",['2001-08-30'] +26,['eng'],"['Chitnis, V R', 'Acharya, B S', 'Bhat, P N', 'Gothe, K S', 'John, A V', 'Majumdar, P', 'Nagesh, B K', 'Rahman, M A', 'Singh, B B', 'Upadhyaya, S S', 'Murthy, B L V', 'Vishwanath, P R']",['Pachmarhi Array of \\v{C}erenkov Telescopes and its Sensitivity'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'Cherenkov counter', 'photoelectron, amplifier', 'optics, reflection', 'energy, threshold']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108455'],"['Pachmarhi Array of \\v{C}erenkov Telescopes (PACT) has been designed to search for celestial TeV $\\gamma-$rays using the wavefront sampling technique. PACT, located at Pachmarhi, (latitude 22$^\\circ$ 28$^\\prime$ N, longitude 76$^\\circ$ 26$^\\prime$ E, altitude 1075 m) consists of 25 telescopes deployed over an area of 80 m $\\times$ 100m. Each telescopes consists of 7 parabolic reflectors, each viewed by a fast phototube behind a 3$^\\circ$ mask at the focus. The density and the arrival time of the photons at the PMT are recorded for each shower. The energy threshold and collection area of the array are estimated, from Monte Carlo simulations, to be $\\sim$ 900 GeV and 10$^5$ m$^2$ respectively. The accuracy in determination of arrival angle of a shower is estimated to be about 0.1$^\\circ$ in the near vertical direction. About 99% of the off-axis hadronic events could be rejected from directional information alone. Further, at least 75% of the on-axis hadronic events could be rejected using species sensitive parameters derived from timing and density measurements. These cuts on data to reject background would retain $\\sim$ 44% of the $\\gamma-$ray signal. The sensitivity of the array for a 5$\\sigma$ detection of $\\gamma-$ray signal at a threshold energy of 1 TeV has been estimated to be $\\sim$ 4.1 $\\times$ 10$^{-12}$ photons cm$^{-2}$ s$^{-1}$ for an on source exposure of 50 hours. The PACT set-up has been fully commissioned and is collecting data. The details of the system parameters and sensitivity will be presented.']",['2001-08-29'] +27,['eng'],"['Beall, J H', 'Bednarek, W']","['Neutrinos from Early-Phase, Pulsar-Driven Supernovae']",['Astrophysics and Astronomy'],"['supernova', 'pulsar', 'neutrino, cosmic radiation', 'n, matter', 'p, acceleration', 'photon p, scattering', 'pi, photoproduction', 'pi, leptonic decay', 'neutrino/mu, flux', 'magnetic field', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108447'],"['Neutron stars, just after their formation, are surrounded by expanding, dense, and very hot envelopes which radiate thermal photons. Protons can be accelerated in the wind zones of such energetic pulsars to very high energies. These protons lose energy efficiently in collisions with thermal photons and with the matter of the envelope, mainly via pion production. When the temperature of radiation inside the envelope of supernovae drops below ~ 3x10^6 K, these pions decay before losing energy and produce high energy neutrinos. We estimate the flux of muon neutrinos emitted during such an early phase of the pulsar - supernova envelope interaction. We find that a 0.1 km^2 neutrino detector should be able to detect on the order of hundreds of neutrinos above 1 TeV within about one year after the explosion from a supernova in our Galaxy. This result holds if these pulsars have surface magnetic fields typical of those observed for radio pulsars, and for initial periods on the order of a few milliseconds when the pulsar is formed.']",['2001-08-29'] +28,['eng'],"['Aharonian, F A', 'Timokhin, A N', 'Plyasheshnikov, A V']",['On the origin of highest energy gamma-rays from Mkn 501'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'blazar', 'cosmic radiation, primary', 'cosmic radiation, background', 'photon, absorption', 'cosmic radiation, energy spectrum', 'cosmic radiation, cascade', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108419'],"['The spectra of very high energy gamma-radiation observed from distant extragalactic objects suffer significant deformations during the passage of primary gamma-rays through the intergalactic medium. The recently reported fluxes of diffuse infrared background radiation indicate that we detect, most probably, heavily absorbed TeV radiation from BL Lac objects Mkn 421 and Mkn 501, especially at energies above 10 TeV. This implies that the source spectrum of Mkn 501 corrected for the intergalactic absorption may contain a sharp-pile which generally contradicts to the predictions of current models of TeV emission of BL Lac objects, and thus leads to the so-called ""IR-TeV crisis"". To overcome this difficulty, in this paper we study two possibilities assuming that (i) the TeV gamma-rays from Mkn 501 have a secondary origin, i.e. are formed during development of electron-photon cascades in the intergalactic medium initiated by primary gamma-rays; (ii) the pile-up in the source spectrum is a result of comptonization (in deep Klein-Nishina regime) of ambient optical radiation by the ultrarelativistic cold conical outflow (jet) with bulk motion Lorentz factor \\Gamma ~ 3.3 x 10^7. We show that the first hypothesis cannot reproduce the spectral shape of the TeV emission from Mkn 501. At the same time we demonstrate that the inverse Compton radiation of the ultrarelativistic cold jet hypothesis can quite satisfactorily explain the unusual spectral features of the ""reconstructed"" TeV radiation. We briefly discuss the astrophysical implications of this hypothesis.']",['2001-08-28'] +29,['eng'],"['Wetterich, C']",['Are Galaxies Cosmon Lumps?'],['Astrophysics and Astronomy'],"['galaxy', 'field theory, scalar', 'cosmon', 'quintessence', 'gravitation', 'mass', 'velocity, rotational', 'black hole, singularity']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108411'],"[""The scalar ``cosmon'' field mediating quintessence influences the dynamics of extended objects in the universe. We discuss cosmon lumps -- spherically symmetric solutions for the scalar field coupled to gravity. The two integration constants can be associated to the mass and the rotational velocity in a halo-like region with constant rotation curve. The presence of the scalar field also changes the singularity of the black hole solution. We ask if galaxies could be associated with cosmon lumps.""]",['2001-08-28'] +30,['eng'],"[""O'Neill, S"", 'Olinto, A V', 'Blasi, P']",['Galactic Magnetic Field Structure and Ultra High Energy Cosmic Ray Propagation'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'nucleus, cosmic radiation', 'cosmic radiation, trajectory', 'magnetic field, galaxy', 'iron, antinucleus', 'cosmic radiation, energy spectrum', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108401'],"['We consider the effects of the Galactic magnetic field on the propagation of ultra high energy cosmic rays (UHECRs). By employing two methods of trajectory simulation, we investigate the possibility that UHECRs are produced within the Galaxy with paths strongly influenced by the Galactic magnetic field. Such trajectories have the potential to reconcile the existing conflict between proposed local sources and isotropic UHECR arrival directions.']",['2001-08-27'] +31,['eng'],"['Vishwanath, P R']",['Lateral Distribution Studies for the PACT Experiment'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'photon, showers', 'showers, spatial distribution', 'radiation, Cherenkov', 'cosmic radiation, energy', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108393'],"['Monte Carlo calculations have been done to study the possibilities of using different spatial distributions, local fluctuations and the number of Cerenkov photons in gamma ray showers to increase the sensitivity of the PACT experiment. After matching the trigger rates in data with the predictions of simulations, the energy threshold of the array for gamma rays is found to be about 900 GeV. It is shown that a lateral distribution parameter $\\beta$ can increase the signal to noise ratio in the experiment. A typical season of 15 nights should be able to conclusively establish any source with Crab level fluxes. Two other possible parameters for increase of sensitivity are also discussed. Preliminary results on the application of the $\\beta$ parameter to the data from PACT experiment are discussed.']",['2001-08-27'] +32,['eng'],"['Cowsik, R', 'Bhat, P N', 'Chitnis, V R', 'Acharya, B S', 'Vishwanath, P R']",['A Possible High Altitude High Energy Gamma Ray Observatory in India'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'Cherenkov counter', 'photoelectron, amplifier', 'optics, reflection', 'particle identification, (hadron photon)']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108392'],"['Recently an Indian Astronomical Observatory has been set up at Hanle (32$^\\circ$ 46$^\\prime$ 46$^{\\prime\\prime}$ N, 78$^\\circ$ 57$^\\prime$ 51$^{\\prime\\prime}$ E, 4515m amsl) situated in the high altitude cold desert in the Himalayas. The Observatory has 2-m aperture optical-infrared telescope, recently built by the Indian Institute of Astrophysics. We have carried out systematic simulations for this observation level to study the nature of \\v{C}erenkov light pool generated by gamma ray and proton primaries incident vertically at the top of the atmosphere. The differences in the shape of the lateral distributions of \\v{C}erenkov light with respect to that at lower altitudes is striking. This arises primarily due to the proximity of the shower maximum to the observation site. The limited lateral spread of the \\v{C}erenkov light pool and near 90% atmospheric transmission at this high altitude location makes it an ideal site for a gamma ray observatory. This results in a decrease in the gamma ray energy threshold by a factor of 2.9 compared to that at sea-level. Several parameters based on density and timing information of \\v{C}erenkov photons, including local and medium range photon density fluctuations as well as photon arrival time jitter could be efficiently used to discriminate gamma rays from more abundant cosmic rays at tens of GeV energies.']",['2001-08-27'] +33,['eng'],"['Bhat, P N', 'Chitnis, V R']",['Gamma-Hadron Separation using \\v{C}erenkov Photon Density Fluctuations'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'Cherenkov counter', 'photoelectron, amplifier', 'particle identification, (hadron photon)', 'photon, density', 'statistical analysis']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108391'],"['In atmospheric \\v{C}erenkov technique $\\gamma-$rays are detected against abundant background produced by hadronic showers. In order to improve signal to noise ratio of the experiment, it is necessary to reject a significant fraction of hadronic showers. The temporal and spectral differences, the lateral distributions and density fluctuations of \\v{C}erenkov photons generated by $\\gamma-$ray and hadron primaries are often used for this purpose. Here we study the differences in \\v{C}erenkov photon density fluctuations at the observation level based on Monte Carlo simulations. Various types of density fluctuations like the short range (or local), medium range fluctuations and flatness parameter are studied. The estimated quality factors reflect the efficiencies with which the hadrons can be rejected from the data. It has been found that we can reject around 80% of proton showers while retaining about 70% of $\\gamma-$ray showers in the data, based only on the differences in the flatness parameter. Density fluctuations particularly suited for wavefront sampling observations seem to be a good technique to improve the signal to noise ratio.']",['2001-08-27'] +34,['eng'],"['Vishwanath, P R', 'Acharya, B S', 'Bhat, P N', 'Chitnis, V R', 'Majumdar, P', 'Rahman, M A', 'Singh, B B']",['Very High Energy Gamma Ray Emission from Crab and Geminga Pulsars'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'pulsar', 'Cherenkov counter, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108385'],"[""The main inference from the experiments of the '80s that the time-averaged energy spectra of pulsars had to steepen in the GeV-TeV energy region has been reinforced in the '90s from experiments with higher sensitivities. However, results from several experiments from the past and the more sensitive experiments at present can be reconciled by invoking a possibly different component arising in the TeV region. The results of the preliminary analysis of the data being collected with the PACT array will be presented.""]",['2001-12-14'] +35,['eng'],"['Vishwanath, P R', 'Acharya, B S', 'Bhat, P N', 'Chitnis, V R', 'Majumdar, P', 'Rahman, M A', 'Singh, B B']",['Very High Energy Gamma Ray Emission from Crab Nebula with the PACT Array'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, angular distribution', 'Cherenkov counter, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108372'],"['The Crab nebula has proved to be the nearest to a standard candle in VHE $\\gamma-$ ray astronomy. Results on the gamma ray emission from the nebula at various energies have come in the last decade mostly from imaging telescopes. The aim of the new Pachmarhi Atmospheric Cerenkov Telescope (PACT) array has been to use the temporal and spatial distribution of Cerenkov photons in distinguishing between proton and gamma ray showers. The array, with timing information from 175 mirrors, is ideally suited for precise estimation of the arrival direction. Preliminary results from the recent data taken on Crab has shown a 12$\\sigma$ signal with the flux in good agreement with those of the other experiments.']",['2001-08-24'] +36,['eng'],"['Kogan, I I']",['Brane world-ultralight states and multigravity'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2001/03/10', 'gravitation, model', 'Kaluza-Klein model', 'membrane model', 'higher-dimensional', 'graviton, massive', 'astrophysics, missing-mass', 'quintessence', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108220'],"['This is a talk presented at XXXVIth Rencontres de Moriond, ElectroWeak Interactions and Unified Theories, March 2001. A short review of modern status of multigravity, i.e. modification of gravity at both short and large distances is given.']",['2001-08-14'] +37,['eng'],"['Horowitz, C J']",['Supernova SN1987A Bound on Neutrino Spectra for R-Process Nucleosynthesis'],['Astrophysics and Astronomy'],"['supernova', 'neutrino, cosmic radiation', 'light nucleus, production', 'electron, yield', 'energy dependence', 'antineutrino, energy', 'antineutrino, luminosity', 'conservation law', 'lepton number', 'neutrino, sterile', 'neutrino, oscillation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0108113'],"['The neutrino driven wind during a core collapse supernova is an attractive site for r-process nucleosynthesis. The electron fraction $Y_e$ in the wind depends on observable neutrino energies and luminosities. The mean antineutrino energy is limited by supernova SN1987A data while lepton number conservation constrains the ratio of antineutrino to neutrino luminosities. If $Y_e$, in the wind, is to be suitable for rapid neutron capture nucleosynthesis, then the mean electron neutrino energy may be significantly lower then that predicted in present supernova simulations, or there may be new neutrino physics such as oscillations to sterile neutrinos.']",['2001-08-08'] +38,['eng'],"['Mondragón, A', 'Allen, R E']",['Vacuum Energy Tuned by Effective Volume of Internal Space'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'energy, vacuum state', 'tensor, energy-momentum', 'gravitation', 'superfluid, velocity', 'gauge field theory, SU(2) x U(1)', 'condensation', 'instanton']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103161'],['We investigate the viability of a proposal that the vacuum stress-energy tensor is naturally tuned to zero in the vacuum state (and nearly to zero in a state with matter present) through cancellation of a negative contribution from condensed Higgs fields and a positive contribution from the other bosonic and fermionic fields. The parameter which does the tuning is the effective volume of an internal space. In the present paper we find that this parameter can range arbitrarily over all positive values.'],['2001-03-13'] +39,['eng'],"['Overduin, J', 'Priester, W']",['How dominant is the vacuum?'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'vacuum state, energy', 'baryon', 'matter, exotic', 'neutrino', 'Einstein equation', 'axion', 'WIMP', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101484'],"[""It would be hard to find a cosmologist today who does not believe that the vast bulk of the Universe (ninety-five percent or more) is hidden from our eyes. We review the evidence for this remarkable consensus, and for the latest proposal, that the mysterious dark matter consists of as many as {\\em four separate ingredients}: baryons, massive neutrinos, ``exotic'' dark matter particles, and vacuum energy, also known as the cosmological constant (Lambda). Of these, only baryons fit within standard theoretical physics; the others, if their existence is confirmed, will mean rewriting textbooks. New experimental evidence has recently appeared for and against all four components, so that the subject is in a state of turmoil and excitement. The past three years in particular have seen the fourth (vacuum) component come into new prominence, largely at the expense of the third (exotic dark matter). We conclude our review by exploring the possibility that the energy density of the vacuum is in fact so dominant as to leave little room for significant amounts of exotic dark matter.""]",['2001-01-29'] +40,['eng'],"['Pina-Avelino, P', 'Martins, C J A P']",['Primordial Gaussian Fluctuations from Cosmic Defects'],['Astrophysics and Astronomy'],"['gravitation, model', 'defect, topological', 'density, perturbation', 'defect, network']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006303'],"[""We extend our recent work on ``two-metric'' theories of gravity by showing how in such models cosmic defects can produce a spectrum of primordial Gaussian density perturbations. This will happen when the speed characterising the decay products of the defect network is much larger than the speed characterising gravity and all standard model particles. This model will exactly mimic all the standard predictions of inflationary models, and the only way of distinguishing the two will be via the detection of the decay products of the network.""]",['2000-06-22'] +41,['eng'],"['Kino, M', 'Takahara, F', 'Kusunose, M']",['Energetics of Tev Blazars and Physical Constraints on their Emission Regions'],['Astrophysics and Astronomy'],"['blazar', 'cosmic radiation, emission', 'electron, energy spectrum', 'energy, density', 'magnetic field', 'photon, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107436'],"['Using multi-frequency spectra from TeV blazars in quiescent states, we obtain the physical parameters of the emission region of blazars within the framework of the one-zone synchrotron self-Compton (SSC) model. We numerically calculate the steady-state energy spectra of electrons by self-consistently taking into account the effects of radiative cooling with a proper account of the Klein-Nishina effects. Here electrons are assumed to be injected with a power-law spectrum and to escape on a finite time scale, which naturally leads to the existence of a break energy scale. Although we do not use time variabilities but utilize a model of electron escape to constrain the size of the emission region, the resultant size turns out to be similar to that obtained based on time variabilities. Through detailed comparison of the predicted emission spectra with observations, we find that for Mrk 421, Mrk 501, and PKS 2155--304, the energy density of relativistic electrons is about an order of magnitude larger than that of magnetic fields with an uncertainty within a factor of a few.']",['2001-07-24'] +42,['eng'],"['Covault, C E', 'Boone, L M', 'Bramel, D', 'Chae, E', 'Fortin, P', 'Gingrich, D M', 'Hinton, J A', 'Hanna, D S', 'Mukherjee, R', 'Ong, R A', 'Ragan, K', 'Scalzo, R A', 'Schütte, D R', 'Theoret, C G', 'Williams, D A', 'Müller, C']",['The Status of the STACEE Observatory'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'radiation, Cherenkov', 'photoelectron, amplifier', 'electronics', 'analog-to-digital converter']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107427'],"['The Solar Tower Atmospheric Cherenkov Effect Experiment (STACEE) is a ground-based instrument designed to study astrophysical sources of gamma radiation in the energy range of 50 to 500 GeV. STACEE uses an array of large heliostat mirrors at the National Solar Thermal Test Facility in Albuquerque, New Mexico, USA. The heliostats are used to collect Cherenkov light produced in gamma-ray air showers. The light is concentrated onto an array of photomultiplier tubes located near the top of a tower. The construction of STACEE started in 1997 and has been completed in 2001. During the 1998-99 observing season, we used a portion of the experiment, STACEE-32, to detect gamma-rays from the Crab Nebula. The completed version of STACEE uses 64 heliostat mirrors, having a total collection area of 2300 m^2. During the last year, we have also installed custom electronics for pulse delay and triggering, and 1 GHz Flash ADCs to read out the photomultiplier tubes. The commissioning of the full STACEE instrument is underway. Preliminary observations and simulation work indicate that STACEE will have an energy threshold below 70 GeV and a reach for extragalactic gamma-ray sources out to redshift of ~1.0. In this paper we describe the design and performance of STACEE.']",['2001-07-24'] +43,['eng'],"['Riazuelo, A', 'Uzan, J P']",['Cosmological observations in scalar-tensor quintessence'],['Astrophysics and Astronomy'],"['quintessence', 'field theory, scalar', 'field theory, tensor', 'gravitation, fundamental constant', 'fundamental constant, time variation', 'light nucleus, production', 'supernova, model', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, perturbation', 'potential', 'supergravity', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107386'],"['The framework for considering the astronomical and cosmological observations in the context of scalar-tensor quintessence in which the quintessence field also accounts for a time dependence of the gravitational constant is developed. The constraints arising from nucleosynthesis, the variation of the constant and the post-Newtonian measurements are taken into account. A simple model of supernovae is presented in order to extract the dependence of their light curves with the gravitational constant; this implies a correction when fitting the luminosity distance. The properties of perturbations as well as CMB anisotropies are also investigated.']",['2001-07-20'] +44,['eng'],"['Corasaniti, P S', 'Copeland, E J']",['Constraining the quintessence equation of state with SnIa data and CMB peaks'],['Astrophysics and Astronomy'],"['supernova', 'quintessence', 'energy, density', 'cosmic radiation, background', 'cosmic radiation, spectra', 'cosmic radiation, anisotropy', 'dark energy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107378'],"['Quintessence has been introduced as an alternative to the cosmological constant scenario to account for the current acceleration of the universe. This new dark energy component allows values of the equation of state parameter $w_{Q}\\geq-1$, and in principle measurements of cosmological distances to Type Ia supernovae can be used to distinguish between these two types of models. Assuming a flat universe, we use the supernovae data and measurements of the position of the acoustic peaks in the Cosmic Microwave Background (CMB) spectra to constrain a rather general class of quintessence potentials, including inverse power law models and recently proposed Supergravity inspired potentials. The likelihood analysis gives an upper limit on the present value of the equation of state parameter, $-1\\leq w_{Q}^0\\leq-0.96$ at $2\\sigma$, a result that appears to rule out a class of recently proposed potentials.']",['2001-07-20'] +45,['eng'],"['Lara, J F']",['Neutrino Heating in an Inhomogeneous Big Bang Nucleosynthesis Model'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/11', 'astrophysics, model', 'light nucleus, production', 'electron positron, annihilation', 'electron nucleon, interaction', 'neutrino, production', 'Boltzmann equation', 'transport theory', 'diffusion', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107360'],"['The effect of the heating of neutrinos by scattering with electrons and positrons and by e-e+ annihilation on nucleosynthesis is calculated for a spherically symmetric baryon inhomogeneous model of the universe. The model has a high baryon density core and a low density outer region. The heating effect is calculated by solving the Boltzmann Transport Equation for the distribution functions of electron and muon/tau neutrinos. For a range of baryon-to-photon ratio = [ 0, 1.5 ] x 10^-10 and distance scale = [ 10^2, 10^8 ] cm the heating effect increases the mass fraction of He4 by a range of [1, 2] x 10^-4. The change of the value of the mass fraction of He4 appears similiar to the change caused by an upward shift in the value of the baryon-to-photon ratio. But the change to deuterium is a decrease in abundance ratio Y(d)/Y(p) on the order of 10^-3, one order less than the decrease due to a shift in baryon-to-photon ratio.']",['2001-07-20'] +46,['eng'],"['Blanch, O', 'López, J', 'Martínez, M']",['Testing the effective scale of Quantum Gravity with the next generation of Gamma Ray Telescopes'],['Astrophysics and Astronomy'],"['quantum gravity, validity test', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, horizon', 'violation, Lorentz', 'time delay, energy dependence', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107334'],"['The actual potential of the next generation of Gamma Ray Telescopes in improving the existing tests of an effective Quantum Gravity scale from the study of the propagation delay for gamma rays of different energies coming from a distant astrophysical source is discussed. It is shown that the existence of a cosmological Gamma Ray Horizon, will impose very demanding conditions on the observations of the telescopes to try to test a Quantum Gravity scale close to the Planck mass.']",['2001-07-19'] +47,['eng'],"['Terrero-Escalante, C A', 'Garcia, A A']",['Is the observable Universe generic?'],['Astrophysics and Astronomy'],"['talk, Huatulco 2000/12/03', 'inflationary universe', 'potential', 'perturbation, tensor', 'perturbation, scalar', 'cosmic radiation, background', 'cosmic radiation, spectra', 'scaling, dependence', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107325'],['Recently an inflationary potential yielding power spectra characterized by a scale-invariant tensorial spectral index and a scale-dependent scalar spectral index was introduced. We analize here the implications that this potential could have for the large-scale structure formation in the multiverses scenario of eternal inflation.'],['2001-07-19'] +48,['eng'],"['Ng, S C C', 'Nunes, N J', 'Rosati, F']",['Applications of scalar attractor solutions to Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'field theory, scalar', 'fluid, background', 'phase space', 'attractor, scalar', 'quintessence', 'inflationary universe', 'space-time, Robertson-Walker', 'energy, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107321'],"['We develop a framework to study the phase space of a system consisting of a scalar field rolling down an arbitrary potential with varying slope and a background fluid, in a cosmological setting. We give analytical approximate solutions of the field evolution and discuss applications of its features to the issues of quintessence, moduli stabilisation and quintessential inflation.']",['2001-07-18'] +49,['eng'],"['Berezinsky, Veniamin Sergeevich']",['Puzzles in astrophysics in the past and present'],['Astrophysics and Astronomy'],"['review, Venice 2001/03/06', 'astrophysics, history', 'cosmic radiation, absorption', 'violation, Lorentz', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'GZK effect', 'gamma ray burst', 'cosmic radiation, particle source', 'astrophysics, string', 'interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107306'],"['About 400 years have passed since the great discoveries by Galilei, Kepler and Newton, but astronomy still remains an important source of discoveries in physics. They start with puzzles, with phenomena difficult to explain, and which in fact need for explanation the new physics. Are such puzzles existing now? There are at least three candidates: absence of absorption of TeV gamma radiation in extragalactic space (violation of Lorentz invariance?), absence of GZK cutoff in the spectrum of Ultra High Energy Cosmic Rays (new particle physics?), tremendous energy (up to $10^{54}$ ergs) released in Gamma Ray Bursts during a time scale of a second (collapsing stars or sources of a new type?). Do these puzzles really exist? A critical review of these phenomena is given.']",['2001-07-18'] +50,['eng'],"['De la Calle-Perez, I', 'Contreras, J L', 'Cortina, J', 'Fonseca, V']",['A possible use for polarizers in imaging atmospheric Cherenkov telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, primary', 'showers, air', 'radiation, Cherenkov', 'radiation, polarization', 'photoelectron, amplifier', 'particle identification, (hadron photon)', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107271'],"['Cherenkov radiation produced in Extensive Air Showers shows a net polarization. This article discusses its properties and physical origin, and proposes an arrangement of polarizers potentially useful for Imaging Atmospheric Cherenkov Telescopes.']",['2001-07-17'] +51,['eng'],"['Loredo, T J', 'Lamb, D Q']",['Bayesian analysis of neutrinos observed from supernova SN 1987A'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'supernova', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'antineutrino/e, mass', 'counters and detectors, efficiency', 'positron, neutrinoproduction', 'statistical analysis', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107260'],"['We present a Bayesian analysis of the energies and arrival times of the neutrinos from supernova SN 1987A detected by the Kamiokande II, IMB, and Baksan detectors, and find strong evidence for two components in the neutrino signal: a long time scale component from thermal Kelvin-Helmholtz cooling of the nascent neutron star, and a brief (~< 1 s), softer component similar to that expected from emission by accreting material in the delayed supernova scenario. In the context of this model, we show that the data constrain the electron antineutrino rest mass to be less than 5.7 eV with 95% probability. Our analysis takes advantage of significant advances that have occured in the years since the detections in both our understanding of the supernova mechanism and our ability to analyze sparse data. As a result there are substantial differences between our inferences and those found in earlier studies. We find that two-component models for the neutrino signal make the data >100 times more probable than single-component models. In addition, the radius and binding energy of the nascent neutron star implied by single-component models deviates significantly from the values predicted by current neutron star models, whereas those implied by models with an accretion component are in complete agreement with the predictions. As a result, two-component models are hundreds to thousands of times more probable than single-component models. The neutrino data thus provide the first direct observational evidence in favor of the delayed supernova scenario over the prompt scenario. (Abridged abstract)']",['2001-07-17'] +52,['eng'],"['Malkov, M A', 'Diamond, P H', 'Jones, T W']",['Intrinsic energy cut-off in diffusive shock acceleration'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'cosmic radiation, acceleration', 'shock waves', 'diffusion', 'particle, confinement', 'energy, density', 'p, cosmic radiation', 'supernova', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107259'],"['The linear theory of shock acceleration predicts the maximum particle energy to be limited only by the acceleration time and the size of the shock. We study the combined effect of acceleration nonlinearity (shock modification by accelerated particles, that must be present in strong astrophysical shocks) and propagation of Alfven waves that are responsible for particle confinement to the shock front. We show that wave refraction to larger wave numbers in the nonlinearly modified flow causes enhanced losses of particles in the momentum range p_max/R < p < p_max, where R>1 is the nonlinear pre-compression of the flow and p_max is a conventional maximum momentum, that could be reached if there was no refraction.']",['2001-07-17'] +53,['eng'],"['Ahluwalia, D V', 'Kirchbach, M']",['Primordial space-time foam as an origin of cosmological matter-antimatter asymmetry'],['Astrophysics and Astronomy'],"['space-time, foam', 'matter, asymmetry', 'antimatter', 'spin, 1/2', 'space-time, fluctuation', 'fundamental constant, fine structure', 'invariance, gauge']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107246'],"['The possibility is raised that the observed cosmological matter-antimatter asymmetry may reside in asymmetric space-time fluctuations and their interplay with the St\\""ckelberg-Feynman interpretation of antimatter. The presented thesis also suggests that the effect of space-time fluctuations is to diminish the fine structure constant in the past. Recent studies of the QSO absorption lines provide a 4.1 standard deviation support for this prediction. Our considerations suggest that in the presence of space-time fluctuations, the principle of local gauge invariance, and the related notion of parallel transport, must undergo fundamental changes.']",['2001-07-16'] +54,['eng'],"['Bridgman, H A', 'Malik, K A', 'Wands, D']",['Cosmological perturbations in the bulk and on the brane'],['Astrophysics and Astronomy'],"['Friedman model', 'space-time, perturbation', 'membrane model', 'perturbation, linear', 'matter, perturbation', 'invariance, gauge', 'gauge, longitudinal', 'dimension, 5', 'dimension, 4', 'tensor, Weyl', 'matter, density', 'momentum', 'pressure']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107245'],"['We study cosmological perturbations in a brane-world scenario where the matter fields live on a four-dimensional brane and gravity propagates in the five-dimensional bulk. We present the equations of motion in an arbitrary gauge for metric perturbations in the bulk and matter perturbations on the brane. Gauge-invariant perturbations are then constructed corresponding to perturbations in longitudinal and Gaussian normal gauges. Longitudinal gauge metric perturbations may be directly derived from three master variables (separately describing scalar, vector and tensor metric perturbations) which obey five-dimensional wave-equations. Gaussian normal gauge perturbations are directly related to the induced metric perturbations on the brane with the additional bulk degrees of freedom interpreted as an effective Weyl energy-momentum tensor on the brane. We construct gauge-invariant perturbations describing the effective density, momentum and pressures of this Weyl fluid at the brane and throughout the bulk. We show that there exist gauge-invariant curvature perturbations on the brane and in the bulk that are conserved on large-scales when three-dimensional spatial gradients are negligible.']",['2001-07-16'] +55,['eng'],"['Zhu, Z H', 'Fujimoto, M K', 'Tatsumi, D']",['Determining the Cosmic Equation of State Using Future Gravitational Wave Detectors'],['Astrophysics and Astronomy'],"['gravitational radiation', 'counters and detectors', 'dark energy', 'fluid, exotic', 'n, matter', 'mass spectrum', 'binary', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107234'],"['The expected chirp mass distribution of observed events for future gravitational wave detectors is extensively investigated in the presence of an exotic fluid component with an arbitrary equation of state, $-1 \\leq \\omega_x \\equiv p_x/\\rho_x < 0$, i.e., the so-called dark energy component. The results for a flat model dominated by a dark energy are compared to those for the standard flat model dominated by cold dark matter. It is found that for a flat universe the chirp mass distribution shows a sensitive dependence on $\\omega_x$, which may provide an independent and robust constraint on the cosmic equation of state.']",['2001-07-16'] +56,['eng'],"['Wagoner, R V', 'Hennawi, J F', 'Liu, J']",['Gravitational Radiation Evolution of Accreting Neutron Stars'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'n, matter', 'matter, accretion', 'gravitational radiation', 'superfluid', 'amplitude analysis', 'temperature, oscillation', 'viscosity', 'temperature, dependence', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107229'],"['The gravitational-wave and accretion driven evolution of neutron stars in low mass X-ray binaries and similar systems is analyzed, while the amplitude of the radiating perturbation (here assumed to be an r-mode) remains small. If most of the star is superfluid, with (temperature independent) mutual friction dominating the ordinary (temperature dependent) shear viscosity, the amplitude of the mode and the angular velocity of the star oscillate about their equilibrium values with a period of at least a few hundred years. The resulting oscillation of the neutron star temperature is also computed. For temperature dependent viscosity, the general conditions for the equilibrium to be stable are found.']",['2001-07-16'] +57,['eng'],"['Sigurdsson, S']",['Experimental hints of Gravity in Large Extra Dimensions?'],['Astrophysics and Astronomy'],"['gravitation', 'space-time, higher-dimensional', 'coalescence', 'angular momentum', 'spontaneous compactification', 'proposed experiment']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107169'],"[""Recent conjectures suggest the universe may have large extra dimensions, through which gravity propagates. This implies gross departures from Newton's law of gravity at small length scales. Here I consider some implications for particle dynamics on scales comparable to the compactification radius, $R_c \\ltorder 1$ mm. During planet formation, coalescence of micron sized dust grains to planetesimals is a rate critical step. Blum et al (2000) found dust grain aggregates form low fractal dimension structures in microgravity, consistent with high angular momentum coalescence. I consider the effects of non-Newtonian gravity on dust aggregation on scales less than $R_c$ and show they naturally coalesce into low dimensional structures with high specific angular momentum. We infer $R_c \\approx 80$ microns.""]",['2001-07-11'] +58,['eng'],"['Lin, W']",['Remark on the Theory of Cosmological Perturbation'],['Astrophysics and Astronomy'],"['astrophysics, model', 'density, perturbation', 'spectra, perturbation', 'dependence, gauge', 'cosmic radiation, background', 'temperature, fluctuation', 'astrophysics, missing-mass', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107162'],"['It is generally predicted that there exists non-vanishing power spectrum for the wavenumbers outside the Hubble radius in the inflationary scenario. The power spectrums differ dramatically for these wavenumbers in different gauges, so we must adopt a proper power spectrum to calculate the predictions of the cosmological model. In this paper I try to show that the power spectrum defined in the Synchronous Gauge can not be directly used to calculate the predictions of cosmological models on the large-scale structure of universe. These predictions should be calculated directly by the gauge-invariant power spectrum which characterizes the density fluctuation relative to the unperturbed expanding background of universe, or, by the power spectrum defined in the Newtonian Gauge.']",['2001-07-10'] +59,['eng'],"['Krennrich, F', 'Badran, H M', 'Bond, I H', 'Bradbury, S M', 'Buckley, J H', 'Carter-Lewis, D A', 'Catanese, M', 'Cui, W', 'Dunlea, S', 'Das, D', 'De la Calle-Perez, I', 'Fegan, D J', 'Fegan, S J', 'Finley, J P', 'Gaidos, J A', 'Gibbs, K', 'Gillanders, G H', 'Hall, T A', 'Hillas, A M', 'Holder, J', 'Horan, D', 'Jordan, M', 'Kertzman, M P', 'Kieda, D B', 'Kildea, J', 'Knapp, J', 'Kosack, K', 'Lang, M J', 'Le Bohec, S', 'McKernan, B', 'Moriarty, P', 'Müller, D', 'Ong, R', 'Pallassini, R', 'Petry, D', 'Quinn, J', 'Reay, N W', 'Reynolds, P T', 'Rose, H J', 'Sembroski, G H', 'Sidwell, R A', 'Stanton, N', 'Swordy, S P', 'Vasilev, V', 'Wakely, S P', 'Weekes, T C']",['Cutoff in the TeV Energy Spectrum of Markarian 421 During Strong Flares in 2001'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'blazar', 'cosmic radiation, energy spectrum', 'statistical analysis', 'energy, density', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107113'],"['Exceptionally strong and long lasting flaring activity of the blazar Markarian 421 (Mrk 421) occurred between January and March 2001. Based on the excellent signal-to-noise ratio of the data we derive the energy spectrum between 260 GeV - 17 TeV with unprecedented statistical precision. The spectrum is not well described by a simple power law even with a curvature term. Instead the data can be described by a power law with exponential cutoff: $\\rm {{dN}\\over{dE}} \\propto \\rm E^{-2.14 \\pm 0.03_{stat}} \\times e^{-E/E_{0}} m^{-2} s^{-1} TeV^{-1}$ with $\\rm E_{0} = 4.3 \\pm 0.3_{stat} TeV$. Mrk 421 is the second $\\gamma$-ray blazar that unambiguously exhibits an absorption-like feature in its spectral energy distribution at 3-6 TeV suggesting that this may be a universal phenomenon, possibly due to the extragalactic infra-red background radiation.']",['2001-07-06'] +60,['eng'],"['De Jager, O C', 'Stecker, F W']",['Extragalactic Gamma-Ray Absorption and the Intrinsic Spectrum of Mkn 501 During the 1977 Flare'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'blazar', 'cosmic radiation, energy spectrum', 'cosmic radiation, absorption', 'cosmic radiation, diffusion', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107103'],"['Using the recent models of Malkan & Stecker (2001) for the infrared background radiation and extrapolating them into the optical and UV range using recent galaxy count data, we rederive the optical depth of the Universe to high energy gamma-rays as a function of energy and redshift for energies between 50 GeV and 100 TeV and redshifts between 0.03 and 0.3. We then use these results to derive the intrinsic gamma-ray spectrum of Mkn 501 during its 1997 high state. We find that the spectral energy distribution of Mkn 501 while flaring had a broad, flat peak in the 5-10 TeV range which corresponds to the broad, flat peak in the 50-100 keV range observed during the flare. The differential spectral index of our derived intrinsic gamma-ray spectrum at energies below about 2 TeV was found to be about 1.6 to 1.7. This corresponds to a time averaged index of 1.76 found in soft X-rays at energies below the X-ray synchrotron peak. These results appear to favor a synchrotron-self Compton origin for the TeV emission together with jet parameters which are consistent with time variability constraints and previous theoretical studies.']",['2001-07-06'] +61,['eng'],"['Amendola, L', 'Gordon, C', 'Wands, D', 'Sasaki, M']",['Correlated perturbations from inflation and the cosmic microwave background'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'perturbation, correlation', 'baryon, density', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107089'],"['We compare the latest cosmic microwave background data with theoretical predictions including correlated adiabatic and isocurvature perturbations with a simple power-law dependence. We find that there is a degeneracy between the amplitude of correlated isocurvature perturbations and the spectral tilt. A negative (red) tilt is found to be compatible with a larger isocurvature contribution. Estimates of the baryon and CDM density estimates are found to be almost independent of the isocurvature amplitude. The main result is that current microwave background data do not exclude a dominant contribution from CDM isocurvature fluctuations on large scales, and marginally favour a significant fraction.']",['2001-07-06'] +62,['eng'],"['Mendes, S O', 'Opher, R']",['Sub-mm gravity'],['Astrophysics and Astronomy'],"['gravitation, correction', 'gravitation, model', 'validity test', 'space-time, higher-dimensional', 'acceleration', 'proposed experiment', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107081'],"['We propose that future experiments aiming at the detection of deviations from the inverse square gravitational law on submillimetric scales can be used to test the modified Newtonian dynamics theory (MOND). Current experiments are able to test the gravitational field of masses of approximately 1g at distances around 200 micrometers, implying that they are probing accelerations well above the MOND limit (1.2 X 10^{-8} cms^{-2}). We show that MONDian effects begin to be important at the submillimetric level for masses below 1 mg. MOND makes predictions that are clearly distinguishable from those expected in a scenario with compact extra dimensions. This will enable direct confrontation between the two theories if future experiments can improve their mass scales to the milligram level.']",['2001-12-14'] +63,['eng'],"['Chernin, A D']",['Physical vacuum and cosmic coincidence problem'],['Astrophysics and Astronomy'],"['Friedman model', 'astrophysics, energy', 'vacuum state', 'astrophysics, missing-mass', 'electroweak interaction', 'astrophysics, acceleration']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107071'],"['A framework is suggested in which the energy integrals of the Friedmann cosmology are identified as genuine time-independent physical characteristics for both vacuum and non-vacuum forms of cosmic energy. The integrals are found to be numerically coincident within two orders of magnitude. It is assumed that this coincidence reveals a symmetry that relates vacuum to non-vacuum forms of cosmic energy at fundamental level. The symmetry shows the well-known cosmic coincidence problem and the naturalness problem as two inter-related aspects of a more general problem: Why are the energy integrals numerically coincident and equal to $ \\sim 10^{60} M_{Pl}^{-1}$? A simple kinetics model of cosmological freeze out is used to examine how -- at least, in principle -- the electroweak scale physics might explain the nature of the symmetry between vacuum and non-vacuum cosmic energies and determine the value of the energy integrals in terms of the fundamental energy scales.']",['2001-07-05'] +64,['eng'],"['Noh, H', 'Hwang, J']",['Inflationary spectra in generalized gravity'],['Astrophysics and Astronomy'],"['inflationary universe', 'gravitation', 'spectra', 'perturbation, scalar', 'perturbation, tensor']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107069'],"['The classical evolution and the quantum generation processes of the scalar- and tensor-type cosmological perturbations in the context of a broad class of generalized gravity theories are presented in unified forms. The exact forms of final spectra of the two types of structures generated during a generalized slow-roll inflation are derived. Results in generalized gravity are characterized by two additional parameters which are the coupling between gravity and field, and the nonminimal coupling in the kinetic part of the field. Our general results include widely studied gravity theories and inflation models as special cases, and show how the well known consistency relation and spectra in ordinary Einstein gravity inflation models are affected by the generalized nature of the gravity theories.']",['2001-07-05'] +65,['eng'],"['Aharonian, F A', 'Akhperjanian, A G', 'Barrio, J A']","[""A study of Tycho's SNR at TeV energies with the HEGRA CT-System""]",['Astrophysics and Astronomy'],"['supernova', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'photon, flux', 'time dependence', 'synchrotron radiation', 'cosmic radiation, acceleration', 'shock waves', 'pi0, radiative decay', 'model, fluid', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107044'],"[""Tycho's supernova remnant (SNR) was observed during 1997 and 1998 with the HEGRA Cherenkov Telescope System in a search for gamma-ray emission at energies above ~1 TeV. An analysis of these data, ~65 hours in total, resulted in no evidence for TeV gamma-ray emission. The 3sigma upper limit to the gamma-ray flux (>1 TeV) from Tycho is estimated at 5.78x10^{-13} photons cm^{-2} s^{-1}, or 33 milli-Crab. We interpret our upper limit within the framework of the following scenarios: (1) that the observed hard X-ray tail is due to synchrotron emission. A lower limit on the magnetic field within Tycho may be estimated B>=22 microG, assuming that the RXTE-detected X-rays were due to synchrotron emission. However, using results from a detailed model of the ASCA emission, a more conservative lower limit B>=6 microG is derived. (2) the hadronic model of Drury, Aharonian & Voelk, and (3) the more recent time-dependent kinetic theory of Berezhko & Voelk. Our upper limit lies within the range of predicted values of both hadronic models, according to uncertainties in physical parameters of Tycho, and shock acceleration details. In the latter case, the model was scaled to suit the parameters of Tycho and re-normalised to account for a simplification of the original model. We find that we cannot rule out Tycho as a potential contributor at an average level to the Galactic cosmic-ray flux.""]",['2001-07-04'] +66,['eng'],"['Papadopoulos, D B', 'Stergioulas, N', 'Vlahos, L', 'Kuijpers, J']",['Fast Magnetosonic Waves Driven by Gravitational Waves'],['Astrophysics and Astronomy'],"['gravitational radiation', 'plasma, magnetic', 'field equations, hydrodynamical', 'dispersion relations', 'space-time, background', 'space-time, perturbation', 'pulsar', 'gamma ray burst']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107043'],"['The propagation of a gravitational wave (GW) through a magnetized plasma is considered. In particular, we study the excitation of fast magnetosonic waves (MSW) by a gravitational wave, using the linearized general-relativistic hydromagnetic equations. We derive the dispersion relation for the plasma, treating the gravitational wave as a perturbation in a Minkowski background space-time. We show that the presence of gravitational waves will drive magnetosonic waves in the plasma and discuss the potential astrophysical implications.']",['2001-07-04'] +67,['eng'],"['Usov, V V']",['Response of bare strange stars to energy input onto their surfaces'],['Astrophysics and Astronomy'],"['matter, strangeness', 'energy, surface', 'electron, pair production', 'luminosity', 'quark, matter', 'superconducting', 'photon, cosmic radiation', 'energy, gap', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107020'],"['We study numerically the thermal emission of $e^+e^-$ pairs from a bare strange star heated by energy input onto its surface; heating starts at some moment, and is steady afterwards. The thermal luminosity in $e^+e^-$ pairs increases to some constant value. The rise time and the steady thermal luminosity are evaluated. Both normal and colour superconducting states of strange quark matter are considered. The results are used to test the magnetar model of soft gamma-ray repeaters where the bursting activity is explained by fast decay of superstrong magnetic fields and heating of the strange star surface. It is shown that the rise times observed in typical bursts may be explained in this model only if strange quark matter is a superconductor with an energy gap of more that 1 MeV.']",['2001-07-03'] +68,['eng'],"['Van Putten, M H P M']",['Gravitational radiation from a torus around a black hole'],['Astrophysics and Astronomy'],"['black hole, rotational', 'torus', 'gravitational radiation, emission', 'black hole, spin', 'black hole, energy', 'accretion', 'pulsar', 'gamma ray burst']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107007'],"['Long gamma-ray bursts (GRBs) from rapidly spinning black hole-torus systems may represent hypernovae or black hole-neutron star coalescence. We show that the torus may radiate gravitational radiation powered by the spin-energy of the black hole in the presence of non-axisymmetries. The coupling to the spin-energy of the black hole is due to equivalence in poloidal topology to pulsar magnetospheres. Results calculated in the suspended accretion state indicate that GRBs are potentially the most powerful LIGO/VIRGO burst-sources in the Universe, with an expected duration of 10-15s on a horizontal branch of 1-2kHz in the $\\dot{f}(f)-$diagram.']",['2001-07-03'] +69,['eng'],"['Di Stefano, R', 'Ford, L H', 'Yu, H', 'Fixsen, D J']",['Quantum Gravity and Astrophysics'],['Astrophysics and Astronomy'],"['quantum gravity, validity test', 'light cone, fluctuation', 'space-time, fluctuation', 'spectra, perturbation', 'cosmic radiation, background', 'time, correlation', 'photon, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107001'],"['The problem of formulating a fully consistent quantum gravity theory (QGT) has not yet been solved. Even before we are able to work out the details of a complete theory, however, we do know some important qualitative features to be expected in any quantum theory. Fluctuations of the metric, for example, are expected and are associated with fluctuations of the lightcone. Lightcone fluctuations affect the arrival time of signals from distant sources in potentially measurable ways, broadening the spectra. In this paper, we start with a thermal spectrum and derive the form of spectral changes expected in a wide class of QGTs. We apply these results, valid for any thermal spectrum, to the cosmic microwave background (CMB). The CMB offers two advantages: (1) deviations from a thermal spectrum are well constrained, and (2) the radiation emanates from the most distant source of light, the surface of last scattering. We use existing CMB data to derive an upper bound on the value of $\\Delta t,$ the mean spread in arrival times due to metric fluctuations: ${\\Delta t} < 2.1 \\times 10^{-14}$ s at the 95% confidence limit. This limit applies to a wide range of QGTs, and falsifies those predicting a larger spread in arrival times. We find this limit rules out at least one QGT, the 5-dimensional theory in which the ""extra"" dimension is flat. Tests of other models may also be possible, depending on the results of calculations to predict values of \\Delta t,$ and also a second time scale, $\\tau_c,$ the correlation time, which is the characteristic time scale of the metric fluctuations. We show that stronger limits on the value of $\\Delta t,$ hence on lightcone fluctuations, can likely be derived through observations of of higher-T sources, e.g., in the X-ray and gamma-ray regimes.']",['2001-07-03'] +70,['eng'],"['Ignatiev, V B', 'Kuranov, A G', 'Postnov, K A', 'Prokhorov, M E']",['Orbital Eccentricity Effects on the Stochastic Gravitational Wave Background from Coalescing Binary Neutron Stars'],['Astrophysics and Astronomy'],"['talk, Karbardino-Balkaria 2001/04/18', 'n, matter', 'binary, orbit', 'gravitational radiation, emission', 'background, stochastic', 'counters and detectors, satellite', 'galaxy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106569'],"['Unresolved coalescing binary neutron stars in the Galaxy and beyond produce a stochastic gravitational wave background within the LISA frequency band, which can be potentially dangerous for possible detection of fundamentally more interesting relic cosmological backgrounds. Here we address the question what effects the unavoidable eccentricity of orbits of these systems should have on the properties of this backgrounds. In particularly, we examine starting from which frequency one-year observations with LISA can be secure from contamination by the noise produced by galactic binary neutron stars in eccentric orbits. We come to the conclusion that harmonics from such binaries do not contribute significantly above $\\sim 10^{-3}$ Hz.']",['2001-07-02'] +71,['eng'],"['Chiba, T']",['Extended Quintessence and its Late-time Domination'],['Astrophysics and Astronomy'],"['quintessence', 'dark energy', 'energy, density']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106550'],['Various astronomical observations point towards the evidence for dark energy. One of the most mysterious problem is the coincidence problem: why dark energy becomes dominant only recently. We present a scenario based on extended quintessence models to explain the late-time domination of dark energy without severe fine-tuning of initial conditions and model parameters.'],['2001-07-02'] +72,['eng'],"['Strong, A W', 'Moskalenko, I V']",['A 3D time-dependent model for Galactic cosmic rays and gamma rays'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'time dependence', 'galaxy', 'dimension, 3', 'electron, spectra', 'cosmic radiation, fluctuation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106505'],"['In studies of cosmic-ray (CR) propagation and diffuse continuum gamma-ray emission from the Galaxy it has usually been assumed that the source function can be taken as smooth and time-independent. However, especially for electrons at high energies where energy losses are rapid, the effect of the stochastic nature of the sources becomes apparent and indeed has been invoked to explain the GeV excess in the diffuse emission observed by EGRET. In order to address this problem in detail a model with explicit time-dependence and a stochastic SNR population has been developed, which follows the propagation in three dimensions. The results indicate that although the inhomogeneities are large they are insufficient to easily explain the GeV excess. However the fluctuations should show up in the gamma-ray distribution at high energies and this should be observable with GLAST. Estimates of the TeV continuum emission from the plane are consistent with the Whipple upper limit.']",['2001-06-28'] +73,['eng'],"['González-Diáz, P F']",['Classical and quantum quintessence cosmology'],['Astrophysics and Astronomy'],"['quintessence', 'quantum cosmology', 'dimension, 5', 'dimension, 4', 'membrane model', 'instanton', 'space-time, anti-de Sitter', 'constraint', 'wormhole']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106421'],"['This paper implements the idea of considering the instantonic creation of brane worlds whose five-dimensional bulk contains a negative cosmological constant and a scalar quintessence field with time-dependent equation of state, restricting to the case that the quintessence field couples minimally to Hilbert-Einstein gravity. We construct an Euclidean formalism, both for the four- and five-dimensional cases, singling out a Hamiltonian constraint that depends on the parameter defining the quintessence state equation. Specializing at several particular values of that parameter, we obtain solutions to the constraint equation and analyse them both classically and quantum mechanically. It is found that these solutions can represent either asymptotically anti-de Sitter wormholes or pure anti-de Sitter spaces whose quantum states are obtained by means of the Wheeler de Witt equation. Starting with the different five-dimensional solutions, an instantonic procedure is applied to describe the creation of geometrically equivalent inflating de Sitter branes whose quantum states are also evaluated in some cases. We thus consider the quantum state of the universe to be contributed by all the instantonic paths that correspond to these particular brane worlds.']",['2001-12-14'] +74,['eng'],"['Bento, M C', 'Bertolami, O', 'Santos, N C']",['A Two-Field Quintessence Model'],['Astrophysics and Astronomy'],"['quintessence', 'field theory, scalar', 'energy, density', 'asymptotic behavior', 'astrophysics, expansion', 'expansion, acceleration', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106405'],"['We study the dynamics of a quintessence model based on two interacting scalar fields. The model can account for the (recent) accelerated expansion of the Universe suggested by astronomical observations. Acceleration can be permanent or temporary and, for both scenarios, it is possible to obtain suitable values for the cosmological parameters while satisfying the nucleosynthesis constraint on the quintessence energy density. We argue that the model dynamics can be made consistent with a stable zero-energy relaxing supersymmetric vacuum.']",['2001-12-14'] +75,['eng'],"['Yahiro, M', 'Mathews, G J', 'Ichiki, K', 'Kajino, T', 'Orito, M']",['Constraints on Cosmic Quintessence'],['Astrophysics and Astronomy'],"['quintessence', 'energy, density', 'effective potential', 'cosmic radiation, background', 'supergravity, correction', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106349'],"['Recently, attempts have been made to understand the apparent near coincidence of the present vacuum energy and matter energy in terms of a dynamical attractor-like solution for the evolution of a ""quintessence"" scalar field. In these models the field couples with the dominant constituent and only acts like a cosmological constant after the onset of the matter dominated epoch. A generic feature of such solutions, however, is the possibility of significant energy density in the scalar field during the radiation dominated epoch. As such, these models can affect, and therefore be constrained by, primordial nucleosynthesis and the epoch of photon decoupling. Here we analyze one popular form for the quintessence field (with and without a supergravity correction) and quantify constraints on the allowed initial conditions and parameters for the effective potential.']",['2001-06-21'] +76,['eng'],"['Mori, M', 'Asahara, A', 'Bicknell, G V', 'Clay, R W', 'Edwards, P G', 'Enomoto, R', 'Gunji, S', 'Hara, S', 'Hara, T', 'Hayashi, S', 'Itoh, C', 'Kabuki, S', 'Kajino, F', 'Katagiri, H', 'Kawachi, A', 'Kifune, T', 'Kubo, H', 'Kushida, J', 'Maeda, S', 'Maeshiro, A', 'Matsubara, Y', 'Mizumoto, Y', 'Muraishi, H', 'Muraki, Y', 'Naito}, T', 'Nakase, T', 'Nishijima, K', 'Ohishi, M', 'Okumura, K', 'Patterson, J R', 'Protheroe, R J', 'Sakurazawa, K', 'Suzuki, R', 'Swaby, D L', 'Tanimori, T', 'Tokanai, F', 'Tsuchiya, K', 'Tsunoo, H', 'Uruma, K', 'Watanabe, A', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['The CANGAROO-III Project'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'photon, cosmic radiation', 'Cherenkov counter, performance', 'optics, reflection', 'imaging', 'electronics']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106346'],"['We report on the status of the construction of an array of four 10 m atmospheric Cherenkov telescopes for gamma-ray astronomy, near Woomera, in South Australia -- the CANGAROO-III project. The first telescope of this array is the upgraded version of the CANGAROO-II 7 m telescope and has been in operation since March 2000. The second telescope, an improved version of the first, is being constructed for installation in late 2001. Stereoscopic observation of sub TeV gamma-rays with the two 10 m telescopes will begin in 2002 and the full array will be operational in 2004.']",['2001-06-21'] +77,['eng'],"['Chatterjee, L', 'Strayer, M R', 'Wu, J S']",['Bremsstrahlung of Flavor-Degenerate Pairs by Neutrinos in the Nuclear Field'],['Astrophysics and Astronomy'],"['talk, Washington 2001/04/28', 'neutrino nucleus, nuclear reaction', 'electron, pair production', 'electron, bremsstrahlung', 'neutrino/e', 'neutrino/mu', 'lead', 'iron', 'effective Lagrangian', 'cross section, energy dependence', 'lepton, angular distribution', 'lepton, energy spectrum', 'neutrino electron, elastic scattering', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106317'],['Neutrino Bremsstrahlung of flavor-degenerate pairs in the field of a nucleus is of potential importance for neutrino astrophysics and is representative of a class of processes connecting leptonic electroweak sectors to real or virtual photons. We focus on first generation flavor production by both electron and muon neutrinos and present Standard Model cross sections and distributions for lead and iron nuclei. The results (of order 10-41 cm2 for electron neutrino - lead collisions at 100 MeV) have been fitted to empirical formulae that can be used to estimate backgrounds to neutrino detection experiments and flux normalizations. A compact form of the matrix element obtained by analytic reduction is used to explain the distributions. The V-A limits of the cross sections are shown to agree with published work from the pre-neutral current era. Event signatures and the possible roles of these processes in stellar and laboratory neutrino physics are discussed. Cross sections are compared with those for neutrino-electron scattering for neutrino spectra corresponding to typical supernovae temperatures.'],['2001-06-20'] +78,['eng'],"['De la Macorra, A', 'Stephan-Otto, C']",['Natural Quintessence with Gauge Coupling Unification'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'gauge field theory, SU(N)', 'coupling constant, gauge', 'quintessence', 'condensation, chiral', 'astrophysics, fundamental constant', 'field theory, scalar', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106316'],"['We show that a positive accelerating universe can be obtained simply by the dynamics of a non-abelian gauge group. It is the condensates of the chiral fields that obtain a negative power potential, below the condensation scale, and allow for a quintessence interpretation of these fields. The only free parameters in this model are $N_c$ and $N_f$ and the number of dynamically gauge singlet bilinear fields $\\phi$ generated below the condensation scale. We show that it is possible to have unification of all coupling constants, including the standard and non standard model couplings, while having an acceptable phenomenology of $\\phi$ as the cosmological constant. This is done without any fine tuning of the initial conditions. The problem of coincidence (why the universe has only recently started an accelerating period) is not solved but it is put at the same level as what the particle content of the standard model is.']",['2001-06-20'] +79,['eng'],"['Altmann, M', 'Angloher, G', 'Bruckmayer, M', 'Bucci, C', 'Cooper, S', 'Cozzini, C', 'Di Stefano, P', 'Von Feilitzsch, F', 'Frank, T', 'Hauff, D', 'Jagemann, T', 'Jochum, J', 'Keeling, R', 'Kraus, H', 'MacAllister, J', 'Pröbst, F', 'Ramachers, Y', 'Schnagl, J', 'Seidel, W', 'Sergeyev, I', 'Stark, M', 'Stodolsky, L', 'Wulandari, H']",['Results and plans of the CRESST dark matter search'],['Astrophysics and Astronomy'],"['talk, Rome 2001/07/23', 'astrophysics, missing-mass', 'WIMP, search for', 'calorimeter, cryogenics', 'crystal', 'scattering, WIMP nucleon', 'total cross section, mass', 'spin, dependence', 'deep underground detector, Gran Sasso', 'scintillation counter, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106314'],"['Data taken by CRESST in 2000 with a cryogenic detector system based on 262 g sapphire crystals is used to place limits on WIMP dark matter in the Galactic Halo. The detector is especially sensitive for low-mass WIMPS with spin-dependent cross sections and improves on existing limits in this region. CRESST is now preparing for a second phase, which will use a 10 kg detector consisting of 300 g CaWO4 crystals with simultaneous detection of phonons and scintillation light to reduce background.']",['2001-12-14'] +80,['eng'],"['Prokopec, Tomislav']",['Cosmological magnetic fields from photon coupling to fermions and bosons in inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'coupling, (fermion photon)', 'coupling, (boson photon)', 'gravitation', 'gauge field theory', 'field theory, scalar', 'field theory, pseudoscalar', 'operator, higher-dimensional', 'invariance, gauge', 'symmetry breaking, conformal', 'magnetic field, production', 'space-time, perturbation', 'birefringence', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106247'],"['We consider several gauge invariant higher dimensional operators that couple gravity, gauge fields and scalar or fermionic fields and thus break conformal invariance. In particular, we consider terms that break conformal invariance by the photon coupling to heavy and light fermions. While the coupling to heavy fermions typically do not induce significant magnetic fields, the coupling to light fermions may produce observable magnetic fields when there are a few hundred light fermions. Next we consider Planck scale modifications of the kinetic gauge terms of the form f(phi) F_{mu nu} F^{mu nu} and h(psi) F_{mu nu} \\~F^{mu nu}, where f and h are functions of scalar and pseudoscalar fields phi, psi, and F_{mu nu}, ~F^{mu nu} are the gauge field strength and its dual, respectively. For a suitable choice of f sufficiently strong magnetic fields may be produced in inflation to be potentially observable today. The pseudoscalar coupling may lead to birefringence in inflation, but no observable magnetic field amplification. Finally, we show that the photon coupling to metric perturbations produces by far too weak fields to be of cosmological interest.']",['2001-12-14'] +81,['eng'],"['Caprini, C', 'Durrer, R']",['Gravitational wave production'],['Astrophysics and Astronomy'],"['gravitational radiation, production', 'magnetic field, stochastic', 'light nucleus, production', 'magnetic field, energy', 'tensor, energy-momentum', 'back reaction', 'coherence, length', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106244'],"['We compute the gravity waves induced by anisotropic stresses of stochastic primordial magnetic fields. The nucleosynthesis bound on gravity waves is then used to derive a limit on the magnetic field amplitude as function of the spectral index. The obtained limits are extraordinarily strong: If the primordial magnetic field is produced by a causal process, leading to a spectral index $n\\ge 2$ on super horizon scales, galactic magnetic fields produced at the electroweak phase transition or earlier have to be weaker than $B_\\la \\le 10^{-27}$Gauss! If they are induced during an inflationary phase (reheating temperature $T\\sim 10^{15}$GeV) with a spectral index $n\\sim 0$, the magnetic field has to be weaker than $B_\\la \\le 10^{-39}$Gauss! Only very red magnetic field spectra, $n\\sim -3$ are not strongly constrained. We also find that a considerable amount of the magnetic field energy is converted into gravity waves. The gravity wave limit derived in this work rules out most of the proposed processes for primordial seeds for the large scale coherent magnetic fields observed in galaxies and clusters.']",['2001-06-14'] +82,['eng'],"['Fiandrini, E', 'Esposito, G', 'Bertucci, B', 'Alpat, B', 'Battiston, R', 'Burger, W J', 'Lamanna, G', 'Zuccon, P']","[""Leptons with E>200 MeV trapped in the Earth's radiation belts""]",['Astrophysics and Astronomy'],"['electron, cosmic radiation', 'positron, cosmic radiation', 'cosmic radiation, flux', 'geophysics, magnetic field', 'time, spectra', 'cosmic radiation, energy spectrum', 'magnetic spectrometer, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106241'],"['For the first time accurate measurements of electron and positron fluxes in the energy range 0.2$\\div$10 GeV have been performed with the Alpha Magnetic Spectometer (AMS) instrument at altitudes of 370-390 Km in the geographic latitude interval +/- 51.7 deg. We present an original analysis of the AMS data, focused on the study of the under-cutoff component of these fluxes, outside the region of the South Atlantic Anomaly (SAA). A separation in quasi-trapped, long lifetime (O(10 s)), and albedo, short life time (O(100 ms)), components is found. The flux maps as a function of the canonical adiabatic variables L, alpha0 are determined in the interval (L,alpha0)=(0.95-3,0-90) for electrons with E less than 10 GeV, and positrons with E less than 3 GeV. The results are compared with existing data at lower energies and in similar L, alpha0 range. The properties of the observed under-cutoff particles are also investigated in terms of their residence times and geographical origin. The resulting distributions are discussed and related to the characteristics of the drift shells observed by AMS.']",['2001-06-14'] +83,['eng'],"['Fargion, D']",['Horizontal and Upward Tau Airshowers in Valleys from Mountains and Space'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'neutrino, cosmic radiation', 'antineutrino, cosmic radiation', 'showers, air', 'tau, decay modes', 'tau, lifetime', 'neutrino/tau', 'antineutrino/e', 'neutrino nucleon, interaction', 'antineutrino electron, interaction', 'interaction, length', 'cosmic radiation, energy spectrum', 'neutrino, oscillation', 'numerical calculations', 'neutrino/tau nucleus --> tau anything', 'antineutrino/e electron --> tau antineutrino/tau']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106239'],"['Upward and horizontal tau Air-showers emerging from the Earth crust or mountain chains are the most powerful signals of Ultra High Energy UHE neutrinos nu_{tau}, bar\\nu_{tau} and bar{nu}_e at PeVs and higher energy. The multiplicity in tau Air-showers secondary particles, N_{opt}=10^{12}(E_{tau}/PeV), N_{gamma}= 10^8*E_{tau}/PeV, N_{e^- e^+}= 2*10^7 E_{tau}/PeV, N_{mu}= 3 *10^5 (E_{tau}/PeV)^{0.85} make easy their discover. UHE nu_tau,bar\\nu_tau, following Super Kamiokande evidence of neutrino flavor mixing, nu_mu<--->nu_tau, should be as abundant as nu_mu, bar\\nu_mu. Also anti-neutrino electrons, bar\\nu_e, near the Glashow W resonance energy peak, E_{bar\\nu_e} = M^2_W / 2m_e = 6.3*10^{15} eV may generate tau Air-showers. Upward UHE nu_tau- N interaction on Earth crust at horizontal edge and from below, their consequent upward UHE tau air-showers beaming toward high mountains, air-planes, ballons and satellites should flash gamma, mu, X and Cherenkov lights toward detectors. Such upward tau air-shower may already hit nearby satellite GRO gamma detectors flashing them by short, hard, diluted gamma-burst at the edge of BATSE threshold. The tau air-shower may test the UHE neutrino interactions leading to additional fine-tuned test of New TeV Physics both in Mountain Valleys and in Upward showers.']",['2001-06-14'] +84,['eng'],"['Usov, V V']",['Strange Star Heating Events as a Model for Giant Flares of Soft Gamma-ray Repeaters'],['Astrophysics and Astronomy'],"['matter, strangeness', 'matter, accretion', 'quark, surface', 'gamma ray burst', 'luminosity, time dependence', 'energy', 'temperature', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106226'],"['Two giant flares were observed on 5 March 1979 and 27 August 1998 from the soft gamma-ray repeaters SGR 0526-66 and SGR 1900+14, respectively. The striking similarity between these remarkable bursts strongly implies a common nature. We show that the light curves of the giant bursts may be easily explained in the model where the burst radiation is produced by the bare quark surface of a strange star heated, for example, by impact of a massive comet-like object.']",['2001-06-14'] +85,['eng'],"['Bazhutov, Y N', 'Baranov, D S']","['Observation of Excess Flux for Negative Cosmic Ray Penetrating Particles in Bubble Chamber ""SKAT"" for Momentum Range (30GeV/c5) orders of magnitude spread in the possible interaction rates for models consistent with existing Cosmology and Accelerator bounds. Some theorists, but certainly not all, are able to generate models, that lead to interaction rates at the few /kg/day that would be implied by the current DAMA annual modulation signal. All theorists demonstrate models that generate much lower interaction rates. This paper takes an unashamed experimentalist`s view of the issues that arise when looking forward to constructing 1 tonne WIMP detectors.']",['2001-06-13'] +89,['eng'],"['Cartier, C', 'Hwang, J', 'Copeland, E J']",['Evolution of cosmological perturbations in non-singular string cosmologies'],['Astrophysics and Astronomy'],"['astrophysics', 'boson, string model', 'correction, higher-order', 'perturbation, scalar', 'perturbation, vector', 'perturbation, tensor', 'field equations, solution', 'space-time, perturbation', 'fluid, angular momentum', 'inflationary universe', 'dilaton', 'vacuum state, fluctuation', 'spectra, perturbation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106197'],"['In a class of non-singular cosmologies derived from higher-order corrections to the low-energy bosonic string action, we derive evolution equations for the most general cosmological scalar, vector and tensor perturbations. In the large scale limit, the evolutions of both scalar and tensor perturbations are characterised by conserved quantities, the usual curvature perturbation in the uniform-field gauge and the tensor-type perturbed metric. The vector perturbation is not affected, being described by the conservation of the angular momentum of the fluid component in the absence of any additional dissipative process. For the scalar- and tensor-type perturbations, we show how, given a background evolution during kinetic driven inflation of the dilaton field, we can obtain the final power spectra generated from the vacuum quantum fluctuations of the metric and the dilaton field during the inflation.']",['2001-06-13'] +90,['eng'],"['Piron, F', 'Djannati-Atai, A', 'Punch, M', 'Tavernet, J P', 'Barrau, A', 'Bazer-Bachi, R', 'Chounet, L M', 'Debiais, G', 'Degrange, B', 'Dezalay, J P', 'Espigat, P', 'Fabre, B', 'Fleury, P', 'Fontaine, G', 'Goret, P', 'Gouiffes, C', 'Khelifi, B', 'Malet, I', 'Masterson, C', 'Mohanty, G', 'Nuss, E', 'Renault, C', 'Rivoal, M', 'Rob, L', 'Vorobiov, S']",['Temporal and spectral gamma-ray properties of Mkn421 above 250 GeV from CAT observations between 1996 and 2000'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'blazar', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation', 'Cherenkov counter, imaging', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106196'],"['The gamma-ray emission above 250 GeV from the BL Lac object Markarian 421 was observed by the CAT Cherenkov imaging telescope between December, 1996, and June, 2000. In 1998, the source produced a series of small flares, making it the second extragalactic source detected by CAT. The time-averaged differential spectrum has been measured from 0.3 to 5 TeV, which is well fitted with a power law with an index of -2.88+-0.12(stat)+-0.06(syst). In 2000, the source showed an unprecedented activity, with variability time-scales as short as one hour, as for instance observed during the night between 4 and 5 February. The 2000 time-averaged spectrum measured is compatible with that of 1998, but some indication of a spectral curvature is found between 0.3 and 5 TeV. The possibility of TeV spectral hardening during flares is also discussed, and the results are compared to those obtained on the other TeV BL Lac, Markarian 501.']",['2001-06-13'] +91,['eng'],"['Ma, F']",['Possible Signatures of Quark-Hadron Phase Transitions inside Neutron Stars'],['Astrophysics and Astronomy'],"['talk, Lake Louise 2000/02/20', 'n, matter', 'critical phenomena', 'transition, quark hadron', 'pulsar, spin', 'gamma ray burst', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106169'],"['The spin-down power of an isolated neutron star can drive its central density increase and overall structural changes, and trigger a quark-hadron phase transition. A series of observational signatures may be seen as a result of the phase transition, including pulsar spin-down and glitch behaviors, Soft Gamma Repeaters or Gamma-Ray Bursts.']",['2001-06-12'] +92,['eng'],"['Dolgov, A D', 'Grasso, D']",['Generation of Cosmic Magnetic Fields and Gravitational Waves at Neutrino Decoupling'],['Astrophysics and Astronomy'],"['astrophysics, model', 'plasma', 'lepton number', 'turbulence, production', 'magnetic field, production', 'gravitational radiation, background', 'lepton, asymmetry', 'neutrino, oscillation', 'neutrino, sterile', 'baryon, production', 'neutrino, decoupling', 'velocity, fluid', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106154'],['We show that an inhomogeneous cosmological lepton number may have produced turbulence in the primordial plasma when neutrinos entered (almost) free-streaming regime. This effect may be responsible for the origin of cosmic magnetic fields and give rise to a detectable background of gravitational waves. An existence of inhomogeneous lepton asymmetry could be naturally generated by active-sterile neutrino oscillations or by some versions of Affleck and Dine baryogenesis scenario.'],['2001-06-11'] +93,['eng'],"['Chernin, A D', 'Santiago, D I', 'Silbergleit, A S']",['Interplay Between Gravity and Quintessence'],['Astrophysics and Astronomy'],"['relativity theory, general', 'gravitation, antigravitation', 'quintessence', 'field theory, space-time', 'Einstein equation, solution']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106144'],"[""A set of new exact analytical General Relativity (GR) solutions with time-dependent and spatially inhomogeneous quintessence demonstrate 1) a static non-empty space-time with a horizon-type singular surface; 2) time-dependent spatially homogeneous `spheres' which are completely different in geometry from the Friedmann isotropic models; 3) infinitely strong anti-gravity at a `true' singularity where the density is infinitely large. It is also found that 4) the GR solutions allow for an extreme `density-free' form of energy that can generate regular space-time geometries.""]",['2001-06-11'] +94,['eng'],"['Ter-Antonian, S V']",['Anisotropy analysis of EAS data in the knee region'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, anisotropy', 'showers, air', 'showers, spatial distribution', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106124'],['Based on MAKET-ANI EAS data the distributions of equatorial coordinates of EAS core directions are obtained in the knee region. Anisotropy of primary cosmic rays is displayed only by declination equatorial coordinates (20+/-3 degrees) at primary energies more than 5-10 PeV. The fraction of anisotropic component turns out ~10% in the knee region.'],['2001-06-08'] +95,['eng'],"['Wickramasinghe, T', 'Benacquista, M J']",['Detection of Gravitational Waves from Gravitationally Lensed Systems'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'gravitational radiation, counters and detectors', 'counters and detectors, satellite', 'optics, interference', 'gravitation, lens', 'quasar', 'black hole']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106087'],"['It is accepted that quasars are powered by supermassive black holes (SMBH) with masses in the range 10^6 - 10^9 solar masses in their cores. Occasionally, compact stars can plunge into SMBH. In addition, there may be a number of such compact objects circling the central SMBH in any given quasar. Both of these processes are known to emit gravitational waves. LISA has the right sensitivity to detect these waves. We show that gravitational lenses amplify the amplitudes of these gravitational waves just as they amplify the observed light of quasars. Given the geometry of the lensing configuration, this amplification can be as large as a factor of 2 to 10, allowing the waves to be above the detection threshold of LISA. We also show that waves from lensed quasars arrive with time delays which are much larger than the coherence time of the gravitational waves, making interference effects negligible. Thus, a simple geometrical optics application leads to the lensing theory of gravitational waves. In this context, we analyze and show in this preliminary analysis that there is an enhancement of the amplitudes of gravitational radiation coming from observed lensed quasars.']",['2001-12-14'] +96,['eng'],"['Hill, G C']",['Bayesian event reconstruction and background rejection in neutrino detectors'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'neutrino, cosmic radiation', 'deep underground detector, AMANDA', 'statistical analysis', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106081'],"['Several large volume, high energy neutrino detectors are in operation or in the design stage. Upward going signal neutrino events must be separated from large backgrounds of downgoing cosmic ray induced atmospheric muons. To this end, a Bayesian extension of the traditional maximum likelihood reconstruction method will be described. Further, it will be shown how signals can be separated from backgrounds through integration of Bayesian posterior probability densities.']",['2001-06-06'] +97,['eng'],"['Ruffini, R J']","['Analogies, new paradigms and observational data as growing factors of Relativistic Astrophysics']",['Astrophysics and Astronomy'],"['astrophysics, relativistic', 'cosmic radiation, trajectory', 'relativity theory, general', 'pulsar', 'energy, rotational', 'thermodynamics', 'galaxy', 'black hole, charge', 'gamma ray burst, angular distribution', 'vacuum polarization', 'plasma, fluid', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106075'],['Patterns in the scientific developments of Relativistic Astrophysics are analyzed with special attention to the physics and astrophysics of Black Holes and Gamma Ray Bursts.'],['2001-06-06'] +98,['eng'],"['Pavlov, M', 'Rubano, C', 'Sazhin, M V', 'Scudellaro, P']",['Analysis of two quintessence models with SN Ia data'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'quintessence', 'supernova', 'matter, density', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106068'],"['The supernovae Ia data are used to analyze two general exact solutions for quintessence models. The best fit values for $\\Omega_{m0}$ are smaller than in the $\\Lambda $-term model, but still acceptable. With present-day data, it is not possible to discriminate among the various situations.']",['2001-06-06'] +99,['eng'],"['Hill, G C']",['Amanda results'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2001/03/17', 'neutrino, cosmic radiation', 'neutrino, flux', 'cosmic radiation, particle source', 'cosmic radiation, angular distribution', 'gamma ray burst', 'new particle, search for', 'astrophysics, missing-mass', 'WIMP, annihilation', 'magnetic monopole', 'deep underground detector, AMANDA', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106064'],"['The AMANDA (Antarctic Muon And Neutrino Detector Array) detector, located at the South Pole station, Antarctica, was recently expanded with the addition of six new strings, completing the phase referred to as AMANDA-II. This detector has been calibrated and in operation since January 2000. The first data analyses are currently underway. In this report we present an update on the results from the AMANDA-B10 detector, which operated during the austral winter 1997.']",['2001-06-06'] +100,['eng'],"['Glendenning, N K', 'Weber, F']",['Signal of Quark Deconfinement in Millisecond Pulsars and Reconfinement in Accreting X-ray Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'quark, confinement', 'critical phenomena', 'pulsar, spin', 'quark, matter', 'mass, accretion', 'binary', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106054'],"['Theoretically, the phase transition between the confined and deconfined phases of quarks can have a remarkable effect on the spin properties of millisecond pulsars and on the spin distribution of the population of x-ray neutron stars in low-mass binaries. In the latter class of stars, the effect has already been observed---a strong clustering in the population in a narrow band of spins. The observed clustering cannot presently be uniquely assigned to the phase transition as cause. However, there is another possible signal---not so far observed---in millisecond pulsars that we also discuss. It would have the same origin, and its discovery would tend to confirm the interpretation in terms of a phase transition in the stellar core and that the high density phase exists in the higer mass canonical neutron stars.']",['2001-06-05'] +101,['eng'],"[""O'Connor-Drury, L"", 'Ellison, D C', 'Aharonian, F A', 'Berezhko, E G', 'Bykov, A', 'Decourchelle, A', 'Diehl, R', 'Meynet, G', 'Parizot, E', 'Raymond, J', 'Reynolds, S', 'Spangler, S']",['Tests of Galactic Cosmic Ray Source Models'],['Astrophysics and Astronomy'],"['galaxy', 'cosmic radiation, particle source', 'particle source, model', 'validity test', 'cosmic radiation, acceleration', 'cosmic radiation, energy', 'supernova', 'shock waves', 'bubble', 'interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106046'],['This report discusses the possibilities for observational tests of current models and ideas regarding the origin of the Galactic Cosmic Rays using facilities which are already available.'],['2001-06-05'] +102,['eng'],"['Sciutto, S J']",['The AIRES system for air shower simulations. An update'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'showers, air', 'energy spectrum', 'transverse momentum, spectra', 'cosmic radiation, flux', 'programming, Monte Carlo', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106044'],"['A report on the characteristics of ultra-high energy air showers simulated with the current version of the AIRES program is presented. The AIRES system includes a fast simulating program, originally designed on the basis of the well-known MOCCA program, and progressively improved and tested. The AIRES algorithms are briefly described and some results coming from the simulations are analyzed.']",['2001-06-05'] +103,['eng'],"['Aharonian, F A']",['Proton synchrotron radiation of large-scale jets in active galactic nuclei'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'p, acceleration', 'synchrotron radiation', 'photon, cosmic radiation', 'cosmic radiation, jet', 'AGN', 'photon p, interaction', 'electron, photoproduction', 'electron, cosmic radiation', 'cosmic radiation, secondary radiation', 'cosmic radiation, energy spectrum', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106037'],"['I propose a new mechanism for explanation of nonthernal X-ray emission of large-scale AGN jets. Namely, I assume that this radiation has synchrotron origin emitted by extremely high energy protons, and discuss implications of this model for several prominent hot spots and knots resolved by Chandra in Pictor A, 3C 120, PKS 0637-752, 3C 273.']",['2001-06-05'] +104,['eng'],"['Plaga, R']",['A possible Universal Origin of Hadronic Cosmic Rays from Ultrarelativistic Ejecta of Bipolar Supernovae'],['Astrophysics and Astronomy'],"['hadron, cosmic radiation', 'cosmic radiation, particle source', 'gamma ray burst', 'baryon, plasma', 'plasma, ejection', 'supernova', 'cosmic radiation, acceleration', 'shock waves', 'cosmic radiation, spectra', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106033'],"[""Based on the ``cannonball model'' for gamma-ray bursts of Dar and De Rujula (astro-ph/0012227) it is proposed that masses of baryonic plasma (``cannonballs''), ejected in bipolar supernova explosions in our Galaxy are the sources of hadronic Galactic cosmic rays (CRs) at all energies. The propagation of the cannonballs in the Galactic disk and halo is studied. Two mechanisms for the acceleration of the observed CRs are proposed. The first is based on ultrarelativistic shocks in the interstellar medium and could accelerate the bulk of CRs up to the ``knee'' energy of 4 x 10^{15} eV. The second operates with second-order Fermi acceleration within the cannonball. If the total initial energy of the ejected plasmoids in a SN explosion is 10^{53} ergs or higher this second mechanism may explain the CR spectrum above the knee up to the highest observed energies.It is shown that with plausible assumptions about CR propagation in the Galactic confinement volume many phenomenological properties of CRs can be understood to first order.""]",['2001-06-05'] +105,['eng'],"['Fryer, C L', 'Holz, D E', 'Hughes, S A']",['Gravitational Wave Emission From Core-Collapse of Massive Stars'],['Astrophysics and Astronomy'],"['star, massive', 'gravitational radiation, emission', 'moment, multipole', 'black hole', 'supernova', 'white dwarf', 'n, matter', 'matter, accretion', 'matter, production', 'matter, angular momentum', 'counters and detectors', 'laser, interference', 'energy, rotational', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106113'],"['We derive estimates for the characteristics of gravitational radiation from stellar collapse, using recent models of the core-collapse of Chandrasekhar mass white dwarfs (accretion induced collapse), core-collapse supernovae and collapsars, and the collapse of very massive stars (~> 300 Msun). We study gravitational-wave emission mechanisms using several estimation techniques, including two-dimensional numerical computation of quadrupole wave emission, estimates of bar-mode strength, estimates of r-mode emission, and estimates of waves from black hole ringing. We also review the rate at which the relevant collapses are believed to occur, which has a major impact on their relevance as astrophysical sources. Although the latest supernova progenitor simulations produce cores rotating much slower than those used in the past, we find that bar-mode and r-mode instabilities from core-collapse supernovae remain among the leading candidate sources for LIGO-II. Accretion induced collapse (AIC) of a white dwarf could produce gravitational-wave signals similar to those from core-collapse. In the models that we examine, such collapses are not unstable to bar modes (though we note that models recently examined by Liu and Lindblom, which have slightly more angular momentum, are certainly unstable to bar formation), but the collapsed remnant is a potentially interesting source of r-mode radiation. Because AIC events are probably 1,000 times less common than core-collapse supernovae, the typical AIC event will be much further away, and thus produce much weaker waves. In the most optimistic circumstances, we find it may be possible to detect gravitational waves from the collapse of 300 Msun Population III stars.']",['2001-06-07'] +106,['eng'],"['Hansen, S H', 'Lesgourgues, Julien', 'Pastor, S', 'Silk, J']",['Closing the Window on Warm Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutrino, sterile', 'neutrino, mass', 'neutrino, momentum spectrum', 'coherence, violation', 'neutrino, decoupling']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106108'],['Sterile neutrinos may be one of the best Warm Dark Matter candidates we have today. Both lower and upper bounds on the mass of the sterile neutrino come from astronomical observations. We show that the proper inclusion of the neutrino momentum distribution and the solution of the kinetic equations with the correct coherence breaking terms lead to the near exclusion of the sterile neutrino as a dark matter candidate.'],['2001-06-07'] +107,['eng'],"['Benoit, A', 'Bergé, L', 'Broniatowski, A', 'Chambon, B', 'Chapellier, M', 'Chardin, G', 'Charvin, P', 'De Jésus, M', 'Stefano, P D', 'Drain, D', 'Dumoulin, L', 'Gascon, J', 'Gerbier, G', 'Goldbach, C', 'Goyot, M', 'Gros, M H', 'Hadjout, J P', 'Juillard, A', 'de Lesquen, A', 'Loidl, M', 'Mallet, J', 'Marnieros, S', 'Martineau, O', 'Mirabolfathi, N', 'Mosca, L', 'Miramonti, L', 'Navick, X F', 'Nollez, G', 'Pari, P', 'Stern, M', 'Vagneron, L']",['First Results of the EDELWEISS WIMP Search using a 320 g Heat-and-Ionization Ge Detector'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, search for', 'scattering, WIMP nucleus', 'energy spectrum, recoil', 'ionization', 'scattering, WIMP nucleon', 'supersymmetry', 'cross section, mass', 'upper limit', 'semiconductor detector, germanium', 'cryogenics', 'deep underground detector, Frejus', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106094'],['The EDELWEISS collaboration has performed a direct search for WIMP dark matter using a 320 g heat-and-ionization cryogenic Ge detector operated in a low-background environment in the Laboratoire Souterrain de Modane. No nuclear recoils are observed in the fiducial volume in the 30-200 keV energy range during an effective exposure of 4.53 kg.days. Limits for the cross-section for the spin-independent interaction of WIMPs and nucleons are set in the framework of the Minimal Supersymmetric Standard Model (MSSM). The central value of the signal reported by the experiment DAMA is excluded at 90% CL.'],['2001-06-07'] +108,['eng'],"['Ter-Antonian, S V', 'Biermann, P L']",['Test of primary model predictions by EAS size spectra'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'nucleus, cosmic radiation', 'showers, air', 'cosmic radiation, particle source', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106091'],"['High statistical accuracy of experiments KASCADE and ANI allowed to obtain approximations of primary energy spectra and elemental composition in the ""knee"" region. Obtained results point out to the correctness of QGSJET interaction model and 2-component model of primary cosmic ray origin up to 100 PeV energies.']",['2001-06-07'] +109,['eng'],"['Crocker, R M', 'Melia, F', 'Volkas, R R']",['Discovering Long Wavelength Neutrino Oscillations in the Distorted Neutrino Spectrum of Galactic Supernova Remnants'],['Astrophysics and Astronomy'],"['supernova', 'galaxy', 'neutrino, cosmic radiation', 'neutrino, particle source', 'neutrino, oscillation', 'neutrino, atmosphere', 'neutrino, solar', 'neutrino, flux', 'neutrino, mass difference', 'counters and detectors, resolution', 'numerical calculations', 'experimental methods, proposed', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106090'],"[""We investigate the muon neutrino event rate in km$^3$ neutrino telescopes due to a number of galactic supernova remnants expected on the basis of these objects' known $\\gamma$-ray signals. We evaluate the potential of these neutrino signals to exhibit evidence of the sub-dominant neutrino oscillations expected in various neutrino mixing schemes including pseudo-Dirac scenarios and the Exact Parity Model. With ten years' data, neutrino signals from Sgr A East should either discover or exclude neutrino oscillations governed by a $\\delta m^2$ parameter in the range $10^{-12}$ to $10^{-15}$ eV$^2$. Such a capability is not available to terrestrial or solar system neutrino experiments.""]",['2001-06-07'] +110,['eng'],"['Bartolo, N', 'Matarrese, S', 'Riotto, A']",['Oscillations During Inflation and Cosmological Density Perturbations'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'perturbation, adiabatic', 'oscillation', 'energy, density', 'entropy, perturbation', 'perturbation, correlation', 'boundary condition']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106022'],"['Adiabatic (curvature) perturbations are produced during a period of cosmological inflation that is driven by a single scalar field, the inflaton. On particle physics grounds -- though -- it is natural to expect that this scalar field is coupled to other scalar degrees of freedom. This gives rise to oscillations between the perturbation of the inflaton field and the perturbations of the other scalar degrees of freedom, similar to the phenomenon of neutrino oscillations. Since the degree of the mixing is governed by the squared mass matrix of the scalar fields, the oscillations can occur even if the energy density of the extra scalar fields is much smaller than the energy density of the inflaton field. The probability of oscillation is resonantly amplified when perturbations cross the horizon and the perturbations in the inflaton field may disappear at horizon crossing giving rise to perturbations in scalar fields other than the inflaton. Adiabatic and isocurvature perturbations are inevitably correlated at the end of inflation and we provide a simple expression for the cross-correlation in terms of the slow-roll parameters.']",['2001-06-04'] +111,['eng'],"['Schwarz, Dominik J', 'Terrero-Escalante, C A', 'Garcia, A A']",['Higher order corrections to primordial spectra from cosmological inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'spectra, perturbation', 'correction, higher-order', 'Hubble constant', 'approximation', 'space-time, horizon', 'spectra, scalar', 'spectra, tensor', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106020'],"['We calculate power spectra of cosmological perturbations at high accuracy for two classes of inflation models. We classify the models according to the behaviour of the Hubble distance during inflation. Our approximation works if the Hubble distance can be approximated either to be a constant or to grow linearly with cosmic time. Many popular inflationary models can be described in this way, e.g., chaotic inflation with a monomial potential, power-law inflation and inflation at a maximum. Our scheme of approximation does not rely on a slow-roll expansion. Thus we can make accurate predictions for some of the models with large slow-roll parameters.']",['2001-06-04'] +112,['eng'],"['Kusenko, A', 'Steinhardt, Paul Joseph']",['Q-ball candidates for self-interacting dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'Q-ball, interaction', 'scattering, Q-ball p', 'cross section', 'astrophysics, model', 'Q-ball, production', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0106008'],"['We show that non-topological solitons, known as Q-balls, are promising candidates for self-interacting dark matter. They can satisfy the cross-section requirements for a broad range of masses. Unlike previously considered examples, Q-balls can stick together after collision, reducing the effective self-interaction rate to a negligible value after a few collisions per particle. This feature modifies predictions for halo formation. We also discuss the possibility that Q-balls have large interaction cross-sections with ordinary matter.']",['2001-06-04'] +113,['eng'],"['McGuire, P C', 'Steinhardt, Paul Joseph']",['Cracking Open the Window for Strongly Interacting Massive Particles as the Halo Dark Matter'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'astrophysics, missing-mass', 'SIMP, mass', 'scattering, SIMP nucleon', 'cross section', 'mass, dependence', 'WIMP', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105567'],"[""In the early 1990's, an analysis was completed by several theorists of the available mass/cross-section parameter space for unusual particle candidates to solve the dark matter problem, e.g. strongly interacting massive particles (SIMPs). This analysis found several unconstrained windows, such that for SIMP masses and cross-sections within these windows, SIMPs could still be the dominant dark matter in our Galactic halo. Since the early 1990's, some of these windows have been narrowed or closed, and some of these windows have been widened further by more careful analysis. We summarize the present state of the SIMP parameter space, and point to the cosmological salience of SIMPs as dark matter, given some of the present inadequacies of the WIMP solution to the dark matter problem.""]",['2001-06-01'] +114,['eng'],"['Arbey, A', 'Lesgourgues, Julien', 'Salati, Pierre']",['Quintessential Haloes around Galaxies'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'galaxy', 'quintessence', 'field theory, scalar', 'massive', 'boson, condensation', 'gravitation', 'coupling, matter', 'luminosity', 'statistical analysis', 'Einstein equation', 'Klein-Gordon equation, solution', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105564'],['The nature of the dark matter that binds galaxies remains an open question. The favoured candidate has been so far the neutralino. This massive species with evanescent interactions is now in difficulty. It would actually collapse in dense clumps and would therefore play havoc with the matter it is supposed to shepherd. We focus here on a massive and non-interacting charged scalar field as an alternate option to the astronomical missing mass. We investigate the classical solutions that describe the Bose condensate of such a field in gravitational interaction with matter. This simplistic model accounts quite well for the dark matter inside low-luminosity spirals whereas the agreement lessens for the brightest objects where baryons dominate. A scalar mass around m = 10^{-24} eV is derived when both high and low-luminosity spirals are fitted at the same time. Comparison with astronomical observations is made quantitative through a chi-squared analysis. We conclude that scalar fields offer a promising direction worth being explored.'],['2001-06-01'] +115,['eng'],"['Hirotani, K', 'Shibata, S']",['Electrodynamic Structure of an Outer-Gap Accelerator'],['Astrophysics and Astronomy'],"['n, matter', 'sphere, magnetic', 'electron, pair production', 'electron, acceleration', 'photon, emission', 'photon, cosmic radiation', 'cosmic radiation, flux', 'Vlasov equation, solution', 'current, density', 'gap', 'pulsar', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105549'],"['We investigate a stationary pair production cascade in the outer magnetosphere of a spinning neutron star. The charge depletion due to global flows of charged particles, causes a large electric field along the magnetic field lines. Migratory electrons and/or positrons are accelerated by this field to radiate curvature gamma-rays, some of which collide with the X-rays to materialize as pairs in the gap. The replenished charges partially screen the electric field, which is self-consistently solved, together with the distribution functions of particles and gamma-rays. By solving the Vlasov equations describing this pair production cascade, we demonstrate the existence of a stationary gap in the outer magnetosphere of PSR B1055-52 for a wide range of current densities flowing in the accelerator: From sub to super Goldreich-Julian values. However, we find that the expected GeV spectrum becomes very soft if the current density exceeds the Goldreich-Julian value. We also demonstrate that the GeV spectrum softens with decreasing magnetic inclination and with increasing distance to this pulsar. We thus conclude that a sub-Goldreich-Julian current, a large magnetic inclination, and a small distance (500 pc, say) are plausible to account for EGRET observations. Furthermore, it is found that the TeV flux due to inverse Compton scatterings of infrared photons whose spectrum is inferred from the Rayleigh-Jeans side of the soft blackbody spectrum is much less than the observational upper limit.']",['2001-06-01'] +116,['eng'],"['Mücke, A', 'Protheroe, R J']",['Neutrino Emission from HBLs and LBLs'],['Astrophysics and Astronomy'],"['talk, Hamburg 2001/08/07', 'p, cosmic radiation', 'blazar', 'synchrotron radiation', 'p, acceleration', 'energy loss', 'neutrino, cosmic radiation', 'neutrino, energy spectrum', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105543'],"['The Synchrotron Proton Blazar model is a promising model to explain high energy emission from gamma-ray loud BL Lac objects like Mkn 421. In contrast to leptonic models, the hadronic explanation of gamma-ray emission predicts ultrahigh energy neutrinos. The predicted neutrino spectra from a typical High-energy cutoff BL Lac Object (HBL) and a Low-energy cutoff BL Lac Object (LBL) are presented. We find that cooling due to muon synchrotron radiation causes a cutoff of the neutrino spectrum at $\\sim 10^{18}$ eV, with the exception of $\\nu_\\mu$ from kaon decay which may extend to higher energies if meson production takes place in the secondary resonance region of the cross section. The impact of the neutrino output from both source populations to the diffuse neutrino background is discussed.']",['2001-06-01'] +117,['eng'],"['Majumdar, A S']",['From brane assisted inflation to quintessence through a single scalar field'],['Astrophysics and Astronomy'],"['inflationary universe', 'quintessence', 'membrane model', 'field theory, scalar', 'potential']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105518'],['We explore within the context of brane cosmology whether it is possible to obtain both early inflation and accelerated expansion during the present epoch through the dynamics of the same scalar field in an exponential potential. Considerations from successful inflation and viable radiation and matter dominated eras impose constraints on the parameters of the potential. We find that the additional requirement of late time quintessence behaviour in conformity with present observations necessitates the inclusion of two exponential terms in the potential.'],['2001-05-31'] +118,['eng'],"['Mok, H M']",['A Possible Solution to the Cosmological Constant Problem By Discrete Space-time Hypothesis'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'space-time, discrete', 'astrophysics, acceleration', 'supernova', 'cosmic radiation, background', 'inflationary universe', 'mass, density', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105513'],['The cosmological constant problem is explained by a theory based on the discrete space-time hypothesis. The calculated cosmological constant value is of the order of 10^-52[m]^-2 or equivalent to about 0.7 of the critical mass density. It is in excellent agreement with Type Ia SN observational data and recent results of BOOMERANG and MAXIMA. Our theory also implies that the quantization of the space-time metric is not necessary since it is not a fundamental field. The divergence problem of quantum gravity is then of no interest. Cosmic inflation is given out as a consequence of the theory and the universe is found to be alternatively dominated by the cosmological constant and the mass density at different cosmic time period. Our calculation also shows that the mass energy density is of similar order of magnitude as the vacuum energy density in the present universe but it is just a coincidence. This result supports the anthropic principle.'],['2001-05-31'] +119,['eng'],"['Dimopoulos, K']",['Galactic Magnetic Fields as a consequence of Inflation'],['Astrophysics and Astronomy'],"['talk, Penteli 2001/04/19', 'inflationary universe', 'magnetic field, galaxy', 'Z0, production', 'horizon']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105488'],"['The generation of a magnetic field in the Early Universe is considered, due to the gravitational production of the Z-boson field during inflation. Scaled to the epoch of galaxy formation this magnetic field suffices to trigger the galactic dynamo and explain the observed galactic magnetic fields. The mechanism is independent of the inflationary model.']",['2001-05-29'] +120,['eng'],"['Zimdahl, W', 'Pavón, D']",['Interacting Quintessence'],['Astrophysics and Astronomy'],"['quintessence', 'astrophysics, missing-mass', 'fluid', 'energy, density', 'attractor']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105479'],['We demonstrate that a suitable coupling between a quintessence scalar field and a pressureless cold dark matter (CDM) fluid leads to a constant ratio of the energy densities of both components which is compatible with an accelerated expansion of the Universe.'],['2001-05-29'] +121,['eng'],[],['Search for Supernova Neutrino-Bursts with the AMANDA Detector'],['Astrophysics and Astronomy'],"['astrophysics', 'supernova', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'antineutrino p, interaction', 'antineutrino/e', 'charged current', 'data analysis method', 'Cherenkov counter, water', 'performance', 'trigger', 'deep underground detector, AMANDA', 'experimental results', 'antineutrino/e p --> n positron']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105460'],"[""The core collapse of a massive star in the Milky Way will produce a neutrino burst, intense enough to be detected by existing underground detectors. The AMANDA neutrino telescope located deep in the South Pole ice can detect MeV neutrinos by a collective rate increase in all photo-multipliers on top of dark noise. The main source of light comes from positrons produced in the CC-reaction of anti-electron neutrinos on free protons $\\antinue + p \\to e^+ + n$. This paper describes the first supernova search performed on the full sets of data taken during 1997 and 1998 (215 days of live time) with 302 of the detector's optical modules. No candidate events resulted from this search. The performance of the detector is calculated, yielding a 70% coverage of the Galaxy with one background fake per year with 90% efficiency for the detector configuration under study. An upper limit at the 90% c.l. on the rate of stellar collapses in the Milky Way is derived, yielding 4.3 events per year. A trigger algorithm is presented and its performance estimated. Possible improvements of the detector hardware are reviewed.""]",['2001-05-28'] +122,['eng'],"['Doran, M', 'Lilley, M', 'Wetterich, C']",['Constraining Quintessence with the New CMB Data'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'quintessence', 'astrophysics, acceleration', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105457'],"['The CMB data recently released by BOOMERANG and MAXIMA suggest that the anisotropy spectrum has a third peak in the range 8001 are disfavoured. Models with more than 5% quintessence before last scattering require a spectral index greater than 1. We also show that the CMB alone now provides strong evidence for an accelerating universe.']",['2001-05-28'] +123,['eng'],"['Watanabe, S', 'Shibahashi, H']",['Solar Models with Helioseismic Constraints and the Solar Neutrino Problem'],['Astrophysics and Astronomy'],"['model, solar', 'neutrino, solar', 'neutrino, flux', 'velocity, acoustic', 'metal, density', 'neutrino, oscillation', 'neutrino, capture', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105445'],"['Imposing a constraint of the sound-speed profile determined from helioseismology and updating the microphysics, we have revised our seismic solar model, constructed with the assumption of a homogeneous metal abundance distribution, and have shown that the theoretically expected neutrino fluxes are still significantly more than the observations. With the same sound-speed profile constraint, we also constructed solar models with low metal abundance in the core, and evaluated the neutrino fluxes of these models to see if nonstandard solar models with a low metal core can solve the solar neutrino problem. Some of these models are in agreement with the Homestake data, the Super-Kamiokande data, and the sound-speed profile simultaneously, but none of these satisfy both the neutrino flux data, including GALLEX and SAGE, and the helioseismically determined density profile.']",['2001-05-28'] +124,['eng'],"['Krawczynski, H', 'Sambruna, R M', 'Kohnle, A', 'Coppi, P S', 'Aharonian, F A']",['Simultaneous X-Ray and TeV Gamma-Ray Observations of the TeV Blazar Markarian 421 during February and May 2000'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'time dependence', 'blazar', 'photon, energy spectrum', 'counters and detectors, satellite', 'Cherenkov counter, experimental results', 'tables']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105331'],"['In this paper we present the results of simultaneous observations of the TeV blazar Markarian 421 (Mrk 421) at X-ray and TeV Gamma-ray energies with the Rossi X-Ray Timing Explorer (RXTE) and the stereoscopic Cherenkov Telescope system of the HEGRA (High Energy Gamma Ray Astronomy) experiment, respectively. The source was monitored from February 2nd to February 16th and from May 3rd to May 8th, 2000. We discuss in detail the temporal and spectral properties of the source. Remarkably, the TeV observations of February 7th/8th showed statistically significant evidence for substantial TeV flux variability on 30 min time scale. We show the results of modeling the data with a time dependent homogeneous Synchrotron Self-Compton (SSC) model. The X-ray and TeV gamma-ray emission strengths and energy spectra together with the rapid flux variability strongly suggest that the emission volume is approaching the observer with a Doppler factor of 50 or higher. The different flux variability time scales observed at X-rays and TeV Gamma-rays indicate that a more detailed analysis will require inhomogeneous models with several emission zones.']",['2001-05-21'] +125,['eng'],"['Cline, David B', 'Sergiampietri, F', 'Learned, J G', 'McDonald, K F']","['LANNDD---A Massive Liquid Argon Detector for Proton Decay, Supernova and Solar Neutrino Studies, and a Neutrino Factory Detector']",['Astrophysics and Astronomy'],"['talk, Tsukuba 2001/05/24', 'neutrino, solar', 'neutrino, cosmic radiation', 'showers, air', 'neutrino, oscillation', 'supernova', 'p, decay', 'drift chamber, time projection', 'drift chamber, liquid argon', 'deep underground detector']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105442'],['We describe a possible Liquid Argon Neutrino and Nuclear Decay Detector (LANNDD) that consists of a 70kt magnetized liquid argon tracking detector. The detector is being designed for the Carlsbad Underground Laboratory.'],['2001-12-14'] +126,['eng'],"['Van Putten, M H P M', 'Levinson, A']",['Calorimetry of gamma-ray bursts'],['Astrophysics and Astronomy'],"['black hole, luminosity', 'torus', 'gravitational radiation', 'gamma ray burst', 'energy', 'jet']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105429'],"['Black holes surrounded by a disk or torus may drive the enigmatic cosmological gamma-ray bursts (GRBs). Equivalence in poloidal topology to pulsar magnetospheres shows a high incidence of the black hole-luminosity $L_H$ into the surrounding magnetized matter. We argue that this emission is re-radiated into gravitational waves at $L_{GW}\\simeq L_H/3$ in frequencies of order 1kHz, winds and, potentially, MeV neutrinos. The total energy budget and input to the GRB from baryon poor jets are expected to be standard in this scenario, consistent with recent analysis of afterglow data. Collimation of these outflows by baryon rich disk or torus winds may account for the observed spread in opening angles up to about $35^o$. This model may be tested by future LIGO/VIRGO observations.']",['2001-05-25'] +127,['eng'],"['Kasuya, S']",['Difficulty of a spinning complex scalar field to be dark energy'],['Astrophysics and Astronomy'],"['field theory, scalar', 'dark energy', 'soliton', 'Q-ball', 'field theory, fluctuation', 'astrophysics, acceleration']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105408'],"['We comment on the possibility of a spinning complex scalar field to be dark energy. We show that it deforms (almost) completely into a nontopological soliton state, a Q ball, and the equation of state becomes that of the matter or radiation, depending on the fate of the Q ball. Thus, the spinning complex scalar field cannot play the role of the dark energy.']",['2001-05-24'] +128,['eng'],"['Hansen, S H', 'Mangano, G', 'Melchiorri, A', 'Miele, G', 'Pisanti, O']",['Constraining neutrino physics with BBN and CMBR'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'neutrino, flavor', 'potential, chemical', 'supernova', 'data analysis method', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105385'],"['We perform a likelihood analysis of the recent results on the anisotropy of Cosmic Microwave Background Radiation from the BOOMERanG and DASI experiments to show that they single out an effective number of neutrinos in good agreement with standard Big Bang Nucleosynthesis. We also consider degenerate Big Bang Nucleosynthesis to provide new bounds on effective relativistic degrees of freedom $N_\\nu$ and, in particular, on neutrino chemical potential $\\xi_\\alpha$. When including Supernova Ia data we find, at $2\\sigma$, $N_\\nu \\leq 7$ and $-0.01 \\leq \\xi_e \\leq 0.22$, $|\\xi_{\\mu,\\tau}|\\leq 2.6$.']",['2001-05-23'] +129,['eng'],"['Cornish, N J']",['Mapping the gravitational wave background'],['Astrophysics and Astronomy'],"['gravitational radiation, background', 'gravitational radiation, anisotropy', 'counters and detectors', 'laser, interference', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105374'],"['The gravitational wave sky is expected to have isolated bright sources superimposed on a diffuse gravitational wave background. The background radiation has two components: a confusion limited background from unresolved astrophysical sources; and a cosmological component formed during the birth of the universe. A map of the gravitational wave background can be made by sweeping a gravitational wave detector across the sky. The detector output is a complicated convolution of the sky luminosity distribution, the detector response function and the scan pattern. Here we study the general de-convolution problem, and show how LIGO (Laser Interferometric Gravitational Observatory) and LISA (Laser Interferometer Space Antenna) can be used to detect anisotropies in the gravitational wave background.']",['2001-05-23'] +130,['eng'],"['Lesgourgues, Julien', 'Liddle, A R']",['The lepton asymmetry'],['Astrophysics and Astronomy'],"['astrophysics, model', 'lepton, asymmetry', 'statistical analysis', 'neutrino, massless', 'neutrino, massive', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105361'],"['We use a wide range of observations to constrain cosmological models possessing a significant asymmetry in the lepton sector, which offer perhaps the best chance of reconciling a critical-density Universe with current observations. The simplest case, with massless neutrinos, fails to fit many experimental data and does not lead to an acceptable model. If the neutrinos have mass of order one electron-volt (which is favoured by some neutrino observations), then models can be implemented which prove a good fit to microwave anisotropies and large-scale structure data. However, taking into account the latest microwave anisotropy results, especially those from Boomerang, we show that the model can no longer accommodate the observed baryon fraction in clusters. Together with the observed acceleration of the present Universe, this puts considerable pressure on such critical-density models.']",['2001-05-22'] +131,['eng'],"['Lahav, O']","[""New Cosmological Data and the `Best-Fit' FRW Universe""]",['Astrophysics and Astronomy'],"['talk, Lisbon 2000/07/27', 'Friedman model', 'space-time, Robertson-Walker', 'cosmic radiation, background', 'supernova', 'velocity', 'galaxy, cluster', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105353'],"['Observational tests for the homogeneity of the Universe on large scales are reviewed. Assuming the Cosmological Principle we then estimate cosmological parameters by joint analysis of the Cosmic Microwave Background, Supernovae Ia, peculiar velocities, cluster abundance and redshift surveys. Our results are consistent with results obtained by other groups, suggesting a best-fit FRW Universe with $\\omegam = 1 -\\lambda \\approx 0.3$ and $H_0 \\approx 75$ km/sec/Mpc. We point out some potential problems with this currently popular model.']",['2001-05-22'] +132,['eng'],"['Boyle, L A', 'Caldwell, R R', 'Kamionkowski, M P']",['Spintessence! New Models for Dark Matter and Dark Energy'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'dark energy', 'field theory, scalar', 'potential', 'symmetry, U(1)', 'spintessence', 'quintessence', 'baryon, production', 'dark matter, fuzzy', 'density, perturbation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105318'],"[""We propose a new class of ``spintessence'' models for dark matter and/or negative-pressure, dynamical dark energy consisting of a complex scalar field $\\phi$ spinning in a U(1)-symmetric potential $V(\\phi)=V(|\\phi|)$. As the Universe expands, the field spirals slowly toward the origin. The choice of $V(\\phi)$ determines the equation-of-state parameter ${w}$, which may be either constant or evolving with time. Spintessence models can introduce a variety of novel effects in the growth of density perturbations. We discuss connections with quintessence and self-interacting and fuzzy cold dark matter, possible implications for the coincidence problem, baryogenesis, and cosmological birefringence, as well as generalizations of spintessence to models with higher global symmetry and models in which the symmetry is not exact.""]",['2001-05-21'] +133,['eng'],"['Lindner, M', 'Ohlsson, T', 'Winter, W']",['Decays of supernova neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'supernova', 'neutrino, decay', 'neutrino, width', 'neutrino, oscillation', 'neutrino, flux', 'time dependence', 'coherence', 'mass, dispersion', 'Majoron, decay', 'interference, effect', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105309'],"['Supernova neutrinos could be well-suited for probing neutrino decay, since decay may be observed even for very small decay rates or coupling constants. We will use a combined description of neutrino decay and neutrino oscillations for supernova neutrinos, especially taking into account two properties: One is the radially symmetric neutrino flux, allowing a decay product to be re-directed towards the observer, even if the parent neutrino had a different original direction of propagation. The other is decoherence, because of the long baselines. We will demonstrate how supernova neutrino decay and oscillations can be described by an effective theory, which allows us to calculate the time-dependent fluxes at the detector. In addition, we will show the implications of a Majoron-like decay model. As a result, we will observe some effects which may also mimic signals similar to the ones expected from supernova models, making it in general harder to separate neutrino and supernova properties.']",['2001-05-18'] +134,['eng'],"['Dzhilkibaev, Z A']",['A search for very high energy neutrinos with the Baikal Neutrino Telescope'],['Astrophysics and Astronomy'],"['talk, Venice 2001/03/06', 'neutrino, cosmic radiation', 'neutrino, energy', 'neutrino/e, flux', 'Cherenkov counter, water', 'deep underground detector, Baikal', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105269'],"['We present the results of a search for high energy neutrinos with the Baikal underwater Cherenkov detector {\\it NT-200.} An upper limit on the ($\\nu_e+\\tilde{\\nu_e}$) diffuse flux of $E^2 \\Phi_{\\nu}(E)<(1.3 \\div 1.9)\\cdot 10^{-6} {cm}^{-2} {s}^{-1} {sr}^{-1} {GeV}$ within a neutrino energy range $10^4 \\div 10^7 {GeV}$ is obtained, assuming an $E^{-2}$ behaviour of the neutrino spectrum and flavor ratio $(\\nu_e+\\tilde{\\nu_e}):(\\nu_{\\mu}+\\tilde{\\nu_{\\mu}})$=1:2.']",['2001-05-17'] +135,['eng'],"['Regimbau, T', 'De Pacheco, J A F']",['Cosmic Background of Gravitational Waves from Rotating Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'rotational', 'gravitational radiation, background', 'background, measurement', 'magnetic field, pulsar', 'energy, density', 'counters and detectors', 'resonance, mass', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105260'],"[""The extragalactic background of gravitational waves produced by tri-axial rotating neutron stars was calculated, under the assumption that the properties of the underlying pulsar population are the same of those of the galactic population, recently derived by Regimbau & de Freitas Pacheco (2000). For an equatorial ellipticity of $\\epsilon$ = 10$^{-6}$, the equivalent density parameter due to gravitational waves has a maximum amplitude in the range 2$\\times10^{-11}-3\\times10^{-9}$, around 0.9-1.5 kHz. The main reasons affecting the theoretical predictions are discussed. This background is comparable to that produced by the ''ring-down'' emission from distorted black holes. The detection possibility of this background by a future generation of gravitational antennas is also examined.""]",['2001-05-16'] +136,['eng'],"['Green, A M']",['Viability of evaporating primordial black holes as short period gamma-ray bursts'],['Astrophysics and Astronomy'],"['black hole, radiation', 'gamma ray burst', 'density, perturbation', 'black hole, mass', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105253'],"['It has been proposed that the short period gamma-ray bursts, which occur at a rate of 10 yr^{-1} may be evaporating primordial black holes (PBHs). Calculations of the present PBH evaporation rate have traditionally assumed that the PBH mass function varies as M^{-5/2}. This mass function only arises if the density perturbations from which the PBHs form have a scale invariant power spectrum. It is now known that for a scale invariant power spectrum, normalised to COBE on large scales, the PBH density is completely negligible, so that this mass function is cosmologically irrelevant. For non-scale-invariant power spectra, if all PBHs which form at given epoch have a fixed mass then the PBH mass function is sharply peaked around that mass, whilst if the PBH mass depends on the size of the density perturbation from which it forms, as is expected when critical phenomena are taken into account, then the PBH mass function will be far broader than M^{-5/2}. In this paper we calculate the present day PBH evaporation rate, using constraints from the diffuse gamma-ray background, for both of these mass functions. If the PBH mass function has significant finite width, as recent numerical simulations suggest, then it is not possible to produce a present day PBH evaporation rate comparable with the observed short period gamma-ray burst rate. This could also have implications for other attempts to detect evaporating PBHs.']",['2001-05-16'] +137,['eng'],"['Raffelt, G G']",['Mu- and Tau-Neutrino Spectra Formation in Supernovae'],['Astrophysics and Astronomy'],"['supernova', 'neutrino/tau, flux', 'neutrino/mu, flux', 'neutrino nucleon, elastic scattering', 'nucleon nucleon, bremsstrahlung', 'flux, spectra', 'temperature, dependence', 'transport theory', 'nucleon, recoil', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105250'],"['The mu- and tau-neutrinos emitted from a proto-neutron star are produced by nucleonic bremsstrahlung N + N -> N + N + nu + nu-bar and pair annihilation e^+ + e^- -> nu + nu-bar, reactions which freeze out at the ""energy sphere."" Before escaping from there to infinity the neutrinos diffuse through the ""scattering atmosphere,"" a layer where their main interaction is elastic scattering on nucleons nu + N -> N + nu. If these collisions are taken to be iso-energetic as in all numerical supernova simulations, the neutrino flux spectrum escaping to infinity depends only on the medium temperature T_ES and the thermally averaged optical depth tau_ES at the energy sphere. For tau_ES = 10-50 one finds for the spectral flux temperature of the escaping neutrinos T_flux = 0.5-0.6 T_ES. Including energy exchange (nucleon recoil) in nu + N -> N + nu can shift T_flux both up or down. Delta T_flux depends on tau_ES, on the scattering atmosphere\'s temperature profile, and on T_ES. Based on a numerical study we find that for typical conditions Delta T_flux/T_flux is between -10% and -20%, and even for extreme parameter choices does not exceed -30%. The exact value of Delta T_flux/T_flux is surprisingly insensitive to the assumed value of the nucleon mass, i.e. the exact efficiency of energy transfer between neutrinos and nucleons is not important as long as it can occur at all. Therefore, calculating the nu_mu and nu_tau spectra does not seem to require a precise knowledge of the nuclear medium\'s dynamical structure functions.']",['2001-05-16'] +138,['eng'],"['Blasi, P', 'Dick, R', 'Kolb, E W']",['Ultra-high energy cosmic rays from annihilation of superheavy dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMPZILLA, annihilation', 'cosmic radiation, production', 'cross section', 'GZK effect', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'galaxy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105232'],"['We consider the possibility that ultra-high energy cosmic rays originate from the annihilation of relic superheavy dark-matter particles. We find that a cross section of ~ 10^{-26}cm^2 (M_X/10^{12}GeV)^{3/2} is required to account for the observed rate of super-GZK events if the superheavy dark matter follows a Navarro-Frenk-White density profile. We also calculate the possible signature from annihilation in sub-galactic clumps of dark matter and find that the signal from sub-galactic structures may dominate. Finally, we discuss the expected anisotropy in the arrival directions of the cosmic rays, which is a characteristic signature of this scenario.']",['2001-05-15'] +139,['eng'],"['Jaikumar, P', 'Prakash, M']",['Neutrino Pair Emission from Cooper Pair Breaking and Recombination in Superfluid Quark Matter'],['Astrophysics and Astronomy'],"['quark, matter', 'superfluid', 'neutrino, pair production', 'critical phenomena', 'neutrino quark, interaction', 'effective Hamiltonian', 'neutral current']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105225'],"['For the low energy Standard Model neutrino-matter interactions, we calculate neutrino pair ($\\nu\\bar\\nu$) emissivites in superfluid quark matter. Just below the critical temperature, Cooper pairs continuously break and recombine, resulting in the emission of $\\nu\\bar \\nu$ pairs with a rate that greatly exceeds the standard quark modified Urca and bremsstrahlung rates. At the same baryon density in baryonic and quark matter, the ratio of baryon to quark $\\nu\\bar\\nu$ emissivites lies in the range 2-5 for the densities of interest in the long-term cooling of solar mass compact stars. We also find that in matter containing hyperons, $\\nu\\bar\\nu$ emission can occur with hyperons of all species.']",['2001-05-15'] +140,['eng'],"['Nelemans, G', 'Yungelson, L R', 'Zwart, S F P']",['The gravitational wave signal from the Galactic disk population of binaries containing two compact objects'],['Astrophysics and Astronomy'],"['galaxy', 'binary', 'matter, compact', 'gravitational radiation, emission', 'white dwarf', 'n, matter', 'black hole', 'background', 'gravitational radiation, counters and detectors', 'interference, laser', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105221'],"['We review the properties of Galactic binaries containing two compact objects, as derived by means of population synthesis. Using this information we calculate the gravitational wave signal of these binaries. At frequencies below f ~< 2 mHz the double white dwarf population forms an unresolved background for the low-frequency gravitational wave detector LISA. Above this limit some few thousand double white dwarfs and few tens of binaries containing neutron stars will be resolved. Of the resolved double white dwarfs ~500 have a total mass above the Chandrasekhar limit. About ~95 of these have a measurable frequency change allowing a determination of their chirp mass. We discuss the properties of the resolved systems.']",['2001-05-15'] +141,['eng'],"['Hannestad, S']",['New CMBR data and the cosmic neutrino background'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'neutrino, cosmic radiation', 'neutrino, flavor', 'light nucleus, production', 'cosmic radiation, spectra', 'matter, spectra', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105220'],"['New precision Cosmic Microwave Background Radiation (CMBR) anisotropy data are beginning to constrain physics beyond the standard model, for example in the form of additional light particle species. These constraints are complementary to what can be obtained from big bang nucleosynthesis (BBN) considerations because they apply to much later times. We derive a constraint on the equivalent number of neutrino species, N_\\nu, from the presently available data. Specifically we analyse two different CMBR data sets to test the robustness of our results. Analyzing only CMBR data yields an upper bound of N_\\nu < 17 (95% confidence). Adding large scale structure (LSS) data from the PSC-z survey tightens the upper bound slightly. However, the addition of LSS data gives a non-trivial {\\it lower} bound of N_\\nu > 1.5/2.5 (95% confidence) for the two data sets. This is the first independent indication of the presence of the cosmological neutrino background which is predicted by the standard model, and seen in big bang nucleosynthesis. The value $N_\\nu = 0$ is disfavoured at 3\\sigma and 4\\sigma for the two data sets respectively.']",['2001-05-15'] +142,['eng'],"['Kawasaki, M', 'Moroi, T', 'Takahashi, T']",['Cosmic Microwave Background Anisotropy with Cosine-Type Quintessence'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'quintessence', 'fluctuation, adiabatic', 'space-time, fluctuation', 'field theory, scalar', 'zero mode', 'inflationary universe', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105161'],"['We study the Cosmic Microwave Background (CMB) anisotropies produced by cosine-type quintessence models. In our analysis, effects of the adiabatic and isocurvature fluctuations are both taken into account. For purely adiabatic fluctuations with scale invariant spectrum, we obtain a stringent constraint on the model parameters using the CMB data from COBE, BOOMERanG and MAXIMA. Furthermore, it is shown that isocurvature fluctuations have significant effects on the CMB angular power spectrum at low multipoles in some parameter space, which may be detectable in future satellite experiments. Such a signal may be used to distinguish the cosine-type quintessence models from the tracker-type ones.']",['2001-05-11'] +143,['eng'],"['Medvedev, M V']",['Constraints on SIDM with flavor mixing'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'interference', 'astrophysics, model', 'mass', 'quantum mechanics, wave function']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105156'],"['The self-interacting dark matter (SIDM) model with flavor mixing (astro-ph/0010616) was proposed to resolve problems of the CDM model on small scales by keeping attractive features of both SIDM and annihilating dark matter, and simultaneously avoid their drawbacks. A dark particle produced in a flavor eigenstate will separate into two mass eigenstates because they propagate with different velocities and, in a gravitational filed, along different geodesics, see Fig. 1. Thus, in the flavor-mixed SIDM, dark halos are made of heavy eigenstates, whereas light eigenstates may leave the halo. Collisions (elastic scattering) of mass states results in eigenstate conversion, see Fig. 2, which leads to the gradual decrease of the halo mass in high-density cusps. On the other hand, in the early Universe, one may expect a problem of over-production of light (hot) particles over heavy (cold) when the temperature of dark matter falls below the mass of the heavy component. We show how this problem is avoided.']",['2001-12-14'] +144,['eng'],"['Zinkernagel, H']","['Cosmology, Particles, and the Unity of Science']",['Astrophysics and Astronomy'],"['astrophysics, model', 'particle physics', 'astrophysics, fundamental constant', 'inflationary universe', 'baryon, asymmetry', 'space-time', 'astrophysics, missing-mass', 'philosophy']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105130'],"['During the last three decades, there has been a growing realization among physicists and cosmologists that the relation between particle physics and cosmology may constitute yet another successful example of the unity of science. However, there are important conceptual problems in the unification of the two disciplines, e.g. in connection with the cosmological constant and the conjecture of inflation. The present article will outline some of these problems, and argue that the victory for the unity of science in the context of cosmology and particle physics is still far from obvious.']",['2001-05-09'] +145,['eng'],"['Ouyed, R', 'Dey, J', 'Dey, M']",['Quark-Nova as Gamma Ray Burst Precursor'],['Astrophysics and Astronomy'],"['n, matter', 'matter, strangeness', 'energy, emission', 'quark, matter', 'fireball', 'gamma ray burst', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105109'],"[""We explore the scenario where the core of a proto-neutron star (with densities above deconfinement value) shrinks into the equilibrated strange matter object. The left-out matter (the envelope of mass $M_{env.}$) free-falls following the core contraction releasing tremendous energies, up to $E_{QN} \\simeq 4 \\times 10^{52} {\\rm ergs}$ as a result of strangeness contamination or conversion or baryons to quarks - a phenomena we call Quark-Nova. We show that `dirty' fireballs are a natural outcome of Quark-Novae and could in principle account for Gamma Ray Burst precursor activity. We argue that in general the Quark-Nova ejecta (the `dirty' fireball) is absorbed or attenuated by the slow preceding Supernova ejecta explaining why only 3% of bursts exhibit precursor activity.""]",['2001-05-08'] +146,['eng'],"['Gu, J A', 'Hwang, W Y P']",['Can the quintessence be a complex scalar field?'],['Astrophysics and Astronomy'],"['astrophysics, expansion', 'expansion, accelerator', 'field theory, scalar', 'quintessence', 'energy, density', 'pressure', 'astrophysics, fundamental constant']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105099'],"['In light of the recent observations of type Ia supernovae (SNe Ia) suggesting an accelerating expansion of the Universe, we wish in this paper to point out the possibility of using a complex scalar field as the quintessence to account for the acceleration. In particular, we extend the idea of Huterer and Turner in deriving the reconstruction equations for the complex quintessence, showing the feasibility of making use of a complex scalar field (instead of a real scalar field) while maintaining the uniqueness feature of the reconstruction. We discuss very briefly how future observations may help to distinguish the different quintessence scenarios, including the scenario with a positive cosmological constant.']",['2001-05-08'] +147,['eng'],"['Dar, Arnon', 'De Rújula, Alvaro']",['The Cannonball Model of Gamma Ray Bursts'],['Astrophysics and Astronomy'],"['gamma ray burst, model', 'supernova', 'shell model', 'pi, decay modes', 'neutrino, production', 'neutrino, cosmic radiation', 'pi0, radiative decay', 'photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, energy', 'cosmic radiation, particle source', 'muon, cosmic radiation', 'angular distribution', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105094'],"['Recent observations suggest that $\\gamma$-ray bursts (GRBs) and their afterglows are produced by jets of highly relativistic cannonballs (CBs), emitted in supernova (SN) explosions. The CBs, reheated by their collision with the shell, emit radiation that is collimated along their direction of motion and Doppler-boosted to the typical few-hundred keV energy of the GRB. Accompanying the GRB, there should be an intense burst of neutrinos of a few hundreds of GeV energy, made by the decay of charged pions produced in the collisions of the CBs with the SN shell . The neutrino beam carries almost all of the emitted energy, but is much narrower than the GRB beam and should only be detected in coincidence with the small fraction of GRBs whose CBs are moving very close to the line of sight. The neutral pions made in the transparent outskirts of the SN shell decay into energetic $\\gamma$-rays (EGRs) of energy of ${\\cal{O}}$(100) GeV. The EGR beam, whose energy fluence is comparable to that of the companion GRB, is as wide as the GRB beam and should be observable, in coincidence with GRBs, with existing or planned detectors. We derive in detail these predictions of the CB model.']",['2001-05-08'] +148,['eng'],"['Deffayet, C', 'Dvali, G', 'Gabadadze, Gregory T']",['Accelerated Universe from Gravity Leaking to Extra Dimensions'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'gravitation, potential', 'space-time, higher-dimensional', 'Hubble constant', 'astrophysics, fundamental constant', 'membrane model', 'dimension, 4', 'dissipation', 'string model', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105068'],['We discuss the idea that the accelerated Universe could be the result of the gravitational leakage into extra dimensions on Hubble distances rather than the consequence of non-zero cosmological constant.'],['2001-05-07'] +149,['eng'],"['Bergström, L', 'Edsjö, J', 'Ullio, P']",['Spectral Gamma-ray Signatures of Cosmological Dark Matter Annihilation'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, annihilation', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'WIMP, mass', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0105048'],"['We propose a new signature for weakly interacting massive particle (WIMP) dark matter, a spectral feature in the diffuse extragalactic gamma-ray radiation. This feature, a sudden drop of the gamma-ray intensity at an energy corresponding to the WIMP mass, comes from the asymmetric distortion of the line due to WIMP annihilation into two gamma-rays caused by the cosmological redshift. Unlike other proposed searches for a line signal, this method is not very sensitive to the exact dark matter density distribution in halos and subhalos. The only requirement is that the mass distribution of substructure on small scales follows approximately the Press-Schechter law, and that smaller halos are on the average denser than large halos, which is a generic outcome of N-body simulations of Cold Dark Matter, and which has observational support. The upcoming Gamma-ray Large Area Space Telescope (GLAST) will be eminently suited to search for these spectral features. For numerical examples, we use rates computed for supersymmetric particle dark matter, where a detectable signal is possible.']",['2001-05-04'] +150,['eng'],"['Weinberg, S']",['Conference Summary - 20th Texas Symposium on Relativistic Astrophysics'],['Astrophysics and Astronomy'],"['conference, review', 'Austin 2000/12/10', 'astrophysics, relativistic', 'astrophysics, fundamental constant', 'space-time, higher-dimensional', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, fluctuation', 'vacuum state, energy', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104482'],"['This is the written version of the summary talk given at the 20th Texas Symposium on Relativistic Astrophysics in Austin, Texas, on December 15, 2000. After a brief summary of some of the highlights at the conference, comments are offered on three special topics: theories with large additional spatial dimensions, the cosmological constant problems, and the analysis of fluctuations in the cosmic microwave background.']",['2001-05-01'] +151,['eng'],"['Bean, R']",['Perturbation evolution with a non-minimally coupled scalar field'],['Astrophysics and Astronomy'],"['field theory, scalar', 'astrophysics, missing-mass', 'quintessence', 'dilaton', 'matter, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'galaxy, production', 'expansion, acceleration', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104464'],"[""We recently proposed a simple dilaton-derived quintessence model in which the scalar field was non-minimally coupled to cold dark matter, but not to `visible' matter. Such couplings can be attributed to the dilaton in the low energy limit of string theory, beyond tree level. In this paper we discuss the implications of such a model on structure formation, looking at its impact on matter perturbations and CMB anisotropies. We find that the model only deviates from $\\Lambda$CDM and minimally coupled theories at late times, and is well fitted to current observational data. The signature left by the coupling, when it breaks degeneracy at late times, presents a valuable opportunity to constrain non-minimal couplings given the wealth of new observational data promised in the near future.""]",['2001-05-01'] +152,['eng'],"['Bertou, X', 'Billoir, P', 'Deligny, O', 'Lachaud, C', 'Letessier-Selvon, A A']",['Tau Neutrinos in the Auger Observatory'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'cosmic radiation, secondary radiation', 'neutrino/tau, search for', 'neutrino, oscillation', 'GZK effect', 'tau, decay modes', 'showers, air', 'showers, production', 'Cherenkov counter', 'numerical calculations, Monte Carlo']","['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104452', 'http://documents.cern.ch/archive/electronic/other/uploader/MORIOND/nap-t8.ps']","['The cosmic ray spectrum has been shown to extend well beyond 10^{20}eV. With nearly 20 events observed in the last 40 years, it is now established that particles are accelerated or produced in the universe with energies near 10^{21}eV. In all production models neutrinos and photons are part of the cosmic ray flux. In acceleration models (bottom-up models), they are produced as secondaries of the possible interactions of the accelerated charged particle; in direct production models (top-down models) they are a dominant fraction of the decay chain. In addition, hadrons above the GZK threshold energy will also produce, along their path in the Universe, neutrinos and photons as secondaries of the pion photo-production processes. Therefore, photons and neutrinos are very distinctive signatures of the nature and distribution of the potential sources of ultra high energy cosmic rays. In the following we describe the tau neutrino detection and identification capabilities of the Auger observatory. We show that in the range 3x10^{17}-3x10^{20}eV the Auger effective apperture reaches a few tenths of km^2.sr, making the observatory sensitive to fluxes as low as a few tau neutrinos per km^2.sr.year. In the hypothesis of nu_mu <-->nu_tau oscillations with full mixing, this sensitivity allows to probe the GZK cutoff as well as to provide model independent constraints on the mechanisms of production of ultra high energy cosmic rays.']",['2001-04-30'] +153,['eng'],"['Benabed, K', 'Bernardeau, F']",['Testing Quintessence models with large-scale structure growth'],['Astrophysics and Astronomy'],"['quintessence', 'fluctuation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'matter, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104371'],['We explore the possibility of putting constraints on quintessence models with large-scale structure observations. In particular we compute the linear and second order growth rate of the fluctuations in different flavors of quintessence scenarios. We show that effective models of quintessence (e.g. with a constant equation of state) do not account of the results found in more realistic scenarios. The impact of these results on observational quantities such as the shape of the non-linear power spectrum in weak lensing surveys or the skewness of the convergence field are investigated. It appears that the observational signature of quintessence models are specific and rather large. They clearly cannot be mistaken with a change of (\\Omega_{0}).'],['2001-04-24'] +154,['eng'],"['Ramos, R O']",['Fine-Tuning Solution for Hybrid Inflation in Dissipative Chaotic Dynamics'],['Astrophysics and Astronomy'],"['inflationary universe, hybrid', 'chaos', 'phase space', 'dissipation', 'dimension, fractals', 'boundary condition', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104379'],"['We study the presence of chaotic behavior in phase space in the pre-inflationary stage of hybrid inflation models. This is closely related to the problem of initial conditions associated to these inflationary type of models. We then show how an expected dissipative dynamics of fields right prior to the onset of inflation can solve or easy considerable the problem of initial conditions, driving naturally the system towards inflation. The chaotic behavior of the corresponding dynamical system is studied by the computation of the fractal dimension of the boundary, in phase space, separating inflationary to non-inflationary trajectories. The fractal dimension for this boundary is determined as a function of the fields dissipation.']",['2001-04-24'] +155,['eng'],"['Bean, R', 'Hansen, S H', 'Melchiorri, A']",['Early-universe constraints on a Primordial Scaling Field'],['Astrophysics and Astronomy'],"['astrophysics, expansion', 'expansion, acceleration', 'dark energy', 'energy, density', 'potential', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, fundamental constant', 'astrophysics, missing-mass', 'light nucleus, production', 'finite temperature', 'quintessence', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104162'],"[""In the past years 'quintessence' models have been considered which can produce the accelerated expansion in the universe suggested by astronomical observations. One of the key differences between quintessence and a cosmological constant is that the energy density in quintessence Omega_Q could be a significant fraction of the overall energy even in the early universe, while the cosmological constant will be relevant only at late times. We use standard Big Bang Nucleosynthesis and the observed abundances of primordial nuclides to put constraints on Omega_Q at temperatures near T = 1Mev. We point out that current experimental data does not support the presence of such a field, providing the strong constraint Omega_Q(MeV) < 0.045 at 2-sigma C.L. and strengthening previous results. We also consider the effect a scaling field has on CMB anisotropies providing the CMB constraint Omega_Q < 0.62 at 2-sigma C.L. in the radiation dominated epoch.""]",['2001-04-11'] +156,['eng'],"['Gaisser, T K']",['Semi-analytic approximations for production of atmospheric muons and neutrinos'],['Astrophysics and Astronomy'],"['muon, cosmic radiation', 'neutrino/mu, cosmic radiation', 'cosmic radiation, flux', 'approximation', 'nucleon, cosmic radiation', 'cosmic radiation, primary', 'pi, production', 'K, production', 'cosmic radiation, energy spectrum', 'cross section, energy dependence', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104327'],['Simple approximations for fluxes of atmospheric muons and muon neutrinos are developed which display explicitly how the fluxes depend on primary cosmic ray energy and on features of pion production. For energies of approximately 10 GeV and above the results are sufficiently accurate to calculate response functions and to use for estimates of systematic uncertainties.'],['2001-04-20'] +157,['eng'],"['Giovannini, M']",['On the variation of the gauge couplings during inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'gauge field theory, abelian', 'coupling, gauge', 'magnetic field, production', 'magnetic field, fluctuation', 'fluctuation, correlation function', 'space-time, de Sitter', 'field theory, scalar', 'massive', 'model, hydrodynamical']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104290'],"['It is shown that the evolution of the (Abelian) gauge coupling during an inflationary phase of de Sitter type drives the growth of the two-point function of the magnetic inhomogeneities. After examining the constraints on the variation of the gauge coupling arising in a standard model of inflationary and post-inflationary evolution, magnetohydrodynamical equations are generalized to the case of time evolving gauge coupling. It is argued that large scale magnetic fields can be copiously generated. Other possible implications of the model are outlined.']",['2001-04-18'] +158,['eng'],"['Isola, C', 'Lemoine, M', 'Sigl, G']",['Centaurus A as the Source of ultra-high energy cosmic rays?'],['Astrophysics and Astronomy'],"['nucleon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, angular distribution', 'magnetic field, galaxy', 'gas', 'photon, emission', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104289'],"[""We present numerical simulations for energy spectra and angular distributions of nucleons above 10^{19} eV injected by the radio-galaxy Centaurus A at a distance 3.4 Mpc and propagating in extra-galactic magnetic fields in the sub-micro Gauss range. We show that field strengths B~0.3 micro Gauss, as proposed by Farrar and Piran, cannot provide sufficient angular deflection to explain the observational data. A magnetic field of intensity ~1 micro Gauss could reproduce the observed large-scale isotropy and could marginally explain the observed energy spectrum. However, it would not readily account for the E=320 plusminus 93 EeV Fly's Eye event that was detected at an angle 136 degrees away from Cen-A. Such a strong magnetic field also saturates observational upper limits from Faraday rotation observations and X-ray bremsstrahlung emission from the ambient gas (assuming equipartition of energy). This scenario may already be tested by improving magnetic field limits with existing instruments. We also show that high energy cosmic ray experiments now under construction will be able to detect the level of anisotropy predicted by this scenario. We conclude that for magnetic fields B~0.1-0.5 micro Gauss, considered as more reasonable for the local Supercluster environment, in all likelihood at least a few sources within ~10 Mpc from the Earth should contribute to the observed ultra high energy cosmic ray flux.""]",['2001-04-18'] +159,['eng'],"['Schatz, G']",['A Search for Fine Structure of the Knee in EAS Size Spectra'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'showers, air', 'parametrization', 'cosmic radiation, flux', 'cosmic radiation, primary', 'iron', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104282'],"['Twenty-eight size spectra of extensive air showersfrom 7 different experiments are analysed consistently. They are fitted by adjusting either 4 or 5 parameters: knee position, power law exponents above and below the knee, overall intensity and, in addition, a parameter describing the smoothness of the bend. The residuals are then normalized to the same knee position and averaged. When 5 parameters are employed no systematic deviation from a single smooth knee is apparent at the 1% level up to a factor of 4 above the knee. At larger shower sizes a moderately significant deviation can be seen whose shape and position are compatible with a second knee caused by iron group nuclei.']",['2001-04-18'] +160,['eng'],"['Hogan, C J', 'Bender, P L']",['Estimating Stochastic Gravitational Wave Backgrounds with Sagnac Calibration'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'background, stochastic', 'laser, interference', 'calibration', 'energy, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104266'],"['Armstrong et al. have recently presented new ways of combining signals to precisely cancel laser frequency noise in spaceborne interferometric gravitational wave detectors such as LISA. One of these combinations, the symmetrized Sagnac observable, is much less sensitive to external signals at low frequencies than other combinations, and thus can be used to determine the instrumental noise level. We note here that this calibration of the instrumental noise permits smoothed versions of the power spectral density of stochastic gravitational wave backgrounds to be determined with considerably higher accuracy than earlier estimates, at frequencies where one type of noise strongly dominates and is not substantially correlated between the six main signals generated by the antenna. We illustrate this technique by analyzing simple estimators of gravitational wave background power, and show that the instrumental sensitivity to broad-band backgrounds at some frequencies can be improved by more than an order of magnitude over the standard method, comparable to that which would be achieved by cross-correlating two separate antennas. The applications of this approach to studies of astrophysical gravitational wave backgrounds generated after recombination and to searches for a possible primordial background are discussed.']",['2001-04-17'] +161,['eng'],"['Huang, M H A']",['Physics Results From Alpha Magnetic Spectrometer 1998 Shuttle Flight'],['Astrophysics and Astronomy'],"['talk, Taipei 2000/10/18', 'antimatter, search for', 'helium, antinucleus', 'upper limit', 'p, cosmic radiation', 'positron, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'geophysics, magnetic field', 'magnetic field, confinement', 'magnetic spectrometer, satellite', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104229'],"['The Alpha Magnetic Spectrometer (AMS) is a particle detector designed to detect antimatter. During the 10-day test flight on the space shuttle in June 1998, AMS detected $10^8$ events. Upon analysis, no antimatter was found and the antimatter limit was reduced to $1.1\\times10^{-6}$. The proton spectrum shows some differences with the cosmic ray flux used in atmospheric neutrino simulation. A large amount of protons, positrons, and electrons were found below the geomagnetic rigidity cutoff. The energy of these particles are as high as several GeV, one order of magnitude higher than any previously measured energy in radiation belts. These particles also exhibit many interesting features. This paper reviews the results in the four published papers of the AMS collaboration and provides explanation for some features of the albedo particles.']",['2001-04-16'] +162,['eng'],"['Juillard, A', 'Benoit, A', 'Bergé, L', 'Bonnevaux, A', 'Bouvier, R', 'Broniatowski, A', 'Chambon, B', 'Chapellier, M', 'Chardin, G', 'Charvin, P', 'Cluzel, P', 'De Jésus, M', 'Stefano, P D', 'Drain, D', 'Dumoulin, L', 'Gascon, J', 'Gerbier, G', 'Goldbach, C', 'Goyot, M', 'Gros, M H', 'Hadjout, J P', 'de Lesquen, A', 'Loidl, M', 'Loiseau, D', 'Mallet, J', 'Marnieros, S', 'Martineau, O', 'Mirabolfathi, N', 'Mosca, L', 'Navick, X F', 'Nollez, G', 'Pari, P', 'Pastor, C', 'Simon, E', 'Stern, M', 'Vagneron, L']",['Dark Matter Search in the EDELWEISS experiment'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, search for', 'WIMP nucleus, elastic scattering', 'electron, recoil', 'nucleus, recoil', 'recoil, energy spectrum', 'cross section', 'semiconductor detector, germanium', 'bolometer, experimental results']","['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104192', 'http://documents.cern.ch/archive/electronic/other/uploader/MORIOND/dms-t6.ps']","['The EDELWEISS Dark Matter Search uses low-temperature Ge detectors with heat and ionisation read-out to identify nuclear recoils induced by elastic collisions with WIMPs from the galactic halo. Preliminary results obtained with 320g bolometers are described. After a few weeks of data taking, data accumulated with one of these detectors already allow to reach the upper part of the DAMA region. Prospects for the present run and the second stage of the experiment, EDELWEISS-II, using an innovative reversed cryostat allowing data taking with 100 detectors, are briefly described.']",['2001-04-12'] +163,['eng'],"['Hofmann, S', 'Schwarz, Dominik J', 'Stöcker, H']",['Damping scales of neutralino cold dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'density, fluctuation', 'spectra, fluctuation', 'neutralino, decoupling', 'neutralino, scattering', 'temperature', 'perturbation, acoustic', 'energy loss', 'neutralino, mass', 'sfermion, mass', 'model, fluid', 'transport theory', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104173'],"['The lightest supersymmetric particle, most likely the neutralino, might account for a large fraction of dark matter in the Universe. We show that the primordial spectrum of density fluctuations in neutralino cold dark matter (CDM) has a sharp cut-off due to two damping mechanisms: collisional damping during the kinetic decoupling of the neutralinos at about 30 MeV (for typical neutralino and sfermion masses) and free streaming after last scattering of neutralinos. The last scattering temperature is lower than the kinetic decoupling temperature by one order of magnitude. The cut-off in the primordial spectrum defines a minimal mass for CDM objects in hierarchical structure formation. For typical neutralino and sfermion masses the first gravitationally bound neutralino clouds have to have masses above $10^{-7}$ solar masses.']",['2001-04-11'] +164,['eng'],"['Biesiada, M']",['Cosmic Equation of State and Advanced LIGO Type Gravity Wave Experiments'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'laser, interference', 'quintessence', 'astrophysics, model', 'matter, density', 'energy, density', 'cosmic radiation, background', 'redshift', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104166'],"[""Future generation of interferometric gravitational wave detectors is hoped to provide accurate measurements of the final stages of binary inspirals. The sources probed by such experiments are of extragalactic origin and the observed chirp mass is the intrinsic chirp mass multiplied by $(1+z)$ where $z$ is the redshift of the source. Moreover the luminosity distance is a direct observable is such experiments. This creates the possibility to establish a new kind of cosmological tests, supplementary to more standard ones. Recent observations of distant type Ia supernovae light-curves suggest that the expansion of the universe has recently begun to accelerate. A popular explanation of present accelerating expansion of the universe is to assume that some part $\\Omega_Q$ of the matter-energy density is in the form of dark component called ``the quintessence'' with the equation of state $p_Q = w \\rho_Q$ with $w \\geq -1.$ In this paper we consider the predictions concerning observations of binary inspirals in future LIGO type interferometric experiments assuming a ``quintessence cosmology''. In particular we compute the expected redshift distributions of observed events in the a priori admissible range of parameters describing the equation of state for the quintessence. We find that this distribution has a robust dependence on the cosmic equation of state.""]",['2001-04-11'] +165,['eng'],"['Mannheim, K']",['Bounds on the neutrino flux from cosmic sources of relativistic particles'],['Astrophysics and Astronomy'],"['neutrino, particle source', 'neutrino, cosmic radiation', 'neutrino, flux', 'black hole', 'mass, accretion', 'photon, cosmic radiation', 'p, acceleration', 'galaxy, cluster', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104165'],"['In order to facilitate the identification of possible new physics signatures in neutrino telescopes, such as neutrinos from the annihilation of neutralinos or decaying relics, it is essential to gain full control over the astrophysical inventory of neutrino sources in the Universe. The total available accretion power, the extragalactic gamma ray background, and the cosmic ray proton intensity can be used to constrain astrophysical models of neutrino production in extragalactic sources. The resulting upper limit on the extragalactic muon neutrino intensity from cosmic particle accelerators combined with a reasonable minimum intensity of neutrinos due to cosmic rays stored in clusters of galaxies demark a zone of opportunity for neutrino astronomy over a broad range of energies between 100 MeV and 1 EeV. Discovery of this neutrino background would open a new era for astronomy and provide the first un-obscured view to the early Universe.']",['2001-04-11'] +166,['eng'],"['Rahman, M A', 'Bhat, P N', 'Acharya, B S', 'Chitnis, V R', 'Majumdar, P', 'Vishwanath, P R']",['Gamma Ray and Hadron generated \\v{C}erenkov Photon Spectra at Various Observation Altitudes'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'hadron, cosmic radiation', 'radiation, Cherenkov', 'showers, spatial distribution', 'longitudinal', 'photon, energy spectrum', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104143'],"[""We study the propagation of Cerenkov photons generated by Very High Energy gamma-rays and hadrons in the atmosphere. The photon production height distributions are estimated from semi-empirical methods and compared with those derived by standard simulation techniques. Incident spectra at various observation altitudes are then derived after applying wavelength dependent corrections due to photon attenuation in the atmosphere during the propagation of photons from the height of production to the height of observation. These are generated both for gamma- and hadron primaries of various energies. The derived production height distributions agree very well with those generated by the simulation package `CORSIKA' at all energies and for both gamma-$ray and proton primaries. The incident photon spectra are found to be both altitude dependent and primary energy dependent. The peak of the incident spectrum shifts towards the shorter wavelength with increasing altitude of observation for a given primary. Also the peak of the photon spectrum shifts towards the shorter wavelength with increasing energy of the primary at given altitude. The fraction of the UV component in the incident Cerenkov spectrum is estimated both for gamma-ray and hadronic primaries at various observation altitudes and energies. Hadron generated Cerenkov spectra are marginally richer in UV light and the difference increases slightly at higher altitudes. The fraction of the UV to the visible light in the Cerenkov spectrum could be a useful parameter to separate gamma-rays from cosmic ray background only if one can measure this fraction very accurately.""]",['2001-04-10'] +167,['eng'],"['Zdunik, J L', 'Haensel, P', 'Gourgoulhon, E']",['The crust of rotating strange quark stars'],['Astrophysics and Astronomy'],"['quark, matter', 'rotational', 'matter, strangeness', 'relativity theory, general', 'bag model', 'n, matter', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104116'],"['Calculations of the properties of rotating strange stars with crusts are performed within the framework of general relativity. We employ an equation of state (EOS) of strange quark matter based on the MIT Bag Model with massive strange quarks and lowest order QCD interactions. The crust is described by the BPS equation of state. A significant increase of the stellar radius is found close to the Keplerian (mass-shedding limit) configuration. This leads to the disappearance of the gap between the stellar surface and the innermost stable circular orbit (ISCO) at very high rotation rates, for a rather broad range of stellar masses. The Keplerian configuration for the strange star with crust corresponds to values of J, T/W which are about 20% smaller than in the case of bare strange stars. Because the Keplerian configuration is achieved due to the increase of the stellar oblateness, the Keplerian frequency (of the rotation) remains almost unaltered. The lack of the gap close to the Keplerian rotation could imply a more stringent limit on the frequency of the ISCO, if the existence of such a gap is supported by observations, as in the source 4U 1820-30 with the upper QPO frequency 1.07 kHz. During the spin-down of a magnetized strange quark star with crust, the crust matter is absorbed in the equatorial region by the strange matter core. The deconfinement of absorbed crust matter is a strongly exothermic process, which would influence the cooling curve of this compact object.']",['2001-04-09'] +168,['eng'],"['Baryshev, Yu V', 'Paturel, G']",['Statistics of the detection rates for tensor and scalar gravitational waves from the local galaxy universe'],['Astrophysics and Astronomy'],"['gravitational radiation, scalar', 'gravitational radiation, tensor', 'statistical analysis', 'supernova', 'galaxy, cluster', 'amplitude analysis, time dependence', 'gravitational radiation, energy', 'gravitational radiation, counters and detectors', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104115'],"['We use data on the local 3-dimensional galaxy distribution for studying the statistics of the detection rates of gravitational waves (GW) coming from supernova explosions. We consider both tensor and scalar gravitational waves which are possible in a wide range of relativistic and quantum gravity theories. We show that statistics of GW events as a function of sidereal time can be used for distinction between scalar and tensor gravitational waves because of the anisotropy of spatial galaxy distribution. For calculation of the expected amplitudes of GW signals we use the values of the released GW energy, frequency and duration of GW pulse which are consistent with existing scenarios of SN core collapse. The amplitudes of the signals produced by Virgo and the Great Attractor clusters of galaxies is expressed as a function of the sidereal time for resonant bar detectors operating now (IGEC) and for forthcoming laser interferometric detectors (VIRGO).Then, we calculate the expected number of GW events as a function of sidereal time produced by all the galaxies within 100 Mpc. In the case of axisymmetric rotational core collapse which radiates a GW energy of $10^{-9}M_{\\odot}c^2$, only the closest explosions can be detected. However, in the case of nonaxisymmetric supernova explosion, due to such phenomena as centrifugal hangup, bar and lump formation, the GW radiation could be as strong as that from a coalescing neutron-star binary. For radiated GW energy higher than $10^{-6}M_{\\odot}c^2$ and sensitivity of detectors at the level $h \\approx 10^{-23}$ it is possible to detect Virgo cluster and Great Attractor, and hence to use the statistics of GW events for testing gravity theories.']",['2001-04-09'] +169,['eng'],"['Schulz, A E', 'White, M']",['The Tensor to Scalar Ratio of Phantom Dark Energy Models'],['Astrophysics and Astronomy'],"['dark energy', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'perturbation, scalar', 'perturbation, tensor', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104112'],"['We investigate the anisotropies in the cosmic microwave background in a class of models which possess a positive cosmic energy density but negative pressure, with a constant equation of state w = p/rho < -1. We calculate the temperature and polarization anisotropy spectra for both scalar and tensor perturbations by modifying the publicly available code CMBfast. For a constant initial curvature perturbation or tensor normalization, we have calculated the final anisotropy spectra as a function of the dark energy density and equation of state w and of the scalar and tensor spectral indices. This allows us to calculate the dependence of the tensor-to-scalar ratio on w in a model with phantom dark energy, which may be important for interpreting any future detection of long-wavelength gravitational waves.']",['2001-04-09'] +170,['eng'],"['Hogan, C J']",['Particle Annihilation in Cold Dark Matter Micropancakes'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'particle, annihilation', 'WIMP', 'photon, cosmic radiation', 'phase space', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104106'],"[""Cold primordial particle dark matter forms with a distribution in six-dimensional phase space closely approximating a three-dimensional sheet. Folds in the mapping of this sheet onto configuration space create ubiquitous sheetlike caustics (``micropancakes''). A typical WIMP dark matter halo has many micropancakes, each with a scale comparable to the halo itself, a width about $10^{-8}$ of the halo size and a typical maximum density up to about $10^4$ times the halo mean. It is demonstrated here that the total annihilation rate of dark matter particles is dominated by particles close to these micropancakes, so radiation is emitted predominantly from highly contorted two-dimensional surfaces rather than a filled volume. The total annihilation rate of particles is about a factor of 5 higher than predicted from N-body simulations, which cannot resolve these features. Micropancakes also produce sharp line discontinuities in the surface brightness of annihilation radiation.""]",['2001-04-06'] +171,['eng'],"['Hogan, C J']",['Brane World Astronomy'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'membrane model', 'unified field theory', 'space-time, higher-dimensional', 'astrophysics, model', 'gravitational radiation, counters and detectors']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104105'],"[""Unified theories suggest that space is intrinsically 10 dimensional, even though everyday phenomena seem to take place in only 3 large dimensions. In ``Brane World'' models, matter and radiation are localized to a ``brane'' which has a thickness less than 1/TeV in all but the usual three dimensions, while gravity propagates in additional dimensions, some of which may extend as far as submillimeter scales. A brief review is presented of some of these models and their astrophysical phenomenology. One distinctive possibility is a gravitational wave background originating in the mesoscopic early universe, at temperatures above about 1 TeV and on scales smaller than a millimeter, during the formation of our 3-dimensional brane within a 10-dimensional space.""]",['2001-04-06'] +172,['eng'],"['Zhu, Z H']",['Gravitational lensing statistical properties in general FRW cosmologies with dark energy component(s)'],['Astrophysics and Astronomy'],"['Friedman model', 'space-time, Robertson-Walker', 'dark energy', 'gravitation, lens', 'statistics', 'kinematics']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0107233'],"['Various astronomical observations have been consistently making a strong case for the existence of a component of dark energy with negative pressure in the universe. It is now necessary to take the dark energy component(s) into account in gravitational lensing statistics and other cosmological tests. By using the comoving distance we derive analytic but simple expressions for the optical depth of multiple image, the expected value of image separation and the probability distribution of image separation caused by an assemble of singular isothermal spheres in general FRW cosmological models with dark energy component(s). We also present the kinematical and dynamical properties of these kinds of cosmological models and calculate the age of the universe and the distance measures, which are often used in classical cosmological tests. In some cases we are able to give formulae that are simpler than those found elsewhere in the literature, which could make the cosmological tests for dark energy component(s) more convenient.']",['2001-07-16'] +173,['eng'],"['Litwin, C', 'Rosner, R A']",['On a mechanism of highest-energy cosmic ray acceleration'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'cosmic radiation, acceleration', 'electric field, polarization', 'plasma', 'n, matter', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'magnetic field, confinement', 'energy dependence']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104093'],['A recently proposed mechanism of acceleration of highest energy cosmic rays by polarization electric fields arising in plasmoids injected into neutron star magnetospheres is discussed.'],['2001-04-05'] +174,['eng'],"['Litwin, C', 'Rosner, R A']",['Plasmoid impacts on neutron stars and highest energy cosmic rays'],['Astrophysics and Astronomy'],"['n, matter', 'particle, acceleration', 'electric field, polarization', 'plasma', 'magnetic field', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104090'],"['Particle acceleration by electrostatic polarization fields that arise in plasmas streaming across magnetic fields is discussed as a possible acceleration mechanism of highest-energy cosmic rays. Specifically, plasmoids arising in planetoid impacts onto neutron star magnetospheres are considered. We find that such impacts at plausible rates may account for the observed flux and energy spectrum of the highest energy cosmic rays.']",['2001-04-05'] +175,['eng'],"['Valle, José W F']",['Status of Neutrino Oscillations'],['Astrophysics and Astronomy'],"['neutrino, oscillation', 'neutrino, solar', 'neutrino, cosmic radiation', 'flavor, 3', 'neutrino, mixing angle', 'neutrino, flux', 'angular distribution', 'data analysis method', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104085'],"['Solar and atmospheric neutrino data require physics beyond the Standard Model of particle physics. The simplest, most generic, but not yet unique, interpretation of the data is in terms of neutrino oscillations. I summarize the results of the latest three-neutrino oscillation global fit of the data, in particular the bounds on the angle $\\theta_{13}$ probed in reactor experiments. Even though not implied by the data, bi-maximal neutrino mixing emerges as an attractive possibility either in hierarchical or quasi-degenerate neutrino scenarios.']",['2001-04-05'] +176,['eng'],"['Thoma, M H']",['Quantum Field Theoretic Description of Matter in the Universe'],['Astrophysics and Astronomy'],"['talk, Bern 2001/03/19', 'supernova', 'n, matter', 'plasma', 'field theory, finite temperature', 'density, finite', 'scattering, neutrino plasma', 'neutrino antineutrino, annihilation', 'quark, matter', 'matter, strangeness', 'cosmic radiation, background', 'photon photon, scattering', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104078'],"['Quantum field theory at finite temperature and density can be used for describing the physics of relativistic plasmas. Such systems are frequently encountered in astrophysical situations, such as the early Universe, Supernova explosions, and the interior of neutron stars. After a brief introduction to thermal field theory the usefulness of this approach in astrophysics will be exemplified in three different cases. First the interaction of neutrinos within a Supernova plasma will be discussed. Then the possible presence of quark matter in a neutron star core and finally the interaction of light with the Cosmic Microwave Background will be considered.']",['2001-04-05'] +177,['eng'],"['Totani, T', 'Inoue, S']",['Preheating in the Universe Suppressing High Energy Gamma-rays from Structure Formation'],['Astrophysics and Astronomy'],"['inflationary universe', 'electron, acceleration', 'photon, production', 'photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, flux', 'cosmic radiation, cluster', 'cosmic radiation, energy spectrum', 'preheating', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104072'],"['Structure formation in the universe can produce high energy gamma-rays from shock-accelerated electrons, and this process may be the origin of the extragalactic gamma-ray background (EGRB) as well as a part of the unidentified sources detected by EGRET in the GeV band, if about 5% of the kinetic energy of the shock is going into electron acceleration. However, we point out that the production of gamma-rays may be severely suppressed if the collapsing matter has been preheated by external entropy sources at the time of gravitational collapse, as can be inferred from the luminosity-temperature (LT) relation of galaxy clusters and groups. We also make a rough estimate of this effect by a simple model, showing that the EGRB flux may be suppressed by a factor of about 30. Hence structure formation is difficult to be the dominant origin of EGRB if preheating is actually responsible for the observed anomary in the LT relation. The detectable number of gamma-ray clusters is also reduced, but about 5-10 forming clusters should still be detectable by EGRET all sky, and this number is similar to that of the steady and high-latitude unidentified sources in the EGRET catalog. The future GLAST mission should detect 10^2-10^3 gamma-ray clusters of galaxies even if the intergalactic medium has been preheated.']",['2001-04-05'] +178,['eng'],"['Starobinsky, A A']",['Robustness of the inflationary perturbation spectrum to trans-Planckian physics'],['Astrophysics and Astronomy'],"['inflationary universe', 'perturbation, tensor', 'perturbation, scalar', 'spectra, perturbation', 'vacuum state, fluctuation', 'energy, density', 'particle, production']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104043'],"['It is investigated if predictions of the inflationary scenario regarding spectra of scalar and tensor perturbations generated from quantum vacuum fluctuations are robust with respect to a modification of the dispersion law for frequencies beyond the Planck scale. For a large class of such modifications of special and general relativity, for which the WKB condition is not violated at super-high frequencies, the predictions remain unchanged. The opposite possibility is excluded by the absence of large amount of created particles due to the present Universe expansion. Creation of particles in the quantum state minimizing the energy density of a given mode at the moment of Planck boundary crossing is prohibited by the latter argument, too (contrary to creation in the adiabatic vacuum state which is very small now).']",['2001-04-04'] +179,['eng'],"['Goliath, M', 'Amanullah, R', 'Astier, P', 'Goobar, A', 'Pain, R']",['Supernovae and the Nature of the Dark Energy'],['Astrophysics and Astronomy'],"['supernova', 'dark energy', 'luminosity', 'mass, density', 'gravitation, lens', 'statistical analysis', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104009'],"[""The use of Type Ia supernovae as calibrated standard candles is one of the most powerful tools to study the expansion history of the universe and thereby its energy components. While the analysis of some ~50 supernovae at redshifts around z~0.5 have provided strong evidence for an energy component with negative pressure, ``dark energy'', more data is needed to enable an accurate estimate of the amount and nature of this energy. This might be accomplished by a dedicated space telescope, the SuperNova / Acceleration Probe (2000; SNAP), which aims at collecting a large number of supernovae with z<2. In this paper we assess the ability of the SNAP mission to determine various properties of the ``dark energy.'' To exemplify, we expect SNAP, if operated for three years to study Type Ia supernovae, to be able to determine the parameters in a linear equation of state w(z)=w0 + w1 z to within a statistical uncertainty of +-0.04 for w0 and +0.15,-0.17 for w1 assuming that the universe is known to be flat and an independent high precision (sigma_{Omega_m}=0.015) measurement of the mass density Omega_m, is used to constrain the fit. An additional improvement can be obtained if a large number of low-z, as well as high-z, supernovae are included in the sample.""]",['2001-04-03'] +180,['eng'],"['Huey, G', 'Lidsey, J E']","['Inflation, braneworlds and quintessence']",['Astrophysics and Astronomy'],"['inflationary universe', 'membrane model', 'quintessence', 'Randall-Sundrum model', 'perturbation, scalar', 'perturbation, tensor']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0104006'],"['Inflationary cosmology is developed in the second Randall-Sundrum braneworld scenario, where the accelerated expansion arises through potentials that are too steep to drive inflation in conventional cosmology. A relationship between the scalar and tensor perturbation spectra is derived that is independent of both the inflaton potential and the brane tension. It is found that a single field with an inverse power law potential can act as both the inflaton and the quintessence field for suitable values of the brane tension.']",['2001-04-03'] +181,['eng'],[],['The Cosmic-Ray antiproton flux between 3 and 49 GeV'],['Astrophysics and Astronomy'],"['anti-p, cosmic radiation', 'p, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'anti-p p, ratio', 'Cherenkov counter, ring imaging', 'magnetic spectrometer, satellite', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103513'],"['We report on a new measurement of the cosmic ray antiproton spectrum. The data were collected by the balloon-borne experiment CAPRICE98 which was flown on 28-29 May 1998 from Fort Sumner, New Mexico, USA. The experiment used the NMSU-WIZARD/CAPRICE98 balloon-borne magnet spectrometer equipped with a gas Ring Imaging Cherenkov (RICH) detector, a time-of-flight system, a tracking device consisting of drift chambers and a superconducting magnet and a silicon-tungsten calorimeter. The RICH detector was the first ever flown capable of identifying charge one particles at energies above 5 GeV. A total of 31 antiprotons with rigidities between 4 and 50 GV at the spectrometer were identified with small backgrounds from other particles. The absolute antiproton energy spectrum was determined in the kinetic energy region at the top of the atmosphere between 3.2 and 49.1 GeV. We found that the observed antiproton spectrum and the antiproton to proton ratio are consistent with a pure secondary origin. However, a primary component may not be excluded.']",['2001-04-02'] +182,['eng'],"['Hettlage, C', 'Mannheim, K']",['High Energy Neutrino Fluxes from Cosmic Accelerators'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2001/01/20', 'neutrino, cosmic radiation', 'neutrino, flux', 'photon, flux', 'neutrino/mu', 'neutrino, oscillation', 'blazar', 'Cherenkov counter, water', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103499'],"['We constrain high-energy neutrino fluxes with the observed cosmic ray and gamma ray fluxes, include flavor oscillations and propagation through Earth, and show that blazars could possibly be detected by cubic-kilometer neutrino telescopes.']",['2001-03-30'] +183,['eng'],"['Barrau, A']",['AMS'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2001/01/20', 'antimatter, cosmic radiation', 'electron, cosmic radiation', 'p, cosmic radiation', 'photon, cosmic radiation', 'astrophysics, missing-mass', 'magnetic spectrometer, satellite', 'magnetic spectrometer, superconducting']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103493'],"['The expected physics and astrophysics capabilities of the AMS experiment on board the International Space Station are briefly reviewed : high statistics study of cosmic rays in a wide range of energies, search for primordial antimatter, search for non-baryonic dark matter and, to some extent, gamma-ray astronomy.']",['2001-03-30'] +184,['eng'],"['Erlykin, A D', 'Wolfendale, A W']",['The Origin of the Knee in the Cosmic-Ray Energy Spectrum'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2001/01/20', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'showers, air', 'supernova', 'cosmic radiation, mass', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103477'],"[""A sudden steepening of the cosmic-ray energy spectrum (the knee) is observed at an energy of about 3 PeV (1 PeV = 10$^{15}$eV). The recent results on extensive air showers allow us to conclude that: a) the knee has an astrophysical origin; b) the 'sharpness' and the fine structure of the knee rule out 'Galactic Modulation' as the origin of the knee; c) most likely the knee is the result of the explosion of a single, recent, nearby supernova.""]",['2001-03-29'] +185,['eng'],"['Roxburgh, I W', 'Polnarev, A G', 'Giampieri, G', 'Vorontsov, S V']",['Response of a Spaceborn Gravitational Wave Antenna to Solar Oscillations'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'counters and detectors, satellite', 'radiation, laser', 'optics, interference', 'effect, solar', 'oscillation, solar']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103472'],"['We investigate the possibility of observing very small amplitude low frequency solar oscillations with the proposed laser interferometer space antenna LISA. For frequencies below $\\sim 2\\times 10^{-4}$ Hz the dominant contribution is from the near zone time dependent gravitational quadrupole moments associated with the normal modes of oscillation. For frequencies $\\nu$ above $\\sim 3\\times 10^{-4}$ Hz the dominant contribution is from gravitational radiation generated by the quadrupole oscillations which is larger than the Newtonian signal by a factor $\\sim (2 \\pi r \\nu/ c)^4$, where $r$ is the distance to the Sun, and $c$ is the velocity of light. The low order solar quadrupole pressure and gravity oscillation modes have not yet been detected above the solar background by helioseismic velocity and intensity measurements. Our estimates of the amplitudes needed to give a detectable signal on a LISA type space laser interferometer imply surface velocity amplitudes on the sun of the order of 1-10 mm/sec in the frequency range $1 - 5~10^{-4}$Hz. Such surface velocities are below the current sensitivity limits on helioseismic measurements. If modes exist with frequencies and amplitudes in this range they could be detected with a LISA type laser interferometer.']",['2001-03-29'] +186,['eng'],"['Hanhart, C']",['Constraints on high energy phenomena from low energy nuclear physics'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2001/01/20', 'supernova', 'neutrino, cosmic radiation', 'particle, exotic', 'nucleon, coupling', 'graviton', 'space-time, higher-dimensional', 'statistical analysis', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103470'],"['A procedure to derive bounds on coupling strengths of exotic particles to nucleons from the neutrino signal of supernovae is outlined. The analysis is based on a model independent calculation for the emissivities for the exotic, detailed simulation for the evolution of the early proto-neutron star as well as a Likelihood analysis. As an example we derive confidence levels for the upper bound of the size of gravity only extra dimensions.']",['2001-03-29'] +187,['eng'],"['Zimbe, J']",['A New Cosmological Model'],['Astrophysics and Astronomy'],"['astrophysics, model', 'matter, production', 'space-time, singularity', 'hydrogen, gas', 'galaxy', 'matter, density', 'thermodynamics']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103457'],"['It is only human nature to be reluctant to accept something new and different. This feeling is exacerbated given the success of the Big Bang model. However, there are cogent reasons for considering this new model. Some of the advantages of this new model over the existing Big Bang model are as follows: (1) It does not violate any known laws of physics. This contrasts with the Big Bang model where all known laws of physics break down in the consideration of the universe beginning as a singular point of infinite density. (2) The cause behind the initial explosion is provided in this new model. The Big Bang model does not explain what caused the initial explosion. (3) The homogenous nature of the universe is intrinsically explained in this new model. Whereas, the Big Bang model relies on an ""extraneous"" concept like inflation to explain the homogeneity of the universe. (4) This new model eliminates the mystery of why there is a preponderance of matter over anti-matter. These are some of the advantages of this new model. There are others. Given these qualitative advantages, this new model is worthy of serious consideration even though it is new and different.']",['2001-03-28'] +188,['eng'],"['Chen, X', 'Kamionkowski, M P', 'Zhang, X']",['Kinetic decoupling of neutralino dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutralino, elastic scattering', 'neutralino, decoupling', 'cross section']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103452'],"['After neutralinos cease annihilating in the early Universe, they may still scatter elastically from other particles in the primordial plasma. At some point in time, however, they will eventually stop scattering. We calculate the cross sections for neutralino elastic scattering from standard-model particles to determine the time at which this kinetic decoupling occurs. We show that kinetic decoupling occurs above a temperature $T\\sim$ MeV. Thereafter, neutralinos act as collisionless cold dark matter.']",['2001-03-28'] +189,['eng'],"['Chang, Z', 'Huang, X B']",['Matching the observed cosmological constant with vacuum energy density in AdS'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'energy, density', 'space-time, anti-de Sitter', 'field theory, scalar', 'mass spectrum, discrete', 'dimension, 5']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103437'],"['The question of why the observational cosmological constant is so small in comparison with the vacuum energy density in particle physics has become a celebrated puzzle for a long time. We calculate the vacuum energy density by taking into account of different massive scalar fields in AdS spacetime. It is found that the mass spectrum of a scalar field in AdS spacetime is discrete because of a natural boundary condition. After supposed a reasonable magnitude ($6.93\\times 10^{26}$ m) of the radius of AdS, we match well the observed cosmological constant with the energy density of vacuum.']",['2001-03-28'] +190,['eng'],"['Kohri, K']",['Primordial nucleosynthesis and hadronic decay of a massive particle with a relatively short lifetime'],['Astrophysics and Astronomy'],"['particle, massive', 'particle, hadronic decay', 'particle, lifetime', 'light nucleus, production', 'hadron, injection', 'electron positron, annihilation', 'jet, electroproduction', 'hadron, mass spectrum', 'hadron nucleon, interaction', 'cross section', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103411'],"['In this paper we consider the effects on big bang nucleosynthesis (BBN) of the hadronic decay of a long-lived massive particle. If high-energy hadrons are emitted near the BBN epoch ($t \\sim 10^{-2}$ -- $10^2 \\sec$), they extraordinarily inter-convert the background nucleons each other even after the freeze-out time of the neutron to proton ratio. Then, produced light element abundances are changed, and that may result in a significant discrepancy between standard BBN and observations. Especially on the theoretical side, now we can obtain a lot of experimental data of hadrons and simulate the hadronic decay process executing the numerical code of the hadron fragmentation even in the high energy region where we have no experimental data. Using the light element abundances computed in the hadron-injection scenario, we derive a constraint on properties of such a particle by comparing our theoretical results with observations.']",['2001-03-27'] +191,['eng'],"['Clem, J', 'Droege, W', 'Evenson, P A', 'Fischer, H', 'Green, G', 'Hüber, D', 'Kunow, H', 'Seckel, D']",['A Measurement of the Flux of Cosmic Ray Iron at 5 x 10^13 eV'],['Astrophysics and Astronomy'],"['iron, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, energy', 'Cherenkov counter, satellite', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103397'],"['We present results from the initial flight of our Balloon Air CHerenkov (BACH) payload. BACH detects air Cherenkov radiation from cosmic ray nuclei as coincident flashes in two optical modules. The flight (dubbed PDQ BACH) took place on April 22, 1998 from Ft. Sumner, New Mexico. During an exposure of 2.75 hours, with a typical threshold energy for iron nuclei of 2.2$\\times10^{13}$ eV, we observed several events cleanly identifiable as iron group nuclei. Analysis of the data yields a new flux measurement that is fully consistent with that reported by other investigations.']",['2001-03-26'] +192,['eng'],"['Petruk, O']",['A New Model for the Thermal X-ray Composites and the Neutral Pion Decay Gamma-Rays from Supernova Remnants'],['Astrophysics and Astronomy'],"['talk, Erice 2000/11/11', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'p, acceleration', 'p, cosmic radiation', 'p nucleon, interaction', 'pi0, hadroproduction', 'pi0, radiative decay', 'photon, production', 'luminosity', 'supernova', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103396'],"['Recent nonthermal X-ray and gamma-ray observations, attributed to electron emission processes, for the first time give an experimental confirmation that electrons are accelerated on SNR shocks up to the energy 10^{14} eV. We have no direct observational confirmations about proton acceleration by SNR. Different models of gamma-emission from SNRs predict different emission mechanisms as dominating. Only decays of neutral pion created in proton-nucleon interactions allow us to look inside the CR nuclear component acceleration processes. A new model for the thermal X-ray composites strongly suggest that thermal X-ray peak inside the radio shell of SNR tells us about entering of one part of SNR shock into a denser medium compared with other parts of the shell. This makes a TXCs promising sites for gamma-ray generation via neutral pion decays. Detailed consideration of SNR-cloud interaction allows to increase an expected proton induced gamma-ray flux from SNR at least on an order of magnitude, that allows to adjust the theoretical proton origin gamma-luminosities with observed fluxes at least for a few SNRs even for low density (n=10-100 cm^{-3}) cloud.']",['2001-03-26'] +193,['eng'],"['Bhowmick, S', 'Dey, J', 'Dey, M', 'Ray, S', 'Ray, R']",['Stability of realistic strange stars (RSS)'],['Astrophysics and Astronomy'],"['quark, matter', 'matter, strangeness', 'star, stability', 'bag model', 'pulsar']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103389'],"['Strange stars (SS) calculated from a realistic equation of state (EOS) are very stable, for example under fast rotation but have a soft surface, on which ripples may occur when radiation is emitted close to it. We suggest this as a natural explanation of the fluctuations observed in the intensity profile of X-ray pulsars. In contrast, SS based on EOS derived from the bag models (Bag SS) are less stable against fast rotation and do not have a hard surface and cannot explain these ripples. There are other important differences between Bag SS and the SS, based on a realistic EOS, which we call realistic strange stars (RSS).']",['2001-03-26'] +194,['eng'],"['Lee, W H', 'Nix, J', 'Kluzniak, W']",['Coalescence of a strange star with a black hole'],['Astrophysics and Astronomy'],"['talk, Alicante 2000/09/04', 'matter, strangeness', 'black hole', 'coalescence', 'binary', 'mass, accretion']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103380'],"['We present the first numerical results on the binary coalescence of a quark star with a black hole, obtained with a 3-D Newtonian smooth particle hydro (SPH) code. The star is initially represented by 17,000 particles modeling a self-gravitating fluid with the equation of state P= (rho - rho0)c**2/3, and the black hole by a point mass with an absorbing boundary at the Schwarzschild radius. As in similar calculations carried out for a stiff polytrope, the stellar core survives the initial episode of mass transfer, but here an accretion disk is clearly formed as well.']",['2001-03-23'] +195,['eng'],"['Zas, E']",['ZeV Air Showers'],['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'neutrino, cosmic radiation', 'muon, cosmic radiation', 'showers, air', 'showers, angular distribution', 'shower detector', 'Cherenkov counter, water', 'counters and detectors, fluorescence', 'proposed experiment', '>10**11 GeV']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103371'],"['In this article I briefly discuss the characteristics of the Auger observatories paying particular attention to the role of inclined showers, both in the search for high energy neutrino interactions deep in the atmosphere and as an alternative tool for the study of cosmic rays, particulartly their composition.']",['2001-03-23'] +196,['eng'],"['Zas, E']",['Astroparticle physics'],['Astrophysics and Astronomy'],"['talk, San Feliu de Guixols 2000/09/30', 'showers, air', 'photon, cosmic radiation', 'particle, acceleration', 'p, cosmic radiation', 'muon, cosmic radiation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103370'],"['In this article I review the main theoretical problems that are posed by the highest energy end of the observed cosmic ray spectrum, stressing the importance of establishing their composition in order to decide between proposed scenarios. I then discuss the possibilities that are opened by the detection of inclined showers with extensive air shower arrays. Recent progress in modelling magnetic deviations for these showers has allowed the analysis of inclined showers that were detected by the Haverah Park experiment. This analysis disfavours models that predict a large proportion of photons in the highest energy cosmic rays and open up new possibilities for future shower array detectors particularly those, like the Pierre Auger Observatory, using water Cherenkov detectors.']",['2001-03-23'] +197,['eng'],"['Alvarez-Muñiz, J', 'Zas, E']",['Calculations of radio pulses from High Energy Showers'],['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'cosmic radiation', 'showers, air', 'radiation, electromagnetic', 'radiation, Cherenkov', 'approximation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103369'],['In this article we review the progress made in understanding the main characteristics of coherent \\v{C}erenkov radiation induced by high energy showers in dense media. A specific code developed for this purpose is described because it took a significant part in this process. Subsequent approximations developed for the calculation of radio pulses from EeV showers are reviewed. Emphasis is given to the relation between the shower characteristics and different features of the corresponding radio emission.'],['2001-03-23'] +198,['eng'],"['Antoni, T', 'Apel, W D', 'Badea, F', 'Bekk, K', 'Bernlöhr, K', 'Blümer, H', 'Bollmann, E', 'Bozdog, H', 'Brancus, I M', 'Büttner, C', 'Chilingarian, A A', 'Daumiller, K', 'Doll, P', 'Engler, J', 'Fessler, F', 'Gils, H J', 'Glasstetter, R', 'Haeusler, R', 'Haungs, A', 'Heck, D', 'Holst, T', 'Hörandel, J R', 'Kampert, K H', 'Kempa, J', 'Klages, H O', 'Knapp, J', 'Kohler, K U', 'Maier, G', 'Mathes, H J', 'Mayer, H J', 'Milke, J', 'Müller, M', 'Oehlschläger, J', 'Petcu, M', 'Rebel, H', 'Risse, M', 'Roth, M', 'Schatz, G', 'Scholz, J', 'Sokhoyan, S H', 'Thouw, T J', 'Ulrich, H', 'Vulpescu, B', 'Weber, J H', 'Wentz, J', 'Wochele, J', 'Zabierowski, J', 'Zagromski, S']",['Myon Density Measurements with the KASCADE Central Detector'],['Astrophysics and Astronomy'],"['muon, cosmic radiation', 'showers, air', 'showers, spatial distribution', 'muon, density', 'muon, energy', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103363'],"['Frequency distributions of local muon densities in high-energy extensive air-showers (EAS) are presented as signature of the primary cosmic ray energy spectrum in the knee region. Together with the gross shower variables like shower core position, angle of incidence, and the shower sizes, the KASCADE experiment is able to measure local muon densities for two different muon energy thresholds. The spectra have been reconstructed for various core distances, as well as for particular subsamples, classified on the basis of the shower size ratio N_mu/N_e. The measured density spectra of the total sample exhibit clear kinks reflecting the knee of the primary energy spectrum. While relatively sharp changes of the slopes are observed in the spectrum of EAS with small values of the shower size ratio, no such feature is detected at EAS of large N_mu/N_e ratio in the energy range of 1--10 PeV. Comparing the spectra for various thresholds and core distances with detailed Monte Carlo simulations the validity of EAS simulations is discussed.']",['2001-03-23'] +199,['eng'],"['Usov, V V']",['Thermal emission from bare quark matter surfaces of hot strange stars'],['Astrophysics and Astronomy'],"['matter, strangeness', 'quark, matter', 'star, surface', 'energy, flux', 'photon, emission', 'electron, pair production', 'luminosity', 'temperature', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103361'],"['We consider the thermal emission of photons and electron-positron pairs from the bare quark surface of a hot strange star. The radiation of high-energy (> 20 MeV) equilibrium photons prevails at the surface temperature T_S > 5 x 10^{10} K, while below this temperature, 8 x 10^8 < T_S < 5 x 10^{10} K, emission of electron-positron pairs created by the Coulomb barrier at the quark surface dominates. The thermal luminosity of a hot strange star in both photons and pairs is estimated.']",['2001-03-23'] +200,['eng'],"['Wang, K', 'Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G']",['A survey of the northern sky for TeV point sources'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'cosmic radiation, flux', 'upper limit', 'shower detector, experimental results', '>1000 GeV']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103353'],['The first search for steady TeV point sources anywhere in the northern sky has been made with data from the Milagrito air-shower-particle detector. Over 3 x 10**9 events collected from 1997 February to 1998 May have been used in this study. No statistically significant excess above the background from the isotropic flux of cosmic rays was found for any direction of the sky with declination between -5 degrees and 71.7 degrees. Upper limits are derived for the photon flux above 1 TeV from any steady point source in the northern sky.'],['2001-03-22'] +201,['eng'],"['Cardenas, R', 'Martin, O', 'Quirós, I']",['Comments on the paper astro-ph/0103335 by C Rubano and P Scudellaro'],['Astrophysics and Astronomy'],"['astrophysics, model', 'quintessence', 'field theory, scalar', 'potential', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0112316'],['We briefly comment on a paper by Rubano and Scudellaro [astro-ph/0103335] where they found general exact solutions for two classes of exponential potentials in a scalar field model for quintessence. In that paper the authors were led to some interesting conclusions after a proper choice of the integration constants. By using dimensionless variables we show that the integration constants can be found explicitly without additional assumptions. In consequence we revise some results and conclusions in that paper.'],['2001-12-17'] +202,['eng'],"['Rubano, C', 'Scudellaro, P']",['On Some Exponential Potentials for a Cosmological Scalar Field as Quintessence'],['Astrophysics and Astronomy'],"['astrophysics, model', 'quintessence', 'field theory, scalar', 'potential', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103335'],"['We present general exact solutions for two classes of exponential potentials in scalar field models for quintessence. The coupling is minimal and we consider only dust and scalar field. To some extent, it is possible to reproduce experimental results from supernovae.']",['2001-03-22'] +203,['eng'],"['Virtue, C J']",['SNO and Supernovae'],['Astrophysics and Astronomy'],"['talk, Otranto 2000/09/09', 'supernova', 'neutrino, cosmic radiation', 'neutrino, luminosity', 'neutrino, energy', 'time dependence', 'cross section, energy dependence', 'neutrino, particle identification', 'Cherenkov counter, water', 'deep underground detector, Sudbury', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103324'],"['The Sudbury Neutrino Observatory (SNO) has unique capabilities as a supernova detector. In the event of a galactic supernova there are opportunities, with the data that SNO would collect, to constrain certain intrinsic neutrino properties significantly, to test details of the various models of supernova dynamics, and to provide prompt notification to the astronomical community through the Supernova Early Warning System (SNEWS). This paper consists of a discussion of these opportunities illustrated by some preliminary Monte Carlo results.']",['2001-03-21'] +204,['eng'],"['González, J A', 'Quevedo, H', 'Salgado, M', 'Sudarsky, D']",['Local Constraints on the Oscillating G Model'],['Astrophysics and Astronomy'],"['Brans-Dicke model', 'gravitation, fundamental constant', 'time variation', 'constraint, local', 'astrophysics, model', 'field theory, scalar', 'massive', 'gravitation, coupling', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103314'],"['We analyze the observational constraints on the effective Brans-Dicke parameter and on the temporal variation of the effective gravitational constant within the context of the oscillating G model, a cosmological model based on a massive scalar field non-minimally coupled to gravity. We show that these local constraints cannot be satisfied simultaneously once the values of the free parameters entering the model become fixed by the global attributes of our Universe. In particular, we show that the lower observational bound for the effective Brans-Dicke parameter and the upper bound of the variation of the effective gravitational constant lead to a specific value of the oscillation amplitude which lies well below the value required to explain the periodicity of 128 Mpc h^{-1} in the galaxy distribution observed in the pencil beam surveys.']",['2001-03-21'] +205,['eng'],"['Leinson, L B', 'Pérez, A']",['Neutrino-pair radiation form neutron star crusts'],['Astrophysics and Astronomy'],"['n, matter', 'energy loss', 'neutrino, pair production', 'collective phenomena', 'electron, plasma', 'plasma, decay', 'bremsstrahlung', 'optical theorem', 'charged current, correlation function', 'polarization, tensor', 'fluctuation, dissipation', 'finite temperature', 'potential, chemical', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103309'],"['We present a method to calculate $\\nu \\bar{\\nu}$ energy losses from neutron star crusts, which automatically takes into account for collective effects, and allows to calculate the total emissivity without a separate consideration of particular processes. We show that the formula we obtain describe the known results for the emissivity due to plasmon decay and Bremsstrahlung from degenerate electrons, when one of this processes dominates. In the case of low temperatures, our formula gives a suppression of the electron vector weak-current contribution to $\\nu \\bar{\\nu}$ Bremsstrahlung, due to the collective effects discussed in this paper.']",['2001-03-21'] +206,['eng'],"['Seckel, D']",['In ice radio detection of GZK neutrinos'],['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'GZK effect', 'showers, air', 'radiation, Cherenkov', 'cosmic radiation, measurement', 'cosmic radiation, flux', 'data analysis method', 'Cherenkov counter, optical', 'proposed experiment', 'counters and detectors, proposed', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103300'],"['Models for the source and propagation of cosmic rays are stressed by observations of cosmic rays with energies $E>10^{20}$ eV. A key discriminant between different models may be complementary observations of neutrinos with energies $E>10^{18}$ eV. Independent of the source of the cosmic rays, neutrinos are produced during propagation via the GZK mechanism. Event rates for GZK neutrinos are expected to be in the range of $0.01-0.1$ per km$^3$ yr, suggesting a detector mass in excess of 1 Eg. Detection of radio cherenkov emission from showers produced in Antarctic ice may be an economical way to instrument such a large mass. It is suggested that a 100 km$^2$ array of antennas centered on Icecube may allow confirmation of the radio technique and also increase the science achievable with Icecube by providing vertex information for events with throughgoing muons.']",['2001-03-20'] +207,['eng'],"['Mészáros, P', 'Waxman, E']",['TeV Neutrinos from Bursting and Choked Fireballs'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, particle source', 'matter, massive', 'fireball, jet', 'gamma ray burst', 'p, acceleration', 'p, shock waves', 'photon p, interaction', 'pi, photoproduction', 'threshold, energy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103275'],"['Core collapse of massive stars resulting in a relativistic fireball jet which breaks through the stellar envelope is a widely discussed scenario for gamma-ray burst production. For very extended or slow rotating stars, the fireball may be unable to break through the envelope. Both penetrating and choked fireballs will produce, by photo-meson interactions of accelerated protons, a burst of $\\gtrsim$ 5 TeV neutrinos while propagating in the envelope. The predicted flux, from both penetrating and chocked fireballs, should be easily detectable by planned cubic kilometer neutrino telescopes.']",['2001-03-20'] +208,['eng'],"['Bugaev, E V', 'Konishchev, K V']",['Extragalactic neutrino background from PBHs evaporation'],['Astrophysics and Astronomy'],"['astrophysics, model', 'black hole, radiation', 'black hole, mass spectrum', 'neutrino/e, energy spectrum', 'neutrino/e, flux', 'neutrino/e, background', 'density, fluctuation', 'neutrino, absorption', 'neutrino, diffusion', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'amplitude analysis', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103265'],['We calculated the energy spectra and the fluxes of electron neutrinos in extragalactic space emitted in the process of the evaporation of primordial black holes (PBHs) in the early universe. It was assumed that PBHs are formed by a blue power-law spectrum of primordial density fluctuations. In the calculations of neutrino spectra the spectral index of density fluctuations and the reheating temperature were used as free parameters. The absorption of neutrinos during propagation in the space was taken into account. We obtained the bounds on the spectral index assuming validity of the standard picture of gravitational collapse and using the available data of several experiments with atmospheric and solar neutrinos. The comparison of our results with the previous constraints (which had been obtained using diffuse photon background data) shows that such bounds are quite sensitive to an assumed form of the initial PBH mass function.'],['2001-03-19'] +209,['eng'],"['Hwang, J', 'Noh, H']",['Cosmological Perturbations with Multiple Fluids and Fields'],['Astrophysics and Astronomy'],"['space-time, perturbation', 'fluid, multiple', 'relativity theory, general', 'perturbation, adiabatic', 'field theory, scalar', 'field equations', 'inflationary universe', 'quintessence', 'density, perturbation', 'invariance, gauge', 'scaling']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103244'],"['We consider the evolution of perturbed cosmological spacetime with multiple fluid and field system in Einstein gravity. Equations are presented in gauge-ready forms, and are presented using the adiabatic and isocurvature perturbation variables. We present equations in the general background with $K$ and $\\Lambda$. We also clarify the conditions for conserved adiabatic and isocurvature perturbations in the large-scale limit. One interesting conclusion is that, for ideal fluid system, although the isocurvature modes can seed the adiabatic mode in the large-scale limit, the isocurvature modes decouple from the adiabatic one which is not the case for the field system. Useful sets of equations readily applicable to the quintessence models and the warm inflation scenario can be found in this work. An application to the scaling regime with an exponential field potential is made in the Appendix.']",['2001-03-16'] +210,['eng'],"['Kempf, A', 'Niemeyer, J C']",['Perturbation spectrum in inflation with cutoff'],['Astrophysics and Astronomy'],"['inflationary universe', 'spectra, perturbation', 'oscillator', 'approximation, adiabatic', 'scaling', 'dispersion relations', 'cosmic radiation, background', 'cosmic radiation, fluctuation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103225'],"['As a potentially accessible window to aspects of Planck scale physics it has been pointed out that the perturbation spectrum predicted by inflation may be sensitive to a natural ultraviolet cutoff. A fairly general classification of the possible short-distance cutoffs that one may encounter at the Planck scale has also recently been given. Indeed, various studies of quantum gravity and string theory point towards one of the types of cutoff in this classification. This cutoff has been implemented into the standard inflationary scenario. We here continue this approach by investigating its effects on the predicted perturbation spectrum. We find that the size of the effect depends crucially on the scale separation between cutoff and horizon scales during inflation, becoming negligibly small if the cutoff scale is as small as the Planck length.']",['2001-03-15'] +211,['eng'],"['Huterer, D', 'Turner, M S']",['Constraining the Properties of Dark Energy'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'dark energy', 'density, perturbation', 'galaxy, cluster', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'supernova', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103175'],"['The presence of dark energy in the Universe is inferred directly from the accelerated expansion of the Universe, and indirectly, from measurements of cosmic microwave background (CMB) anisotropy. Dark energy contributes about 2/3 of the critical density, is very smoothly distributed, and has large negative pressure. Its nature is very much unknown. Most of its discernible consequences follow from its effect on evolution of the expansion rate of the Universe, which in turn affects the growth of density perturbations and the age of the Universe, and can be probed by the classical kinematic cosmological tests. Absent a compelling theoretical model (or even a class of models), we describe dark energy by an effective equation of state w=p_X/rho_X which is allowed to vary with time. We describe and compare different approaches for determining w(t), including magnitude-redshift (Hubble) diagram, number counts of galaxies and clusters, and CMB anisotropy, focusing particular attention on the use of a sample of several thousand type Ia supernova with redshifts z < 1.7, as might be gathered by the proposed SNAP satellite. Among other things, we derive optimal strategies for constraining cosmological parameters using type Ia supernovae. While in the near term CMB anisotropy will provide the first measurements of w, supernovae and number counts appear to have the most potential to probe dark energy.']",['2001-03-13'] +212,['eng'],"['Cline, David B']",['Supernova II Neutrino Bursts and Neutrino Massive Mixing'],['Astrophysics and Astronomy'],"['talk, Coral Gables 2000/12/14', 'supernova', 'neutrino, cosmic radiation', 'neutrino, interference', 'neutrino, energy spectrum', 'neutrino, mass spectrum', 'neutrino, solar', 'neutrino, oscillation', 'neutrino, flux', 'counters and detectors', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103138'],"['We describe the Neutrino Spectrum and detection for SN II sources. We discuss the effects of neutrino mixing in the SN II. A new analysis of SN1987A is described. We discuss the possible detection of the diffuse relic SN II flux. Finally we discuss a new detection concept, OMNIS, for Nu sub mu and Nu sub tau and detection and compare with other present and future SN detectors.']",['2001-03-09'] +213,['eng'],"['Halzen, Francis']",['High Energy Neutrino Astronomy'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'Cherenkov counter, water', 'cosmic radiation, angular distribution', 'muon, cosmic radiation', 'deep underground detector', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103195'],"[""Of all high-energy particles, only neutrinos can directly convey astronomical information from the edge of the universe---and from deep inside the most cataclysmic high-energy processes. Copiously produced in high-energy collisions, travelling at the velocity of light, and not deflected by magnetic fields, neutrinos meet the basic requirements for astronomy. Their unique advantage arises from a fundamental property: they are affected only by the weakest of nature's forces (but for gravity) and are therefore essentially unabsorbed as they travel cosmological distances between their origin and us. Many of the outstanding mysteries of astrophysics may be hidden from our sight at all wavelengths of the electromagnetic spectrum because of absorption by matter and radiation between us and the source. For example, the hot dense regions that form the central engines of stars and galaxies are opaque to photons. In other cases, such as supernova remnants, gamma ray bursters, and active galaxies, all of which may involve compact objects or black holes at their cores, the precise origin of the high-energy photons emerging from their surface regions is uncertain. Therefore, data obtained through a variety of observational windows---and especially through direct observations with neutrinos---may be of cardinal importance. In this talk, the scientific goals of high energy neutrino astronomy and the technical aspects of water and ice Cherenkov detectors are examined, and future experimental possibilities, including a kilometer-square deep ice neutrino telescope, are explored.""]",['2001-03-14'] +214,['eng'],"['González-Diáz, P F']",['Quintessence and the first Doppler peak'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'topology, dependence', 'quintessence', 'astrophysics, fundamental constant', 'matter, density', 'supernova', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103194'],"['By using a tracking quintessence model we obtain that the position of the first Doppler peak in the spectrum of CMB anisotropies only depends on the topology of the universe, $\\Omega_k$, for any value of the ratio $\\Omega_{\\Lambda}/\\Omega_M$, so that such a dependence is perfectly valid in the range suggested by supernova observations.']",['2001-03-14'] +215,['eng'],"['Waxman, E']",['High energy particles from gamma-ray bursts'],['Astrophysics and Astronomy'],"['lectures, Campinas 2000/07/17', 'lectures, Trieste 2000/06/12', 'gamma ray burst', 'fireball', 'p, cosmic radiation', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'numerical calculations, Monte Carlo', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103186'],"['A review is presented of the fireball model of gamma-ray bursts (GRBs), and of the production in GRB fireballs of high energy protons and neutrinos. Constraints imposed on the model by recent afterglow observations, which support the association of GRB and ultra-high energy cosmic-ray (UHECR) sources, are discussed. Predictions of the GRB model for UHECR production, which can be tested with planned large area UHECR detectors and with planned high energy neutrino telescopes, are reviewed.']",['2001-03-14'] +216,['eng'],"['Corasaniti, P S', 'Amendola, L', 'Occhionero, F']",['Signals of primordial phase transitions on CMB maps'],['Astrophysics and Astronomy'],"['talk, Rome 2000/07/02', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'critical phenomena', 'inflationary universe', 'vacuum state, bubble', 'statistical analysis', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103173'],"['The analysis of the CMB anisotropies is a rich source of cosmological informations. In our study, we simulated the signals produced by the relics of a first order phase transition occured during an inflationary epoch in the early Universe. These relics are bubbles of true vacuum that leave a characteristic non-Gaussian imprint on the CMB. We use different statistical estimators in order to evaluate this non-Gaussianity. We obtain some limits on the allowed values of the bubble parameters comparing our results with the experimental data. We also predict the possibility to detect this signal with the next high resolution experiments.']",['2001-03-13'] +217,['eng'],"['Sturrock, P A', 'Weber, M A']",['Comparative Analysis of GALLEX-GNO Solar Neutrino Data and SOHO/MDI Helioseismology Data; Further Evidence for Rotational Modulation of the Solar Neutrino Flux'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'flux, oscillation', 'magnetic field, solar', 'resonance', 'statistical analysis', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103154'],"['We carry out a comparative analysis of the GALLEX-GNO solar neutrino data and estimates of the solar internal rotation rate derived from the MDI helioseismology experiment on the SOHO spacecraft. We introduce a statistic, which we evaluate as a function of radius and latitude, that is a measure of the degree of ""resonance"" of oscillations in the neutrino flux and the synodic solar rotation rate at that radius and latitude. A map of this statistic indicates that the probable location is deep in the convection zone near the equator. We also examine the integral of this statistic over the equatorial section of the convection zone. This provides a measure of the likelihood that the variability of the solar neutrino flux, as measured by the GALLEX-GNO data, has its origin in the equatorial section of the convection zone. We apply the shuffle test, randomly reassigning measurements among runs, to estimate the significance of the value of the statistic computed from the actual data. This test implies that the result is significant at the 0.2% level. When, for comparison, we repeat this analysis for the radiative zone, we find that the integral resonance statistic is not significant. These results support earlier evidence for rotational modulation of the solar neutrino flux.']",['2001-03-13'] +218,['eng'],"['Donato, F', 'Maurin, D', 'Salati, Pierre', 'Barrau, A', 'Boudoul, G', 'Taillet, R']",['Antiprotons from spallation of cosmic rays on interstellar matter'],['Astrophysics and Astronomy'],"['anti-p, cosmic radiation', 'cosmic radiation, secondary radiation', 'cosmic radiation, flux', 'p, cosmic radiation', 'cosmic radiation, primary', 'p p, interaction', 'nucleus nucleus, nuclear reaction', 'anti-p, hadroproduction', 'galaxy', 'helium, nuclide', 'differential cross section, momentum dependence', 'nuclear physics', 'diffusion, model', 'acceleration, stochastic', 'energy loss', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103150'],"['Cosmic ray antiprotons provide an important probe for the study of the galactic Dark Matter, as they could be produced by exotic sources. On the other hand, antiprotons are anyway produced by standard nuclear reactions of cosmic ray nuclei on interstellar matter. This process is responsible for a background flux that must be carefully determined to estimate the detectability of an hypothetical exotic signal. Estimates of this background suffer from potential uncertainties of various origins. The propagation of cosmic antiprotons depends on several physical characteristics of the Galaxy which are poorly known. Antiprotons are created from cosmic protons and helium nuclei whose fluxes were not measured with great accuracy until very recently. Calculations of antiproton fluxes make use of nuclear physics models with their own shortcomings and uncertainties. The goal of this paper is to give a new evaluation of the cosmic antiproton flux along with the associated uncertainties. The propagation parameters were tightly constrained in Maurin et al. 2001 by an analysis of cosmic ray nuclei data in the framework of a two-zone diffusion model and we apply these parameters to the propagation of antiprotons. We use the recently published data on proton and helion fluxes, and we find that this particular source of uncertainty has become negligible. The Monte Carlo program DTUNUC was used to carefully examine nuclear reactions. We find that all the cosmic antiproton fluxes naturally coming out of the calculation are fully compatible with experimental data. Uncertainties in this flux have been strongly reduced. Those related to propagation are less than 25%. All other possible sources of uncertainty have also been studied.']",['2001-03-12'] +219,['eng'],"['Kazanas, D', 'Nicolaidis, A']","['Cosmic Ray ""Knee""']",['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'cosmic radiation, primary', 'p p, interaction', 'showers, air', 'gauge field theory, SU(3) x SU(2) x U(1)', 'supersymmetry', 'technicolor', 'gravitation', 'gluon, fusion', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103147'],"['We propose that the knee in the cosmic ray spectrum at energies E ~ 10^{15.5} eV is due to ""new physics"", namely to a channel in the high energy (~ TeV in the CM) proton interactions hitherto unaccounted for in estimating the energies of the air shower cosmic rays. The new interaction transfers part of the primary particle\'s energy to modes which do not trigger the experimental arragement (neutrinos, lightest supersymmetric particle, gravitons) thus underestimating its true energy. We show that this underestimate leads naturally to the observed break (the ""knee"") in the inferred cosmic ray spectrum. The suggestion we advance fits nicely to current theoretical extensions of the Standard Model (supersymmetry, technicolor, low scale gravity) where new physics at the TeV scale manifests with the distinct signature of missing energy. We present a simple model where the new physics proceeds via gluon fusion and assuming a single power law for the galactic (E~ 10^{18.5} eV) cosmic ray spectrum, we produce a good fit to the data in the 10^{14}-10^{18.5} eV range. Our proposal should be testable in laboratory experiments (LHC) in the near future and, should it be proven correct, it would signal besides the presence of new physics in high energy interactions, a drastically different interpretation of the sources and acceleration of cosmic rays.']",['2001-03-12'] +220,['eng'],"['Linke, F', 'Font, J A', 'Janka, H T', 'Müller, E', 'Papadopoulos, P P']",['Spherical collapse of supermassive stars'],['Astrophysics and Astronomy'],"['astrophysics, matter', 'model, hydrodynamical', 'relativity theory, general', 'Einstein equation, solution', 'model, fluid', 'space-time', 'neutrino, emission', 'energy loss', 'black hole, production', 'neutrino antineutrino, annihilation', 'neutrino, energy', 'gamma ray burst', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103144'],"['We present the results of numerical simulations of the spherically symmetric gravitational collapse of supermassive stars (SMS). The collapse is studied using a general relativistic hydrodynamics code. The coupled system of Einstein and fluid equations is solved employing observer time coordinates, by foliating the spacetime by means of outgoing null hypersurfaces. The code contains an equation of state which includes effects due to radiation, electrons and baryons, and detailed microphysics to account for electron-positron pairs. In addition energy losses by thermal neutrino emission are included. We are able to follow the collapse of SMS from the onset of instability up to the point of black hole formation. Several SMS with masses in the range $5\\times 10^5 M_{\\odot}- 10^9 M_{\\odot}$ are simulated. In all models an apparent horizon forms initially, enclosing the innermost 25% of the stellar mass. From the computed neutrino luminosities, estimates of the energy deposition by $\\nu\\bar{\\nu}$-annihilation are obtained. Only a small fraction of this energy is deposited near the surface of the star, where, as proposed recently by Fuller & Shi (1998), it could cause the ultrarelativistic flow believed to be responsible for $\\gamma$-ray bursts. Our simulations show that for collapsing SMS with masses larger than $5\\times 10^5 M_{\\odot}$ the energy deposition is at least two orders of magnitude too small to explain the energetics of observed long-duration bursts at cosmological redshifts. In addition, in the absence of rotational effects the energy is deposited in a region containing most of the stellar mass. Therefore relativistic ejection of matter is impossible.']",['2001-03-12'] +221,['eng'],"['Roszkowski, K']",['Diffusion of the scalar field energy due to the backscattering off Schwarzschild geometry'],['Astrophysics and Astronomy'],"['field theory, scalar', 'energy, diffusion', 'backscatter', 'space-time, Schwarzschild', 'space-time, horizon']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103139'],['This note tackles the problem of the backscattering of a mass-less scalar field in the case of Schwarzschildean space-time. It shows that the effect depends both on a distance from the horizon and on the wave length. The obtained estimates significantly improve former results.'],['2001-03-12'] +222,['eng'],"['Dubovsky, S L', 'Gorbunov, D S']",['Small Second Acoustic Peak from Interacting Cold Dark Matter?'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, acoustic', 'astrophysics, missing-mass', 'dark matter, elastic scattering', 'baryon, matter', 'cross section, elastic scattering', 'charged particle, decay', 'tunneling', 'charge, fractional', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103122'],"['We consider a possibility to explain the observed suppression of the second acoustic peak in the anisotropy spectrum of the Cosmic Microwave Background (CMB) by interaction between a fraction of non-baryonic Cold Dark Matter (CDM) and normal baryonic matter. This scenario does not require any modifications in the standard Big Bang Nucleosynthesis (BBN). We estimate the required values of the cross-section-to-mass ratio for elastic scattering of CDM particles off baryons. In case of velocity-independent elastic scattering (in the velocity interval 10^{-5}--10^{-3}) we find that such particles do not contradict observational limits if they are heavier than \\sim 10^5 GeV or lighter than \\sim 0.5 GeV. Another candidate, which may appear in the models with infinite extra dimensions, is a quasistable charged particle decaying through tunneling into extra dimensions. Finally a millicharged particle with the electric charge ranging from \\sim 10^{-4} to \\sim 10^{-1} and with mass M\\sim 0.1 GeV--1 TeV also may be responsible for the suppression of the second acoustic peak. As a byproduct we point out that CMB measurements set new limits on the allowed parameter space for the millicharged particles.']",['2001-03-08'] +223,['eng'],"['Picozza, P', 'Morselli, A']",['Exotic Matter research in Space'],['Astrophysics and Astronomy'],"['talk, Rome 2000/07/02', 'astrophysics, missing-mass', 'matter, exotic', 'neutralino, annihilation', 'anti-p, cosmic radiation', 'cosmic radiation, flux', 'positron, cosmic radiation', 'cosmic radiation, energy spectrum', 'antimatter, search for', 'transition radiation detector', 'scintillation counter', 'counters and detectors, satellite', 'proposed experiment']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103117'],['The direct detection of annihilation products in cosmic rays offer an alternative way to search for dark matter particles candidates. Here we will see in particular that the study of the spectrum of antiproton and positrons offer good possibilities to perform this search and we will review our experimental effort in this direction.'],['2001-03-08'] +224,['eng'],"['Prakash, M', 'Lattimer, J M', 'Sawyer, R F', 'Volkas, R R']",['Neutrino Propagation in Dense Astrophysical Systems'],['Astrophysics and Astronomy'],"['review', 'neutrino, diffusion', 'neutrino, mixing angle', 'neutrino, scattering', 'neutrino, path length', 'astrophysics, model', 'neutrino, oscillation', 'neutrino, sterile', 'supernova', 'n, matter', 'neutrino, luminosity', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103095'],"['Even the elusive neutrinos are trapped in matter, albeit transiently, in several astrophysical circumstances. Their interactions with the ambient matter not only reveal the properties of such exotic matter itself, but also shed light on the fundamental properties of the neutrinos themselves. The physical sites of interest include the early universe, supernovae, and newly-born neutron stars. Detection of neutrinos from these vastly different eras using the new generation of neutrino detectors holds great promise for enhancing our understanding of neutrino-matter interactions and astrophysical phenomena.']",['2001-03-07'] +225,['eng'],"['Dimmelmeier, H', 'Font, J A', 'Müller, E']",['Gravitational waves from relativistic rotational core collapse'],['Astrophysics and Astronomy'],"['gravitational radiation', 'model, hydrodynamical', 'supernova', 'symmetry, axial', 'boundary condition']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103088'],"['We present results from simulations of axisymmetric relativistic rotational core collapse. The general relativistic hydrodynamic equations are formulated in flux-conservative form and solved using a high-resolution shock-capturing scheme. The Einstein equations are approximated with a conformally flat 3-metric. We use the quadrupole formula to extract waveforms of the gravitational radiation emitted during the collapse. A comparison of our results with those of Newtonian simulations shows that the wave amplitudes agree within 30%. Surprisingly, in some cases, relativistic effects actually diminish the amplitude of the gravitational wave signal. We further find that the parameter range of models suffering multiple coherent bounces due to centrifugal forces is considerably smaller than in Newtonian simulations.']",['2001-03-07'] +226,['eng'],"['Evans, W', 'Ferrer, F', 'Sarkar, S']",['The Anisotropy of the Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'cosmic radiation, anisotropy', 'signal processing', 'galaxy', 'data analysis method', 'astrophysics, missing-mass', 'particle, massive', 'particle, decay', 'cosmic radiation, production', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103085'],"['Ultra-high energy cosmic rays (UHECRs) may originate from the decay of massive relic particles in the dark halo of the Galaxy, or they may be produced by supermassive black holes in the nuclei of nearby galaxies. The anisotropy in the arrival directions is studied in four dark halo models (cusped, isothermal, triaxial and tilted) and in four galaxy samples (galaxies intrinsically brighter than Centaurus A within 50 and 100 Mpc, and brighter than M32 within 50 and 100 Mpc). In decaying dark matter models, the amplitude of the anisotropy is controlled by the size of the Galactic halo, while the phase is controlled by the shape. In the northern hemisphere, the amplitude is about 0.5 for cusped haloes, but falls to roughly 0.3 for isothermal haloes. The phase points in the direction of the Galactic Centre, with deviations of up to 30 degrees possible for triaxial and tilted haloes. The effect of the halo of M31 is too weak to provide conclusive evidence for the decaying dark matter origin of UHECRs. In extragalactic models, samples of galaxies brighter than Centaurus A produce substantial anisotropies (roughly 1.8), much larger than the limits set by the available data. If all galaxies brighter than M32 contribute, then the anisotropy is more modest (roughly 0.5) and is directed toward mass concentrations in the supergalactic plane, like the Virgo cluster. Predictions are made for the southern hemisphere station of the Pierre Auger Observatory. If the UHECRs have a Galactic origin, then the phase points towards the Galactic Centre. If they have an extragalactic origin, then it points in the rough direction of the Fornax cluster. This provides an unambiguous discriminant and requires about 350-500 events at South Auger.']",['2001-03-07'] +227,['eng'],"['Pina-Avelino, P', 'De Carvalho, J P M', 'Martins, C J A P']",['Supernovae constraints on spatial variations of the vacuum energy density'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'vacuum state, energy', 'energy, density', 'energy, spatial distribution', 'luminosity', 'perturbation theory, linear', 'supernova', 'space-time, perturbation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103075'],"[""We consider a very simple toy model for a spatially varying `cosmological constant', where we are inside a spherical bubble (with a given set of cosmological parameters) that is surrounded by a larger region where these parameters are different. This model includes essential features of more realistic scenarios with a minimum number of parameters. We calculate the luminosity distance in the presence of spatial variations of the vacuum energy density using linear perturbation theory and discuss the use of type Ia supernovae to impose constraints on this type of models. We find that presently available observations are only constraining at very low redshifts, but also provide independent confirmation that the high red-shift supernovae data does prefer a relatively large positive cosmological constant.""]",['2001-03-06'] +228,['eng'],"['Heck, D']",['Extensive Air Shower Simulations with CORSIKA and the Influence of High-Energy Hadronic Interaction Models'],['Astrophysics and Astronomy'],"['talk, Tihany 2000/10/09', 'hadron, cosmic radiation', 'hadron nucleus, interaction', 'showers, air', 'cross section, inelastic scattering', 'cosmic radiation, energy spectrum', 'particle, diffusion', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103073'],"[""When high-energy cosmic rays (gamma's, protons, or heavy nuclei) impinge onto the Earth's atmosphere, they interact at high altitude with the air nuclei as targets. By repeated interaction of the secondaries an `extensive air shower' (EAS) is generated with huge particle numbers in the maximum of the shower development. Such cascades are quantitatively simulated by the Monte Carlo computer program CORSIKA. The most important uncertainties in simulations arise from modeling of high-energy hadronic interactions: a) The inelastic hadron-air cross sections. b) The energies occurring in EAS may extend far above the energies available in man-made accelerators, and when extrapolating towards higher energies one has to rely on theoretical guidelines. c) In collider experiments which are used to adjust the interaction models the very forward particles are not accessible, but just those particles carry most of the hadronic energy, and in the EAS development they transport a large energy fraction down into the atmosphere. CORSIKA is coupled alternatively with 6 high-energy hadronic interaction codes (DPMJET, HDPM, neXus, QGSJET, SIBYLL, VENUS). The influence of those interaction models on observables of simulated EAS is discussed.""]",['2001-03-06'] +229,['eng'],"['Hannestad, S', 'Hansen, S H', 'Villante, F L', 'Hamilton, A J S']",['Constraints on inflation from CMB and Lyman-alpha forest'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time, perturbation', 'spectra, perturbation', 'cosmic radiation, background', 'perturbation, scalar', 'perturbation, tensor', 'data analysis method', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103047'],"['We constrain the spectrum of primordial curvature perturbations by using recent Cosmic Microwave Background (CMB) and Large Scale Structure (LSS) data. Specifically, we consider CMB data from the COBE, Boomerang and Maxima experiments, the real space galaxy power spectrum from the IRAS PSCz survey, and the linear matter power spectrum inferred from Ly-alpha forest spectra. We study the case of single field slow roll inflationary models, and we extract bounds on the scalar spectral index, n, the tensor to scalar ratio, r, and the running of the scalar spectral index, dlnk, for various combinations of the observational data. We find that CMB data, when combined with data from Lyman-alpha forest, place strong constraints on the inflationary parameters. Specifically, we obtain n \\approx 0.9, r < 0.3 and dlnk \\approx 0, indicating that single field hybrid models are ruled out.']",['2001-03-05'] +230,['eng'],"['Anchordoqui, L A', 'Goldberg, H', 'Weiler, Thomas J']",['An Auger test of the Cen A model of highest energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'nucleon, cosmic radiation', 'nucleon, flux', 'magnetic field', 'cosmic radiation, energy spectrum', 'GZK effect', 'cosmic radiation, anisotropy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103043'],"[""If, as recently proposed by Farrar and Piran, Cen A is the source of cosmic rays detected above the Greisen-Zatsepin-Kuz'min cutoff, neutrons are $\\approx 700$ more probable than protons to be observed along its line of sight. This is because the proton flux is rendered nearly isotropic by ${\\cal O}(\\mu$G) intergalactic magnetic fields. With the anticipated aperture of the Southern Auger Observatory, one may expect on the order of 10 neutron events/year above $10^{20}$ eV in the line of sight of Cen A.""]",['2001-03-05'] +231,['eng'],"['Poirier, J', 'Roesler, S', 'Fassò, Alberto']",['Distributions of secondary muons at sea level from cosmic gamma rays below 10 TeV'],['Astrophysics and Astronomy'],"['muon, cosmic radiation', 'cosmic radiation, secondary radiation', 'photon, cosmic radiation', 'cosmic radiation, primary', 'showers, air', 'counters and detectors, angular resolution', 'cosmic radiation, angular correlation', 'data analysis method', 'muon, production', 'cosmic radiation, angular distribution', 'effect, pressure', 'effect, temperature', 'muon, energy spectrum', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103030'],"['In experiments sensitive to secondary cosmic ray muons reaching ground level, one of the main goals of the experimental data analysis is to deduce the features of the primary progenitors of the muons. For this purpose, the FLUKA Monte Carlo program is used to predict the distributions of the muons which originate from primary cosmic gamma rays and reach sea level. Various physical effects are found to affect these distributions in differing proportions.']",['2001-03-05'] +232,['eng'],"['Janka, H T', 'Kifonidis, K', 'Rampp, M']",['Supernova Explosions and Neutron Star Formation'],['Astrophysics and Astronomy'],"['talk, Trento 2000/06/19', 'supernova', 'n, matter', 'matter, production', 'neutrino, emission', 'transport theory', 'Boltzmann equation, solution', 'light nucleus, production', 'stability, hydrodynamical', 'dimension, 2', 'effect, rotational', 'neutrino nucleon, interaction', 'nucleon, correlation', 'nuclear matter', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0103015'],"['The current picture of the collapse and explosion of massive stars and the formation of neutron stars is reviewed. According to the favored scenario, however by no means proven and undisputed, neutrinos deposit the energy of the explosion in the stellar medium which surrounds the nascent neutron star. Observations, in particular of Supernova~1987A, suggest that mixing processes play an important role in the expanding star, and multi-dimensional simulations show that these are linked to convective instabilities in the immediate vicinity of the neutron star. Convectively enhanced energy transport inside the neutron star can have important consequences for the neutrino emission and thus the neutrino-heating mechanism. This also holds for a suppression of the neutrino interactions at nuclear densities. Multi-dimensional hydrodynamics, general relativity, and a better understanding of the neutrino interactions in neutron star matter may be crucial to resolve the problem that state-of-the-art spherical models do not yield explosions even with a very accurate treatment of neutrino transport by solving the Boltzmann equation.']",['2001-03-02'] +233,['eng'],"['Guetta, D', 'Spada, M', 'Waxman, E']",['On the Neutrino Flux from Gamma-Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'gamma ray burst', 'fireball, relativistic', 'energy, dissipation', 'photon p, interaction', 'synchrotron radiation', 'neutrino, production', 'neutrino, flux', 'neutrino, energy', 'pi, energy loss', 'muon, energy loss', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102487'],"['Observations imply that gamma-ray bursts (GRBs) are produced by the dissipation of the kinetic energy of a highly relativistic fireball. Photo-meson interactions of protons with gamma-rays within the fireball dissipation region are expected to convert a significant fraction of fireball energy to >10^14 eV neutrinos. We present an analysis of the internal shock model of GRBs, where production of synchrotron photons and photo-meson neutrinos are self-consistently calculated, and show that the fraction of fireball energy converted to high energy neutrinos is not sensitive to uncertainties in fireball model parameters, such as the expansion Lorentz factor and characteristic variability time. This is due in part to the constraints imposed on fireball parameters by observed GRB characteristics, and in part to the fact that for parameter values for which the photo-meson optical depth is high (implying high proton energy loss to pion production) neutrino production is suppressed by pion and muon synchrotron losses. The neutrino flux is therefore expected to be correlated mainly with the observed gamma-ray flux. The time averaged neutrino intensity predicted by the model, ~10^-8.5 GeV/cm^2 s sr, is consistent with the flux predicted by the assumption that GRBs are the sources of >10^19 eV cosmic-rays.']",['2001-03-01'] +234,['eng'],"['Boyanovsky, D', 'Cao, F J', 'De Vega, H J']",['Inflation from Tsunami-waves'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'condensation', 'expansion 1/N', 'chaos', 'field equations', 'renormalization', 'boundary condition', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102474'],"['We investigate inflation driven by the evolution of highly excited quantum states within the framework of out of equilibrium field dynamics. These states are characterized by a non-perturbatively large number of quanta in a band of momenta but with vanishing expectation value of the scalar field.They represent the situation in which initially a non-perturbatively large energy density is localized in a band of high energy quantum modes and are coined tsunami-waves. The self-consistent evolution of this quantum state and the scale factor is studied analytically and numerically. It is shown that the time evolution of these quantum states lead to two consecutive stages of inflation under conditions that are the quantum analogue of slow-roll. The evolution of the scale factor during the first stage has new features that are characteristic of the quantum state. During this initial stage the quantum fluctuations in the highly excited band build up an effective homogeneous condensate with a non- perturbatively large amplitude as a consequence of the large number of quanta. The second stage of inflation is similar to the usual classical chaotic scenario but driven by this effective condensate.The excited quantum modes are already superhorizon in the first stage and do not affect the power spectrum of scalar perturbations. Thus, this tsunami quantum state provides a field theoretical justification for chaotic scenarios driven by a classical homogeneous scalar field of large amplitude.']",['2001-02-28'] +235,['eng'],"['Ott, T']",['Gauge Invariant Perturbation Analysis for Quintessence with an Exponential Potential'],['Astrophysics and Astronomy'],"['quintessence', 'field theory, scalar', 'fluid', 'perturbation, adiabatic', 'invariance, gauge', 'attractor', 'fluctuation', 'energy, density', 'cosmic radiation, background', 'matter, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102448'],['Adiabatic perturbations in the cosmology of a quintessential scalar field with exponential potential gravitationally coupled to radiation/matter are investigated in a gauge invariant formalism. The main question addressed in this paper is if the inhomogenous fluctuations can be ignored as often argued and the result is that this is not always the case. Consequences for microwave background radiation and structure formation in the matter dominated era are considered.'],['2001-02-27'] +236,['eng'],"['Antoni, T']",['A Non-Parametric Approach to Infer the Energy Spectrum and the Mass Composition of Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, hadronic component', 'showers, air', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'p, cosmic radiation', 'oxygen, cosmic radiation', 'iron, cosmic radiation', 'cosmic radiation, primary', 'cosmic radiation, mass', 'statistical analysis', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102443'],"['The experiment KASCADE observes simultaneously the electron-photon, muon, and hadron components of high-energy extensive air showers (EAS). The analysis of EAS observables for an estimate of energy and mass of the primary particle invokes extensive Monte Carlo simulations of the EAS development for preparing reference patterns. The present studies utilize the air shower simulation code CORSIKA with the hadronic interaction models VENUS, QGSJet and Sibyll, including simulations of the detector response and efficiency. By applying non-parametric techniques the measured data have been analyzed in an event-by-event mode and the mass and energy of the EAS inducing particles are reconstructed. Special emphasis is given to methodical limitations and the dependence of the results on the hadronic interaction model used. The results obtained from KASCADE data reproduce the knee in the primary spectrum, but reveal a strong model dependence. Owing to the systematic uncertainties introduced by the hadronic interaction models no strong change of chemical composition can be claimed in the energy range around the knee.']",['2001-02-27'] +237,['eng'],"['Fargion, D', 'Grossi, M', 'De Sanctis-Lucentini, P G', 'Troia, C D', 'Konoplich, R V']",['Shadows of Relic Neutrino Masses and Spectra on Highest Energy GZK Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/07/10', 'neutrino, cosmic radiation', 'GZK effect', 'neutrino antineutrino, interaction', 'Z0, pair production', 'W, pair production', 'channel cross section, energy dependence', 'W, hadronic decay', 'W, leptonic decay', 'Z0, decay modes', 'cosmic radiation, particle source', 'neutrino, mass', 'neutrino, energy spectrum', 'neutrino, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102426'],"['The Ultra High Energy (UHE) neutrino scattering onto relic cosmic neutrinos in galactic and local halos offers an unique way to overcome GZK cut-off. The UHE nu secondary of UHE photo-pion decays may escape the GZK cut-off and travel on cosmic distances hitting local light relic neutrinos clustered in dark halos. The Z resonant production and the competitive W^+W^-, ZZ pair production define a characteristic imprint on hadronic consequent UHECR spectra. This imprint keeps memory both of the primary UHE nu spectra as well as of the possible relic neutrino masses values, energy spectra and relic densities. Such an hadronic showering imprint should reflect into spectra morphology of cosmic rays near and above GZK 10^{19}-10^{21}eV cut-off energies. A possible neutrino degenerate masses at eVs or a more complex and significant neutrino mass split below or near Super-Kamiokande \\triangle m_{\\nu_{SK}}= 0.1 eV masses might be reflected after each corresponding Z peak showering, into new twin unexpected UHECR flux modulation behind GZK energies: E_{p} sim 3(frac{triangle m_{\\nu_{SK}}}/m_{\\nu}10^{21}),eV. Other shadowsof lightest, nearly massless, neutrinos m_{nu_{2K} simeq 0.001eV simeq kT_{\\nu}, their lowest relic temperatures, energies and densities might be also reflected at even higher energies edges near Grand Unification: E_{p} \\sim 2.2(m_{\\nu_{2K}/E_{\\nu}})10^{23}, eV .']",['2001-02-27'] +238,['eng'],"['Hwang, J', 'Noh, H']",['f(R) gravity theory and CMBR constraints'],['Astrophysics and Astronomy'],"['gravitation, model', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, spectra', 'perturbation, scalar', 'perturbation, tensor', 'coupling constant', 'energy', 'gravitational radiation', 'transformation, conformal', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102423'],"[""We consider the large-scale cosmic structure generation by an inflation based on a pure f(R)-type gravity theory. Comparison with recent CMBR observations gives the following results: (1) The near Zel'dovich spectral conditions uniquely choose R^2-type gravity. (2) The R^2 gravity predicts specific nearly scale-invariant Zel'dovich spectra for both the scalar- and tensor-type perturbations. Thus, (3) the considered model survives current observational data. The COBE-DMR quadrupole data (4) give constraints on the coupling constant and the energy scale during inflation, and (5) require the gravitational wave contribution to be suppressed. (6) Therefore, future observations of (2) and (5) can provide strong tests of the inflation scenario based on R^2 gravity. Parallel analyses made in the conformally transformed Einstein frame give the observationally identical results.""]",['2001-02-26'] +239,['eng'],"['Dvali, G', 'Gabadadze, Gregory T', 'Shifman, M']",['Ultralight Scalars and Spiral Galaxies'],['Astrophysics and Astronomy'],"['dilaton', 'field theory, scalar', 'domain wall, network', 'galaxy', 'zero mode', 'scalar particle, massless', 'dimension, 3', 'tensor, energy-momentum', 'matter, coupling', 'astrophysics, missing-mass', 'inflationary universe', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102422'],"[""We study some possible astrophysical implications of a very weakly coupled ultralight dilaton-type scalar field. Such a field may develop an (approximately stable) network of domain walls. The domain wall thickness is assumed to be comparable with the thickness of the luminous part of the spiral galaxies. The walls provide trapping for galactic matter. This is used to motivate the very existence of the spiral galaxies. A zero mode existing on the domain wall is a massless scalar particle confined to 1+2 dimensions. At distances much larger than the galaxy/wall thickness, the zero-mode exchange generates a logarithmic potential, acting as an additional term with respect to Newton's gravity. The logarithmic term naturally leads to constant rotational velocities at the periphery. We estimate the scalar field coupling to the matter energy-momentum tensor needed to fit the observable flat rotational curves of the spiral galaxies. The value of this coupling turns out to be reasonable -- we find no contradiction with the existing data.""]",['2001-02-26'] +240,['eng'],"['Medvedev, M V']",['Self-Interacting Dark Matter with Flavor Mixing'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'astrophysics, missing-mass', 'flavor, interference', 'gravitation, external field', 'dark matter, interaction']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102400'],"['The crisis of the cold dark matter and problems of the self-interacting dark matter models is resolved by postulating flavor mixing of dark matter particles. Flavor-mixed particles segregate in the gravitational field to form dark halos composed of heavy mass eigenstates. Since these particles are mixed in the interaction basis, elastic collisions convert some of heavy eigenstates into light ones which leave dense central regions of the halo. This annihilation-like process will soften dense central cusps of halos. The proposed model accumulates most of the attractive features of self-interacting and annihilating dark matter models, but does not suffer from their severe drawbacks. This model is natural; it does not require fine tuning.']",['2001-02-26'] +241,['eng'],"['Aharonian, F A']",['Evidence for TeV gamma ray emission from Cassiopeia A'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'supernova', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'Cherenkov counter', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102391'],"['232 hours of data were accumulated from 1997 to 1999, using the HEGRA Stereoscopic Cherenkov Telescope System to observe the supernova remnant Cassiopeia A. TeV gamma ray emission was detected at the 5 sigma level, and a flux of (5.8 +- 1.2(stat) +- 1.2(syst)) 10^(-9) ph m^(-2) s^(-1) above 1 TeV was derived. The spectral distribution is consistent with a power law with a differential spectral index of -2.5 +- 0.4(stat) +- 0.1(syst) between 1 and 10 TeV. As this is the first report of the detection of a TeV gamma ray source on the ""centi-Crab"" scale, we present the analysis in some detail. Implications for the acceleration of cosmic rays depend on the details of the source modeling. We discuss some important aspects in this paper.']",['2001-02-23'] +242,['eng'],"['Carr, B J']",['Primordial black holes as a probe of the early universe and a varying gravitational constant'],['Astrophysics and Astronomy'],"['talk, Erice 2000/12/06', 'astrophysics, model', 'black hole, production', 'black hole, radiation', 'gravitation, fundamental constant', 'time variation', 'gravitation, scalar', 'gravitation, tensor', 'fluid, accretion', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102390'],"['We discuss recent developments in the study of primordial black holes, focussing particularly on their formation and quantum evaporation. Such studies can place important constraints on models of the early Universe. An especially interesting development has been the realization that such constraints may be severely modified if the value of the gravitational ""constant"" G varies with cosmological epoch, a possibility which arises in many scenarios for the early Universe. The nature of the modification depends upon whether the value of $G$ near a black hole maintains the value it had at its formation epoch (corresponding to gravitational memory) or whether it tracks the background cosmological value. This is still uncertain but we discuss various approaches which might help to resolve the issue.']",['2001-02-23'] +243,['eng'],"['Cuesta, H J M', 'González, D M']",['Bursts of gravitational radiation from superconducting cosmic strings and the neutrino mass spectrum'],['Astrophysics and Astronomy'],"['astrophysics, string', 'superconducting, string', 'gamma ray burst, particle source', 'gravitational radiation, particle source', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'cosmic radiation, time delay', 'neutrino, mass spectrum', 'counters and detectors', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102454'],"['Berezinsky, Hnatyk and Vilenkin showed that superconducting cosmic strings could be central engines for cosmological gamma-ray bursts and for producing the neutrino component of ultra-high energy cosmic rays. A consequence of this mechanism would be that a detectable cusp-triggered gravitational wave burst should be released simultaneously with the $\\gamma$-ray surge. If contemporary measurements of both $\\gamma$ and $\\nu$ radiation could be made for any particular source, then the cosmological time-delay between them might be useful for putting unprecedently tight bounds on the neutrino mass spectrum. Such measurements could consistently verify or rule out the model, since strictly correlated behaviour is expected for the duration of the event and for the time variability of the spectra.']",['2001-02-27'] +244,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Hnatyk, B I', 'Vilenkin, A']",['Gamma ray bursts from superconducting cosmic strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'superconducting, string', 'current, electric', 'gamma ray burst, particle source', 'model, hydrodynamical', 'gravitational radiation', 'counters and detectors', 'photon, cosmic radiation', 'electron, cosmic radiation', 'cosmic radiation, acceleration', 'synchrotron radiation', 'cosmic radiation, background', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102366'],"['Cusps of superconducting strings can serve as GRB engines. A powerful beamed pulse of electromagnetic radiation from a cusp produces a jet of accelerated particles, whose propagation is terminated by the shock responsible for GRB. A single free parameter, the string scale of symmetry breaking $\\eta \\sim 10^{14} GeV$, together with reasonable assumptions about the magnitude of cosmic magnetic fields and the fraction of volume that they occupy, explains the GRB rate, duration and fluence, as well as the observed ranges of these quantities. The wiggles on the string can drive the short-time structures of GRB. This model predicts that GRBs are accompanied by strong bursts of gravitational radiation which should be detectable by LIGO, VIRGO and LISA detectors. Another prediction is the diffuse X- and gamma-ray radiation at 8 MeV - 100 GeV with a spectrum and flux comparable to the observed.The model does not account for the observed association between long GRBs and galaxies. This suggests that GRBs from cusps may be responsible for only a subset of the observed GRBs.']",['2001-02-22'] +245,['eng'],"['Campos, A', 'Sopuerta, C F']",['Dynamics of Cosmological Models in the Brane-world Scenario'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'membrane model', 'space-time, Robertson-Walker', 'space-time, Bianchi', 'Randall-Sundrum model']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102355'],['We present the results of a systematic investigation of the qualitative behaviour of the Friedmann-Lemaitre-Robertson-Walker (FLRW) and Bianchi I and V cosmological models in Randall-Sundrum brane-world type scenarios.'],['2001-02-22'] +246,['eng'],"['Kampert, K H']",['Cosmic Rays in the Energy Range of the Knee - Recent Results from KASCADE --'],['Astrophysics and Astronomy'],"['talk, Tihany 2000/10/09', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'galaxy', 'magnetic field, confinement', 'showers, air', 'ratio, (muon electron)', 'antineutrino p, interaction', 'charged current', 'hadron hadron, interaction', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102266'],"[""A brief motivation for studying cosmic rays at energies 10^14 < E < 10^17 eV is given. Besides astrophysical interests in identifying and understanding their sources, there are also particle physics aspects related to their transport properties in the galaxy or to their detection via extensive air showers. The KASCADE air shower experiment taking data at Forschungszentrum Karlsruhe (Germany) provides important information to both of these topics of particle-astrophysics research. A target of particular interest is the so-called 'knee' in the cosmic ray energy spectrum at E_k = 4 x 10^15 eV. Recent results adding knowledge to an understanding its origin will be presented as well as results on tests of high-energy hadronic interaction models required for air shower simulations.""]",['2001-02-16'] +247,['eng'],"['Frampton, Paul H']",['Quintessence and Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['talk, Coral Gables 2000/12/14', 'cosmic radiation, background', 'temperature, anisotropy', 'dark energy, time dependence', 'energy, density', 'quintessence', 'astrophysics, fundamental constant', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102344'],"['Analytic formulas for the position of the first acoustic peak in the CMB are derived and discussed. They are generalized to the case of a time-dependent dark energy component and it is shown how the cosmic parameters $\\Omega_M$ and $\\Lambda_{\\Lambda}$, extracted from observations, have an intrinsic uncertainty until one knows whether the dark energy density is, or is not, time dependent.']",['2001-02-21'] +248,['eng'],"['Weekes, T C']",['Radio Pulses from Cosmic Ray Air Showers'],['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'cosmic radiation, particle source', 'showers, air', 'trigger', 'Cherenkov counter', 'signal processing', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102342'],"['The first experiment in which radio emission was detected from high energy particles is described. An array of dipoles was operated by a team of British and Irish physicists in 1964-5 at the Jodrell Bank Radio Observatory in conjunction with a simple air shower trigger. The array operated at 44 MHz with 2.75 MHz bandwidth. Out of 4,500 triggers a clear bandwidth-limited radio pulse was seen in 11 events. This corresponded to a cosmic ray trigger threshold of 5x10^16 eV and was of intensity close to that predicted. The early experiments which followed this discovery and their interpretation is described.']",['2001-02-21'] +249,['eng'],"['Waxman, E', 'Loeb, A']",['TeV Neutrinos and GeV Photons from Shock Breakout in Supernovae'],['Astrophysics and Astronomy'],"['supernova', 'shock waves', 'p, acceleration', 'neutrino, production', 'photon, production', 'cosmic radiation, flux']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102317'],"['We show that as a Type II supernova shock breaks out of its progenitor star, it becomes collisionless and may accelerate protons to energies >10 TeV. Inelastic nuclear collisions of these protons produce a ~1 hr long flash of TeV neutrinos and 10 GeV photons, about 10 hr after the thermal (10 MeV) neutrino burst from the cooling neutron star. A Galactic supernova in a red supergiant star would produce a photon and neutrino flux of ~10^{-4} erg/cm^2 s. A km^2 neutrino detector will detect ~100 muons, thus allowing to constrain both supernova models and neutrino properties.']",['2001-04-04'] +250,['eng'],"['Piran, T']",['Gravitational Radiation from Gamma-Ray Bursts'],['Astrophysics and Astronomy'],"['talk, Trieste 2000/06/05', 'gamma ray burst', 'gravitational radiation', 'n, matter', 'black hole', 'fireball', 'supernova', 'counters and detectors', 'laser, interference']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102315'],"['Gamma Ray Bursts (GRBs) are the most relativistic objects known so far, involving, on one hand an ultra-relativistic motion with a Lorentz factor $\\Gamma > 100$ and on the other hand an accreting newborn black hole. The two main routes leading to this scenario: binary neutron star mergers and Collapsar - the collapse of a rotating star to a black hole, are classical sources for gravitational radiation. Additionally one expect a specific a gravitational radiation pulse associated with the acceleration of the relativistic ejecta. I consider here the implication of the observed rates of GRBs to the possibility of detection of a gravitational radiation signal associated with a GRB. Unfortunately I find that, with currently planned detectors it is impossible to detect the direct gravitational radiation associated with the GRB. It is also quite unlikely to detect gravitational radiation associated with Collapsars. However, the detection of gravitational radiation from a neutron star merger associated with a GRB is likely.']",['2001-04-04'] +251,['eng'],"['Noh, H', 'Hwang, J']",['Observational constraints on inflation models with nonminimal scalar field'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'inflationary universe', 'field theory, scalar', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102311'],['We present the power spectra of the scalar- and tensor-type structures generated in an inflation model based on the nonminimally coupled scalar field with a self coupling. By comparing the contributions of these structures to the anisotropy of the cosmic microwave background radiation with the four year COBE DMR data we derive strong constraints on model parameters and the inflation model.'],['2001-04-04'] +252,['eng'],"['Foot, R']",['Seven (and a half) reasons to believe in Mirror Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'matter, mirror', 'neutrino, oscillation', 'positronium, lifetime', 'Higgs particle, production', 'Higgs particle, width', 'MACHO', 'neutrino, cosmic radiation', 'neutrino, solar', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102294'],"['Parity and time reversal are obvious and plausible candidates for fundamental symmetries of nature. Hypothesising that these symmetries exist implies the existence of a new form of matter, called mirror matter. The mirror matter theory (or exact parity model) makes four main predictions: 1) Dark matter in the form of mirror matter should exist in the Universe (i.e. mirror galaxies, stars, planets, meteoroids...), 2) Maximal ordinary neutrino - mirror neutrino oscillations if neutrinos have mass, 3) Orthopositronium should have a shorter effective lifetime than predicted by QED (in ""vacuum"" experiments) because of the effects of photon-mirror photon mixing and 4) Higgs production and decay rate should be 50% lower than in the standard model due to Higgs mirror - Higgs mixing. At the present time there is strong experimental/observational evidence supporting the first three of these predictions, while the fourth one is not tested yet because the Higgs boson, predicted in the standard model of particle physics, is yet to be found. This experimental/observational evidence is rich and varied ranging from the atmospheric and solar neutrino deficits, MACHO gravitational microlensing events, strange properties of extra-solar planets, the existence of ""isolated"" planets, orthopositronium lifetime anomaly, Tunguska and other strange ""meteor"" events including perhaps, the origin of the moon. The purpose of this article is to provide a not too technical review of these ideas along with some ne results.']",['2001-02-19'] +253,['eng'],"['Adams, J', 'Cresswell, B', 'Easther, R']",['Inflationary perturbations from a potential with a step'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'spectra, oscillation', 'inflaton, potential', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102236'],['We use a numerical code to compute the density perturbations generated during an inflationary epoch which includes a spontaneous symmetry breaking phase transition. A sharp step in the inflaton potential generates $k$ dependent oscillations in the spectrum of primordial density perturbations. The amplitude and extent in wavenumber of these oscillations depends on both the magnitude and gradient of the step in the inflaton potential. We show that observations of the cosmic microwave background anisotropy place strong constraints on the step parameters.'],['2001-02-14'] +254,['eng'],"['Stecker, F W', 'Glashow, Sheldon Lee']",['New Tests of Lorentz Invariance Following from Observations of the Highest Energy Cosmic Gamma Rays'],['Astrophysics and Astronomy'],"['symmetry, Lorentz', 'validity test', 'photon, cosmic radiation', 'electron, velocity', 'electron, cosmic radiation', 'cosmic radiation, energy', 'blazar', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102226'],['We use the recent reanalysis of multi-TeV gamma-ray observations of Mrk 501 to constrain the Lorentz invariance breaking parameter involving the maximum electron velocity. Our limit is two orders of magnitude better than that obtained from the maximum observed cosmic-ray electron energy.'],['2001-02-14'] +255,['eng'],"['Moskalenko, I V', 'Christian, E R', 'Moiseev, A A', 'Ormes, J F', 'Strong, A W']",['Antiprotons below 200 MeV in the interstellar medium'],['Astrophysics and Astronomy'],"['talk, Potsdam 2000/07/24', 'anti-p, cosmic radiation', 'cosmic radiation, secondary radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'cosmic radiation, background', 'cosmic radiation, secondary radiation', 'cosmic radiation, time variation', 'scintillation counter, bismuth-germanate', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102207'],"['Most cosmic ray antiprotons observed near the Earth are secondaries produced in collisions of energetic cosmic ray (CR) particles with interstellar gas. The spectrum of secondary antiprotons is expected to peak at ~2 GeV and decrease sharply at lower energies. This leaves a low energy window in which to look for signatures of exotic processes such as evaporation of primordial black holes or dark matter annihilation. In the inner heliosphere, however, modulation of CRs by the solar wind makes analysis difficult. Detecting these antiprotons outside the heliosphere on an interstellar probe removes most of the complications of modulation. We present a new calculation of the expected secondary antiproton flux (the background) as well as a preliminary design of a light-weight, low-power instrument for the interstellar probe to make such measurements.']",['2001-02-13'] +256,['eng'],"['Terrero-Escalante, C A', 'Schwarz, Dominik J', 'Garcia, A A']",['Revisiting the calculations of inflationary perturbations'],['Astrophysics and Astronomy'],"['talk, Mexico City 2000/10/01', 'inflationary universe', 'perturbation, scalar', 'perturbation, tensor']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102174'],"['We present a new approximation scheme that allows us to increase the accuracy of analytical predictions of the power spectra of inflationary perturbations for two specific classes of inflationary models. Among these models are chaotic inflation with a monomial potential, power-law inflation and natural inflation (inflation at a maximum). After reviewing the established first order results we calculate the amplitudes and spectral indices for these classes of models at higher orders in the slow-roll parameters for scalar and tensorial perturbations.']",['2001-02-12'] +257,['eng'],"['Alvarez-Muñiz, J', 'Zas, E']",['Prospects for radio detection of extremely high energy cosmic rays and neutrinos in the Moon'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, interaction', 'cosmic radiation, flux', 'surface, lunar', 'showers', 'radiation, Cherenkov', 'electric field', 'energy, threshold', 'Cherenkov counter', 'efficiency']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102173'],['We explore the feasibility of using the Moon as a detector of extremely high energy (>10^19 eV) cosmic rays and neutrinos. The idea is to use the existing radiotelescopes on Earth to look for short pulses of Cherenkov radiation in the GHz range emitted by showers induced just below the surface of the Moon when cosmic rays or neutrinos strike it. We estimate the energy threshold of the technique and the effective aperture and volume of the Moon for this detection. We apply our calculation to obtain the expected event rates from the observed cosmic ray flux and several representative theoretical neutrino fluxes.'],['2001-02-12'] +258,['eng'],"['Kosowsky, A', 'Mack, A M', 'Kahniashvili, T A']",['Stochastic Gravitational Radiation from Phase Transitions'],['Astrophysics and Astronomy'],"['talk, Philadelphia 2000/10/30', 'gravitational radiation, stochastic', 'critical phenomena', 'bubble, interaction', 'turbulence', 'counters and detectors, satellite', 'laser, interference']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102169'],"['A stochastic background of gravitational radiation from cosmological processes in the very early Universe is potentially detectable. We review the gravitational radiation which may arise from cosmological phase transitions, covering both bubble collisions and turbulence as sources. Prospects for detecting a direct signal from the electroweak phase transition or other cosmological sources with a space-based laser interferometer are discussed.']",['2001-02-12'] +259,['eng'],"['Barkovich, M', 'Casini, H', ""D'Olivo, J C"", 'Montemayor, R']",['Pulsar motions from neutrino oscillations induced by a violation of the equivalence principle'],['Astrophysics and Astronomy'],"['pulsar', 'neutrino, oscillation', 'oscillation, length', 'resonance', 'equivalence principle, violation', 'neutrino, momentum', 'neutrino, angular momentum', 'anisotropy']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102157'],"['We analize a possible explanation of the pulsar motions in terms of resonant neutrino transitions induced by a violation of the equivalence principle (VEP). Our approach, based on a parametrized post-Newtonian (PPN) expansion, shows that VEP effects give rise to highly directional contributions to the neutrino oscillation length. These terms induce anisotropies in the linear and angular momentum of the emitted neutrinos, which can account for both the observed translational and rotational pulsar motions. The violation needed to produce the actual motions is completely compatible with the existing bounds.']",['2001-02-12'] +260,['eng'],"['Pina-Avelino, P', 'Esposito, S', 'Mangano, G', 'Martins, C J A P', 'Melchiorri, A', 'Miele, G', 'Pisanti, O', 'Rocha, G', 'Viana, P T P']",['Early-universe constraints on a time-varying fine structure constant'],['Astrophysics and Astronomy'],"['fundamental constant, fine structure', 'time variation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'baryon, density', 'light nucleus, production', 'astrophysics', 'data analysis method', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102144'],"['Recent high-resolution CMB anisotropy data seem to point to a value for the baryon density larger than what is predicted by Standard Big Bang Nucleosynthesis, ruling out a large set of standard cosmological models. However, present CMB data can be made compatible with a lower value for the baryon density if the fine-structure constant alpha was smaller in the past. In this letter we produce early-universe constraints on a time-varying alpha by a joint analysis of the latest CMB and BBN data. We find strong constraints on the variation of alpha from BBN, Delta alpha/alpha=(-7 \\pm 9)10^-3 (95% C.L.), marginally compatible with the CMB result, Delta alpha/alpha=-0.10 \\pm 0.05 (68 % C.L.). We conclude that the varying alpha scenario may still solve the CMB-BBN discrepancy, but that may require a non-monotonic red-shift behaviour for the fine structure constant']",['2001-02-09'] +261,['eng'],"['Alvarez-Muñiz, J', 'Halzen, Francis']",['10^20 eV Cosmic Ray and Particle Physics with IceCube'],['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'neutrino, cosmic radiation', 'topology, defect', 'astrophysics, model', 'postulated particle, heavy', 'neutrino, flux', 'neutrino, production', 'deep underground detector, proposed', 'water, solids', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102106'],"['We show that a kilometer-scale neutrino observatory, though optimized for detecting neutrinos of TeV to PeV energy, can reveal the science associated with the enigmatic super-EeV radiation in the Universe. Speculations regarding its origin include heavy relics from the early Universe, particle interactions associated with the Greisen cutoff, and topological defects which are remnant cosmic structures associated with phase transitions in grand unified gauge theories. We show that it is a misconception that new instruments optimized to EeV energy can exclusively do this important science. Because kilometer-scale neutrino telescopes such as IceCube can reject the atmospheric neutrino background by identifying the very high energy of the signal events, they have sensitivity over the full solid angle, including the horizon where most of the signal is concentrated. This is critical because upgoing neutrino-induced muons, considered in previous calculations, are absorbed by the Earth. Previous calculations have und erestimated the event rates of IceCube for EeV signals by over one order of magnitude.']",['2001-02-07'] +262,['eng'],"['Irina, D', 'Yu, K M']",['Decay of cosmological constant as Bose condensate evaporation'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'fundamental constant, decay', 'Higgs particle, condensation', 'energy, density', 'symmetry, spontaneously broken', 'vacuum state, stability', 'oscillation, coherence', 'inflationary universe']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102094'],"['We consider the process of decay of symmetric vacuum state as evaporation of a Bose condensate of physical Higgs particles, defined over asymmetric vacuum state. Energy density of their selfinteraction is identified with cosmological constant $\\Lambda$ in the Einstein equation. $\\Lambda$ decay then provides dynamical realization of spontaneous symmetry breaking. The effective mechanism is found for damping of coherent oscillations of a scalar field, leading to slow evaporation regime as the effective mechanism for $\\Lambda$ decay responsible for inflation without special fine-tuning of the microphysical parameters. This mechanism is able to incorporate reheating, generation of proper primordial fluctuations, and nonzero cosmological constant today.']",['2001-02-07'] +263,['eng'],"['Olinto, A V']",['The Origin of the Highest Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Caraguatatuba 2000/10/17', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'magnetic field, galaxy', 'cosmic radiation, energy spectrum', 'GZK effect', 'photon, cosmic radiation', 'p, cosmic radiation', 'cosmic radiation, primary', 'astrophysics, acceleration', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102077'],"['Contrary to expectations, several cosmic ray events with energies above $10^{20}$ eV have been observed. The flux of such events is well above the predicted Greisen-Zatsepin-Kuzmin cutoff due to the pion production (via the $\\Delta$ resonace) of extragalactic cosmic ray protons off the cosmic microwave background. In addition to the relatively high flux of events, the isotropic distribution of arrival directions and an indication of hadronic primaries strongly challenge all models proposed to resolve this puzzle. Models based on astrophysical accelerators need to invoke strong Galactic and extragalactic magnetic fields with specific properties which are yet to be observed, while models based on physics beyond the standard model of particle physics generally predict photon primaries contrary to experimental indications. The resolution of this puzzle awaits a significant increase in the data at these energies which will be provided by future experiments.']",['2001-02-06'] +264,['eng'],"['Hanhart, C', 'Pons, J A', 'Phillips, D R', 'Reddy, S']","[""The likelihood of GODs' existence""]",['Astrophysics and Astronomy'],"['supernova', 'energy loss', 'space-time, higher-dimensional', 'n, matter', 'Kaluza-Klein model, graviton', 'neutrino, emission', 'graviton, emission', 'temperature, dependence', 'many-body problem', 'bootstrap', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102063'],"['The existence of compact dimensions which are accessible only to gravity represents an intriguing possible solution to the hierarchy problem. At present the strongest constraint on the existence of such compact Gravity-Only Dimensions (GODs) comes from SN1987a. Here we report on the first self-consistent simulations of the early, neutrino-emitting phase of a proto-neutron star which include energy losses due to the coupling of the Kaluza-Klein modes of the graviton which arise in a world with GODs. We compare the neutrino signals from these simulations to that from SN1987a and use a rigorous probabilistic analysis to derive improved bounds for the radii of such GODs. We find that the possibility that there are two compact extra dimensions with radii larger than 0.66 $\\mu$m is excluded at the 95% confidence level---as is the possibility that there are three compact extra dimensions larger than 0.8 nm.']",['2001-02-06'] +265,['eng'],"['Bianco, C L', 'Ruffini, R J', 'Xue, S S']",['The elementary spike produced by a pure $e^+e^-$ pair-electromagnetic pulse from a Black Hole'],['Astrophysics and Astronomy'],"['black hole', 'electron positron, plasma', 'gamma ray burst', 'effect, relativistic', 'radiation, flux', 'fireball', 'radiation, energy spectrum', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102060'],"['In the framework of the model that uses black holes endowed with electromagnetic structure (EMBH) as the energy source, we study how an elementary spike appears to the detectors. We consider the simplest possible case of a pulse produced by a pure $e^+e^-$ pair-electro-magnetic plasma, the PEM pulse, in the absence of any baryonic matter. The resulting time profiles show a {\\em Fast-Rise-Exponential-Decay} shape, followed by a power-law tail. This is obtained without any special fitting procedure, but only by fixing the energetics of the process taking place in a given EMBH of selected mass, varying in the range from 10 to $10^3$ $M_\\odot$ and considering the relativistic effects to be expected in an electron-positron plasma gradually reaching transparency. Special attention is given to the contributions from all regimes with Lorentz $\\gamma$ factor varying from $\\gamma=1$ to $\\gamma=10^4$ in a few hundreds of the PEM pulse travel time. Although the main goal of this paper is to obtain the elementary spike intensity as a function of the arrival time, and its observed duration, some qualitative considerations are also presented regarding the expected spectrum and on its departure from the thermal one. The results of this paper will be comparable, when data will become available, with a subfamily of particularly short GRBs not followed by any afterglow. They can also be propedeutical to the study of longer bursts in presence of baryonic matter currently observed in GRBs.']",['2001-02-06'] +266,['eng'],"['Harada, T', 'Carr, B J', 'Goymer, C A']",['Gravitational Memory ? - a Perturbative Approach'],['Astrophysics and Astronomy'],"['talk, Osaka 2000/09/10', 'gravitation, fundamental constant', 'space-time, Robertson-Walker', 'Brans-Dicke model', 'black hole']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102058'],"[""It has been pointed out that the value of the gravitational ``constant'' in the early universe may be different from that at present. In that case, it was conjectured that primordial black holes may ``remember'' the value of the gravitational constant in the early universe. The present analysis shows that this is not the case, at least in certain contexts.""]",['2001-02-06'] +267,['eng'],"['Carmeli, M', 'Kuzmenko, T Y']",['Value of the Cosmological Constant'],['Astrophysics and Astronomy'],"['talk, Austin 2000/12/10', 'astrophysics, fundamental constant', 'astrophysics, model', 'dark energy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102033'],['The numerical value of the cosmological constant is calculated using a recently suggested cosmological model and found to be 2.036 x 10^(-35) s^(-2). This value of the cosmological constant is in excellent agreement with the measurements recently obtained by the High-Z Supernova Team and the Supernova Cosmology Project.'],['2001-02-05'] +268,['eng'],"['Gangui, A']",['In Support of Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'horizon, acoustic', 'expansion, multipole', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102032'],"['The cosmic microwave background (CMB) provides a snapshot of the early Universe when matter began to become structured and has been the focus of several recent observational campaigns. In this Perspective, we discuss the results from these campaigns, which provide support for inflationary models of the Universe.']",['2001-02-05'] +269,['eng'],"['Pons, J A', 'Steiner, A W', 'Prakash, M', 'Lattimer, J M']",['EVOLUTION OF PROTO-NEUTRON STARS WITH KAON CONDENSATES'],['Astrophysics and Astronomy'],"['n, matter', 'neutrino, cosmic radiation', 'neutrino, flux', 'black hole', 'quark, strangeness', 'hyperon, condensation', 'K, condensation', 'baryon, density', 'matter, stability', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102015'],"['Neutrino fluxes from proto-neutron stars with and without quarks are studied. Observable differences become apparent after 10--20 s of evolution. Sufficiently massive stars containing negatively-charged, strongly interacting, particles collapse to black holes during the first minute of evolution. Since the neutrino flux vanishes when a black hole forms, this is the most obvious signal that quarks (or other types of strange matter) have appeared. The metastability timescales for stars with quarks are intermediate between those containing hyperons and kaon condensates.']",['2001-02-02'] +270,['eng'],"['Wick, S D', 'Kephart, T W', 'Weiler, Thomas J']",['Signature Studies of Cosmic Magnetic Monopoles'],['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'magnetic monopole, relativistic', 'magnetic field', 'energy loss', 'magnetic monopole, mass', 'magnetic monopole, flux', 'magnetic monopole, acceleration', 'radiation, Cherenkov', 'baryon, monopole', 'showers, air', 'electromagnetic interaction', 'geophysics', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0102002'],"['This talk explores the possibility that the Universe may be populated with relic magnetic monopoles. Observations of galactic and extragalactic magnetic fields, lead to the conclusion that monopoles of mass < 10^{14} GeV are accelerated in these fields to relativistic velocities. The relativistic monopole signatures and features we derive are (i) the protracted shower development, (ii) the Cherenkov signals, (iii) the tomography of the Earth with monopoles, and (iv) a model for monopole airshowers above the GZK cutoff.']",['2001-02-02'] +271,['eng'],"['Steiner, A W', 'Prakash, M', 'Lattimer, J M']",['Diffusion of Neutrinos in Proto-Neutron Star Matter with Quarks'],['Astrophysics and Astronomy'],"['n, matter', 'nucleon, star', 'neutrino, diffusion', 'neutrino, opacity', 'quark, matter', 'neutrino nucleon, interaction', 'neutrino lepton, interaction', 'neutrino quark, interaction', 'cross section', 'neutrino, absorption', 'coupling constant, axial-vector', 'coupling constant, vector', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101566'],"[""Neutrino opacities important in the evolution of a proto-neutron star containing quark matter are studied. The results for pure quark matter are compared with limiting expressions previously derived, and are generalized to the temperatures, neutrino degeneracies and lepton contents encountered in a proto-neutron star's evolution. We find that the appearance of quarks in baryonic matter drastically reduces the neutrino opacity for a given entropy, the reduction being sensitive to the thermodynamic conditions in the mixed quark-hadron phase.""]",['2001-02-02'] +272,['eng'],"['Fargion, D']",['Tau Air-Showers Signature of Ultra High Energy Neutrinos'],['Astrophysics and Astronomy'],"['talk, Vulcano 2000/05/22', 'neutrino, cosmic radiation', 'neutrino/tau, flux', 'neutrino/e', 'neutrino/mu', 'cosmic radiation, particle source', 'astrophysics, missing-mass', 'photon, cosmic radiation', 'showers, air', 'showers, spatial distribution', 'multiplicity, high', 'neutrino nucleon, interaction', 'neutrino electron, interaction', 'charged current', 'tau, neutrinoproduction', 'neutrino, interference', 'mass difference, (neutrino/tau neutrino/mu)', 'neutrino, path length', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101565'],"['The discover of Ultra High Energy Neutrino of astrophysical nature may be already reached. Indeed upward and horizontal tau Air-showers emerging from the Earth crust or mountain chains offer the best and most powerful signal of Ultra High Energy UHE neutrinos nu_tau}, bar\\nu_tau and bar{\\nu}_e at PeV and higher energy. The multiplicity in tau Air-showers secondary particles,N_{opt} =10^{12}, (E_tau}/ PeV, N_{\\gamma}= 10^8 E_tau/ PeV, N_{e^- e^+}= 2 10^7 E_tau/PeV, N_mu =3 10^5 (E_tau/PeV)^{0.85}, make easy its over-amplified discover. Indeed UHE nu_tau, following Super Kamiokande evidence of neutrino flavour mixing, should be as abundant as nu_mu. Also anti-neutrino electrons, bar{\\nu}_e, near the Glashow W resonance peak, E_{\\bar{\\nu_e}} = M^2_W / 2m_e, may generate tau Air-showers. Such horizontal tau air-showers by nu_{\\tau}-N and UHE bar\\nu_{e}-e at PeVs emerging from mountain high chain is one of the most power-full UHE neutrino imprint. Upward UHE nu_{\\tau}- N interaction on Earth crust at horizontal edge and from below, their consequent UHE tau air-showers beaming toward high mountains should flash gamma,mu,X and Cherenkov lights toward detectors located on the top of the mountains or on balloons. Such upward tau air-shower may hit also nearby satellite flashing them by short, hard, diluted gamma-burst at the edge of most sensitive Gamma Ray Observatory BATSE threshold. We identify already these rarest gamma events with recent (1994) discovered upward Terrestrial Gamma Flashes (TGF); we show their very probable UHE tau-UHE \\nu_\\tau origin. Partial TGF Galactic signature and known galactic and extra-galactic source location are discovered within known 47 TGF events at low, 2 10^{-3}, probability threshold.']",['2001-02-02'] +273,['eng'],"['Malik, K A']",['Cosmological Perturbations in an Inflationary Universe'],['Astrophysics and Astronomy'],"['thesis', 'inflationary universe', 'space-time, perturbation', 'perturbation, scalar', 'perturbation, vector', 'perturbation, tensor', 'dependence, gauge', 'space-time, Robertson-Walker', 'fluid', 'Einstein equation', 'Klein-Gordon equation', 'conservation law', 'spectra, perturbation', 'vacuum state, fluctuation', 'preheating', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101563'],"[""After introducing gauge-invariant cosmological perturbation theory we give an improved set of governing equations for multiple fluids including energy transfer. Having defined adiabatic and entropic perturbations we derive the ``conservation law'' for the curvature perturbation on large scales using only the energy conservation equation. We then investigate the dynamics of assisted inflation. By choosing an appropriate rotation in field space we can write down explicitly the potential for the weighted mean field along the scaling solution and for fields orthogonal to it. This allows us to present analytic solutions describing homogeneous and inhomogeneous perturbations about the attractor solution without resorting to slow-roll approximations. Finally we analyze the simplest model of preheating analytically, and show that in linear perturbation theory the effect of preheating on the amplitude of the curvature perturbation on large scales is negligible. We end with some concluding remarks, possible extensions and an outlook to future work.""]",['2001-02-02'] +274,['eng'],"['Lipari, P']","['The fluxes of sub--cutoff particles detected by AMS, the cosmic ray albedo and atmospheric neutrinos']",['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, flux', 'flux, ratio', 'geophysics, magnetic field', 'cosmic radiation, secondary radiation', 'neutrino, cosmic radiation', 'neutrino, flux', 'astrophysics', 'numerical calculations, Monte Carlo', 'magnetic spectrometer, satellite', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101559'],"['New measurements of the cosmic ray fluxes (p, e+, e- and Helium) performed by the Alpha Magnetic Spectrometer (AMS) during a ten days flight of space shuttle have revealed the existence of significant fluxes of particles below the geomagnetic cutoff. These fluxes exhibit a number of remarkable properties, such as a He-3/He-4 ratio of order ~10, an e+/e- ratio of order ~4 and production from well defined regions of the Earth that are distinct for positively and negatively charged particles. In this work we show that the natural hypothesis, that these subcutoff particles are generated as secondary products of primary cosmic ray interactions in the atmosphere can reproduce all the observed properties. We also discuss the implications of the subcutoff fluxes for the estimate of the atmospheric neutrino fluxes, and find that they represent a negligibly small correction. On the other hand the AMS results give important confirmations about the assumption of isotropy for the interplanetary cosmic ray fluxes also on large angular scales, and on the validity of the geomagnetic effects that are important elements for the prediction of the atmospheric neutrino fluxes.']",['2001-02-02'] +275,['eng'],"['Saavedra, O', 'Jones, L']",['Chacaltaya'],['Astrophysics and Astronomy'],"['talk, La Paz 2000/07/23', 'cosmic radiation, primary', 'energy spectrum, cosmic radiation', 'showers, air', 'cosmic radiation, flux', 'cosmic radiation, hadronic component', 'p, energy spectrum', 'hadron hadron, interaction', 'proposed experiment']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101554'],['Cosmic rays physics is currently being studied with rather sophisticated detectors running in a variety of experimental conditions and atmospheric depths around the world. In this paper we describe the reasons why cosmic ray physics experiments at high altitudes like Chacaltaya are so important for resolving some of the open problems in cosmic physics. A discussion on the future prospects of the high altitude mountain laboratories such as Chacaltaya for cosmic ray physics is presented.'],['2001-02-02'] +276,['eng'],"['Chimento, L P', 'Jakubi, A S', 'Zuccalá, N A']",['Quintessence dissipative superattractor cosmology'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'attractor', 'dissipation', 'quintessence', 'asymptotic behavior', 'supernova, luminosity', 'density, fluctuation', 'entropy, fluctuation', 'invariance, gauge', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101549'],"[""We investigate the simplest quintessence dissipative dark matter attractor cosmology characterized by a constant quintessence baryotropic index and a power-law expansion. We show that a class of accelerated coincidence--solving attractor solutions converge into this asymptotic behavior. Despite of its simplicity, such ``superattractor'' regime provides a model of the recent universe that also exhibits an excellent fit to supernovae luminosity observations and no age conflict. Our best fit gives $\\alpha=1.71\\pm 0.29$ for the power-law exponent. We calculate for this regime the evolution of density and entropy fluctuations.""]",['2001-02-02'] +277,['eng'],"['Bradbury, S M']",['Imaging Atmospheric Cerenkov Telescopes'],['Astrophysics and Astronomy'],"['talk, Tihany 2000/10/09', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'Cherenkov counter, imaging']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101533'],"['The hunt for cosmic TeV particle accelerators is prospering through Imaging Atmospheric Cerenkov Telescopes. We face challenges such as low light levels and MHz trigger rates, and the need to distinguish between particle air showers stemming from primary gamma rays and those due to the hadronic cosmic ray background. Our test beam is provided by the Crab Nebula, a steady accelerator of particles to energies beyond 20 TeV. Highly variable gamma-ray emission, coincident with flares at longer wavelengths, is revealing the particle acceleration mechanisms at work in the relativistic jets of Active Galaxies. These 200 GeV to 20 TeV photons propagating over cosmological distances allow us to place a limit on the infra-red background linked to galaxy formation and, some speculate, to the decay of massive relic neutrinos. Gamma rays produced in neutralino annihilation or the evaporation of primordial black holes may also be detectable. These phenomena and a zoo of astrophysical objects will be the targets of the next generation multi-national telescope facilities.']",['2001-01-31'] +278,['eng'],"['Chernin, A D']",['New appearance of cosmic coincidence problem'],['Astrophysics and Astronomy'],"['Friedman model', 'vacuum state, energy', 'energy, density', 'electroweak interaction', 'expansion, acceleration', 'symmetry']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101532'],['The integrals of the Friedmann cosmology equations are identified as constant physical characteristics for both vacuum and non-vacuum cosmic energies. The integrals are found to be numerically coincident. A model shows that the coincidence can naturally originate in the electroweak scale physics at TeV temperatures. The coincidence seems to reflect a new type of symmetry that relates vacuum and non-vacuum energies.'],['2001-01-31'] +279,['eng'],"['Abazajian, K N', 'Fuller, G M', 'Patel, M']","['Sterile Neutrino Hot, Warm, and Cold Dark Matter']",['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, sterile', 'neutrino, production', 'neutrino, mass', 'neutrino, mixing angle', 'lepton, asymmetry', 'lepton number', 'Boltzmann equation', 'astrophysics, missing-mass', 'energy loss', 'energy, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'MSW effect', 'finite temperature, effect', 'particle antiparticle, scattering', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101524'],"['We calculate the incoherent resonant and non-resonant scattering production of sterile neutrinos in the early universe. We find ranges of sterile neutrino masses, vacuum mixing angles, and initial lepton numbers which allow these species to constitute viable Hot, Warm, and Cold Dark Matter (HDM, WDM, CDM) candidates which meet observational constraints. The constraints considered here include energy loss in core collapse supernovae, energy density limits at big bang nucleosynthesis, and those stemming from sterile neutrino decay: limits from observed cosmic microwave background anisotropies, diffuse extragalactic background radiation, and Li-6/D overproduction. Our calculations explicitly include matter effects, both effective mixing angle suppression and enhancement (MSW resonance), as well as quantum damping. We for the first time properly include all finite temperature effects, dilution resulting from the annihilation/disappearance of relativistic degrees of freedom, and the scattering-rate-enhancing effects of particle-antiparticle pairs (muons, tauons, quarks) at high temperature in the early universe.']",['2001-01-31'] +280,['eng'],"['Terrero-Escalante, C A', 'Ayón-Beato, E', 'García, A']",['Inflationary scenarios with scale-invariant spectral tensorial index'],['Astrophysics and Astronomy'],"['inflationary universe', 'spectra, tensor', 'scaling, invariance', 'density, perturbation', 'gravitational radiation', 'cosmic radiation, background', 'cosmic radiation, spectra', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101522'],"['Next-to-leading order expressions related to Stewart-Lyth inverse problem are used to determine the inflationary models with tensorial power spectrum described by a scale-invariant spectral index. Beyond power-law inflation, solutions are characterized by scale dependent scalar indices. These models can be used as assumption on the generation of primordial perturbations to test for scale dependence of the scalar index at large angular scales. If such a dependence is detected, a nonzero contribution of gravitational waves to the CMB spectrum must be expected.']",['2001-01-31'] +281,['eng'],"['Kapusta, J I']",['Quark-Gluon Plasma in the Early Universe'],['Astrophysics and Astronomy'],"['talk, Erice 2000/12/06', 'astrophysics, model', 'quark gluon, plasma', 'quantum chromodynamics', 'critical phenomena', 'light nucleus, production', 'perturbation theory', 'lattice field theory', 'bubble, production', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101516'],"['A QCD phase transition in the early universe could have left inhomogeneities in the baryon to photon ratio and in isospin that might have affected nucleosynthesis later on. At very high temperature QCD plasma can be described by perturbation theory because of asymptotic freedom, but a possible phase transition requires a nonperturbative approach like lattice gauge theory. Assuming that a first order transition did occur, a dynamical set of equations can be solved to evolve the universe through it and to quantify the scale of inhomogeneity. Unfortunately this scale appears to be too small by two orders of magnitude to affect nucleosynthesis.']",['2001-01-30'] +282,['eng'],"['Voskresensky, D N']",['Neutrino Cooling of Neutron Stars. Medium effects'],['Astrophysics and Astronomy'],"['n, matter', 'neutrino, emission', 'nuclear matter, collective phenomena', 'model, liquid', 'nucleon nucleon, interaction', 'scattering amplitude', 'pi, exchange', 'pi, condensation', 'neutrino, opacity', 'propagator', 'color, superconducting', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101514'],"['This review demonstrates that neutrino emission from dense hadronic component in neutron stars is subject of strong modifications due to collective effects in the nuclear matter. With the most important in-medium processes incorporated in the cooling code an overall agreement with available soft X ray data can be easily achieved. With these findings so called ""standard"" and ""non-standard"" cooling scenarios are replaced by one general ""nuclear medium cooling scenario"" which relates slow and rapid neutron star coolings to the star masses (interior densities). In-medium effects take important part also at early hot stage of neutron star evolution decreasing the neutrino opacity for less massive and increasing for more massive neutron stars. A formalism for calculation of neutrino radiation from nuclear matter is presented that treats on equal footing one-nucleon and multiple-nucleon processes as well as reactions with resonance bosons and condensates. Cooling history of neutron stars with quark cores is also discussed.']",['2001-01-30'] +283,['eng'],"['Kak, S']","['Collapse, Expansion, and a Variable Speed of Light']",['Astrophysics and Astronomy'],"['quantum mechanics, wave function', 'coherent state', 'singularity', 'inflationary universe', 'photon, velocity', 'information theory', 'astrophysics, expansion', 'decoherence']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101455'],"[""This paper presents an information-theoretic view of how an observer within a quantum system will perceive his world. It is argued that because of the indistinguishability of quantum particles, a coherent state will appear to an observer within the system like a singularity. As superposition is lost, space appears to expand, although to the outsider it is merely the collapse of the wave function. Implications of these ideas to cosmology are considered. The superluminal expansion of space provides a basis to understand inflationary cosmologies. This expansion may be taken to be equivalent to a much faster speed of light during the inflationary period. These ideas can be tested by checking for `higher' speed of light from photons emitted by decohering atoms.""]",['2001-01-26'] +284,['eng'],"['Kanekar, N', 'Sahni, V', 'Shtanov, Yu V']",['Recycling the universe using scalar fields'],['Astrophysics and Astronomy'],"['astrophysics, oscillation', 'field theory, scalar', 'amplitude analysis', 'inflationary universe', 'chaos', 'entropy, production', 'matter, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101448'],"['We examine the behaviour of a closed oscillating universe filled with a homogeneous scalar field and find that, contrary to naive expectations, such a universe expands to larger volumes during successive expansion epochs. This intriguing behaviour introduces an arrow of time in a system which is time-reversible. The increase in the maximum size of the universe is closely related to the work done on/by the scalar field during one complete oscillatory cycle which, in turn, is related to the asymmetry in the scalar field equation of state during expansion and collapse. Our analysis shows that scalar fields with polynomial potentials $V(\\phi) = \\lambda \\phi^q$, $q > 1$ lead to a growing oscillation amplitude for the universe: the increase in amplitude between successive oscillations is more significant for smaller values of $q$. Such behaviour allows for the effective recycling of the universe. A recycled universe can be quite old and can resolve the flatness problem. These results have strong bearing on cosmological models in which the role of dark matter is played by a scalar field. They are also relevant for chaotic inflationary models of the early universe since they demonstrate that, even if the universe fails to inflate the first time around, it will eventually do so during future oscillatory cycles. Thus, the space of initial conditions favourable for chaotic inflation increases significantly.']",['2001-01-26'] +285,['eng'],"['Leach, S M', 'Sasaki, M', 'Wands, D', 'Liddle, A R']",['Enhancement of superhorizon scale inflationary curvature perturbations'],['Astrophysics and Astronomy'],"['inflationary universe', 'horizon', 'space-time, perturbation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101406'],"['We show that there exists a simple mechanism which can enhance the amplitude of curvature perturbations on superhorizon scales during inflation, relative to their amplitude at horizon crossing. The enhancement may occur even in a single-field inflaton model, and occurs if the quantity $a\\dot\\phi/H$ becomes sufficiently small, as compared to its value at horizon crossing, for some time interval during inflation. We give a criterion for this enhancement in general single-field inflation models.']",['2001-01-24'] +286,['eng'],"['Sikora, M', 'Madejski, G M']",['Blazars'],['Astrophysics and Astronomy'],"['review, Heidelberg 2000/06/26', 'blazar, model', 'jet, energy', 'energy, dissipation', 'particle, acceleration', 'radiation, production', 'synchrotron radiation', 'model, hadronic', 'Compton scattering', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101382'],"['In our review of the blazar phenomenon, we discuss blazar models, with a focus on the following issues: sub-parsec jets and their environment; energy dissipation and particle acceleration; and radiative processes.']",['2001-01-23'] +287,['eng'],"['Dova, M T']",['Future directions in astroparticle physics and the AUGER experiment'],['Astrophysics and Astronomy'],"['talk, Tihany 2000/10/09', 'astrophysics', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'showers, spatial distribution', 'shower detector', 'Cherenkov counter', 'counters and detectors, fluorescence', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101379'],"['The observation of cosmic ray particles with unexpected high energies is pushing astroparticle physics into a period of rapid progress both theoretically and experimentally. Different proposed models for the generation of these particles are constrained by the absence of the predicted GZK cutoff in the cosmic ray spectrum and by the composition and the distribution of arrival directions observed. The database increase due to the Pierre Auger Observatory will provide a clearer picture of the spectral anisotropy and properties of such high energy particles, enabling tests of their origin and nature.']",['2001-01-23'] +288,['eng'],"['Tegmark, M']",['Measuring the metric'],['Astrophysics and Astronomy'],"['dark energy', 'matter, density', 'space-time, geometry', 'supernova', 'gravitation, lens', 'galaxy, cluster', 'cosmic radiation, background', 'perturbation theory', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101354'],"[""We argue for a ``parametrized post-Friedmanian'' approach to linear cosmology, where the history of expansion and perturbation growth is measured without assuming that the Einstein Field Equations hold. As an illustration, a model-independent analysis of 92 type Ia supernovae demonstrates that the curve giving the expansion history has the wrong shape to be explained without some form of dark energy or modified gravity. We discuss how upcoming lensing, galaxy clustering, cosmic microwave background and Lyman alpha forest observations can be combined to carry though this program, which generalizes the quest for a dark energy equation of state, and forecast the accuracy that the proposed SNAP satellite can attain.""]",['2001-01-23'] +289,['eng'],"['Bento, M C', 'Bertolami, O', 'Rosenfeld, R', 'Teodoro, L']",['Self-Interacting Scalar Dark Matter and Higgs Decay'],['Astrophysics and Astronomy'],"['talk, Lisbon 2000/07/12', 'astrophysics, missing-mass', 'coupling, (Higgs particle scalar particle)', 'singlet, gauge', 'Higgs particle, decay']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101349'],"['Self-interacting dark matter has been suggested in order to overcome the difficulties of the Cold Dark Matter model on galactic scales. We argue that a scalar gauge singlet coupled to the Higgs boson, leading to an invisibly decaying Higgs, is an interesting candidate for this self-interacting dark matter particle.']",['2001-01-22'] +290,['eng'],"['Nagataki, S', 'Kohri, K']",['Rapid-Process Nucleosynthesis in Neutrino-Magneto-Centrifugally Driven Winds'],['Astrophysics and Astronomy'],"['light nucleus, production', 'magnetic field', 'neutrino, luminosity', 'matter, rotational', 'matter, mass', 'entropy', 'velocity', 'n, matter', 'supernova', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101347'],"['We have studied whether the rotation and magnetic fields in neutrino-driven winds can be key processes for the rapid-process (r-process) nucleosynthesis. We have examined the features of a steady and subsonic wind solutions which extend the model of Weber and Davis (1967), which is a representative solar wind model. As a result, we found that the entropy per baryon becomes lower and the dynamical timescale becomes longer as the angular velocity becomes higher. These results are inappropriate for the production of the r-process nuclei. As for the effects of magnetic fields, we found that a solution as a steady wind from the surface of the proto-neutron star can not be obtained when the strength of the magnetic field becomes $\\ge$ $10^{11}$ G. Since the magnetic field in normal pulsars is of order $10^{12}$ G, a steady wind solution might not be realized there, which means that the models in this study may not be adopted for normal proto-neutron stars. In this situation, we have little choice but to conclude that it is difficult to realize a successful r-process nucleosynthesis in the wind models in this framework.']",['2001-01-22'] +291,['eng'],"['Kampert, K H']",['Cosmic Rays and Particle Physics'],['Astrophysics and Astronomy'],"['talk, Bad Honnef 2000/09/25', 'astrophysics, model', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'astrophysics, missing-mass', 'antimatter', 'showers, air', 'hadron, energy spectrum', 'muon, flux', 'electron, flux', 'flux, ratio', 'cosmic radiation, particle source', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101331'],"['The study of high energy cosmic rays is a diversified field of observational and phenomenological physics addressing questions ranging from shock acceleration of charged particles in various astrophysical objects, via transport properties through galactic and extragalactic space, to questions of dark matter, and even to those of particle physics beyond the Standard Model including processes taking place in the earliest moments of our Universe. After decades of mostly independent evolution of nuclear-, particle- and high energy cosmic ray physics we find ourselves entering a symbiotic era of these fields of research. Some examples of interrelations will be given from the perspective of modern Particle-Astrophysics and new major experiments will briefly be sketched.']",['2001-01-19'] +292,['eng'],"['Schaefer, B M', 'Hofmann, W', 'Lampeitl, H', 'Hemberger, M']",['Particle Identification by Multifractal Parameters in Gamma-Astronomy with the HEGRA-Cherenkov-Telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'particle identification', 'data analysis method', 'expansion, wavelet', 'neural network']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101318'],"['Cherenkov images of air showers can also be classified using multifractal and wavelet parameters, as compared to the conventional Hillas image parameters. This technique was applied to the images recorded by the cameras of the stereoscopic imaging air Cherenkov-telescopes operated by the HEGRA collaboration. With respect to the identification of particles, the performance of multifractal and wavelet parameters was examined using a data sample from the observation of the active galaxy Mkn 501 that showed a high gamma-ray flux. The multifractal parameters were also combined with the Hillas parameters using a neural network approach in order to further improve the gamma/hadron-separation.']",['2001-01-19'] +293,['eng'],"['Razzaque, S', 'Seunarine, S', 'Besson, D Z', 'McKay, D W']",['Signal Characteristics from Electromagnetic Cascades in Ice'],['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'cosmic radiation', 'Cherenkov counter, water', 'solids, water', 'showers, electromagnetic', 'showers, beam profile', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101315'],"['We investigate the development of electromagnetic cascades in ice using a GEANT Monte Carlo simulation. We examine the Cherenkov pulse that is generated by the charge excess that develops and propagates with the shower. This study is important for the RICE experiment at the South Pole, as well as any test beam experiment which seeks to measure coherent Cherenkov radiation from an electromagnetic shower.']",['2001-01-19'] +294,['eng'],"['Mukherjee, R']",['Egret (GeV) Blazars'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'blazar', 'cosmic radiation, energy spectrum', 'quasar', 'cosmic radiation, background', 'counters and detectors, satellite', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101301'],"['The EGRET instrument on the Compton Gamma Ray Observatory (1991-2000) has positively detected high energy gamma-ray emission from more than 67 active galaxies of the blazar class. The majority of the EGRET blazars are flat-spectrum radio quasars, which are characterized by inferred isotropic luminosities often as high as 3E49 ergs/s. The remainder are BL Lac objects, some of which have been detected at TeV energies (> 250 GeV) by ground-based atmospheric Cherenkov telescopes. One of the remarkable characteristics observed in blazars is that the gamma-ray luminosity often dominates the bolometric power in these sources. The detection of blazars by EGRET has undoubtedly been one of the highlights of the mission, and has forever impacted upon our understanding of the emission mechanisms in these objects. In this article, we summarize the properties of EGRET blazars, and review the constraints that the EGRET observations place on the various models of gamma-ray production in these sources.']",['2001-01-18'] +295,['eng'],"['Kampert, K H']",['Methods of Determination of the Energy and Mass of Primary Cosmic Ray Particles at Extensive Air Shower Energies'],['Astrophysics and Astronomy'],"['talk, Lodz 2000/07/24', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, mass', 'showers, air', 'experimental methods', 'data analysis method', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101283'],"['Measurements of cosmic ray particles at energies above E = 5 x 10^{14} eV are performed by large area ground based air shower experiments. Only they provide the collection power required for obtaining sufficient statistics at the low flux levels involved. In this review we briefly outline the physics and astrophysics interests of such measurements and discuss in more detail various experimental techniques applied for reconstructing the energy and mass of the primary particles. These include surface arrays of particle detectors as well as observations of Cherenkov- and of fluorescence light. A large variety of air shower observables is then reconstructed from such data and used to infer the properties of the primary particles via comparisons to air shower simulations. Advantages, limitations, and systematic uncertainties of different approaches will be critically discussed.']",['2001-01-18'] +296,['eng'],"['Rooprai, N', 'Lohiya, D']",['Dynamically tuning away the cosmological constant in effective scalar tensor theories'],['Astrophysics and Astronomy'],"['gravitation, scalar', 'gravitation, tensor', 'astrophysics, fundamental constant', 'gravitation, fundamental constant', 'field theory, scalar', 'coupling', 'effective potential', 'tensor, energy-momentum', 'energy, density', 'soliton']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101280'],"[""It is known that the cosmological constant can be dynamically tuned to an arbitrary small value in classes of scalar tensor theories. The trouble with such schemes is that effective gravity itself vanishes. We explore the possibility of avoiding this ``no-go'' with a spatially varying effective gravity. We demonstrate this in principle with the non-minimally coupled scalar field having an additional coupling to a fermionic field. The expectation value of the scalar field gets anchored to a non-trivial value inside compact domains. But for the non-minimal coupling to the scalar curvature, these configurations are analogous to the non-topological solutions suggested by Lee and Wick. With non-minimal coupling, this leads to a peculiar spatial variation of effective gravity. As before, one can dynamically have the long distance (global) gravitational constant $G$ and ${\\Lambda}$, the cosmological constant, tending to zero. However, inside compact domains, $G$ can be held to a universal (non-vanishing) value. Long distance gravitational effects turn out to be indistinguishable from those expected of general theory of relativity (GTR). There are two ways in which the ensuing theory may lead to a viable effective gravity theory: (a) the compact domains could be of microscopic (sub-nuclear) size, or (b) the domains could be large enough to accommodate structures as large as a typical galaxy. Aspects of effective gravity and cosmology that follow are described. A toy Freidman - Robertson - Walker (FRW) model free from several standard model pathologies and characteristic features emerges.""]",['2001-01-18'] +297,['eng'],"['Hanauske, M', 'Satarov, L M', 'Mishustin, I N', 'Stöcker, H', 'Greiner, W']",['Strange quark stars within the Nambu-Jona-Lasinio model'],['Astrophysics and Astronomy'],"['matter, strangeness', 'quark, matter', 'Jona-Lasinio-Nambu model', 'coupling constant, vector', 'coupling constant, scalar', 'coupling constant, ratio', 'four-fermion interaction', 'critical phenomena', 'pressure', 'potential, chemical', 'baryon, density', 'n, matter', 'hadron, model', 'symmetry, chiral', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101267'],"['We investigate the properties of charge-neutral $\\beta$-equilibrium cold quark matter within the Nambu-Jona-Lasinio model. The calculations are carried out for different ratios of coupling constants characterizing the vector and scalar 4-fermion interaction, $\\xi\\equiv G_V/G_S$. It is shown that for $\\xi < 0.4$ matter is self-bound and for $\\xi < 0.65$ it has a first order phase transition of the liquid-gas type. The Gibbs conditions in the mixed phase are applied for the case of two chemical potentials associated with the baryon number and electric charge. The characteristics of the quark stars are calculated for $\\xi = 0, 0.5$ and 1. It is found that the phase transition leads to a strong density variation at the surface of these stars. For $\\xi = 1$ the properties of quark stars show behaviors typical for neutron stars. At $\\xi\\goo 0.4$ the stars near to the maximum mass have a large admixture of strange quarks in their interiors.']",['2001-01-17'] +298,['eng'],"['Vachaspati, T']",['Estimate of the primordial magnetic field helicity'],['Astrophysics and Astronomy'],"['astrophysics, model', 'magnetic field', 'helicity, density', 'baryon number, density', 'baryon, production', 'electroweak interaction', 'Chern-Simons term', 'decay, string', 'monopole']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101261'],['Electroweak baryogenesis proceeds via changes in the non-Abelian Chern-Simons number. It is argued that these changes generate the helicity of a primordial magnetic field. The average helicity density of the primordial magnetic field is then estimated to be given by ~10^2 n_b where n_b ~10^{-6} /cm^3 is the present cosmological baryon number density.'],['2001-01-17'] +299,['eng'],"['Quenby, J', 'Begley, A M A']",['Numerical Simulations Of Particle Acceleration In Relativistic Shocks With Application To AGN Central Engines'],['Astrophysics and Astronomy'],"['talk, Oxford 2000/08', 'plasma, gamma ray burst', 'cosmic radiation, acceleration', 'cosmic radiation, diffusion', 'shock waves, relativistic', 'cosmic radiation, energy spectrum', 'galaxy, AGN', 'black hole', 'photon p, interaction', 'neutrino, emission', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101247'],"['Numerical modelling is performed for extreme relativistic parallel shocks with upstream Lorentz factor Gamma=50. Assuming the scattering is either large angle or over pitch angles ~ Gamma^(-1), spectral flattening and shock aaceleration speed-up is found. The energy gain for the first shock cycle is ~ Gamma^2. The likely output from relativistic shocks due to the infall from the accretion disk to the AGN black hole is computed. Neutrinos from proton-gamma interactions may be detectable with planned neutrino telescopes but the gamma-ray output may contribute only 1/100 th of the observed 3C273 flux.']",['2001-01-16'] +300,['eng'],"['Meli, A', 'Quenby, J']",['Particle Spectra Of Ultra-Relativistic Shock Waves'],['Astrophysics and Astronomy'],"['talk, Lodz 2000/07', 'photon, cosmic radiation', 'cosmic radiation, acceleration', 'shock waves, relativistic', 'astrophysics, plasma', 'galaxy, AGN', 'cosmic radiation, gamma ray burst', 'cosmic radiation, diffusion', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101246'],['Numerical Monte Carlo simulations of the diffusive shock acceleration in the test particle limit are investigated. We simulate high relativistic flow astrophysical plasmas for upstream $\\gamma$ $\\sim5$ and up to $\\gamma$ $\\sim1000$. These gamma values are relevant to the diffusive shock acceleration models of Active Galactic Nuclei (AGN) and Gamma Ray Bursts (GRBs). The spectral shape for the above high relativistic processes will be calculated. This work presents distinctive spectral shapes with plateau-like characteristics due to the relativistic effects and the spectral indexes are found to be as flat as the flow becomes relativistic; the latter is in a very good agreement with previous theoretical and numerical works concerning relativistic plasma flows.'],['2001-01-16'] +301,['eng'],"['Meli, A', 'Quenby, J J']",['Particle Energy And Acceleration Efficiencies In Highly Relativistic Shocks'],['Astrophysics and Astronomy'],"['talk, Lodz 2000/07', 'photon, cosmic radiation', 'gamma ray burst', 'cosmic radiation, acceleration', 'astrophysics, plasma', 'shock waves, relativistic', 'particle, energy', 'time', 'cosmic radiation, diffusion', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101245'],"['In this paper we present an investigation of numerical Monte Carlo simulations of the diffusive shock acceleration in the test particle limit. Very high gamma flow astrophysical plasmas, have been used, from $\\gamma_{up}$ $\\sim50$ up to $\\gamma_{up}$ $\\sim1000$, which could be relevant to the suggested models of AGNs Jets and their Central Engines as well as the ultra-relativistic shock particle acceleration in Gamma Ray Burst (GRB) fireballs. Particularly the energy gain per shock crossing and the time constant for the above high relativistic processes is numerically calculated. We explicitly find a considerable $\\gamma^{2}$ energy boosting in the first shock cycle, and in all subsequent shock cycles the particle energy is multiplied by a large factor. Also a noted acceleration speed-up for the same acceleration process has been observed. Both of those results are connected with theoretical suggestions that a significant enhancement of the acceleration process is possible due to relativistic effects not present at lower plasma flow speeds. The acceleration speed-up and the mean energy-gain per shock cycle found could efficiently justify the theory of the origin of Ultra High Energy Cosmic Rays (UHECR) from the sites of GRBs.']",['2001-01-16'] +302,['eng'],"['Sihvola, E']",['Determination of Omega_b From Big Bang Nucleosynthesis in the Presence of Regions of Antimatter'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'baryon, density', 'antimatter, annihilation', 'helium, yield', 'lithium, yield', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101236'],"['Production of regions of antimatter in the early universe is predicted in many baryogenesis models. Small scale antimatter regions would annihilate during or soon after nucleosynthesis, affecting the abundances of the light elements. In this paper we study how the acceptable range in Omega_b changes in the presence of antimatter regions, as compared to the Standard Big Bang Nucleosynthesis (SBBN). It turns out that it is possible to produce at the same time both a low 4He value (Y_p < 0.240) and a low D/H value (D/H < 4e-5), but overproduction of 7Li is unavoidable at large Omega_b.']",['2001-01-16'] +303,['eng'],"['Engel, R', 'Stanev, T']",['Neutrinos from propagation of ultra-high energy protons'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'photon p, interaction', 'neutrino, photoproduction', 'neutrino, flux', 'cosmic radiation, flux', 'flux, ratio', 'neutrino, energy spectrum', 'astrophysics, model', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101216'],"['We present a calculation of the production of neutrinos during propagation of ultra-high energy cosmic rays from their astrophysical sources to us. Photoproduction interactions are modeled with the event generator SOPHIA that represents very well the experimentally measured particle production cross sections at accelerator energies. We give the fluxes expected from different assumptions on cosmic ray source distributions, cosmic ray injection spectra, cosmological evolution of the sources and different cosmologies, and compare them to the Waxman-Bahcall limit on source neutrinos. The ratio of the local high energy neutrino flux to the ultra-high energy cosmic ray flux is a crucial parameter in distinguishing between astrophysical and cosmological (top-down) scenarios of the ultra-high energy cosmic ray origin.']",['2001-01-16'] +304,['eng'],"['Collar, J I', 'Girard, T A', 'Limagne, D', 'Miley, H S', 'Morlat, T', 'Puibasset, J', 'Waysand, G']",['WIMP searches with superheated droplet detectors'],['Astrophysics and Astronomy'],"['talk, York 2000/09/18', 'astrophysics, missing-mass', 'WIMP, search for', 'counters and detectors, droplet', 'calibration', 'scattering, p WIMP', 'cross section', 'deep underground detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101176'],"['SIMPLE (Superheated Instrument for Massive ParticLE searches) employs superheated droplet detectors (SDDs) to search for Weakly Interacting Massive Particle (WIMP) dark matter. As a result of the intrinsic SDD insensitivity to minimum ionizing particles and high fluorine content of target liquids, competitive WIMP limits were already obtained at the early prototype stage. We comment here on the expected immediate increase in sensitivity of the program and on future plans to exploit this promising technnique.']",['2001-01-12'] +305,['eng'],"['Kirk, J G', 'Dendy, R O']",['Shock Acceleration of Cosmic Rays - a critical review'],['Astrophysics and Astronomy'],"['talk, Lodz 2000/07', 'cosmic radiation, acceleration', 'model, injection', 'particle, energy', 'supernova', 'shock waves', 'cosmic radiation, energy spectrum', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101175'],"['Motivated by recent unsuccessful efforts to detect the predicted flux of TeV gamma-rays from supernova remnants, we present a critical examination of the theory on which these predictions are based. Three crucial problems are identified: injection, maximum achievable particle energy and spectral index. In each case significant new advances in understanding have been achieved, which cast doubt on prevailing paradigms such as Bohm diffusion and single-fluid MHD. This indicates that more realistic analytical models, backed by more sophisticated numerical techniques should be employed to obtain reliable predictions. Preliminary work on incorporating the effects of anomalous transport suggest that the resulting spectrum should be significantly softer than that predicted by conventional theory.']",['2001-01-12'] +306,['eng'],"['Maartens, R', 'Tsagas, C G', 'Ungarelli, C']",['Magnetised gravitational waves'],['Astrophysics and Astronomy'],"['gravitational radiation, perturbation', 'perturbation, tensor', 'magnetic field, effect', 'cosmic radiation, anisotropy', 'cosmic radiation, background', 'energy, density']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101151'],"['We investigate the influence of cosmic magnetic fields on gravitational wave perturbations. We show that a large-scale magnetic field can generate large-scale non-decaying gravitational waves. In the general case where gravitational waves are generated by other mechanisms, a large-scale magnetic field introduces a new decaying tensor mode and modifies the non-decaying mode. This leads to a breaking of statistical isotropy, and the magnetic imprint on the tensor spectrum in principle provides a means of detecting a primordial field and limiting its strength.']",['2001-01-11'] +307,['eng'],"['Jernigan, J G']",['KiloHertz QPO and Gravitational Wave Emission as the Signature of the Rotation and Precession of a LMXB Neutron Star Near Breakup'],['Astrophysics and Astronomy'],"['n, matter', 'oscillation', 'pulsar', 'gravitational radiation, counters and detectors', 'interference, laser', 'energy, rotational', 'angular momentum', 'cosmic radiation, particle source', 'gamma ray burst', 'radiation, magnetic', 'proposed experiment', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101048'],"['The basic theory of torque free precession (TFP) of the outer crust of a neutron star (NS) as the signature of the approach to NS breakup is a viable explanation of the uniform properties of kHz Quasi-periodic Oscillations (QPO) observed in X-rays emitted by Low Mass X-ray Binary (LMXB) sources. The theory outlined in this paper relates the intrinsic properties of NS structure to the observed kHz frequencies. The range of kHz frequencies and the observed quality factors (Qs) are also explained by this simple dynamical model. A scenario that begins with the melting of the inner crust of an LMXB NS creates the conditions necessary for the generation of kHz QPO. The theory relates the ratio of the observed kHz frequencies to the ratios of the components of the moments of inertia of the NS, thereby tightly constraining the equation of state (EOS) of NS matter (polytrope index ~1.0). The TFP model is in strong contrast to existing models which primarily relate the kHz QPO phenomenon to the physics of gas dynamics near the inner edge of the accretion disk and the transition flow onto the surface of the NS. We suggest the possibility of the direct detection of very low frequency (~1 kHz) radio waves from magnetic dipole radiation and also predict kHz gravitational wave emission from the LMXB Sco X-1 that may be detectable by LIGO. The high accretion rates consistent with the predicted GW emission indicate the likely conversion of some LMXBs to maximally rotating Kerr black holes (BH) and further suggest that these systems are progenitors of some gamma-ray bursts (GRB).']",['2001-01-23'] +308,['eng'],"['Thompson, D J']",['Gamma Ray Pulsars'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'pulsar', 'photon, flux', 'photon, energy', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101039'],"['High-energy gamma rays are a valuable tool for studying particle acceleration and radiation in the magnetospheres of energetic pulsars. The six or more pulsars seen by CGRO/EGRET show that: the light curves usually have double-peak structures (suggesting a broad cone of emission); gamma rays are frequently the dominant component of the radiated power; and all the spectra show evidence of a high-energy turnover. Unless a new pulsed component appears at higher energies, progress in gamma-ray pulsar studies will be greatest in the 1-20 GeV range. Ground-based telescopes whose energy ranges extend downward toward 10 GeV should make important measurements of the spectral cutoffs. The Gamma-ray Large Area Space Telescope (GLAST), now in planning for a launch in 2005, will provide a major advance in sensitivity, energy range, and sky coverage.']",['2001-01-23'] +309,['eng'],"['Hofmann, W']",['How to focus a Cherenkov telescope'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'photoelectron, amplifier', 'Cherenkov counter, imaging', 'optics, beam focusing', 'optics, reflection', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101030'],"[""Cherenkov telescopes image the Cherenkov emission from air showers. A priori, it is not obvious if the `best' images are achieved by measuring Cherenkov photon angles, i.e. focusing the telescope at infinity, or by considering the air shower as an object to be imaged, in which case one might focus the telescope on the central region of the shower. The issue is addressed using shower simulations.""]",['2001-01-23'] +310,['eng'],"['Rudak, B']",['Neutron Stars as Sources of High Energy Particles - the case of RPP'],['Astrophysics and Astronomy'],"['talk, Meudon 2000/06/26', 'n, matter', 'charged particle, acceleration', 'pulsar, rotational', 'energy, rotational', 'charged particle, cosmic radiation', 'cosmic radiation, particle source', 'electric field', 'magnetic field', 'cosmic radiation, energy spectrum', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101138'],"['Highly magnetised rapidly spinning neutron stars are widely considered to be natural sites for acceleration of charged particles. Powerful acceleration mechanism due to unipolar induction is thought to operate in the magnetospheres of isolated neutron stars, bringing the particles to ultrarelativistic energies at the expense of the neutron star rotational energy, with inevitable emission of high energy photons. The aim of this review is to present basic ingredients of modern models of magnetospheric activity of rotation powered pulsars in the context of high-energy radiation from these objects. Several aspects of pulsar activity are addressed and related to spectacular results of pulsar observations with two major satellite missions of the past - CGRO and ROSAT. It is then argued that high sensitivity experiments of the future - GLAST, VERITAS and MAGIC - will be vital for a progress in our understanding of pulsar magnetospheric processes. In a conservative approach rotation powered pulsars are not expected to be the sources of UHE Cosmic Rays. However, several scenarios have been proposed recently to explain the UHECR events above the GZK limit with the help of acceleration processes in the immediate surrounding of newly born pulsars. Major features of these scenarios are reviewed along with references to contemporary models of magnetospheric activity.']",['2001-01-10'] +311,['eng'],"['Lindblom, L']",['Neutron Star Pulsations and Instabilities'],['Astrophysics and Astronomy'],"['lectures, Trieste 2000/06/05', 'n, matter', 'star, rotator', 'star, stability', 'gravitational radiation', 'angular momentum', 'temperature, dependence', 'effect, hydrodynamical', 'dissipation, effect', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101136'],"['Gravitational radiation (GR) drives an instability in certain modes of rotating stars. This instability is strong enough in the case of the r-modes to cause their amplitudes to grow on a timescale of tens of seconds in rapidly rotating neutron stars. GR emitted by these modes removes angular momentum from the star at a rate which would spin it down to a relatively small angular velocity within about one year, if the dimensionless amplitude of the mode grows to order unity. A pedagogical level discussion is given here on the mechanism of GR instability in rotating stars, on the relevant properties of the r-modes, and on our present understanding of the dissipation mechanisms that tend to suppress this instability in neutron stars. The astrophysical implications of this GR driven instability are discussed for young neutron stars, and for older systems such as low mass x-ray binaries. Recent work on the non-linear evolution of the r-modes is also presented.']",['2001-01-10'] +312,['eng'],"['Bertone, G', 'Sigl, G', 'Silk, J']",['Astrophysical Limits on Massive Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, annihilation', 'black hole, massive', 'electron, pair production', 'synchrotron radiation', 'magnetic field, galaxy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101134'],"['Annihilations of weakly interacting dark matter particles provide an important signature for the possibility of indirect detection of dark matter in galaxy halos. These self-annihilations can be greatly enhanced in the vicinity of a massive black hole. We show that the massive black hole present at the centre of our galaxy accretes dark matter particles, creating a region of very high particle density. Consequently the annihilation rate is considerably increased, with a large number of $e^+e^-$ pairs being produced either directly or by successive decays of mesons. We evaluate the synchrotron emission (and self-absorption) associated with the propagation of these particles through the galactic magnetic field, and are able to constrain the allowed values of masses and cross sections of dark matter particles.']",['2001-01-10'] +313,['eng'],"['Lee, W H']",['Simulations of black hole-neutron star binary coalescence'],['Astrophysics and Astronomy'],"['black hole', 'n, matter', 'binary, coalescence', 'gravitational radiation', 'back reaction', 'approximation, multipole', 'angular momentum', 'mass ratio', 'boundary condition', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101132'],"['We show the results of dynamical simulations of the coalescence of black hole-neutron star binaries. We use a Newtonian Smooth Particle Hydrodynamics code, and include the effects of gravitational radiation back reaction with the quadrupole approximation for point masses, and compute the gravitational radiation waveforms. We assume a polytropic equation of state determines the structure of the neutron star in equilibrium, and use an ideal gas law to follow the dynamical evolution. Three main parameters are explored: (i) The distribution of angular momentum in the system in the initial configuration, namely tidally locked systems vs. irrotational binaries; (ii) The stiffness of the equation of state through the value of the adiabatic index Gamma (ranging from Gamma=5/3 to Gamma=3); (iii) The initial mass ratio q=M(NS)/M(BH). We find that it is the value of Gamma that determines how the coalescence takes place, with immediate and complete tidal disruption for Gamma less than 2, while the core of the neutron star survives and stays in orbit around the black hole for Gamma=3. This result is largely independent of the initial mass ratio and spin configuration, and is reflected directly in the gravitational radiation signal. For a wide range of mass ratios, massive accretion disks are formed (M(disk)~0.2 solar masses), with baryon-free regions that could possibly give rise to gamma ray bursts.']",['2001-01-10'] +314,['eng'],"['Krennrich, F']",['TeV Gamma-Ray Astronomy in the new Millennium'],['Astrophysics and Astronomy'],"['review', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'astrophysics', 'supernova', 'galaxy', 'pulsar', 'blazar', 'cosmic radiation, energy spectrum', 'experimental results', 'proposed experiment', 'Cherenkov counter', 'counters and detectors, satellite', 'tables', 'bibliography', '>1000 GeV']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101120'],"['The field of TeV gamma-ray astronomy is reviewed with emphasis on its relation to the origin of cosmic rays. The discovery of TeV photons from supernova remnants and active galaxies has provided the first direct observational link between specific astrophysical objects and particle production at the TeV scale. TeV gamma-ray observations constrain the high end of the electromagnetic spectrum, a regime most sensitive for testing particle acceleration and emission models. TeV telescopes have made important contributions to the understanding of blazars and supernova remnants, however, it will take the next generation atmospheric Cherenkov telescopes and satellite-based gamma-ray detectors to unravel the mystery of hadronic cosmic-ray sources. A short review of TeV observations is followed by a discussion of the capabilities and scientific potential of the next generation ground-based atmospheric Cherenkov telescopes.']",['2001-01-10'] +315,['eng'],"['Wang, Y', 'Garnavich, P M']",['Measuring Time-Dependence of Dark Energy Density from Type Ia Supernova Data'],['Astrophysics and Astronomy'],"['supernova', 'dark energy, density', 'time dependence', 'astrophysics, fundamental constant', 'density, parametrization', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101040'],"['Observations of high redshift supernovae imply an accelerating Universe which can only be explained by an unusual energy component such as vacuum energy or quintessence. To assess the ability of current and future supernova data to constrain the properties of the dark energy, we allow its density to have arbitrary time-dependence, $\\rho_X(z)$. This leads to an equation of state for the dark energy, $w_X(z)=p_X(z)/\\rho_X(z)$, which is a free function of redshift $z$. We find that current type Ia supernova (SNe Ia) data are consistent with a cosmological constant, with large uncertainties at $z\\ga 0.5$. We show that $\\rho_X(z)/\\rho_X(z=0)$ can be measured reasonably well to about $z=1.5$ using type Ia supernova data from realistic future SN Ia pencil beam surveys, provided that the weak energy condition (energy density of matter is nonnegative for any observer) is imposed. While it is only possible to differentiate between different models (say, quintessence and k-essence) at $z \\la 1.5$ using realistic data, the correct trend in the time-dependence of the dark energy density can be clearly detected out to $z=2$, even in the presence of plausible systematic effects. This would allow us to determine whether the dark energy is a cosmological constant, or some exotic form of energy with a time-dependent density.']",['2001-01-23'] +316,['eng'],"['Rosner, Jonathan L', 'Suprun, D A']",['Extensive Air Shower Radio Detection'],['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'cosmic radiation', 'showers, air', 'electromagnetic field, measurement', 'background', 'signal processing', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101089'],"['A prototype system for detecting radio pulses associated with extensive cosmic ray air showers is described. Sensitivity is compared with that in previous experiments, and lessons are noted for future studies.']",['2001-01-08'] +317,['eng'],"['Kirilova, Daniela P', 'Chizhov, M V']",['Lepton asymmetry effect on neutrino oscillations and primordial He-4'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'neutrino, oscillation', 'neutrino, sterile', 'light nucleus, production', 'helium, yield', 'lepton, asymmetry', 'neutrino, mixing angle', 'neutrino, mass difference', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101083'],"['We analyze the effects of lepton asymmetry on neutrino oscillations and on cosmological nucleosynthesis with active-sterile oscillating neutrinos. It is shown that small lepton asymmetries, L < 0.01, whose direct kinetic effect on nucleosynthesis is negligible, still effect nucleosynthesis considerably through their influence on oscillating neutrinos. Two different cases of lepton asymmetry are discussed: an initially present and a dynamically generated in oscillations. Dynamically generated in resonant oscillations asymmetry at small mixing angles suppresses oscillations, hence, the nucleosynthesis bounds on neutrino mass differences at small mixings are relaxed. Initially present asymmetry may suppress or enhance oscillations. The enhancement is a result of interchanging resonances between neutrino and antineutrino ensembles due to resonance waves passing through the neutrino and antineutrino spectrum. Updated nucleosynthesis bounds on neutrino oscillation parameters accounting for lepton asymmetry are presented.']",['2001-01-08'] +318,['eng'],"['Stecker, F W']",['The Curious Adventure of the Ultrahigh Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Erice 2000/12/06', 'cosmic radiation, primary', 'showers, air', 'effect, Greisen-Zatsepin-Kuzmin', 'cosmic radiation, energy spectrum', 'gamma ray burst', 'cosmic radiation, particle source', 'nucleus, heavy', 'energy loss', 'grand unified theory', 'neutrino nucleus, interaction', 'cross section', 'new particle', 'symmetry breaking, Lorentz', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101072'],['These lectures discuss the mysteries involving the production and extragalactic propagation of ultrahigh energy cosmic rays and suggested possible solutions.'],['2001-01-23'] +319,['eng'],"['Ostrowski, M']",['Mechanisms and sites of ultra high energy cosmic ray origin'],['Astrophysics and Astronomy'],"['talk, Lodz 2000', 'cosmic radiation, acceleration', 'jet, relativistic', 'cosmic radiation, particle source', 'magnetic field', 'shock waves', 'n, matter', 'rotational', 'gamma ray burst', 'quasar']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101053'],"['We shortly discuss several astrophysical scenarios leading to cosmic ray acceleration up to extremely high energies reaching the scale of 10^{20} eV. The processes suggested in the literature include acceleration at relativistic jet terminal shocks and shear boundary layers, shocks in large scale accretion flows onto supergalactic cosmic structures, particle reflections from ultra-relativistic shocks postulated to exist in sources of gamma ray bursts, the processes involving the neutron star rotating magnetospheres and dormant quasars. Some of these objects can explain cosmic rays with highest energies if one tunes the model parameters to limits enabling the highest acceleration efficiency. We also note that some of the considered processes allow for acceleration efficiency in the Hillas diagram, beta, to be much larger than unity.']",['2001-01-23'] +320,['eng'],"[""D'Araújo, J C N"", 'Miranda, O D', 'Aguiar, O D']",['Possible Strong Gravitational Wave Sources for the LISA Antenna'],['Astrophysics and Astronomy'],"['gravitational radiation, particle source', 'black hole, massive', 'gamma ray burst', 'counters and detectors, interference', 'interference, laser', 'astrophysics, model', 'Hubble constant', 'matter, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101022'],"['Recently Fuller & Shi proposed that the gravitational collapse of supermassive objects ($M \\gtrsim 10^4M_\\odot$) could be a cosmological source of $\\gamma$-ray bursts (GRBs). The major advantage of their model is that supermassive object collapses are far more energetic than solar mass-scale compact mergers. Also, in their proposal the seeds of supermassive black holes (SMBHs) thus formed could give rise to the SMBHs observed at the center of many galaxies. We argue here that, besides the generation of GRBs, there could well occur a strong generation of gravitational waves (GWs) during the formation of SMBHs. As a result, the rate of such GW bursts could be as high as the rate of GRBs in the model by Fuller & Shi. In this case, the detection of GRBs and bursts of GWs should occur with a small time difference. We also argue that the GWs produced by the SMBHs studied here could be detected when the Laser Interferometric Space Antenna (LISA) becomes operative.']",['2001-01-23'] +321,['eng'],"['Sahni, V']",['Scalar field models for an accelerating universe'],['Astrophysics and Astronomy'],"['talk, Manchester 2000/08/07', 'field theory, scalar', 'quintessence', 'astrophysics, missing-mass', 'field theory, oscillation', 'supernova', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101016'],"['I describe a new class of quintessence+CDM models in which late time scalar field oscillations can give rise to both quintessence and cold dark matter. Additionally, a versatile ansatz for the luminosity distance is used to reconstruct the quintessence equation of state in a model independent manner from observations of high redshift supernovae.']",['2001-01-23'] +322,['eng'],"['Abramo, L R', 'Finelli, F']",['Attractors and Isocurvature Perturbations in Quintessence Models'],['Astrophysics and Astronomy'],"['quintessence', 'attractor', 'astrophysics, perturbation', 'energy, density', 'boundary condition']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101014'],"['We investigate the evolution of cosmological perturbations in scenarios with a quintessence scalar field, both analytically and numerically. In the tracking regime for quintessence, we find the long wavelength solutions for quintessential perturbations. We discuss the possibility of isocurvature modes generated by the quintessence sector and their impact on observations.']",['2001-01-23'] +323,['eng'],"['Xu, R X', 'Xu, X B', 'Wu, X J']",['The fastest rotating pulsar'],['Astrophysics and Astronomy'],"['pulsar, rotational', 'matter, strangeness', 'n, matter', 'matter, mass', 'magnetic field', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101013'],"['According to the observational limits on the radius and mass, PSR 1937+21 is probably a strange star, or some neutron star equations of state should be ruled out, if we alternatively suggest that a dipole magnetic field (rather than a quadrupole one) is relevant to its radio emission. It is conjectured that PSR 1937+21 and PSR 1257+12 (and possibly some or all of the isolated millisecond pulsars) may have weaker dynamo-originated magnetic field due to a less effective field magnification process.']",['2001-01-23'] +324,['eng'],"['Xu, R X', 'Busse, F H']",['The birth of strange stars and their dynamo-originated magnetic fields'],['Astrophysics and Astronomy'],"['matter, strangeness', 'star, production', 'magnetic field', 'supernova', 'n, matter', 'turbulence', 'energy, rotational', 'neutrino, velocity', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101011'],"['It is shown that protostrange stars can be convective, and there are two possible scenarios for turbulence. Besides the local turbulence on the scale which is less than the mean free path of neutrinos also large-scale (1 km) convection may occur with properties that are similar to those of convection in protoneutron stars. We thus suggest that strange stars can also create dynamo-originated magnetic fields during the deleptonization episode soon after a supernova explosion. Further detailed investigations are needed to see whether or not strange stars and neutron stars can be distinguished according to the differences in dynamo actions in strange quark matter and in neutron matter. The magnetic fields of strange stars and neutron stars may also behave very differently during the accretion-phase when the fields decay.']",['2001-01-23'] +325,['eng'],"['Dar, Arnon']","['Supernova, Hypernova and Gamma Ray Bursts']",['Astrophysics and Astronomy'],"['talk, College Park 2000/10/17', 'photon, cosmic radiation', 'gamma ray burst', 'jet, relativistic', 'supernova', 'cosmic radiation, energy spectrum', 'synchrotron radiation, emission', 'galaxy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101007'],"[""Recent observations suggest that gamma ray bursts (GRBs) and their afterglows are produced by highly relativistic jets emitted in core collapse supernova explosions (SNe). The result of the event, probably, is not just a compact object plus a spherical ejecta: within days, a fraction of the parent star falls back to produce a thick accretion disk around the compact object. Instabilities in the disk induce sudden collapses with ejection of highly relativistic ``cannonballs'' of plasma, similar to those ejected by microquasars. The jet of cannonballs exit the supernova shell/ejecta reheated by their collision with it, emitting highly forward-collimated radiation which is Doppler shifted to $\\gamma$-ray energy. Each cannonball corresponds to an individual pulse in a GRB. They decelerate by sweeping up the ionised interstellar matter in front of them, part of which is accelerated to cosmic-ray energies and emits synchrotron radiation: the afterglow. The Cannonball Model cannot predict the timing sequence of these pulses, but it fares very well in describing the total energy, energy spectrum, and time-dependence of the individual $\\gamma$-ray pulses and afterglows. It also predicts that GRB pulses are accompanied by detectable short pulses of TeV neutrinos and sub TeV $\\gamma$-rays, that are much more energetic and begin and peak a little earlier.""]",['2001-01-23'] +326,['eng'],"['Poghosyan, G', 'Grigorian, H', 'Blaschke, David B']",['Population clustering as a signal for deconfinement in accreting compact stars'],['Astrophysics and Astronomy'],"['matter, compact', 'rotational', 'mass, accretion', 'quark, matter', 'critical phenomena, confinement', 'baryon number', 'charge, electric', 'spin, time variation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0101002'],"[""We study the evolution of the rotation frequency of compact stars with mass accretion. The discontinuous change of the moment of inertia of a fastly rotating star due to the possible quark core appearance entails a characteristic change of spin evolution. Numerical solutions have been performed using a model equation of state describing the deconfinement phase transition as constrained by the conservation of total baryon number and electric charge. A phase diagram for compact stars in the angular velocity - baryon number plane is obtained with a dividing line for quark core configurations. Trajectories of spin evolution in this diagram are studied for different accretion scenarios defined by the initial mass and magnetic field of the star, the mass accretion rate and magnetic field decay time. We observe a characteristic increase in the ``waiting time'' when a configuration enters the quark core regime. Overclustering of the population of Z-sources of LMXBs in the phase diagram is suggested as a direct measurement of the critical line for the deconfinement phase transition since it is correlated to a maximum in the moment of inertia of the compact star.""]",['2001-01-23'] +327,['eng'],"['Gondek-Rosinska, D', 'Bulik, T', 'Kluzniak, W', 'Zdunik, J L', 'Gourgoulhon, E']",['Innermost stable circular orbits around rotating compact quark stars and QPOs'],['Astrophysics and Astronomy'],"['talk, Alicante 2000/09/04', 'quark, matter', 'rotational', 'orbit, stability', 'photon, cosmic radiation', 'cosmic radiation, flux', 'matter, strangeness', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012540'],"['It has been suggested that observations of quasi periodic oscillations (QPOs) in the X-ray fluxes from low mass X-ray binaries can be used to constrain the mass of the compact object and the equation of state of its matter. A specific suggestion that the kHz QPO frequency saturates at the maximum orbital frequency has been widely considered. We examine rotating compact stars described by a new model of strange quark matter (Dey et al. 1998). We calculate the maximum orbital frequencies for both normal and supramassive strange stars described by the Dey model, and present these frequencies for sequences of equilibrium models with constant baryon mass. The maximum orbital frequencies for these compact objects are always higher than the kHz QPO frequencies observed to date.']",['2001-01-01'] +328,['eng'],"['Spiering, C']",['Future High Energy Neutrino Telescopes'],['Astrophysics and Astronomy'],"['talk, Sudbury 2000/06/16', 'neutrino, cosmic radiation', 'Cherenkov counter, water', 'solids, water', 'deep underground detector, water', 'magnetic monopole, search for', 'WIMP, search for', 'counters and detectors, acoustic', 'showers, electromagnetic', 'deep underground detector, proposed', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012532'],['This talk summarizes the main physics goals and basic methods of telescopes for high energy neutrinos. It reviews the present status of deep underwater telescopes and sketches the ICECUBE project as an example for a cube kilometer detector. It is suggested to develop techniques for radio and acoustic detection hand in hand with big optical arrays. These large arrays should be complemented by medium-size detectors in the Megaton range.'],['2001-01-01'] +329,['eng'],"['Huterer, D', 'Turner, M S']",['Probing the dark energy'],['Astrophysics and Astronomy'],"['astrophysics', 'dark energy', 'energy, density', 'expansion, acceleration', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'supernova', 'galaxy, cluster', 'time variation', 'density, perturbation', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012510'],"['The presence of dark energy in the Universe is inferred directly from the accelerated expansion of the Universe, and indirectly, from measurements of cosmic microwave background (CMB) anisotropy. Dark energy contributes about 2/3 of the critical density, is very smoothly distributed, and has large negative pressure. Its nature is very much unknown. Most of its discernible consequences follow from its effect on evolution of the expansion rate of the Universe, which in turn affects the growth of density perturbations and the age of the Universe, and can be probed by the classical kinematic cosmological tests. Absent a compelling theoretical model (or even a class of models), we describe the dark energy by an effective equation-of-state w=p_X/\\rho_X which is allowed to vary with time. We describe and compare different approaches for determining w(t), including magnitude-redshift (Hubble) diagram, number counts of galaxies and clusters, and CMB anisotropy, focusing particular attention on the use of a sample of several thousand type Ia supernova with redshifts z\\lesssim 1.7, as might be gathered by the proposed SNAP satellite. Among other things, we derive optimal strategies for constraining cosmological parameters using type Ia supernovae. While in the near term CMB anisotropy will provide the first measurements of w, supernovae and number counts appear to have the most potential to probe dark energy.']",['2000-12-29'] +330,['eng'],"['Böhm, C', 'Fayet, Pierre', 'Schäffer, R']",['Constraining Dark Matter candidates from structure formation'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'fluctuation, adiabatic', 'energy loss', 'cross section', 'photon, decoupling', 'neutrino, decoupling', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012504'],"['We show that collisional damping of adiabatic primordial fluctuations yields stringent constraints on the possible range of mass and interaction rates of Dark Matter particles. Our analysis relies on a general classification of Dark Matter candidates, that we establish independently of any specific particle theory or model. We find that only Dark Matter candidates having cross-sections at decoupling smaller than $10^{-38} cm^2$ with photons and $10^{-40} cm^2$ with neutrinos can explain the observed primordial structures of $10^9$ Solar mass. These are severe constraints which may restrict or exclude even standard WIMP candidates like Supersymmetric particles. When just satisfied, they provide a natural place for Warm Dark Matter candidates. These damping constraints, on the other hand, leave open (less known) regions of parameter space corresponding to particles having rather high interaction rates, with other species than neutrinos and photons.']",['2000-12-28'] +331,['eng'],"['Dermer, C D']",['Maximum Particle Energy by Fermi Acceleration in Relativistic Flows'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'cosmic radiation, energy spectrum', 'fireball', 'gamma ray burst', 'resonance, stochastic', 'supernova', 'diffusion']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012490'],"['An expression for maximum accelerated particle energy E_max due to the first-order shock-Fermi process is generalized to relativistic flows. Given the Bohm diffusion approximation and a mean ISM magnetic field of 3 mu G, then E_max approx 8\\times 10^{15} \\beta_0 Z (m_odot/n_0)^{1/3} eV for an uncollimated explosion expanding into a uniform medium with density n_0. The initial flow speed of the explosion is \\beta_0 c, and the total ejecta energy, in Solar rest-mass energy units, is m_\\odot. Second-order stochastic processes in relativistic flows can accelerate cosmic rays to ultra-high energies. Sources of mildly relativistic or relativistic flows with adequate power, namely fireball transients and gamma-ray bursts, are proposed as the sources of cosmic rays near and above the knee of the cosmic-ray spectrum.']",['2000-12-25'] +332,['eng'],"['Jones, T W']",['Cosmic Particle Acceleration'],['Astrophysics and Astronomy'],"['talk, Taipei 1999', 'cosmic radiation, acceleration', 'cosmic radiation, particle source', 'energy spectrum, cosmic radiation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012483'],"['Cosmic-rays are ubiquitous, but their origins are surprisingly difficult to understand. A review is presented of some of the basic issues common to cosmic particle accelerators and arguments leading to the likely importance of diffusive shock acceleration as a general explanation. The basic theory of diffusive shock acceleration is outlined, followed by a discussion of some of the key issues that still prevent us from a full understanding of its outcomes. Some recent insights are mentioned at the end that may help direct ultimate resolution of our uncertainties.']",['2000-12-25'] +333,['eng'],"['Bertolami, O']",['Ultra-High Energy Cosmic Rays and Symmetries of Spacetime'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'cosmic radiation, acceleration', 'cosmic radiation, particle source', 'symmetry breaking, Lorentz']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012462'],"['High energy cosmic rays allow probing phenomena that are inacessible to accelerators. Observation of cosmic rays, presumebly protons, with energies beyond $4 \\times 10^{19} eV$, the so-called Greisen-Zatsepin-Kuzmin (GZK) cut-off, give origin to two puzzles: How do particles accelerate to such energies ? Are their sources within $50 - 100 Mpc$ from Earth, or Lorentz invariance is actually a broken symmetry ?']",['2000-12-22'] +334,['eng'],"['Singh, S', 'Devi, N C', 'Gupta, V K', 'Sen-Gupta, A', 'Anand, J D']",['Radial Oscillations of Rotating Strange Stars in Strong Magnetic Fields'],['Astrophysics and Astronomy'],"['matter, strangeness', 'rotational', 'star, oscillation', 'magnetic field, high', 'quark, mass', 'dependence, density', 'star, mass', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012427'],['In this paper we study radial oscillations of rotating strange stars in strong magnetic fields in the Density Dependent Quark Mass (DDQM) model. We see that increase of frequency i.e. difference in frequency of rotating and non-rotating stars is more for higher magnetic fields. The change is small for low mass stars but it increases with the mass of the star. This change of frequency is significant for maximum mass whereas it is marginal for a 1.4 solar mass star.'],['2000-12-21'] +335,['eng'],"['Aharonian, F A']",['Search for a TeV gamma-ray halo of Mkn 501'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, angular distribution', 'blazar', 'cosmic radiation, flux', 'upper limit', 'Cherenkov counter, imaging', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012401'],"['For distant extragalactic sources of gamma-rays in the PeV energy range, interactions of the gamma rays with intergalactic diffuse radiation fields will initiate a pair cascade. Depending on the magnetic fields in the vicinity of the source, the cascade can either result in an isotropic halo around an initially beamed source, or remain more or less collimated. Data recorded by the HEGRA system of imaging atmospheric Cherenkov telescopes are used to derive limits on the halo flux from the AGN Mrk 501. This is achieved by comparing the angular distribution of TeV gamma-rays during the 1997 burst phase -- where direct photons should dominate -- with the distribution during the 1998/99 quiescent state, where a steady-state halo contribution should be most pronounced. The results depend on the assumptions concerning the angular distribution of the halo; limits on the halo flux within 0.5 to 1 degr. from the source range between 0.1% and 1% of the peak burst flux.']",['2000-12-20'] +336,['eng'],"['Green, A M']",['A potential WIMP signature for the caustic ring halo model'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, search for', 'energy dependence', 'model, halo', 'time variation', 'recoil, energy', 'matter, velocity', 'density, local', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012393'],"[""Weakly Interacting Massive Particle (WIMP) direct detection event rate calculations usually rely on fairly simple, essentially static, analytic halo models. This is largely since the resolution of numerical simulations not yet being large enough to allow the full numerical calculation of the WIMP density and velocity distribution. In this paper we study the direct detection rate, in particular its energy dependence and annual modulation, for the caustic ring halo model. In this model, which uses simple assumptions to model the infall of dark matter onto the halo, the distribution of the cold dark matter particles at the Earth's location has a series of peaks in velocity space. We find that the sign of the annual modulation in the event rate changes as a function of recoil energy, providing a potentially distinctive experimental signal. We then compare the theoretical predictions of this models with the experimental signal found by the DAMA experiment. We find that the DAMA data allow less than $\\sim 30%$ of the local halo density to be in the form of velocity flows.""]",['2000-12-19'] +337,['eng'],"['Van der Swaluw, E', 'Achterberg, A', 'Gallant, Y A']",['Nonthermal X-ray emission from young Supernova Remnants'],['Astrophysics and Astronomy'],"['supernova', 'photon, cosmic radiation', 'photon, emission', 'cosmic radiation, acceleration', 'electron, cosmic radiation', 'model, hydrodynamical', 'synchrotron radiation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012385'],"['The cosmic-ray spectrum up to the knee ($E\\sim 10^{15}$ eV) is attributed to acceleration processes taking place at the blastwaves which bound supernova remnants. Theoretical predictions give a similar estimate for the maximum energy which can be reached at supernova remnant shocks by particle acceleration. Electrons with energies of the order $\\sim 10^{15}$ eV should give a nonthermal X-ray component in young supernova remnants. Recent observations of SN1006 and G347.3-0.5 confirm this prediction. We present a method which uses hydrodynamical simulations to describe the evolution of a young remnant. These results are combined with an algorithm which simultaneously calculates the associated particle acceleration. We use the test particle approximation, which means that the back-reaction on the dynamics of the remnant by the energetic particles is neglected. We present synchrotron maps in the X-ray domain, and present spectra of the energies of the electrons in the supernova remnant. Some of our results can be compared directly with earlier semi-analytical work on this subject by Reynolds [1].']",['2000-12-19'] +338,['eng'],"['Bordes, J', 'Chan, H M', 'Tsou, S T']",['Suggestions for Identifying the Primary of Post-GZK Air Showers'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'showers, air', 'cross section', 'angular dependence', 'energy dependence', 'p, showers', 'nucleus, showers', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012384'],"[""A procedure is suggested for systematically narrowing the choice of possible primaries for (UHECR) air showers with energies beyond the Greisen-Zatsepin-Kuz'min cut-off of $4 \\times 10^{19} eV$.""]",['2000-12-19'] +339,['eng'],"['Thuan, T X', 'Izotov, Yu I']",['Big Bang nucleosynthesis and the baryonic content of the universe'],['Astrophysics and Astronomy'],"['talk, Hanoi 2000/07/18', 'astrophysics, model', 'light nucleus, production', 'light nucleus, yield', 'galaxy', 'neutrino, flavor', 'density', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012382'],"[""A review of the latest measurements of the primordial abundances of the light nuclei D, 3He, 4He and 7Li is given. We discuss in particular the primordial abundance Yp of 4He as measured in blue compact dwarf galaxies. We argue that the best measurements now give a ``high'' value of Yp along with a ``low'' value of D/H, and that the two independent measurements are consistent within the framework of standard Big Bang nucleosynthesis with a number of light neutrino species Nnu = 3.0+/-0.3 (2sigma).""]",['2000-12-19'] +340,['eng'],"['Bergström, L', 'Edsjö, J', 'Gunnarsson, C']",['Neutralino Gamma-ray Signals from Accreting Halo Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'galaxy', 'photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, yield', 'neutralino, annihilation', 'supersymmetry', 'many-body problem', 'cluster', 'counters and detectors, proposed', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012346'],"[""There is mounting evidence that a self-consistent model for particle cold dark matter has to take into consideration spatial inhomogeneities on sub-galactic scales seen, for instance, in high-resolution N-body simulations of structure formation. Also in more idealized, analytic models, there appear density enhancements in certain regions of the halo. We use the results from a recent N-body simulation of the Milky Way halo and investigate the gamma-ray flux which would be produced when a specific dark matter candidate, the neutralino, annihilates in regions of enhanced density. The clumpiness found on all scales in the simulation results in very strong gamma-ray signals which seem to already rule out some regions of the supersymmetric parameter space, and would be further probed by upcoming experiments, such as the GLAST gamma-ray satellite. As an orthogonal model of structure formation, we also consider Sikivie's simple infall model of dark matter which predicts that there should exist continuous regions of enhanced density, caustic rings, in the dark matter halo of the Milky Way. We find, however, that the gamma-ray signal from caustic rings is generally too small to be detectable.""]",['2000-12-18'] +341,['eng'],"['Inoue, Y', 'Namba, T', 'Moriyama, S', 'Minowa, M', 'Takasu, Y', 'Horiuchi, T', 'Yamamoto, A']",['Recent results from the Tokyo axion helioscope experiment'],['Astrophysics and Astronomy'],"['talk, York 2000/09/18', 'axion, solar', 'axion, search for', 'coupling, (axion 2photon)', 'experimental methods', 'magnetic detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012338'],['We have searched for axions which could have been produced in the solar core using an axion helioscope with a 2.3m-long 4T superconducting magnet. Axion mass region up to m_a=0.26eV was newly explored by introducing dispersion-matching gas. Preliminary analysis sets a limit on axion-photon coupling constant to be less than (6.4--9.6)e-10 GeV^{-1} (95%CL) for this mass region from the absence of the axion signal. This is more stringent than the limit inferred from the solar age consideration and also more stringent than the recent helioseismological bound.'],['2000-12-18'] +342,['eng'],"['Strobel, K', 'Weigel, M K']",['On the minimum and maximum mass of neutron stars and the delayed collapse'],['Astrophysics and Astronomy'],"['n, matter', 'matter, mass', 'hyperon', 'black hole, production', 'meson, condensation', 'pressure', 'baryon number, density', 'baryon, mass difference', 'nuclear matter', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012321'],"['The minimum and maximum mass of protoneutron stars and neutron stars are investigated. The hot dense matter is described by relativistic (including hyperons) and non-relativistic equations of state. We show that the minimum mass ($\\sim$ 0.88 - 1.28 $M_{\\sun}$) of a neutron star is determined by the earliest stage of its evolution and is nearly unaffected by the presence of hyperons. The maximum mass of a neutron star is limited by the protoneutron star or hot neutron star stage. Further we find that the delayed collapse of a neutron star into a black hole during deleptonization is not only possible for equations of state with softening components, as for instance, hyperons, meson condensates etc., but also for neutron stars with a pure nucleonic-leptonic equation of state.']",['2000-12-15'] +343,['eng'],"['Maeda, K I']",['Brane Quintessence'],['Astrophysics and Astronomy'],"['astrophysics, model', 'Randall-Sundrum model', 'membrane model', 'quintessence', 'energy, density', 'attractor']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012313'],"['We propose a new quintessence scenario in the brane cosmology, assuming that a quintessence field $Q$ is confined in our 3-dimensional brane world. With a potential $V(Q)= \\mu^{\\alpha+4} Q^{-\\alpha}~(\\alpha\\geq 2)$, we find that the density parameter of the scalar field decreases as $\\Omega_Q \\sim a^{-4(\\alpha-2)/(\\alpha+2)}$ in the epoch of quadratic energy density dominance, if $\\alpha\\leq 6$. This attractor solution is followed by the usual tracking quintessence scenario after a conventional Friedmann universe is recovered. With an equipartition of initial energy density, we find a natural and successful quintessence model for $\\alpha\\gsim 4$.']",['2000-12-15'] +344,['eng'],"['Gnedin, O Yu', 'Yakovlev, D G', 'Potekhin, A Yu']",['Thermal Relaxation in Young Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'superfluid', 'temperature', 'neutrino, emission', 'dependence, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012306'],"['The internal properties of the neutron star crust can be probed by observing the epoch of thermal relaxation. After the supernova explosion, powerful neutrino emission quickly cools the stellar core, while the crust stays hot. The cooling wave then propagates through the crust, due to its finite thermal conductivity. When the cooling wave reaches the surface (age 10-100 yr), the effective temperature drops sharply from 250 eV to 30 or 100 eV, depending on the cooling model. The crust relaxation time is sensitive to the (poorly known) microscopic properties of matter of subnuclear density, such as the heat capacity, thermal conductivity, and superfluidity of free neutrons. We calculate the cooling models with the new values of the electron thermal conductivity in the inner crust, based on a realistic treatment of the shapes of atomic nuclei. Superfluid effects may shorten the relaxation time by a factor of 4. The comparison of theoretical cooling curves with observations provides a potentially powerful method of studying the properties of the neutron superfluid and highly unusual atomic nuclei in the inner crust.']",['2000-12-15'] +345,['eng'],"['Dimopoulos, K']",['Towards a model of Quintessential Inflation'],['Astrophysics and Astronomy'],"['talk, San Feliu de Guixols 2000/09/30', 'inflationary universe', 'quintessence']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012298'],"['A model of quintessential inflation is presented, which manages to achieve the requirements of both inflation and quintessence with natural values of the mass-scales and parameters.']",['2000-12-14'] +346,['eng'],"['Mangano, G', 'Melchiorri, A', 'Pisanti, O']","['Primordial Nucleosynthesis, Cosmic Microwave Background and Neutrinos']",['Astrophysics and Astronomy'],"['talk, Otranto 2000/09/09', 'light nucleus, production', 'light nucleus, yield', 'cosmic radiation, background', 'microwaves, cosmic radiation', 'cosmic radiation, anisotropy', 'neutrino, flavor', 'potential, chemical', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012291'],"['We report the results of a recent likelihood analysis combining the primordial nucleosynthesis and the BOOMERanG and MAXIMA-1 data on cosmic microwave background radiation anisotropies. We discuss the possible implications for relic neutrino background of a high value for the baryonic matter content of the universe, larger than what is expected in a standard nucleosynthesis scenario.']",['2000-12-14'] +347,['eng'],"['Bai, X']",['WIMP searches with AMANDA-B10'],['Astrophysics and Astronomy'],"['talk, York 2000/09/18', 'WIMP, search for', 'WIMP, annihilation', 'neutrino, angular distribution', 'neutrino, cosmic radiation', 'muon, cosmic radiation', 'cosmic radiation, flux', 'deep underground detector, AMANDA', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012285'],"['We report on the search for nearly vertical up-going muon neutrinos from WIMP annihilations in the center of the Earth with the AMANDA-B10 detector. The whole data sample collected in 1997, 10^9 events, has been analyzed and a final sample of 15 up-going events is found in a restricted zenith angular region where a signal from WIMP annihilations is expected. A preliminary upper limit at 90% confidence level on the annihilation rate of WIMPs in the center of the Earth is presented.']",['2000-12-14'] +348,['eng'],"['Barriga, J', 'Gaztañaga, E', 'Santos, M G', 'Sarkar, S']",['Evidence for an inflationary phase transition from the LSS and CMB anisotropy data'],['Astrophysics and Astronomy'],"['talk, San Feliu de Guixols 2000/09/30', 'inflationary universe', 'symmetry, spontaneously broken', 'scaling, violation', 'galaxy', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012284'],"[""In the light of the recent Boomerang and Maxima observations of the CMB which show an anomalously low second acoustic peak, we reexamine the prediction by Adams et al (1997) that this would be the consequence of a 'step' in the primordial spectrum induced by a spontaneous symmetry breaking phase transition during primordial inflation. We demonstrate that a deviation from scale-invariance around $k\\sim0.1h$~Mpc$^{-1}$ can simultaneously explain both the feature identified earlier in the APM galaxy power spectrum as well the recent CMB anisotropy data, with a baryon density consistent with the BBN value. Such a break also allows a good fit to the data on cluster abundances even for a critical density matter-dominated universe with zero cosmological constant.""]",['2000-12-14'] +349,['eng'],"['Postma, M']","['""Signature"" neutrinos from photon sources at high redshift']",['Astrophysics and Astronomy'],"['talk, Los Angeles 2000/11/16', 'photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, particle source', 'photon electron, interaction', 'muon, pair production', 'pi, pair production', 'muon, leptonic decay', 'pi, leptonic decay', 'neutrino, flux', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012279'],"[""The temperature of the cosmic microwave background increases with redshift; at sufficiently high redshift it becomes possible for ultrahigh-energy photons and electrons to produce muons and pions through interactions with background photons. At the same time, energy losses due to interactions with radio background and intergalactic magnetic fields are negligible. The energetic muons and pions decay, yielding a flux of ``signature'' neutrinos with energies $E_\\nu \\sim 10^{17}$eV. Detection of these neutrinos can help understand the origin of ultrahigh-energy cosmic rays.""]",['2000-12-13'] +350,['eng'],"['Gupta, V K', 'Sen-Gupta, A', 'Singh, S', 'Anand, J D']",['Effect of Magnetic Field on the Phase Transition from Nuclear Matter to Quark Matter during Proto-Neutron Star Evolution'],['Astrophysics and Astronomy'],"['n, matter', 'critical phenomena', 'hadron, matter', 'quark, matter', 'transition, quark hadron', 'magnetic field, effect', 'neutrino/e, potential', 'finite temperature', 'quark, mass', 'dependence, density', 'mean field approximation, relativistic', 'energy, density', 'supernova', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012260'],['We have studied phase transition from hadron matter to quark matter in the presence of high magnetic fields incorporating the trapped electron neutrinos at finite temperatures. We have used the density dependent quark mass (DDQM) model for the quark phase while the hadron phase is treated in the frame-work of relativistic mean field theory. It is seen that the nuclear energy at phase transition decreases with both magnetic field and temperature. A brief discussion of the effect of magnetic field in supernova explosions and proto-neutron star evolution is given.'],['2000-12-13'] +351,['eng'],"['Fiorentini, G', 'Ricci, B', 'Villante, F L']",['Helioseismology and solar neutrinos'],['Astrophysics and Astronomy'],"['review, San Feliu de Guixols 2000/09/30', 'neutrino, solar', 'model, solar', 'neutrino, flux', 'beryllium', 'nuclear reaction, screening', 'velocity, acoustic', 'helium, nuclide', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012239'],"['We review recent advances concerning helioseismology, solar models and solar neutrinos. Particularly we address the following points: i) helioseismic tests of recent SSMs; ii) predictions of the Beryllium neutrino flux based on helioseismology; iii) helioseismic tests regarding the screening of nuclear reactions in the Sun.']",['2000-12-12'] +352,['eng'],"['Bergström, L', 'Damour, Thibault Marie Alban Guillaume', 'Edsjö, J', 'Krauss, L M', 'Ullio, P']",['A new population of WIMPs in the solar system and indirect detection rates'],['Astrophysics and Astronomy'],"['talk, York 2000/09/18', 'astrophysics, missing-mass', 'WIMP, search for', 'matter, solar', 'neutralino', 'supersymmetry', 'WIMP, velocity', 'WIMP, capture', 'muon, flux', 'WIMP, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012235'],"['A new Solar System population of Weakly Interacting Massive Particle (WIMP) dark matter has been proposed to exist. We investigate the implications of this population on indirect signals in neutrino telescopes (due to WIMP annihilations in the Earth) for the case when the WIMP is the lightest neutralino of the MSSM, the minimal supersymmetric extension of the standard model. The velocity distribution and capture rate of this new population is evaluated and the flux of neutrino-induced muons from the center of the Earth in neutrino telescopes is calculated. We show that the effects of the new population can be crucial for masses around 60-120 GeV, where enhancements of the predicted muon flux from the center of the Earth by up to a factor of 100 compared to previously published estimates occur. As a result of the new WIMP population, neutrino telescopes should be able to probe a much larger region of parameter space in this mass range.']",['2000-12-12'] +353,['eng'],"['Gondolo, P', 'Edsjö, J', 'Bergström, L', 'Ullio, P', 'Baltz, E A']",['DarkSUSY - A numerical package for dark matter calculations in the MSSM'],['Astrophysics and Astronomy'],"['talk, York 2000/09/18', 'astrophysics, missing-mass', 'supersymmetry', 'neutralino, density', 'neutralino, annihilation', 'programming']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012234'],"['The question of the nature of the dark matter in the Universe remains one of the most outstanding unsolved problems in basic science. One of the best motivated particle physics candidates is the lightest supersymmetric particle, assumed to be the lightest neutralino. We here describe DarkSUSY, an advanced numerical FORTRAN package for supersymmetric dark matter calculations which we release for public use. With the help of this package, the masses and compositions of various supersymmetric particles can be computed, for given input parameters of the minimal supersymmetric extension of the Standard Model (MSSM). For the lightest neutralino, the relic density is computed, using accurate methods which include the effects of resonances, pair production thresholds and coannihilations. Accelerator bounds are checked to identify viable dark matter candidates. Finally, detection rates are computed for a variety of detection methods, such as direct detection and indirect detection through antiprotons, gamma-rays and positrons from the Galactic halo or neutrinos from the center of the Earth or the Sun.']",['2000-12-12'] +354,['eng'],"['Graber, J S']",['Young Collapsed Supernova Remnants'],['Astrophysics and Astronomy'],"['talk, College Park 2000/10/16', 'supernova', 'n, matter', 'black hole', 'surface', 'horizon', 'space-time, singularity', 'matter, exotic']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012203'],"['Type Ia supernovae are thought to explode completely, leaving no condensed remnant, only an expanding shell. Other types of supernovae are thought to involve core collapse and are expected to leave a condensed remnant, which could be either a neutron star or a black hole, or just possibly, something more exotic, such as a quark orstrange star, a naked singularity, a frozen star, a wormhole or a red hole. It has proven surprisingly difficult to determine which type of condensed remnant has been formed in those cases where the diagnostic highly regular pulsar signature of a neutron star is absent. We consider possible observational differences between the two standard candidates, as well as the more speculative alternatives. We classify condensed remnants according to whether they do or do not possess three major features: 1)a hard surface, 2)an event horizon, and 3)a singularity. Black holes and neutron stars differ on all three criteria. Some of the less frequently considered alternatives are ""intermediate,"" in the sense that they possess some of the traits of a black hole and some of the traits of a neutron star. This possibility makes distinguishing the various possibilities even more difficult.']",['2000-12-12'] +355,['eng'],"['Skordis, C', 'Albrecht, Andreas']",['Planck-scale quintessence and the physics of structure formation'],['Astrophysics and Astronomy'],"['quintessence', 'field theory, scalar', 'astrophysics, acceleration', 'cosmic radiation, anisotropy', 'potential', 'density, perturbation', 'membrane model', 'polarization', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012195'],"['In a recent paper we considered the possibility of a scalar field providing an explanation for the cosmic acceleration. Our model had the interesting properties of attractor-like behavior and having its parameters of O(1) in Planck units. Here we discuss the effect of the field on large scale structure and CMB anisotropies. We show how some versions of our model inspired by ""brane"" physics have novel features due to the fact that the scalar field has a significant role over a wider range of redshifts than for typical ""dark energy"" models. One of these features is the additional suppression of the formation of large scale structure, as compared with cosmological constant models. In light of the new pressures being placed on cosmological parameters (in particular H_0) by CMB data, this added suppression allows our ""brane"" models to give excellent fits to both CMB and large scale structure data.']",['2000-12-12'] +356,['eng'],"['Belczynski, K', 'Kalogera, V']",['A New Formation Channel for Double Neutron Stars Without Recycling'],['Astrophysics and Astronomy'],"['n, matter', 'binary', 'carbon', 'oxygen', 'pulsar', 'gravitational radiation', 'coalescence', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012172'],"['We report on a new evolutionary path leading to the formation of close double neutron stars (NS), with the unique characteristic that none of the two NS ever had the chance to be recycled by accretion. The existence of this channel stems from the evolution of helium-rich stars (cores of massive NS progenitors), which has been neglected in most previous studies of double compact object formation. We find that these non-recycled NS-NS binaries are formed from bare carbon-oxygen cores in tight orbits, with formation rates comparable to or maybe even higher than those of recycled NS-NS binaries. On the other hand, their detection probability as binary pulsars is greatly reduced (by about 1000) relative to recycled pulsars, because of their short lifetimes. We conclude that, in the context of gravitational-wave detection of NS-NS inspiral events, this new type of binaries calls for an increase of the rate estimates derived from the observed NS-NS with recycled pulsars, typically by factors of 1.5-3 or even higher.']",['2000-12-11'] +357,['eng'],"['Nasseri, F', 'Rahvar, S']",['Chaotic Inflation with Variable Space Dimensions'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'inflationary universe', 'chaos', 'dimension, upper limit', 'inflaton, mass']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012157'],"['Assuming the space dimension is not constant but decreases during the expansion of the Universe, we study chaotic inflation with the potential $m^2 \\phi^2/2$. We write down field equations in the slow-roll approximation and define slow -roll parameters by assuming the space dimension to be a dynamical parameter. The dynamical character of the space dimension shifts the initial and final value of the inflaton field to larger values, producing delayed chaotic inflation. We obtain an upper limit for the space dimension at the Planck length. This result is in agreement with previous works on the effective time variation of the Newtonian gravitational constant in a model Universe with variable space dimensions. We present some cosmological consequences and calculate observable quantities including the spectral indices, their scale-dependence, and the mass of the inflaton field.']",['2000-12-08'] +358,['eng'],"['Pacheco, J A F']",['Potential Sources of Gravitational Wave Emission and Laser Beam Interferometers'],['Astrophysics and Astronomy'],"['talk, Caraguatatuba 2000/10/17', 'gravitational radiation, particle source', 'gravitational radiation, search for', 'n, matter', 'pulsar', 'black hole', 'binary', 'counters and detectors', 'laser, interference', 'background, stochastic', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012128'],[],['2000-12-07'] +359,['eng'],"['Yakovlev, D G', 'Kaminker, A D', 'Gnedin, O Yu', 'Haensel, P']",['Neutrino Emission from Neutron Stars'],['Astrophysics and Astronomy'],"['review', 'n, matter', 'electron positron, annihilation', 'electron nucleus, elastic scattering', 'neutrino, bremsstrahlung', 'electron positron, annihilation', 'plasma, decay', 'n, semileptonic decay', 'energy loss', 'pi, condensation', 'K, condensation', 'quark, matter', 'magnetic field, effect', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012122'],"['We review the main neutrino emission mechanisms in neutron star crusts and cores. Among them are the well-known reactions such as the electron-positron annihilation, plasmon decay, neutrino bremsstrahlung of electrons colliding with atomic nuclei in the crust, as well as the Urca processes and neutrino bremsstrahlung in nucleon-nucleon collisions in the core. We emphasize recent theoretical achievements, for instance, band structure effects in neutrino emission due to scattering of electrons in Coulomb crystals of atomic nuclei. We consider the standard composition of matter (neutrons, protons, electrons, muons, hyperons) in the core, and also the case of exotic constituents such as the pion or kaon condensates and quark matter. We discuss the reduction of the neutrino emissivities by nucleon superfluidity, as well as the specific neutrino emission produced by Cooper pairing of the superfluid particles. We also analyze the effects of strong magnetic fields on some reactions, such as the direct Urca process and the neutrino synchrotron emission of electrons. The results are presented in the form convenient for practical use. We illustrate the effects of various neutrino reactions on the cooling of neutron stars. In particular, the neutrino emission in the crust is critical in setting the initial thermal relaxation between the core and the crust. Finally, we discuss the prospects of exploring the properties of supernuclear matter by confronting cooling simulations with observations of the thermal radiation from isolated neutron stars.']",['2000-12-07'] +360,['eng'],"['Renault, C', 'Barrau, A', 'Lagache, G', 'Puget, J L']",['New constraints on the Cosmic Mid-Infrared Background using TeV gamma-ray astronomy'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, background', 'density, upper limit', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'cosmic radiation, diffusion', 'cosmic radiation, particle source', 'AGN', 'cosmic radiation, absorption', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012094'],"['Very high energy gamma-ray data obtained by CAT and HEGRA from active galactic nucleus Mkn 501 are used to constrain the cosmic Mid-Infrared background. While the entire infrared and submillimeter spectrum shape based on models has been fixed and the density scaled as a whole in previous studies, recent measures on the low and high energy infrared background are extensively used in this paper. In this original approach, the infrared distribution is only varied in the unexplored 3.5-100 microns region. With conservative hypothesis on the intrinsic spectra of Mkn 501, an upper limit of 4.7 nW.m-2.sr-1 between 5 and 15 microns is derived, which is very close to the lower limit inferred from deep ISOCAM cosmological surveys at 15 microns. This result is shown to be independent of the exact density of the lambda < 3.5 microns and lambda > 100 microns infrared distribution within the uncertainties of the measurements. Moreover, the study presented here rules out a complete extragalactic origin for the 60 microns excess found by Finkbeiner et al. (2000).']",['2000-12-06'] +361,['eng'],"['Garcia de Andrade, L C']",['Decay of inhomogeneities from the spin-torsion fluctuations in the early stages of inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'spin, torsion', 'effect, fluctuation', 'space-time, de Sitter', 'density, perturbation', 'cosmic radiation, background', 'temperature, anisotropy', 'galaxy, production']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012058'],['The spin-torsion fluctuations are shown to act as source of decay of inhomogeneities in the early stages of inflationary de Sitter universe.This seems to be a resul of the repulsive nature of the spin-torsion effects.This result is shown through the investigation of the evolution equation of density perturbations in Einstein-Cartan cosmology.We also show that it is possible to place limits on torsion in the universe from the CMBR temperature anisotropy from the computations we made.The decay of inhomogeneities is not enough however to stop the structure formation as galaxies because the growth of inhomogeneitis dominates the torsion effects and the only effect of torsion seems to decrease very weakly the speed of formation of galaxies.'],['2000-12-05'] +362,['eng'],"['Cuesta, H J M']",['Astrophysical tests for the Novello-De Lorenci-Luciane theory of gravity'],['Astrophysics and Astronomy'],"['lectures, Trieste 2000/06/05', 'relativity theory, equivalence principle', 'gravitation, model', 'validity test', 'gravitational radiation, velocity', 'neutrino, cosmic radiation', 'supernova', 'gravitation, lens', 'black hole', 'gravitational radiation, birefringence', 'approximation, geometrical', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012047'],"[""The Novello-DeLorenci-Luciane (NDL) field theory of gravitation predicts that gravitational waves (GWs) follow geodesics of a modified (effective) geometry with a speed lower than the velocity of light. The theory also demonstrates that GWs exhibit the phenomenon of birefringence, formerly believed to be exclusive of electromagnetic waves. Here prospective astrophysical tests of these predictions are proposed. I point out that future measurements of gravitational waves in coincidence with a non-gravitational process such as {\\it a neutrino burst} (and likely a burst of gamma-rays) may prove useful to discriminate among all the existing theories of gravity. It is also stressed that microlensing of gravitational waves emitted by known galactic sources (i.e., pulsars) in the bulge, lensed by either the Galaxy's central black hole (Sgr A$^\\ast$) or a MACHO object adrift among the Milky Way's stars, may provide a clean test of the birefringence phenomenon implied by the NDL gravity theory.""]",['2000-12-05'] +363,['eng'],"['Kusenko, A', 'Kuzmin, V A']",['Possible galactic sources of ultrahigh-energy cosmic rays and a strategy for their detection via gravitational lensing'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'postulated particle, heavy', 'postulated particle, decay', 'particle, cluster', 'mass, cluster', 'gravitation, lens', 'cosmic radiation, anisotropy', 'galaxy', 'proposed experiment', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012040'],"['If decays of superheavy relic particles in the galactic halo are responsible for ultrahigh-energy cosmic rays, these particles must be clustered to account for small-scale anisotropy in the AGASA data. We show that the masses of such clusters are large enough for them to gravitationally lens stars and galaxies in the background. We propose a general strategy that can be used to detect such clusters via gravitational lensing, or to rule out the hypothesis of decaying relic particles as the origin of highest-energy cosmic rays.']",['2000-12-05'] +364,['eng'],"['Mikheeva, E V']","['Current Status of cos,ological models with mixed dark matter']",['Astrophysics and Astronomy'],"['talk, Warsaw 2000/07/16', 'astrophysics, model', 'astrophysics, missing-mass', 'gravitational radiation', 'mass, fluctuation', 'density, perturbation', 'spectra, perturbation', 'baryon, matter', 'Hubble constant', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'statistical analysis', 'temperature, fluctuation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012018'],"['An analysis of cosmological mixed dark matter models in spatially flat Friedmann Universe with zero $\\Lambda$-term is presented. We argue that the introduction of cosmic gravity waves helps to satisfy observational constraints. The analysis of models is based on the confrontation with the mass function of clusters of galaxies and the CMB anisotropy. The implication of Press-Schechter formalism allowed to constrain $\\sigma_8=0.52 \\pm 0.01$. This normalisation of the spectrum of density perturbations has been used to calculate numerically the value of the large scale CMB anisotropy and the relative contribution of cosmological gravitational waves, T/S. We found that increasing $\\Omega_\\nu$ weakens the requirements to the value of T/S, however even for $\\Omega_\\nu\\le 0.4$ the models with $h+n\\ge 1.5$ suggest considerable abundance of gravitational waves, T/S${}^>_\\sim 0.3$. Minimisation of the value T/S is possible only in the range of the red spectra ($n<1$) and small $h$ ($<0.6$). However the parameter $\\Omega_\\nu$ is strongly constrained by $\\Delta T/T$ data on the first acoustic peak of Sakharov oscillations. Assuming that T/S $\\in[0,3]$ and taking into account observational data on the amplitude of the first acoustic peak we constrain the model parameters. We show that the considered models admit both moderate red and blue spectra of density perturbations $n\\in [0.9,1.2]$ with rather high abundance hot dark matter, $\\Omega_\\nu \\in [0.2,0.4]$. Any condition, $n<0.9$ or $\\Omega_\\nu<0.2$, decreases the relative amplitude of the first acoustic peak for more than 30% in comparison with its height measured by BOOMERanG.']",['2000-12-20'] +365,['eng'],"['Lukash, V N']",['$\\Lambda$-Inflation and CMBR Anisotropy'],['Astrophysics and Astronomy'],"['inflationary universe', 'astrophysics, fundamental constant', 'astrophysics, missing-mass', 'gravitational radiation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'temperature, fluctuation', 'density, perturbation', 'spectra, perturbation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0012014'],['We argue that a $\\Lambda$-inflation model can ensure large relative contribution of cosmic gravity waves into the $\\Delta T/T$ at COBE scale preserving at the same time a near scale-invariant spectrum of cosmological density perturbations favored by observational data ($n_S\\simeq 1$). High efficiency of these models to meet observational tests is discussed.'],['2000-12-20'] +366,['eng'],"['Roulet, Esteban']",['Neutrino Astrophysics'],['Astrophysics and Astronomy'],"['lectures, Miramare 2000/06/12', 'neutrino, history', 'gauge field theory, SU(2) x U(1)', 'neutrino, mass', 'neutrino, oscillation', 'neutrino, solar', 'neutrino, cosmic radiation', 'supernova', 'lepton, production', 'astrophysics, missing-mass', 'light nucleus, production', 'proposed experiment', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011570'],"['A general overview of neutrino physics and astrophysics is given, starting with a historical account of the development of our understanding of neutrinos and how they helped to unravel the structure of the Standard Model. We discuss why it is so important to establish if neutrinos are massive and introduce the main scenarios to provide them a mass. The present bounds and the positive indications in favor of non-zero neutrino masses are discussed, including the recent results on atmospheric and solar neutrinos. The major role that neutrinos play in astrophysics and cosmology is illustrated.']",['2000-12-01'] +367,['eng'],"['Bertone, G', 'Sigl, G', 'Silk, J']",['Annihilations from the Galactic Centre'],['Astrophysics and Astronomy'],"['talk, York 2000/09/18', 'black hole, massive', 'galaxy', 'astrophysics, missing-mass', 'dark matter, annihilation', 'electron, pair production', 'synchrotron radiation', 'magnetic field', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011553'],"['A massive black hole is present at the centre of our galaxy and inevitably accretes dark matter particles, creating a region of very high particle density. The annihilation rate is enhanced with a large number of e+e- pairs produced either directly or by successive decays of mesons. We evaluate the synchrotron emission (and self-absorption) associated with the propagation of these particles through the galactic magnetic field and give constraints on the values of mass and cross section of the dark matter particles.']",['2000-11-30'] +368,['eng'],"['Chen, X']",['The Helium abundance problem and non-minimally coupled quintessence'],['Astrophysics and Astronomy'],"['talk, Cheju Island 2000/09/04', 'astrophysics, model', 'light nucleus, production', 'helium, density', 'quintessence', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011533'],['There is a tension between observed Helium abundance and the prediction of the standard Big Bang Nucleosynthesis. We show that non-minimally quintessence model may help to reduce this tension between theory and observation.'],['2000-11-29'] +369,['eng'],"['Chen, X']",['How to get less helium and more neutrinos from BBN'],['Astrophysics and Astronomy'],"['talk, Columbus 2000/08/09', 'astrophysics, model', 'light nucleus, production', 'quintessence', 'helium, yield', 'neutrino, yield', 'astrophysics, expansion', 'cosmic radiation, background', 'neutrino, cosmic radiation', 'neutrino, flavor', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011532'],"['We discuss BBN in the presence of a non-minimally coupled quintessence model. In some of these models, the gravitational constant and cosmic expansion rate are smaller than standard model predicts. The Helium abundance is then smaller, possibly resolve the marginal disagreement between theory and observation. Furthermore, the constraint on neutrino species may also be relaxed.']",['2000-11-29'] +370,['eng'],"['Chen, X', 'Scherrer, R J', 'Steigman, G']",['Extended quintessence and the primordial helium abundance'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'quintessence', 'field theory, scalar', 'energy, density', 'helium, density', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011531'],"['In extended quintessence models, a scalar field which couples to the curvature scalar R provides most of the energy density of the universe. We point out that such models can also lead naturally to a decrease in the primordial abundance of helium-4, relieving the tension which currently exists between the primordial helium-4 abundance inferred from observations and the amount predicted by Standard Big Bang Nucleosynthesis (SBBN) corresponding to the observed deuterium abundance. Using negative power-law potentials for the quintessence field, we determine the range of model parameters which can lead to an interesting reduction in the helium-4 abundance, and we show that it overlaps with the region allowed by other constraints on extended quintessence models.']",['2000-11-29'] +371,['eng'],"['Hansen, S H']","[""Heavy sterile neutrinos - what they can be and what they can't""]",['Astrophysics and Astronomy'],"['review, San Feliu de Guixols 2000/09/30', 'neutrino, sterile', 'neutrino, lifetime', 'astrophysics, missing-mass', 'neutrino, mass', 'neutrino, mixing angle', 'light nucleus, production', 'supernova', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011526'],"['We review current astrophysical bounds on MeV sterile neutrinos, and then we discuss why a sterile keV neutrino is a natural warm dark matter candidate.']",['2000-11-29'] +372,['eng'],"['Gaisser, T K']",['High Energy Neutrino Astronomy - the cosmic-ray connection'],['Astrophysics and Astronomy'],"['talk, Metepec 2000/08/09', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, measurement', 'neutrino, flux', 'muon, cosmic radiation', 'counters and detectors, proposed', 'AGN', 'gamma ray burst', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011525'],['Several of the models for origin of the highest energy cosmic rays also predict significant neutrino fluxes. A common factor of the models is that they must provide sufficient power to supply the observed energy in the extragalactic component of the cosmic radiation. The assumption that a comparable amount of energy goes into high-energy neutrinos allows a model-independent estimate of the neutrino signal that may be expected.'],['2000-11-29'] +373,['eng'],"['Gaisser, T K']",['Origin of Cosmic Radiation'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'cosmic radiation, particle source', 'cosmic radiation, solar', 'galaxy', 'supernova', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'p, cosmic radiation', 'cosmic radiation, primary', 'proposed experiment', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011524'],"['I give a brief overview of cosmic ray physics, highlighting some key questions and how they will be addressed by new experiments.']",['2000-11-29'] +374,['eng'],"['Ave, M', 'Vázquez, R A', 'Zas, E']",['Modelling Horizontal Air Showers Induced by Cosmic Rays'],['Astrophysics and Astronomy'],"['p, showers', 'muon, showers', 'muon, density', 'showers, air', 'showers, production', 'magnetic field, geophysics', 'muon, energy spectrum', 'muon, angular distribution', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011490'],['We present a framework for the study of muon density patterns on the ground due to showers produced in the atmosphere by cosmic rays incident at high zenith angles. As a checking procedure predictions of a model based on such a framework are compared to simulation results.'],['2000-12-20'] +375,['eng'],"['Aharonian, F A']",['Reanalysis of the high energy cutoff of the 1997 Mkn 501 TeV energy spectrum'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'showers', 'cosmic radiation, background', 'Cherenkov counter, energy resolution', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011483'],"['Data taken with the HEGRA system of imaging atmospheric Cherenkov telescopes during the 1997 flares of Mkn 501 are reanalyzed using an algorithm providing improved energy resolution. A resolution of 10% to 12% is obtained by accounting for the variation of the Cherenkov light yield with the height of the shower maximum in the atmosphere. The improved energy resolution is particularly relevant for the study of the high-energy cutoff in the spectrum, which might be caused by interactions with the intergalactic infrared background radiation. The reanalysis presented here confirms the results obtained in the previous analysis, but hints a steeper slope of the spectrum in the region around 20 TeV.']",['2000-12-20'] +376,['eng'],"['Primack, Joel R', 'Somerville, R S', 'Bullock, J S', 'Devriendt, J E G']",['Probing Galaxy Formation with High Energy Gamma-Rays'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, absorption', 'galaxy, production', 'photon, background', 'energy spectrum', 'astrophysics, missing-mass', 'matter, density', 'matter, mass', 'gas', 'cosmic radiation, luminosity', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011475'],"['We discuss how measurements of the absorption of $\\gamma$-rays from GeV to TeV energies via pair production on the extragalactic background light (EBL) can probe important issues in galaxy formation. We use semi-analytic models (SAMs) of galaxy formation, set within the hierarchical structure formation scenario, to obtain predictions of the EBL for 0.1-1000$\\mu$m. SAMs incorporate simplified physical treatments of the key processes of galaxy formation --- including gravitational collapse and merging of dark matter halos, gas cooling and dissipation, star formation, supernova feedback and metal production --- and have been shown to reproduce key observations at low and high redshift. Here we also introduce improved modelling of the spectral energy distributions in the mid-to-far-IR arising from emission by dust grains. Assuming a flat \\lcdm cosmology with $\\Omega_m=0.3$ and Hubble parameter $h=0.65$, we investigate the consequences of variations in input assumptions such as the stellar initial mass function (IMF) and the efficiency of converting cold gas into stars. We conclude that observational studies of the absorption of $\\gamma$-rays with energies from 10s of Gev to 10s of TeV will help to determine the EBL, and also help to explain its origin by constraining some of the most uncertain features of galaxy formation theory, including the IMF, the history of star formation, and the reprocessing of light by dust.']",['2000-12-20'] +377,['eng'],"['Amendola, L', 'Tocchini-Valentini, D']",['Stationary dark energy'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, missing-mass', 'energy, density', 'attractor', 'expansion, acceleration', 'cosmic radiation, background', 'matter, density', 'dark energy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011243'],"['We propose a cosmological model that makes a significant step toward solving the coincidence problem of the near similarity at the present of the dark energy and dark matter components. Our cosmology has the following properties: a) among flat and homogeneous spaces, the present universe is a global attractor: all the possible initial conditions lead to the observed proportion of dark energy and dark matter; once reached, it remains fixed forever; b) the expansion is accelerated at the present, as requested by the supernovae observations; c) the model is consistent with the large-scale structure and microwave background data. Moreover, contrary to all the other models we know of, the dark energy and the dark matter densities always scale similarly after equivalence and are close to within two orders of magnitude. The model makes use of a non-linear coupling of the dark energy to the dark matter that switches on after structure formation.']",['2000-11-14'] +378,['eng'],"['Medina-Tanco, G A', 'Ensslin, T A']",['Isotropization of Ultra-High Energy Cosmic Ray Arrival Directions by Radio Ghosts'],['Astrophysics and Astronomy'],"['cosmic radiation, flux', 'ghost', 'magnetic field', 'galaxy', 'p, scattering', 'differential cross section, angular dependence', 'astrophysics, missing-mass', 'numerical calculations, Monte Carlo', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011454'],"['The isotropy in the ultra high energy cosmic ray (UHECR) flux observed by Yakutsk and AGASA experiments, is a very strong constraint to production and propagation models alike. Most of the scenarios proposed in the literature should produce a sizable anisotropy as either extragalactic luminous or dark matter is normally associated with the invoked particle sources. We explore the possibility that the magnetic fields in fossil cocoons of former radio galaxies -- so called {\\it radio ghosts} -- are able to scatter UHECR in the intergalactic medium giving rise to the observed isotropy. We show, through numerical simulations, under which conditions this process can be operative and the magnitude of the effect. We further demonstrate, that if radio ghosts mix with the ambient medium, they might be able to produce the observed magnetic fields in clusters of galaxies. In the case of mixing, the UHECR isotropization would be even stronger than in our conservative estimates.']",['2000-12-20'] +379,['eng'],"['Zas, E']",['A New Approach to Mass Measurements of UHECR'],['Astrophysics and Astronomy'],"['talk, Metepec 2000/08/09', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'showers, air', 'angular distribution, asymmetry', 'muon, cosmic radiation', 'p, cosmic radiation', 'spatial distribution', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011416'],"['The role of Horizontal Showers induced by cosmic rays is discussed in detail. A new approach to the calculation of the muon component in horizontal air showers induced by protons, heavier nuclei or photons is presented which allows a simple analytical evaluation of the muon density profiles at ground level. The results of the first application of these results to horizontal air showers detected at the Haverah Park Array by the recently started {\\sl Leeds-Santiago collaboration}, leading to important restrictions on composition at ultra high energies, are reported.']",['2000-11-23'] +380,['eng'],"['Barriga, J', 'Gaztañaga, E', 'Santos, M', 'Sarkar, S']",['On the APM power spectrum and the CMB anisotropy'],['Astrophysics and Astronomy'],"['inflationary universe', 'critical phenomena', 'density, perturbation', 'spectra, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'light nucleus, production', 'baryon, density', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011398'],"['Adams et al. (1997b) have noted that according to our current understanding of the unification of fundamental interactions, there should have been phase transitions associated with spontaneous symmetry breaking {\\em during} the inflationary era. This may have resulted in the breaking of scale-invariance of the primordial density perturbation for brief periods. A possible such feature was identified in the power spectrum of galaxy clustering in the APM survey at the scale $k \\sim 0.1 h$ Mpc^{-1} and it was shown that the secondary acoustic peaks in the power spectrum of the CMB anisotropy should consequently be suppressed. We demonstrate that this prediction is confirmed by the recent Boomerang and Maxima observations, which favour a step-like spectral feature in the range $k \\sim (0.06-0.6)h$ Mpc^{-1}, independently of the similar previous indication from the APM data. Such a spectral break enables an excellent fit to both APM and CMB data with a baryon density consistent with the BBN value. It also allows the possibility of a matter-dominated universe with zero cosmological constant, which we show can now account for even the evolution of the abundance of rich clusters.']",['2000-11-22'] +381,['eng'],"['Bond, J R', 'Pogosian, D Y', 'Prunet, S', 'Sigurdson, K', 'Ade, P', 'Balbi, A', 'Bock, J J', 'Borrill, J', 'Boscaleri, A', 'Coble, K', 'Crill, B P', 'De Bernardis, P', 'Farese, P', 'Ferreira, P', 'Ganga, K', 'Giacometti, M', 'Hanany, S', 'Hivon, E', 'Hristov, V V', 'Iacoangeli, A', 'Jaffe, A', 'Lange, A', 'Lee, A', 'Martinis, L', 'Masi, S', 'Mauskopf, P', 'Melchiorri, A', 'Montroy, T', 'Netterfield, C B', 'Oh, S', 'Pascale, E', 'Piacentini, F', 'Rabii, B', 'Rao, S', 'Richards, P', 'Romeo, G', 'Ruhl, J E', 'Scaramuzzi, F', 'Sforza, D M', 'Smoot, G F', 'Stompor, R', 'Winant, C', 'Wu, P']","['The Quintessential CMB, Past & Future']",['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'quintessence', 'galaxy, cluster', 'supernova', 'inflationary universe', 'astrophysics, missing-mass', 'matter, density', 'neutrino, massive', 'energy', 'error', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011379'],"['The past, present and future of cosmic microwave background (CMB) anisotropy research is discussed, with emphasis on the Boomerang and Maxima balloon experiments. These data are combined with large scale structure (LSS) information and high redshift supernova (SN1) observations to explore the inflation-based cosmic structure formation paradigm. Here we primarily focus on a simplified inflation parameter set, {omega_b,omega_{cdm},Omega_{tot}, Omega_Q,w_Q, n_s,tau_C, sigma_8}. After marginalizing over the other cosmic and experimental variables, we find the current CMB+LSS+SN1 data gives Omega_{tot}=1.04\\pm 0.05, consistent with (non-baroque) inflation theory. Restricting to Omega_{tot}=1, we find a nearly scale invariant spectrum, n_s =1.03 \\pm 0.07. The CDM density, omega_{cdm}=0.17\\pm 0.02, is in the expected range, but the baryon density, omega_b=0.030\\pm 0.004, is slightly larger than the current nucleosynthesis estimate. Substantial dark energy is inferred, Omega_Q\\approx 0.68\\pm 0.05, and CMB+LSS Omega_Q values are compatible with the independent SN1 estimates. The dark energy equation of state, parameterized by a quintessence-field pressure-to-density ratio w_Q, is not well determined by CMB+LSS (w_Q<-0.3 at 95%CL), but when combined with SN1 the resulting w_Q<-0.7 limit is quite consistent with the w_Q=-1 cosmological constant case. Though forecasts of statistical errors on parameters for current and future experiments are rosy, rooting out systematic errors will define the true progress.']",['2000-11-22'] +382,['eng'],"['Taylor, A N', 'Liddle, A R']",['Gravitino production in the warm inflationary scenario'],['Astrophysics and Astronomy'],"['inflationary universe', 'gravitino, production', 'dissipation', 'energy, density', 'light nucleus, production', 'density, perturbation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011365'],"['We estimate the production of gravitinos during and after the end of a period of warm inflation, a model in which radiation is produced continuously as the field rolls down the potential producing dissipation. We find that gravitino production is efficient for models in the strong dissipation regime, with the result that standard nucleosynthesis is disrupted unless the magnitude of the inflaton potential is very small. Combining this with the constraint from the thermal production of adiabatic density perturbations we find the dissipation rate must be extraordinarily strong, or that the potential is very flat.']",['2000-11-21'] +383,['eng'],"['Berti, E', 'Ferrari, V']",['Gravitational waves emitted by solar-type stars excited by orbiting planets'],['Astrophysics and Astronomy'],"['binary', 'star, perturbation', 'gravitational radiation, emission', 'approximation, quadrupole', 'Einstein equation', 'tensor, energy-momentum', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011364'],"['The possibility of exciting the g-modes of a solar-type star as a consequence of the gravitational interaction with a close companion (a planet or a brown dwarf) is studied by a perturbative approach. The amplitude of the emitted gravitational wave is computed and compared with the quadrupole emission of the system, showing that in some cases it can be considerably larger. The effects of radiation reaction are considered to evaluate the timescale of the emission process, and a Roche lobe analysis is used to establish the region where the companion can orbit without being disrupted by tidal interactions with the star.']",['2000-11-21'] +384,['eng'],"['Nagataki, S']",['Implications of the Discovery of Millisecond Pulsar in SN 1987A'],['Astrophysics and Astronomy'],"['supernova', 'pulsar, velocity', 'gravitational radiation, emission', 'shock waves, deformation', 'neutrino, oscillation', 'stability, hydrodynamical', 'n, matter', 'angular momentum', 'amplitude analysis', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011363'],"['From the observation of the millisecond pulsar in SN 1987A, the following implications are obtained. 1) The pulsar spindown in SN 1987A is caused by radiating gravitational waves rather than by magnetic dipole radiation and/or relativistic pulsar winds. 2) A mildly deformed shock wave would be formed at the core-collapse and explosion in SN 1987A, which is consistent with the conclusion derived in Nagataki (2000). 3) The gravitational waves from the pulsar will be detected in (5-10) years by the Fabry-Perot-Michelson interferometer as the gravitational detector such as LIGO and TAMA. 4) The neutrino oscillation model is not a promising one for the explanation of the kick velocity of the pulsar in SN 1987A. The hydrodynamical instability model will be more favored.']",['2000-11-21'] +385,['eng'],"['Kamionkowski, M P', 'Jaffe, A H']",['Detection of Gravitational Waves from Inflation'],['Astrophysics and Astronomy'],"['talk, Columbus 2000/08/09', 'talk, Trieste 2000/06/05', 'gravitational radiation, search for', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, polarization', 'temperature, fluctuation', 'density, perturbation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011329'],"[""Recent measurements of temperature fluctuations in the cosmic microwave background (CMB) indicate that the Universe is flat and that large-scale structure grew via gravitational infall from primordial adiabatic perturbations. Both of these observations seem to indicate that we are on the right track with inflation. But what is the new physics responsible for inflation? This question can be answered with observations of the polarization of the CMB. Inflation predicts robustly the existence of a stochastic background of cosmological gravitational waves with an amplitude proportional to the square of the energy scale of inflation. This gravitational-wave background induces a unique signature in the polarization of the CMB. If inflation took place at an energy scale much smaller than that of grand unification, then the signal will be too small to be detectable. However, if inflation had something to do with grand unification or Planck-scale physics, then the signal is conceivably detectable in the optimistic case by the Planck satellite, or if not, then by a dedicated post-Planck CMB polarization experiment. Realistic developments in detector technology as well as a proper scan strategy could produce such a post-Planck experiment that would improve on Planck's sensitivity to the gravitational-wave background by several orders of magnitude in a decade timescale.""]",['2000-11-20'] +386,['eng'],"['Doroshkevich, A G', 'Naselsky, P D']",['Ultra - High Energy Cosmic Rays from decay of the Super Heavy Dark Matter Relics'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'p, cosmic radiation', 'cosmic radiation, energy', 'cosmic radiation, background', 'microwaves', 'cosmic radiation, anisotropy', 'black hole, decay', 'p, density', 'p, energy loss', 'numerical calculations', '> 10**11 GeV']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011320'],"['In this paper we briefly discuss the problem of the origin of Ultra High Energy Cosmic Rays in the framework of Top-Down models. We show that, for high energy of decays and in a wide range of spectra of injected protons, their extragalactic flux is consistent with the observed fluxes of cosmic rays in the energy range 0.1 E_{GZK}< E < 10E_{GZK}. For suitable energy and spectra of injected protons, the contribution of galactic sources is moderate, in this energy range, but it dominates at smaller and larger energies. In such models we can expect that at these energies the anisotropy of cosmic rays distribution over sky will be especially small. Some possible manifestations of decays of super massive particles such as, for example, primordial black holes with masses M_{pbh} ~ 10^{-5} g, are considered. In particular, we show that partial conversion of energy released during these decays at redshifts z ~ 1000 to Ly-alpha photons can delay the hydrogen recombination and distort the spectrum of fluctuations of the cosmic microwave background radiation.']",['2000-11-17'] +387,['eng'],"['Domogatsky, G V']",['The BAIKAL neutrino project'],['Astrophysics and Astronomy'],"['talk, Sudbury 2000/06/16', 'neutrino, cosmic radiation', 'neutrino, angular distribution', 'new particle, search for', 'WIMP', 'magnetic monopole', 'muon, cosmic radiation', 'muon, particle identification', 'muon, angular distribution', 'flux, upper limit', 'Cherenkov counter, water', 'deep underground detector, Baikal', 'experimental results', 'talk, Heidelberg 2000/07/10']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011313'],"['We review the present status of the Baikal Neutrino Project and present preliminary results of a search for upward going atmospheric neutrinos, WIMPs and magnetic monopoles obtained with the detector NT-2000 during 1998. Also the results of a search for very high energy neutrinos with partially completed detector in 1996 are presented.']",['2000-11-17'] +388,['eng'],"['Balbi, A']",['Cosmological Parameter Estimation from CMB Experiments'],['Astrophysics and Astronomy'],"['review, Verbier 2000/07/17', 'inflationary universe', 'model, adiabatic', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, fluctuation', 'supernova', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011202'],"['I review the general aspects of cosmological parameter estimation from observations of the cosmic microwave background (CMB) temperature anisotropies in the framework of inflationary adiabatic models. The most recent CMB datasets are starting to give good constraints on the relevant parameters of inflationary adiabatic models. They point toward a model consistent with the basic predictions of inflation: a nearly flat universe, with a nearly scale invariant spectrum of primordial fluctuation.']",['2000-11-10'] +389,['eng'],"['Tornkvist, O', 'Davis, A C', 'Dimopoulos, K', 'Prokopec, Tomislav']",['Large-Scale Primordial Magnetic Fields from Inflation and Preheating'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'inflationary universe', 'photon, mass', 'field theory, scalar', 'vacuum state, fluctuation', 'magnetic field, galaxy', 'gauge field theory', 'preheating']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011278'],"['We consider models in which the (transverse) photon mass is non-zero during inflation and drops to zero non-adiabatically at the end of inflation. Through this process, vacuum fluctuations of the photon field are converted into physical, long-wavelength modes with high amplitude. The resulting spectrum of the field strength is approximately B_l ~ 1/l, where l is the relevant coherence scale. With a reasonable model of field evolution we obtain, on comoving galactic scales, a magnetic field strong enough to seed a dynamo mechanism and generate the observed galactic magnetic fields.']",['2000-11-15'] +390,['eng'],[],['Upper limits to low energy antineutrino flux from GRB990705'],['Astrophysics and Astronomy'],"['gamma ray burst', 'neutrino, cosmic radiation', 'antineutrino/e, flux', 'upper limit', 'antineutrino p, interaction', 'deep underground detector, Gran Sasso', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011249'],"['The detection of Gamma Ray Burst GRB990705 on 1999, July 5.66765 UT, pointing to the Large Magellanic Clouds, suggested the search for a possible neutrino counterpart, both in coincidence with and slightly before (or after) the photon burst. We exploited such a possibility by means of the LVD neutrino telescope (National Gran Sasso Laboratory, Italy), which has the capability to study low-energy cosmic neutrinos. No evidence for any neutrino signal, over a wide range of time durations, has been found, at the occurrence of GRB990705. Due to the lack of information about both the source distance and its emission spectrum, the results of the search are expressed in terms of upper limits, at the Earth, to the antineutrino flux $\\cdot$ cross-section, integrated over different time durations. Moreover, assuming thermal antineutrino spectra at the source, upper limits to the antineutrino flux, integrated over time duration, for different spectral temperatures, are obtained. Based on these limits and on the expectations for neutrino emission from collapsing astrophysical objects, the occurrence of a gravitational stellar collapse can be excluded up to a distance r approximately 50 kpc, in the case of time coincidence with GRB990705, and r approximately 20 kpc, for the 24 hours preceding it.']",['2000-11-14'] +391,['eng'],"['Steer, D A']",['Self-intersections and gravitational properties of chiral cosmic strings in Minkowski space'],['Astrophysics and Astronomy'],"['astrophysics, string', 'symmetry, chiral', 'space-time, Minkowski', 'approximation, weak field', 'angular momentum', 'charge, chiral', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'effective potential', 'renormalization', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011233'],"['Chiral cosmic strings are naturally produced at the end of D-term inflation and they may have interesting cosmological consequences. As was first proved by Carter and Peter, the equations of motion for chiral cosmic strings in Minkowski space are integrable (just as for Nambu-Goto strings). Their solutions are labeled by a function $k(\\sigma - t)$ where $t$ is time and $\\sigma$ is the invariant length along the string, and the constraints on $k$, which determines the charge on the string, are that $0 \\leq k^2 \\leq 1$. We review the origin of this parameter and also discuss some general properties of such strings which can be deduced from the equations of motion. The metric around infinite chiral strings is then constructed in the weak field limit, and studied as a function of $k$. We also consider the angular momentum of circular chiral loops, and extend previous work to consider the evolution and self-intersection properties of a more general family of chiral cosmic string loops for which $k^2(\\sigma-t)$ is not constant.']",['2000-11-14'] +392,['eng'],"['Kachelriess, M']",['Ultrahigh energy cosmic rays and new particle physics'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'astrophysics, missing-mass', 'particle, massive', 'hadron, cosmic radiation', 'spectra', 'spectra, fragmentation', 'neutrino, cosmic radiation', 'neutrino, flux', 'neutrino nucleon, interaction', 'total cross section, energy dependence', 'showers, air', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011231'],"['The current status of the ultrahigh energy cosmic ray (UHE CR) enigma and several proposed solutions involving particle physics beyond the standard model are discussed. Emphasis is given to top--down models, and as a main example, supermassive dark matter as galactic source for UHE CR and the status of its experimental signatures (galactic anisotropy, chemical composition and clustering) is reviewed. Then different approaches to calculate fragmentation spectra of supermassive particles are discussed. Finally, it is argued that UHE neutrinos cannot be - neither directly or indirectly - responsible for the observed vertical air showers.']",['2000-11-14'] +393,['eng'],"['Sturrock, P A', 'Scargle, J D']","['Histogram Analysis of Gallex, GNO and Sage Neutrino Data']",['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'data analysis method', 'time variation', 'statistical analysis', 'magnetic field, solar', 'neutrino, magnetic moment', 'numerical calculations', 'deep underground detector, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011228'],"['If the solar neutrino flux were constant, as is widely assumed, the histogram of flux measurements would be unimodal. On the other hand, sinusoidal or square-wave modulation (either periodic or stochastic) may lead to a bimodal histogram. We here present evidence that the neutrino flux histogram is in fact bimodal. We analyze all available data from gallium experiments, coordinating results from the GALLEX and GNO experiments into one data set, and adopting results from the SAGE experiment as another data set. The two histograms, from the two data sets, are consistent in showing peaks in the range 45-75 SNU and 90-120 SNU, with a valley in between. By combining the data into one data set, we may form more detailed histograms; these strengthen the case that the flux is bimodal. A preliminary statistical analysis indicates that the bimodal character of the solar neutrino flux is highly significant. Since the upper peak is close to the expected flux (120-140 SNU), we may infer that the neutrino deficit is due to time-varying attenuation of the flux produced in the core. We estimate the time scale of this variation to be in the range 10-60 days. Attenuation that varies on such a time scale is suggestive of the influence of solar rotation, and points towards a process involving the solar magnetic field in conjunction with a nonzero neutrino magnetic moment.']",['2000-11-14'] +394,['eng'],"['Kaplinghat, M', 'Turner, M S']",['Precision Cosmology and the Density of Baryons in the Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'baryon, density', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007454'],"['Big-bang Nucleosynthesis (BBN) and Cosmic Microwave Background (CMB) anisotropy measurements give independent, accurate measurements of the baryon density and can test the framework of the standard cosmology. Early CMB data are consistent with the longstanding conclusion from BBN that baryons constitute a small fraction of matter in the Universe. We clarify precisely what the two methods determine, and point out that differing values for the baryon density need not indicate inconsistency if the entropy has changed since BBN. Such an entropy change has a clear signature in the CMB anisotropy.']",['2000-08-01'] +395,['eng'],"['Castellina, A']",['Cosmic ray composition and energy spectrum above 1 TeV'],['Astrophysics and Astronomy'],"['talk, Campinas 2000/07/17', 'nucleus, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, primary', 'showers, air', 'charged particle, spectra', 'radiation, Cherenkov', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011221'],"[""The most recent experimental results on the cosmic ray composition and energy spectrum above 1 TeV are reviewed and discussed. All data agree on the presence of the so-called ``knee'' at an energy E(knee) = 3-4 PeV; the knee is seen in all the components of the Extensive Air Showers. These results support the hypothesis of an astrophysical origin of the knee, while no new features in the hadronic interactions at high energies are envisaged. The cosmic ray composition below and above the knee region is still an open question. According to most experiments, the knee seems to be due to the light component of the primary beam, with a composition getting heavier above the knee. However, results contradicting this conclusion have to be considered and understood.""]",['2000-11-13'] +396,['eng'],"['Vernizzi, F', 'Durrer, R']",['CMB anisotropies in pre-big bang cosmology'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'density, fluctuation', 'axion', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011197'],"['We present an alternative scenario for cosmic structure formation where initial fluctuations are due to Kalb-Ramond axions produced during a pre-big bang phase of inflation. We investigate whether this scenario, where the fluctuations are induced by seeds and therefore are of isocurvature nature, can be brought in agreement with present observations by a suitable choice of cosmological parameters. We also discuss several observational signatures which can distinguish axion seeds from standard inflationary models.']",['2000-11-10'] +397,['eng'],"['Belczynski, K', 'Bulik, T', 'Kluzniak, W']","['Population synthesis of neutron stars, strange (quark) stars and black holes']",['Astrophysics and Astronomy'],"['talk, Alicante 2000/09/04', 'n, matter', 'matter, strangeness', 'black hole', 'matter, mass', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011183'],"['We compute and present the distribution in mass of single and binary neutron stars, strange stars, and black holes. The calculations were performed using a stellar population synthesis code. We follow all phases of single and binary evolution, starting from a ZAMS binary and ending in the creation of one compact object (neutron star, black hole, strange star) and a white dwarf, or two compact objects (single or binary). We assume that neutron stars are formed in the collapse of iron/nickel cores in the mass range M0 < M < M1, quark stars in the range M1 < M < M2, and black holes for core masses M > M2 and find that the population of quark stars can easily be as large as the population of black holes, even if there is only a small mass window for their formation.']",['2000-11-10'] +398,['eng'],"['González-Mestres, L']",['Lorentz Symmetry Violation and Acceleration in Relativistic Shocks'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'symmetry breaking, Lorentz', 'kinematics, deformation', 'shock waves, relativistic', 'effect, acceleration', 'neutrino, cosmic radiation', 'pi, photoproduction']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011182'],"['In previous papers (e.g. physics/0003080 and references therein), it was pointed out that Lorentz symmetry violation (LSV) at Planck scale can play a crucial role in astrophysical processes at very high energy. It can potentially inhibit radiation under external forces (e.g. synchrotron-like), GZK-like cutoffs, decays, photodisintegration of nuclei, momentum loss trough collisions (e.g. with a photon wind in reverse shocks), production of lower-energy secondaries... An updated description of this phenomenon is presented, focusing on acceleration in relativistic shocks and having in mind a model where the effective parameter driving LSV would vary like the square of the momentum scale (Quadratically Deformed Relativistic Kinematics, QDRK). Implications for ultra-high energy (UHE) neutrino production are equally discussed.']",['2000-11-10'] +399,['eng'],"['González-Mestres, L']",['Gamma and Cosmic-Ray Tests of Special Relativity'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'relativity theory, validity test', 'symmetry breaking, Lorentz', 'cosmic radiation', 'kinematics, deformation', 'relativistic', 'pi, photoproduction', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011181'],"['Lorentz symmetry violation (LSV) at Planck scale can be tested (see e.g. physics/0003080) through ultra-high energy cosmic rays (UHECR). In a deformed Lorentz symmetry (DLS) pattern where the effective LSV parameter varies like the square of the momentum scale (quadratically deformed relativistic kinematics, QDRK), a 10E-6 LSV at Planck scale would be enough to produce observable effects on the properties of cosmic rays at the 10E20 eV scale: absence of GZK cutoff, stability of unstable particles, lower interaction rates, kinematical failure of any parton model and of standard formulae for Lorentz contraction and time dilation... Its phenomenological implications are compatible with existing data. If the effective LSV parameter is taken to vary linearly with the momentum scale (linearly deformed relativistic kinematics, LDRK), a LSV at Planck scale larger than 10E-7 eV seems to lead to contradictions with data above TeV energies. Consequences are important for high-energy gamma-ray experiments, as well as for high-energy cosmic rays and gravitational waves.']",['2000-11-10'] +400,['eng'],"['Ugoccioni, R', 'Teodoro, L', 'Wichoski, U']",['Large Scale Structure and Cosmic Rays revisited'],['Astrophysics and Astronomy'],"['talk, Lisbon 2000/07/27', 'talk, Faro 2000/09/01', 'cosmic radiation, primary', 'p, cosmic radiation', 'cosmic radiation, particle source', 'matter, density', 'p, energy loss', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011171'],['We investigate the possibility that ultra high energy cosmic rays (E > 10^19 eV) are related to the distribution of matter on large scales. The large scale structure (LSS) data stems from the recent IRAS PSCz redshift survey. We present preliminary predictions drawn from an anisotropic distribution of sources which follows the galaxy distribution.'],['2000-11-09'] +401,['eng'],"['Foot, R', 'Ignatiev, A Yu', 'Volkas, R R']",['Physics of mirror photons'],['Astrophysics and Astronomy'],"['quantum electrodynamics', 'symmetry, U(1) x U(1)', 'electron, mirror particle', 'photon, mirror particle', 'photon, sterile', 'photon, mixing angle', 'quantum mechanics, decoherence', 'quantum mechanics, density matrix', 'time dependence', 'astrophysics', 'matter, mirror']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011156'],"['The physics of kinetic mixing between ordinary and mirror photons is elucidated. An important role is played by four linear combinations we dub the physical photon, the sterile photon, the physical mirror photon, and the sterile mirror photon. Because of the mass degeneracy between the two gauge bosons, quantum coherence effects are important. The physical photon becomes a certain coherent superposition of the bare ordinary photon and the bare mirror photon. Similarly, the physical mirror photon is another, but {\\it not orthogonal}, coherent superposition. Using a Bloch equation analysis, we show that the physical mirror photon decoheres into a mixture of the physical (ordinary) photon and the sterile photon when it propagates through ordinary matter. Observational signatures for some hybrid ordinary/mirror binary astrophysical systems are qualitatively discussed, and speculative connections with as yet mysterious observed objects are made. In particular, we speculate that the recently reported halo white dwarfs might actually be mirror halo stars.']",['2000-11-09'] +402,['eng'],"['Protheroe, R J', 'Mücke, A']",['Application of the synchrotron proton blazar model to BL Lac objects'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'p, cosmic radiation', 'blazar', 'proton synchrotron', 'p, acceleration', 'cosmic radiation, energy spectrum', 'photon, density', 'synchrotron radiation', 'magnetic field', 'photon p, interaction', 'pi, photoproduction', 'electron, pair production', 'luminosity, dependence', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011154'],"['We apply the synchrotron proton blazar (SPB) model to the April 1997 flare of Markarian 501 and find we are able to fit the observed spectral energy distribution. We explore the effect of target photon density on the high energy part of the spectral energy distribution (SED) for fixed assumed magnetic field, emission region size and Doppler factor and find that the luminosity and peak frequency of the high energy part of the SED may depend on the luminosity of the low energy part of the SED in high-frequency peaked BL Lac objects (HBL).']",['2000-11-09'] +403,['eng'],"['Novosyadlyj, B', 'Durrer, R', 'Apunevych, S']",['Constraints on the tensor mode from large scale structure observations'],['Astrophysics and Astronomy'],"['talk, Manchester 2000/08/07', 'inflationary universe, adiabatic', 'cosmic radiation, background', 'cosmic radiation, temperature', 'fluctuation, tensor', 'fluctuation, scalar', 'fluctuation, ratio', 'upper limit', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011149'],['Observational data on the large scale structure (LSS) of the Universe are used to establish an upper limit for the amplitude of the tensor mode marginalized over all other cosmological parameters within the class of adiabatic inflationary models. It is shown that the upper 1$\\sigma$ limit for the contribution of a tensor mode to the COBE DMR data is T/S$<1$.'],['2000-12-20'] +404,['eng'],"['Giovi, F', 'Occhionero, F', 'Amendola, L']",['The Dyer-Roeder distance in quintessence cosmology and the estimation of H_0 through time-delays'],['Astrophysics and Astronomy'],"['supernova', 'quintessence', 'model, fluid', 'time delay', 'astrophysics, fundamental constant', 'matter, density', 'Hubble constant, measurement', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011109'],"['We calculate analytically and numerically the Dyer-Roeder distance in perfect fluid quintessence models and give an accurate fit to the numerical solutions for all the values of the density parameter and the quintessence equation of state. Then we apply our solutions to the estimation of $H_{0}$ from multiple image time delays and find that the inclusion of quintessence modifies sensibly the likelihood distribution of $H_{0}$, generally reducing the best estimate with respect to a pure cosmological constant. Marginalizing over the other parameters ($\\Omega_{m}$ and the quintessence equation of state), we obtain $H_{0}=71\\pm 6$ km/sec/Mpc for an empty beam and $H_{0}=64\\pm 4$ km/sec/Mpc for a filled beam. We also discuss the future prospects for distinguishing quintessence from a cosmological constant with time delays.']",['2000-11-07'] +405,['eng'],"['Olinto, A V']",['From the Galaxy to the Edge of the Universe'],['Astrophysics and Astronomy'],"['talk, Metepec 2000/08/09', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'flux, energy spectrum', 'cosmic radiation, acceleration', 'photon, cosmic radiation', 'p, cosmic radiation', 'galaxy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011106'],['The lack of a high energy cutoff in the cosmic ray spectrum together with an apparently isotropic distribution of arrival directions for the highest energy events have strongly constrained most models proposed for the generation of these particles. An overview of the theoretical proposals are presented along with their most general signatures. Future experimental tests of the different proposals are discussed.'],['2000-11-07'] +406,['eng'],"['Ivanov, A N', 'Oberhummer, H', 'Troitskaya, N I', 'Faber, M']",['Dynamics of low-energy nuclear forces and Solar Neutrino Problems in the Nambu-Jona-Lasinio model of light nuclei'],['Astrophysics and Astronomy'],"['Jona-Lasinio-Nambu model', 'light nucleus, nuclear model', 'deuteron', 'nuclear force', 'neutrino, solar', 'neutrino, flux', 'model, solar', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011103'],"[""The Solar Neutrino Problems (SNP's) are analysed in the Nambu-Jona-Lasinio model of light nuclei. In this model a possible clue to the solution of the SNP's is in the reduction of the solar neutrino fluxes relative to the predicted by the Standard Solar Model through the decrease of the solar core temperature. The former can be realized through the enhancement of the astrophysical factor for the solar proton burning. The enhancement the upper bound of which is restricted by the helioseismological data goes dynamically via the contribution of the nucleon tensor current coupled to the deuteron. The agreement of the reduced solar neutrino fluxes with the experimental data can be reached within a scenario of vacuum two-flavour neutrino oscillations without a fine tuning of the neutrino-flavour oscillation parameters. In the Nambu-Jona-Lasinio model of light nuclei an enhancement of the astrophysical factor for the solar proton burning entails a change of the cross sections for neutrino and anti-neutrino disintegration of the deuteron at low energies. This provides a theoretical foundation for a new check of a value of the astrophysical factor in terrestrial laboratories.""]",['2000-11-07'] +407,['eng'],"['Erlykin, A D', 'Wolfendale, A W']",['Models for the Origin of the Knee in the Cosmic-Ray Spectrum'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'showers, air', 'astrophysics, particle source', 'galaxy', 'supernova', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011057'],"[""A sudden steepening of the cosmic-ray energy spectrum (the knee) is observed at an energy of about 3 PeV (1 PeV = $10^{15}$ eV). The experimental study of the PeV cosmic rays has intensified greatly during the last 3 years. The recent results on extensive air showers allow us to conclude that: a) the knee has an astrophysical origin; b) the `sharpness' and the fine structure of the knee rule out `Galactic Modulation' as the origin of the knee; c) most likely the knee is the result of the explosion of a single, recent, nearby supernova.""]",['2000-11-03'] +408,['eng'],"['Novosyadlyj, B', 'Durrer, R', 'Apunevych, S']",['Constraints on the neutrino mass and the cosmological constant from large scale structure observations'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'neutrino, mass', 'upper limit', 'neutrino, density', 'astrophysics, fundamental constant', 'cosmic radiation, background', 'cosmic radiation, temperature', 'astrophysics, missing-mass', 'inflationary universe', 'spectra, fluctuation', 'statistical analysis', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011055'],"['The observational data on the large scale structure (LSS) of the Universe are used to establish the upper limit on the neutrino content marginalized over all other cosmological parameters within the class of adiabatic inflationary models. It is shown that the upper 2$\\sigma$ limit on the neutrino content can be expressed in the form $\\Omega_{\\nu}h^2/N_{\\nu}^{0.64}\\le0.042$ or, via the neutrino mass, $m_{\\nu}\\le4.0$eV.']",['2000-11-03'] +409,['eng'],"['Ignatius, J', 'Schwarz, Dominik J']",['QCD phase transition and primordial density perturbations'],['Astrophysics and Astronomy'],"['talk, Cheju Island 2000/09/04', 'astrophysics, model', 'quantum chromodynamics, critical phenomena', 'density, perturbation', 'hadron, effect', 'bubble, production', 'cosmic radiation, background', 'light nucleus, production']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011036'],['We analyze the effect of primordial density perturbations on the cosmic QCD phase transition. According to our results hadron bubbles nucleate at the cold perturbations. We call this mechanism inhomogeneous nucleation. We find the typical distance between bubble centers to be a few meters. This exceeds the estimates from homogeneous nucleation by two orders of magnitude. The resulting baryon inhomogeneities may affect primordial nucleosynthesis.'],['2000-11-03'] +410,['eng'],"['Candia, J', 'Epele, L N', 'Roulet, Esteban']",['Cosmic ray photodisintegration and the knee of the spectrum'],['Astrophysics and Astronomy'],"['nucleon, cosmic radiation', 'nucleus, cosmic radiation', 'cosmic radiation, energy spectrum', 'photon nucleus, interaction', 'nucleus, photofission', 'photon, density', 'threshold', 'pi, photoproduction', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011010'],"['We explore in some detail the scenario proposed to explain the observed knee of the cosmic ray (CR) spectrum as due to the effects of photodisintegration of the CR nuclei by interactions with optical and soft UV photons in the source region. We show that the photon column densities needed to explain the experimental data are significantly lower than those obtained in previous estimations which neglected multinucleon emission in the photodisintegration process. We also treat more accurately the photodisintegration thresholds, we discuss the effects of photopion production processes and the neutron escape mechanism, identifying the physical processes responsible for the qualitative features of the results. This scenario would require the CR nuclei to traverse column densities of $\\sim 5 \\times 10^{27}- 2 \\times 10^{28}$ eV/cm$^2$ after being accelerated in order to reproduce the observed knee, and predicts that the CR composition should become lighter above $\\sim 10^{16}$ eV.']",['2000-11-02'] +411,['eng'],"['Zdunik, J L', 'Gourgoulhon, E']",['Small strange stars and marginally stable orbit in Newtonian theory'],['Astrophysics and Astronomy'],"['matter, strangeness', 'rotational', 'orbit, stability', 'gravitation', 'n, matter', 'energy, ratio', 'moment, multipole', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011028'],"[""It is shown that for very rapidly rotating low mass strange stars the marginally stable orbit is located above the stellar surface. This effect is explained by the very important role of the oblateness of the rotating strange star. The comparison with some ``academic'' examples is presented. This feature is purely Newtonian in its nature and has nothing to do with relativistic marginally stable orbit. The effect is very large and cannot be treated in a perturbative way. It seems that strange stars as a very dense self-bound objects are the only possibility in Nature to represent these toy models.""]",['2000-11-02'] +412,['eng'],"['Günther, U', 'Zhuk, A']",['Gravitational Excitons as Dark Matter'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'astrophysics, missing-mass', 'field theory, scalar', 'massive', 'space-time, higher-dimensional', 'excited state, gravitation', 'weak interaction', 'exciton, mass', 'effective potential', 'stability']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011017'],"['In earlier work it was pointed out that for warped product spacetimes the conformal (geometrical moduli) excitations of the internal compactified factor spaces should be observable as massive scalar fields in the external spacetime. Here we show that these scalar fields (gravitational excitons) describe weakly interacting particles and can be considered as dark matter component. Masses of the gravexcitons are defined by the form of the effective potential of the theory and the stabilization scales of the internal space. This implies that different stabilization scales result in different types of DM. An essential role is played by the effective potential. On the one hand, its minima fix possible stabilization scales of the internal spaces; on the other hand, they provide possible values for the effective cosmological constant.']",['2000-11-02'] +413,['eng'],"['Rieger, F M', 'Mannheim, K']",['A possible black hole binary in Mkn 501'],['Astrophysics and Astronomy'],"['blazar', 'black hole, binary', 'black hole, mass', 'upper limit', 'gas, accretion', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0011015'],"['A simple binary model for Mkn~501 is considered under the assumption that the TeV and X-ray periodicity of $\\sim 23$ days, observed during the flaring state in 1997, may be basically interpreted as a doppler-shifted flux modulation due to the orbital motion of the relativistic jet. For the typical jet properties inferred from emission models, we find an intrinsic orbital period of $(6-14)$ yrs and a centre-of-mass distance of $(2-3.5) \\times 10^{16}$ cm, the binary thus being a very close system. If the binary separation corresponds to that at which gravitational radiation becomes dominant, one may obtain a maximum allowed primary mass of $\\sim 10^8 M_{\\odot}$ and a corresponding maximum allowed secondary mass in the range of $\\sim (1-9)\\times 10^7 M_{\\odot}$ assuming that gas accretion occurs on around the salpeter time scale. Interestingly such values agree with the black hole masses expected from merger scenarios.']",['2000-11-02'] +414,['eng'],"['Abu-Zayyad, T', 'Belov, K', 'Bird, D J', 'Boyer, J', 'Cao, Z', 'Catanese, M', 'Chen, G F', 'Clay, R W', 'Covault, C E', 'Dai, H Y', 'Dawson, B R', 'Elbert, J W', 'Fick, B E', 'Fortson, Lucy F', 'Fowler, J W', 'Gibbs, K G', 'Glasmacher, M A K', 'Green, K D', 'Huang, A', 'Jui, C', 'Kidd, M J', 'Kieda, D B', 'Knapp, B C', 'Larsen, C G', 'Lee, W', 'Loh, E C', 'Mannel, E J', 'Matthews, J', 'Matthews, J N', 'Newport, B J', 'Nitz, D F', 'Ong, R A', 'Simpson, K M', 'Smith, J D', 'Sinclair, D', 'Sokolsky, P', 'Sommers, P', 'Song, C', 'Tang, J K K', 'Thomas, S B', 'Der Velde, J', 'Wiencke, L R', 'Wilkinson, C R', 'Yoshida, S', 'Zhang, X Z']",['Measurement of the Cosmic Ray Energy Spectrum and Composition from 10^{17} to 10^{18.3} eV Using a Hybrid Fluorescence Technique'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'cosmic radiation, mass spectrum', 'cosmic radiation, flux', 'showers, air', 'showers, energy', 'showers, spatial distribution', 'time dependence', 'counters and detectors, fluorescence', 'muon, counters and detectors', 'trigger', 'resolution', 'numerical calculations, Monte Carlo', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010652'],"[""We study the spectrum and average mass composition of cosmic rays with primary energies between 10^{17} eV and 10^{18} eV using a hybrid detector consisting of the High Resolution Fly's Eye (HiRes) prototype and the MIA muon array. Measurements have been made of the change in the depth of shower maximum as a function of energy. A complete Monte Carlo simulation of the detector response and comparisons with shower simulations leads to the conclusion that the cosmic ray intensity is changing f rom a heavier to a lighter composition in this energy range. The spectrum is consistent with earlier Fly's Eye measurements and supports the previously found steepening near 4 \\times 10^{17} eV .""]",['2000-11-01'] +415,['eng'],"['Malik, K A', 'Wands, D', 'Lyth, D H', 'Liddle, A R']",['Super-horizon perturbations and preheating'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'space-time, Robertson-Walker', 'perturbation, linear', 'perturbation, scalar', 'conservation law, energy-momentum', 'inflationary universe', 'preheating']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010639'],"['We discuss the evolution of linear perturbations about a Friedmann-Robertson-Walker background metric, using only the local conservation of energy-momentum. We show that on sufficiently large scales the curvature perturbation on spatial hypersurfaces of uniform-density is constant when the non-adiabatic pressure perturbation is negligible. We clarify the conditions under which super-horizon curvature perturbations may vary, using preheating as an example.']",['2000-11-01'] +416,['eng'],"['Bassett, B A', 'Pollifrone, G', 'Tsujikawa, S', 'Viniegra, F']",['Preheating as cosmic magnetic dynamo'],['Astrophysics and Astronomy'],"['inflationary universe', 'preheating', 'magnetic field', 'resonance, production', 'space-time, background', 'space-time, perturbation', 'Maxwell equation', 'symmetry breaking, conformal', 'back reaction', 'Hartree approximation', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010628'],"['We study the amplification of large-scale magnetic fields during preheating and inflation in several different models. Preheating can resonantly amplify seed fields on cosmological scales - a process which is illustrated with scalar QED and geometric magnetisation where amplification of magnetic fields occurs through coupling to curvature invariants. The latter is very efficient during inflation due to a negative coupling instability. Both mechanisms can easily provide the required magnetic fields, and in some cases, over-produce them. Finally we discuss the breaking of the conformal flatness of the background metric whereby magnetic fields can be stimulated through the growth of scalar metric perturbations during metric preheating.']",['2000-11-01'] +417,['eng'],"['Liberati, S', 'Bassett, B A', 'Molina-Paris, C', 'Visser, M']",['Chi-Variable-Speed-of-Light Cosmologies'],['Astrophysics and Astronomy'],"['talk, Villasimius 1999/09/14']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001481'],"[""Variable-Speed-of-Light (VSL) cosmologies are currently attracting much interest as a possible alternative to cosmological inflation. We discuss the fundamental geometrodynamic aspects of VSL cosmologies, and provide several alternative implementations. These implementations provide a large class of VSL cosmologies that pass the zeroth-order consistency tests of being compatible with both classical Einstein gravity and low-energy particle physics. While they solve the ``kinematic'' puzzles as well as inflation does, VSL cosmologies typically do not solve the flatness problem since in their purest form no violation of the strong energy condition occurs. Nevertheless, these models are easy to unify with inflation.""]",['2000-01-28'] +418,['eng'],"['Vergados, J D']",['Searching for Supersymmetric Dark Matter- The Modulation Effect Due to Caustc Rings'],['Astrophysics and Astronomy'],"['talk, Columbia 2000/03/10', 'astrophysics, missing-mass', 'supersymmetry', 'scattering, LSP nucleus', 'differential cross section', 'astrophysics, model', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010598'],['The detection of the theoretically expected dark matter is central to particle physics and cosmology. Current fashionable supersymmetric models provide a natural dark matter candidate which is the lightest supersymmetric particle (LSP). The theoretically obtained event rates are usually very low or even undetectable. So the experimentalists would like to exploit the modulation effect. In the present paper we study a specific class of non-isothermal models involving flows of caustic rings. We find that the modulation effect arising from such models is smaller than that predicted by the isothermal models.'],['2000-10-31'] +419,['eng'],"['Kieda, D B', 'Swordy, S P', 'Wakely, S P']",['A High Resolution Method for Measuring Cosmic Ray Composition beyond 10 TeV'],['Astrophysics and Astronomy'],"['elements, cosmic radiation', 'cosmic radiation, energy', 'radiation, Cherenkov', 'showers, air', 'angular dependence', 'time dependence', 'background', 'Cherenkov counter, imaging', 'charge, resolution', 'angular resolution', 'numerical calculations, Monte Carlo', 'experimental methods, proposed']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010554'],"[""The accurate determination of the elemental composition of cosmic rays at high energies is expected to provide crucial clues on the origin of these particles. Previous direct measurements of composition have been limited by experiment collecting power, resulting in marginal statistics above $10^{14}$ eV, precisely the region where the ``knee'' of the cosmic-ray energy spectrum is starting to develop. In contrast, indirect measurements using extensive air showers can produce sufficient statistics in this region but generate elemental measurements which have relatively large uncertainties. Here we discuss a technique which has become possible through the use of modern ground-based Cerenkov imaging detectors. We combine a measurement of the Cerenkov light produced by the incoming cosmic-ray nucleus in the upper atmosphere with an estimate of the total nucleus energy produced by the extensive air shower initiated when the particle interacts deeper in the atmosphere. The emission regions prior to and after the first hadronic interaction can be separated by an imaging Cerenkov system with sufficient angular and temporal resolution. Monte Carlo simulations indicate an expected charge resolution of $\\Delta Z/Z <5%$ for incident iron nuclei in the region of the ``knee'' of the cosmic-ray energy spectrum. This technique also has the intriguing possibility to unambiguously discover nuclei heavier than iron at energies above 10$^{14}$ eV. The identification and rejection of background produced by charged particles in ground based gamma-ray telescopes is also discussed.""]",['2000-10-30'] +420,['eng'],"['Vergados, J D']",['Searching for SUSY Dark Matter- The Directional Rate and the Modulation Effect'],['Astrophysics and Astronomy'],"['talk, Cascais 2000/06/26', 'astrophysics, missing-mass', 'supersymmetry', 'LSP', 'scattering, LSP nucleus', 'differential cross section', 'sparticle, mass', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010536'],"[""The detection of dark matter is central to particle physics and cosmology. Current fashionable supersymmetric models provide a dark matter candidate, the lightest supersymmetric particle (LSP). When combined with fairly well understood physics (quark structure of the nucleon and some nuclear structure, they yield direct event rates. The obtained rates are, however, very low. So we exploit characteristic signatures, like the modulation effect, i.e. the dependence of the rate on the earth's annual motion, and the directional rate, i.e its dependence on the direction of the recoiling nucleus, employing various velocity distributions, isothermal (symmetric and axially asymmetric) and non isothermal (due to to caustic rings).""]",['2000-10-27'] +421,['eng'],"['Cillis, A N', 'Sciutto, S J']",['Extended Air Showers and Muon Interactions'],['Astrophysics and Astronomy'],"['astrophysics', 'cosmic radiation', 'showers, air', 'muon, bremsstrahlung', 'muon, pair production', 'muon nucleus, nuclear reaction', 'Feynman graph', 'muon, path length', 'differential cross section, energy dependence', 'showers, spatial distribution', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010488'],"['The objective of this work is to report on the influence of muon interactions on the development of air showers initiated by astroparticles. We make a comparative study of the different theoretical approaches to muon bremsstrahlung and muonic pair production interactions. A detailed algorithm that includes all the relevant characteristics of such processes has been implemented in the AIRES air shower simulation system. We have simulated ultra high energy showers in different conditions in order to measure the influence of these muonic electromagnetic interactions. We have found that during the late stages of the shower development (well beyond the shower maximum) many global observables are significantly modified in relative terms when the mentioned interactions are taken into account. This is most evident in the case of the electromagnetic component of very inclined showers. On the other hand, our simulations indicate that the studied processes do not induce significant changes either in the position of the shower maximum or the structure of the shower front surface.']",['2000-10-25'] +422,['eng'],"['Ellis, Jonathan Richard']",['Testing Fundamental Physics with High-Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, La Paz 2000/07/23', 'cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, angular distribution', 'quantum gravity, validity test', 'astrophysics, missing-mass', 'space-time, higher-dimensional', 'membrane model', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010474'],"['Cosmic rays may provide opportunities for probing fundamental physics. For example, ultra-high-energy cosmic rays might originate from the decays of metastable heavy particles, and astrophysical gamma rays can be used to test models of quantum gravity. Both scenarios offer ways to avoid the GZK cut-off.']",['2000-10-25'] +423,['eng'],"['Schwarz, Dominik J', 'Martín, J', 'Riazuelo, A']",['Precision of inflationary predictions and recent CMB anisotropy data'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'moment, multipole', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010453'],['Inflationary predictions of the cosmic microwave background anisotropy are often based on the slow-roll approximation. We study the precision of these predictions and compare them with the recent data from BOOMERanG and MAXIMA-1.'],['2000-10-24'] +424,['eng'],"['Bento, M C', 'Bertolami, O', 'Silva, P T']",['Fitting BOOMERANG and MAXIMA-1 data with a Einstein-Yang-Mills Cosmological Model'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, spectra', 'inflationary universe, higher-dimensional', 'field equations, Yang-Mills', 'Einstein equation', 'spontaneous compactification', 'astrophysics, fundamental constant', 'moment, multipole', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010451'],"['We analyse the implications of recent Cosmic Microwave Background (CMB) data for a specific cosmological model, based on the higher-dimensional Einstein-Yang-Mills System compactified on a $R\\times S^3\\times S^d$ topology and conclude that the model parameters are tightly constrained by CMB spectra. Moreover, the model predicts a relationship between the deceleration parameter at present, $q_0$, and some characteristic features of CMB spectra, namely the height of the first peak and the location of the second peak, that is consistent with the observations and which can be further tested by future CMB and other experiments.']",['2000-10-24'] +425,['eng'],"['Wiltshire, D L']","['Supernovae Ia, evolution and quintessence']",['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'supernova', 'quintessence', 'expansion, acceleration', 'Friedman model', 'luminosity', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010443'],"['Quintessence models with a dark energy generated by pseudo Nambu-Goldstone bosons provide a natural framework in which to test the possibility that type Ia supernovae luminosity distance measurements are at least partially due to an evolution of the sources, since these models can have parameter values for which the expansion of the Universe is decelerating as well as values for which it is accelerating, while being spatially flat in all cases and allowing for a low density of clumped matter. The results of a recent investigation (astro-ph/0004138) of current observational bounds which allow for SNe Ia source evolution are discussed. It is found that models with source evolution still favour cosmologies with an appreciable amount of acceleration in the recent past, but that the region of parameter space which is most favoured shifts significantly.']",['2000-10-24'] +426,['eng'],"['Durrer, R', 'Kunze, K E', 'Sakellariadou, M']",['Particle Creation in Pre-Big-Bang Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'particle, production', 'background field, perturbation', 'magnetic field, galaxy', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'axion, production', 'photon, production', 'string model', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010408'],"[""We present some phenomenological aspects of the pre-big-bang cosmological model inspired by the duality properties of string theory. In particular, assuming the spatial sections of the homogeneous background geometry to be isotropic, we discuss the quantum production of perturbations of the background fields (gravitons, dilatons, moduli fields), as well as the production of particles which do not contribute to the background, which we call ``seeds''. As such we consider the cases of electromagnetic and axionic seeds. We also discuss their possible observational consequences, for example, we study whether they can provide the origin of primordial galactic magnetic fields, and whether they can generate the initial fluctuations leading to the formation of large-scale structure and the measured cosmic microwave background anisotropies. We finally analyze axion and photon production in four dimensional anisotropic pre-big-bang cosmological models.""]",['2000-10-23'] +427,['eng'],"['Crooks, J L', 'Dunn, J O', 'Frampton, Paul H', 'Ng, Y J', 'Rohm, R M']",['CMB with Quintessence'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'quintessence', 'astrophysics, fundamental constant', 'time dependence', 'energy, conservation law', 'matter, density', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010404'],"['A particular kind of quintessence is considered, with equation of motion $p_Q/\\rho_Q = -1$, corresponding to a cosmological term with time-dependence $\\Lambda(t) = \\Lambda(t_0) (R(t_0)/R(t))^{P}$ which we examine initially for $0 \\leq P < 3$. Energy conservation is imposed, as is consistency with big-bang nucleosynthesis, and the range of allowed $P$ is thereby much restricted to $0 \\leq P < 0.2$. The position of the first Doppler peak is computed analytically and the result combined with analysis of high-Z supernovae to find how values of $\\Omega_m$ and $\\Omega_{\\Lambda}$ depend on $P$. Some comparison is made to the CMBFAST public code.']",['2000-10-20'] +428,['eng'],"['Beacom, J F', 'Boyd, R N', 'Mezzacappa, A']",['Black Hole Formation in Core-Collapse Supernovae and Time-of-Flight Measurements of the Neutrino Masses'],['Astrophysics and Astronomy'],"['supernova', 'black hole, production', 'neutrino, cosmic radiation', 'neutrino, flux', 'neutrino, mass', 'mass, measurement', 'antineutrino p, interaction', 'cross section, energy dependence', 'counters and detectors, lead', 'numerical calculations', 'bibliography', 'antineutrino p --> n positron']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010398'],"['Early black hole formation in core-collapse supernovae may be triggered by mass accretion or a change in the high-density equation of state. We consider the possibility that black hole formation happens when the flux of neutrinos is still measurably high. If this occurs, then the neutrino signal from the supernova will be terminated abruptly (the transition takes $\\lesssim 0.5$ ms). The properties and duration of the signal before the cutoff are important measures of both the physics and astrophysics of the cooling proto-neutron star. For the event rates expected in present and proposed detectors, the cutoff will generally appear sharp, thus allowing model-independent time-of-flight mass tests for the neutrinos after the cutoff. If black hole formation occurs relatively early, within a few ($\\sim 1$) seconds after core collapse, then the expected luminosities are of order $L_{BH} = 10^{52}$ erg/s per flavor. In this case, the neutrino mass sensitivity can be extraordinary. For a supernova at a distance $D = 10$ kpc, SuperKamiokande can detect a $\\bar{\\nu}_e$ mass down to 1.8 eV by comparing the arrival times of the high-energy and low-energy neutrinos in $\\bar{\\nu}_e + p \\to e^+ + n$. This test will also measure the cutoff time, and will thus allow a mass test of $\\nu_\\mu$ and $\\nu_\\tau$ relative to $\\bar{\\nu}_e$. Assuming that $\\nu_\\mu$ and $\\nu_\\tau$ are nearly degenerate, as suggested by the atmospheric neutrino results, masses down to about 6 eV can be probed with a proposed lead detector of mass $M_D = 4$ kton (OMNIS). Remarkably, the neutrino mass sensitivity scales as $(D/L_{BH} M_D)^{1/2}$. Therefore, {\\it direct} sensitivity to all three neutrino masses in the interesting few-eV range is realistically possible; {\\it there are no other known techniques that have this capability}.']",['2000-10-20'] +429,['eng'],"['Maeno, T', 'Orito, S', 'Matsunaga, H']",['Successive Measurements of Cosmic-Ray Antiproton Spectrum in a Positive Phase of the Solar Cycle'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'anti-p, cosmic radiation', 'anti-p, energy spectrum', 'model, solar', 'anti-p, flux', 'p, flux', 'flux, ratio', 'anti-p, particle identification', 'spectrometer, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010381'],"['The energy spectrum of cosmic-ray antiprotons has been measured by BESS successively in 1993, 1995, 1997 and 1998. In total, 848 antiprotons were clearly identified in energy range 0.18 to 4.20 GeV. From these successive measurements of the antiproton spectrum at various solar activity, we discuss about the effect of the solar modulation and the origin of cosmic-ray antiprotons. Measured antiproton ratios were nearly identical during this period, and were consistent with a prediction taking the charge dependent solar modulation into account.']",['2000-10-20'] +430,['eng'],"['Mitra, A']",['General Relativistic Collapse of Neutron Stars to Strange Stars'],['Astrophysics and Astronomy'],"['n, matter', 'matter, strangeness', 'gravitation, effect', 'relativity theory, general', 'binding energy', 'fireball, electromagnetic', 'neutrino antineutrino, annihilation', 'gamma ray burst']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010311'],"[""It is known that Neutron Stars may be converted into more compact Strange Stars (SS) on capture/formation of a ``seed'' of strange matter. It is also known that the binding energy of the nascent hot SS is likely to be radiated as $\\nu -\\bar\\nu$s so that an electromagnetic pair fireball (FB) may be created by neutrino annihilation. And already this process has been considered as a probable source of Gamma Ray Bursts (GRB) by several authors, the most notable of which is due to Cheng & Dai (PRL, 77, 1210, 1996). They mentioned that this process may generate a FB luminosity (outside the neutrinosphere) of 10**(49) erg. But we point out here that a SS is a relativistic object with surface gravitation z=0.5. Accordingly, we present here a Relativistic Model of this process, and show that, for a massive SS with M=2 solar mass, one may explain a GRB energy of ~ 10**(53) erg., which is 4 orders higher than previous non-relativistic estimate. Further since the baryonic mass of the thin crust of a strange star is negligible, this FB will generate an extremely relativistic blast wave. Thus this process may be one of the viable routes for the genesis of hitherto unexplained cosmic Gamma Ray Bursts. While some of the GRBs might be beamed, many of them do not show any long term spectral break in their afterglows and are likely to be quasi-spherical. A particular example is GRB 971214 for which estimated GRB energy is 3. 10**(53) erg. Our model may be useful for understanding the genesis of such powerful and unexplained bursts.""]",['2000-10-17'] +431,['eng'],"['Farrar, Glennys R S', 'Piran, T']",['Deducing the Source of Ultrahigh Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'galaxy', 'magnetic field', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010370'],"['The apparent lack of suitable astrophysical sources for cosmic rays with E > 10^{19.7} eV (UHECRs) is the ""GZK Paradox"". We argue that whatever mechanism produces them must also account for events down to ~10^{18.7} eV, including their isotropy and spectral smoothness. This rules out galactic sources, distributed sources such as topological defects, and Gamma Ray Bursts (GRBs). We are lead to identify the powerful radio galaxy Cen A, at 3.4 Mpc, as the probable source of most UHECRs observed at Earth today, and to estimate the extragalactic magnetic field to be ~0.3 microG.']",['2000-10-19'] +432,['eng'],"['Mannheim, K']",['Neutrinos from Gamma Ray Bursts'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'cosmic radiation, flux', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'gamma ray burst', 'p, cosmic radiation', 'neutrino, flux', 'upper limit', 'photon p, interaction', 'pi, photoproduction', 'neutrino, particle source', 'counters and detectors', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010353'],"['The observed fluxes of cosmic rays and gamma rays are used to infer the maximum allowed high-energy neutrino flux allowed for Gamma Ray Bursts (GRBs), following Mannheim, Protheroe, and Rachen (2000). It is shown that if GRBs produce the ultrahigh-energy cosmic rays, they should contribute (a) at least 10% of the extragalactic gamma ray background between 3 MeV and 30 GeV, contrary to their observed energy flux which is only a minute fraction of this flux, and (b) a cumulative neutrino flux a factor of 20 below the AMANDA (Neutrino 2000) limit on isotropic neutrinos. This could have two implications, either GRBs do not produce the ultrahigh energy cosmic rays or that the GRBs are strongly beamed and emit most of their power at energies well above 100 GeV implausibly increasing the energy requirements, but consistent with the marginal detections of a few low-redshift GRBs by MILAGRITO, HEGRA-AIROBICC, and the Tibet-Array. All crucial measurements to test the models will be available in the next few years. These are measurements of (i) high-energy neutrinos with AMANDA-ICECUBE or an enlarged ANTARES/NESTOR ocean detector, (ii) GRB redshifts from HETE-2 follow-up studies, and (iii) GRB spectra above 10 GeV with low-threshold imaging air Cherenkov telescopes such as MAGIC and the space telescopes AGILE and GLAST.']",['2000-10-19'] +433,['eng'],"['Cline, David B']",['Is the LMA solar-neutrino solution ruled out by SN1987A data?'],['Astrophysics and Astronomy'],"['talk, Otranto 2000/09/09', 'neutrino, solar', 'supernova', 'neutrino, cosmic radiation', 'neutrino, mixing angle', 'neutrino/tau', 'neutrino/mu', 'deep underground detector', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010339'],"['The development of new supernova neutrino detectors relies on the expected hard energy spectrum of the nu_mu and nu_tau emitted in the supernova. We show that SN1987A was sensitive to the large mixing angle (LMA) and ""just so"" solution to the solar neutrino problem. We review the previous analysis of the SN1987A data and propose a new analysis. The results of this analysis strongly disfavor the LMA solution, provided the nu_mu and nu_tau are hard as predicted']",['2000-10-18'] +434,['eng'],"['Wang, X Y', 'Dai, Z G', 'Lu, T']",['Prompt High Energy $\\gamma$-Ray Emission From the Synchrotron Self-Compton Process in the Reverse Shocks of $\\gamma$-Ray Bursts'],['Astrophysics and Astronomy'],"['astrophysics', 'gamma ray burst', 'photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'synchrotron radiation', 'Compton scattering', 'fireball', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010320'],"['In the standard scenario of the fireball model of gamma-ray bursts(GRBs), the huge initial energy release produces a relativistic blast wave expanding into the external medium and a reverse shock moving into and heating the fireball ejecta. We calculate the high energy gamma-ray emission due to inverse Compton scattering of the synchrotron photons from relativistic electrons in the reverse shock. Under the favorable values of the physical parameters of the GRBs and the interstellar medium, our result shows that during the prompt phase, this emission dominates over the component from the forward shock at high energy gamma-ray bands. This mechanism can excellently account for the observations of the prompt high energy gamma-rays detected by EGRET, such as from GRB930131.']",['2000-10-18'] +435,['eng'],"['Steer, D A']",['Strings after D-term inflation'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'astrophysics, string', 'inflationary universe', 'string, chiral', 'field theory, scalar']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010295'],"['We motivate the study of chiral cosmic strings through a scenario of structure formation which mixes D-term inflation and strings. We then discuss some properties of chiral cosmic strings, and results regarding their evolution and possible cosmological consequences are presented.']",['2000-10-17'] +436,['eng'],"['De Naurois, M']",['Status and Current Sensitivity of the CELESTE Experiment'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'cosmic radiation, energy', 'track data analysis', 'trigger', 'threshold', 'numerical calculations, Monte Carlo', 'Cherenkov counter, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010265'],['The CELESTE experiment uses the heliostats of an old solar farm in the French Pyrenees to detect gamma ray air showers by the atmospheric Cerenkov technique. CELESTE has been operating since November 1999 with an array of 40 heliostats fully instrumented with 1GHz flash ADCs. Significant advances have been made in the detector simulations and in the data analysis techniques. We report here on results from recent observations of the Crab nebula above an energy threshold of 50GeV. The results and simulations illustrate the current sensitivity of the experiment.'],['2000-10-16'] +437,['eng'],"['Holder, J']",['Observations of Mkn 421 with the CELESTE Experiment'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000/06/26', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'blazar', 'cosmic radiation, time variation', 'Cherenkov counter, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010264'],['The CELESTE experiment uses the heliostats of an old solar farm in the French Pyrenees to detect gamma ray air showers by the atmospheric Cerenkov technique. Observations of the TeV blazar Markarian 421 have been made with the fully instrumented CELESTE experiment since December 1999. The detection of gamma ray emission from this source at energies greater than 50 GeV is presented here. A comparison is made with the light curve from the CAT experiment at the same site which shows correlation between the observed gamma ray fluxes and the detection of short duration flaring episodes.'],['2000-10-16'] +438,['eng'],"['Barancourt, D', 'Barão, F', 'Barbier, G', 'Barreira, G', 'Buénerd, M', 'Castellini, G', 'Choumilov, E', 'Favier, J', 'Fouque, N', 'Gougas, A', 'Hermel, V', 'Kossakowski, R', 'Laborie, G', 'Laurenti, G', 'Lee, S C', 'Mayet, F', 'Meillon, B', 'Oyang, J Y T', 'Plyaskin, V', 'Pozhidaev, V', 'Rossin, C', 'Santos, D', 'Vezzu, F', 'Vialle, J P']",['The AMS-01 Aerogel Threshold Cherenkov counter'],['Astrophysics and Astronomy'],"['antimatter, cosmic radiation', 'counters and detectors, satellite', 'particle identification, (p positron)', 'Cherenkov counter, threshold', 'Cherenkov counter, aerogel', 'electronics']","['http://arXiv.org/ps/astro-ph/0010242', 'http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010242']","['The Alpha Magnetic Spectrometer in a precursor version (AMS-01), was flown in June 1998 on a 51.6 degrees orbit and at altitudes ranging between 320 and 390 km, on board of the space shuttle Discovery (flight STS-91). AMS-01 included an Aerogel Threshold Cherenkov counter (ATC) to separate antiprotons from electrons and positrons from protons, for momenta below 3.5 GeV/c. This paper presents a description of the ATC counter and reports on its performances during the flight STS-91.']",['2000-10-13'] +439,['eng'],"['Virmani, A', 'Bhattacharya, S', 'Jain, P L', 'Razzaque, S', 'Ralston, J P', 'McKay, D W']",['Correlation of Ultra High Energy Cosmic Rays with Compact Radio Loud Quasars'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'astrophysics, quasar', 'angular correlation', 'statistical analysis', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010235'],"['Angular correlations of ultra-high energy cosmic rays with cosmologically distant sources may provide clues to these mysterious events. We compare cosmic ray tracks with energies above $ 10^{20}eV$ to a compilation of radio-loud compact QSO positions. The statistical method emphasizes invariant quantities and a test of {\\it statistical independence} of track and source distributions. Statistical independence is ruled out by several independent statistics at confidence levels of less that $10^{-3}$ ($99.9% $.), indicating that track directions and QSO source positions are correlated at a highly significant level.']",['2000-10-13'] +440,['eng'],"['Matos, T', 'Urena-Lopez, L A']","['Scalar Field Dark Matter, Cross Section and Planck-Scale Physics']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'field theory, scalar', 'potential, renormalization', 'scattering, missing-mass', 'cross section', 'galaxy']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010226'],"['In recent papers we have proposed that the dark matter of the Universe could be from scalar field origin. In this letter, we find that if the scale of renormalization of the model is of order of the Planck Mass, then a scalar field $\\Phi $ endowed with the scalar potential $V=V_{o}[\\cosh {(\\lambda \\sqrt{\\kappa_{0}}\\Phi)}-1] can be a reliable model for dark matter in galaxies. The predicted scattering cross section fits the value required for self-interacting dark matter and the additional degree of freedom of the theory is of order of hundreds of TeV.']",['2000-10-12'] +441,['eng'],"['De Jager, O C', 'Konopelko, A K', 'Raubenheimer, B C', 'Visser, B']",['Prospects of observing pulsed radiation from gamma-ray pulsars with H.E.S.S'],['Astrophysics and Astronomy'],"['talk, Heidelberg 2000', 'pulsar', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'photon, flux', 'proposed experiment']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010179'],"['Observations and theoretical studies have demonstrated that the pulsed spectra of all gamma-ray pulsars terminate at energies below a few hundred GeV. In most cases we expect this cutoff energy E_o to be around 10 GeV. Only with next generation ground-based gamma-ray telescopes, which are expected to have non-zero trigger probabilities near 10 GeV, can we expect to detect pulsations. The large gamma-ray fluxes below E_o, together with the associated sharp pulse profiles, compensate for the lack of imaging capability near threshold. For H.E.S.S. we find that the pulsed component of PSR B1706-44 should be detectable near threshold, whereas the unidentified GeV EGRET sources should be detectable if the superexponential cutoff energy is larger that approximately 30 GeV for relatively hard pulsar photon spectra (~E^-1.5).']",['2000-10-11'] +442,['eng'],"['Lachièze-Rey, M']",['The Friedmann-Lemaitre models in perspective'],['Astrophysics and Astronomy'],"['Friedman model', 'space-time, Robertson-Walker', 'dimension, 5', 'space-time, Minkowski', 'space-time, de Sitter', 'space-time, embedding']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010163'],"['I show that all FRW models (four dimensional pseudo-Riemannian manifolds with maximally symmetric space) can be embedded in a flat Minkowski manifold with 5 dimensions. The pseudo Riemannian metric of space-time is induced by the flat metric. This generalizes the usual embedding widely used for the \\dS ~models. I give the coordinate transformations for the embedding. Taking into account the spatial isotropy, one can reduce space-time to a two-dimensional surface, embedded in a three-dimensional Minkowski space. This allows to give exact graphic representations of the FRW models, and in particular of their curvature.']",['2000-10-10'] +443,['eng'],"['Burles, S M', 'Nollett, K M', 'Turner, M S']",['What Is The BBN Prediction for the Baryon Density and How Reliable Is It?'],['Astrophysics and Astronomy'],"['astrophysics, model', 'baryon, density', 'light nucleus, production', 'deuterium, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008495'],"['Together, the standard theory of big-bang nucleosynthesis (BBN) and the primeval deuterium abundance very precisely peg the baryon density, Omega_B h^2 = 0.0190\\pm 0.0018 (95% cl). The uncertainty is due to that in the deuterium abundance and input nuclear data, in the ratio of about 2 to 1. We discuss critically the reliability of the BBN baryon density, and conclude that within the standard cosmology and standard theory of BBN a baryon density Omega_B h^2 = 0.030 (the central value implied by recent CMB anisotropy measurements) simply cannot be accommodated.']",['2000-08-31'] +444,['eng'],"['Cline, David B']",['Liquid Xenon for a Very Sensitive WIMP Search'],['Astrophysics and Astronomy'],"['talk, Verbier 2000/07/17', 'astrophysics, missing-mass', 'search for, WIMP', 'scintillation counter, liquid', 'xenon', 'deep underground detector, Boulby']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010124'],"['We describe the research and development efforts of the UCLA Torino group to develop a large, powerful, discriminating WIMP detector. We also discuss the possible amplifications of the WIMP signal. The first real detector, ZEPLIN II, is being prepared for the UKDMC Boulby Mine Laboratory.']",['2000-10-09'] +445,['eng'],"['Viana, P T P']",['Constraints on Inflation'],['Astrophysics and Astronomy'],"['talk, Cargese 2000/04/25', 'inflationary universe', 'density, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation, measurement', 'background, stochastic', 'energy, density', 'interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009492'],"['A short introduction to structure formation is given, followed by a discussion of the possible characteristics of the initial perturbations assuming a generic inflationary origin. Observational data related to large-scale structure and the cosmic microwave background radiation is then used in an attempt to constrain the characteristics of such perturbations. Future directions are also explored. The possibility of direct detection of a stochastic gravitational wave background produced during an inflationary phase in the early Universe is briefly discussed, as well as the available evidence regarding the present value of the total energy density in the Universe.']",['2000-10-02'] +446,['eng'],"['Liddle, A R']",['Acceleration of the Universe'],['Astrophysics and Astronomy'],"['lectures, Cargese 2000/04/25', 'inflationary universe', 'expansion, acceleration', 'matter, density', 'field theory, scalar', 'density, perturbation', 'gravitational radiation', 'cosmic radiation, background', 'quintessence']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009491'],[],['2000-10-02'] +447,['eng'],"['Boratav, M', 'Watson, A A']",['Cosmic Rays above $10^{14}$ eV'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'showers, air', 'elements, cosmic radiation', 'cosmic radiation, mass', 'cosmic radiation, particle source', 'interpretation of experiments', 'proposed experiment']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009469'],"[""We briefly review the status of cosmic ray studies between $10^{14}$ eV and the highest observed energies, namely a few times $10^{20}$ eV. Because of the rather low incident fluxes in this energy range, the studies mostly rely on ground based, large aperture detectors reconstructing the cosmic ray's properties through the detection of the air-showers they generate by interacting with the atmosphere. We stress the fact that many issues such as the chemical composition of the cosmic rays, their acceleration mechanisms, the structures displayed in their energy spectrum are mostly open questions which may be answered by the next generation of experiments.""]",['2000-09-29'] +448,['eng'],"['Blanton, M R', 'Blasi, P', 'Olinto, A V']",['The GZK Feature in our Neighborhood of the Universe'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'galaxy', 'cosmic radiation, acceleration', 'numerical calculations, interpretation of experiments', 'proposed experiment']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009466'],"['We calculate numerically the spectrum of ultra-high energy cosmic rays on Earth assuming that their sources are distributed in space like the observed galaxies. We use the CfA2 and the PSCz galaxy redshift surveys to model the local galaxy distribution, properly taking into account the galaxy selection functions for each survey. When the survey selection effects are included, we find that the local overdensity is only a factor of two, an order of magnitude less than used in some earlier studies. An overdensity of two is not enough to bridge the gap between the predicted number of events above $10^{20}$ eV and the measured flux at these highest energies. This conclusion is particularly strong for soft injection spectra ($\\propto E^{-3}$) where the observed number of events is 6 $\\sigma$ higher than the expected one. However, if the injection spectrum is hard ($\\propto E^{-2}$), the small local overdensity helps bring the present data within 2$\\sigma$ of the low number of events predicted above $10^{20}$ eV. In this case, the Greisen-Zatzepin-Kuzmin cutoff is not a {\\it cutoff} but rather a {\\it feature} in the cosmic ray spectrum.']",['2000-09-29'] +449,['eng'],"['Asano, K', 'Fukuyama, T']",['Relativistic Effects on Neutrino Pair Annihilation above a Kerr Black Hole with the Accretion Disk'],['Astrophysics and Astronomy'],"['black hole, Kerr', 'neutrino antineutrino, annihilation', 'energy', 'effect, relativistic', 'neutrino, emission', 'accretion', 'photon, cosmic radiation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009453'],"[""Using idealized models of the accretion disk we investigate the relativistic effects on the energy deposition rate via neutrino pair annihilation near the rotation axis of a Kerr black hole. Neutrinos are emitted from the accretion disk. The bending of neutrino trajectories and the redshift due to the disk rotation and gravitation are taken into consideration. The Kerr parameter, $a$, affects not only neutrinos' behavior but also the inner radius of the accretion disk. When the deposition energy is mainly contributed by the neutrinos coming from the central part, the redshift effect becomes dominant as $a$ becomes large and the energy deposition rate is reduced compared with that neglecting the relativistic effects. On the other hand, for small $a$ the bending effect gets dominant and makes energy increase by factor 2 compared with that neglecting the relativistic effects. For the disk with temperature gradient, the energy deposition rate for a small inner radius of the accretion disk is smaller than that estimated by neglecting the relativistic effects. The relativistic effects, especially for large $a$, play a negative role in avoiding the baryon contamination problem in gamma-ray bursts.""]",['2000-09-29'] +450,['eng'],"['Balberg, S', 'Farrar, Glennys R S', 'Piran, T']","['Neutron Stars with a Stable, Light Supersymmetric Baryon']",['Astrophysics and Astronomy'],"['n, matter', 'astrophysics, missing-mass', 'gluino', 'supersymmetry', 'baryon, sparticle', 'baryon, density', 'hyperon, matter', 'energy, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010112'],"['If a light gluino exists, the lightest gluino-containing baryon, the ${\\rm S}^0$, is a possible candidate for self-interacting dark matter. In this scenario, the simplest explanation for the observed ratio $\\Omega_{dm}/\\Omega_b \\approx 6-10$ is that $m_{S^0} \\sim 900 $MeVc$^{-2}$; this is not at present excluded by particle physics. Such an ${\\rm S}^0$ could be present in neutron stars, with hyperon formation serving as an intermediate stage. We calculate equilibrium compositions and equation of state for high density matter with ${\\rm S}^0$, and find that for a wide range of parameters the properties of neutron stars with the ${\\rm S}^0$ are consistent with observations. In particular, the maximum mass of a nonrotating star is $1.7-1.8 M_\\odot$, and the presence of the ${\\rm S}^0$ is helpful in reconciling observed cooling rates with hyperon formation.']",['2000-10-06'] +451,['eng'],"['Leach, S M', 'Liddle, A R']",['Inflationary perturbations near horizon crossing'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'horizon, crossing', 'field theory, scalar', 'entropy, perturbation', 'black hole, production', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010082'],"['We study the behaviour of inflationary density perturbations in the vicinity of horizon crossing, using numerical evolution of the relevant mode equations. We explore two specific scenarios. In one, inflation is temporarily ended because a portion of the potential is too steep to support inflation. We find that perturbations on super-horizon scales can be modified, usually leading to a large amplification, because of entropy perturbations in the scalar field. This leads to a broad feature in the power spectrum, and the slow-roll and Stewart-Lyth approximations, which assume the perturbations reach an asymptotic regime well outside the horizon, can fail by many orders of magnitude in this regime. In the second scenario we consider perturbations generated right at the end of inflation, which re-enter shortly after inflation ends -- such perturbations can be relevant for primordial black hole formation.']",['2000-10-05'] +452,['eng'],"['Chimento, L P', 'Jakubi, A S', 'Pavón, D']",['Quintessence Energy and Dissipation'],['Astrophysics and Astronomy'],"['talk, Lisbon 2000/07/12', 'supernova', 'expansion, acceleration', 'energy, quintessence', 'fluid, dissipation', 'tensor, energy-momentum', 'astrophysics, missing-mass']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010079'],['The combined effect of a dissipative fluid and quintessence energy can simultaneously drive an accelerated expansion phase at the present time and solve the coincidence problem of our current Universe. A solution compatible with the observed cosmic acceleration is succinctly presented.'],['2000-10-05'] +453,['eng'],"['Harari, D', 'Mollerach, S', 'Roulet, Esteban']",['Magnetic lensing of ultra high energy cosmic rays'],['Astrophysics and Astronomy'],"['talk, Metepec 2000/08/09', 'cosmic radiation, lens', 'magnetic field, galaxy', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010068'],"['We discuss several effects due to lensing of ultra high energy cosmic rays by the regular component of the galactic magnetic field. Large flux magnification around caustics can be a significant source of clustering in the arrival directions of UHECRs of comparable energy. We also discuss lensing effects in a hypothetical galactic magnetic wind model recently proposed to explain the extremely high energy cosmic rays so far observed as originating from a single source (M87). This model implies large flux magnifications, which reduce the power requirements on the source, and a significant asymmetry in the expected flux between the north and south galactic hemispheres.']",['2000-10-04'] +454,['eng'],"['Calcaneo-Roldan, C', 'Moore, B']",['The surface brightness of dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutralino, annihilation', 'galaxy', 'photon, cosmic radiation', 'photon, background', 'cosmic radiation, flux', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010056'],"['We use high resolution numerical simulations of the formation of cold dark matter halos to simulate the background of decay products from neutralino annihilation, such as gamma-rays or neutrinos. Halos are non-spherical, have steep singular density profiles and contain many thousands of surviving dark matter substructure clumps. This leads to several unique signatures in the gamma-ray background that may be confirmed or rejected by the next generation of gamma-ray experiments. Most importantly, the diffuse background is enhanced by over two orders of magnitude due to annihilation within substructure halos. The largest dark substructures are easily visibly above the background and may account for the unidentified EGRET sources. A deep strip survey of the gamma-ray background would allow the shape of the Galactic halo to be quantified.']",['2000-10-04'] +455,['eng'],"['Blasi, P']",['Dark matter distribution in the universe and ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['talk, Metepec 2000/08/09', 'astrophysics, missing-mass', 'cosmic radiation, spectra', 'cosmic radiation, particle source', 'postulated particle, heavy', 'postulated particle, decay', 'cosmic radiation, production', 'galaxy, density', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010050'],"['Two of the greatest mysteries of modern physics are the origin of the dark matter in the universe and the nature of the highest energy particles in the cosmic ray spectrum. We discuss here possible direct and indirect connections between these two problems, with particular attention to two cases: in the first we study the local clustering of possible sources of ultra-high energy cosmic rays (UHECRs) driven by the local dark matter overdensity. In the second case we study the possibility that UHECRs are directly generated by the decay of weakly unstable super heavy dark matter.']",['2000-10-03'] +456,['eng'],"['Horowitz, C J', 'Li, G']",['Charge Conjugation Violation in Supernovae and The Neutron Shortage for R-Process Nucelosynthesis'],['Astrophysics and Astronomy'],"['talk, Quebec 2000/05/22', 'supernova', 'neutrino nucleon, interaction', 'neutrino, capture', 'antineutrino, capture', 'channel cross section', 'charge conjugation, violation', 'light nucleus, production', 'n, density']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010042'],"['Core collapse supernovae are dominated by energy transport from neutrinos. Therefore, some supernova properties could depend on symetries and features of the standard model weak interactions. The cross section for neutrino capture is larger than that for antineutrino capture by one term of order the neutrino energy over the nucleon mass. This reduces the ratio of neutrons to protons in the $\\nu$-driven wind above a protoneutron star by approximately 20 % and may significantly hinder r-process nucleosynthesis.']",['2000-10-03'] +457,['eng'],"['Stecker, F W']",['TeV Gamma-Ray Absorption and the Intergalactic Infrared Background'],['Astrophysics and Astronomy'],"['talk, Manchester 2000/08/15', 'photon, cosmic radiation', 'photon, absorption', 'cosmic radiation, background', 'galaxy', 'cosmic radiation, energy spectrum', 'symmetry breaking, Lorentz', 'cosmic radiation, opacity', 'blazar', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0010015'],[],['2000-10-03'] +458,['eng'],"['Copi, C J', 'Krauss, L M']",['Angular Signatures for Galactic Halo WIMP Scattering in Direct Detectors'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, search for', 'counters and detectors', 'signal processing', 'background', 'scattering, WIMP nucleus', 'form factor', 'differential cross section', 'spin, dependence', 'angular distribution', 'nucleus, recoil', 'threshold, energy', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009467'],"['Angular Sensitivity can provide a key additional tool which might allow unambiguous separation of a signal due to Galactic halo WIMPs from other possible backgrounds in direct detectors. We provide a formalism which allows a calculation of the expected angular distribution of events in terrestrial detectors with angular sensitivity for any incident distribution of Galactic halo dark matter. This can be used as an input when studying the sensitivity of specific detectors to halo WIMPs. We utilize this formalism to examine the expected signature for WIMP dark matter using a variety of existing analytic halo models in order to explore how uncertainty in the Galactic halo distribution impact on the the event rates that may be required to separate a possible WIMP signal from other terrestrial backgrounds. We find that as few as 30 events might be required to disentangle the signal from backgrounds if the WIMP distribution resembles an isothermal sphere distribution. On the other hand, for certain halo distributions, even detectors with fine scale resolution may require in excess of a 100-400 events to distinguish a WIMP signal from backgrounds using angular sensitivity. We also note that for finite thresholds the different energy dependence of spin-dependent scattering cross sections may require a greater number of events to discern a WIMP signal than for spin independent interactions. Finally, we briefly describe ongoing studies aimed at developing strategies to better exploit angular signatures, and the use of N-body simulations to better model the expected halo distribution in predicting the expected signature for direct WIMP detectors.']",['2000-09-29'] +459,['eng'],"['Thompson, T A', 'Burrows, A']",['Neutrino Processes in Supernovae and the Physics of Protoneutron Star Winds'],['Astrophysics and Astronomy'],"['talk, Aarhus 2000/06/27', 'supernova', 'n, matter', 'nuclear matter', 'neutrino/mu, production', 'neutrino/tau, production', 'neutrino electron, interaction', 'electron positron, annihilation', 'nucleon nucleon, bremsstrahlung', 'neutrino nucleon, interaction', 'velocity', 'baryon, entropy', 'expansion, acceleration', 'light nucleus, production', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009449'],"['In preparation for a set of hydrodynamical simulations of core-collapse supernovae and protoneutron star winds, we investigate the rates of production and thermalization of $\\nu_\\mu$ and $\\nu_\\tau$ neutrinos in dense nuclear matter. Included are contributions from electron scattering, electron-positron annihilation, nucleon-nucleon bremsstrahlung, and nucleon scattering. We find that nucleon scattering dominates electron scattering as a thermalization process at neutrino energies greater than $\\sim$15 MeV. In addition, nucleon-nucleon bremsstrahlung dominates electron-positron annihilation as a production mechanism at low neutrino energies, near and below the $\\nu_\\mu$ and $\\nu_\\tau$ neutrinospheres. Furthermore, we have begun a study of steady-state general relativistic protoneutron star winds employing simple neutrino heating and cooling terms. From this analysis we obtain acceleration profiles as well as asymptotic lepton fractions and baryon entropies essential in assessing the wind as a potential site for $r$-process nucleosynthesis.']",['2000-09-29'] +460,['eng'],"['Letessier-Selvon, A A']",['Establishing The GZK Cutoff With Ultra High Energy Tau Neutrinos'],['Astrophysics and Astronomy'],"['talk, Metepec 2000/08/09', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'neutrino/tau', 'neutrino/mu', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'photon p, interaction', 'pi, photoproduction', 'charged particle, acceleration', 'showers, air', 'Cherenkov counter', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009444'],"['The cosmic ray spectrum has been shown to extend well beyond 10^20 eV. With nearly 20 events observed in the last 40 years, it is now established that particles are accelerated or produced in the universe with energy near 10^21 eV. In all production models neutrinos and photons are part of the cosmic ray flux. In acceleration models (bottom-up models), they are produced as secondaries of the possible interactions of the accelerated charged particle, in direct production models (top-down models) they are a dominant fraction of the decay chain. In addition, hadrons above the GZK threshold energy will also produce, along their path in the Universe, neutrinos and photons as secondaries of the pion photo-production processes. Therefore, photons and in particular neutrinos, are very distinctive signatures of the nature and distribution of the potential sources of ultra high energy cosmic rays. In the following we expose the identification capabilities of the Auger observatories. In the hypothesis of nu_mu-->nu_tau oscillations with full mixing, special emphasis is placed on the observation of tau neutrinos, with which Auger is able to establish the GZK cutoff as well as to provide a strong and model independant constraint on the top-down sources of ultra high energy cosmic rays.']",['2000-09-28'] +461,['eng'],"['Balbi, A', 'Baccigalupi, C', 'Matarrese, S', 'Perrotta, F', 'Vittorio, N']",['Implications on quintessence models from MAXIMA-1 and BOOMERANG-98'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'supernova', 'quintessence', 'energy, density', 'inflationary universe, adiabatic', 'astrophysics, fundamental constant', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009432'],"['Prompted by the recent MAXIMA-1 and BOOMERANG-98 measurements of the cosmic microwave background (CMB) anisotropy power spectrum, and motivated by the results from the observation of high-redshift Type Ia supernovae, we investigate CMB anisotropies in quintessence models in order to characterize the nature of the dark energy today. We perform a Bayesian likelihood analysis, using the MAXIMA-1 and BOOMERANG-98 published bandpowers, in combination with COBE/DMR, to explore the space of quintessence parameters: the quintessence energy density \\Omega_\\phi and equation of state w_\\phi. We restrict our analysis to flat, scale-invariant, inflationary adiabatic models. We find that this simple class of inflationary models, with a quintessence component \\Omega_\\phi < 0.7, -1 < w_\\phi < -0.5, is in good agreement with the data. Within the assumptions of our analysis, pure quintessence models seem to be slightly favored, although the simple cosmological constant scenario is consistent with the data.']",['2000-09-28'] +462,['eng'],"['Popa, L', 'Burigana, C', 'Finelli, F', 'Mandolesi, N']",['On the detection of neutrino oscillations with Planck surveyor'],['Astrophysics and Astronomy'],"['neutrino, oscillation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'polarization', 'astrophysics, model', 'lepton, asymmetry', 'neutrino, mass difference', 'neutrino, mixing angle', 'numerical calculations', 'proposed experiment, satellite', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009417'],"['The imprint of neutrino oscillations on the Cosmic Microwave Background (CMB) anisotropy and polarization power spectra is evaluated in a $\\Lambda$CHDM model with two active neutrino flavors, consistent with the structure formation models and the atmospheric neutrino oscillations data. We show the existence of a significant overlap between the region of the oscillation parameter space that can be measured by sc Planck surveyor and that implied by the atmospheric neutrino oscillations data.']",['2000-09-27'] +463,['eng'],"['Letessier-Selvon, A A']",['Neutrinos and the Highest Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Sudbury 2000/06/16', 'cosmic radiation, primary', 'energy spectrum, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'postulated particle, massive', 'counters and detectors', 'showers, air', 'neutrino, flux', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009416'],"[""Observation of Ultra High Energy Cosmic Rays (UHECR) -whose energy exceeds $10^20$eV- is still a puzzle for modern astrophysics. The transfer of more than 16 Joules to a microscopic particle can hardly be achieved, even in the most powerful cosmic accelerators such as AGN's, GRB's or FR-II radio galaxy lobes. Potential sources must also lie within 100 Mpc of the Earth as the interaction length of protons, nuclei or photons is less than 10Mpc. However no visible counterpart of those sources has been observed. Calling upon new physics such as Topological Defect interactions or Super Massive Relic Particle decays is therefore very tempting, but such objects are yet to be proven to exist. Due to the very low flux of UHECR only very large dedicated experiments, such as the Auger observatories, will allow to shed some light on the origin of those cosmic rays. In this quest neutrinos, if they can be detected, are an invaluable messengers of the nature of the sources.""]",['2000-09-27'] +464,['eng'],"['Dolgov, A D', 'Naselsky, P D', 'Novikov, I D']","['Gravitational waves, baryogenesis, and dark matter from primordial black holes']",['Astrophysics and Astronomy'],"['astrophysics, model', 'baryon, asymmetry', 'entropy, production', 'black hole, radiation', 'astrophysics, missing-mass', 'graviton, energy', 'energy, density', 'gravitational radiation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009407'],['We discuss the hypothesis that the cosmological baryon asymmetry and entropy were produced in the early Universe by the primordial black hole (PBHs) evaporation.'],['2000-09-27'] +465,['eng'],"['Levinson, A']","['UHECR Production and Curvature TeV Emission in Nearby, Dormant AGNs']",['Astrophysics and Astronomy'],"['black hole, rotational', 'quasar', 'cosmic radiation, production', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'cosmic radiation, acceleration', 'galaxy, AGN', 'energy loss']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009383'],"['The possibility that rapidly rotating supermassive black holes associated with quasar remnants may provide sites for the acceleration of ultra-high energy cosmic rays (UHECRs) is considered. It is shown that prodigious TeV emission through curvature losses is an important consequence of this mechanism. Given the measured UHECR flux, it is expected that nearby dormant AGNs will be detectable by current Tev experiments. The implications for the Sgr A* source are also briefly considered.']",['2000-09-26'] +466,['eng'],"['Goldberg, H', 'Weiler, Thomas J']",['Clustering in Highest Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'energy spectrum, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, cluster', 'statistical analysis', 'angular correlation', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009378'],"['Directional clustering can be expected in cosmic ray observations due to purely statistical fluctuations for sources distributed randomly in the sky. We develop an analytic approach to estimate the probability of random cluster configurations, and use these results to study the strong potential of the HiRes, Auger, Telescope Array and EUSO/OWL/AirWatch facilities for deciding whether any observed clustering is most likely due to non-random sources.']",['2000-09-25'] +467,['eng'],"['Mukherjee, R']",['High Energy Gamma Rays'],['Astrophysics and Astronomy'],"['talk, Sudbury 2000/06/16', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'astrophysics', 'gamma ray burst', 'pulsar', 'galaxy, AGN', 'blazar', 'experimental methods', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009369'],"['This article reviews the present status of high energy gamma-ray astronomy at energies above 30 MeV. Observations in the past decade using both space- and ground-based experiments have been primarily responsible for giving a tremendous boost to our knowledge of the high energy Universe. High energy gamma-rays have been detected from a wide range of Galactic and extragalactic astrophysical sources, such as gamma-ray bursters, pulsars, and active galaxies. These observations have established high energy gamma-ray astronomy as a vital and exciting field, that has a bright future. This review summarizes the experimental techniques, observations and results obtained with recent experiments, and concludes with a short description of future prospects.']",['2000-09-25'] +468,['eng'],"['Giulini, D', 'Straumann, N']",['The mystery of cosmological vacuum energy density and the accelerated expansion of the universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'vacuum state, energy', 'energy, density', 'expansion, acceleration', 'astrophysics, fundamental constant', 'supernova', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009368'],"['The principles of General Relativity allow for a non-vanishing cosmological constant, which can possibly be interpreted at least partially in terms of quantum-fluctuations of matter fields. Depending on sign and magnitude it can cause accelerated or decelerated expansion at certain stages of cosmic evolution. Recent observations in cosmology seem to indicate that we presently live in an accelerated phase. We recall the history and fundamental issues connected with the cosmological constant and then discuss present evidences for a positive value, which causes the accelerated expansion.']",['2000-09-25'] +469,['eng'],"['Bahcall, J N']",['How the sun shines'],['Astrophysics and Astronomy'],"['introductory', 'matter, solar', 'energy, emission', 'history', 'nucleus nucleus, nuclear reaction', 'hydrogen, fusion', 'helium', 'neutrino, emission', 'neutrino, solar', 'neutrino, oscillation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009259'],['This historical essay describes the struggle to understand how the sun shines. The saga begins with the disagreement between Kelvin and Darwin over the age of the sun in the middle of the 19th century and continues through the revelations of solar neutrino experiments at the conclusion of the 20th century.'],['2000-09-19'] +470,['eng'],"['Medina-Tanco, G A']",['Ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009336'],"['From the analysis of AGASA data above $4 \\times 10^{19}$ eV, we show that the ultra-high energy cosmic rays flux is neither purely isotropic, nor reflects the expected anisotropy from a pure source distribution that maps large scale structure in the local universe. The arrival distribution seems to be the result of a mixture of fluxes (e.g., dark matter halo plus large scale structure) or the superposition of a direct and a diffuse radiation field components respectively. Another viable option is an arbitrary extragalactic flux reprocessed by a magnetized galactic wind model as recently proposed in the literature.']",['2000-09-21'] +471,['eng'],"['Pogosian, L E']",['Cosmic Defects and CMB anisotropy'],['Astrophysics and Astronomy'],"['talk, Capri 2000/09/07', 'talk, Columbus 2000/08/09', 'astrophysics, string', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'topology, defect', 'astrophysics, missing-mass', 'matter, density', 'inflationary universe', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009307'],"[""Recent measurements of the cosmic microwave background (CMB) anisotropies by BOOMERANG and MAXIMA collaborations have tightened the observational constraints on theories of structure formation. They disagree with the predictions of conventional topological defect models. Considering the fact that topological defects are predicted by the majority of realistic particle physics models, the exact nature of the constraints imposed by the recent data on the population and the properties of the defects must be fully understood. We show that the predictions of current cosmic string models can be brought into a closer agreement with the observations by choosing a closed universe with $\\Omega=1.3$ and by including the effects of the small-scale structure and radiation products of the strings. These alone, however, are not sufficient for obtaining a good fit to the measured shape of the angular power spectrum. To fit the data cosmic strings would either have to be correlated on large (perhaps superhorizon) scales or would have to possess a higher degree of coherence, i.e. be more ``time-correlated'.""]",['2000-09-20'] +472,['eng'],"['Hannestad, S']",['Reconstructing the inflationary power spectrum from CMBR data'],['Astrophysics and Astronomy'],"['inflationary universe', 'spectra, fluctuation', 'cosmic radiation, background', 'data analysis method', 'matter, density', 'astrophysics, fundamental constant', 'Hubble constant', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009296'],"['The Cosmic Microwave Background Radiation (CMBR) holds information about almost all the fundamental cosmological parameters, and by performing a likelihood analysis of high precision CMBR fluctuation data, these parameters can be inferred. However, this analysis relies on assumptions about the initial power spectrum, which is usually taken to be a featureless power-law, P(k) ~ k^{n_s-1}. Many inflationary models predict power spectra with non-power law features. We discuss the possibility for detecting such features by describing the power spectrum as bins in k-space. This method for power spectrum reconstruction is demonstrated in practise by performing likelihood optimization on synthetic spectra, and the difficulties arising from reconstructing smooth features using discontinuous bins are discussed in detail.']",['2000-09-20'] +473,['eng'],"['Simatos, N', 'Perivolaropoulos, L']",['Construction of Cosmic String Induced Temperature Anisotropy Maps with CMBFAST and Statistical Analysis'],['Astrophysics and Astronomy'],"['astrophysics, string', 'cosmic radiation, background', 'temperature, anisotropy', 'statistical analysis', 'spectra, fluctuation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009294'],"['We use the publicly available code CMBFAST as modified by L. Pogosian and T. Vachaspati to simulate the effects of wiggly cosmic strings on the Cosmic Microwave Background (CMB). Using the modified CMBFAST code which takes into account vector modes and models wiggly cosmic strings by the one scale model, we go beyond the angular power spectrum to construct CMB temperature maps with resolution of a few degrees. The statistics of these maps are then studied using conventional and recently proposed statistical tests optimized for the detection of hidden temperature discontinuities induced by the Gott-Kaiser-Stebbins effect. We show however, that these realistic maps can not be distinguished in a statistically significant way from purely Gaussian maps with identical power spectrum.']",['2000-09-20'] +474,['eng'],"['Gondek-Rosinska, D', 'Haensel, P', 'Zdunik, J L', 'Gourgoulhon, E']",['Rapidly rotating strange stars'],['Astrophysics and Astronomy'],"['talk, Bonn 1999/08/30', 'quark, matter', 'mass, strangeness', 'strong interaction, coupling constant', 'energy, rotational', 'potential, gravitation', 'gravitational radiation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009282'],['We study effects of the strange quark mass and of the QCD coupling constant in the MIT bag model of quark matter with lowest order quark-gluon interactions on the rapid rotation of strange stars. The influence of rotation on global parameters of strange stars is greater than in the case of the neutron star models. We show that independently of the strange quark mass and the coupling constans the ratio of the rotational kinetic energy to the absolute value of the gravitational potential energy for rotating strange stars is significantly higher than for ordinary neutron stars. This might indicate that rapidly rotating strange stars could be important sources of gravitational waves.'],['2000-09-19'] +475,['eng'],"['Prakash, M']",['Strange Pathways for Black Hole Formation'],['Astrophysics and Astronomy'],"['talk, Sudbury 2000/06/16', 'black hole, production', 'n, matter', 'entropy', 'baryon, density', 'nucleon, density', 'neutrino, cosmic radiation', 'K, condensation', 'hyperon, density', 'matter, lifetime', 'neutrino, luminosity', 'counters and detectors', 'quark, strangeness', 'quark, matter', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009279'],"['Immediately after they are born, neutron stars are characterized by an entropy per baryon of order unity and by the presence of trapped neutrinos. If the only hadrons in the star are nucleons, these effects slightly reduce the maximum mass relative to cold, catalyzed matter. However, if stangeness-bearing hyperons, a kaon condensate, or quarks are also present, these effects result in an increase in the maximum mass of up to $\\sim 0.3{\\rm M}_{\\odot}$ compared to that of a cold, neutrino-free star. This makes a sufficiently massive proto-neutron star metastable, so that after a delay of 10--100 seconds, the PNS collapses into a black hole. Such an event might be straightforward to observe as an abrupt cessation of neutrinos when the instability is triggered.']",['2000-09-19'] +476,['eng'],"['De Angelis, A']","['GLAST, the Gamma-ray Large Area Space Telescope']",['Astrophysics and Astronomy'],"['talk, Faro 2000/09/01', 'photon, cosmic radiation', 'counters and detectors, satellite', 'gamma ray burst', 'astrophysics, missing-mass', 'semiconductor detector, microstrip', 'scintillation counter, plastics', 'scintillation counter, hodoscope']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009271'],"['GLAST, a detector for cosmic gamma rays in the range from 20 MeV to 300 GeV, will be launched in space in 2005. Breakthroughs are expected in particular in the study of particle acceleration mechanisms in space and of gamma ray bursts, and maybe on the search for cold dark matter; but of course the most exciting discoveries could come from the unexpected.']",['2000-09-19'] +477,['eng'],"['Hwang, J', 'Noh, H']",['Cosmological Perturbations with Multiple Scalar Fields'],['Astrophysics and Astronomy'],"['space-time, perturbation', 'field theory, scalar', 'multiple', 'conservation law', 'field equations, solution', 'slow-roll approximation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009268'],"['We consider the evolution of perturbed cosmological spacetime with multiple scalar fields in Einstein gravity. A complete set of scalar-type perturbation equations is presented in a gauge-ready form, and we derived the closed set of second-order differential equations in several useful forms. Conserved behaviors of the perturbed three-space curvature in the comoving gauge, $\\phi_v$, under several conditions are clarified. Under the slow-roll conditions, the adiabatic and isocurvature modes decouple from each other, and in the large-scale limit we have (i) the adiabatic mode is generally conserved, (ii) for a couple of special potential the isocurvature modes decouple from each other and are described by conserved quantities, (iii) in the two field system, the isocurvature mode is described by a conserved quantity for the general potential.']",['2000-09-19'] +478,['eng'],"['Barger, V', 'Marfatia, D M']",['Supernova data may be unable to distinguish between quintessence and k-essence'],['Astrophysics and Astronomy'],"['supernova', 'dark energy', 'luminosity, measurement', 'quintessence', 'matter, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009256'],"['We consider the efficacy of using luminosity distance measurements of deep redshift supernovae to discriminate between two forms of dark energy, quintessence (a scalar field with canonical kinetic terms rolling down a potential) and $k$-essence (a scalar field whose cosmic evolution is driven entirely by non-linear kinetic terms). The primary phenomenological distinction between the two types of models that can be quantified by supernova searches (at least in principle) is that the equation of state $w\\equiv p/\\rho$ of quintessence is falling today while that of $k$-essence is rising. By simulating $10^5$ possible datasets that SNAP could obtain, we show that even if the mass density $\\Omega_m$ is known exactly, an ambiguity remains that may not allow a definitive distinction to be made between the two types of theories.']",['2000-09-18'] +479,['eng'],"['Andrés, E C', 'Askebjer, P', 'Bai, X', 'Barouch, G', 'Barwick, S W', 'Barwick, S W']",['Results from the AMANDA High Energy Neutrino Detector'],['Astrophysics and Astronomy'],"['talk, Sudbury 2000/06/16', 'neutrino, cosmic radiation', 'astrophysics, particle source', 'neutrino, flux', 'upper limit', 'gamma ray burst', 'astrophysics, missing-mass', 'WIMP, annihilation', 'Cherenkov counter, water', 'deep underground detector, AMANDA', 'angular resolution', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009242'],"['This paper briefly summarizes the search for astronomical sources of high-energy neutrinos using the AMANDA-B10 detector. The complete data set from 1997 was analyzed. For E_mu>10 TeV, the detector exceeds 10,000 m^2 in effective area between declinations of 25 and 90 degrees. Neutrinos generated in the atmosphere by cosmic ray interactions were used to verify the overall sensitivity of the detector. The absolute pointing accuracy and angular resolution has been confirmed by the analysis of coincident events between the SPASE air shower array and the AMANDA detector. Preliminary flux limits from point source candidates are presented. For declinations larger than +45 degrees, our results compare favorably to existing limits for sources in the Southern sky. We also present the current status of the searches for high energy neutrino emission from diffusely distributed sources, GRBs, and WIMPs from the center of the earth.']",['2000-09-18'] +480,['eng'],"['Kempf, A']",['Mode Generating Mechanism in Inflation with Cutoff'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time', 'cosmic radiation, background', 'quantum gravity', 'commutation relations', 'field theory, scalar']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009209'],"['In most inflationary models, space-time inflated to the extent that modes of cosmological size originated as modes of wavelengths at least several orders of magnitude smaller than the Planck length. Recent studies confirmed that, therefore, inflationary predictions for the cosmic microwave background perturbations are generally sensitive to what is assumed about the Planck scale. Here, we propose a framework for field theories on curved backgrounds with a plausible type of ultraviolet cutoff. We find an explicit mechanism by which during cosmic expansion new (comoving) modes are generated continuously. Our results allow the numerical calculation of a prediction for the CMB perturbation spectrum.']",['2000-09-14'] +481,['eng'],"['Hogan, C J']",['Scales of the Extra Dimensions and their Gravitational Wave Backgrounds'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'membrane model', 'symmetry breaking', 'space-time, higher-dimensional', 'radion, perturbation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009136'],"['Circumstances are described in which symmetry breaking during the formation of our three-dimensional brane within a higher-dimensional space in the early universe excites mesoscopic classical radion or brane-displacement degrees of freedom and produces a detectable stochastic background of gravitational radiation. The spectrum of the background is related to the unification energy scale and the the sizes and numbers of large extra dimensions. It is shown that properties of the background observable by gravitational-wave observatories at frequencies $f\\approx 10^{-4}$ Hz to $10^3$ Hz contain information about unification on energy scales from 1 to $10^{10}$ TeV, gravity propagating through extra-dimension sizes from 1 mm to $10^{-18}$mm, and the dynamical history and stabilization of from one to seven extra dimensions.']",['2000-09-11'] +482,['eng'],"['Cordero, R', 'Rojas, E L']",['Chiral Superconducting Membranes'],['Astrophysics and Astronomy'],"['membrane model, superconducting', 'symmetry, chiral', 'Lagrangian formalism', 'Hamiltonian formalism', 'string model', 'integrability', 'light cone gauge', 'domain wall']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009140'],"['We develop the dynamics of the chiral superconducting membranes in a geometric approach either making a Lagrangian description and a Hamiltonian point of view. Besides, we show the equivalence of the resulting descriptions to the one known Dirac-Nambu-Goto (DNG) case. Integrability for chiral string model is obtained using a proposed light-cone gauge. In a similar way, domain walls are integrated by means of a special ansatz. We compare the results with recently works appeared in the literature.']",['2000-09-12'] +483,['eng'],"['Gordon, C', 'Wands, D', 'Bassett, B A', 'Maartens, R']",['Adiabatic and entropy perturbations from inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time, perturbation', 'adiabatic', 'entropy, perturbation', 'field theory, scalar', 'correlation, perturbation', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009131'],"['We study adiabatic (curvature) and entropy (isocurvature) perturbations produced during a period of cosmological inflation that is driven by multiple scalar fields with an arbitrary interaction potential. A local rotation in field space is performed to separate out the adiabatic and entropy modes. The resulting field equations show explicitly how on large scales entropy perturbations can source adiabatic perturbations if the background solution follows a curved trajectory in field space, and how adiabatic perturbations cannot source entropy perturbations in the long-wavelength limit. It is the effective mass of the entropy field that determines the amplitude of entropy perturbations during inflation. We present two applications of the equations. First, we show why one in general expects the adiabatic and entropy perturbations to be correlated at the end of inflation, and calculate the cross-correlation in the context of a double inflation model with two non-interacting fields. Second, we consider two-field preheating after inflation, examining conditions under which entropy perturbations can alter the large-scale curvature perturbation and showing how our new formalism has advantages in numerical stability when the background solution follows a non-trivial trajectory in field space.']",['2000-09-11'] +484,['eng'],"['Albrecht, Andreas']",['Defect models of cosmic structure in light of the new CMB data'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2000/01/22', 'astrophysics, string', 'topology, defect', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, oscillation', 'coherence', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009129'],"['Defect models of cosmic structure formation have faced a number of difficult challenges over recent years. Yet interestingly, new CMB data does not show strong evidence for secondary oscillations in the anisotropy power. Here I review the current standing of the cosmic defect models of structure formation in light of the current data.']",['2000-09-11'] +485,['eng'],"['Blaschke, David B', 'Grigorian, H', 'Voskresensky, D N']",['Cooling of Hybrid Neutron Stars and Hypothetical Self-bound Objects with Superconducting Quark Cores'],['Astrophysics and Astronomy'],"['n, matter', 'quark, matter', 'superconducting', 'matter, hybrid', 'quark, gap', 'temperature', 'neutrino, emission', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009120'],"['We study the consequences of superconducting quark cores (with color-flavor-locked phase as representative example) for evolution of temperature profiles and the cooling curves in quark-hadron hybrid stars and in hypothetical self-bounded objects having no a hadron shell (quark core neutron stars). The quark gaps are varied from 0 to $\\Delta_q =50$ MeV. For hybrid stars we find time scales of $1\\div5$, $5\\div10$ and $50\\div100$ years for the formation of a quasistationary temperature distribution in the cases $\\Delta_q =0$, 0.1 MeV and $\\gsim$ 1 MeV, respectively. These time scales are governed by the heat transport within quark cores for large diquark gaps ($\\Delta \\gsim$ 1 MeV) and within the hadron shell for small diquark gaps ($\\Delta \\lsim 0.1$ MeV). For quark core neutron stars we find a time scale $\\simeq 300$ years for the formation of a quasistationary temperature distribution in the case $\\Delta \\gsim$ 10 MeV and a very short one for $\\Delta \\lsim$ 1 MeV. If hot young compact objects will be observed they can be interpreted as manifestation of large gap color superconductivity. Depending on the size of the pairing gaps, the compact star takes different paths in the ${lg}T_s $ vs. ${lg} t$ diagram where $T_s$ is the surface temperature. Compared to the corresponding hadronic model which well fits existing data the model for the hybrid neutron star (with a large diquark gap) shows too fast cooling. The same conclusion can be drawn for the corresponding self-bound objects.']",['2000-09-08'] +486,['eng'],"['Banik, S', 'Bandyopadhyay, D']",['Antikaon condensation and the metastability of protoneutron stars'],['Astrophysics and Astronomy'],"['astrophysics', 'n, matter', 'anti-K, condensation', 'matter, density', 'condensation, density', 'critical phenomena', 'anti-K, potential', 'effective Lagrangian', 'mean field approximation, relativistic', 'meson, exchange', 'dispersion relations', 'potential, chemical', 'potential, optical', 'coupling constant, (nucleon meson)', 'energy, condensation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009113'],"['We investigate the condensation of $\\bar K^0$ meson along with $K^-$ condensation in the neutrino trapped matter with and without hyperons. Calculations are performed in the relativistic mean field models in which both the baryon-baryon and (anti)kaon-baryon interactions are mediated by meson exchange. In the neutrino trapped matter relevant to protoneutron stars, the critical density of $K^-$ condensation is shifted considerably to higher density whereas that of $\\bar K^0$ condensation is shifted slightly to higher density with respect to that of the neutrino free case. The onset of $K^-$ condensation always occurs earlier than that of $\\bar K^0$ condensation. A significant region of maximum mass protoneutron stars is found to contain $\\bar K^0$ condensate for larger values of the antikaon potential. With the appearance of $\\bar K^0$ condensation, there is a region of symmetric nuclear matter in the inner core of a protoneutron star. It is found that the maximum mass of a protoneutron star containing $K^-$ and $\\bar K^0$ condensate is greater than that of the corresponding neutron star. We revisit the implication of this scenario in the context of the metastability of protoneutron stars and their evolution to low mass black holes.']",['2000-09-08'] +487,['eng'],"['Huang, M H A']",['Atmospheric Secondary Particles In Near Earth Space'],['Astrophysics and Astronomy'],"['talk, Taipei 2000/08/07', 'p, cosmic radiation', 'lepton, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'magnetic field', 'lifetime', 'magnetic spectrometer, satellite', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009106'],"['The Alpha Magnetic Spectrometer detects a large amount of particles below rigidity cutoff. Those high energy particles create questions related to radiation belts and atmospheric neutrinos. To understand the origin of these particles, we use a trajectory tracing program to simulate particle trajectories in realistic geomagnetic field. The complex behaviors and large e^+/e^- are explained here.']",['2000-09-08'] +488,['eng'],"['Voskresensky, D N']",['Medium Effects in Neutrino Cooling of Neutron Stars'],['Astrophysics and Astronomy'],"['talk, Trento 2000/06/19', 'n, matter', 'neutrino, emission', 'collective phenomena', 'nuclear matter', 'exchange, one-pion', 'nucleon nucleon, interaction', 'multiple scattering', 'renormalization, vertex', 'effective Lagrangian', 'model, liquid', 'pi, condensation', 'neutrino, opacity', 'approximation, pseudoparticle', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009093'],"['This review demonstrates that neutrino emission from dense hadronic component in neutron stars is subject of strong modifications due to collective effects in the nuclear matter. With the most important in-medium processes incorporated in the cooling code an overall agreement with available soft $X$ ray data can be easily achieved. With these findings so called ""standard"" and ""non-standard"" cooling scenarios are replaced by one general ""nuclear medium cooling scenario"" which relates slow and rapid neutron star coolings to the star masses (interior densities). In-medium effects take important part also at early hot stage of neutron star evolution decreasing the neutrino opacity for less massive and increasing for more massive neutron stars. A formalism for calculation of neutrino radiation from nuclear matter is presented that treats on equal footing one-nucleon and multiple-nucleon processes as well as reactions with resonance bosons and condensates.']",['2000-09-07'] +489,['eng'],"['Sellwood, J A', 'Kosowsky, A']",['Does Dark Matter Exist?'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'galaxy, production', 'mass spectrum', 'astrophysics, fundamental constant', 'gravitation', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009074'],"['The success of the Lambda-CDM model on large scales does not extend down to galaxy scales. We list a dozen problems of the dark matter hypothesis, some of which arise in specific models for the formation of structure in the universe, while others are generic and require fine tuning in any dark matter theory. Modifications to the theory, such as adding properties to the DM particles beyond gravitational interactions, or simply a better understanding of the physics of galaxy formation, may resolve some problems, but a number of conspiracies and correlations are unlikely to yield to this approach. The alternative is that mass discrepancies result from of a non-Newtonian law of gravity, a hypothesis which avoids many of the more intractable problems of dark matter. A modified law of gravity is not without formidable difficulties of its own, but it is no longer obvious that they are any more daunting than those facing DM.']",['2000-09-06'] +490,['eng'],"['Grasso, D', 'Rubinstein, H R']",['Magnetic Fields in the Early Universe'],['Astrophysics and Astronomy'],"['review', 'astrophysics, model', 'magnetic field, production', 'galaxy, cluster', 'cosmic radiation, background', 'temperature, anisotropy', 'polarization, anisotropy', 'light nucleus, production', 'p, coupling', 'n, coupling', 'electron, coupling', 'magnetic field, high', 'particle, mass', 'sphaleron', 'B+L number, violation', 'baryon, production', 'electroweak interaction, critical phenomena', 'symmetry breaking, chiral', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009061'],"['This review concerns the origin and the possible effects of magnetic fields in the early Universe. We start by providing to the reader with a short overview of the current state of art of observations of cosmic magnetic fields. We then illustrate the arguments in favour of a primordial origin of magnetic fields in the galaxies and in the clusters of galaxies. We argue that the most promising way to test this hypothesis is to look for possible imprints of magnetic fields on the temperature and polarization anisotropies of the cosmic microwave background radiation (CMBR). With this purpose in mind, we provide a review of the most relevant effects of magnetic fields on the CMBR. A long chapter of this review is dedicated to particle physics inspired models which predict the generation of magnetic fields during the early Universe evolution. Although it is still unclear if any of these models can really explain the origin of galactic and intergalactic magnetic fields, we show that interesting effects may arise anyhow. Among these effects, we discuss the consequences of strong magnetic fields on the big-bang nucleosynthesis, on the masses and couplings of the matter constituents, on the electroweak phase transition, and on the baryon and lepton number violating sphaleron processes. Several intriguing common aspects, and possible interplay, of magnetogenesis and baryogenesis are also dicussed.']",['2000-09-06'] +491,['eng'],"['Bellido, J A', 'Clay, R W', 'Dawson, B R', 'Johnston-Hollitt, M']",['Southern Hemisphere Observation of a $10^{18}$eV Cosmic Ray Near the Direction of the Galactic Centre'],['Astrophysics and Astronomy'],"['cosmic radiation, flux', 'cosmic radiation, measurement', 'galaxy', 'data analysis method', 'scintillation counter, angular resolution', 'showers, air', 'cosmic radiation, anisotropy', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009039'],"['We report on an analysis of data from the southern hemisphere SUGAR cosmic ray detector. We confirm the existence of an excess of $10^{18}$eV cosmic rays from a direction close to the Galactic Centre, first reported by the AGASA group. We find that the signal is consistent with that from a point source, and we find evidence for an excess of cosmic rays coming from the direction of the Galactic Centre itself.']",['2000-09-05'] +492,['eng'],"['Lin, W B', 'Huang, D H', 'Zhang, X', 'Brandenberger, R H']",['Non-Thermal Production of WIMPs and the Sub-Galactic Structure of the Universe'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, production', 'spectra, fluctuation', 'phase space, density', 'energy, density', 'cosmic radiation, background', 'defect, topological', 'defect, decay', 'neutralino, production', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0009003'],"['There is increasing evidence that conventional cold dark matter (CDM) models lead to conflicts between observations and numerical simulations of dark matter halos on sub-galactic scales. Spergel and Steinhardt showed that if the CDM is strongly self-interacting, then the conflicts disappear. However, the assumption of strong self-interaction would rule out the favored candidates for CDM, namely weakly interacting massive particles (WIMPs), such as the neutralino. In this paper we propose a mechanism of non-thermal production of WIMPs and study its implications on the power spectrum. We find that the non-vanishing velocity of the WIMPs suppresses the power spectrum on small scales compared to what it obtained in the conventional CDM model. Our results show that, in this context, WIMPs as candidates for dark matter can work well both on large scales and on sub-galactic scales.']",['2000-09-04'] +493,['eng'],"['Masperi, L', 'Orsaria, M']",['Comparison of UHECR spectra from necklaces and vortons'],['Astrophysics and Astronomy'],"['talk, La Paz 2000/07/23', 'cosmic radiation, energy spectrum', 'topology, defect', 'magnetic monopole', 'vorton', 'astrophysics, string', 'cosmic radiation, anisotropy', 'grand unified theory, SO(10)', 'symmetry, Z(2)', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008525'],"['Cosmic rays of energy higher than 10^19 eV may be explained by topological defects produced in the early stages of universe. Two suitable alternatives are: necklaces formed by magnetic monopoles connected by strings, and vortons which are loops stabilized by superconducting currents. The former are uniformly distributed in the universe, may account for cosmic rays above the ankle, suffer a transient GZK cutoff with a subsequent recovery and isotropy of observations is expected. The latter are concentrated in the galactic halo, require an additional extragalactic contribution between the ankle and the GZK cutoff, beyond which give a harder component and predict anisotropy related to mass concentration.']",['2000-09-03'] +494,['eng'],"['Takahashi, T', 'Kataoka, J', 'Madejski, G M', 'Mattox, J R', 'Urry, C M', 'Wagner, S', 'Aharonian, F A', 'Catanese, M', 'Chiappetti, L', 'Coppi, P S', 'Degrange, B', 'Fossati, G', 'Kubo, H', 'Krawczynski, H', 'Makino, F', 'Marshall, H', 'Maraschi, L', 'Piron, F', 'Remillard, R A', 'Takahara, F', 'Tashiro, M', 'Terasranta, H', 'Weekes, T']",['Complex Spectral Variability from Intensive Multi-wavelength Monitoring of Mrk421 in 1998'],['Astrophysics and Astronomy'],"['blazar', 'cosmic radiation, flux', 'Cherenkov counter', 'structure function', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'correlation function', 'synchrotron radiation, emission', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008505'],"['We conducted a multi-frequency campaign for the TeV blazar Mrk~421 in 1998 April. The campaign started from a pronounced high amplitude flare recorded by SAX and Whipple; ASCA observation started three days later. In the X-ray data, we detected multiple flares, occuring on time scales of about one day. ASCA data clearly reveal spectral variability. The comparison of the data from ASCA, EUVE and RXTE indicates that the variability amplitudes in the low energy synchrotron component are larger at higher photon energies. In TeV Gamma-rays, large intra-day variations -- which were correlated with the X-ray flux -- were observed when results from three Cherenkov telescopes are combined. The RMS variability of TeV Gamma--rays was similar to that observed in hard X-rays, above 10 keV. The X-ray light curve reveals flares which are almost symmetric for most of cases, implying the dominant time scale is the light crossing time through the emitting region. The structure function analysis based on the continuous X-ray light curve of seven days indicates that the characteristic time scale is ~0.5 day. The analysis of ASCA light curves in various energy bands appears to show both soft (positive) and hard (negative) lags. These may not be real, as systematic effects could also produce these lags, which are all much smaller than an orbit. If the lags of both signs are real, these imply that the particle acceleration and X-ray cooling time scales are similar.']",['2000-09-03'] +495,['eng'],"['Qian, Y Z']",['Neutrinos and the Supernova Origin of the Elements'],['Astrophysics and Astronomy'],"['talk, Sudbury 2000/06/16', 'neutrino, cosmic radiation', 'neutrino, flux', 'supernova', 'n, matter', 'light nucleus, production', 'neutrino, oscillation', 'neutrino, mixing angle', 'proposed experiment', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008494'],"['Intense fluxes of neutrinos are emitted by the hot neutron star produced in a supernova. The electron neutrino and antineutrino capture reactions on neutrons and protons, respectively, provide heating to drive a wind from the hot neutron star. The same reactions also determine the neutron-richness of the wind material. Nucleosynthesis via rapid neutron capture, the r-process, may occur in the wind material as it expands away from the neutron star. The neutron-richness of the wind material, and hence, the r-process nucleosynthesis therein, are sensitive to mixing between the muon (or tauon) neutrino/antineutrino and the electron (or sterile) neutrino/antineutrino. Indirect arguments and direct tests for the supernova origin of the r-process elements are discussed with a goal to establish supernova r-process nucleosynthesis as an important probe for neutrino mixing.']",['2000-08-31'] +496,['eng'],"['Grillo, A F', 'Aloisio, R']",['Cosmic Rays and the Structure of Space-Time'],['Astrophysics and Astronomy'],"['talk, Vulcano 2000/05/22', 'invariance, Lorentz', 'validity test', 'photon, cosmic radiation', 'cosmic radiation, interaction', 'cosmic radiation, background', 'cosmic radiation, absorption', 'energy, threshold', 'space-time', 'proposed experiment', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008491'],['Even a fundamental symmetry like Lorentz Invariance is an experimental fact and must be experimentally verified. We show that the study of the interactions of Cosmic Rays with universal diffuse background radiation can provide very stringent tests of this symmetry. The interactions we consider are the ones characterized by well defined energy thresholds whose energy position can be predicted on the basis of Special Relativity. We argue that the experimental verification of these thresholds can address the physics of supra-Planckian scales.'],['2000-08-31'] +497,['eng'],"['Grishchuk, L P', 'Lipunov, V M', 'Postnov, K A', 'Prokhorov, M E', 'Sathyaprakash, B S']",['Gravitational Wave Astronomy'],['Astrophysics and Astronomy'],"['review', 'gravitational radiation, measurement', 'gravitational radiation, particle source', 'counters and detectors, performance', 'experimental methods', 'laser, interference', 'n, matter', 'black hole', 'background, stochastic', 'signal processing', 'data analysis method', 'costs', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008481'],"['The first generation of long-baseline laser interferometric detectors of gravitational waves will start collecting data in 2001-2003. We carefully analyse their planned performance and compare it with the expected strengths of astrophysical sources. The scientific importance of the anticipated discovery of various gravitatinal wave signals and the reliability of theoretical predictions are taken into account in our analysis. We try to be conservative both in evaluating the theoretical uncertainties about a source and the prospects of its detection. After having considered many possible sources, we place our emphasis on (1) inspiraling binaries consisting of stellar mass black holes and (2) relic gravitational waves. We draw the conclusion that inspiraling binary black holes are likely to be detected first by the initial ground-based interferometers. We estimate that the initial interferometers will see 2-3 events per year from black hole binaries with component masses 10-15M_\\odot, with a signal-to-noise ratio of around 2-3, in each of a network of detectors consisting of GEO, VIRGO and the two LIGOs. It appears that other possible sources, including coalescing neutron stars, are unlikely to be detected by the initial instruments. We also argue that relic gravitational waves may be discovered by the space-based interferometers in the frequency interval 2x10^{-3}-10^{-2} Hz, at the signal-to-noise ratio level around 3.']",['2000-08-31'] +498,['eng'],"['Hardy, S J', 'Thoma, M H']",['Neutrino-electron processes in a strongly magnetized thermal plasma'],['Astrophysics and Astronomy'],"['neutrino electron, interaction', 'magnetic field, high', 'field theory, finite temperature', 'plasma, magnetic', 'neutrino antineutrino, annihilation', 'electron, pair production', 'polarization, tensor', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008473'],"['We present a new method of calculating the rate of neutrino-electron interactions in a strong magnetic field based on finite temperature field theory. Using this method, in which the effect of the magnetic field on the electron states is taken into account exactly, we calculate the rates of all of the lowest order neutrino-electron interactions in a plasma. As an example of the use of this technique, we explicitly calculate the rate at which neutrinos and antineutrinos annihilate in a highly magnetized plasma, and compare that to the rate in an unmagnetized plasma. The most important channel for energy deposition is the gyromagnetic absorption of a neutrino-antineutrino pair on an electron or positron in the plasma ($\\nu\\bar{\\nu} e^\\pm\\leftrightarrow e^\\pm$). Our results show that the rate of annihilation increases with the magnetic field strength once it reaches a certain critical value, which is dependent on the incident neutrino energies and the ambient temperature of the plasma. It is also shown that the annihilation rates are strongly dependent on the angle between the incident particles and the direction of the magnetic field. If sufficiently strong fields exist in the regions surrounding the core of a type II supernovae or in the central engines of gamma ray bursts, these processes will lead to more efficient plasma heating mechanism than in an unmagnetized medium, and moreover, one which is intrinsically anisotropic.']",['2000-08-31'] +499,['eng'],"['Hannestad, S']",['Massive warm dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'particle, massive', 'particle, decay', 'neutrino antineutrino, annihilation', 'energy, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008451'],"['Many independent high resolution simulations have indicated that the standard collisionless cold dark matter model does not reproduce the structure of observed present day galaxies well. Several possible solutions in the form of modifications to the physics of the dark matter particles have been proposed. One of the most promising is warm dark matter (WDM), particles with significant thermal motion in the early universe. It is usually assumed that such particles are relativistically decoupled particles with a mass of approximately 1 keV. However, here we have investigated the possibility that much more massive particles with highly non-thermal spectra could make up warm dark matter. Several possible production mechanisms are reviewed and the only one found to be viable is that the WDM is produced by the non-relativistic decay of some massive species in the early universe. Such very massive warm dark matter could possibly be detected in direct detection experiments, as opposed to standard thermal warm dark matter.']",['2000-08-30'] +500,['eng'],"['Chamoun, N', 'Landau, S J', 'Vucetich, H']",['Bekenstein model and the time variation of the strong coupling constant'],['Astrophysics and Astronomy'],"['fundamental constant, fine structure', 'strong interaction, coupling constant', 'time variation', 'quantum chromodynamics', 'gluon, condensation', 'astrophysics', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008436'],"['We propose to generalize Bekenstein model for the time variation of the fine structure ""constant"" $\\alpha_{em}$ to QCD strong coupling constant $\\alpha_S$. We find that, except for a ``fine tuned\'\' choice of the free parameters, the extension can not be performed trivially without being in conflict with experimental constraints and this rules out $\\alpha_S$ variability. This is due largely to the huge numerical value of the QCD vacuum gluon condensate when compared to the mass density of the universe.']",['2000-08-29'] +501,['eng'],"['Janka, H T']",['Conditions for Shock Revival by Neutrino Heating in Core-Collapse Supernovae'],['Astrophysics and Astronomy'],"['supernova', 'neutrino, cosmic radiation', 'shock waves', 'model, hydrodynamical', 'n, matter', 'mass, accretion', 'neutrino, energy', 'neutrino, velocity', 'energy loss', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008432'],"['Energy deposition by neutrinos can rejuvenate the stalled bounce shock and can provide the energy for the supernova explosion of a massive star. This neutrino-heating mechanism, however, is not finally accepted or proven as the trigger of the explosion. Part of the problem is that different groups have obtained seemingly discrepant results, and the complexity of the hydrodynamic models often hampers a clear and simple interpretation of the results. This demands a deeper theoretical understanding of the requirements of a successful shock revival. An approach is described here which allows one to discuss the neutrino heating phase analytically by a time-dependent treatment. A criterion is derived which formulates the minimum requirements for shock revival. It shows that the success of the supernova shock does not only depend on the neutrino heating in the gain region and the mass infall to the shock. It is also sensitive to the energy loss by neutrino emission in the cooling layer outside the neutrinosphere, which governs the accretion of matter into the nascent neutron star. The analysis shows that neutrino-driven shock expansion and acceleration are neither likely to occur at very early times after core bounce, when the mass infall rate is still very high, nor at late times when the accretion rate has become too low. However, there is a window of conditions, realized at intermediate post-bounce times, where the mass accretion by the shock and the neutrinospheric luminosity define favorable conditions for shock revival. This space of advantageous conditions widens with a larger value of the shock stagnation radius. The importance of convective energy transport in the neutrino-heating region is confirmed.']",['2000-08-29'] +502,['eng'],"['Khokhlov, D L']",['The state of two neutrinos moving in the opposite directions'],['Astrophysics and Astronomy'],"['neutrino, flux', 'neutrino, solar', 'boron', 'chlorine', 'gallium', 'parity, transformation', 'numerical calculations', 'interpretation of experiments, deep underground detector']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008413'],"['It is considered the flux of neutrinos moving from the source in the opposite directions. The state of two neutrinos moving in the opposite directions is a superposition of the state $|\\psi_{12}>$ and the state $|\\psi_{21}>$ in which the positions of neutrinos are interchanged. Neutrinos in the state $|\\psi_{21}>$ are P-transformed with respect to neutrinos in the state $|\\psi_{12}>$ therefore if one detects neutrinos in the state $|\\psi_{12}>$ it is forbidden to detect neutrinos in the state $|\\psi_{21}>$. Under detection the number of neutrinos decreases two times, and the energy of neutrinos increases two times. Hence one can detect only one half of the solar neutrino flux predicted by the SSM that may provide a solution for the solar neutrino puzzle.']",['2000-08-29'] +503,['eng'],"['Pons, J A', 'Miralles, J A', 'Prakash, M', 'Lattimer, J M']",['Evolution of Proto-Neutron stars with kaon condensates'],['Astrophysics and Astronomy'],"['n, matter', 'p, matter', 'K, condensation', 'finite temperature, effect', 'neutrino, cosmic radiation', 'baryon, density', 'critical phenomena', 'matter, lifetime', 'neutrino, opacity', 'time variation', 'neutrino, luminosity', 'black hole', 'supernova', 'deep underground detector', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008389'],"[""We present simulations of the evolution of a proto-neutron star in which kaon-condensed matter might exist, including the effects of finite temperature and trapped neutrinos. The phase transition from pure nucleonic matter to the kaon condensate phase is described using Gibbs' rules for phase equilibrium, which permit the existence of a mixed phase. A general property of neutron stars containing kaon condensates, as well as other forms of strangeness, is that the maximum mass for cold, neutrino-free matter can be less than the maximum mass for matter containing trapped neutrinos or which has a finite entropy. A proto-neutron star formed with a baryon mass exceeding that of the maximum mass of cold, neutrino-free matter is therefore metastable, that is, it will collapse to a black hole at some time during the Kelvin-Helmholtz cooling stage. The effects of kaon condensation on metastable stars are dramatic. In these cases, the neutrino signal from a hypothetical galactic supernova (distance $\\sim8.5$ kpc) will stop suddenly, generally at a level above the background in the SuperK and SNO detectors, which have low energy thresholds and backgrounds. This is in contrast to the case of a stable star, for which the signal exponentially decays, eventually disappearing into the background. We find the lifetimes of kaon-condensed metastable stars to be restricted to the range 40--70 s and weakly dependent on the proto-neutron star mass, in sharp contrast to the significantly larger mass dependence and range (1--100 s) of hyperon-rich metastable stars.""]",['2000-08-25'] +504,['eng'],"['Weber, F']",['Strangeness in Neutron Stars'],['Astrophysics and Astronomy'],"['talk, Berkeley 2000/07/20', 'n, matter', 'quark, strangeness', 'quark, matter', 'hyperon', 'K-, condensation', 'baryon resonance, dibaryon', 'H baryon, matter', 'quark, confinement', 'matter, stability', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008376'],"['It is generally agreed on that the tremendous densities reached in the centers of neutron stars provide a high-pressure environment in which numerous novel particles processes are likely to compete with each other. These processes range from the generation of hyperons to quark deconfinement to the formation of kaon condensates and H-matter. There are theoretical suggestions of even more exotic processes inside neutron stars, such as the formation of absolutely stable strange quark matter, a configuration of matter even more stable than the most stable atomic nucleus, iron. In the latter event, neutron stars would be largely composed of pure quark matter, eventually enveloped in a thin nuclear crust. No matter which physical processes are actually realized inside neutron stars, each one leads to fingerprints, some more pronounced than others though, in the observable stellar quantities. This feature combined with the unprecedented progress in observational astronomy, which allows us to see vistas with remarkable clarity that previously were only imagined, renders neutron stars to nearly ideal probes for a wide range of physical studies, including the role of strangeness in dense matter.']",['2000-08-25'] +505,['eng'],"['Sigl, G']",['Particle and Astrophysics Aspects of Ultrahigh Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Guanajuato 1999/08/04', 'talk, Trieste 2000/06/12', 'cosmic radiation, particle source', 'neutrino, cosmic radiation', 'cosmic radiation, flux', 'photon, acceleration', 'photon, cosmic radiation', 'magnetic field, galaxy', 'cosmic radiation, primary', 'neutrino nucleon, new interaction', 'nucleon, cosmic radiation', 'sparticle, search for', 'astrophysics, model', 'numerical calculations, Monte Carlo', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008364'],"['The origin of cosmic rays is one of the major unresolved astrophysical questions. In particular, the highest energy cosmic rays observed possess macroscopic energies and their origin is likely to be associated with the most energetic processes in the Universe. Their existence triggered a flurry of theoretical explanations ranging from conventional shock acceleration to particle physics beyond the Standard Model and processes taking place at the earliest moments of our Universe. Furthermore, many new experimental activities promise a strong increase of statistics at the highest energies and a combination with gamma-ray and neutrino astrophysics will put strong constraints on these theoretical models. Detailed Monte Carlo simulations indicate that charged ultra-high energy cosmic rays can also be used as probes of large scale magnetic fields whose origin may open another window into the very early Universe. We give an overview over this quickly evolving reasearch field.']",['2000-08-24'] +506,['eng'],"['Sigl, G', 'Torres, D', 'Anchordoqui, L A', 'Romero, G']",['Testing the Correlation of Ultra-High Energy Cosmic Rays with High Redshift Sources'],['Astrophysics and Astronomy'],"['quasar', 'photon, cosmic radiation', 'blazar', 'correction, validity test', 'showers, air', 'nucleon, cosmic radiation', 'nucleon, acceleration', 'threshold, energy', 'neutrino nucleon, interaction', 'cross section', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008363'],"['We study the correlation between compact radio quasars and ultra-high energy cosmic rays using an updated list of air shower detections. We estimate the level of positional correlation between both samples and the probability of pure chance association through simulations of random sets of synthetic cosmic ray events. We find that there are no reasons to claim for a physical association and that some previous results appear to be an effect of the small size of the sample used. This is also true when, instead of compact radio quasars, 3EG gamma-ray blazars are considered. Consequently, unless somehow severely deflected, it is unlikely that the high energy CR primaries are new particles or particles with new interactions beyond the electroweak scale, produced in high-redshift active galactic nuclei.']",['2000-08-24'] +507,['eng'],"['Anchordoqui, L A', 'Kirasirova, M', 'McCauley, T P', 'Reucroft, S', 'Swain, J D']","[""On the nature of cosmic rays above the Greisen--Zatsepin--Kuz'min cut off""]",['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'cosmic radiation, primary', 'nucleus, cosmic radiation', 'mass number', 'showers, air', 'calcium', 'GZK effect', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007403'],"['A re-examination of the atmospheric cascade profile of the highest energy cosmic ray is presented. The study includes air-shower simulations considering different cross sections, particle multiplicity and variation of the hadronic-event-generator to model interactions above 200 GeV. The analysis provides evidence that a medium mass nucleus, say $^{41}$Ca, resembles the shower profile quite well (in agreement with previous studies). This result does not support the idea, increasingly popular at present, that the highest energy particles are protons, derived from the decay of supermassive relic particles. On the other hand, we show that debris of relativistic super-heavy nuclei, which can survive a 100 Mpc journey through the primeval radiation are likely to generate such a kind of cascade.']",['2000-07-27'] +508,['eng'],"['Anchordoqui, L A', 'Dova, M T', 'McCauley, T P', 'Paul, T', 'Reucroft, S', 'Swain, J D']","['A pot of gold at the end of the cosmic ""raynbow""?']",['Astrophysics and Astronomy'],"['talk, Campinas 2000/07/17', 'p, cosmic radiation', 'nucleus, cosmic radiation', 'cosmic radiation, primary', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'showers, air', 'proposed experiment', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006071'],"[""We critically review the common belief that ultrahigh energy cosmic rays are protons or atomic nuclei with masses not exceeding that of iron. We find that heavier nuclei are indeed possible, and discuss possible sources and acceleration mechanisms for such primaries. We also show detailed simulations of extensive air showers produced by ``superheavy'' nuclei, and discuss prospects for their detection in future experiments.""]",['2000-08-29'] +509,['eng'],"['Baudis, L', 'Dietz, A', 'Majorovits, B', 'Schwamm, F', 'Strecker, H', 'Klapdor-Kleingrothaus, H V']",['First Results from the Heidelberg Dark Matter Search Experiment'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, search for', 'semiconductor detector, germanium', 'semiconductor detector, performance', 'scattering, WIMP nucleon', 'total cross section, upper limit', 'deep underground detector, Gran Sasso', 'threshold, energy', 'experimental equipment', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008339'],"['The Heidelberg Dark Matter Search Experiment (HDMS) is a new ionization Germanium experiment in a special design. Two concentric Ge crystals are housed by one cryostat system, the outer detector acting as an effective shield against multiple scattered photons for the inner crystal, which is the actual dark matter target. We present first results after successfully running the prototype detector for a period of about 15 months in the Gran Sasso Underground Laboratory. We analyze the results in terms of limits on WIMP-nucleon cross sections and present the status of the full scale experiment, which will be installed in Gran Sasso in the course of this year.']",['2000-08-23'] +510,['eng'],"['Folomeev, V N', 'Gurovich, V T', 'Usupov, R']",['Phenomenon of Gamma-Ray Bursts as Relativistic Detonation of Scalar Fields'],['Astrophysics and Astronomy'],"['gamma ray burst', 'photon, cosmic radiation', 'field theory, scalar', 'energy, density', 'plasma, relativistic', 'matter, scalar', 'potential, gravitation', 'fireball', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008334'],"['In the modern Universe the existence of various forms of scalar fields is supposed. On the one hand these fields can explain recently discovered positive $\\Lambda$-term(see e.g. Ref. \\cite{ref:Sahni}), on the other hand its form cluster systems creating gravitational wells for galaxies and their clusters. At that a natural hypothesis is the existence of compact configurations (""stars"") from scalar fields with a large enough energy density and total mass. The hypothesis is that the energy of these fields can be converted in relativistic plasma by an explosive way. Such process can be initiated by collision of relativistic particles which form a relativistic microscopic fireball. Thus effective temperature can amount to value sufficient for change of phase for scalar fields. Then the wave of relativistic ""detonation"" similar to the same process in classical physics will be spread from this source. In this paper the parameters of such field star and process of detonation are estimated. If the effect of the indicated change of phase (or something similar to one) exists, it is possible to get the parameters of relativistic plasma (macroscopic fireball) which could generate gamma - bursts. If in the modern Universe there is such unique form of a matter as fields of high density it would be strange for Nature not to take advantage of the possibility to convert their energy to radiation by an explosive way.']",['2000-08-23'] +511,['eng'],"['Green, A M']",['The WIMP annual modulation signal and non-standard halo models'],['Astrophysics and Astronomy'],"['WIMP, search for', 'cosmic radiation, time variation', 'signal processing', 'WIMP, mass', 'matter, solar', 'velocity, rotational', 'geophysics', 'recoil, energy', 'data analysis method', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008318'],"[""Currently the best prospect for detecting Weakly Interacting Massive Particles (WIMPs) is via the annual modulation, which occurs due to the Earth's rotation around the Sun, of the direct detection signal. We investigate the effect of uncertainties in our knowledge of the structure of the galactic halo on the WIMP annual modulation signal. We evaluate the signal for three non-standard halo models: Evans' power-law halos, Michie models with an asymmetric velocity distribution and Maxwellian halos with bulk rotation. We then compare the theoretical predictions of these models with the experimental signal found by the DAMA experiment and investigate how the WIMP mass and interaction cross section determined depend on the halo model assumed. We find that the WIMP mass confidence limits are significantly extended to larger masses, with the shape of the allowed region in the mass-cross section plane depending on the model.""]",['2000-08-22'] +512,['eng'],"['Blanco-Pillado, J J', 'Olum, K D']",['Electromagnetic radiation from superconducting string cusps'],['Astrophysics and Astronomy'],"['astrophysics, string', 'superconducting, string', 'radiation, electromagnetic', 'radiation, emission', 'energy', 'current, chiral']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008297'],"['Cusps in superconducting cosmic strings produce strongly beamed electromagnetic radiation. To calculate the energy emitted requires taking into account the effect of the charge carriers on the string motion, which has previously been done only heuristically. Here, we use the known exact solution to the equations of motion for the case where the current is chiral to update previous calculations for the total energy, spectrum and angular distribution in that case. We analyze the dependence of the radiated energy on the cusp parameters, and discuss which types of cusp dominate the total radiation emitted from an ensemble.']",['2000-08-21'] +513,['eng'],"['Martins, C J A P']",['Cosmology with Varying Constants'],['Astrophysics and Astronomy'],"['talk, Lisbon 2000/07/27', 'talk, Lisbon 2000/07/12', 'inflationary universe', 'fundamental constant, fine structure', 'time variation', 'relativity theory, general', 'density, fluctuation', 'adiabatic', 'topology, defect', 'cosmic radiation, background', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008287'],"['I motivate and discuss some recent work on theories with varying constants, and consider some possible observational consequences and tests. Particular emphasis is given to models which can (almost) exactly mimic the predictions of standard inflationary models.']",['2000-08-21'] +514,['eng'],"['Dalal, N', 'Griest, K']",['Black Holes Must Die'],['Astrophysics and Astronomy'],"['black hole, horizon', 'astrophysics, fundamental constant', 'radiation, Hawking', 'vacuum state, energy', 'dimension, 2', 'tensor, energy-momentum']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008260'],"['In light of recent evidence suggesting a nonzero present-day cosmological constant, Adams, Mbonye, & Laughlin (1999) have considered the evolution of black holes in the presence of vacuum energy. Using the assumption that Lambda remains constant with time, and a conjecture based on a paper by Mallett (1986), they reach the remarkable conclusion that black holes with current mass greater than about 2*10^(-9) Msun will not Hawking evaporate in the distant future, but will instead absorb vacuum energy and grow to roughly the de Sitter horizon size. In this letter we reexamine black hole evaporation in the presence of vacuum energy, and find instead that all known black holes will eventually evaporate.']",['2000-08-18'] +515,['eng'],"['Bay, R C']",['Search for High Energy Neutrino Emission from Gamma-Ray Bursts with the A ntarctic Muon and Neutrino Detector Array (AMANDA)'],['Astrophysics and Astronomy'],"['thesis', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics', 'gamma ray burst', 'neutrino, flux', 'muon, cosmic radiation', 'muon, angular distribution', 'deep underground detector, AMANDA', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008255'],"['The photo-meson production of pions by shock-accelerated protons could generate a burst of ~10^14 eV neutrinos from gamma-ray bursts (GRBs) observable in the Antarctic Muon and Neutrino Detector Array (AMANDA) or its larger successors. Measurement of this flux can test the hypothesis that GRBs are the sources of the highest-energy cosmic rays, and GRB neutrinos could permit high-precision experiments in neutrino limiting speed, neutrino oscillations, and the weak equivalence principle. Neutrino emission can be expected primarily during the prompt gamma-ray flash and satellite coincidence provides a well-defined window in position and time that can be searched for an excess of upgoing muon events in AMANDA from bursts in the Northern Hemisphere. Using an event quality analysis to further reduce background in a sample of 78 GRBs from the 1997 AMANDA-B10 data set, I find a fluence limit of (E_nu)^2 (dN_nu)/(dE_nu)<3.8*10^-4 min(1,E_nu/E_break) [TeV cm^-2] per average burst, which is orders of magnitude more stringent than in similar previous searches.']",['2000-08-18'] +516,['eng'],"['Vernizzi, F', 'Melchiorri, A', 'Durrer, R']",['CMB anisotropies from pre-big bang cosmology'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'inflationary universe', 'axion, production', 'axion, fluctuation', 'astrophysics, string', 'astrophysics, missing-mass', 'matter, spectra', 'matter, perturbation', 'tensor, energy-momentum', 'decoherence', 'gravitational radiation, background', 'supernova', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008232'],"['We present an alternative scenario for cosmic structure formation where initial fluctuations are due to Kalb-Ramond axions produced during a pre-big bang phase of inflation. We investigate whether this scenario, where the fluctuations are induced by seeds and therefore are of isocurvature nature, can be brought in agreement with present observations by a suitable choice of cosmological parameters. We also discuss several observational signatures which can distinguish axion seeds from standard inflationary models. We finally discuss the gravitational wave background induced in this model and we show that it may be well within the range of future observations.']",['2000-08-17'] +517,['eng'],"['Bilic, N', 'Lindebaum, R J', 'Tupper, G B', 'Viollier, R D']",['The Dynamics of the Formation of Degenerate Heavy Neutrino Stars'],['Astrophysics and Astronomy'],"['neutrino, star', 'neutrino, heavy', 'star, production', 'fermion, gas', 'boson, condensation', 'black hole', 'galaxy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008230'],"['Through reformulating the cold, self-gravitating fermion gas as a Bose condensate by identifying their mutual Thomas-Fermi limits, the dissipationless formation of a heavy neutrino star in gravitational collapse is numerically demonstrated. Such stars offer an alternative to supermassive black holes for the compact dark objects at the centers of galaxies.']",['2000-08-17'] +518,['eng'],"['Cline, David B']",['A New Underground Laboratory in the USA for a Neutrino Factory Detector and Other Scientific Projects'],['Astrophysics and Astronomy'],"['talk, Monterey 2000/05/22', 'neutrino, counters and detectors', 'neutrino, oscillation', 'calorimeter, liquid argon', 'iron', 'magnet, ferromagnet', 'deep underground detector, Gran Sasso', 'deep underground detector, proposed']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008225'],"['A neutrino factory storage ring can provide beams to various locations. We discuss the ICANOE detector (at LNGS) at one such site. We then describe the prospects for the use of the underground location at Carlsbad, NM for a neutrino factory detector. A brief discussion is given of a simple magnetized Fe detector of 10 50 kT for this site.']",['2000-08-16'] +519,['eng'],"['Aharonian, F A', 'Akhperjanian, A G', 'Barrio, J A']",['The TeV Energy Spectrum of Mkn 501 Measured with the Stereoscopic Telescope System of HEGRA during 1998 and 1999'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'blazar', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008211'],"['During 1997, the BL Lac object Mkn 501 went into an extraordinary state of high X-ray and TeV gamma-ray activity, lasting more than 6 months. In this paper we report on the TeV emission characteristics of the source in the subsequent years of 1998 and 1999 as measured with the Stereoscopic Cherenkov Telescope System of HEGRA (La Palma, Canary Islands). Our observations reveal a 1998-1999 mean emission level at 1 TeV of 1/3 of the flux of the Crab Nebula, a factor of 10 lower than during the year of 1997. A dataset of 122 observations hours with the HEGRA telescope system makes it possible to assess for the first time the Mkn 501 TeV energy spectrum for a mean flux level substantially below that of the Crab Nebula with reasonable statistical accuracy. Excluding the data of a strong flare, we find evidence that the 1998--1999 low-flux spectrum is substantially softer (by 0.44+-0.1(stat) in spectral index) than the 1997 time averaged spectrum. The 500 GeV to 10 TeV energy spectrum can well be described by a power law model with exponential cutoff: dN/dE ~ E^(-alpha) exp(-E/E0) with alpha=2.31+-0.22(stat), and E0=5.1 (-2.3+7.8)(stat) TeV. Within statistical accuracy, also a pure power law model gives an acceptable fit to the data: dN/dE ~ E^(-Gamma) with Gamma=2.76+-0.08(stat). After presenting the 1998-1999 TeV characteristics of the source we discuss the implications of the results.']",['2000-08-16'] +520,['eng'],"['Kobayakawa, K', 'Sato, Y', 'Samura, T']",['Acceleration of Particles by Oblique Shocks and Cosmic Ray Spectra around the Knee Region'],['Astrophysics and Astronomy'],"['particle, acceleration', 'shock waves, oblique', 'magnetic field', 'cosmic radiation, primary', 'cosmic radiation, flux', 'energy spectrum', 'nucleus, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008209'],"['We consider the first order Fermi acceleration on the presumption that the shock fronts around supernova remnants cross outer magnetic fields with various angles. These oblique shocks concerned with, accelerate particles more efficiently than parallel shocks and elevate the achievable maximum energies. The primary cosmic ray spectrum is strongly dependent upon these energies. When indices and absolute fluxes at $10^{12}$ eV are given for several nuclear groups from experimental data, the total primary spectrum shows a smooth knee behavior at $\\sim 10^{15}$ eV and fits the flux data well up to several times of $10^{17}$ eV. It is also shown that the chemical composition changes significantly from lighter to heavier nuclei as energies of particles exceed the knee. It is compared with data, too.']",['2000-08-16'] +521,['eng'],"['Chiba, T', 'Nakamura, T']",['Feasibility of Reconstructing the Quintessential Potential Using SNIa Data'],['Astrophysics and Astronomy'],"['supernova', 'quintessence', 'effective potential', 'luminosity', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008175'],"['We investigate the feasibility of the method for reconstructing the equation of state and the effective potential of the quintessence field from SNIa data. We introduce a useful functional form to fit the luminosity distance with good accuracy (the relative error is less than 0.1%). We assess the ambiguity in reconstructing the equation of state and the effective potential which originates from the uncertainty in $\\Omega_M$. We find that the equation of state is sensitive to the assumed $\\Omega_M$, while the shape of the effective potential is not. We also demonstrate the actual reconstruction procedure using the data created by Monte-Carlo simulation. Future high precision measurements of distances to thousands of SNIa could reveal the shape of the quintessential potential.']",['2000-08-14'] +522,['eng'],"['Evans, N W', 'Carollo, C M', 'De Zeeuw, P T']",['Triaxial Haloes and Particle Dark Matter Detection'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'velocity, dispersion', 'scattering, WIMP nucleus', 'galaxy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008156'],"[""This paper presents the properties of a family of scale-free triaxial haloes. We adduce arguments to suggest that the velocity ellipsoids of such models are aligned in conical coordinates. We provide an algorithm to find the set of conically aligned velocity second moments that support a given density against the gravity field of the halo. The case of the logarithmic ellipsoidal model -- the simplest triaxial generalisation of the familiar isothermal sphere -- is examined in detail. The velocity dispersions required to hold up the self-consistent model are analytic. The velocity distribution of the dark matter can be approximated as a triaxial Gaussian with semiaxes equal to the velocity dispersions. There are roughly twenty experiments worldwide that are searching for evidence of scarce interactions between weakly-interacting massive-particle dark matter (WIMPs) and detector nuclei. The annual modulation signal, caused by the Earth's rotation around the Sun, is a crucial discriminant between WIMP events and the background. The greatest rate is in June, the least in December. We compute the differential detection rate for energy deposited by the rare WIMP-nucleus interactions in our logarithmic ellipsoidal halo models. Triaxiality and velocity anisotropy change the total rate by up to 40 %, and have a substantial effect on the amplitude of the annual modulation signal. The overall rate is greatest, but the amplitude of the modulation is weakest, in our radially anisotropic halo models. Even the sign of the signal can be changed. Restricting attention to low energy events, the models predict that the maximum rate occurs in December, and not in June.""]",['2000-08-11'] +523,['eng'],"['McDonald, P', 'Scherrer, R J', 'Walker, T P']",['Cosmic Microwave Background constraint on residual annihilations of relic particles'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, energy spectrum', 'particle, annihilation', 'cross section', 'mass', 'particle, density', 'energy, injection', 'helium, photofission', 'deuteron, production']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008134'],"['Energy injected into the Cosmic Microwave Background at redshifts z<10^6 will distort its spectrum permanently. In this paper we discuss the distortion caused by annihilations of relic particles. We use the observational bounds on deviations from a Planck spectrum to constrain a combination of annihilation cross section, mass, and abundance. For particles with (s-wave) annihilation cross section, <\\sigma|v|>=\\sigma_0, the bound is f[(\\sigma_0/6e-27cm^3/s)(\\Omega_{X\\bar{X}}h^2)^2]/(m_X/MeV)<0.2, where m_X is the particle mass, \\Omega_{X\\bar{X}} is the fraction of the critical density the particle and its antiparticle contribute if they survive to the present time, h=H_0/(100km/s/Mpc), H_0 is the Hubble constant, and f is the fraction of the annihilation energy that interacts electromagnetically. We also compute the less stringent limits for p-wave annihilation. We update other bounds on residual annihilations and compare them to our CMB bound.']",['2000-08-10'] +524,['eng'],"['Colafrancesco, Sergio', 'Melé, B']",['Neutralinos and the Origin of Radio Halos in Clusters of Galaxies'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutralino, annihilation', 'electron, cosmic radiation', 'electron, energy spectrum', 'galaxy, cluster', 'magnetic field', 'neutralino, mass', 'pi, cosmic radiation', 'numerical calculations, Monte Carlo', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008127'],"['We assume that the supersymmetric lightest neutralino is a good candidate for the CDM and explore the possibility to produce diffuse radio emission from high-energy electrons arising from the neutralino annihilation in galaxy clusters whose intracluster medium is filled with a large-scale magnetic field. We show that these electrons fit the population of seed relativistic electrons postulated in many models for the origin of cluster radio halos. For magnetic fields with central values $3 \\div 30$ $\\mu$G (depending on the DM profile), the population of seed relativistic electrons from neutralino annihilation can fit the radio halo spectra of Coma and 1E0657-56. The shape and the frequency extension of the radio halo spectra are connected with the mass and physical composition of the neutralino. A pure-gaugino neutralino with mass $M_{\\chi} \\geq 80$ GeV can reasonably fit the spectra of both Coma and 1E0657-56. This model provides a number of extra predictions that make it definitely testable. On the one hand, it agrees with the observations that {\\it (i)} the radio halo is centered on the cluster dynamical center, usually coincident with the X-ray center, {\\it (ii)} the radio halo surface brightness is similar to the X-ray one, and {\\it (iii)} the monochromatic radio luminosity at 1.4 GHz correlates strongly with the IC gas temperature. On the other hand, the model predicts that radio halos should be present in every cluster, which is not actually observed, although the predicted radio halo luminosities can change by a large amount ($\\sim 10^2 \\div 10^6$), depending on the amplitude and the structure of the IC magnetic field. Also, neutral pions arising from neutralino annihilation should give rise to substantial gamma-ray emission that could be tested by the next generation gamma-ray experiments.']",['2000-08-09'] +525,['eng'],"['Feng, J L', 'Matchev, K T', 'Wilczek, Frank']",['Prospects for Indirect Detection of Neutralino Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'supergravity, minimal', 'neutralino, annihilation', 'LSP, mass', 'neutrino, cosmic radiation', 'muon, flux', 'gaugino', 'Higgsino', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'positron, cosmic radiation', 'proposed experiment', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008115'],"[""Dark matter candidates arising in models of particle physics incorporating weak scale supersymmetry may produce detectable signals through their annihilation into neutrinos, photons, or positrons. A large number of relevant experiments are planned or underway. The `logically possible' parameter space is unwieldy. By working in the framework of minimal supergravity, we can survey the implications of the experiments for each other, as well as for direct searches, collider searches, low-energy experiments, and naturalness in a transparent fashion. We find that a wide variety of experiments provide interesting probes. Particularly promising signals arise in the mixed gaugino-Higgsino region. This region is favored by low-energy particle physics constraints and arises naturally from minimal supergravity due to the focus point mechanism. Indirect dark matter searches and traditional particle searches are highly complementary. In cosmologically preferred models, if there are charged superpartners with masses below 250 GeV, then some signature of supersymmetry must appear before the LHC begins operation.""]",['2000-08-08'] +526,['eng'],"['Watanabe, G', 'Iida, K']","[""Effects of Neutrino Trapping on Thermodynamic Properties of Nuclear ``Pasta''""]",['Astrophysics and Astronomy'],"['astrophysics, matter', 'supernova', 'nuclear matter, density', 'neutrino, gas', 'thermodynamics', 'model, liquid', 'critical phenomena', 'bubble', 'temperature, fluctuation', 'nucleon, energy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008108'],"['Geometrical structure of matter at subnuclear densities is investigated in the presence of a degenerate gas of neutrinos as encountered in stellar collapse. The crystalline phases with spherical, cylindrical and planar nuclei as well as with spherical and cylindrical nuclear bubbles are considered by using a compressible liquid-drop model. This model allows for uncertainties in the lepton fraction $Y_{\\rm L}$ in addition to those in the nuclear surface tension $E_{\\rm surf}$ and in the proton chemical potential in bulk neutron matter $\\mu_{\\rm p}^{(0)}$. The phase diagrams obtained at zero temperature show that only the phases with rod-like and slab-like nuclei occur at typical values of $Y_{\\rm L}$, $E_{\\rm surf}$ and $\\mu_{\\rm p}^{(0)}$, whereas the bubble phases, especially with spherical bubbles, are at best expected at hypothetically low values of $Y_{\\rm L}$ and/or $E_{\\rm surf}$. For the rod-like and slab-like nuclei, thermally induced displacements are calculated from their respective elastic constants. It is found that at temperatures appropriate to supernova cores, thermal fluctuations would destroy the layered lattice of slab-like nuclei almost independently of the nuclear models and of the degree of the neutrino degeneracy.']",['2000-08-08'] +527,['eng'],"['Amelino-Camelia, G', 'Piran, T']",['Planck-scale deformation of Lorentz symmetry as a solution to the UHECR and the TeV-$\\gamma$ paradoxes'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'space-time', 'symmetry breaking, Lorentz', 'dispersion relations, deformation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008107'],"['One of the most puzzling current experimental physics paradoxes is the arrival on Earth of Ultra High Energy Cosmic Rays with energies above the GZK threshold. The recent observation of 20TeV photons from Mk 501 is another somewhat similar paradox. Several models have been proposed for the UHECR paradox. No solution has yet been proposed for the TeV-$\\gamma$ paradox. Remarkably, the drastic assumption of a violation of ordinary Lorentz invariance would resolve both paradoxes. We present a formalism for the description of the type of Lorentz-invariance deformation (LID) that could be induced by non-trivial short-distance structure of space-time, and we show that this formalism is well suited for comparison of experimental data with LID predictions. We use the UHECR and TeV-$\\gamma$ data, as well as bounds on time-of-flight differences between photons of different energies, to constrain the LID parameter space. A model with only two parameters, an energy scale and a dimensionless parameter characterizing the functional dependence on the energy scale, is shown to be sufficient to solve both the UHECR and the TeV-$\\gamma$ threshold anomalies while satisfying the time-of-flight bounds. The allowed region of the two-parameter space is relatively small, but, remarkably, it fits perfectly the expectations of the quantum-gravity-motivated space-time models known to support such deformations of Lorentz invariance: integer value of the dimensionless parameter and characteristic energy scale constrained to a narrow interval in the neighborhood of the Planck scale.']",['2000-08-08'] +528,['eng'],"['Hayashida, N', 'Honda, K', 'Inoue, N', 'Kadota, K', 'Kakimoto, F', 'Kakizawa, S', 'Kamata, K', 'Kawaguchi, S', 'Kawasaki, Y', 'Kawasumi, N', 'Kusano, E', 'Mahrous, A M', 'Mase, K', 'Minagawa, T', 'Nagano, M', 'Nishikawa, D', 'Ohoka, H', 'Osone, S', 'Sakaki, N', 'Sasaki, M', 'Shinozaki, K', 'Takeda, M', 'Teshima, M', 'Torii, R', 'Tsushima, I', 'Uchihori, Y', 'Yamamoto, T', 'Yoshida, S', 'Yoshii, H']",['Updated AGASA event list above 4x10^19eV'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'showers, air', 'cosmic radiation, spatial distribution', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008102'],"['After our Ap.J. publication of the Akeno Giant Air Shower Array (AGASA) results in 1999 (Takeda et al., 1999), we observed nine events with energies above 4 $\\times$ 10$^{19}$eV until May 2000. This short report lists the coordinates of these events, and shows the updated energy spectrum and arrival direction map. The analysis was carried out with the same procedure employed in the Ap.J. publication.']",['2000-08-08'] +529,['eng'],"['Clarkson, C A']",['On the Observational Characteristics of Inhomogeneous Cosmologies'],['Astrophysics and Astronomy'],"['thesis', 'Thesis']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008089'],"[""This thesis concerns the compatibility of inhomogeneous cosmologies with our present understanding of the universe. It is a problem of some interest to find the class of all relativistic cosmological models which are capable of providing a reasonable `fit' to the universe. This thesis, in some respects, is part of this process. We consider Stephani models, which are a generalisation of the standard Friedmann-Lemaitre-Robertson-Walker (FLRW) models, which can be thought of as FLRW models with acceleration and pressure gradients. Thus these models generalise the `dust' assumption of standard cosmology. The crucial aspect of this work is the retention of the Copernican principle -- an assumption regarded by many as crucial to cosmology. It states that we are not at a special location in the universe. This is a vital aspect of the original work in this thesis: consideration of an inhomogeneous model, while retaining the Copernican principle has, as far as the author is aware, not been considered in detail before. We start by generalising the Ehlers-Geren-Sachs Theorem to identify the class of inhomogeneous spacetimes which allow an isotropic radiation field for all observers in the spacetime. We then investigate observational and physical aspects of these models from all observer locations. We conclude that there exist spacetimes which conform to present observational constraints (especially anisotropy constraints) for any location in the spacetime, while at the same time being significantly inhomogeneous; ie, not `almost-FLRW'.""]",['2000-08-07'] +530,['eng'],"['De Angelis, A']",['Study of Hadronic Decays of the Z Boson at LEP'],['Astrophysics and Astronomy'],"['talk, Osaka 2000/07/27', 'electron positron, colliding beams', 'electron positron, annihilation', 'Z0, electroproduction', 'Z0, hadronic decay', 'quark, pair production', 'hadron, multiple production', 'charged particle, multiplicity', 'final state, (2jet)', 'final state, (3jet)', 'pseudoscalar meson, yield', 'omega(783), yield', 'p, pair production', 'rapidity, difference', 'model, production', 'experimental results', 'CERN LEP Stor', 'approx. 91 GeV-cms']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008077'],"['This report summarizes four recent papers on the characteristics of the hadronic decays of the Z by the LEP collaborations ALEPH, DELPHI and OPAL.']",['2000-08-07'] +531,['eng'],"['Amenomori, M', 'Ayabe, S']",['Measurement of air shower cores to study the cosmic ray composition in the knee energy region'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'showers, air', 'showers, spatial distribution', 'cosmic radiation, energy spectrum', 'scintillation counter', 'nuclear emulsion', 'numerical calculations, Monte Carlo', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008043'],"['Since 1996, a hybrid experiment consisting of an emulsion chamber and a burst detector array and the Tibet-II air shower array has been operated at Yangbajing (4300 m above sea level) in Tibet. This experiment can detect air-shower cores, called burst events, accompanied by air showers in excess of about 100 TeV. Using the burst event data observed by this experiment, we discuss the primary cosmic ray composition around the knee in comparison with the Monte Carlo simulations. In this paper, we show that all the features of burst events are wholly compatible with the heavy enriched composition in the knee energy region.']",['2000-08-03'] +532,['eng'],"['Biermann, P L', 'Ahn, E J', 'Medina-Tanco, G A', 'Stanev, T']",['Origin of the highest energy cosmic rays observed'],['Astrophysics and Astronomy'],"['talk, Paris 1999/09/06', 'cosmic radiation, particle source', 'galaxy', 'magnetic field', 'particle, production']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008063'],"['Introducing a simple Galactic wind model patterned after the solar wind we show that back-tracing the orbits of the highest energy cosmic events suggests that they may all come from the Virgo cluster, and so probably from the active radio galaxy M87. This confirms a long standing expectation. Those powerful radio galaxies that have their relativistic jets stuck in the interstellar medium of the host galaxy, such as 3C147, will then enable us to derive limits on the production of any new kind of particle, expected in some extensions of the standard model in particle physics. New data from HIRES will be crucial in testing the model proposed here.']",['2000-08-04'] +533,['eng'],"['Blaschke, David B', 'Grigorian, H', 'Poghosyan, G']",['Conditions for deconfinement transition signals from compact star rotation'],['Astrophysics and Astronomy'],"['matter, rotational', 'accretion', 'critical phenomena, confinement', 'velocity', 'baryon number', 'quark, matter', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0008005'],['A phase diagram for compact stars in the angular velocity (Omega) - baryon number (N) plane is obtained with a dividing line for quark core configurations. Trajectories of compact star evolution in this diagram are studied for different scenarios defined by the external torque acting on the star due to radiation and/or mass accretion. They show a characteristic change in the rotational kinematics when entering the quark core regime. As a model independent signal for the existence of a deconfinement phase transition in compact stars a population clustering of accreting low-mass X-ray binaries in the Omega-N plane at the dividing line is suggested. We present the conditions under which this signal appears most pronounced.'],['2000-08-02'] +534,['eng'],"['Ayón-Beato, E', 'García, A', 'Mansilla, R', 'Terrero-Escalante, C A']",['The Stewart-Lyth Inverse Problem'],['Astrophysics and Astronomy'],"['inflationary universe', 'differential equations, nonlinear', 'differential equations, solution', 'potential, inflaton', 'perturbation, scalar', 'perturbation, tensor', 'geometry', 'phase space', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007477'],"['In this paper the Stewart-Lyth inverse problem is introduced. It consists of solving two non-linear differential equations for the first slow-roll parameter and finding the inflaton potential. The equations are derived from the Stewart-Lyth equations for the scalar and tensorial perturbations produced during the inflationary period. The geometry of the phase planes transverse to the trajectories is analyzed, and conclusions about the possible behaviour for general solutions are drawn.']",['2000-08-01'] +535,['eng'],"['Garcia de Andrade, L C']",['Cosmological density perturbation on spin dominated universes and COBE data'],['Astrophysics and Astronomy'],"['relativity theory, general', 'density, perturbation', 'spin, torsion', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, fluctuation', 'Friedman model, stability', 'gravitation, Einstein-Cartan', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007463'],['The evolution equation of cosmic density perturbation of a spin dominated universe in Einstein-Cartan gravity is obtained.Examples of inflationary cosmologies with spin are also given where we compute the density perturbations in terms of redshift and show that spin-torsion effects produce a growth on the inhomogeneity of the universe as the redshift is high.Spin-torsion effects are redshifted out when the Universe expands and would be rarely of importance in present day phase of the universe.Comparison with the primordial density fluctuation of COBE data is also obtained.From our computations a COBE type experiment could be proposed to measure the spin-torsion effects in large scale structure objects such as spiral Galaxies and globular clusters.'],['2000-08-01'] +536,['eng'],"['Binétruy, P', 'Silk, J']",['Probing large-distance higher-dimensional gravity with Cosmic Microwave Background measurements'],['Astrophysics and Astronomy'],"['gravitation, higher-dimensional', 'cosmic radiation, background', 'spectra, fluctuation', 'potential, gravitation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007452'],['It has been recently argued that higher dimensional gravity theories may manifest themselves not only at short microscopic distances but also at large cosmological scales. We study the constraints that cosmic microwave background measurements set on such large distance modifications of the gravitational potential.'],['2000-08-01'] +537,['eng'],"['Ave, M', 'Hinton, J A', 'Vázquez, R A', 'Watson, A A', 'Zas, E']",['New constraints from Haverah Park data on the photon and iron fluxes of UHE cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'energy spectrum, cosmic radiation', 'photon, cosmic radiation', 'iron, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007386'],"['Using data from inclined events ($60^{\\circ}<\\theta<80^{\\circ}$) recorded by the Haverah Park shower detector, we show that above 10^19 eV less than 30% of the primary cosmic rays can be photons or iron nuclei at the 95% confidence level. Above 4 10^19 eV less than 55% of the cosmic rays can be photonic at the same confidence level. These limits place important constraints on some models of the origin of ultra high energy cosmic rays. Details of two new events above 10^20 eV are reported.']",['2000-07-27'] +538,['eng'],"['Kinney, W H', 'Melchiorri, A', 'Riotto, A']",['New Constraints on inflation from the Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'field theory, scalar', 'baryon, density', 'light nucleus, production', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007375'],"[""The recent data from the Boomerang and MAXIMA-1 balloon flights have marked the beginning of the precision era of Cosmic Microwave Background anisotropy (CMB) measurements. We investigate the observational constraints from the current CMB anisotropy measurements on the simplest inflation models, characterized by a single scalar field $\\phi$, in the parameter space consisting of scalar spectral index $n_S$ and tensor/scalar ratio $r$. If we include constraints on the baryon density from big bang nucleosynthesis (BBN), we show that the favored inflationary models have negligible tensor amplitude and a ``red'' tilt, with a best fit of $n_S \\simeq 0.93$, which is consistent with the simplest ``small-field'' inflation models, but rules out large-field models at the $1\\sigma$ level. Without including BBN constraints, a broader range of models are consistent with the data. The best fit (assuming negligible reionization) is a scale-invariant spectrum, $n_S \\simeq 1$, which includes large-field and hybrid scenarios. Large-field models (such as chaotic and power-law inflation) with tilt $n_S < 0.9$ are strongly disfavored in all cases.""]",['2000-07-26'] +539,['eng'],"['Aharonian, F A']",['Optimizing the angular resolution of the HEGRA telescope system to study the emission region of VHE gamma rays in the Crab Nebula'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, angular distribution', 'Cherenkov counter, imaging', 'angular resolution', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007367'],"[""The HEGRA system of imaging atmospheric Cherenkov telescopes provides for specially selected classes of events an angular resolution of better than 3'. By comparing the measured angular distribution of TeV gamma rays from the Crab Nebula with the distribution expected on the basis of Monte Carlo simulations, and with measurements of gamma rays from the point source Mrk 501, we conclude that the rms size of the VHE gamma-ray emission region in the Crab Nebula is less than 1.5'.""]",['2000-07-26'] +540,['eng'],"['Bucher, M', 'Moodley, K', 'Turok, Neil G']",['Characterising the Primordial Cosmic Perturbations'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'density, perturbation', 'perturbation, adiabatic', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'space-time, perturbation', 'inflationary universe', 'numerical calculations', 'tables', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007360'],"[""The most general homogeneous statistical ensemble of linear scalar perturbations which are regular at early times, in a universe with only photons, baryons, neutrinos, and a cold dark matter (CDM) component, is described by a 5x5 symmetric matrix-valued generalization of the power spectrum. This description is complete if the perturbations are Gaussian, and even in the non-Gaussian case describes all observables quadratic in the small perturbations. The matrix valued power spectrum describes the auto- and cross-correlations of the adiabatic, baryon isocurvature, CDM isocurvature, neutrino density isocurvature, and neutrino velocity isocurvature modes. In this paper we examine the prospects for constraining or discovering isocurvature modes using forthcoming MAP and PLANCK measurements of the cosmic microwave background (CMB) anisotropy. We also consider the degradation in estimates of the cosmological parameters resulting from the inclusion of these modes. In the case of MAP measurements of the temperature alone, the degradation is drastic. When isocurvature modes are admitted, uncertainties in the amplitudes of the mode auto-- and cross--correlations, and in the cosmological parameters, become of order one. With the inclusion of polarisation (at an optimistic sensitivity) the situation improves but the isocurvature modes are still only weakly constrained. Measurements with PLANCK's estimated errors are far more constraining, especially so with the inclusion of polarisation. If PLANCK operates as planned the amplitudes of isocurvature modes will be constrained to less than ten per cent of the adiabatic mode and simultaneously the key cosmological parameters will be estimated to a few per cent or better.""]",['2000-07-25'] +541,['eng'],"['Garcia de Andrade, L C']",['Cosmological Density Perturbations in two fluid models on spin dominated inflation and the stability of Friedmann metric'],['Astrophysics and Astronomy'],"['inflationary universe', 'spin, fluid', 'Friedman model', 'density, perturbation', 'spin, torsion', 'matter', 'radiation', 'field equations, solution', 'stability', 'space-time, Einstein-Cartan']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007340'],['A spinning fluid embedded in a space section flat Friedmann model is used to compute the cosmological density perturbation of the model.The spinning fluid obeys the Einstein-Cartan field equations while the Friedmann embedded model is assumed to obey the general the Friedmann equation in General Relativity.It is shown that at the early epochs of the Universe the spin-torsion contribution to the density perturbation on the matter phase dominates over the radiation perturbation.On the other hand at the present epochs of the Universe the spin-torsion contribution is more efficient in the matter perturbation.Stability of the Friedmann solution in Einstein-Cartan cosmology is also discussed.'],['2000-07-25'] +542,['eng'],"['Alvarez-Muñiz, J', 'Halzen, Francis']",['10^20 eV Cosmic-Ray and Particle Physics with Kilometer-Scale Neutrino Telelscopes'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'energy spectrum, cosmic radiation', 'cosmic radiation, particle source', 'neutrino, flux', 'neutrino/mu', 'antineutrino/mu', 'particle physics', 'topology, defect', 'neutrino, energy spectrum', 'neutrino, cosmic radiation', 'angular distribution', 'counters and detectors, proposed', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007329'],"['We show that a kilometer-scale neutrino observatory, though optimized for TeV to PeV energy, is sensitive to the neutrinos associated with super-EeV sources. These include super-heavy relics, neutrinos associated with the Greisen cutoff, and topological defects which are remnant cosmic structures associated with phase transitions in grand unified gauge theories. It is a misconception that new instruments optimized to EeV energy are required to do this important science. Because kilometer-scale neutrino telescopes can reject atmospheric backgrounds by establishing the very high energy of the signal events, they have sensitivity over the full solid angle, including the horizon where most of the signal is concentrated. This is important because up-going neutrino-induced muons, routinely considered in previous calculations, are absorbed by the Earth.']",['2000-07-24'] +543,['eng'],[],['First search for gravitational wave bursts with a network of detectors'],['Astrophysics and Astronomy'],"['gravitational radiation, search for', 'counters and detectors, resonance', 'correlation, time', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007308'],"['We report the initial results of a multiple detector search for short bursts of gravitational radiation, covering 1997 and 1998 with data from a network of five cryogenic resonant detectors. This is the first significant search with more than two detectors observing simultaneously. A false alarm rate lower than 1 per $10^4$ years has been achieved when three or more detectors were operating simultaneously. The typical threshold was H ~ 4 10^{-21} Hz^{-1} on the Fourier component of the gravitational wave strain amplitude. New upper limits on amplitude and rate of g.w. bursts have been set.']",['2000-07-21'] +544,['eng'],"['Finelli, F']",['Cosmological magnetic fields by parametric resonance?'],['Astrophysics and Astronomy'],"['talk, Trieste 1999/09/27', 'astrophysics, model', 'fluctuation, electromagnetic', 'resonance', 'field theory, scalar', 'stability', 'magnetic field', 'Higgs model, abelian']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007290'],"['We investigate the possibility that electromagnetic fluctuations are amplified in expanding universe by parametric resonance, during the oscillatory regime of a scalar field to which they are coupled. We consider scalar electrodynamics and we find that electromagnetic fluctuations undergo exponential instabilities. This mechanism could have some relevance for the problem of large scale primordial magnetic fields.']",['2000-07-20'] +545,['eng'],"['Albrecht, Andreas']",['Cosmic Inflation'],['Astrophysics and Astronomy'],"['lectures, Cambridge 1999/07/26', 'Friedman model', 'inflationary universe', 'density, perturbation', 'coherence', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'phase space', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007247'],"[""I review the current status of the theory of Cosmic Inflation. My discussion covers the motivation and implementation of the idea, as well as an analysis of recent successes and open questions. There is a special discussion of the physics of ``cosmic coherence'' in the primordial perturbations. The issue of coherence is at the heart of much of the success inflation theory has achieved at the hands of the new microwave background data. While much of this review should be useful to anyone seeking to update their knowledge of inflation theory, I have also made a point of including basic material directed at students just starting research.""]",['2000-07-19'] +546,['eng'],"['Davis, A C', 'Dimopoulos, K', 'Prokopec, Tomislav', 'Tornkvist, O']",['Primordial Spectrum of Gauge Fields from Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'gauge field theory', 'invariance, conformal', 'symmetry breaking', 'spectra, perturbation', 'quantum electrodynamics, scalar', 'coupling, (Higgs particle Z0)', 'electroweak interaction, critical phenomena', 'magnetic field, production', 'magnetic field, spectra', 'photon, spectra', 'preheating', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007214'],"['We show that conformal invariance of gauge fields is naturally broken in inflation, having as a consequence amplification of gauge fields. The resulting spectrum of the field strength is approximately B_L ~ L^(-1), where L is the relevant coherence scale. One realisation of our scenario is scalar electrodynamics with a scalar whose mass is large enough to evade observational constraints - the obvious candidates being supersymmetric partners of the standard-model fermions. Our mechanism also leads naturally to amplification of the standard-model Z-boson field due to its coupling to the electroweak Higgs field. At preheating, the spectrum of the Z field is transferred to the hypercharge field, which remains frozen in the plasma and is converted into a magnetic field at the electroweak phase transition. With a reasonable model of field evolution one obtains a magnetic field strength of the order of $10^{-29}$ Gauss on a scale of 100 pc, the size of the largest turbulent eddy in a virialised galaxy. Resonant amplification in preheating can lead to primordial fields as large as $10^{-24}$ Gauss, consistent with the seed field required for the galactic dynamo mechanism.']",['2000-07-17'] +547,['eng'],"['Blasi, P']",['Opening the ultra high energy cosmic ray window from the top'],['Astrophysics and Astronomy'],"['talk, Vulcano 2000/05/22', 'cosmic radiation, primary', 'energy spectrum', 'particle source', 'particle physics, model', 'defect, topological', 'string model', 'bound state, monopole', 'postulated particle, heavy', 'postulated particle, lifetime', 'astrophysics, missing-mass', 'numerical calculations, Monte Carlo', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007209'],"['While several arguments can be proposed against the existence of particles with energy in excess of $(3-5)\\times 10^{19}$ eV in the cosmic ray spectrum, these particles are actually observed and their origin seeks for an explanation. After a description of the problems encountered in explaining these ultra-high energy cosmic rays (UHECRs) in the context of astrophysical sources, we will review the so-called {\\it Top-Down} (TD) Models, in which UHECRs are the result of the decay of very massive unstable particles, possibly created in the Early Universe. Particular emphasis will be given to the signatures of the TD models, likely to be accessible to upcoming experiments like Auger.']",['2000-07-17'] +548,['eng'],"['Bean, R', 'Magueijo, J']",['Dilaton-derived quintessence scenario leading naturally to the late-time acceleration of the Universe'],['Astrophysics and Astronomy'],"['matter, acceleration', 'quintessence', 'dilaton', 'relativity theory, general', 'astrophysics, missing-mass', 'string model', 'astrophysics, fundamental constant', 'potential', 'astrophysics, acceleration', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007199'],"[""Quintessence scenarios provide a simple explanation for the observed acceleration of the Universe. Yet, explaining why acceleration did not start a long time ago remains a challenge. The idea that the transition from radiation to matter domination played a dynamical role in triggering acceleration has been put forward in various guises. We propose a simple dilaton-derived quintessence model in which temporary vacuum domination is naturally triggered by the radiation to matter transition. In this model Einstein's gravity is preserved but quintessence couples non-minimally to the cold dark matter, but not to ``visible'' matter. Such couplings have been attributed to the dilaton in the low-energy limit of string theory beyond tree level. We also show how a cosmological constant in the string frame translates into a quintessence-type of potential in the atomic frame.""]",['2000-07-17'] +549,['eng'],"['Kawachi, A', 'Hayami, Y', 'Jimbo, J', 'Kamei, S', 'Kifune, T', 'Kubo, H', 'Kushida, J', 'Le Bohec, S', 'Miyawaki, K', 'Mori, M', 'Nishijima, K', 'Patterson, J R', 'Suzuki, R', 'Tanimori, T', 'Yanagita, S', 'Yoshikoshi, T', 'Yuki, A']",['The optical reflector system for the CANGAROO-II imaging atmospheric Cherenkov telescope'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'optics, reflection', 'photoelectron, amplifier', 'semiconductor, optical']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007194'],"['A new imaging atmospheric Cherenkov telescope (CANGAROO-II) with a light-weight reflector has been constructed. Light, robust, and durable mirror facets of containing CFRP (Carbon Fiber Reinforced Plastic) laminates were developed for the telescope. The attitude of each facet can be adjusted by stepping motors. In this paper, we describe the design, manufacturing, alignment procedure, and the performance of the CANGAROO-II optical reflector system.']",['2000-07-17'] +550,['eng'],"['Bednarek, W']",['Escape of VHE gamma-rays from close massive binary Cen X-3'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, primary', 'binary', 'radiation, background field', 'matter, massive', 'electron, cosmic radiation', 'electron, injection', 'pulsar', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'cosmic radiation, secondary radiation', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007183'],"[""We consider propagation of very high energy (VHE) gamma-rays in the radiation field of a massive star in the binary system Cen X-3, which has been reported as a source of gamma-ray photons in the GeV and TeV energies. VHE gamma-rays or electrons, injected by the compact object, should develop inverse Compton pair cascades. We predict the gamma-ray spectra and light curves for the parameters of Cen X-3 system. It is found that the gamma-ray spectra, observed at different directions, have different shape and intensity. The gamma-ray light curves, produced in the case of electron injection by the compact object in the Cen X-3 system, should have opposite tendencies for photons with energies above 100 MeV and above 300 GeV, i.e. the photon intensities increases with phase in the first case and decreases with phase in the second case. However the model with injection of primary electrons seems to be in contrary with the reported modulation of the GeV gamma-ray flux with the pulsar's period. The model with injection of primary photons allows such modulation with the pulsar's period, but predicts strong modulation of the TeV flux with the orbital period of the binary. Modulation of TeV emission with the orbital period has been reported by the early Cherenkov observations, but was not confirmed by the recent, more sensitive observations by the Durham Mark 6 telescope.""]",['2000-07-14'] +551,['eng'],"['Foschini, L']",['On the close encounter of stars and antistars'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'photon, cosmic radiation', 'galaxy, AGN', 'antimatter', 'accretion', 'matter, ejection', 'galaxy, cluster', 'radiation, pressure', 'luminosity', 'gamma ray burst']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007180'],"['The existence of large domains of antimatter is still an open question. Some space mission and experiments in the near future are expected to give reasonable answer to that question. Meanwhile, we can try to search for other signatures of the presence of antimatter. This paper presents a discussion about possible effects of the close encounter of stars and antistars. It is shown that the accretion power can be higher in presence of antimatter, because of high-energy photons generated in annihilation, which result in a smaller radiation pressure. Therefore, the Eddington luminosity can reach higher values.']",['2000-07-14'] +552,['eng'],"['Fryer, C L', 'Woosley, S E', 'Heger, A']","['Pair-Instability Supernovae, Gravity Waves, and Gamma-Ray Transients']",['Astrophysics and Astronomy'],"['matter, massive', 'supernova', 'light nucleus, production', 'angular momentum', 'black hole, production', 'stability, rotational', 'gravitational radiation', 'black hole, accretion', 'photon, cosmic radiation', 'neutrino, emission', 'transport theory', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007176'],"['Growing theoretical evidence suggests that the first generation of stars may have been quite massive (~100-300 solar masses). If they retain their high mass until death, such stars will, after about 3Myr, make pair-instability supernovae. We consider the complete evolution of two zero-metallicity stars of 250 and 300 solar masses. Explosive oxygen and silicon burning cause the 130 solar mass helium core to explode, but explosive burning is unable to drive an explosion in the 300 solar mass star and it collapses to a black hole. For this star, the calculated angular momentum in the presupernova model is sufficient to delay black hole formation and the star initially forms a 50 solar mass, 1000km core within which neutrinos are trapped. Although the star does not become dynamically unstable, the calculated growth time of secular rotational instabilities is shorter than the black hole formation time, and such instabilities may develop. We estimate the energy and amplitude of the gravitational waves emitted during this collapse. After the black hole forms, accretion continues through a disk. Although the disk is far too large and cool to transport energy efficiently to the rotational axis by neutrino annihilation, it has ample potential energy to produce a 1e54erg jet driven by magnetic fields. The interaction of this jet with surrounding circumstellar gas may produce an energetic gamma-ray transient, but given the redshift and time scale, this is probably not a model for typical gamma-ray bursts.']",['2000-07-14'] +553,['eng'],"['Primack, Joel R', 'Gross, M A K']",['Hot Dark Matter in Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'galaxy, production', 'matter, density', 'neutrino, oscillation', 'neutrino, mass', 'spectra, nonlinear', 'spectra, missing-mass', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007165'],"['Cosmological dark matter in the form of neutrinos with masses of up to a few electron volts is known as hot dark matter. After an historical review of the subject, this article considers constraints on hot dark matter from current data on neutrino oscillations and on cosmology. The atmospheric neutrino oscillation data imply a lower limit on the HDM contribution to the cosmological density $\\Omega_\\nu \\gsim 0.001$. The possible improvement of low-$\\Omega_m$ flat ($\\Lambda$CDM) cosmological models with the addition of light neutrinos appears to be rather limited, but$\\Lambda$CDM models with $\\Omega_\\nu \\lsim 0.1$ may be consistent with presently available data. Data expected soon may permit detection of such a hot dark matter contribution, or alternatively provide stronger upper limits on $\\Omega_\\nu$ and neutrino masses.']",['2000-07-13'] +554,['eng'],"['Larson, S L', 'Schild, R']",['Can gravitational waves be detected in quasar microlensing?'],['Astrophysics and Astronomy'],"['gravitational radiation, measurement', 'quasar', 'gravitation, lens', 'black hole, binary', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007142'],"['Studies of the lensed quasar ${\\rm Q}0957+561 {\\rm A,B}$ have shown evidence for microlensing in the brightness history of the quasar images. It had been suggested that a frequency offset between the brightness fluctuations in each of the two images might possibly be caused by gravitational radiation generated by a massive black hole binary at the center of the lensing galaxy. This paper demonstrates that the fluctuations produced by such a source of gravitational waves will be too small to account for the observed frequency offsets.']",['2000-07-12'] +555,['eng'],"['Kerins, E J']",['MACHOs and the clouds of uncertainty'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2000/03/11', 'gravitation, lens', 'MACHO, mass', 'baryon, matter', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007137'],"['I review proposals for explaining the current gravitational microlensing results from the EROS and MACHO surveys towards the Magellanic Clouds. Solutions involving massive compact halo objects (MACHOs), both baryonic and non-baryonic, as well as solutions that do not require MACHOs, are discussed. Whilst the existence and nature of MACHOs remains to be established, the prospects for achieving this over the next few years are good.']",['2000-07-12'] +556,['eng'],"['De Ritis, R', 'Marino, A A']","['Effective cosmological ""constant "" and quintessence']",['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'quintessence', 'fundamental constant, decay', 'astrophysics, expansion', 'asymptotic behavior', 'space-time, Robertson-Walker', 'Friedman model', 'symmetry, Noether', 'potential', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007128'],"['In this paper we present exactly solved extended quintessence models; furthermore, through a dynamical effective Q-cosmological ""constant"", we recover some of the L decaying cases found in the literature. Finally we introduce a sort of complementarity between the Q-dominated or L-dominated expansions of the Universe.']",['2000-07-12'] +557,['eng'],"['Levinson, A']",['A Note on TeV Cerenkov Events as Bose-Einstein Gamma Condensations'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'showers, air', 'radiation, Cherenkov', 'critical phenomena', 'boson, statistics', 'optics, laser', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007109'],"['The idea that the TeV air showers, thought to be produced by >10 TeV gamma rays from Mrk 501, can be mimicked by coherent bunches of sub-TeV photons is reexamined, focusing on fundamental considerations. In particular, it is shown that the minimum spot size of the beam of pulsed TeV photons arriving at Earth is on the order of a few kilometers, unless a lens with certain characteristics is placed between the TeV laser and Earth. The viability of the laser production mechanism proposed by Harwit et al. (2000) is also reassessed.']",['2000-07-12'] +558,['eng'],"['Mészáros, P', 'Rees, M J']",['Multi-GeV Neutrinos from Internal Dissipation in GRB Fireballs'],['Astrophysics and Astronomy'],"['GRB', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'neutrino, cosmic radiation', 'neutrino, flux', 'neutrino/mu', 'neutrino/e', 'fireball, relativistic', 'shock waves', 'n, diffusion', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007102'],"['Sub-photospheric internal shocks and transverse differences of the bulk Lorentz factor in relativistic fireball models of GRB lead to neutron diffusion relative to protons, resulting in inelastic nuclear collisions. This produces significant fluxes of ~3 GeV muon neutrinos (antineutrinos) and ~2 GeV electron neutrinos (antineutrinos), scaling with the Lorentz factor eta < 400. This extends significantly the parameter space for which neutrinos from inelastic collision are expected, which in the absence of the above effects requires eta > 400. A model with sideways diffusion of neutrons from a slower wind into a fast jet can lead to production of muon and electron neutrinos (antineutrinos) in the 2-25 GeV or higher range, depending on the value of eta. The emission from either of these mechanisms at z~1 may be detectable in suitably densely spaced detectors.']",['2000-07-12'] +559,['eng'],"['Pelletier, G', 'Kersale, E']",['Acceleration of UHE Cosmic Rays in Gamma-Ray Bursts'],['Astrophysics and Astronomy'],"['GRB', 'cosmic radiation, primary', 'cosmic radiation, acceleration', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'plasma, stability', 'fireball', 'baryon, flux', 'model, hydrodynamical', 'magnetic field', 'backscatter', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007096'],"[""Gamma-Ray Bursts are good candidates of the ``bottom up'' scenario for the generation of the UHE Cosmic Rays. In the most discussed model of GRBs, namely the ``fireball'' model, a highly relativistic shock forms and seems capable of accelerating the cosmic rays up to the EeV range. However, only the first Fermi cycle produces a large energy gain to particles coming from the external medium. Thus, a complementary acceleration is proposed, downstream of the external shock, in the relativistic plasma of the GRBs, where crossings of relativistic fronts are likely to occur. Both forward and backward fronts are necessary for the internal Fermi acceleration to work and the physical process that generates them is presented. We found that there exists a relevant physical process similar to Brillouin backscattering that redistributes the incoming energy in the plasma shell. This redistribution occurs through the generation of sound waves that heat the plasma shell and also through the generation of both forward and backward relativistic Alfven fronts that accelerate cosmic rays by the Fermi process. We show that this ensemble of processes is able to account for the generation of UHE cosmic rays. There are two opportunities for these combined processes, first during the ``primary'' Gamma-Ray Burst where baryons are entrained by the relativistic pair wind, second during the predeceleration and deceleration stages when the fireball interacts with the interstellar medium. However, because of the synchrotron losses, only the second stage can produce the UHE cosmic rays.""]",['2000-07-10'] +560,['eng'],"['Ushomirsky, G', 'Cutler, C', 'Bildsten, L']",['Deformations of Accreting Neutron Star Crusts and Gravitational Wave Emission'],['Astrophysics and Astronomy'],"['n, matter', 'accretion', 'gravitational radiation, emission', 'electron, capture', 'temperature, asymmetry', 'moment, multipole', 'temperature, perturbation', 'flux, perturbation', 'dependence, pressure', 'matter, deformation', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001136'],"['Motivated by the narrow range of spin frequencies of nearly 20 accreting neutron stars, Bildsten (1998) conjectured that their spin-up had been halted by the emission of gravitational waves. He also pointed out that small nonaxisymmetric temperature variations in the accreted crust will lead to ""wavy"" electron capture layers, whose horizontal density variations naturally create a mass quadrupole moment. We present a full calculation of the crust\'s elastic adjustment to these density perturbations and find that the elastic response of the crust reduces Bildsten\'s original estimate of the quadrupole moment in the thin outer crust by a factor of 20-50. However, this basic picture, when applied to capture layers in the deep inner crust, can generate quadrupoles in the necessary range as long as there are ~5% lateral temperature variations in the inner crust. By calculating the thermal flow throughout the core and the crust, we find that temperature gradients this large are easily maintained by asymmetric heat sources or lateral composition gradients in the crust. We also derive a general relation between the stresses and strains in the crust and the maximum quadrupole moment they can generate. We show under quite general conditions that maintaining a quadrupole of the magnitude necessary to balance the accretion torque requires dimensionless strains close to 0.01 at near-Eddington accretion rates, of order the breaking strain of conventional materials.']",['2000-01-11'] +561,['eng'],"['Johri, V B']",['Constraints over Cosmological Constant and Quintessence Fields in an Accelerating Universe'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'astrophysics, missing-mass', 'quintessence', 'expansion, acceleration', 'matter, density', 'light nucleus, production', 'galaxy, production', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007079'],"['A brief account of the current cosmological observations is given and their implications for QCDM and $\\Lambda$CDM cosmologies are discussed. The nucleosynthesis and the galaxy formation constraints have been used to put limits on $\\Omega_\\phi$ during cosmic evolution, and develop a realistic approach to the tracking behaviour of quintessence fields. The astrophysical constraints are applied to interpolate the value of the tracking parameter $\\epsilon \\simeq 0.75$ at the present epoch and also to find the lower and the upper limits for $\\Lambda$ in the accelerating universe. It is shown that the transition from deceleration to acceleration in the cosmic expansion occurs earlier in $\\Lambda$CDM cosmology compared to QCDM cosmology.']",['2000-07-07'] +562,['eng'],"['Cea, P', 'Fogli, G L', 'Tedesco, L']",['Influence of the Magnetic Field on the Fermion Scattering off Bubble and Kink Walls'],['Astrophysics and Astronomy'],"['fermion, scattering', 'domain wall, bubble', 'domain wall, kink', 'electroweak interaction, critical phenomena', 'magnetic field', 'Dirac equation, solution', 'zero mode', 'baryon, production', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007053'],"['We investigate the scattering of fermions off domain walls at the electroweak phase transition in presence of a magnetic field. We consider both the bubble wall and the kink domain wall. We derive and solve the Dirac equation for fermions with momentum perpendicular to the walls, and compute the transmission and reflection coefficients. In the case of kink domain wall, we briefly discuss the zero mode solutions localized on the wall. The possibile role of the magnetic field for the electroweak baryogenesis is also discussed.']",['2000-07-06'] +563,['eng'],"['Elze, H T', 'Kodama, T', 'Opher, R']","[""Collective Modes in Neutrino `Beam' Electron-Positron Plasma Interactions""]",['Astrophysics and Astronomy'],"['neutrino electron, interaction', 'electron, plasma', 'neutrino, beam', 'transport theory, quasiclassical', 'Dirac equation', 'cross section, energy dependence', 'collective phenomena, pharon', 'temperature, dependence', 'momentum dependence', 'supernova', 'neutrino, energy', 'dispersion relations', 'stability']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007024'],"['We derive semiclassical neutrino-electron transport equations in the collisionless (Vlasov) limit from the coupled Dirac equations, incorporating the charged and neutral weak current-current as well as electromagnetic interactions. A corresponding linear response theory is derived. In particular, we calculate the response functions for a variety of beam-plasma geometries, which are of interest in a supernova scenario. We apply this to the study of plasmons and to a new class of collective {\\it pharon} resonance modes, which are characterized by $\\omega < q$. We find that the growth rates of the unstable modes correspond to a strongly temperature ($\\propto T_\\nu^2T_e^3$) and linearly momentum dependent e-folding length of about $10^{10}$ km (optimistically estimated) under typical conditions for Type II supernovae. This appears to rule out such long-wavelength collective modes as an efficient means of depositing neutrino energy into the plasma sphere.']",['2000-07-04'] +564,['eng'],"['Karaca, K', 'Bayin, S S']",['An Open Singularity-Free Cosmological Model with Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'Hubble constant', 'temperature', 'critical phenomena', 'matter, density', 'space-time, Robertson-Walker', 'boundary condition', 'radiation', 'Einstein equation, solution', 'numerical calculations', 'tables']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007019'],"['In the light of recent observations which point to an open universe $\\Omega_0<1$, we consider the singularity-free models, originally constructed for closed universes. Our model starts from a nonsingular state called prematter, governed by an inflationary equation of state $P=(\\gamma_p-1)\\rho$, where $\\gamma_p$ is a small positive parameter representing the initial vacuum dominance of the universe. Unlike the closed models universe cannot be initially static hence, starts with an initial ecxpansion rate represented by the initial value of the Hubble constant H(0). Therefore, our model is a two-parameter universe model ($\\gamma_p$, H(0)). During the prematter phase, due to the unusual characteristic of the equation of state, universe heats up even though it expands. When the temperature in the universe reaches the Planck temperature $T_{pl}$ which is taken as the maximum attainable physical temperature, a first order phase transition carries the universe into the radiation era. Then the universe starts to behave as predicted in the standard model. The model proposed in this work predicts a value between 60 and 80 Km/sec/Mpc for the present value of the Hubble constant ($H_{0}$) and the predicted value of $\\Omega_0$ lies between 0.3 and 0.6. Comparing the predictions of this model for the present properties of the universe with the recent observational results, we argue that the model constructed in this paper could be used as a realistic universe model.']",['2000-07-04'] +565,['eng'],[],['Searches for astronomical neutrino sources and WIMPs with Super-Kamiokande'],['Astrophysics and Astronomy'],"['talk, Osaka 2000/07/27', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'WIMP, search for', 'muon, cosmic radiation', 'WIMP, annihilation', 'muon, flux', 'WIMP, mass', 'Cherenkov counter, water', 'data analysis method', 'deep underground detector, KAMIOKANDE', 'experimental results']","['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0007003', 'http://arXiv.org/abs/astro-ph/?0007003']","['Searches for astronomical neutrino sources and weakly interactive massive particles (WIMPs) using the Super-Kamiokande detector have been performed. We select the neutrino-induced upward muon events for the first 4 years, which is already the world largest data sample, and look for statistically significant excesses compared to the atmospheric neutrino background. No excess has been found so far. Limits of upward muon flux from various potential sources are obtained. Also limits of upward muon flux due to annihilations of WIMPs in the Earth core, the Sun and the Galactic center are obtained as a function of WIMP masses.']",['2000-07-04'] +566,['eng'],"['Brisudova, M M']",['An attempt to do without dark matter'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, missing-mass', 'baryon number', 'galaxy, cluster', 'gravitation, correction', 'gravitation, lens', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006453'],"[""The discrepancy between dynamical mass measures of objects such as galaxies and the observed distribution of luminous matter in the universe is typically explained by invoking an unseen ``dark matter'' component. Dark matter must necessarily be non-baryonic. We introduce a simple hypothesis to do away with the necessity for dark matter by introducing an additional non-gravitational force coupled to baryon number as a charge. We compare this hypothesis to Milgrom's Modified Newtonian Dynamics. The model ultimately fails when confronted with observation, but it fails in an interesting way.""]",['2000-07-03'] +567,['eng'],"['Kurki-Suonio, H', 'Sihvola, E']",['Antimatter Regions in the Early Universe and Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'antimatter, annihilation', 'helium, yield', 'helium, nuclide', 'deuterium', 'cosmic radiation, background', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006448'],"['We have studied big bang nucleosynthesis in the presence of regions of antimatter. Depending on the distance scale of the antimatter region, and thus the epoch of their annihilation, the amount of antimatter in the early universe is constrained by the observed abundances. Small regions, which annihilate after weak freezeout but before nucleosynthesis, lead to a reduction in the 4He yield, because of neutron annihilation. Large regions, which annihilate after nucleosynthesis, lead to an increased 3He yield. Deuterium production is also affected but not as much. The three most important production mechanisms of 3He are 1) photodisintegration of 4He by the annihilation radiation, 2) pbar-4He annihilation, and 3) nbar-4He annihilation by ""secondary"" antineutrons produced in anti-4He annihilation. Although pbar-4He annihilation produces more 3He than the secondary nbar-4He annihilation, the products of the latter survive later annihilation much better, since they are distributed further away from the annihilation zone.']",['2000-07-03'] +568,['eng'],"['Boyanovsky, D', 'De Vega, H J']",['Out of Equilibrium Fields in Self-consistent Inflationary Dynamics. Density Fluctuations'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time, Robertson-Walker', 'space-time, de Sitter', 'thermodynamics', 'inflaton, fluctuation', 'particle, production', 'symmetry breaking', 'expansion 1/N', 'renormalization', 'tensor, energy-momentum', 'symmetry, O(N)', 'approximation, quasiclassical', 'nonperturbative', 'density, perturbation', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006446'],"[""The physics during the inflationary stage of the universe is of quantum nature involving extremely high energy densities. Moreover, it is out of equilibrium on a fastly expanding dynamical geometry.We present in these lectures non-perturbative out of equilibrium field theoretical methods in cosmological universes. We then study the non-linear dynamics of quantum fields in matter and radiation dominated FRW and de Sitter universes. We investigate the explosive particle production due to spinodal instabilities and parametric amplification in FRW and deSitter universes with and without symmetry breaking. We show how the particle production is sensitive to the expansion of the universe.We present a complete renormalization scheme for the equation of motion and the energy momentum tensor in flat cosmologies. We then consider an O(N) inflaton model coupled self-consistently to gravity in the semiclassical approximation, with `new inflation' type initial conditions. We study the dynamics self-consistently and non-perturbatively with non-equilibrium field theory methods in the large N limit. We find that spinodal instabilities drive the growth of non-perturbatively large quantum fluctuations which shut off the inflationary growth of the scale factor. A very specific combination of these large quantum fluctuations plus the inflaton zero mode assemble into a new effective field. This new field behaves classically and it is the object which actually rolls down. The metric perturbations during inflation are computed using this effective field and the Bardeen variable for superhorizon modes during inflation. We compute the amplitude and index for the spectrum of scalar density and tensorperturbations and find for these models that the spinodal instabilities are responsible for a `red' primordial spectrum.""]",['2000-07-03'] +569,['eng'],"['Kanazawa, T', 'Kawasaki, M', 'Sugiyama, N', 'Yanagida, T']",['Double Inflation in Supergravity and the Boomerang Observations'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'supergravity', 'density, fluctuation', 'baryon, density', 'light nucleus, production', 'galaxy, cluster', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006445'],"['One of the biggest mystery of the recent observation of cosmic microwave background anisotropies by the boomerang team is insignificance of the second acoustic peak in the angular power spectrum. It is very difficult to explain such a low amplitude without assuming the higher baryon density than predicted by the Big Bang Nucleosynthesis (BBN). Employing the double inflation model in supergravity, we show that the density fluctuations produced by this inflation model can produce a sufficient low second acoustic peak with the standard value of the baryon density from BBN. It is shown that these density fluctuations are also consistent with the observations of cluster abundances and galaxy distributions.']",['2000-07-03'] +570,['eng'],"['Kutschera, M', 'Niemiec, J']",['Mixed quark-nucleon phase in neutron stars and nuclear symmetry energy'],['Astrophysics and Astronomy'],"['n, matter', 'matter, mass', 'critical phenomena, quark hadron', 'quark, matter', 'nuclear matter, parametrization', 'bag model', 'symmetry, energy', 'pressure', 'quark, droplet', 'effect, finite size', 'potential, Coulomb', 'surface tension', 'potential, chemical', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006440'],"['The influence of the nuclear symmetry energy on the formation of a mixed quark-nucleon phase in neutron star cores is studied. We use simple parametrizations of the nuclear matter equation of state, and the bag model for the quark phase. The behavior of nucleon matter isobars, which is responsible for the existence of the mixed phase, is investigated. The role of the nuclear symmetry energy changes with the value of the bag constant B. For lower values of B the properties of the mixed phase do not depend strongly on the symmetry energy. For larger B we find that a critical pressure for the first quark droplets to form is strongly dependent on the nuclear symmetry energy, but the pressure at which last nucleons disappear is independent of it.']",['2000-07-03'] +571,['eng'],"['Copeland, E J', 'Liddle, A R', 'Lidsey, J E']",['Steep inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'membrane model', 'particle, production', 'gravitation', 'potential', 'density, perturbation', 'field theory, scalar', 'dimension, 5', 'cosmic radiation, background', 'scaling']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006421'],"['We propose a scenario for inflation based upon the braneworld picture, in which high-energy corrections to the Friedmann equation permit inflation to take place with potentials ordinarily too steep to sustain it. Inflation ends when the braneworld corrections begin to lose their dominance. Reheating may naturally be brought about via gravitational particle production, rather than the usual inflaton decay mechanism; the reheat temperature may be low enough to satisfy the gravitino bound and the Universe becomes radiation dominated early enough for nucleosynthesis. We illustrate the idea by considering steep exponential potentials, and show they can give satisfactory density perturbations (both amplitude and slope) and reheat successfully. The scalar field may survive to the present epoch without violating observational bounds, and could be invoked in the quintessential inflation scenario of Peebles and Vilenkin.']",['2000-06-30'] +572,['eng'],"['Liebendoerfer, M', 'Mezzacappa, A', 'Thielemann, F K', 'Messer, O E B', 'Hix, W R', 'Bruenn, S W']",['Tapping the Gravitational Well'],['Astrophysics and Astronomy'],"['relativity theory, general', 'supernova', 'neutrino, cosmic radiation', 'transport theory', 'Boltzmann equation', 'energy', 'model, hydrodynamical', 'neutrino, luminosity', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006418'],"['We report on the vigorous supernova explosion of a 13 solar mass star, obtained in a general relativistic spherically symmetric simulation based on Boltzmann neutrino transport. Contrary to the prevailing opinion, the shock revival is more efficient than in the corresponding Newtonian simulation, producing an explosion energy of 10^{51} erg (1 foe) at 187 ms after bounce.']",['2000-06-29'] +573,['eng'],"['Brown, L S', 'Sawyer, R F']",['Finite temperature corrections to weak rates prior to nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'p n, transition', 'weak interaction', 'correction, electromagnetic', 'electron p, interaction', 'plasma, correction', 'finite temperature', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006370'],"['We have reexamined the electromagnetic corrections to the weak interaction rates for the transformation of neutrons to protons, and protons to neutrons, in the early universe, before freeze-out. We derive compact expressions for these rates in terms of thermal expectation values of products of fields, and we give explicit constructions of the terms to order e^2. We disagree in several respects with results in the literature.']",['2000-06-27'] +574,['eng'],"['Martín, J', 'Riazuelo, A', 'Schwarz, Dominik J']",['Slow-roll inflation and CMB anisotropy data'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'moment, multipole', 'data analysis method', 'gravitational radiation', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006392'],"['We emphasize that the estimation of cosmological parameters from CMB anisotropy data, such as the recent high resolution maps from BOOMERanG and MAXIMA-1, requires assumptions on the primordial spectra. The latter are predicted from inflation. The physically best motivated scenario is slow-roll inflation. However, very often the unphysical power-law inflation scenario is (implicitly) assumed in the CMB data analysis. We show that the predicted multipole moments differ significantly in both cases. We identify several misconceptions present in the literature (and in popular numerical codes), among others, generically inflation does neither predict $n_S-1=n_T$ nor that gravitational waves are negligible. We calculate the CMB multipole moments for various values of the slow-roll parameters and demonstrate that an important part of the space of parameters $(n_S,n_T)$ has been overlooked in the CMB data analysis so far.']",['2000-06-28'] +575,['eng'],"['Stodolsky, L']",['Looking Back with Neutrinos'],['Astrophysics and Astronomy'],"['talk, Columbia 2000/03/10', 'neutrino, mass', 'effect, time-of-flight', 'astrophysics, model', 'photon, cosmic radiation', 'WIMP']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006384'],"[""We briefly discuss the history of suggestions for time- of-flight effects due to non-zero neutrino mass and a recent proposal that such effects can be used to determine the parameters of cosmology. With neutrinos there is potentially a much deeper ``look back time'' than with photons. We note a new point, that if future large scale neutrino detection arrays see long-time secular variations in counting rate, this could be due to highly redshifted bursts originating in the early universe.""]",['2000-06-28'] +576,['eng'],"['Rehm, J B', 'Jedamzik, K']",['Limits on Cosmic Matter--Antimatter Domains from Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'baryon, diffusion', 'expansion, hydrodynamical', 'nucleon antinucleon, annihilation', 'baryon, density', 'antimatter', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006381'],"['We present detailed numerical calculations of the light element abundances synthesized in a Universe consisting of matter- and antimatter- domains, as predicted to arise in some electroweak baryogenesis scenarios. In our simulations all relevant physical effects, such as baryon-antibaryon annihilations, production of secondary particles during annihilations, baryon diffusion, and hydrodynamic processes are coupled to the nuclear reaction network. We identify two dominant effects, according to the typical spatial dimensions of the domains. Small antimatter domains are dissipated via neutron diffusion prior to He4 synthesis at T_He4 \\approx 80 keV, leading to a suppression of the primordial He4 mass fraction. Larger domains are dissipated below T_He4 via a combination of proton diffusion and hydrodynamic expansion. In this case the strongest effects on the elemental abundances are due to anti-p He4 annihilations, leading to an overproduction of He3 relative to H2 and to overproduction of Li6 via non-thermal nuclear reactions. Both effects may result in light element abundances deviating substantially from the standard Big Bang Nucleosynthesis yields and from the observationally inferred values. This allows us to derive stringent constraints on the antimatter parameters. For some combinations of the parameters, one may obtain both, low H2 and low He4, at a common value of the cosmic baryon density, a result seemingly favored by current observational data.']",['2000-06-28'] +577,['eng'],"['Armendariz-Picon, C', 'Mukhanov, V', 'Steinhardt, Paul Joseph']",['Essentials of k-essence'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'matter, expansion', 'field theory, scalar', 'attractor', 'energy, density', 'astrophysics, fundamental constant', 'critical phenomena', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006373'],"['We recently introduced the concept of ""k-essence"" as a dynamical solution for explaining naturally why the universe has entered an epoch of accelerated expansion at a late stage of its evolution. The solution avoids fine-tuning of parameters and anthropic arguments. Instead, k-essence is based on the idea of a dynamical attractor solution which causes it to act as a cosmological constant only at the onset of matter-domination. Consequently, k-essence overtakes the matter density and induces cosmic acceleration at about the present epoch. In this paper, we present the basic theory of k-essence and dynamical attractors based on evolving scalar fields with non-linear kinetic energy terms in the action. We present guidelines for constructing concrete examples and show that there are two classes of solutions, one in which cosmic acceleration continues forever and one in which the acceleration has finite duration.']",['2000-06-28'] +578,['eng'],"['Banerjee, S', 'Ghosh, S K', 'Mazumdar, A', 'Raha, S', 'Syam, D']",['Strange quark matter in cosmic ray flux and exotic events'],['Astrophysics and Astronomy'],"['cosmic radiation, flux', 'quark, matter', 'matter, strangeness', 'geophysics', 'matter, mass', 'matter, charge', 'counters and detectors, proposed', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006354'],"['There have been several reports of exotic nuclear fragments, with highly unusual charge to mass ratio, in cosmic ray experiments. Although there exist experimental uncertainties which make them, at best, only candidate ""exotic"" events, it is important to understand what they could be, if they are eventually confirmed. Among other possible explanations, some authors have interpreted them to be lumps of strange quark matter (strangelets). A major problem with such an interpretation is that to reach the earth\'s surface, they must possess an unusually high penetrability through the terrestrial atmosphere. We show that a recently proposed mechanism for the propagation of strangelets through the earth\'s atmosphere, together with a proper account of charge capture and ionisation loss, would solve this problem. We also argue that this could lead to viable strategies for definitive detection of strange quark matter in cosmic ray flux using a ground based large area array of passive detectors.']",['2000-06-27'] +579,['eng'],"['Kalashev, O E', 'Kuzmin, V A', 'Semikoz, D V']","['Ultra High Energy Cosmic Rays, propagation in the Galaxy and anisotropy']",['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'galaxy', 'lepton, cosmic radiation', 'nucleon, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, anisotropy', 'magnetic field', 'astrophysics, missing-mass', 'topology, defect', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006349'],"['We considered propagation of Ultra High Energy Cosmic Rays (UHECR) through the galaxy. We extend our numerical code for calculation of the spectra of leptons, nucleons and $\\gamma$-rays in case of uniform and isotropic source distribution for the case of spherically symmetric source distribution and magnetic field. We investigated models with sources of UHECR distributed in same way as Cold Dark Matter (CDM) in self-consistent way, taking into account both extra-galactic and Galactic contributions.']",['2000-06-27'] +580,['eng'],"['Schunck, F E', 'Mielke, E W']",['Eigenvalues of the Stewart-Lyth equation for inflation with a blue spectrum'],['Astrophysics and Astronomy'],"['inflationary universe', 'Abel equation, nonlinear', 'inflaton, potential', 'spectra, discrete', 'cosmic radiation, background', 'energy, density', 'axion', 'quintessence', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006348'],"['By using the rather stringent nonlinear second order slow-roll approximation, we reconsider the nonlinear second order Abel equation of Stewart and Lyth. We determine a new blue eigenvalue spectrum. Some of the discrete values of the spectral index $n_s$ have consistent fits to the cumulative COBE data as well as to recent ground-base CMB experiments.']",['2000-06-27'] +581,['eng'],"['Hoffman, M B', 'Turner, M S']",['Kinematic Constraints to the Key Inflationary Observables'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'gravitational radiation', 'cosmic radiation, background', 'kinematics', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006321'],"['The observables $T/S$ and $n-1$ are key to testing and understanding inflation. ($T$, $S$, and $n-1$ respectively quantify the gravity-wave and density-perturbation contributions to CMB anisotropy and the deviation of the density perturbations from the scale-invariant form.) Absent a standard model, there is no definite prediction for, or relation between, $T/S$ and $n-1$. By reformulating the equations governing inflation we show that models generally predict $T/S \\approx -5(n-1)$ or 0, and in particular, if $n>0.85$, $T/S$ is expected to be $>10^{-3}$.']",['2000-06-23'] +582,['eng'],"['Blasi, P', 'Sheth, R']",['Halo Dark Matter and Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'galaxy', 'postulated particle, heavy', 'postulated particle, decay', 'cosmic radiation, production', 'cosmic radiation, flux', 'cosmic radiation, spectra', 'cosmic radiation, anisotropy', 'numerical calculations']","['http://fnalpubs.fnal.gov/archive/2000/pub/Pub-00-143-A.html', 'http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006316']","['The decay of very heavy metastable relics of the Early Universe can produce ultra-high energy cosmic rays (UHECRs) in the halo of our own Galaxy. On distance scales of the order of the halo size, energy losses are negligible---no Greisen-Zatsepin-Kuzmin cutoff is expected. In this letter we show that, as a consequence of the hierarchical build up of the halo, this scenario predicts the existence of small scale anisotropies in the arrival directions of UHECRs. We also suggest some consequences of this scenario which will be testable with upcoming experiments, as Auger.']",['2000-06-22'] +583,['eng'],"['Amendola, L']",['Dark energy and the Boomerang data'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'astrophysics, model', 'quintessence', 'field theory, scalar', 'gravitation, coupling', 'tensor, energy-momentum', 'statistical analysis', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006300'],"['The recent high-quality Boomerang data allow to test many competing cosmological models. Here I present a seven-parameter likelihood analysis of dark energy models with exponential potential and explicit coupling to dark matter. Such a model is conformally equivalent to a scalar field with non-minimal coupling to gravity. So far, the constraints on a dark energy - dark matter coupling were extremely weak. The Boomerang data constrain the dimensionless coupling $\\beta $ to be smaller than 0.1, an order of magnitude better than previous limits. In terms of the constant $\\xi $ of non-minimally coupled theories, this amounts to $\\xi <0.01.$ On the other hand, Boomerang has not enough sensitivity to put constraints on the potential slope.']",['2000-06-22'] +584,['eng'],"['Nardi, E', 'Zuluaga, I D']",['Pulsar acceleration by asymmetric emission of sterile neutrinos'],['Astrophysics and Astronomy'],"['pulsar, acceleration', 'neutrino, sterile', 'resonance, production', 'emission, asymmetry', 'magnetic field, anisotropy', 'spin, flavor', 'antineutrino/tau, transition', 'neutrino, diffusion', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006285'],['A convincing explanation for the observed pulsar large peculiar velocities is still missing. We argue that any viable particle physics solution would most likely involve the resonant production of a non-interacting neutrino $\\nu_s$ of mass $m_{\\nu_s}\\sim$ 20--50 keV. We propose a model where anisotropic magnetic field configurations strongly bias the resonant spin flavour precession of tau antineutrinos into $\\nu_s$. The asymmetric emission of $\\nu_s$ from the core can produce sizeable natal kicks and account for recoil velocities of several hundred kilometers per second.'],['2000-06-21'] +585,['eng'],"['Hamilton, J C']",['Preliminary results and perspectives in the Archeops experiment'],['Astrophysics and Astronomy'],"['talk, La Thuile 2000/02/27']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006254'],"['Observations of the Cosmic Microwave Background (CMB) temperature fluctuations are a powerful tool for testing theories of the early Universe and for measuring cosmological parameters. We present basics of CMB physics, review some of the most recent results and discuss their implications for cosmology. The Archeops balloon-borne experiment is designed to map the CMB with an angular resolution of 10 arcminutes and a precision of 30 $\\mu\\mathrm{K}$ per pixel. This will allow the measurement of the CMB fluctuation power spectrum from large to small angular scales. We describe preliminary results from the test flight which took place in July 1999 and present perspectives for upcoming scientific flights (January 2001).']",['2000-06-20'] +586,['eng'],"['Kiefer, C']",['Origin of classical structure from inflation'],['Astrophysics and Astronomy'],"['talk, Villasimius 1999/09/14', 'inflationary universe', 'fluctuation, entropy', 'cosmic radiation, anisotropy', 'cosmic radiation, background', 'decoherence', 'field theory, scalar', 'squeezed state', 'gravitational radiation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006252'],"['According to the inflationary scenario, all structure in the Universe can be traced back to quantum fluctuations of the metric and scalar field(s) during inflation. The seeds of this structure can be observed as classical anisotropies in the cosmic microwave background. I briefly review how the transition from the inherent quantum nature of these fluctuations to classical behaviour comes about. Two features play a crucial role: Firstly, the quantum state of the fluctuations becomes highly squeezed for wavelengths that exceed the Hubble radius. Secondly, decoherence due to other fields distinguishes the field-amplitude basis as the classical pointer basis. I also discuss the entropy of the fluctuations and make a brief comparison with chaotic systems.']",['2000-06-20'] +587,['eng'],"['Kowalski-Glikman, J']",['Testing Dispersion Relations of Quantum $\\kappa$-Poincaré Algebra on Cosmological Ground'],['Astrophysics and Astronomy'],"['astrophysics, model', 'density, perturbation', 'spectra, perturbation', 'dispersion relations', 'quantum algebra, Poincare', 'energy, density']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006250'],"[""Following the procedure proposed recently by Martin and Brandenberger we investigate the spectrum of the cosmological perturbations in the case when the ``trans-Plackian'' dispersion relations are derived from the quantum $\\kappa$-Poincar\\'e algebra. We find that depending on the choice of initial conditions of the perturbations, the spectrum is either $n^3 P \\sim \\frac1n$ for initial conditions minimizing energy density, or the flat one $n^3 P \\sim n^0$ for instantaneous Minkowski vacuum. This latter spectrum leads to the observed scale-invariant Harrison-Zel'dovich spectrum in the Friedmann epoch.""]",['2000-06-20'] +588,['eng'],"['Liu, G C', 'Yamamoto, K', 'Sugiyama, N', 'Nishioka, H']",['Nonlinear Evolution of Very Small Scale Cosmological Baryon Perturbations at Recombination'],['Astrophysics and Astronomy'],"['astrophysics, model', 'baryon, density', 'density, perturbation', 'effect, nonlinear', 'velocity', 'diffusion', 'astrophysics, missing-mass', 'cosmic radiation, background', 'ionization', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006223'],"[""The evolution of baryon density perturbations on very small scales is investigated. In particular, the nonlinear growth induced by the radiation drag force from the shear velocity field on larger scales during the recombination epoch, which is originally proposed by Shaviv in 1998, is studied in detail. It is found that inclusion of the diffusion term which Shaviv neglected in his analysis results in rather mild growth whose growth rate is $\\ll 100$ instead of enormous amplification $\\sim 10^4$ of Shaviv's original claim since the diffusion suppresses the growth. The growth factor strongly depends on the amplitude of the large scale velocity field. The nonlinear growth mechanism is applied to density perturbations of general adiabatic cold dark matter (CDM) models. In these models, it has been found in the previous works that the baryon density perturbations are not completely erased by diffusion damping if there exists gravitational potential of CDM. With employing the perturbed rate equation which is derived in this paper, the nonlinear evolution of baryon density perturbations is investigated. It is found that: (1) The nonlinear growth is larger for smaller scales. This mechanism only affects the perturbations whose scales are smaller than $\\sim 10^2M_\\odot$, which are coincident with the stellar scales. (2) The maximum growth factors of baryon density fluctuations for various COBE normalized CDM models are typically less than factor 10 for $3-\\sigma$ large scale velocity peaks. (3) The growth factor depends on $\\Omega_{\\rm b}$.""]",['2000-06-19'] +589,['eng'],"['Fassò, Alberto', 'Poirier, J']",['Spatial and Energy Distribution of Muons in Gamma-induced Air Showers'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, secondary radiation', 'showers, air', 'muon, energy spectrum', 'spatial distribution', 'muon, flux', 'electron, flux', 'numerical calculations, Monte Carlo', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006196'],"[""The FLUKA Monte Carlo program is used to calculate the effects of gamma hadroproduction. The primary gamma rays are incident upon the earth's atmosphere at a normal angle. The FLUKA code is believed to be quite accurate in reproducing experimental photon hadroproduction data in the 1 GeV to 10 TeV energy range studied. The charged pions which are so produced can decay to muons with sufficient energy to reach ground level. The numbers of these muons and their radial and energy distributions are studied for incident gamma ray energies from 1 GeV to 10 TeV. The number of these muons is not negligible; they can, in certain circumstances, be used to study potential sources of gamma rays like gamma ray bursts. It is found, for example, that a 10 TeV incident primary gamma ray produces, on average, 3.4 muons which reach ground level; the smaller muon production efficiency at lower photon energies is more than compensated by the larger number of photons in the primary spectrum.""]",['2000-06-15'] +590,['eng'],"['Totani, T', 'Kitayama, T']",['Forming Clusters of Galaxies as the Origin of Unidentified GeV Gamma-Ray Sources'],['Astrophysics and Astronomy'],"['astrophysics, model', 'galaxy, cluster', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'flux', 'energy spectrum', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006176'],"['Over half of GeV gamma-ray sources observed by the EGRET experiment have not yet been identified as known astronomical objects. There is an isotropic component of such unidentified sources, whose number is about 60 in the whole sky. Here we calculate the expected number of dynamically forming clusters of galaxies emitting gamma-rays by high energy electrons accelerated in the shock wave when they form, in the framework of the standard theory of structure formation. We find that a few tens of such forming clusters should be detectable by EGRET and hence a considerable fraction of the isotropic unidentified sources can be accounted for. We argue that these clusters are very difficult to detect in x-ray or optical surveys compared with the conventional clusters, because of their extended angular size of about 1 degree. Hence they define a new population of ""gamma-ray clusters"". As a test of this hypothesis, we predict that the next generation gamma-ray telescopes such as GLAST will detect more than a few thousands of gamma-ray clusters. It will provide a new tracer of dynamically evolving structures in the universe, in contrast to the x-ray clusters as a tracer of hydrodynamically stabilized systems. We also derive the strength of magnetic field required for the extragalactic gamma-ray background by structure formation to extend up to 100 GeV as observed, that is about 10^{-5} of the shock-heated baryon energy density.']",['2000-06-14'] +591,['eng'],"['Aharonian, F A', 'Konopelko, A K', 'Völk, H J', 'Quintana, H']",['A 5 GeV energy threshold array of imaging atmospheric Cherenkov telescopes at 5 km altitude'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'energy, threshold', 'geophysics, magnetic field', 'Cherenkov counter, imaging', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006163'],['We discuss the concept and the performance of a powerful future ground-based astronomical instrument - a stereoscopic array of several large imaging atmospheric Cherenkov telescopes installed at a very high mountain elevation of about 5 km a.s.l. or more - for the study of the gamma-ray sky at energies from several GeV to 100 GeV.'],['2000-06-13'] +592,['eng'],"['Dolgov, A D']","['Neutrinos in physics, astrophysics, and cosmology']",['Astrophysics and Astronomy'],"['talk, Rome 2000/04/10', 'neutrino, astrophysics', 'neutrino, solar', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'neutrino, mass', 'astrophysics, model', 'light nucleus, production', 'lepton, asymmetry']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006162'],['A brief review of neutrino anomalies in particle physics and of the role played by neutrinos in cosmology and astrophysics is presented. The main part of the talk is dedicated to the impact of neutrinos and in particular of neutrino oscillations on BBN and to a possible spatial variation of primordial abundances.'],['2000-06-13'] +593,['eng'],"['Derome, L', 'Buénerd, M', 'Barrau, A', 'Bouchet, A', 'Menchaca-Rocha, A', 'Thuillier, T']",['Origin of the high energy proton component below the geomagnetic cutoff in near earth orbit'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'p, cosmic radiation', 'p, flux', 'geophysics, magnetic field', 'p p, inclusive reaction', 'p nucleus, nuclear reaction', 'p, hadroproduction', 'angular distribution', 'energy spectrum', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006160'],['The high flux proton component observed by AMS below the geomagnetic cutoff can be well accounted for by assuming these particles to be secondaries originating from the interaction of Cosmic Ray protons with the atmosphere. Simulation results are reported'],['2000-06-13'] +594,['eng'],"['Zwart, S F P', 'Totani, T']",['Precessing jets interacting with interstellar material as the origin for the light curves of gamma-ray bursts'],['Astrophysics and Astronomy'],"['astrophysics', 'photon, cosmic radiation', 'gamma ray burst', 'time dependence', 'cosmic radiation, particle source', 'black hole', 'model, shock waves', 'jet, relativistic', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006143'],"['We present an internal shock model with external characteristics for explaining the complicated light curves of gamma-ray bursts. Shocks produce gamma-rays in the interaction between a precessing beam of relativistic particles and the interstellar medium. Each time the particle beam passes the same line of sight with the observer the inter stellar medium is pushed outward. Subsequent interactions between the medium and the beam are delayed by the extra distance to be traveled for the particles before the shock can form. This results in a natural retardation and leads to an intrinsic asymmetry in the produced light curves for gamma-ray bursts. In addition we account for the cooling of the electron proton plasma in the shocked region, which gives rise to a exponential decay in the gamma-ray flux. The combination of these effects and the precessing jet of ultra relativistic particles produces light curves which can be directly compared with observed gamma-ray burst light curves. We illustrate the model by fitting a number of observed gamma-ray bursts which are hard to explain with only a precessing jet. With a genetic algorithm we are able to fit several observed gamma-ray bursts with remarkable accuracy. We find that for different bursts the observed fluence, assuming isotripic emission, easily varies over four orders of magnitude from the energy generated intrinsically.']",['2000-06-12'] +595,['eng'],"['Anchordoqui, L A', 'McCauley, T P', 'Paul, T', 'Reucroft, S', 'Swain, J D', 'Taylor, L']",['Simulation of Water Cerenkov Detectors Using {\\sc geant4}'],['Astrophysics and Astronomy'],"['talk, Campinas 2000/07/17', 'cosmic radiation', 'showers, air', 'Cherenkov counter, water', 'programming, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006142'],"['We present a detailed simulation of the performance of water Cerenkov detectors suitable for use in the Pierre Auger Observatory. Using {\\sc geant4}, a flexible object-oriented simulation program, including all known physics processes, has been developed. The program also allows interactive visualization, and can easily be modified for any experimental setup.']",['2000-06-12'] +596,['eng'],"['Anchordoqui, L A', 'Cooperman, G', 'Grinberg, V', 'McCauley, T P', 'Paul, T', 'Reucroft, S', 'Swain, J D', 'Alverson, G']",['Air shower simulation using {\\sc geant4} and commodity parallel computing'],['Astrophysics and Astronomy'],"['talk, Campinas 2000/07/17', 'showers, air', 'showers, spectra', 'programming, Monte Carlo', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006141'],"['We present an evaluation of a simulated cosmic ray shower, based on {\\sc geant4} and {\\sc top-c}, which tracks all the particles in the shower. {\\sc top-c} (Task Oriented Parallel C) provides a framework for parallel algorithm development which makes tractable the problem of following each particle. This method is compared with a simulation program which employs the Hillas thinning algorithm.']",['2000-06-12'] +597,['eng'],"['Chitnis, V R', 'Bhat, P N']",['Possible Discrimination between Gamma Rays and Hadrons using Cerenkov Photon Timing Measurements'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006133'],"['Atmospheric \\v{C}erenkov Technique is an established methodology to study $TeV$ energy gamma rays. However the challenging problem has always been the poor signal to noise ratio due to the presence of abundant cosmic rays. Several ingenious techniques have been employed to alleviate this problem, most of which are centred around the \\v{C}erenkov image characteristics. However there are not many techniques available for improving the signal to noise ratio of the data from wavefront sampling observations. One such possible technique is to use the \\v{C}erenkov photon arrival times and identify the species dependent characteristics in them. Here we carry out systematic monte carlo simulation studies of the timing information of \\v{C}erenkov photons at the observation level. We have parameterized the shape of the \\v{C}erenkov shower front as well as the pulse shapes in terms of experimentally measurable quantities. We demonstrate the sensitivity of the curvature of the shower front, pulse shape parameters as well as the photon arrival time jitter to primary species and show their efficiency in improving the signal to noise ratio. The effect of limiting the \\v{C}erenkov telescope opening angle by using a circular focal point mask, onthe efficacy of the parameters has also been studied for each of the parameters. Radius of the shower front, pulse decay time and photon arrival time jitter have been found to be the most promising parameters which could be used to discriminate $\\gamma -$ray events from the background. We also find that the efficiency of the first two parameters increases with zenith angle and efficiency of pulse decay time decreases with increasing altitude of observation.']",['2000-06-12'] +598,['eng'],"['Pina-Avelino, P', 'De Carvalho, J P M', 'Martins, C J A P', 'Oliveira, J C R E']",['Can our Universe be inhomogeneous on large sub-horizon scales?'],['Astrophysics and Astronomy'],"['astrophysics, model', 'domain wall, network', 'energy, density', 'vacuum state', 'critical phenomena', 'topology, defect', 'density, perturbation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004227'],"['We show that our Universe may be inomogeneous on large sub-horizon scales without us being able to realise it. We assume that a network of domain walls permeates the universe dividing it in domains with slightly different vacuum energy densities. We require that the energy scale of the phase transition which produced the domain walls is sufficiently low so that the walls have a negligible effect on structure formation. Nevertheless, the different vacuum densities of different domains will lead to different values of the cosmological parameters $\\Omega_\\Lambda^0$, $\\Omega_m^0$ and $h$, in each patch thus affecting the growth of cosmological perturbations at recent times. Hence, if our local patch of the universe (with uniform vacuum density) is big enough -- which is likely to happen given that we should have on average about one domain per horizon volume -- we might not notice these large-scale inomogeneities. This happens because in order to see a patch with a different vacuum density one may have to look back at a time when the universe was still very homogeneous.']",['2000-04-18'] +599,['eng'],"['Scully, S T', 'Stecker, F W']",['On the spectrum of Ultrahigh Energy Cosmic Rays and the Gamma Ray Burst Origin Hypothesis'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006112'],"['It has been suggested that cosmological gamma-ray bursts (GRBs) can produce the observed flux of cosmic rays at the highest energies. However, recent studies of GRBs indicate that their redshift distribution likely follows that of the average star formation rate and that GRBs were more numerous at high redshifts. As a consequence, we show that photomeson production energy losses suffered by ultrahigh energy cosmic rays coming from GRBs would produce too sharp a spectral high energy cutoff to be consistent with the air shower data.']",['2000-06-09'] +600,['eng'],"['Letessier-Selvon, A A']",['Theoretical and Experimental Topics on Ultra High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Sanlucar de Barrameda 2000/02/14', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'transport theory', 'p, energy spectrum', 'cosmic radiation, cascade', 'magnetic field', 'cosmic radiation, interaction', 'showers, air', 'cosmic radiation, counters and detectors', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006111'],"[""Since their first observation in 1962, the existence of Ultra High Energy Cosmic Rays (UHECR) remains a mystery in modern astrophysics. Those cosmic rays, with energies well above 50 EeV ($50\\times 10^{18}$eV), can hardly be accelerated, even in the most active parts of our universe such as FR-II radio galaxies or AGNs, nor can they travel on distances larger than 100 Mpc. In the following some of the production and acceleration models for UHECR are reviewed and some of the transport issues are exposed. Finally the detection and identification on Earth of those ``cosmic bullets'' are presented.""]",['2000-06-09'] +601,['eng'],"['Cillis, A N', 'Sciutto, S J']",['Muon Bremsstrahlung and Muonic Pair Production in Air Showers'],['Astrophysics and Astronomy'],"['talk, Campinas 2000/07/17', 'cosmic radiation', 'showers, air', 'muon, bremsstrahlung', 'muon, pair production', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006108'],"['The objective of this work is to report on the modifications in air shower development due to muon bremsstrahlung and muonic pair production. In order to do that we have implemented new muon bremsstrahlung and muonic pair production procedures in the AIRES air shower simulation system, and have used it to simulate ultra high energy showers in different conditions. The influence of the mentioned processes in the global development of the air shower is important for primary particles of large zenith angles, while they do not introduce significant changes in the position of the shower maximum.']",['2000-06-09'] +602,['eng'],"['Novikov, D', 'Schmalzing, J', 'Mukhanov, V F']",['On non-Gaussianity in the Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'inflationary universe', 'statistics', 'data analysis method', 'density, fluctuation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006097'],"['We consider a cosmological model with non-Gaussian initial perturbations, which in principle could be generated in non-standard inflationary scenarios with two or more scalar fields. In particular we focus our attention on the model proposed by Linde & Mukhanov (1997) perturbations are quadratic in a Gaussian field. These perturbations, if they exist, have to be observable as a non-Gaussian distribution of the CMB signal on the sky. In order to efficiently pick up the non-Gaussian signal in CMB maps of degree resolution, one can use Minkowski Functionals and peak statistics. Our paper contains the theoretical predictions of the properties for Minkowski Functionals and distributions of peaks of the CMB anisotropy in the model with ""squared"" Gaussian statistics. Likelihood comparison of the four-year COBE DMR data to this non-Gaussian model and the standard Gaussian model does not select any of them as most likely. We also suggest an efficient algorithm for fast simulation of CMB maps on the whole sky. Using a cylindrical partition of the sphere, we rewrite the spherical harmonics analysis as a Fourier transform in flat space, which makes the problem accessible to numerically advantageous FFT methods.']",['2000-06-08'] +603,['eng'],"['De Paolis, F', 'Ingrosso, G', 'Orlando, D']",['High-energy $\\gamma$-ray emission from GRBs'],['Astrophysics and Astronomy'],"['gamma ray burst', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'nucleon, cosmic radiation', 'p nucleon, interaction', 'pi0, radiative decay', 'photon, production', 'photon, flux', 'photon, absorption', 'magnetic field, effect', 'cosmic radiation, energy spectrum', 'proposed experiment', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006095'],"['GRBs are nowadays a rather well understood phenomenon in the soft (KeV-MeV) $\\gamma$-ray energy band, while only a few GRBs have been observed at high photon energies ($E_{\\gamma} \\ut > 1$ GeV). It is also widely recognized that GRBs accelerate protons to relativistic energies and that dense media are often present nearby the sources. Within this framework we compute in detail the high-energy $\\gamma$-ray flux from the decay of neutral pions produced through the interaction of accelerate protons with nucleons in the surrounding medium. We also take into account the local and intergalactic $\\gamma$-ray absorption. The presence of magnetic fields around the GRB sources causes the deflection of the accelerated protons and so a temporal spread of the produced high-energy $\\gamma$-rays with respect to the signal in the soft $\\gamma$-ray band. Moreover, we analyze the possibility to detect the $\\gamma$-ray signal in the GeV-TeV energy range by the ARGO detector under construction in Tibet.']",['2000-06-08'] +604,['eng'],"['Aharonian, F A', 'Akhperjanian, A G', 'Barrio, J A', 'Bernlöhr, K', 'Borst, H', 'Bojahr, H', 'Contreras, J G', 'Cortina, J', 'Denninghoff, S', 'Fonseca, V', 'González, J', 'Götting, N', 'Heinzelmann, G', 'Hermann, G', 'Heusler, A', 'Hofmann, W', 'Horns, D', 'Ibarra, Alejandro', 'Iserlohe, C', 'Kankanyan, R', 'Kestel, M', 'Kettler, J', 'Kohnle, A', 'Konopelko, A K', 'Kornmayer, H', 'Kranich, D', 'Krawczynski, H', 'Lampeitl, H', 'Lorenz, E', 'Lucarelli, F', 'Magnussen, N', 'Mang, O', 'Meyer, H', 'Mirzoian, R M', 'Moralejo, A', 'Padilla, L', 'Panter, M', 'Plaga, R', 'Plyasheshnikov, A V', 'Prahl, J', 'Pühlhofer, G', 'Rhode, W', 'Röhring, A', 'Rowell, G', 'Sahakian, V V', 'Samorski, M', 'Schilling, M', 'Schröder, F', 'Siems, M', 'Stamm, W', 'Tluczykont, M', 'Völk, H J', 'Wiedner, C A', 'Wittek, W']",['Rejection of the hypothesis that Mkn-501 TeV photons are pure Bose-Einstein condensates'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'boson, condensation', 'cosmic radiation, energy spectrum', 'cosmic radiation, diffusion', 'cosmic radiation, density', 'upper limit', 'showers, air', 'photon, absorption', 'Cherenkov counter', 'galaxy, blazar', 'data analysis method', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006092'],"['The TeV energy spectrum of the Blazar type galaxy Mkn-501 as measured by the HEGRA air Cherenkov telescopes extends beyond 16 TeV and constitutes the most energetic photons observed from an extragalactic object. A fraction of the emitted spectrum is possibly absorbed in interactions with low energy photons of the diffuse extragalactic infrared radiation, which in turn offers the unique possibility to measure the diffuse infrared radiation density by exact TeV spectroscopy. One of the recently published ideas to reduce the absorption of TeV photons is based upon the assumption that sources like Mkn-501 could produce Bose-Einstein condensates of coherent GeV ground-state photons. The condensates would have a higher survival probability during the transport in the diffuse radiation field and could mimic TeV air shower events. The powerful stereoscopic technique of the HEGRA air Cherenkov telescopes allows to test this hypothesis by reconstructing the penetration depths of TeV air shower events: Air showers initiated by Bose-Einstein condensates are expected to reach the maximum of the shower development in the atmosphere earlier than single photon events. By comparing the energy dependent penetration depths of TeV photons from Mkn-501 with those from the TeV standard candle Crab Nebula, we can reject the hypothesis that TeV photons from Mkn-501 are pure Bose-Einstein condensates.']",['2000-06-08'] +605,['eng'],"['Taylor, A N', 'Berera, A']",['Perturbation Spectra in the Warm Inflationary Scenario'],['Astrophysics and Astronomy'],"['inflationary universe', 'inflaton', 'radiation', 'spectra, perturbation', 'perturbation, scalar', 'perturbation, tensor', 'perturbation, adiabatic', 'energy, density', 'potential', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006077'],"['We investigate the phenomenology of warm inflation and present generic results about the evolution of the inflaton and radiation fields. The general conditions required for warm inflation to take place are derived and discussed. A comprehensive approach is presented for the generation of thermally induced adiabatic and isocurvature perturbations and the amplitude of their spectra calculated. In addition we derive the ratio of tensor-to-scalar perturbations and find the spectral indices for adiabatic, isocurvature and tensor perturbations formed in the warm inflationary era. These results are presented in a simplified and compact approach that is generally applicable. Our results are illustrated by inflation models with polynomial and exponential potentials. We compare our analytic results against numerical models and find excellent agreement. Finally, presently available data is used to put constraints on warm inflation and we discuss how near--future observations may distinguish the warm inflationary scenario from standard supercooled inflation. The main observable difference is the different scalar-to- tensor ratio, and that the consistency relation between this and the slope of tensor perturbations does not hold for warm inflation.']",['2000-06-07'] +606,['eng'],"['Madsen, J']",['Dark matter phase space densities'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'phase space, density', 'decoupling, relativistic', 'potential, chemical', 'decoupling, nonrelativistic', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006074'],"['The low velocity part of a kinetic equilibrium dark matter distribution has higher phase space density and is more easily incorporated in formation of a low mass galaxy than the high velocity part. For relativistically decoupling fermions (bosons), this explains 1 (2) orders of magnitude of the observed trend, that phase space densities in dark matter halo cores are highest in the smallest systems, and loosens constraints on particle masses significantly. For non-relativistic decoupling and/or finite chemical potentials even larger effects may occur. It is therefore premature to dismiss dissipationless particle distributions as dark matter on the basis of phase space arguments.']",['2000-06-07'] +607,['eng'],"['Van Putten, M H P M', 'Sarkar, A']",['An $\\dot{f}(f)$-frequency dynamics algorithm for gravitational waves'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'interference, laser', 'n, matter', 'black hole', 'binary', 'coalescence', 'background', 'signal processing', 'numerical methods', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006056'],['Coalescence of low mass compact binaries of neutron stars and black holes are primary burst sources for LIGO and VIRGO.Of importance in the early stages of observations will be the classification of candidate detections by source-type. The diversity in source parameters and serendipity in any new window of observations suggest to consider model-independent detection algorithms. Here a frequency dynamics algorithm is described which extracts a trajectory in the $\\dot{f}(f)$-plane from the noisy signal. The algorithm is studied in simulated binary coalescence. Robust results are obtained with experimental noise data. Experiments show the method to be superior to matched filtering in the presence of model imperfections.'],['2000-08-29'] +608,['eng'],"['Orito, M', 'Kajino, T', 'Mathews, G J', 'Boyd, R N']",['Neutrino Degeneracy and Decoupling'],['Astrophysics and Astronomy'],"['lepton, asymmetry', 'neutrino, decoupling', 'finite temperature', 'astrophysics', 'electron positron, annihilation', 'photon, temperature', 'neutrino, temperature', 'temperature, ratio', 'light nucleus, production', 'photon, decoupling', 'cosmic radiation, background', 'cosmic radiation, spectra', 'baryon, density', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005446'],"['We reanalyze the cosmological constraints on the existence of a net universal lepton asymmetry and neutrino degeneracy. For sufficiently large degeneracy, neutrino decoupling can occur before various particles annihilate and even before the QCD phase transition. These decoupled neutrinos are therefore not heated as the particle degrees of freedom change. The resultant ratio of the relic neutrino-to-photon temperatures after $e^\\pm$ annihilation can then be significantly reduced by more than a factor of two from that of the standard nondegenerate ratio. This changes the expansion rate and subsequent primordial nucleosynthesis, photon decoupling, and structure formation. In particular we analyze physically plausible lepton-asymmetric models with large $\\nu_\\mu$ and $\\nu_\\tau$ degeneracies together with a moderate $\\nu_e$ degeneracy. We show that the nucleosynthesis by itself permits very large neutrino degeneracies $0. \\le \\xinum$, $\\xinut \\le 40$, $0. \\le \\xinue \\le 1.4$ together with large baryon densities $0.1 \\le \\Omega_b \\h502 \\le 1$ as long as some destruction of primordial lithium is assumed. We also show that structure formation and the power spectrum of the cosmic microwave background allows for the possibility of an $\\Omega = 1$, $\\Omega_\\Lambda = 0.4$, cosmological model for which there is both significant lepton asymetry ($| \\xinum | = | \\xinut | \\approx 11$) and a relatively large baryon density ($\\Omega_b \\approx 0.06$). Our best-fit neutrino-degenerate, high-baryon-content models are mainly distinguished by a suppression of the second peak in the microwave background power spectrum. This is consistent with the latest high resolution data from BOOMERANG and MAXIMA-1.']",['2000-05-24'] +609,['eng'],"['Gawiser, E']",['Big Bang Leftovers in the Microwave'],['Astrophysics and Astronomy'],['Thesis'],['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005365'],"[""We combine detections of anisotropy in the Cosmic Microwave Background radiation with observations of inhomogeneity in the large-scale distribution of galaxies to test the predictions of models of cosmological structure formation. This combination probes spatial scales varying by three orders of magnitude, including a significant region where the two types of data overlap. We examine Cold Dark Matter models with adiabatic density perturbations, isocurvature models, and a topological defects model. We set upper limits on the neutrino mass and find the primordial power spectrum needed to reconcile an apparent disagreement between structure formation observations and direct observations of cosmological parameters. Present and future observations of Cosmic Microwave Background anisotropy suffer from foreground contamination. We develop detailed predictions for microwave emission from radio and infrared-bright galaxies and the Sunyaev-Zeldovich effect from clusters. We present realistic simulations of the microwave sky, produced as part of the `WOMBAT Challenge' exercise, and introduce a pixel-space method for subtracting foreground contamination which can be tested on these simulations.""]",['2000-05-19'] +610,['eng'],"['Elliott, S R']",['Measuring Supernova Neutrino Temperatures using Lead Perchlorate'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'supernova', 'neutrino nucleus, nuclear reaction', 'n, production', 'lead, nuclide', 'electron, energy spectrum', 'photon, energy spectrum', 'cross section, energy dependence', 'charged current', 'neutrino, particle identification', 'neutrino/e, temperature', 'antineutrino/e, temperature', 'counters and detectors, proposed', 'deep underground detector', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006041'],"['Neutrino interactions with lead produce neutrons in numbers that depend on neutrino energy and type. A detector based on lead perchlorate, for example, would be able to measure the energy deposited by electrons and gammas in coincidence with the number of neutrons produced. Sorting the electron energy spectra by the number of coincident neutrons permits the identification of the neutrino type that induced the reaction. This separation allows an analysis which can determine the temperatures of electron neutrinos and electron anti-neutrinos from a supernova in one experiment. The neutrino reaction signatures of lead perchlorate and the fundamentals of using this material as a neutrino detector are described.']",['2000-06-05'] +611,['eng'],"['Alvarez-Muñiz, J', 'Halzen, Francis', 'Hooper, D W']",['High Energy Neutrinos from $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'gamma ray burst', 'fireball', 'neutrino, production', 'cosmic radiation, fluctuation', 'neutrino, absorption', 'neutrino, flux', 'tau, decay modes', 'tau, branching ratio', 'neutrino, counters and detectors', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006027'],"['Following Waxman and Bahcall we calculate the event rate, energy and zenith angle dependence of neutrinos produced in the fireball model of gamma ray bursts (GRB). We emphasize the primary importance of i) burst-to-burst fluctuations and ii) absorption of the neutrinos in the Earth. From the astronomical point of view, we draw attention to the sensitivity of neutrino measurements to the boost Lorentz factor of the fireball $\\Gamma$, which is central to the fireball model, and only indirectly determined by follow-up observations. Fluctuations result in single bursts emitting multiple neutrinos, making it possible to determine the flavor composition of a beam observed after a baseline of thousands of Megaparsecs.']",['2000-06-02'] +612,['eng'],"['Matos, T', 'Urena-Lopez, L A']",['A Further Analysis of a Cosmological Model of Quintessence and Scalar Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, model', 'field theory, scalar', 'quintessence', 'astrophysics, missing-mass', 'potential', 'matter, fluctuation', 'perturbation theory, linear', 'energy, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006024'],"['We present the complete solution to a 95% scalar field cosmological model in which the dark matter is modeled by a scalar field $\\Phi $ with the scalar potential $V(\\Phi)=V_{o}[ \\cosh {(\\lambda \\sqrt{\\kappa_{o}}\\Phi)}-1]$ and the dark energy is modeled by a scalar field $\\Psi$, endowed with the scalar potential $\\tilde{V}(\\Psi)=\\tilde{V_{o}}[ \\sinh {(\\alpha \\sqrt{\\kappa_{o}}\\Psi)}] ^{\\beta}$. This model has only two free parameters, $\\lambda$ and the equation of state $\\omega_{\\Psi}$. With this solution, the fine tuning and the cosmic coincidence problems are ameliorated. The dark matter consists of an ultra-light particle, whose mass could be $m_{\\Phi}\\geq 10^{-26}eV$. All the success of the standard cold dark matter model is recovered. In addition, we clarify the meaning of a scalar Jeans lenght. The model predicts a suppression of the Mass Power Spectrum for small scales having a wave number $k > k_{min,\\Phi}$, where $k_{min,\\Phi} \\geq 0.3 Mpc^{-1}$, that could help to explain the dearth of dwarf galaxies and the smoothness of galaxy core halos. In fact, the suppression scale depends on the parameter $\\lambda$ mentioned above. This implies that a scalar field could be a good candidate to be the dark matter of the Universe.']",['2000-06-02'] +613,['eng'],"['Xu, R X', 'Zhang, B', 'Qiao, G J']",['What if pulsars are born as strange stars?'],['Astrophysics and Astronomy'],"['pulsar', 'matter, strangeness', 'charged particle, binding energy', 'quark, surface', 'n, matter', 'supernova', 'critical phenomena', 'photon, cosmic radiation', 'interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006021'],"[""The possibility and the implications of the idea, that pulsars are born as strange stars, are explored. Strange stars are very likely to have atmospheres with typical mass of $\\sim 5\\times 10^{-15}M_\\odot$ but bare polar caps almost throughout their lifetimes, if they are produced during supernova explosions. A direct consequence of the bare polar cap is that the binding energies of both positively and negatively charged particles at the bare quark surface are nearly infinity, so that the vacuum polar gap sparking scenario as proposed by Ruderman & Sutherland should operate above the cap, regardless of the sense of the magnetic pole with respect to the rotational pole. Heat can not accumulate on the polar cap region due to the large thermal conductivity on the bare quark surface. We test this ``bare polar cap strange star'' (BPCSS) idea with the present broad band emission data of pulsars, and propose several possible criteria to distinguish BPCSSs from neutron stars.""]",['2000-06-02'] +614,['eng'],"['Mendes, L E', 'Liddle, A R']",['Initial conditions for hybrid inflation'],['Astrophysics and Astronomy'],"['inflationary universe, hybrid', 'boundary condition', 'membrane model', 'field theory, scalar', 'cosmic radiation, background', 'Friedman model', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0006020'],"['In hybrid inflation models, typically only a tiny fraction of possible initial conditions give rise to successful inflation, even if one assumes spatial homogeneity. We analyze some possible solutions to this initial conditions problem, namely assisted hybrid inflation and hybrid inflation on the brane. While the former is successful in achieving the onset of inflation for a wide range of initial conditions, it lacks sound physical motivation at present. On the other hand, in the context of the presently much discussed brane cosmology, extra friction terms appear in the Friedmann equation which solve this initial conditions problem in a natural way.']",['2000-06-02'] +615,['eng'],"['Pajares, C', 'Sousa, D', 'Vázquez, R A']","[""Consequences of parton's saturation and string's percolation on the developments of cosmic ray showers""]",['Astrophysics and Astronomy'],"['astrophysics', 'cosmic radiation, energy spectrum', 'showers, air', 'nucleus nucleus, nuclear reaction', 'quark gluon, string model', 'critical phenomena, percolation', 'multiple production', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005588'],"[""At high gluon or string densities, gluons' saturation or the strong interaction among strings, either forming colour ropes or giving rise to string's percolation, induces a strong suppression in the particle multiplicities produced at high energy. This suppression implies important modifications on cosmic ray shower development. In particular, it is shown that it affects the depth of maximum, the elongation rate, and the behaviour of the number of muons at energies around 10^{17}-10^{18} eV. The existing cosmic ray data point out in the same direction.""]",['2000-06-01'] +616,['eng'],"['Baccigalupi, C', 'Matarrese, S', 'Perrotta, F']",['Tracking Extended Quintessence'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'field theory, scalar', 'field theory, tensor', 'quintessence', 'effective potential', 'cosmic radiation, background', 'cosmic radiation, spectra', 'astrophysics, fundamental constant', 'matter, spectra', 'energy, density', 'fluctuation, linear', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005543'],"['We study the cosmological role of a Tracking Field $\\phi$ in Extended Quintessence scenarios (TEQ), where the dynamical vacuum energy driving the acceleration of the universe today is coupled with the Ricci scalar, $R$, with a term of the form $F(\\phi)R/2$, where $F(\\phi) = 1/8\\pi G+\\xi(\\phi^{2}-\\phi_{0}^{2})$. Tracker solutions for these NMC models, with inverse power-law potentials, possess an initial enhancement of the scalar field dynamics, named $R$-boost, caused by the Ricci scalar in the Klein-Gordon equation. During this phase the field performs a ""gravitational"" slow rolling which we model analytically, with energy density scaling as $(1+z)^{2}$. We evolve linear perturbations in TEQ models assuming Gaussian scale-invariant initial spectrum. We obtain significant changes in the Integrated Sachs Wolfe effect and in the acoustic peaks locations on the Cosmic Microwave Background, as well as in the turnover on the matter power spectrum. All these corrections may assume positive as well as negative values, depending on the sign of the NMC parameter $\\xi$. We give analytical formulas describing all these effects. We show that they can be as large as $10 - 30%$ with respect to equivalent cosmological constant and ordinary tracking Quintessence models, respecting all the existing experimental constraints on scalar-tensor theories of gravity. These results demonstrate that the next decade data will provide deep constraints on the nature of the dark energy in the Universe, as well as the structure of the theory of gravity.']",['2000-05-29'] +617,['eng'],"['Ricci, B', 'Villante, F L']",['Helioseismic determination of Beryllium neutrinos produced in the Sun'],['Astrophysics and Astronomy'],"['neutrino, solar', 'electron nucleus, nuclear reaction', 'beryllium', 'neutrino, electroproduction', 'luminosity', 'model, solar', 'helium, density', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005538'],"['We provide a determination of the Beryllium neutrino luminosity directly by means of helioseismology, without using additional assumptions. We have constructed solar models where Beryllium neutrino, ($\\nu_{Be}$) production is artificially changed by varying in an arbitrary way the zero energy astrophysical S-factor $S_{34}$ for the reaction $^3{\\rm He}+^4{\\rm He}\\to ^7{\\rm Be}+ \\gamma$. Next we have compared the properties of such models with helioseismic determinations of photospheric helium abundance, depth of the convective zone and sound speed profile. We find that helioseismology directly confirms the production rate of $\\nu_{Be}$ as predicted by SSMs to within $\\pm 25%$ ($1\\sigma$ error). This constraint is somehow weaker than that estimated from uncertainties of the SSM ($\\pm 10%$), however it relies on direct observational data.']",['2000-05-29'] +618,['eng'],"['Esposito, S', 'Miele, G', 'Pastor, S', 'Peloso, M', 'Pisanti, O']",['Non equilibrium spectra of degenerate relic neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, spectra', 'neutrino, asymmetry', 'Boltzmann equation, solution', 'light nucleus, production', 'potential, chemical', 'momentum dependence', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005573'],"['We calculate the exact kinetic evolution of cosmic neutrinos during the epoch previous to Big Bang Nucleosynthesis, in the case when a large neutrino asymmetry exists. By solving numerically the Boltzmann kinetic equations for the neutrino distribution functions, we find the momentum-dependent corrections to the equilibrium spectrum of neutrinos and discuss their phenomenological implications. Motived by recent observations of the Cosmic Microwave Background Radiation, which seem to favour a larger baryon content in the Universe than that required by standard Nucleosynthesis, we also update the Nucleosynthesis bounds on neutrino chemical potentials.']",['2000-05-31'] +619,['eng'],"['Esposito, S', 'Mangano, G', 'Miele, G', 'Pisanti, O']",['The standard and degenerate primordial nucleosynthesis versus recent experimental data'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'differential equations', 'neutrino, flavor', 'baryon, density', 'potential, chemical', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005571'],"['We report the results on Big Bang Nucleosynthesis (BBN) based on an updated code, with accuracy of the order of 0.1% on He4 abundance, compared with the predictions of other recent similar analysis. We discuss the compatibility of the theoretical results, for vanishing neutrino chemical potentials, with the observational data. Bounds on the number of relativistic neutrinos and baryon abundance are obtained by a likelihood analysis. We also analyze the effect of large neutrino chemical potentials on primordial nucleosynthesis, motivated by the recent results on the Cosmic Microwave Background Radiation spectrum. The BBN exclusion plots for electron neutrino chemical potential and the effective number of relativistic neutrinos are reported. We find that the standard BBN seems to be only marginally in agreement with the recent BOOMERANG and MAXIMA-1 results, while the agreement is much better for degenerate BBN scenarios for large effective number of neutrinos, N_\\nu \\sim 10.']",['2000-05-31'] +620,['eng'],"['Martín, J', 'Schwarz, Dominik J']",['New exact solutions for inflationary cosmological perturbations'],['Astrophysics and Astronomy'],"['inflationary universe', 'astrophysics, perturbation', 'effective potential', 'field equations, solution', 'analytic properties', 'potential', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005542'],"[""From a general ansatz for the effective potential of cosmological perturbations we find new, exact solutions in single-scalar-field inflation: A three parameter family of exact solutions that encompasses all exact solutions that have been known previously (power-law inflation, Easther's model, and a generalized version of Starobinsky's solution). The main feature of this new family is that the spectral indices are scale dependent.""]",['2000-05-29'] +621,['eng'],"['Garcia de Andrade, L C']",['The evolution Equation of Cosmological density perturbation in Einstein-Cartan gravity'],['Astrophysics and Astronomy'],"['gravitation, Einstein-Cartan', 'density, perturbation', 'perturbation, linear', 'space-time, fluctuation', 'space-time, de Sitter', 'spin, torsion', 'background, density']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005519'],['The evolution equation of linear cosmic density perturbations in the realm of Einstein-Cartan theory of gravity is obtained.The de Sitter metric fluctuation is computed in terms of the spin-torsion background density.'],['2000-05-26'] +622,['eng'],"['Davis, A C', 'Kibble, Thomas Walter Bannerman', 'Pickles, M', 'Steer, D A']",['Dynamics and properties of chiral cosmic strings in Minkowski space'],['Astrophysics and Astronomy'],"['astrophysics, string', 'string, chiral', 'space-time, Minkowski', 'field equations', 'string, harmonic']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005514'],"['Chiral cosmic strings are produced naturally at the end of inflation in supersymmetric models where the symmetry is broken via a D-term. Consequently in such theories, where both inflation and cosmic strings contribute to the density and CMBR (microwave background) perturbations, it is necessary to understand the evolution of chiral cosmic string networks. We study the dynamics of chiral cosmic strings in Minkowski space and comment on a number of differences with those of Nambu-Goto strings. To do this we follow the work of Carter and Peter who showed that the equations of motion for chiral cosmic strings reduce to a wave equation and two constraints, only one of which is different from the familiar Nambu-Goto constraints. We study chiral string loop solutions consisting of many harmonics and determine their self-intersection probabilities, and comment on the possible cosmological significance of these results.']",['2000-05-26'] +623,['eng'],"['Schaffner-Bielich, J', 'Hanauske, M', 'Stöcker, H', 'Greiner, W']",['Hyperstars'],['Astrophysics and Astronomy'],"['n, matter', 'hyperon, matter', 'critical phenomena', 'matter, strangeness', 'matter, mass', 'hyperon hyperon, interaction', 'energy, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005490'],['Recent progress in the understanding of the high density phase of neutron stars advances the view that a substantial fraction of the matter consists of hyperons. The possible impacts of a highly attractive interaction between hyperons on the properties of compact stars is investigated. We find that the equation of state exhibits a second stable minimum at large hyperon contents which is in accord with existing hypernuclear data. This second solution gives rise to new effects for neutron star properties which are similar to the ones proposed for the deconfinement transition to strange quark matter and absolutely stable strange stars. We find that the corresponding hyperstars can have rather small radii of R=6-8 km independent of the mass.'],['2000-05-25'] +624,['eng'],"['Gawiser, E']",['Limits on Neutrino Masses from Large-Scale Structure'],['Astrophysics and Astronomy'],"['talk, Granlibakken 1999/12/10', 'neutrino, mass', 'upper limit', 'astrophysics, missing-mass', 'astrophysics, fundamental constant', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005475'],"['Massive neutrinos have a detectable effect on cosmological structure formation, in particular on the large-scale distribution of galaxies. Adding Hot Dark Matter to the now-standard Lambda CDM model leads to a worse fit to large-scale structure and CMB anisotropy data. This results in a limit on the mass of the most massive neutrino of 4 eV, assuming a power-law primordial power spectrum.']",['2000-05-25'] +625,['eng'],"['Lessard, R W', 'Buckley, J H', 'Connaughton, V', 'Le Bohec, S']",['A New Analysis Method for Reconstructing the Arrival Direction of TeV $\\gamma$-rays Using a Single Imaging Atmospheric Cherenkov Telescope'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'Cherenkov counter, imaging', 'photoelectron, amplifier', 'angular dependence', 'data analysis method']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005468'],"[""We present a method of atmospheric Cherenkov imaging which reconstructs the unique arrival direction of TeV gamma rays using a single telescope. The method is derived empirically and utilizes several features of gamma-ray induced air showers which determine, to a precision of 0.12 degrees, the arrival direction of photons, on an event-by-event basis. Data from the Whipple Observatory's 10 m gamma-ray telescope is utilized to test selection methods based on source location. The results compare these selection methods with traditional techniques and three different camera fields of view. The method will be discussed in the context of a search for a gamma-ray signal from a point source located anywhere within the field of view and from regions of extended emission.""]",['2000-05-25'] +626,['eng'],"['Brax, P', 'Martín, J']",['High Energy Physics and Quintessence'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2000/01/22', 'supergravity', 'quintessence', 'potential', 'energy, density', 'numerical calculations']","['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005449', 'http://documents.cern.ch/archive/electronic/other/uploader/MORIOND/jmartin']","['It is shown that any realistic model of quintessence should be based on Supergravity (SUGRA) since the value of the quintessence field on the attractor is approximately the Planck mass. Under very general assumptions, the typical shape of a SUGRA tracking potential is derived. Cosmological implications are investigated. In particular, it is demonstrated that, generically, the equation of state parameter is driven to a value close to -1 in agreement with recent observations.']",['2000-05-24'] +627,['eng'],"['Brax, P', 'Martín, J', 'Riazuelo, A']",['Exhaustive Study of Cosmic Microwave Background Anisotropies in Quintessential Scenarios'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'quintessence', 'astrophysics, acceleration', 'field theory, scalar', 'supergravity', 'potential', 'density, perturbation', 'moment, multipole', 'Boltzmann equation', 'spectra, perturbation', 'Hubble constant', 'matter, density', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005428'],"['Recent high precision measurements of the CMB anisotropies performed by the BOOMERanG and MAXIMA-1 experiments provide an unmatched set of data allowing to probe different cosmological models. Among these scenarios, motivated by the recent measurements of the luminosity distance versus redshift relation for type Ia supernovae, is the quintessence hypothesis. It consists in assuming that the acceleration of the Universe is due to a scalar field whose final evolution is insensitive to the initial conditions. Within this framework we investigate the cosmological perturbations for two well-motivated potentials: the Ratra-Peebles and the SUGRA tracking potentials. We show that the solutions of the perturbed equations possess an attractor and that, as a consequence, the insensitivity to the initial conditions is preserved at the perturbed level. Then, we study the predictions of these two models for structure formation and CMB anisotropies and investigate the general features of the multipole moments in the presence of quintessence. We also compare the CMB multipoles calculated with the help of a full Boltzmann code with the BOOMERanG and MAXIMA-1 data. We pay special attention to the location of the second peak and demonstrate that it significantly differs from the location obtained in the cosmological constant case. Finally, we argue that the SUGRA potential is compatible with all the recent data with a standard values of the cosmological parameters. In particular, it fits the MAXIMA-1 data better than a cosmological constant or the Ratra-Peebles potential.']",['2000-05-23'] +628,['eng'],"['Hirotani, K']",['$\\gamma$-Ray Emissions from Pulsars'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'n, matter', 'gap, width', 'particle, acceleration', 'electric field', 'energy', 'luminosity', 'pair production, path length', 'pulsar, spin', 'spin, magnetic moment', 'flux, upper limit', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005421'],"['We study the gamma-ray emissions from an outer-magnetospheric gap around a rotating neutron star. Migratory electrons and positrons are accelerated by the electric field in the gap to radiate copious gamma-rays via curvature process. Some of these gamma-rays materialize as pairs by colliding with the X-rays in the gap, leading to a pair production cascade. Imposing a gap closure condition that a single pair produces one pair in the gap on average, we explicitly solve the strength of the acceleration field and demonstrate how the peak energy and the luminosity of the curvature-radiated, GeV photons depend on the strength of the surface blackbody and the power-law emissions. Some predictions on the GeV emission from twelve rotation-powered pulsars are presented. We further demonstrate that the expected pulsed TeV fluxes are consistent with their observational upper limits. An implication of high-energy pulse phase width versus pulsar age, spin, and magnetic moment is discussed.']",['2000-05-23'] +629,['eng'],"['Golubkov, Yu A', 'Khlopov, M Ya']",['Antiprotons Annihilation in the Galaxy As A Source of Diffuse $\\gamma$ Background'],['Astrophysics and Astronomy'],"['anti-p p, annihilation', 'photon, cosmic radiation', 'photon, flux', 'cosmic radiation, background', 'cosmic radiation, energy spectrum', 'galaxy, cluster', 'antimatter, cluster', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005419'],"['The existence of antimatter domains in baryon asymmetrical Universe can appear as the cosmological consequence of particle theory in inflationary models with non-homogeneous baryosynthesis. Such a domain can survive in the early Universe and form globular cluster of antimatter stars in our Galaxy. The model of antimatter pollution of Galaxy and annihilation with matter gas is developed. The proton-antiproton annihilation gamma flux is shown to reproduce the observed galactic gamma background measured by EGRET. From comparison with observational data the estimation on the maximally allowed amount of antimatter stars, possibly present in our Galaxy, is found.']",['2000-05-23'] +630,['eng'],"['Rampp, M', 'Janka, H T']",['Spherically Symmetric Simulation with Boltzmann Neutrino Transport of Core Collapse and Post-Bounce Evolution of a 15 Solar Mass Star'],['Astrophysics and Astronomy'],"['supernova', 'neutrino/e, transport theory', 'antineutrino/e, transport theory', 'time dependence', 'energy dependence', 'angular dependence', 'Boltzmann equation, solution', 'velocity, fluid', 'electron, yield', 'model, hydrodynamical', 'neutrino, luminosity', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005438'],"['We present results of a spherically symmetric, Newtonian simulation of the core-collapse and post-bounce evolution of a 15 Msun star with a 1.28 Msun iron core. The time-, energy-, and angle-dependent transport of electron neutrinos and antineutrinos was treated with a new code which iteratively solves the Boltzmann equation and the equations for neutrino number, energy and momentum, including the effects of the motion of the stellar medium to order O(v/c) in the fluid velocity v. The supernova shock expands to a maximum radius of 350 km instead of only ~240 km as in a comparable calculation with multi-group flux-limited diffusion (MGFLD) by Bruenn, Mezzacappa, & Dineva (1995). We explain this by stronger neutrino heating due to the more accurate treatment of the transport in our model. Nevertheless, shock expansion breaks down at 180 ms after bounce, and the shock finally recedes to a radius around 250 km (compared to ~170 km in the MGFLD run). The effect of an accurate neutrino transport is helpful, as expected, but not large enough to cause an explosion of the considered 15 Msun star in spherical symmetry. Therefore postshock convection and/or an enhancement of the core neutrino luminosity by convection or reduced neutrino opacities in the neutron star seem necessary for neutrino-driven delayed explosions of such stars. We find that the electron fraction in the neutrino-heating region is larger than 0.5, which suggests that the overproduction problem of neutron-rich nuclei with mass numbers around A = 90 in the neutrino-heated ejecta is absent when electron neutrino and antineutrino spectra and luminosities are calculated with a Boltzmann solver.']",['2000-05-23'] +631,['eng'],"['Brandenberger, R H', 'Martín, J']",['The Robustness of Inflation to Changes in Super-Planck-Scale Physics'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, fluctuation', 'field theory, scalar', 'dispersion relations, nonlinear', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005432'],"['We calculate the spectrum of density fluctuations in models of inflation based on a weakly self-coupled scalar matter field minimally coupled to gravity, and specifically investigate the dependence of the predictions on modifications of the physics on length scales smaller than the Planck length. These modifications are encoded in terms of modified dispersion relations. Whereas for some classes of dispersion relations the predictions are unchanged compared to the usual ones which are based on a linear dispersion relation, for other classes important differences are obtained, involving tilted spectra, spectra with exponential factors and with oscillations. We conclude that the predictions of inflationary cosmology in these models are not robust against changes in the super-Planck-scale physics.']",['2000-05-23'] +632,['eng'],"['Kennedy, Dallas C']",['The Solar Core and Solar Neutrinos'],['Astrophysics and Astronomy'],"['talk, Columbia 2000/03/10', 'neutrino, solar', 'neutrino, flux', 'model, solar', 'homology', 'astrophysics', 'matter, mass', 'matter, density', 'dependence, temperature', 'luminosity', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005412'],"['The long-standing deficit of measured versus predicted solar neutrino fluxes, is re-examined in light of possible astrophysical solutions. In the last decade, solar neutrino flux and helioseismic measurements have greatly strengthened the case for non-astrophysical solutions. But some model- independent tests remain open.']",['2000-05-22'] +633,['eng'],"['Crooks, J L', 'Dunn, J O', 'Frampton, Paul H', 'Ng, Y J']",['Quintessence and CMB'],['Astrophysics and Astronomy'],"['quintessence', 'cosmic radiation, background', 'matter, density', 'astrophysics, fundamental constant', 'time dependence', 'energy, conservation law', 'light nucleus, production', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005406'],"['A particular kind of quintessence is considered, with equation of motion $p_Q/\\rho_Q = -1$, corresponding to a cosmological term with time-dependence $\\Lambda(t) = \\Lambda(t_0) (R(t_0)/R(t))^{P}$ which we examine initially for $0 \\leq P < 3$. Energy conservation is imposed, as is consistency with big-bang nucleosynthesis, and the range of allowed $P$ is thereby much restricted to $0 \\leq P < 0.2$. The position of the first Doppler peak is computed analytically and the result combined with analysis of high-Z supernovae to find how values of $\\Omega_m$ and $\\Omega_{\\Lambda}$ depend on $P$.']",['2000-05-22'] +634,['eng'],"['Lukash, V N', 'Mikheeva, E V', 'Müller, V', 'Malinovsky, A M']",['Generalised inflation with a gravitational wave background'],['Astrophysics and Astronomy'],"['inflationary universe', 'gravitational radiation, background', 'density, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'galaxy, cluster', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005395'],['We propose a Lambda-inflation model which explains a significant part of the COBE signal by primordial cosmic gravitational waves. The primordial density perturbations fulfill both the constraints of large-scale microwave background and galaxy cluster normalization. The model is tested against the galaxy cluster power spectrum and the high-multipole angular CMB anisotropy.'],['2000-05-22'] +635,['eng'],"['Protheroe, R J', 'Meyer, H']",['An infrared background-TeV $\\gamma$-ray crisis?'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'infrared problem', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'photon photon, interaction', 'photon, path length', 'galaxy', 'symmetry breaking, Lorentz', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005349'],"['We consider the implications of the recent determination of the universal infrared background for the propagation of photons up to 20 TeV from the active galaxy Markarian 501 as observed by HEGRA. At 20 TeV the mean free path for photon-photon collisions on the infrared background would be much shorter than the distance to Markarian 501, implying absorption factors of the order of exp(-10), or greater, and consequently an excessive power output for this active galaxy. Possible solutions of this problem are discussed.']",['2000-05-18'] +636,['eng'],"['Kuiper, L', 'Hermsen, W', 'Verbunt, F', 'Thompson, D J', 'Stairs, I H', 'Lyne, A G', 'Strickman, M S', 'Cusumano, G']",['The likely detection of pulsed high-energy gamma-ray emission from millisecond pulsar PSR J0218+4232'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'pulsar', 'luminosity', 'data analysis method', 'n, matter', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005338'],"['We report circumstantial evidence for the first detection of pulsed high-energy gamma-ray emission from a millisecond pulsar, PSR J0218+4232, using data collected with the Energetic Gamma Ray Experiment (EGRET) on board the Compton Gamma Ray Observatory (CGRO). The EGRET source 3EG J0222+4253 is shown to be spatially consistent with PSR J0218+4232 for the energy range 100 - 300 MeV. Above 1 GeV the nearby BL Lac 3C 66A is the evident counterpart, and between 300 MeV and 1 GeV both sources contribute to the gamma-ray excess. Folding the 100-1000 MeV photons with an accurate radio ephemeris of PSR J0218+4232 yields a double peaked pulse profile with a ~3.5 sigma modulation significance and with a peak separation of ~0.45 similar to the 0.1-10 keV pulse profile.']",['2000-05-17'] +637,['eng'],"['Landau, S J', 'Vucetich, H']",['Testing theories that predict time variation of fundamental constants'],['Astrophysics and Astronomy'],"['fundamental constant, time variation', 'Kaluza-Klein model, validity test', 'astrophysics', 'geophysics', 'statistical analysis', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005316'],"[""We consider astronomical and local bounds on time variation of fundamental constants to test some generic Kaluza-Klein-like models and some particular cases of Beckenstein theory. Bounds on the free parameters of the different theories are obtained. Beckenstein's theory can be discarded based on confrotation with experimental data.""]",['2000-05-16'] +638,['eng'],"['Kachelriess, M', 'Plümacher, Michael']",['Ultrahigh energy neutrino interactions and weak-scale string theories'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino nucleon, interaction', 'total cross section, energy dependence', 'graviton, exchange', 'W, exchange', 'Kaluza-Klein model', 'showers, air', 'string model', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005309'],"['It has been suggested that ultrahigh energy neutrinos can acquire cross-sections approaching hadronic size if the string scale is as low as 1-10 TeV. In this case, the vertical air showers observed with energies above the Greisen-Zatsepin-Kuzmin cutoff at E approximately 6x10^{19} eV could be initiated by neutrinos which are the only known primaries able to travel long distances unimpeded. We have calculated the neutrino-nucleon cross-section due to the exchange of Kaluza-Klein excitations of the graviton in a field theoretical framework. We have found that the neutrino-nucleon cross section and the transferred energy per interaction are too small to explain vertical showers even in the most optimistic scenario. However, future cosmic ray experiments like AUGER or OWL which are able to observe horizontal air showers could have a potential to restrict or to discover weak-scale string physics comparable to LHC.']",['2000-05-16'] +639,['eng'],"['Ziaeepour, H']",['A decaying ultra heavy dark matter (WIMPZILLA)'],['Astrophysics and Astronomy'],"['talk, Moscow 1999/10/17', 'astrophysics, missing-mass', 'WIMPZILLA, decay', 'WIMPZILLA, lifetime', 'photon, cosmic radiation', 'p, cosmic radiation', 'energy, flux', 'grand unified theory', 'supersymmetry', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005299'],['Recent theoretical and observational motivations for existence of a decaying Ultra Heavy Dark Matter (UHDM) are reviewed. We show that present data from Ultra High Energy Cosmic Rays (UHECRs) and SN - Ia are compatible with a relatively short lifetime of UHDM.'],['2000-05-16'] +640,['eng'],"['Bugaev, E V', 'Konishchev, K V']",['Constraints on diffuse neutrino background from primordial black holes'],['Astrophysics and Astronomy'],"['astrophysics, model', 'black hole, radiation', 'black hole, mass spectrum', 'neutrino/e, emission', 'neutrino/e, energy spectrum', 'neutrino/e, flux', 'density, fluctuation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005295'],['We calculated the energy spectra and the fluxes of electron neutrino emitted in the process of evaporation of primordial black holes (PBHs) in the early universe. It was assumed that PBHs are formed by a blue power-law spectrum of primordial density fluctuations. We obtained the bounds on the spectral index of density fluctuations assuming validity of the standard picture of gravitational collapse and using the available data of several experiments with atmospheric and solar neutrinos. The comparison of our results with the previous constraints (which had been obtained using diffuse photon background data) shows that such bounds are quite sensitive to an assumed form of the initial PBH mass function.'],['2000-05-16'] +641,['eng'],"['Weinberg, S']",['The Cosmological Constant Problems'],['Astrophysics and Astronomy'],"['talk, Marina del Rey 2000/02/23', 'astrophysics, fundamental constant', 'quintessence', 'energy, density', 'anthropic principle', 'astrophysics, model', 'field theory, scalar']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005265'],"['The old cosmological constant problem is to understand why the vacuum energy is so small; the new problem is to understand why it is comparable to the present mass density. Several approaches to these problems are reviewed. Quintessence does not help with either; anthropic considerations offer a possibility of solving both. In theories with a scalar field that takes random initial values, the anthropic principle may apply to the cosmological constant, but probably to nothing else.']",['2000-05-15'] +642,['eng'],"['Konoplich, R V', 'Rubin, S G']",['Possible Signature of Low Scale Gravity in Ultra High Enegry Cosmic Rays'],['Astrophysics and Astronomy'],"['gravitation, effect', 'neutrino antineutrino, annihilation', 'photon, direct production', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'showers, air', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005225'],['We show that the existence of low scale gravity at TeV scale could lead to a direct production of photons with energies above 10^22 eV due to annihilation of ultra high energy neutrinos on relic massive neutrinos of the galactic halo. Air showers initialized in the terrestrial atmosphere by these ultra energetic photons could be collected in near future by the new generation of cosmic ray experiments.'],['2000-05-11'] +643,['eng'],"['Grandpierre, A']",['New type astrophysical solution to the solar neutrino problems and its predicitons to the SNO'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'neutrino, oscillation', 'model, solar', 'luminosity, constraint', 'nuclear reaction', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005221'],"['The anomalously slow rotation of the solar core is just one from a remarkable lists of fundamental indications showing that the solar core is somehow coupled to the surface activity cycle. On the other hand, the atmospheric, LSND and solar neutrino problems are not consistent, therefore one or more of the neutrino experiments must be attributed - at least in part - to some phenomena other than neutrino oscillations, or a fourth neutrino is required. We use the luminosity constraint in a general case not considered yet, taking into account nuclear reactions occurring in small hot bubbles indicated to be present in the solar core (Grandpierre, 2000). The dynamic solar model fit the observed neutrino fluxes within one-and-half sigma even without oscillations. This fit is shown to be better than the present day MSW and VAC fits. An attracting perspective is obtained for a simultaneous solution of the neutrino problems and the solar core-related astrophysical problems. Predictions of the dynamic solar model are presented for the SNO measurements.']",['2000-05-11'] +644,['eng'],"['Sato, H']",['Extremely High Energy and Violation of Lorentz Invariance'],['Astrophysics and Astronomy'],"['talk, Tsukuba 1999/06/07', 'cosmic radiation', 'symmetry breaking, Lorentz', 'photon, velocity', 'photon, decay', 'radiation, Cherenkov']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005218'],['Extremely high-energy(EHE) cosmic rays might provide a chance to check a violation of the Lorentz symmetry of spacetime. Some theoretical consideration is described about why the Lorentz symmetry might break-down in EHE phenomena in this universe. Some models which introduce the violation of the Lorentz symmetry will be discussed.'],['2000-05-11'] +645,['eng'],"['Kaplinghat, M', 'Knox, L', 'Turner, M S']",['Annihilating the Cold Dark Matter Cusp Crisis'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'cross section, annihilation', 'velocity, dependence', 'galaxy, cluster', 'matter, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005210'],"['Structure formation with cold dark matter (CDM) predicts halos with a central density cusp, which is observationally disfavored. If CDM particles have an annihilation cross section ~ 10^{-28} (m/GeV) cm^2, then annihilations in the dense, central parts of halos will soften the cusps. The predicted softened halo core densities depend critically upon the velocity dependence of the annihilation cross section. We show that from galactic satellites to clusters of galaxies, the halos all have nearly the same core density: rho_core ~ 0.02 M_sun/pc^3 = 0.8 GeV/cm^3. This remarkable fact implicates s-wave annihilation. We discuss the constraints on models for annihilating CDM, which point to a candidate beyond those currently favored.']",['2000-05-11'] +646,['eng'],"['Bednarz, J']",['Acceleration time scale in an ultrarelativistic shock'],['Astrophysics and Astronomy'],"['cosmic radiation, acceleration', 'shock waves, relativistic', 'magnetic field, fluctuation', 'energy spectrum', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005207'],"['The acceleration mechanism at ultrarelativistic shocks is investigated using the Monte Carlo simulations. We apply a method of discrete small amplitude particle momentum scattering to reproduce highly anisotropic conditions at the shock and carefully describe the acceleration mechanism. The obtained acceleration times equal $1.0 r_{g}/c$ if the spectral index reach the value of 2.2, independent of physical conditions in the shock. Some other parameters of the acceleration process are also provided.']",['2000-05-10'] +647,['eng'],"['Totani, T']",['An Interpretation of the Evidence for TeV Emission from Gamma-Ray Burst 970417a'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'cosmic radiation, diffusion', 'particle, acceleration', 'gamma ray burst', 'proton synchrotron, model', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005071'],"['The Milagrito collaboration recently reported evidence for emission of very high energy gamma-rays in the TeV range from one of the BATSE GRBs, GRB 970417a. Here I discuss possible interpretations of this result. Taking into account the intergalactic absorption of TeV gamma-rays by the cosmic infrared background, I found that the detection rate (one per 54 GRBs observed by the Milagrito) and energy fluence can be consistently explained with the redshift of this GRB at z \\sim 0.7 and the isotropic total energy in the TeV range, E_{TeV, iso} >~ 10^{54} erg. This energy scale is not unreasonably large, but interestingly similar to the maximum total GRB energy observed to date, in the sub-MeV range for GRB 990123. On the other hand, the energy emitted in the ordinary sub-MeV range becomes E_{MeV, iso} \\sim 10^{51} erg for the GRB 970417a, which is much smaller than the total energy in the TeV range by a factor of about 10^3. I show that the proton-synchrotron model of GRBs provides a possible explanation for these observational results. I also discuss some observational signatures expected in the future experiments from this model.']",['2000-05-05'] +648,['eng'],"['Gangui, A']",['Superconducting Cosmic Strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'superconducting, string', 'topology, defect', 'crystal, liquid', 'gravitation, effect', 'current', 'symmetry breaking', 'Higgs model', 'cosmic radiation, background', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005186'],['These relics from the early universe could be the answer to many astrophysical conundrums.'],['2000-05-09'] +649,['eng'],"['Balbi, A', 'Ade, P', 'Bock, J J', 'Borrill, J', 'Boscaleri, A', 'De Bernardis, P', 'Ferreira, P G', 'Hanany, S', 'Hristov, V V', 'Jaffe, A H', 'Lee, A T', 'Oh, S', 'Pascale, E', 'Rabii, B', 'Richards, P L', 'Smoot, G F', 'Stompor, R', 'Winant, C D', 'Wu, J H P']",['Constraints on Cosmological Parameters from MAXIMA-1'],['Astrophysics and Astronomy'],"['inflationary universe, adiabatic', 'cosmic radiation, background', 'cosmic radiation, spectra', 'energy, density', 'baryon, density', 'astrophysics, missing-mass', 'density, fluctuation', 'supernova', 'astrophysics, fundamental constant', 'light nucleus, production', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005124'],"['We set new constraints on a seven-dimensional space of cosmological parameters within the class of inflationary adiabatic models. We use the angular power spectrum of the cosmic microwave background measured over a wide range of l in the first flight of the MAXIMA balloon-borne experiment (MAXIMA-1) and the low l results from COBE/DMR. We find constraints on the total energy density of the universe, \\Omega=0.90 +/- 0.15, the physical density of baryons, \\Omega_{b}h^2 = 0.025 +/- 0.010, the physical density of cold dark matter, \\Omega_{cdm}h^2=0.13 +/- 0.10, and the spectral index of primordial scalar fluctuations, n_s=0.99 +/- 0.09, all at the 95% confidence level. By combining our results with measurements of high-redshift supernovae we constrain the value of the cosmological constant and the fractional amount of pressureless matter in the universe to 0.40 < \\Omega_\\Lambda < 0.76 and 0.25< \\Omega_{m} < 0.50, at the 95% confidence level. Our results are consistent with a flat universe, the baryon density from big bang nucleosynthesis and the shape parameter deduced from large scale structure.']",['2000-05-09'] +650,['eng'],"['Contaldi, C R']",['Cosmic strings in the age of Boomerang'],['Astrophysics and Astronomy'],"['astrophysics, string', 'string model, closed', 'inflationary universe, hybrid', 'matter, density', 'astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, spectra', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005115'],"['We show how two simple modifications to the standard cosmic string scenario for structure formation compare to the recently released Boomerang data set. Namely we consider pure string closed models and mixed models where both inflation and strings are responsible for the perturbations. In the closed models we find that pure string models would require a universe with roughly $\\Omega_M=0.8$, $\\Omega_{\\Lambda}=1.6$ to agree with the peak position revealed by the data and in agreement with the SNIa data. In the hybrid scenario with local strings we find that we require even more tilt and baryon content ($n_s\\sim 0.8$, $\\Omega_b=0.08$, $H_0=70$) to match the data than with pure inflation models. The case with global strings fares better with a standard period of $\\Lambda$CDM inflation and a $\\sim30%$ contribution from strings being in good agreement with the data.']",['2000-05-09'] +651,['eng'],"['Hansen, S H', 'Villante, F L']",['Decaying neutrino and a high cosmological baryon density'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'baryon, density', 'cosmic radiation, background', 'neutrino/tau, decay modes', 'neutrino/tau, lifetime', 'neutrino/tau, mass', 'numerical calculations, interpretation of experiments', 'neutrino/tau --> neutrino/e scalar particle']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005114'],"['The low second acoustic peak in the recent Boomerang data may indicate a cosmological baryon density which is larger than allowed by standard big bang nucleosynthesis. We show that the decay of the tau-neutrino: nu_tau -> nu_e + phi, where nu_e is the electron neutrino and phi is a scalar, essentially can assure agreement between BBN calculations and light element observations for a large baryon density.']",['2000-05-09'] +652,['eng'],"['Ivanov, M A']",['Possible manifestations of the graviton background'],['Astrophysics and Astronomy'],"['scattering, photon graviton', 'background, graviton', 'supernova', 'photon, energy loss', 'photon, flux', 'matter, deceleration', 'total cross section, energy dependence', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005084'],"['Possible effects are considered which would be caused by a hypothetical superstrong interaction of photons or massive bodies with single gravitons of the graviton background. If full cosmological redshift magnitudes are caused by the interaction, then the luminosity distance in a flat non-expanding universe as a function of redshift is very similar to the specific function which fits supernova cosmology data by Riess et al. From another side, in this case every massive body, slowly moving relatively to the background, would experience a constant acceleration, proportional to the Hubble constant, of the same order as a small additional acceleration of Pioneer 10, 11.']",['2000-05-05'] +653,['eng'],"['Chimento, L P', 'Jakubi, A S', 'Pavón, D']",['Enlarged Q-matter cosmology'],['Astrophysics and Astronomy'],"['model, fluid', 'pressure, dissipation', 'matter, quintessence', 'field theory, scalar', 'expansion, acceleration', 'attractor', 'astrophysics, missing-mass', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005070'],['We show that the combination of a fluid with a bulk dissipative pressure and quintessence matter can simultaneously drive an accelerated expansion phase and solve the coincidence problem of our current Universe. We then study some scenarios compatible with the observed cosmic acceleration.'],['2000-05-04'] +654,['eng'],"['Collar, J I', 'Puibasset, J', 'Girard, T A', 'Limagne, D', 'Miley, H S', 'Waysand, G']",['Prospects for SIMPLE 2000'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, search for', 'counters and detectors, droplet', 'carbon, chlorine', 'fluorine', 'thermodynamics, critical phenomena', 'neutralino', 'deep underground detector', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005059'],"[""SIMPLE 2000 ({\\underline S}uperheated {\\underline I}nstrument for {\\underline M}assive {\\underline P}artic{\\underline {LE}} searches) will consist of an array of eight to sixteen large active mass ($\\sim15$ g) Superheated Droplet Detectors(SDDs) to be installed in the new underground laboratory of Rustrel-Pays d'Apt. Several factors make of SDDs an attractive approach for the detection of Weakly Interacting Massive Particles (WIMPs), namely their intrinsic insensitivity to minimum ionizing particles, high fluorine content, low cost and operation near ambient pressure and temperature. We comment here on the fabrication, calibration and already-competitive first limits from SIMPLE prototype SDDs, as well as on the expected immediate increase in sensitivity of the program, which aims at an exposure of $>$25 kg-day during the year 2000. The ability of modest-mass fluorine-rich detectors to explore regions of neutralino parameter space beyond the reach of the most ambitious cryogenic projects is pointed out.""]",['2000-05-04'] +655,['eng'],"['Hogan, C J']",['Gravitational Waves from Mesoscopic Dynamics of the Extra Dimensions'],['Astrophysics and Astronomy'],"['gravitational radiation, measurement', 'membrane model', 'spectra, background', 'potential, radion', 'symmetry, spontaneously broken', 'counters and detectors', 'interference, laser', 'space-time, higher-dimensional', 'energy flow', 'turbulence, relativistic', 'Goldstone particle', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005044'],"[""Recent models which describe our world as a brane embedded in a higher dimensional space introduce new geometrical degrees of freedom: the shape and/or size of the extra dimensions, and the position of the brane. These modes can be coherently excited by symmetry breaking in the early universe even on ``mesoscopic'' scales as large as 1 mm, leading to detectable gravitational radiation. Two sources are described: relativistic turbulence caused by a first-order transition of a radion potential, and Kibble excitation of Nambu-Goldstone modes of brane displacement. Characteristic scales and spectral properties are estimated and the prospects for observation by LISA are discussed. Extra dimensions with scale between 10 \\AA and 1 mm, which enter the 3+1-D era at cosmic temperatures between 1 and 1000 TeV, produce backgrounds with energy peaked at observed frequencies in the LISA band, between $10^{-1}$ and $10^{-4}$ Hz. The background is detectable above instrument and astrophysical foregrounds if initial metric perturbations are excited to a fractional amplitude of $10^{-3}$ or more, a likely outcome for the Nambu-Goldstone excitations.""]",['2000-05-03'] +656,['eng'],"['Regimbau, T', 'De Pacheco, J A F']",['Gravitation Wave Emission from Radio Pulsars Revisited'],['Astrophysics and Astronomy'],"['gravitational radiation', 'pulsar', 'counters and detectors, interference', 'signal processing', 'statistical analysis', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005043'],"['We report a new pulsar population synthesis based on Monte Carlo techniques, aiming to estimate the contribution of galactic radio pulsars to the continuous gravitational wave emission. Assuming that the rotation periods of pulsars at birth have a Gaussian distribution, we find that the average initial period is 290 ms. The number of objects with periods equal to or less than 0.4 s, and therefore capable of being detected by an interferometric gravitational antenna like VIRGO, is of the order of 5100-7800. With integration times lasting between 2 and 3 yr, our simulations suggest that about two detections should be possible, if the mean equatorial ellipticity of the pulsars is $\\epsilon$ =10$^{-6}$. A mean ellipticity an order of magnitude higher increases the expected number of detections to 12-18, whereas for $\\epsilon < 10^{-6}$, no detections are expected']",['2000-05-03'] +657,['eng'],"['Bouchet, F R', 'Peter, P', 'Riazuelo, A', 'Sakellariadou, M']",['Is there evidence for topological defects in the BOOMERanG data?'],['Astrophysics and Astronomy'],"['astrophysics, string', 'topology, defect', 'cosmic radiation, background', 'inflationary universe', 'statistical analysis', 'spectra, fluctuation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005022'],"[""The recently released BOOMERanG data show a secondary peak ``contradicting topological defect predictions''. We show that not only is such a statement misleading, but also that the relatively low amplitude of the observed secondary peak might well be an evidence in favor of decoherence, a feature known to characterize topological defect scenarios. The picture that naturally emerges would therefore be of the hybrid kind, yielding the prediction that the third peak should have also a low amplitude.""]",['2000-05-02'] +658,['eng'],"['Hannestad, S']",['New constraints on neutrino physics from Boomerang data'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'data analysis method', 'radiation, density', 'upper limit', 'neutrino, flavor', 'neutrino, decay', 'lepton, asymmetry', 'statistical analysis', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005018'],"['We have performed a likelihood analysis of the recent data on the Cosmic Microwave Background Radiation (CMBR) anisotropy taken by the Boomerang experiment. We find that this data places a strong upper bound on the radiation density present at recombination. Expressed in terms of the equivalent number of neutrino species the $2\\sigma$ bound is N_nu < 13, and the standard model prediction, N_nu = 3.04, is completely consistent the the data. This bound is complementary to the one found from Big Bang nucleosynthesis considerations in that it applies to any type of radiation, i.e. it is not flavour sensitive. It also applies to the universe at a much later epoch, and as such places severe limits on scenarios with decaying neutrinos. The bound also yields a firm upper limit on the lepton asymmetry in the universe.']",['2000-05-02'] +659,['eng'],"['Meliani, M T', ""D'Araújo, J C N"", 'Aguiar, O D']",['Cataclysmic variables as sources of gravitational waves'],['Astrophysics and Astronomy'],"['gravitational radiation, particle source', 'binary', 'counters and detectors', 'interference, laser', 'threshold', 'background', 'amplitude analysis', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004406'],"['General Relativity predicts that binary systems of stars produce gravitational waves of significant intensity. Here we are particularly interested in the cataclysmic variable binaries (CVs). These systems emit low frequency gravitational waves, $ f < 10^{-3} Hz$. We present here a catalog of CVs and argue that part of them are capable of being detected by the Laser Interferometer Space Antenna (LISA).']",['2000-05-01'] +660,['eng'],"['Kämpfer, B']",['Cosmic Phase Transitions'],['Astrophysics and Astronomy'],"['talk, Dresden 2000/03/20', 'astrophysics, model', 'critical phenomena', 'quantum chromodynamics, confinement', 'grand unified theory', 'inflationary universe', 'quark hadron, transition', 'electroweak interaction', 'symmetry breaking', 'thermodynamics', 'field equations', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004403'],"['The sequence of phase transitions during the hot history of the universe is followed within a phenomenological framework. Particular emphasis is put on the QCD confinement transition, which is at reach under earth laboratory conditions. A tepid inflationary scenario on the GUT scale with bubble grow at moderate supercooling is discussed.']",['2000-05-01'] +661,['eng'],"[""D'Araújo, J C N"", 'Miranda, O D', 'Aguiar, O D']",['Stochastic background of gravitational waves'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'energy, flux', 'black hole', 'energy, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004395'],"[""A continuous stochastic background of gravitational waves (GWs) for burst sources is produced if the mean time interval between the occurrence of bursts is smaller than the average time duration of a single burst at the emission, i.e., the so called duty cycle must be greater than one. To evaluate the background of GWs produced by an ensemble of sources, during their formation, for example, one needs to know the average energy flux emitted during the formation of a single object and the formation rate of such objects as well. In many cases the energy flux emitted during an event of production of GWs is not known in detail, only characteristic values for the dimensionless amplitude and frequencies are known. Here we present a shortcut to calculate stochastic backgrounds of GWs produced from cosmological sources. For this approach it is not necessary to know in detail the energy flux emitted at each frequency. Knowing the characteristic values for the ``lumped'' dimensionless amplitude and frequency we show that it is possible to calculate the stochastic background of GWs produced by an ensemble of sources.""]",['2000-05-01'] +662,['eng'],"['Lesgourgues, Julien', 'Peloso, M']","['Remarks on the Boomerang results, the cosmological constant and the leptonic asymmetry']",['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'lepton, asymmetry', 'baryon, density', 'astrophysics, fundamental constant', 'astrophysics, missing-mass', 'light nucleus, production', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004412'],"['The very recent Boomerang results give an estimate of unprecedented precision of the Cosmic Microwave Background anisotropies on sub-angular scales. A puzzling feature for theoretical cosmology is the low amplitude of the second acoustic peak. Through a qualitative discussion, we argue that a scarcely considered category of flat models, with a leptonic asymmetry, a high baryon density and a low (or zero) cosmological constant seem to be in very good agreement with the data, while still being compatible with big bang nucleosynthesis and some other observational constrains. Although this is certainly not the only way to explain the data, we believe that these models deserve to be included in forthcoming likelihood analyses.']",['2000-05-01'] +663,['eng'],"['Blanco-Pillado, J J', 'Olum, K D', 'Vilenkin, A']",['General solution for chiral-current-carrying strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'superconducting, string', 'current, chiral', 'energy, density']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004410'],"['We give a general solution to the equations of motion for superconducting strings with chiral (null) currents not coupled to any long-range fields. We apply this solution to show that the motion of such string loops is strictly periodic, and we briefly analyze cusp-like behavior and vorton-like solutions of arbitrary shape.']",['2000-05-01'] +664,['eng'],"['Cataldo, M', 'Campo, S']",['Scalar fields in an anisotropic closed universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'anisotropy', 'viscosity', 'field theory, scalar', 'matter, density', 'quintessence', 'field equations, solution', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004384'],"['We study in this article a class of homogeneous, but anisotropic cosmological models in which shear viscosity is included. Within the matter content we consider a component (the quintessence component) determined by the barotropic equations of state, $p=\\alpha \\rho$, with $\\alpha < 0$. We establish conditions under which a closed axisymmetrical cosmological model may look flat al low redshift.']",['2000-04-28'] +665,['eng'],"['Poirier, J', 'Lin, T F', 'Gress, J', 'Fragile, P C', 'Mathews, G J']",['Sub-TeV Gammas in Coincidence with BATSE Gamma Ray Bursts'],['Astrophysics and Astronomy'],"['gamma ray burst', 'photon, cosmic radiation', 'cosmic radiation, primary', 'muon, cosmic radiation', 'cosmic radiation, secondary radiation', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004379'],"['We report on results of a search for high-energy gamma-ray-induced muon secondaries in coincidence with gamma ray bursts (GRBs) detected by BATSE. If a gamma ray of 1 TeV energy arrives in coincidence with a GRB, its pion production and decay leads to ~0.23 muons with sufficient energy to reach detection level. Such muons have been identified and their angles measured using the Project GRAND air shower array. A total of six bright bursts have been identified from the BATSE GRB catalog which occurred near zenith while Project GRAND was in operation. Of these six, the GRB with the highest product of GRB flux and geometrical acceptance shows evidence of an enhanced muon count rate at the burst time and angle at the +3.2 sigma level. The chance probability of obtaining our results for these six GRBs is 5E-4. Simple extrapolations of the low-energy BATSE gamma-ray energy spectra for these GRBs to the energy region of GRAND are unable to explain the observed muon count rates. Thus the observed excesses suggest a new component of higher energy gamma rays associated with these bursts.']",['2000-04-28'] +666,['eng'],"['Zdunik, J L']",['Strange stars'],['Astrophysics and Astronomy'],"['matter, strangeness', 'bag model', 'particle, orbit', 'scaling', 'measurement, oscillation', 'mass, dependence', 'strong interaction, coupling constant', 'approximation, linear', 'matter, stability', 'baryon number', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004375'],"['The equation of state of strange matter build of the u,d,s quarks in the framework of the MIT bag model is studied. The scaling relations with bag constant are discussed and applied to the determination of maximum frequency of a particle in stable circular orbit around strange star. The highest QPO frequency of 1.33 kHz observed so far is consistent with the strange stars models for which the maximum QPO frequency is 1.7-2.4 kHz depending on the strange quark mass and the QCD coupling constant. The linear approximation of the equation of state is found and the parameters of this EOS are determined as a functions of strange quark mass, QCD coupling constant and bag constant. This approximation reproduces exact results within an error of the order of 1% and can be used for the complete study of the properties of strange stars including microscopic stability of strange matter and determination of the total baryon number of the star.']",['2000-04-28'] +667,['eng'],"['Guy, J', 'Renault, C', 'Aharonian, F A', 'Rivoal, M', 'Tavernet, J P']",['Constraints on the Cosmic Infra-Red Background based on BeppoSAX and CAT spectra of Mkn 501'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'photon, absorption', 'photon, cosmic radiation', 'Cherenkov counter', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'cosmic radiation, diffusion', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004355'],"[""The TeV and X-ray data obtained by the imaging Cherenkov telescope CAT and X-ray satellite BeppoSAX during the remarkable flare of Mkn 501 in April 16, 1997 are used to constrain the flux of the Cosmic Infrared Background (CIB) using different CIB models. We show that a non-negligible absorption of gamma-rays due to the CIB could take place already in the low-energy (sub-TeV) domain of the spectrum of Mkn 501. This implies that the data of the low-energy threshold CAT telescope contain very important information about the CIB at short wavelengths, 0.4 mum <= lambda <= 3. mum. The analysis of almost simultaneous spectroscopic measurements of Mkn 501 in a high state by CAT and BeppoSAX in the framework of the standard homogeneous Synchrotron-Self-Compton (SSC) framework model leads to the conclusion that the density of the near-infrared background with typical ``starlight spectrum'' around 1 mum should be between 5 and 35 nW m^-2 sr^-1 (99 % CL), with most likely value around 20 nW m^-2 sr^-1. Also we argue that the CAT gamma-ray data alone allow rather robust upper limits on the CIB, lambda F_lambda <= 60 nW m^-2 sr^-1 at 1 mum, taking into account that for any reasonable scenario of gamma-ray production the differential intrinsic spectrum of gamma-ray hardly could be flatter than dN/dE == E^-1. This estimate agrees, within statistical and systematic uncertainties, with recent reports about tentative detections of the CIB at 2.2 and 3.5 mum by the Diffuse Infrared Background Experiment (DIRBE), as well as with the measurements of the background radiation at optical wavelengths from absolute photometry. We also discuss the impact of the intergalactic absorption effect in derivation of the SSC parameters for the jet in Mkn 501.""]",['2000-04-27'] +668,['eng'],"['Weller, J']",['Bubbles from dark energy?'],['Astrophysics and Astronomy'],"['talk, Granlibakken 1999/12/10', 'supernova', 'expansion, acceleration', 'bubble', 'field theory, scalar', 'potential', 'tunneling', 'membrane model, D-brane', 'vacuum state', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004096'],['In a model recently proposed by Albrecht and Skordis it was suggested that the observed accelerated expansion of the universe could be caused by a scalar field which is trapped in a local minimum of an exponential potential modified by a polynomial prefactor. We show that scalar field cosmologies with this kind of local minimum in the potential are stable and do not decay to the true vacuum if they fulfill the observational constraints from the Type Ia Supernovae experiments. Further we briefly sketch how this potential could be related to a potential of interacting D-branes.'],['2000-04-10'] +669,['eng'],"['Berezhko, E G', 'Völk, H J']",['TeV Gamma Rays Expected from Supernova Remnants in Different Uniform Interstellar Media'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'nucleon nucleon, interaction', 'cosmic radiation, acceleration', 'photon, emission', 'supernova', 'cosmic radiation, diffusion', 'momentum spectrum, time dependence', 'pi0, radiative decay', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004354'],"['Calculations of the expected TeV $\\gamma$-ray emission, produced by accelerated cosmic rays (CRs) in nuclear collisions, from supernova remnants evolving in a uniform interstellar medium (ISM) are presented. The aim is to study the sensitivity of $\\gamma$-ray production to a physical parameter set. Apart from its general proportionality to N_H, it is shown that the $\\gamma$-ray production essentially depends upon the ratio of the CR diffusion coefficient $\\kappa$ to a critical value $\\kappa_{crit}=10(B_0/5 \\mu{G})(N_H/0.3 {cm}^{-3})^{-1/3}\\kappa_B$, where B_0 and N_H are the magnetic field and hydrogen number density of the ISM, and $\\kappa_B$ denotes the Bohm diffusion coefficient. If $\\kappa$ is of the same order or lower than $\\kappa_{crit}$, then the peak TeV $\\gamma$-ray flux in the Sedov evolutionary phase, normalized to a distance of 1 kpc, is about 10^{-10}(N_H/0.3 {cm}^{-3}) photons cm^{-2} s^{-1}. For a CR diffusion coefficient that is significantly larger than $\\kappa_{crit}$, the CR cutoff energy is less than 10 TeV and the expected $\\gamma$-ray flux at 1 TeV is considerably below the presently detectable level of 10^{-12} photons cm^{-2} s^{-1}. The same is of course true for a SNR in the rarified, so-called hot ISM.']",['2000-04-27'] +670,['eng'],"['Berezhko, E G', 'Völk, H J']",['Galactic Gamma-Ray Background Radiation from Supernova Remnants'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, particle source', 'supernova', 'photon, luminosity', 'pi0, decay', 'photon, emission', 'galaxy, AGN', 'Compton scattering', 'bremsstrahlung', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004353'],"['The contribution of the Source Cosmic Rays (SCRs), confined in Supernova Remnants, to the diffuse high energy \\gr emission above 1 GeV from the Galactic disk is studied. \\grs produced by the SCRs have a much harder spectrum compared with those generated by the Galactic Cosmic Rays which occupy a much larger residence volume uniformly. SCRs contribute less than 10% at GeV energies and become dominant at \\gr energies above 100 GeV. The contributions from $\\pi^0$-decay and Inverse Compton \\grs have comparable magnitude and spectral shape, whereas the Bremsstrahlung component is negligible. At TeV energies the contribution from SCRs increases the expected diffuse \\gr flux almost by an order of magnitude. It is shown that for the inner Galaxy the discrepancy between the observed diffuse intensity and previous model predictions at energies above a few GeV can be attributed to the SCR contribution.']",['2000-04-27'] +671,['eng'],"['Ng, S C C']",['Observational constraints upon quintessence models arise from moduli fields'],['Astrophysics and Astronomy'],"['quintessence', 'moduli', 'field theory, scalar', 'potential', 'phase space', 'critical phenomena', 'supernova', 'gravitation, lens', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004196'],"['We study observational constraints on cosmological models with a quintessence arises from moduli fields. The scalar field potential is given by a double exponential potential V=V_0 exp(-A e^{sqrt{2} kappa phi}). After reviewing the properties of the solutions, from a dynamical systems phase space analysis, we consider the constraints on parameter values imposed by luminosity distances from the 60 Type IA supernovae published by Perlmutter et al., and also from gravitational lensing statistics of distant quasars. We also update the constraints on models with a single exponential potential V=V_0 e^{-lambda kappa phi}.']",['2000-04-17'] +672,['eng'],"['Matos, T', 'Urena-Lopez, L A']",['Quintessence and Scalar Dark Matter in the Universe'],['Astrophysics and Astronomy'],"['quintessence', 'astrophysics, missing-mass', 'potential', 'field theory, scalar', 'density']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004332'],"['Continuing with previous works, we present a cosmological model in which dark matter and dark energy are modeled by scalar fields $\\Phi $ and $\\Psi$, respectively, endowed with the scalar potentials $V(\\Phi)=V_{o}[ \\cosh {(\\lambda \\sqrt{\\kappa_{o}}\\Phi)}-1] $ and $\\tilde{V}(\\Psi)=\\tilde{V_{o}}[ \\sinh {(\\alpha \\sqrt{\\kappa_{o}}\\Psi)}] ^{\\beta}$. This model contains 95% of scalar field. We obtain that the scalar dark matter mass is $m_{\\Phi}\\sim 10^{-26}eV.$ The solution obtained allows us to recover the success of the standard CDM. The implications on the formation of structure are reviewed. We obtain that the minimal cutoff radio for this model is $r_{c}\\sim 1.2 kpc.$']",['2000-04-25'] +673,['eng'],"['Bludman, Sidney A', 'Roos, M']",['Vacuum Energy'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'vacuum state, energy', 'quintessence', 'mass, asymptotic behavior', 'energy, ratio', 'Friedman model', 'density, low', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004328'],"[""For a flat universe presently dominated by static or dynamic vacuum energy, cosmological constant (LCDM) or quintessence (QCDM), we calculate the asymptotic collapsed mass fraction as function of the present ratio of smooth energy to matter energy $\\rat$. Identifying the normalized collapsed fraction as a conditional probability, we observe that the observed present ratio $\\rat \\sim 2$ is likely in LCDM, but more likely in QCDM. Inverse application of Bayes' Theorem implies that, in any fundamental theory, the prior for $\\rat$ must be essentially flat over the allowed range. This is consistent with a generic class of fundamental theories of initial conditions that are practically indifferent to $\\rat$. It does not demand the existence of potentially observable other universes.""]",['2000-04-25'] +674,['eng'],"['Ray, S', 'Dey, J', 'Dey, M']",['Density dependent strong coupling constant of QCD derived from compact star data'],['Astrophysics and Astronomy'],"['matter, compact', 'binary', 'matter, mass', 'matter, strangeness', 'quantum chromodynamics', 'strong interaction, coupling constant', 'dependence, density', 'quark, mass', 'symmetry, chiral', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004327'],"['The present work is an endeavour to connect the properties of tiny nearly massless objects with those of some of the most massive ones, the compact stars. Since 1996 there is major influx of X-ray and $\\gamma$ ray data from binary stars, one or both of which are compact objects that are difficult to explain as neutron stars since they contain a mass M in too small a radius R . The suggestion has been put forward that these are strange quark stars (SS) explainable in a simple model with chiral symmetry restoration (CSR) for the quarks and the M, R and other properties like QPOs (quasi periodic oscillations) in their X-ray power spectrum. It would be nice if this astrophysical data could shed some light on fundamental properties of quarks obeying QCD. One can relate the strong coupling constant of QCD, $\\alpha_s$ to the quark mass through the Dyson-Schwinger gap equation using the real time formalism of Dolan and Jackiw. This enables us to obtain the density dependence of $\\alpha_s$ from the simple CSR referred to above. This way fundamental physics, difficult to extract from other models like for example lattice QCD, can be constrained from present-day compact star data and may be put back to modelling the dense quark phase of early universe.']",['2000-04-25'] +675,['eng'],"['Barrow, John D', 'Bean, R', 'Magueijo, J']",['Can the Universe escape eternal acceleration?'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'vacuum state, energy', 'gravitation, antigravitation', 'matter, expansion', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004321'],"[""Recent astronomical observations of distant supernovae light-curves suggest that the expansion of the universe has recently begun to accelerate. Acceleration is created by an anti-gravitational repulsive stress, like that produced by a positive cosmological constant, or universal vacuum energy. It creates a rather bleak eschatological picture. An ever-expanding universe's future appears to be increasingly dominated by its constant vacuum energy. A universe doomed to accelerate forever will produce a state of growing uniformity and cosmic loneliness. Structures participating in the cosmological expansion will ultimately leave each others' horizons and information-processing must eventually die out. Here, we examine whether this picture is the only interpretation of the observations. We find that in many well-motivated scenarios the observed spell of vacuum domination is only a transient phenomenon. Soon after acceleration starts, the vacuum energy's anti-gravitational properties are reversed, and a matter-dominated decelerating cosmic expansion resumes. Thus, contrary to general expectations, once an accelerating universe does not mean always an accelerating universe.""]",['2000-04-25'] +676,['eng'],"['Fuller, G M', 'Pruet, J', 'Abazajian, K N']",['Can a Large Neutron Excess Help Solve the Baryon Loading Problem in Gamma-Ray Burst Fireballs?'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'gamma ray burst', 'fireball', 'baryon, transition', 'n, density', 'energy flow', 'n, matter', 'neutrino, oscillation', 'entropy', 'electron, yield', 'pi, production', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004313'],"['We point out that the baryon-loading problem in Gamma-Ray Burst (GRB) models can be amelioriated if a significant fraction of the baryons which inertially confine the electron/positron/photon fireball are converted to neutrons. A high neutron fraction in some circumstances can result in a reduced transfer of energy from relativistic light particles in the fireball to baryons. The energy needed to produce the required relativistic flow in the GRB is consequently reduced, in some cases by orders of magnitude. This could be relevant to GRB models because a high neutron-to-proton ratio has been found in neutron star-merger fireball environments. Significant neutron excess also could occur near condensed objects with high neutrino fluxes on account of matter-enhanced active-sterile neutrino transformation.']",['2000-04-24'] +677,['eng'],"['Leach, S M', 'Grivell, I J', 'Liddle, A R']",['Black hole constraints on the running-mass inflation model'],['Astrophysics and Astronomy'],"['inflationary universe', 'black hole, production', 'density, perturbation', 'potential', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004296'],"['The running-mass inflation model, which has strong motivation from particle physics, predicts density perturbations whose spectral index is strongly scale-dependent. For a large part of parameter space the spectrum rises sharply to short scales. In this paper we compute the production of primordial black holes, using both analytic and numerical calculation of the density perturbation spectra. Observational constraints from black hole production are shown to exclude a large region of otherwise permissible parameter space.']",['2000-04-21'] +678,['eng'],"['Cebrian, S', 'Coron, N', 'Dambier, G', 'García, E', 'González, D', 'Irastorza, I G', 'Leblanc, J', 'Marcillac, P', 'Morales, A', 'Morales, J', 'De Solorzano, A O', 'Peruzzi, A', 'Puimedón, J', 'Sarsa, M L', 'Scopel, S', 'Villar, J A']",['First results of the ROSEBUD Dark Matter experiment'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, search for', 'elastic scattering, nucleus WIMP', 'cross section, mass', 'bolometer, experimental results', 'deep underground detector']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004292'],"['Rare Objects SEarch with Bolometers UndergrounD) is an experiment which attempts to detect low mass Weak Interacting Massive Particles (WIMPs) through their elastic scattering off Al and O nuclei. It consists of three small sapphire bolometers (of a total mass of 100 g) with NTD-Ge sensors in a dilution refrigerator operating at 20 mK in the Canfranc Underground Laboratory. We report in this paper the results of several runs (of about 10 days each) with successively improved energy thresholds, and the progressive background reduction obtained by improvement of the radiopurity of the components and subsequent modifications in the experimental assembly, including the addition of old lead shields. Mid-term plans and perspectives of the experiment are also presented.']",['2000-04-21'] +679,['eng'],"['Rowell, G P', 'Naito, T', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, T', 'Holder, J', 'Kawachi, A', 'Kifune, T', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Roberts, M D', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['Observations of the supernova remnant W28 at TeV energies'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'supernova', 'flux, upper limit', 'Cherenkov counter, imaging', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004280'],"['The atmospheric Cerenkov imaging technique has been used to search for point-like and diffuse TeV gamma-ray emission from the southern supernova remnant, W28, and surrounding region. The search, made with the CANGAROO 3.8m telescope, encompasses a number of interesting features, the supernova remnant itself, the EGRET source 3EG J1800-2338, the pulsar PSR J1801-23, strong 1720 MHz OH masers and molecular clouds on the north and east boundaries of the remnant. An analysis tailored to extended and off-axis point sources was used, and no evidence for TeV gamma-ray emission from any of the features described above was found in data taken over the 1994 and 1995 seasons. Our upper limit (E>1.5 TeV) for a diffuse source of radius 0.25deg encompassing both molecular clouds was calculated at 6.64e-12 photons cm^-2 s^-1 (from 1994 data), and interpreted within the framework of a model predicting TeV gamma-rays from shocked-accelerated hadrons. Our upper limit suggests the need for some cutoff in the parent spectrum of accelerated hadrons and/or slightly steeper parent spectra than that used here (-2.1). As to the nature of 3EG J1800-2338, it possibly does not result entirely from pi-zero decay, a conclusion also consistent with its location in relation to W28.']",['2000-04-20'] +680,['eng'],"['Zdunik, J L', 'Bulik, T', 'Kluzniak, W', 'Haensel, P', 'Gondek-Rosinska, D']",['On the mass of moderately rotating strange stars in the MIT bag model and LMXBs'],['Astrophysics and Astronomy'],"['matter, strangeness', 'rotator', 'matter, mass', 'upper limit', 'strong interaction, coupling constant', 'bag model', 'energy, density', 'vacuum state', 'potential, chemical', 'mass, strangeness', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004278'],"['We compute the maximum mass of moderately rotating strange stars as a function of the strange quark mass, of the QCD coupling constant, $\\alpha_c$, and of the bag constant (vacuum energy density), $B$, in the MIT bag model of quark matter with lowest order quark-gluon interactions. For a fixed value of $B$, the maximum stellar mass depends only weakly on $\\alpha_c$, and is independent of this coupling in the limit of massless quarks. However, if it is the value of the chemical potential of quark matter at zero pressure which is held constant, for example at the value corresponding to the stability limit of nucleons against conversion to quark matter, the maximum mass of the strange star is higher by up to 25% for $\\alpha_c=0.6$, than for non-interacting quarks, and this may be relevant in the discussion of kHz QPO sources. The maximum mass of a non-rotating strange star could be sufficiently high to allow an orbital frequency as low as 1.0 kHz in the marginally stable orbit. However, for all $\\alpha_c<0.6$, the stellar mass cannot exceed $2.6M_\\odot$ at any rotational period $\\ge1.6 $ms.']",['2000-04-20'] +681,['eng'],"['Uzan, J P', 'Bernardeau, F']",['Cosmic Strings Lens Phenomenology'],['Astrophysics and Astronomy'],"['astrophysics, string', 'gravitation, lens', 'photon, beam', 'potential', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004105'],"['We reconsider the general properties of gravitational lensing effects induced by cosmic string systems, taking into account their equation of state and motion equations. We explicitly show that the deflection patterns induced by a string is equivalent to the one of a lineic and static distribution of matter. We then rigorously show that the convergence part of the deformation field is always zero, except on the intersection of the string worldsheet and the observer past light cone, extending previous results obtained in peculiar cases. Phenomenological consequences of this result on multiple image systems are investigated.']",['2000-04-10'] +682,['eng'],"['Bernardeau, F', 'Uzan, J P']",['Cosmic String Lens Phenomenology'],['Astrophysics and Astronomy'],"['astrophysics, string', 'lens', 'energy spectrum', 'critical phenomena', 'coherence, length', 'statistics', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004102'],"['We present a novel approach for investigating lens phenomenology of cosmic strings in order to elaborate detection strategies in galaxy deep field images. To account for the complexity of the projected energy distribution of string networks we assume their lens effects to be similar to those of a straight string carrying a {\\em random} lineic energy distribution. In such a model we show that, unlike the case of uniform strings, critical phenomena naturally appear. We explore the properties of the critical lines and caustics. In particular, assuming that the energy coherence length along the string is much smaller than the observation scale, we succeeded in computing the total length of critical lines per unit string length and found it to be $4/\\sqrt{3} {\\bf E}(3/4)$. The length of the associated caustic lines can also be computed to be $16/(\\pi \\sqrt{3}) {\\bf E}(3/4)$. The picture we obtain here for the phenomenology of cosmic string detection is clearly at variance with common lore.']",['2000-04-10'] +683,['eng'],"['Mavromatos, Nikolaos E']",['The Quest for Quantum Gravity'],['Astrophysics and Astronomy'],"['talk, Lake Louise 2000/02/20', 'quantum gravity, validity test', 'symmetry breaking, Lorentz', 'photon, velocity', 'photon, cosmic radiation', 'photon, energy', 'space-time, foam', 'optics', 'string model', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004225'],"[""I discuss some theoretical ideas concerning the representation of quantum gravity as a Lorentz-symmetry-violating `medium' with non-trivial optical properties, which include a refractive index in `vacuo' and stochastic effects associated with a spread in the arrival times of photons, growing linearly with the photon energy. Some of these properties may be experimentally detectable in future satellite facilities (e.g. GLAST or AMS), using as probes light from distant astrophysical sources such as gamma ray bursters. I also argue that such linear violations of Lorentz symmetry may not always be constrained by ultra-high-energy cosmic-ray data, as seems to be the case with a specific (stringy) model of space-time foam.""]",['2000-04-18'] +684,['eng'],"['Zhang, X']",['The Multiply Scattering Effect on the Energy Measurement of UHE Cosmic Rays using Atmospheric Fluorescence Technique'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, particle source', 'energy, measurement', 'multiple scattering, effect', 'showers, air', 'photon, emission', 'nitrogen', 'counters and detectors, fluorescence', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004173'],"[""Point sources in the atmosphere are surrounded by aureole because of atmospheric scattering. The properties of the time-dependent aureole radiance are calculated by use of a Monte Carlo approach and an iterative method. Since the aureole is particularly important in the ultraviolet, which is the region the Ultra-High-Energy (UHE) cosmic ray experiment using the air fluorescence technique like Fly's Eye or High-Resolution-Fly's-Eye(HiRes) are set in. The effect of the multiply scatteing on the energy measurement is studied.""]",['2000-04-13'] +685,['eng'],"['Erlykin, A D', 'Fatemi, S J', 'Wolfendale, A W']",['Fine Structure in the Energy Spectrum of Cosmic Ray Protons at 50 GeV?'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'p, cosmic radiation', 'cosmic radiation, energy spectrum', 'nucleus, cosmic radiation', 'electron, cosmic radiation', 'data analysis method', 'magnetic spectrometer, satellite', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004163'],"[""The recently published precise spectrum of cosmic ray protons from the Alpha Magnetic Spectrometer has been examined in some detail from the standpoint of a search for deviations from a smooth, simple, power law. We find a significant excess ($\\simeq$ 10% over $\\sim$ 0.3 interval in logE) centered on 50 GeV in the published data. It is possible that the 'unfolding technique' adopted by the experimenters causes an overestimate of the excess but it is difficult to reduce it much below about (5 $\\pm$ 3)%. We have examined other recent data, too. There is also evidence here, for an excess in the same energy region, although of only (1.6 $\\pm$ 0.9)%. A value of (3 $\\pm$ 1.5)% would be consistent with all the data. There are hints of similar excesses for heavier nuclei and electrons. Possible explanations are put forward for an excess, should it prove to be genuine.""]",['2000-04-13'] +686,['eng'],"['Riazuelo, A', 'Uzan, J P']",['Quintessence and Gravitational Waves'],['Astrophysics and Astronomy'],"['field theory, scalar', 'quintessence', 'gravitational radiation, energy loss', 'energy spectrum', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'potential', 'energy, density', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004156'],['We investigate some aspects of quintessence models with a non-minimally coupled scalar field and in particular we show that it can behave as a component of matter with $-3 \\lesssim P/\\rho \\lesssim 0$. We study the properties of gravitational waves in this class of models and discuss their energy spectrum and the cosmic microwave background anisotropies they induce. We also show that gravitational waves are damped by the anisotropic stress of the radiation and that their energy spectrum may help to distinguish between inverse power law potential and supergravity motivated potential. We finish by a discussion on the constraints arising from their density parameter $\\Omega_\\GW$.'],['2000-04-13'] +687,['eng'],"['Ng, S C C', 'Wiltshire, D L']",['Properties of cosmologies with dynamical pseudo Nambu-Goldstone bosons'],['Astrophysics and Astronomy'],"['astrophysics, model', 'Goldstone particle', 'quintessence', 'dynamical system, phase space', 'supernova, luminosity', 'quasar', 'gravitation, lens', 'energy, density', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004138'],"['We study observational constraints on cosmological models with a quintessence field in the form of a dynamical pseudo Nambu--Goldstone boson. After reviewing the properties of the solutions, from a dynamical systems phase space analysis, we consider the constraints on parameter values imposed by luminosity distances from the 60 Type Ia supernovae published by Perlmutter et al., and also from gravitational lensing statistics of distant quasars. In the case of the Type Ia supernovae we explicitly allow for the possibility of evolution of the peak luminosities of the supernovae sources, using simple empirical models which have been recently discussed in the literature. We find weak evidence to suggest that the models with supernovae evolution fit the data better in the context of the quintessence models in question. If source evolution is a reality then the greatest challenge facing these models is the tension between current value of the expansion age, H_0 t_0, and the fraction of the critical energy density, Omega_{phi0}, corresponding to the scalar field. Nonetheless there are ranges of the free parameters which fit all available cosmological data.']",['2000-04-12'] +688,['eng'],"['Armendariz-Picon, C', 'Mukhanov, V', 'Steinhardt, Paul Joseph']",['A Dynamical Solution to the Problem of a Small Cosmological Constant and Late-time Cosmic Acceleration'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'astrophysics, acceleration', 'field theory, scalar', 'pressure, <0', 'energy, density', 'matter, density', 'attractor', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004134'],"['Increasing evidence suggests that most of the energy density of the universe consists of a dark energy component with negative pressure, a ``cosmological constant"" that causes the cosmic expansion to accelerate. In this paper, we address the puzzle of why this component comes to dominate the universe only recently rather than at some much earlier epoch. We present a class of theories based on an evolving scalar field where the explanation is based entirely on internal dynamical properties of the solutions. In the theories we consider, the dynamics causes the scalar field to lock automatically into a negative pressure state at the onset of matter-domination such that the present epoch is the earliest possible time, consistent with nucleosynthesis restrictions, when it can start to dominate.']",['2000-04-12'] +689,['eng'],"['Tornkvist, O']",['Cosmic Magnetic Fields From Particle Physics'],['Astrophysics and Astronomy'],"['talk, Granlibakken 1999/12/10', 'particle physics, model', 'astrophysics', 'magnetic field, production', 'cosmic radiation, background', 'correlation, length', 'bubble, interaction']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004098'],['I review a number of particle-physics models that lead to the creation of magnetic fields in the early universe and address the complex problem of evolving such primordial magnetic fields into the fields observed today. Implications for future observations of the Cosmic Microwave Background (CMB) are briefly discussed.'],['2000-04-10'] +690,['eng'],"['González-Diáz, P F']",['Cosmological models from quintessence'],['Astrophysics and Astronomy'],"['astrophysics, model', 'quintessence', 'potential, scalar', 'luminosity', 'vacuum state']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004125'],"['A generalized quintessence model is presented which corresponds to a richer vacuum structure that, besides a time-dependent, slowly varying scalar field, contains a varying cosmological term. From first principles we determine a number of scalar-field potentials that satisfy the constraints imposed by the field equations and conservations laws, both in the conventional and generalized quintessence models. Besides inverse-power law solutions, these potentials are given in terms of hyperbolic functions or the twelve Jacobian elliptic functions, and are all related to the luminosity distance by means of an integral equation. Integration of this equation for the different solutions leads to a large family of cosmological models characterized by luminosity distance-redshift relations. Out of such models, only four appear to be able to predict a required accelerating universe conforming to observations on supernova Ia, at large or moderate redshifts.']",['2000-04-11'] +691,['eng'],"['Axenides, M', 'Floratos, Emmanuel G', 'Perivolaropoulos, L']",['Some Dynamical Effects of the Cosmological Constant'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'energy, vacuum state', 'gravitation, correction', 'galaxy', 'antigravitation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004080'],"[""Newton's law gets modified in the presence of a cosmological constant by a small repulsive term (antigarvity) that is proportional to the distance. Assuming a value of the cosmological constant consistent with the recent SnIa data ($\\Lambda \\simeq 10^{-52} m^{-2}$) we investigate the significance of this term on various astrophysical scales. We find that on galactic scales or smaller (less than a few tens of kpc) the dynamical effects of the vacuum energy are negligible by several orders of magnitude. On scales of 1Mpc or larger however we find that vacuum energy can significantly affect the dynamics. For example we show that the velocity data in the Local Group of galaxies correspond to galactic masses increased by 35% in the presence of vacuum energy. The effect is even more important on larger low density systems like clusters of galaxies or superclusters.""]",['2000-04-07'] +692,['eng'],"['Carroll, S M']",['The Cosmological Constant'],['Astrophysics and Astronomy'],"['review', 'astrophysics, fundamental constant', 'vacuum state, energy', 'Friedman model', 'supernova', 'cosmic radiation, background', 'matter, density', 'gravitation, lens', 'supersymmetry', 'string model', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004075'],"['This is a review of the physics and cosmology of the cosmological constant. Focusing on recent developments, I present a pedagogical overview of cosmology in the presence of a cosmological constant, observational constraints on its magnitude, and the physics of a small (and potentially nonzero) vacuum energy.']",['2000-04-07'] +693,['eng'],"['Torres, D F', 'Capozziello, S', 'Lambiase, G']",['Supermassive boson star at the galactic center? (15 pages)'],['Astrophysics and Astronomy'],"['galaxy', 'boson, matter', 'matter, scalar', 'matter, accretion', 'neutrino, matter', 'black hole', 'luminosity', 'effective potential', 'matter, mass', 'velocity, dispersion', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004064'],"['We explore whether supermassive non-baryonic stars (in particular boson, mini-boson and non-topological soliton stars) might be at the center of some galaxies, with special attention to the Milky Way. We analyze, from a dynamical point of view, what current observational data show, concluding that they are compatible with a single supermassive object without requiring it to be a black hole. Particularly, we show that scalar stars fit very well into these dynamical requirements. The parameters of different models of scalar stars necessary to reproduce the inferred central mass are derived, and the possible existence of boson particles with the adequate range of masses is commented. Accretion to boson stars is also analyzed, and a comparison with another non-baryonic candidate, a massive neutrino ball, which is also claimed as an alternative to the central black hole, is given. Both models are capable to explain the nature of the object in Sgr A$^*$ without invoking the presence of a singularity. One difficult issue is why the accreted materials will not finally produce, in a sufficiently long time, a black hole. We provide an answer based on stellar disruption in the case of boson stars, and comment several suggestions for its possible solution in neutrino ball scenarios. Finally, we discuss the prospects for the observational detection of these supermassive scalar objects, using the new generation of X-ray and radio interferometry satellites.']",['2000-04-06'] +694,['eng'],"['Tatsumi, T']",['Ferromagnetism of quark liquid and magnetars'],['Astrophysics and Astronomy'],"['n, matter', 'quark, liquid', 'magnetic field', 'model, ferromagnet', 'matter, magnetic', 'quark, strangeness', 'critical phenomena', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004062'],"['Spontaneous magnetization of quark liquid is examined on the analogy with that in electron gas. It is pointed out that quark liquid has potential to be ferromagnetic at rather low densities, around nuclear saturation density. Somme comments are given as for implications on magnetars.']",['2000-04-06'] +695,['eng'],"['Mücke, A', 'Protheroe, R J']",['A Proton Synchrotron Blazar Model for Flaring in Markarian~501'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'blazar, energy spectrum', 'synchrotron radiation', 'p, acceleration', 'photon nucleon, interaction', 'pi, photoproduction', 'pi, cascade decay', 'photon, cosmic radiation', 'muon, decay', 'energy loss', 'neutrino, cosmic radiation', 'neutrino, energy spectrum', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004052'],"['The spectral energy distribution (SED) of blazars typically has a double-humped appearance usually interpreted in terms of synchrotron self-Compton models. In proton blazar models, the SED is instead explained in terms of acceleration of protons and subsequent cascading. We discuss a variation of the Synchrotron Proton Blazar model, first proposed by M\\""ucke & Protheroe (1999), in which the low energy part of the SED is mainly synchrotron radiation by electrons co-accelerated with protons which produce the high energy part of the SED mainly asproton synchrotron radiation. We assume shock acceleration, and consider the case where the maximum energy of the accelerated protons is above the threshold for pion photoproduction interactions on the synchrotron photons of the low energy part of the SED. Using a Monte Carlo/numerical technique to simulate the interactions and subsequent cascading of the accelerated protons, we are able to fit the observed SED of Markarian 501 during the April 1997 flare. We find that the emerging cascade spectra initiated by gamma-rays from $\\pi^0$ decay and by $e^\\pm$ from $\\mu^\\pm$ decay turn out to be relatively featureless. Synchrotron radiation produced by $\\mu^\\pm$ from $\\pi^\\pm$ decay, and even more importantly by protons, and subsequent synchrotron-pair cascading, is able to reproduce well the high energy part of the SED. For this fit we find that synchrotron radiation by protons dominates the TeV emission, pion photoproduction being less important with the consequence that we predict a lower neutrino flux than in other proton blazar models.']",['2000-04-05'] +696,['eng'],"['Mohapatra, R N', 'Teplitz, V L']",['Mirror Dark Matter'],['Astrophysics and Astronomy'],"['talk, Granlibakken 1999/12/10', 'talk, Marina del Rey 2000/02/23', 'astrophysics, missing-mass', 'matter, density', 'model, mirror', 'asymmetry', 'nucleon, mirror', 'mass, solar', 'MACHO', 'galaxy']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004046'],"['There appear to be three challenges that any theory of dark matter must face: (i) why is $\\Omega_{DM}$ of the same order as $\\Omega_{Baryons}$ ? (ii) what are the near solar mass objects ($\\sim 0.5 M_{\\odot}$) observed by the MACHO microlensing project ? and (iii) understanding the shallow core density profile of the halos of dwarf as well as low surface brightness galaxies. The popular cold dark matter candidates, the SUSY LSP and the axion fail to meet these challenges. We argue that in the mirror model suggested recently to explain the neutrino anomalies, the mirror baryons being 15-20 times heavier than familiar baryons, can play the role of the cold dark matter and provide reasonable explanation of all three above properties without extra assumptions.']",['2000-04-05'] +697,['eng'],"['Mikheeva, E V', 'Lukash, V N', 'Arkhipova, N A', 'Malinovsky, A M']",['Current status of cosmological MDM model'],['Astrophysics and Astronomy'],"['talk, Les Arcs 2000/01/22', 'Friedman model', 'gravitational radiation, background', 'density, perturbation', 'spectra, perturbation', 'galaxy, cluster', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0004034'],"['An analysis of cosmological models in spatially flat Friedmann Universe with cosmic gravitational wave background and zero $\\Lambda$-term is presented. The number of free parameters is equal to 5, they are $\\sigma_8$, $n$, $\\Omega_\\nu$, $\\Omega_b$, and $h$. The normalization of the spectrum of density perturbations on galaxy cluster abundance ($\\sigma_8 = 0.52\\pm 0.04$) has been used to calculate numerically the value of the large scale CMB anisotropy ($\\ell\\simeq 10$) and the relative contribution of cosmological gravitational waves T/S. Increasing $\\Omega_\\nu$ weaken the requirements to the value of T/S, however even for $\\Omega_\\nu\\le 0.4$ the models with $h+n\\ge 1.5$ suggest considerable abundance of gravitational waves: T/S${}^>_\\sim 0.3$. In models with $\\Omega_\\nu\\le 0.4$ and scale-invariant spectrum of density perturbations ($n=1$): T/S${}^>_\\sim 10(h-0.47)$. Minimization of the value T/S is possible only in the range of the red spectra ($n<1$) and small $h$ ($<0.6$). It is shown that the models with T/S$\\in [0, 3]$ admit both moderate red and blue spectra of density perturbations, $n\\in[0.9,1.2]$, with rather high abundance hot dark matter, $\\Omega_\\nu\\in [0.2,0.4]$. Any condition, $n<0.9$ or $\\Omega_\\nu<0.2$, decreases the relative amplitude of the first acoustic peak for more than 30% in comparison with its hight in the standard CDM normalized by COBE data.']",['2000-04-05'] +698,['eng'],"['Rosenberg, D E']",['Quintessence as Unrecaptured Matter from a Universe Bounce'],['Astrophysics and Astronomy'],"['astrophysics, model', 'relativity theory, general', 'n, matter', 'energy loss', 'cosmic radiation, background', 'galaxy, production', 'baryon, density', 'quintessence', 'photon, accretion', 'black hole', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003464'],"['Since the universe is accelerating due to a negative vacuum energy, there is great difficulty fitting this into an inflation picture. Using a 160 MeV bounce model, the negative energy can be due to matter remaining outside the universe. For a bounce, collapse to infinite density states must be prevented by energy losses at supranuclear densities. Most other big bang problems are solvable with this model.']",['2000-04-03'] +699,['eng'],"['Kennedy, Dallas C']",['Cosmic Ray Antiprotons'],['Astrophysics and Astronomy'],"['talk, Granlibakken 1999/12/10', 'anti-p, cosmic radiation', 'cosmic radiation, secondary radiation', 'cosmic radiation, particle source', 'violation, CPT', 'cosmic radiation, spectra', 'proposed experiment', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003485'],"['Cosmic ray antiprotons have been detected for over 20 years and are now measured reliably. Standard physics predicts a spectrum and abundance of secondary antiprotons consistent with all current measurements, placing limits on non-standard antiproton properties and soon on exotic Galactic antiproton sources. Future experiments and theoretical developments are discussed.']",['2000-04-03'] +700,['eng'],"['Stanev, T', 'Engel, R', 'Mücke, A', 'Protheroe, R J', 'Rachen, J P']",['Propagation of ultra-high energy protons in the nearby universe'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'p, tracks', 'magnetic field, random', 'photon nucleon, interaction', 'p, energy loss', 'p, injection', 'p, time delay', 'angular distribution', 'cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'correlation', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003484'],"['We present a new calculation of the propagation of protons with energies above $10^{19}$ eV over distances of up to several hundred Mpc. The calculation is based on a Monte Carlo approach using the event generator SOPHIA for the simulation of hadronic nucleon-photon interactions and a realistic integration of the particle trajectories in a random extragalactic magnetic field. Accounting for the proton scattering in the magnetic field affects noticeably the nucleon energy as a function of the distance to their source and allows us to give realistic predictions on arrival energy, time delay, and arrival angle distributions and correlations as well as secondary particle production spectra.']",['2000-04-03'] +701,['eng'],"['Ray, S', 'Dey, J', 'Dey, M', 'Ray, K', 'Samanta, B C']",['Entropy and equation of state for dense hot quark matter and its effect on compact quark stars'],['Astrophysics and Astronomy'],"['quark, matter', 'matter, strangeness', 'quark, mass', 'symmetry, chiral', 'quark antiquark, potential', 'entropy', 'energy, density', 'pressure', 'quark hadron, transition', 'finite temperature', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003472'],"['Dey et al. derived an equation of state (EOS) for matter in strange stars (SS) with quark masses showing chiral symmetry restoration (CSM) and an interquark potential which (i) has asymptotic freedom built into it, (ii) shows confinement at zero density ($\\rho_B = 0$) and deconfinement at high $\\rho_B$. This EOS gives a stable configuration for chargeless, $\\be$-stable quark matter. The SS derived from this EOS fits into the empirical mass -radius (M-R) relations of some stars constraining the CSM parameters. In the present paper we extend the calculation to include high temperatures upto T = 10 MeV \\equiv 1.16 \\times 10^{11}^oK where the quark gas is still degenerate and find that the empirical M-R relation, derived from astrophysical data, is still satisfied. The EOS is tabulated for T = 10 MeV. The entropy is calculated and matches onto that calculated from hadronic models thus supporting the idea that the quark-hadron transition may be continuous.']",['2000-04-03'] +702,['eng'],"['Cline, David B', 'Stecker, F W']",['Exploring the Ultrahigh Energy Neutrino Universe'],['Astrophysics and Astronomy'],"['talk, Los Angeles 1999/11/01', 'neutrino, cosmic radiation', 'gamma ray burst', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'showers, air', 'signal processing, fluorescence', 'radiation, Cherenkov', 'photon, cosmic radiation', 'galaxy, AGN', 'neutrino, oscillation', 'grand unified theory', 'inflationary universe', 'counters and detectors, proposed', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003459'],"['Astronomy at the highest energies observed must be performed by studying neutrinos rather than photons because the universe is opaque to photons of these energies. By making observations of neutrinos with energies above 10 EeV one can deduce information about the distribution and cosmological history of cosmic rays which may have been accelerated to energies above 100 EeV. Very large fluxes of neutrinos at these energies which exhibit a hard spectrum would be evidence of a GUT phase transition or superheavy dark matter particles. Neutrinos at energies around a PeV may be produced in observable quantities in active galaxies from the acceleration and interactions of cosmic rays in the vicinity of massive black holes or in relativistic jets produced by these black holes. Cosmological gamma-ray bursts may also produce PeV neutrinos. Neutrinos at these energies may oscillate into tau neutrinos which can travel through the Earth by the process of regeneration and produce upward moving air-showers. Neutrinos of energies above of 1000 EeV can produce ultrahigh energy cosmic rays thorugh interactions with big-bang neutrinos, producing Z bosons. This ""Z-burst"" phenomenon can be used to study the mass and distribution of big-bang neutrinos.']",['2000-03-31'] +703,['eng'],"['Covi, L']","['Inflation models, spectral index and observational constraints']",['Astrophysics and Astronomy'],"['talk, Les Arcs 2000/01/22', 'inflationary universe', 'astrophysics, missing-mass', 'mass, inflaton', 'cosmic radiation, background', 'Hubble constant', 'matter, density', 'ionization', 'numerical calculations, interpretation of experiments']","['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003458', 'http://documents.cern.ch/archive/electronic/other/uploader/MORIOND/covi']","['We have evaluated the observational constraints on the spectral index $n$, in the context of a $\\Lambda$CDM model. For $n$ scale-independent, as predicted by most models of inflation, present data require $n\\simeq 1.0 \\pm 0.1$ at the 2-$\\sigma$ level. We have also studied the two-parameter scale-dependent spectral index, predicted by running-mass inflation models. Present data allow significant variation of $n$ in this case, within the theoretically preferred region of parameter space.']",['2000-03-31'] +704,['eng'],"['Hanhart, C', 'Phillips, D R', 'Reddy, S']",['Neutrino and axion emissivities of neutron stars from nucleon-nucleon scattering data'],['Astrophysics and Astronomy'],"['n, matter', 'nucleon nucleon, interaction', 'neutrino, hadroproduction', 'axion, hadroproduction', 'bremsstrahlung', 'exchange, one-pion', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003445'],"['Neutrino and axion production in neutron stars occurs mainly as bremsstrahlung from nucleon-nucleon (NN) scattering. The energy radiated via neutrinos or axions is typically very small compared to other scales in the two-nucleon system. The rate of emission of such ""soft"" radiation is directly related to the on-shell NN amplitude, and thereby to the NN experimental data. This facilitates the model-independent calculation of the neutrino and axion radiation rates which is presented here. We find that the resultant rates are a factor of one half to one fifth below earlier estimates based on a one-pion-exchange NN amplitude.']",['2000-03-30'] +705,['eng'],"['Moffat, J W']",['New Developments in Cosmology'],['Astrophysics and Astronomy'],"['talk, Villefranche-sur-Mer 2000/01/03', 'astrophysics, model', 'matter, density', 'Hubble constant', 'gravitation, model', 'light cone, multiple', 'inflationary universe', 'photon, velocity']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003444'],['A brief review is given of the present observational data in cosmology. A review of a new bimetric gravity theory with multiple light cones is presented. The physical consequences of this gravity theory for the early universe are analyzed.'],['2000-03-30'] +706,['eng'],"['Pryke, C L']",['A Comparative Study of the Depth of Maximum of Simulated Air Shower Longitudinal Profiles'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'iron', 'showers, air', 'showers, spatial distribution', 'energy spectrum, cosmic radiation', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003442'],"['A comparative study of simulated air shower longitudinal profiles is presented. An appropriate thinning level for the calculations is first determined empirically. High statistics results are then provided, over a wide energy range, (10^14.0 to 10^20.5 eV), for proton & iron primaries, using four combinations of the MOCCA & CORSIKA program frameworks, and the SIBYLL & QGSJET high energy hadronic interaction models. These results are compared to existing experimental data. The way in which the first interaction controls Xmax is investigated, as is the distribution of Xmax.']",['2000-03-30'] +707,['eng'],"['Baudis, L', 'Klapdor-Kleingrothaus, H V']",['GENIUS'],['Astrophysics and Astronomy'],"['talk, Ringberg Castle 1999/06/06', 'neutrino, solar', 'p p, interaction', 'neutrino/e, hadroproduction', 'neutrino, counters and detectors', 'germanium', 'neutrino, oscillation', 'neutrino electron, elastic scattering', 'deep underground detector, proposed', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003435'],"['The GENIUS project is a proposal for a large supersensitive Germanium detector system for WIMP and double beta decay searches with a much increased sensitivity relative to existing and other future experiments. In this paper, the possibility to detect low energy solar neutrinos with GENIUS in real-time through elastic neutrino-electron scattering is studied.']",['2000-03-30'] +708,['eng'],"['Baudis, L', 'Klapdor-Kleingrothaus, H V']",['Direct Detection of Nonbaryonic Dark Matter'],['Astrophysics and Astronomy'],"['talk, Ringberg Castle 1999/06/06', 'astrophysics, missing-mass', 'WIMP, search for', 'semiconductor detector, germanium', 'scattering, nucleon WIMP', 'total cross section, mass', 'spin, dependence', 'proposed experiment', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003434'],"['Weakly Interacting Massive Particles (WIMPs) are leading candidates for the dominant part of the mass density of the Universe. Here we will review direct WIMP detection techniques by giving examples of currently running experiments, and present the status of the most promising future projects.']",['2000-03-30'] +709,['eng'],"['Glendenning, N K', 'Weber, F']",['Possible Evidence of Quark Matter in Neutron-Star X-Ray Binaries'],['Astrophysics and Astronomy'],"['n, matter', 'binary', 'spin, dependence', 'quark, matter', 'quark, confinement', 'matter, accretion', 'critical phenomena', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003426'],"[""The distribution of matter and the moment of inertia of millisecond pulsars and of neutron stars that are accreting matter from a low-mass companion, change over time with changing centrifugal force. These changes are especially pronounced if a phase transition occurs as a result of internal density changes. In this paper, we study the spin evolution of X-ray neutron stars in binary systems, which are being spun up by mass transfer from accretion disks. Our investigation reveals that quark deconfinement induced by the changing spin, can lead to a pronounced plateau in the star's spin frequency. This finding provides a possible explanation for the anomalous frequency distribution of neutron stars in low-mass X-ray binaries, which all lie in a rather narrow band.""]",['2000-03-29'] +710,['eng'],"['Buniy, R V', 'Ralston, J P']",['Radio Detection of High Energy Particles'],['Astrophysics and Astronomy'],"['cosmic radiation, measurement', 'radiation, Cherenkov', 'showers, electromagnetic', 'form factor', 'charge', 'effect, coherence', 'saddle-point approximation', 'causality', 'electric field', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003408'],"['Radio Cherenkov emission underlines detection of high energy particles via a signal growing like the particle-energy-squared. Cosmic ray-induced electromagnetic showers are a primary application. While many studies have treated the phenomenon approximately, none have attempted to incorporate all the physical scales involved in problems with time- or spatially- evolving charges. We find it is possible to decompose the calculated fields into the product of a form factor, characterizing a moving charge distribution, multiplying a general integral which depends on the charge evolution. In circumstances of interest for cosmic ray physics, the resulting expressions can be evaluated explicitely in terms of a few parameters obtainable from shower codes. The classic issues of Frauhofer and Fresnel zones play a crucial role in the coherence.']",['2000-03-28'] +711,['eng'],"['Digel, S W', 'Moskalenko, I V', 'Ormes, J F', 'Sreekumar, P', 'Williamson, R']",['What can GLAST say about the origin of cosmic rays in other galaxies?'],['Astrophysics and Astronomy'],"['talk, Indian Wells 2000/01/05', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'galaxy', 'proposed experiment', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003407'],"['Gamma rays in the band from 20 MeV to 300 GeV, used in combination with data from radio and X-ray bands, provide a powerful tool for studying the origin of cosmic rays in our sister galaxies Andromeda and the Magellanic Clouds. Gamma-ray Large Area Space Telescope (GLAST) will spatially resolve these galaxies and measure the spectrum and intensity of diffuse gamma radiation from the collisions of cosmic rays with gas and dust in them. Observations of Andromeda will give an external perspective on a spiral galaxy like the Milky Way. Observations of the Magellanic Clouds will permit a study of cosmic rays in dwarf irregular galaxies, where the confinement is certainly different and the massive star formation rate is much greater.']",['2000-03-28'] +712,['eng'],"['Matos, T', 'Guzmán, F', 'Núñez, D']",['Spherical Scalar Field Halo in Galaxies'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'field theory, scalar', 'symmetry, rotational', 'galaxy', 'fluctuation', 'tensor, energy-momentum']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003398'],['We study a spherically symmetric fluctuation of scalar dark matter in cosmos and show that it could be the dark matter in galaxies. The local space-time of the fluctuation contains a three dimensional space-like hypersurface with surplus of angle.'],['2000-03-28'] +713,['eng'],"['Goncharov, Yu P', 'Firsova, N E']",['Increase of the pion-kaon Hawking radiation from Schwarzschild black holes by Dirac monopoles'],['Astrophysics and Astronomy'],"['black hole, Schwarzschild', 'radiation, Hawking', 'magnetic monopole, Dirac', 'radiation, luminosity', 'pi, radiation', 'K, radiation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003375'],['An algorithm for numerical computation of the barrier transparency for the potentials surrounding Schwarzschild black holes is described for massive scalar particles. It is then applied to calculate the total (including all particle species and the contributions of twisted field configurations connected with Dirac monopoles) luminosity for the pion-kaon Hawking radiation from a Schwarzschild black hole with mass $M=10^{12}$ g. It is found that the contribution due to monopoles can be of order 11% of the total pion-kaon luminosity.'],['2000-03-27'] +714,['eng'],"['Battaner, E', 'Lesch, H']",['On the Physics of Primordial Magnetic Fields'],['Astrophysics and Astronomy'],"['inflationary universe', 'magnetic field, galaxy', 'magnetic field, production', 'critical phenomena', 'coherence', 'radiation', 'proposed experiment', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003370'],"['There are at present more then 30 theories about the origin of cosmic magnetic fields at galactic and intergalactic scales. Most of them rely on concepts of elementary particle physics, like phase transitions in the early Universe, string theory and processes during the inflationary epoch. Here we present some more astrophysical arguments to provide some guidance through this large number and variety of models. Especially the fact that the evolution of magnetic fields depends on the spatial coherence scale of the fields leds to some interesting conclusions, which may rule out the majority of the theoretical scenarios. In principle one has to distinguish between the large-scale and small-scale magnetic fields. Large scale fields are defined as those as becoming sub-horizon at that redshift at which the mass energy density becomes equal to the photon energy density, which we name as equality. Small scale fields which are sub-horizon even before equality, i.e. with scales lower than (present) few Mpc cannot survive the radiation era and cannot reach recombination, because of the effects of magnetic diffusion and photon diffusion. Therefore mechanisms based on phase transitions become unlike, as they provide magnetic fields on scales smaller than the horizon. Thus, the observed galactic and intergalactic fields, which are small scales in our terminology must be created after recombination by normal plasma processes during the protogalactic evolution. The large scale fields instead were produced during inflation and may have noticeable implications for the formation of the large scale structure of the Universe. The inclusion of large scale magnetic fields may improve present Cold Dark Matter theories of structure formation.']",['2000-03-27'] +715,['eng'],"['Hu, W', 'Barkana, R', 'Gruzinov, A V']",['Cold and Fuzzy Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'fuzzy', 'scalar particle', 'perturbation, linear', 'scaling', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003365'],"['Cold dark matter (CDM) models predict small-scale structure in excess of observations of the cores and abundance of dwarf galaxies. These problems might be solved, and the virtues of CDM models retained, even without postulating {\\it ad hoc} dark matter particle or field interactions, if the dark matter is composed of ultra-light scalar particles (m ~ 10^{-22}eV), initially in a (cold) Bose-Einstein condensate, similar to axion dark matter models. The wave properties of the dark matter stabilize gravitational collapse providing halo cores and sharply suppressing small-scale linear power.']",['2000-03-27'] +716,['eng'],"['Urena-Lopez, L A', 'Matos, T']",['A new cosmological tracker solution for Quintessence'],['Astrophysics and Astronomy'],"['inflationary universe', 'potential', 'quintessence', 'field theory, scalar', 'asymptotic behavior', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003364'],"['In this paper we propose a quintessence model with the potential $V(\\Phi )=V_{o}[ \\sinh {(\\alpha \\sqrt{\\kappa_{o}}\\Delta \\Phi})] ^{\\beta}$, which asymptotic behavior corresponds to an inverse power-law potential at early times and to an exponential one at late times. We demonstrate that this is a tracker solution and that it could have driven the Universe into its current inflationary stage. The exact solutions and the description for a complete evolution of the Universe are also given. We compare such model with the current cosmological observations.']",['2000-03-24'] +717,['eng'],"['Durrer, R']",['Cosmological Strucure Formation with Topological Defects'],['Astrophysics and Astronomy'],"['astrophysics, string', 'topology, defect', 'critical phenomena', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'inflationary universe', 'decoherence', 'numerical calculations, interpretation of experiments']","['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003363', 'http://documents.cern.ch/archive/electronic/other/uploader/MORIOND/durrer']","[""Structure formation with topological defects is described. The main differences from inflationary models are highlighted. The results are compared with recent observations. It is concluded that all the defect models studied so far are in disagreement with recent observations of CMB anisotropies. Furthermore, present observations do not support 'decoherence', a generic feature of structure formation from topological defects.""]",['2000-03-24'] +718,['eng'],"['Palomba, C']",['Detectability of Gravitational Radiation from Prompt and Delayed Star Collapse to a Blackhole'],['Astrophysics and Astronomy'],"['gravitational radiation, measurement', 'matter, massive', 'black hole, mass spectrum', 'n, matter', 'signal processing', 'background', 'counters and detectors, interference', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003321'],"[""We consider the emission of gravitational waves in the two proposed models for the collapse of a massive star to a black hole: the prompt collapse, in which the interior of the star collapses to a black hole in a dynamical time scale, and the delayed collapse, in which a light black hole, or a neutron star, forms at the beginning. It then accretes matter, due to the fall-back, achieving in the neutron star case the critical mass for black hole formation, until the final black hole mass is reached. We calculate the ``effective'' black hole mass distribution in both cases and estimate the detectability of the gravitational waves emitted, discussing the differences. We show that, due to the slowness of fall-back, the main burst of gravitational radiation is emitted, in the delayed collapse, according to the parameters of the initial, light, black hole. As a consequence, it is less detectable than the ``average'' prompt collapse, due to the higher characteristic frequency of the signals. Nevertheless, both kinds of collapse are not particularly suited for the detection by present resonant detectors and forthcoming interferometers.""]",['2000-03-23'] +719,['eng'],"['Alvarez-Muñiz, J', 'Vázquez, R A', 'Zas, E']",['Calculation Methods for Radio Pulses from High Energy Showers'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'radiation, Cherenkov', 'showers, electromagnetic', 'showers, hadronic', 'angular distribution', 'spectra, parametrization', 'neutrino, cosmic radiation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003315'],"['We present an approximation for the numerical calculation of Cherenkov radio pulses in the Fraunhofer limit from very high energy showers in dense media. We compare it to full Montecarlo simulations in ice studying its range of applicability and show how it can be extended with a simple algorithm. The approximation reproduces well the angular distribution of the pulse around the Cherenkov direction. An improved parameterization for the frequency spectrum in the Cherenkov direction is given for phenomenolgical applications. We extend the method to study the pulses produced by showers at distances at which the Fraunhofer limit does not apply, and give the ranges of distances and frequencies in which Fraunhofer approximation is good enough for interpreting future experimental data. Our results are relevant for the detection of very high energy neutrinos with this technique.']",['2000-03-23'] +720,['eng'],"['Rachen, J P']",['Hadronic blazar models and correlated X-ray/TeV flares'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'cosmic radiation, particle source', 'jet, AGN', 'spectra, blazar', 'model, hadronic', 'model, leptonic', 'synchrotron radiation, cascade', 'cosmic radiation, acceleration', 'electron, cosmic radiation', 'pi, cosmic radiation', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003282'],"['The hypothesis that AGN jets might be the sources of the ultra-high energy cosmic rays has originally motivated the venture of TeV gamma ray astronomy. Surprisingly, after the discovery of TeV emission from blazars the attention has shifted to more traditional explanations which do not involve energetic hadrons, and there is even common believe that a hadronic interpretation is disfavored by observations. It is shown here that this is not the case, and that the currently observed spectra and variability features of blazars can be perfectly understood within hadronic blazar models. I also discuss how hadronic models might be observationally distinguished from common leptonic models, and point out some interesting aspects which could be relevant for the understanding of the differences between blazar classes.']",['2000-03-24'] +721,['eng'],"['Ormes, J F', 'Digel, S W', 'Moskalenko, I V', 'Moiseev, A', 'Williamson, R']",['The origin of cosmic rays'],['Astrophysics and Astronomy'],"['talk, Indian Wells 2000/01/05', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'p, cosmic radiation', 'cosmic radiation, acceleration', 'pi0, radiative decay', 'counters and detectors, satellite', 'resolution', 'numerical calculations', 'proposed experiment']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003270'],"['Gamma rays in the band from 30 MeV to 300 GeV, used in combination with direct measurements and with data from radio and X-ray bands, provide a powerful tool for studying the origin of Galactic cosmic rays. Gamma-ray Large Area Space Telescope (GLAST) with its fine 10-20 arcmin angular resolution will be able to map the sites of acceleration of cosmic rays and their interactions with interstellar matter. It will provide information that is necessary to study the acceleration of energetic particles in supernova shocks, their transport in the interstellar medium and penetration into molecular clouds.']",['2000-03-24'] +722,['eng'],"['Le Bohec, S', 'Bond, I H', 'Bradbury, S M', 'Buckley, J H', 'Burdett, A M', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Dunlea, S', ""D'Vali, M"", 'Fegan, D J', 'Fegan, S J', 'Finley, J P', 'Gaidos, J A', 'Hall, T A', 'Hillas, A M', 'Horan, D', 'Knapp, J', 'Krennrich, F', 'Lessard, R W', 'Macomb, D J', 'Masterson, C', 'Quinn, J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Vasilev, V', 'Weekes, T C']",['$\\gamma$-ray Observations of the Galactic Plane at Energies E > 500 GeV'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'upper limit', 'cosmic radiation, angular distribution', 'Cherenkov counter, imaging', 'experimental results', '> 500 GeV']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003265'],"['In 1998 and 1999 the Whipple Observatory 10 m telescope was used to search for diffuse gamma ray emission from the Galactic Plane. No signifiant evidence of emission was found. Assuming the TeV emission profile matches EGRET observations above 1 GeV with a differential spectral index of 2.4, we derive an upper limit of {$\\rm {3.0\\cdot10^{-8}cm^{-2}s^{-1}sr^{-1}}$} for the average diffuse emission above {{$\\rm500 GeV$}} in the galactic latitude range from {{$\\rm-2^o$ to $\\rm +2^o$}} at galactic longitude {{$\\rm 40^o$}}. Comparisons with EGRET observations provide a lower limit of 2.31 for the differential spectral index of the diffuse emission, assuming there is no break in the spectrum between 30 GeV and 500 GeV. This constrains models for diffuse emission with a significant inverse Compton contribution.']",['2000-03-24'] +723,['eng'],"['Pina-Avelino, P', 'Martins, C J A P']",['Topological defects'],['Astrophysics and Astronomy'],"['defect, topological', 'astrophysics, anisotropy', 'domain wall, network', 'scaling', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003231'],"['We consider the evolution of domain walls produced during an anisotropic phase in the very early universe, showing that the resulting network can be very anisotropic. If the domain walls are produced during an inflationary era, the network will soon freeze out in comoving coordinates retaining the imprints of the anisotropic regime, even though inflation makes the universe isotropic. Only at late times, when the typical size of the major axis of the domain walls becomes smaller than the Hubble radius, does the network evolve rapidly towards isotropy. Hence, we may hope to see imprints of the anisotropic era if by today the typical size of the major axis of the domain walls is of the order of the Hubble radius, or if the walls re-entered it only very recently. Depending on the mass scale of the domain walls, there is also the possibility that they re-enter at earlier times, but their evolution remains friction-dominated until recently, in which case the signatures of the anisotropic era will be much better preserved. These effects are expected to occur in generic topological defect models.']",['2000-03-17'] +724,['eng'],"['Skalsky, V']",['The only non-contradictory model of universe'],['Astrophysics and Astronomy'],"['Friedman model', 'relativity theory, general', 'mechanics, classical', 'quantum mechanics', 'space-time', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003192'],"['The Friedmann equations of universe dynamics describe the infinite number of the Friedmannian models of universe. The consistent and distinguished relativistic, classical-mechanical, quantum-mechanical and formal-logical analysis of the Friedmannian universe models leads to a surprising and unexpected conclusion: The Friedmannian model of the flat expansive homogeneous and isotropic universe with the zero gravitational force state equation is the only model of universe, which does not contradict the: 1st Einstein general theory of relativity (and its special partial solutions: the Einstein special theory of relativity and the Newton theory of gravitation); 2nd quantum mechanics; 3rd fundamental formal principles of logical thinking; and 4th observations.']",['2000-03-15'] +725,['eng'],"['Fowler, J W', 'Fortson, Lucy F', 'Jui, C', 'Kieda, D B', 'Ong, R A', 'Pryke, C L', 'Sommers, P']",['A Measurement of the Cosmic Ray Spectrum and Composition at the Knee'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'elements, cosmic radiation', 'mass spectrum, primary', 'showers, air', 'radiation, Cherenkov', 'scintillation counter', 'Cherenkov counter, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003190'],"['The energy spectrum and primary composition of cosmic rays with energy between $3\\times 10^{14}$ and $3\\times10^{16}\\unit{eV}$ have been studied using the CASA-BLANCA detector. CASA measured the charged particle distribution of air showers, while BLANCA measured the lateral distribution of Cherenkov light. The data are interpreted using the predictions of the CORSIKA air shower simulation coupled with four different hadronic interaction codes. The differential flux of cosmic rays measured by BLANCA exhibits a knee in the range of 2--3 PeV with a width of approximately 0.5 decades in primary energy. The power law indices of the differential flux below and above the knee are $-2.72\\pm0.02$ and $ -2.95\\pm0.02$. We present our data both as a mean depth of shower maximum and as a mean nuclear mass. A multi-component fit using four elemental species shows the same composition trends given by the mean quantities, and also indicates that QGSJET and VENUS are the preferred hadronic interaction models. We find that an initially mixed composition turns lighter between 1 and 3 PeV, and then becomes heavier with increasing energy above 3 PeV.']",['2000-03-15'] +726,['eng'],"['Lima, J A S', 'Alcaniz, J S']",['Angular size in quintessence cosmology'],['Astrophysics and Astronomy'],"['quintessence', 'astrophysics, model', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003189'],"['We investigate the influence of an exotic fluid component (""quintessence"") on the angular size-redshift relation for distant extragalactic sources. Particular emphasis is given for the redshif $z_{m}$ at which the angular size takes its minimal value. We derive an analytical closed form which determines how $z_m$ depends on the parameter of the equation of state describing the exotic component. The results for a flat model dominated by a ""quintessence"" are compared in detail with the ones for the standard open model dominated by cold dark matter. Some consequences of systematic evolutionary effects on the values of $z_{m}$ are also briefly discussed. It is argued that the critical redshift, for all practical purposes, may completely be removed if such effects are taken into account.']",['2000-03-14'] +727,['eng'],"['Ellison, D C', 'Berezhko, E G', 'Baring, M G']",['Nonlinear Shock Acceleration and Photon Emission in Supernova Remnants'],['Astrophysics and Astronomy'],"['supernova', 'electron, acceleration', 'model, nonlinear', 'electron, injection', 'acceleration, shock waves', 'photon, cosmic radiation', 'photon, emission', 'bremsstrahlung', 'synchrotron radiation', 'Compton scattering', 'pi, decay', 'magnetic field', 'phase space', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003188'],"['We have extended a simple model of nonlinear diffusive shock acceleration (Berezhko and Ellison 1999) to include the injection and acceleration of electrons and the production of photons from bremsstrahlung, synchrotron, inverse-Compton, and pion-decay processes. We argue that the results of this model, which is simpler to use than more elaborate ones, offer a significant improvement over test-particle, power-law spectra which are often used in astrophysical applications of diffusive shock acceleration. With an evolutionary supernova remnant (SNR) model to obtain shock parameters as functions of ambient interstellar medium parameters and time, we predict broad-band continuum photon emission from supernova remnants in general, and SN1006 in particular, showing that our results compare well with the more complete time-dependent and spherically symmetric nonlinear model of Berezhko, Ksenofontov, and Petukhov (1999). We discuss the implications nonlinear shock acceleration has for X-ray line emission, and use our model to describe how ambient conditions determine the TeV/radio flux ratio, an important parameter for gamma-ray observations of radio SNRs.']",['2000-03-14'] +728,['eng'],"['Aharonian, F A', 'Akhperjanian, A G', 'Barrio, J A', 'Bernlöhr, K', 'Bojahr, H', 'Calle, I', 'Contreras, J L', 'Cortina, J', 'Denninghoff, S', 'Fonseca, V', 'González, J C', 'Götting, N', 'Heinzelmann, G', 'Hemberger, M', 'Hermann, G', 'Heusler, A', 'Hofmann, W', 'Horns, D', 'Ibarra, Alejandro', 'Kankanyan, R', 'Kestel, M', 'Kettler, J', 'Kohler, C', 'Kohnle, A', 'Konopelko, A K', 'Kornmayer, H', 'Kranich, D', 'Krawczynski, H', 'Lampeitl, H', 'Lindner, A', 'Lorenz, E', 'Lucarelli, F', 'Magnussen, N', 'Mang, O', 'Meyer, H', 'Mirzoian, R M', 'Moralejo, A', 'Padilla, L', 'Panter, M', 'Plaga, R', 'Plyasheshnikov, A V', 'Prahl, J', 'Pühlhofer, G', 'Rauterberg, G', 'Röhring, A', 'Sahakian, V V', 'Samorski, M', 'Schilling, M', 'Schmele, D', 'Schröder, F', 'Stamm, W', 'Tluczykont, M', 'Völk, H J', 'Wiebel-Sooth, B', 'Wiedner, C A', 'Willmer, M', 'Wittek, W']",['The Energy Spectrum of TeV $\\Gamma$-Rays from the Crab Nebula as measured by the HEGRA system of imaging air Cherenkov telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'Cherenkov counter, imaging', 'experimental results', '500-20000 GeV']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003182'],"['The Crab Nebula has been observed by the HEGRA (High-Energy Gamma-Ray Astronomy) stereoscopic system of imaging air Cherenkov telescopes (IACTs) for a total of about 200 hrs during two observational campaigns: from September 1997 to March 1998 and from August 1998 to April 1999. The recent detailed studies of system performance give an energy threshold and an energy resolution for gamma-rays of 500 GeV and ~ 18, respectively. The Crab energy spectrum was measured with the HEGRA IACT system in a very broad energy range up to 20 TeV, using observations at zenith angles up to 65 degrees. The Crab data can be fitted in the energy range from 1 to 20 TeV by a simple power-law, which yields dJg/dE = (2.79+/-0.02 +/- 0.5) 10^{-7} E^{-2.59 +/- 0.03 +/- 0.05}, ph m^{-2} s^{-1} TeV^{-1} The Crab Nebula energy spectrum, as measured with the HEGRA IACT system, agrees within 15 0n the absolute scale and within 0.1 units in the power law index with the latest measurements by the Whipple, CANGAROO and CAT groups, consistent within the statistical and systematic errors quoted by the experiments. The pure power-law spectrum of TeV gamma-rays from the Crab Nebula constrains the physics parameters of the nebula environment as well as the models of photon emission.']",['2000-03-14'] +729,['eng'],"['Aharonian, F A']",['TeV $\\gamma$ Rays from BL Lac Objects due to Synchrotron Radiation of Extremely High Energy Protons'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'blazar', 'p, acceleration', 'synchrotron radiation, production', 'efficiency', 'synchrotron radiation, energy spectrum', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003159'],"['One of remarkable features of the gamma ray blazar Markarian 501 is the reported shape of the TeV spectrum, which during strong flares of the source remains essentially stable despite dramatic variations of the absolute gamma-ray flux. I argue that this (to a large extent unexpected) behavior of the source could be explained assuming that the TeV gamma-ray emission is a result of synchrotron radiation of extremely high energy protons in highly magnetized compact regions of the jet.']",['2000-03-14'] +730,['eng'],"['Bogovalov, S V', 'Aharonian, F A']",['Very-high-energy $\\gamma$ radiation associated with the unshocked wind of the Crab pulsar'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'pulsar', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'photon electron, Compton scattering', 'cosmic radiation, particle source', 'plasma, acceleration', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003157'],"['We show that the relativistic wind in the Crab pulsar, which is commonly thought to be invisible in the region upstream of the termination shock at R < 0.1 pc, in fact could be directly observed through its inverse Compton gamm-ray emission. The search for such specific component of radiation in the gamma-ray spectrum of the Crab can provide unique information about the unshocked pulsar wind that is not accessible at other wavelengths.']",['2000-03-14'] +731,['eng'],"['Nagataki, S', 'Kohri, K']",['Features of Nucleosynthesis and Neutrino Emission from Collapsars'],['Astrophysics and Astronomy'],"['supernova', 'astrophysics, hypernova', 'fusion', 'neutrino, emission', 'iron', 'niobium', 'neutrino/e, energy spectrum', 'mass, accretion', 'velocity, ratio', 'photon, cosmic radiation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003066'],"[""We present in this study two indicators that will reflect the differencebetween collapsars and collapse-driven supernovae. These are products ofexplosive nucleosynthesis and neutrino emission. In the case of collapsars,temperature behind the jet running along to the rotational axis rises highenough to synthesize iron-group nuclei. In this case, we can see two clumps ofiron; one clump is moving towards the north side and the other is movingtowards the south side. The mean velocity of iron-rich matter will be higher inthe case of collapsars because the explosion energy is greater thancollapse-driven supernovae. As for the energy spectrums of neutrinos, these arenot thermalized in collapsars because the density of the accretion disk is muchlower than that of a neutron star. The energy spectrums of (anti-)electronneutrinos from collapsars will be mainly determined by the emission rates dueto electron (positron) capture on free proton (neutron). It is also noted thathigh energy tail is not dumped in the case of collapsars because the density ofemitting region is low. Total neutrino's energy from collapsars will depend onmany physical quantum such as total accreting mass and mass accretion rate. Sothere will be a large variety of total neutrino's energies among collapsars. Inthe case of SN 1998bw, the matter around the equatorial plane might be ejectedfrom the system and only a weak jet might be generated due to the low massaccretion rate.""]",['2000-03-07'] +732,['eng'],"['Thompson, T A', 'Burrows, A', 'Horváth, J E']",['$\\mu$ and $\\tau$ Neutrino Thermalization and Production in Supernovae'],['Astrophysics and Astronomy'],"['supernova', 'n, matter', 'neutrino/mu, production', 'neutrino/tau, production', 'neutrino electron, elastic scattering', 'electron positron, annihilation', 'neutrino, pair production', 'nucleon nucleon, bremsstrahlung', 'neutrino nucleon, elastic scattering', 'structure function', 'Boltzmann equation', 'neutrino, energy', 'time variation', 'temperature, dependence', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003054'],"['We investigate the rates of production and thermalization of $\\nu_\\mu$ and$\\nu_\\tau$ neutrinos at temperatures and densities relevant to core-collapsesupernovae and protoneutron stars. Included are contributions from electronscattering, electron-positron annihilation, nucleon-nucleon bremsstrahlung, andnucleon scattering. For the scattering processes, in order to incorporate thefull scattering kinematics at arbitrary degeneracy, the structure functionformalism developed by Reddy et al. (1998) and Burrows and Sawyer (1998) isemployed. Furthermore, we derive formulae for the total and differential ratesof nucleon-nucleon bremsstrahlung for arbitrary nucleon degeneracy inasymmetric matter. We find that electron scattering dominates nucleonscattering as a thermalization process at low neutrino energies($\\epsilon_\\nu\\lesssim 10$ MeV), but that nucleon scattering is always fasterthan or comparable to electron scattering above $\\epsilon_\\nu\\simeq10$ MeV. Inaddition, for $\\rho\\gtrsim 10^{13}$ g cm$^{-3}$, $T\\lesssim14$ MeV, andneutrino energies $\\lesssim60$ MeV, nucleon-nucleon bremsstrahlung alwaysdominates electron-positron annihilation as a production mechanism for$\\nu_\\mu$ and $\\nu_\\tau$ neutrinos.']",['2000-03-07'] +733,['eng'],"['Noyes, H P']","['Bit-String Physics Prediction of $\\eta$, The Dark Matter/Baryon Ratio and $\\Omega_{M}$']",['Astrophysics and Astronomy'],"['talk, Marina del Rey 2000/02/23', 'light nucleus, production', 'photon baryon, ratio', 'matter, density', 'upper limit', 'astrophysics, fundamental constant', 'astrophysics, missing-mass', 'electroweak interaction', 'quantum number', 'string model', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003051'],"[""Using a simple combinatorial algorithm for generating finite and discreteevents as our numerical cosmology, we predict that the baryon/photon ratio atthe time of nucleogenesis is $\\eta= 1/256^4$, $\\Omega_{DM}/\\Omega_B= 12.7$ and(for a cosmological constant of $\\Omega_{\\Lambda}=0.6\\pm 0.1$ predicted ongeneral grounds by E.D.Jones) that $0.325 > \\Omega_M > 0.183 $. The limits areset not by our theory but by the empirical bounds on the renormalized Hubbleconstant of $0.6 < h_0 < 0.8$. If we impose the additional empirical bound of$t_0 < 14 Gyr$, the predicted upper bound on $\\Omega_M$ falls to 0.26. Thepredictions of $\\Omega_M$ and $\\Omega_{\\Lambda}$were in excellent agreementwith Glanz' analysis in 1998, and are still in excellent agreement withLineweaver's recent analysis despite the reduction of observational uncertaintyby close to an order of magnitude.""]",['2000-03-06'] +734,['eng'],"['Pugliese, G M', 'Falcke, H', 'Wang, Y', 'Biermann, P L']",['The jet-disk symbiosis model for $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'time variation', 'jet, model', 'cosmic radiation, energy spectrum', 'galaxy', 'neutrino, background', 'statistics, production', 'neutrino, flux', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003025'],"['The relation between the cosmological evolution of the jet-disk symbiosismodel for GRBs and the cosmic rays energy distribution is presented. We usedtwo different Star Formation Rates (SFR) as a function of redshift, the SFR byMadau and the one by Miyaji, and a Luminosity Function (LF) distribution toobtain the distribution in fluence of GRBs in our model and compare it with thedata. We show a good agreement between the fluence distribution we obtain andthe corrected data for the 4B BATSE catalogue. The results we obtain aregenerally valid for models that use jet physics to explain GRB properties. Thefluence in the gamma ray band has been used to calculate the energy in cosmicrays both in our Galaxy and at extragalactic distances as a function of theredshift. This energy input has been compared with the Galactic andextragalactic spectrum of cosmic rays and neutrinos. Using our jet disksymbiosis model, we found that in both cases GRBs cannot give any significantcontribution to cosmic rays. We estimate the neutrino background, obtainingsimilar results.']",['2000-03-03'] +735,['eng'],"['Olinto, A V']",['The Mystery of Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Urbino 1999/09/06', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'galaxy', 'model, hybrid', 'cosmic radiation, flux', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003013'],"['The origin of cosmic rays with energies higher than 10$^{20}$ eV remains amystery. Accelerating particles up to these energies is a challenge even forthe most energetic astrophysical objects known. While the isotropy in arrivaldirections argues for an extra-galactic origin, the photon-pion production offthe cosmic background radiation limits the sources of such particles to systemsless than 50 Mpc away from us. The combination of large gyroradii, efficientenergy losses, and isotropic arrival directions defies most of the proposedastrophysical accelerators as well as the more exotic alternatives. I brieflyreview theoretical models for the acceleration and propagation ofultra-high-energy cosmic-rays and discuss the potential for futureobservatories to resolve this cosmic mystery.']",['2000-03-02'] +736,['eng'],"['Ave, M', 'Hinton, J A', 'Vázquez, R A', 'Watson, A A', 'Zas, E']",['The rate of cosmic ray showers at large zenith angles'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'showers, air', 'showers, electromagnetic component', 'muon, flux', 'showers, spatial distribution', 'angular distribution', 'cosmic radiation, energy spectrum', 'background', 'numerical calculations, interpretation of experiments', 'proposed experiment']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003011'],"['It is anticipated that the Pierre Auger Observatory can be used to detectcosmic neutrinos of >10^19 eV that arrive at very large zenith angles. Howevershowers created by neutrino interactions close to the detector must be pickedout against a background of similar events initiated by cosmic ray nuclei. As astep towards understanding this background, we have made the first detailedanalysis of air showers recorded at Haverah Park (an array which used similardetectors to those planned for the Auger Observatory) with zenith angles above60 degs. We find that the differential shower rate from 60 degs to 80 degs. canbe predicted accurately when we adopt the known primary energy spectrum above10^17 eV and assume the QGSJET model and proton primaries. Details of thecalculation are given.']",['2000-03-02'] +737,['eng'],"['Bombaci, I']",['Do strange stars exist in the Universe?'],['Astrophysics and Astronomy'],"['talk, Hong Kong 1999/08/03', 'matter, strangeness', 'quark, matter', 'pulsar', 'n, matter', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002524'],"['Definitely, an affirmative answer to this question would have implications offundamental importance for astrophysics (a new class of compact stars), and forthe physics of strong interactions (deconfined phase of quark matter, andstrange matter hypothesis). In the present work, we use observational data forthe newly discovered millisecond X-ray pulsar SAX J1808.4-3658 and for theatoll source 4U 1728-34 to constrain the radius of the underlying compactstars. Comparing the mass-radius relation of these two compact stars withtheoretical models for both neutron stars and strange stars, we argue that astrange star model is more consistent with SAX J1808.4-3658 and 4U 1728-34, andsuggest that they are likely strange star candidates.']",['2000-03-01'] +738,['eng'],"['Hu, W']",['CMB Anisotropies'],['Astrophysics and Astronomy'],"['talk, Tokyo 1999/11/16', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'density, perturbation', 'inflationary universe', 'astrophysics, missing-mass', 'polarization', 'model, fluid', 'oscillation, acoustic', 'baryon, matter', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002520'],"['We review the theoretical implications of the past decade of CMB anisotropymeasurements, which culminated in the recent detection of the first feature inthe power spectrum, and discuss the tests available to the next decade ofexperiments. The current data already suggest that density perturbationsoriginated in an inflationary epoch, the universe is spatially flat, andbaryonic dark matter is required. We discuss the underlying assumptions ofthese claims and outline the tests required to ensure they are robust. The mostcritical test - the presence of a second feature at the predicted location -should soon be available. Further in the future, secondary anisotropies andpolarization should open new windows to the early and low(er) redshiftuniverse.']",['2000-03-01'] +739,['eng'],"['Yamada, S']",['Boltzmann equations for neutrinos with flavor mixings'],['Astrophysics and Astronomy'],"['supernova', 'n, matter', 'neutrino, mixing angle', 'neutrino, flavor', 'transport theory', 'Boltzmann equation', 'field theory', 'kinematics, relativistic', 'neutrino, propagator', 'mean field approximation', 'Born approximation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002502'],"['With a view of applications to the simulations of supernova explosion andproto neutron star cooling, we derive the Boltzmann equations for the neutrinotransport with the flavor mixing based on the real time formalism of thenonequilibrium field theory and the gradient expansion of the Green function.The relativistic kinematics is properly taken into account. The advection termsare derived in the mean field approximation for the neutrino self-energy whilesthe collision terms are obtained in the Born approximation. The resultingequations take the familiar form of the Boltzmann equation with corrections dueto the mixing both in the advection part and in the collision part. Thesecorrections are essentially the same as those derived by Sirera et al. for theadvection terms and those by Raffelt et al. for the collision terms,respectively, though the formalism employed here is different from theirs. Thederived equations will be easily implemented in numerical codes employed in thesimulations of supernova explosions and proto neutron star cooling.']",['2000-02-29'] +740,['eng'],"['Peebles, P J E']",['Fluid Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'model, fluid', 'galaxy', 'field theory, scalar', 'gravitation', 'potential', 'mass, density']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002495'],['Dark matter modeled as a classical scalar field that interacts only withgravity and with itself by a potential that is close to quartic at large fieldvalues and approaches a quadratic form when the field is small would begravitationally produced by inflation and at the present epoch could act likean ideal fluid with pressure that is a function only of the mass density. Thiscould have observationally interesting effects on the core radii and solid bodyrotation of dark matter halos and on the low mass end of the primeval massfluctuation power spectrum.'],['2000-02-29'] +741,['eng'],"['Abusaidi, R', 'Akerib, D S', 'Barnes, P D', 'Bauer, D A', 'Bolozdynya, A', 'Brink, P L', 'Bunker, R', 'Cabrera, B', 'Caldwell, D O', 'Castle, J P', 'Clarke, R M', 'Colling, P', 'Crisler, M B', 'Cummings, A C', 'Da Silva, A', 'Davies, A K', 'Dixon, R', 'Dougherty, B', 'Driscoll, D', 'Eichblatt, S', 'Emes, J', 'Gaitskell, R J', 'Golwala, S R', 'Hale, D', 'Haller, E E', 'Hellmig, J', 'Huber, M E', 'Irwin, K D', 'Jochum, J', 'Lipschultz, F P', 'Mandic, V', 'Martinis, J M', 'Nam, S W', 'Nelson, H', 'Neuhauser, B', 'Penn, M', 'Perera, T A', 'Perillo-Isaac, M C', 'Pritychenko, B V', 'Ross, R R', 'Saab, T', 'Sadoulet, Bernard', 'Schnee, R W', 'Seitz, D N', 'Shestople, P', 'Shutt, T', 'Smith, A', 'Smith, G W', 'Sonnenschein, A H', 'Spadafora, A L', 'Stockwell, W K', 'Taylor, J D', 'White, S', 'Yellin, S', 'Young, B A']",['Exclusion Limits on the WIMP-Nucleon Cross-Section from the Cryogenic Dark Matter Search'],['Astrophysics and Astronomy'],"['talk, Dalfsen 1999/08/15', 'astrophysics, missing-mass', 'elastic scattering, WIMP nucleus', 'elastic scattering, WIMP nucleon', 'ionization, yield', 'recoil, energy spectrum', 'WIMP, mass', 'channel cross section, mass', 'WIMP, search for', 'semiconductor detector, silicon', 'semiconductor detector, germanium', 'temperature, low', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002471'],"['The Cryogenic Dark Matter Search (CDMS) employs Ge and Si detectors to searchfor WIMPs via their elastic-scattering interactions with nuclei whilediscriminating against interactions of background particles. CDMS data givelimits on the spin-independent WIMP-nucleon elastic-scattering cross-sectionthat exclude unexplored parameter space above 10 GeV~c$^{-2}$ WIMP mass and, at$> 84$L, the entire 3$\\sigma$ allowed region for the WIMP signal reported bythe DAMA experiment.']",['2000-02-28'] +742,['eng'],"['Benoit, A', 'Bergé, L', 'Broniatowski, A', 'Chambon, B', 'Chapellier, M', 'Chardin, G', 'Charvin, P', 'De Jésus, M', 'Stefano, P D', 'Drain, D', 'Dumoulin, L', 'Garoche, P', 'Gascon, J', 'Goldbach, C', 'Gros, M H', 'Juillard, A', 'de Lesquen, A', ""L'Hôte, D"", 'Mallet, L', 'Mangin, J', 'Marnieros, S', 'Mirabolfathi, N', 'Miramonti, L', 'Mosca, L', 'Navick, X F', 'Nollez, G', 'Pari, P', 'Pécourt, S', 'Simon, E', 'Stern, M', 'Torre, J P']",['Event categories in the EDELWEISS WIMP search experiment'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, search for', 'elastic scattering, WIMP nucleus', 'radioactivity, background', 'photon, radiation', 'n, radiation', 'surface, effect', 'electron, recoil', 'nucleus, recoil', 'recoil, energy spectrum', 'semiconductor detector, germanium', 'temperature, low', 'deep underground detector, Frejus']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002462'],"['Four categories of events have been identified in the EDELWEISS-I dark matterexperiment using germanium cryogenic detectors measuring simultaneously chargeand heat signals. These categories of events are interpreted as electron andnuclear interactions occurring in the volume of the detector, and electron andnuclear interactions occurring close to the surface of the detectors(10-20 mu-mof the surface). We discuss the hypothesis that low energy surface nuclearrecoils,which seem to have been unnoticed by previous WIMP searches, mayprovide an interpretation of the anomalous events recorded by the UKDMC andSaclay NaI experiments. The present analysis points to the necessity of takinginto account surface nuclear and electron recoil interactions for a reliableestimate of background rejection factors.']",['2000-02-25'] +743,['eng'],"['Fargion, D']",['Discovering Ultra High Energy Neutrinos by Horizontal and Upward $\\tau$ Air-Showers'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'antineutrino, cosmic radiation', 'neutrino/e', 'neutrino/tau', 'cosmic radiation, particle source', 'neutrino, energy spectrum', 'neutrino, flux', 'showers, air', 'astrophysics', 'neutrino nucleon, interaction', 'antineutrino electron, interaction', 'charged current', 'tau, neutrinoproduction', 'W, leptonic decay', 'mass difference, (neutrino/tau neutrino/mu)', 'neutrino, oscillation', 'tau, path length', 'neutrino, path length', 'energy dependence', 'numerical calculations', 'proposed experiment', 'neutrino/tau nucleus --> tau anything', 'antineutrino/e electron --> W', 'W --> tau neutrino/tau']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002453'],"['Ultra high energy neutrinos UHE $\\nu_{\\tau}$, $\\bar\\nu_{\\tau}$ and$\\bar{\\nu}_e$ at PeV and higher energy may induce $\\tau$ air-showers whosedetectability is million to billion times amplified by their secondaries. Weconsidered UHE $\\nu_{\\tau} N$ and UHE $\\bar\\nu_{e} e$ interactions beyondmountains as a source of such horizontal amplified $\\tau$ air-showers. We alsoconsider upward UHE $\\nu_{\\tau} N$ interaction on Earth crust at horizont andtheir UHE $\\tau$ air-showers beaming toward high mountains $\\gamma$ detectors.We show their detectability. We notice that such rare upward $\\tau$ air-showermay hit even nearby satellite and flash them by short diluted $\\gamma-$burst atthe edge of Gamma Ray Observatory detection threshold. We identify these eventswith recent (1994) discovered (BATSE) Terrestrial Gamma Flashes and we claimtheir probable UHE $\\tau$ - UHE $\\nu_\\tau$ origin. From these first dataapproximated UHE $\\nu_\\tau$ flux and $\\Delta m_{\\nu_\\mu \\nu_\\tau}$ lower boundare derived. Known $X-\\gamma-\\mathrm{TeV}$ active galactic and extragalacticsources have been identified in most TGF arrival directions. Partial TGFGalactic signature is also manifest.']",['2000-02-25'] +744,['eng'],"['Pina-Avelino, P', 'Martins, C J A P']",['Primordial Adiabatic Fluctuations from Cosmic Defects'],['Astrophysics and Astronomy'],"['gravitation, model', 'fluctuation, adiabatic', 'defect, topological', 'defect, network', 'velocity', 'inflationary universe']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002413'],"[""We point out that in the context of ``two-metric'' theories of gravity thereis the possibility that cosmic defects will produce a spectrum of primordialadiabatic density perturbations. This will happen when the speed characterisingthe defect-producing scalar field is much larger than the speed characterisinggravity and all standard model particles. This model will exactly mimic thestandard predictions of inflationary models, with the exception of a smallnon-Gaussian signal which could be detected by future experiments. We brieflydiscuss defect evolution in these scenarios and analyze their cosmologicalconsequences.""]",['2000-02-23'] +745,['eng'],"['Moore, B', 'Gelato, S', 'Jenkins, A', 'Quilis, V', 'Pearce, F R']",['Collisional versus Collisionless Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'strong interaction', 'weak interaction', 'galaxy, production', 'kinematics', 'galaxy, cluster', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002308'],"[""We compare the structure and substructure of dark matter halos in modeluniverses dominated by collisional, strongly self interacting dark matter(SIDM) and collisionless, weakly interacting dark matter (CDM). While SIDMvirialised halos are more nearly spherical than CDM halos, they can berotationally flattened by as much as 20 0n their inner regions. Substructurehalos suffer ram-pressure truncation and drag which are more rapid and severethan their gravitational counterparts tidal stripping and dynamical friction.Lensing constraints on the size of galactic halos in clusters are a factor oftwo smaller than predicted by gravitational stripping, and the recent detectionof tidal streams of stars escaping from the satellite galaxy Carina suggeststhat its tidal radius is close to its optical radius of a few hundred parsecs--- an order of magnitude smaller than predicted by CDM models but consistentwith SIDM. The orbits of SIDM satellites suffer significant velocity bias$\\sigma_{SIDM}/\\sigma_{CDM}=0.85$ and are more circular than CDM,$\\beta_{SIDM}} \\approx 0.5$, in agreement with the inferred orbits of theGalaxy's satellites. In the limit of a short mean free path, SIDM halos havesingular isothermal density profiles, thus in its simplest incarnation SIDM isinconsistent with galactic rotation curves.""]",['2000-02-17'] +746,['eng'],"['Tavecchio, F', 'Maraschi, L']",['Constraints to the SSC model for Mkn 501'],['Astrophysics and Astronomy'],"['talk, Bologna 1999/09/06', 'photon, cosmic radiation', 'blazar', 'photon, absorption', 'cosmic radiation, energy spectrum', 'data analysis method', 'electron, acceleration', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002431'],['We fit the SEDs of the TeV blazar Mkn 501 adopting the homogeneousSynchrotron-Self Compton model to simultaneous X-ray and TeV spectra recentlybecome available. We present detailed model spectra calculated with the aboveconstraints and taking into account the absorption of TeV photons by the IRbackground. We found that the curved TeV spectra can be naturally reproducedeven without IRB absorption. Taking IRB absorption into account changes therequired parameter values only slightly.'],['2000-02-24'] +747,['eng'],"['Dai, Z G', 'Lu, T']",['Prompt Neutrino Emission from Gamma-Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'neutrino, emission', 'fireball, relativistic', 'neutrino, energy spectrum', 'muon, flux', 'shock waves', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002430'],"['Recent observations show that some or possibly all long-duration gamma-raybursts (GRBs) arise from the core collapse of massive stars. In this case, theGRB environments are believed to be preburst stellar winds. We here studyprompt neutrino emission from reverse shocks as a result of the interaction ofrelativistic fireballs with their surrounding wind matter. We find that forreasonable parameters the neutrino differential spectrum $\\propto\\epsilon_\\nu^{-1}$ below $\\sim 3\\times 10^{15}$ eV but the neutrinodifferential spectrum from $3\\times 10^{15}$ to $5\\times 10^{17}$ eV steepensby one power of the energy. In addition, the expected flux of upward movingmuons produced by neutrino interactions below a detector on the surface of theEarth is $\\sim 50$ events per year per km$^2$, which is about twice as large asthat of the previously studied neutrino bursts. Thus, the prompt neutrinoemission discussed here may dominate over neutrino emission from internalshocks. Furthermore, these properties are independent of whether the fireballsare isotropic or highly collimated.']",['2000-02-24'] +748,['eng'],"['Burkert, A']",['The structure and evolution of weakly self-interacting cold dark matter halos'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'many-body problem', 'weak interaction', 'cross section', 'galaxy, production', 'kinematics', 'matter, density', 'velocity, dispersion', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002409'],"['The evolution of halos consisting of weakly self-interacting dark matterparticles is investigated using a new numerical Monte-Carlo N-body method. Thehalos initially contain kinematically cold, dense 1/r-power-law cores. Forinteraction cross sections (sigma/mp) >= 0.01-0.1 cm**2/g weak self-interactionleads to the formation of isothermal, constant density cores within a Hubbletime as a result of heat transfer into the cold inner regions. This corestructure is in good agreement with the observations of dark matter rotationcurves in dwarf galaxies. The isothermal core radii and core densities are afunction of the halo scale radii and scale masses which depend on thecosmological model. Adopting the currently popular LCDM model, the predictedcore radii would be a factor of three to five smaller than observed. Thisresult agrees well with other independent studies which conclude that currentcosmological models overestimate the concentrations of dark matter halos by alarge factor. For large interaction cross sections, massive dark halos withscale radii rs >= 14 cm**2/g/(sigma/mp) kpc could experience core collapseduring their lifetime, leading to cores with singular isothermal densityprofiles.']",['2000-02-23'] +749,['eng'],"['Wang, J M']",['Intrinsic constraints on very high energy emission in $\\gamma$-ray loud blazars'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'blazar', 'galaxy, AGN', 'photon, emission', 'photon, pair production', 'photon photon, interaction', 'photon, synchrotron radiation', 'electron, scattering', 'photon, absorption', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002402'],"[""Photons with very high energy up to TeV (VHE) emitted from active galacticnuclei (AGNs) provide some invaluable information of the origin of $\\gam$-rayemission. Although 66 blazars have been detected by {\\it EGRET}, only three lowredshift X-ray selected BL Lacs (Mrk 421, Mrk 501, and 1ES 2344+514) areconclusive TeV emitters (PKS 2155-304 is a potential TeV emitter) since VHEphotons may be absorbed by cosmological background infrared photons ({\\itexternal} absorption). Based on the ``mirror'' effect of clouds in broad lineregion, we argue that there is an {\\it intrinsic} mechanism for the deficiencyof TeV emission in blazars. Employing the observable quantities we derive thepair production optical depth $\\tgg(\\eps_{\\rm obs})$ due to the interaction ofVHE photons with the reflected synchrotron photons by electron Thomsonscattering in broad line region. This sets a more strong constraints on veryhigh energy emission, and provides a sensitive upper limit of Doppler factor ofthe relativistic bulk motion. It has been suggested to distinguish the {\\itintrinsic} absorption from the {\\it external} by the observation on variationof multiwavelegenth continuum.""]",['2000-02-23'] +750,['eng'],"['Ziaeepour, H']","['Cosmic Equation of State, Quintessence and Decaying Dark Matter']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'decay, missing-mass', 'quintessence', 'astrophysics, fundamental constant', 'supernova', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002400'],"['If CDM particles decay and their lifetime is comparable to the age of theUniverse, they can modify its equation of state. By comparing the results ofnumerical simulations with high redshift SN-Ia observations we show that thishypothesis is consistent with present data. Fitting the simplest quintessencemodels with constant $w_q$ to data leads to $w_q \\lesssim -1$. We show that auniverse with a cosmological constant or quintessence matter with $w_q \\sim -1$and a decaying Dark Matter has an effective $w_q < -1$ and fits SN data betterthan stable CDM or quintessence models with $w_q > -1$.']",['2000-02-22'] +751,['eng'],"['Lyth, D H', 'Covi, L']",['Observational constraints on the spectral index of the cosmological curvature perturbation'],['Astrophysics and Astronomy'],"['inflationary universe', 'astrophysics, missing-mass', 'space-time, perturbation', 'mass, inflaton', 'statistical analysis', 'cosmic radiation, background', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002397'],"['We have evaluated the observational constraints on the spectral index $n$, inthe context of the $\\Lambda$CDM model which is the simplest viable choice. If$n$ is practically scale-independent, as predicted by most models of inflation,present data require $n\\simeq 1.0 \\pm 0.1$ at something like the 2-$\\sigma$level. We also exhibit the much tighter constraint, obtained if one fixes theepoch of reionization, and the height of the first acoustic peak in the cmbanisotropy. The former has a preferred range 20 to 30, while the latter maysoon be accurately known. We have also investigated the two-parameterscale-dependent spectral index, predicted by running-mass inflation models.Present data allow significant variation of of $n$ in this case, which occursin a physically reasonable regime of parameter space.']",['2000-02-22'] +752,['eng'],"['Zdunik, J L', 'Haensel, P', 'Gondek-Rosinska, D', 'Gourgoulhon, E']",['Innermost stable circular orbits around strange stars and kHz QPOs in low-mass X-ray binaries'],['Astrophysics and Astronomy'],"['matter, strangeness', 'rotational', 'binary', 'orbit, stability', 'relativity theory, general', 'photon, cosmic radiation', 'flux, oscillation', 'matter, mass', 'bag model', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002394'],"['Exact calculations of innermost stable circular orbit (ISCO) around rotatingstrange stars are performed within the framework of general relativity.Equations of state (EOS) of strange quark matter based on the MIT Bag Modelwith massive strange quarks and lowest order QCD interactions, are used. Thepresence of a solid crust of normal matter on rotating, mass accreting strangestars in LMXBs is taken into account. It is found that, contrary to neutronstars, above some minimum mass a gap always separates the ISCO and stellarsurface, independently of the strange star rotation rate. For a given baryonmass of strange star, we calculate the ISCO frequency as function of stellarrotation frequency, from static to Keplerian configuration. For masses close tothe maximum mass of static configurations the ISCO frequencies for static andKeplerian configurations are similar. However, for masses significantly lowerthan the maximum mass of static configurations, the minimum value of the ISCOfrequency is reached in the Keplerian limit. Presence of a solid crustincreases the ISCO frequency for the Keplerian configuration by about tenpercent compared to that for a bare strange star of the same mass.']",['2000-02-22'] +753,['eng'],"['Weinberg, S']",['A Priori Probability Distribution of the Cosmological Constant'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'statistics', 'field theory, scalar', 'vacuum state, energy', 'potential', 'inflationary universe', 'quantum cosmology']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002387'],"['In calculations of the probability distribution for the cosmologicalconstant, it has been previously assumed that the a priori probabilitydistribution is essentially constant in the very narrow range that isanthropically allowed. This assumption has recently been challenged. Here weidentify large classes of theories in which this assumption is justified.']",['2000-02-22'] +754,['eng'],"['Oldershaw, R L']",['A Review of Mass Estimates for Galactic Dark Matter Objects'],['Astrophysics and Astronomy'],"['review', 'astrophysics, missing-mass', 'galaxy', 'mass, measurement', 'gravitation, lens', 'astrophysics, model', 'fractals', 'data analysis method', 'interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002363'],"['Empirical mass estimates for galactic dark matter objects, published betweenDecember 1991 and May 1999, are presented in tabular and graphical forms.Trends in the data are identified and uncertainties are discussed. Similaritiesamong various stellar and dark matter mass functions are noted, and a possibleidentification of the galactic dark matter objects is suggested.']",['2000-02-22'] +755,['eng'],"['Yoshida, N', 'Springel, V', 'White, S D M', 'Tormen, G']",['Collisional dark matter and the structure of dark halos'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'elastic scattering', 'matter, cluster', 'galaxy, cluster', 'many-body problem', 'gas, fluid', 'gas, entropy', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002362'],"['We study how the internal structure of dark halos is affected if Cold DarkMatter particles are assumed to have a large cross-section for elasticcollisions. We identify a cluster halo in a large cosmological N-bodysimulation and resimulate its formation with progressively increasingresolution. We compare the structure found in the two cases where dark matteris treated as collisionless or as a fluid. For the collisionless case ourresults agree with those of other workers. Collisional dark matter results in acluster which is more nearly spherical and has a more singular central densityprofile. Substructure within the cluster is only weakly suppressed relative tothe collisionless case. The observed structure of dwarf galaxies argues againstself-interacting dark matter if, as seems likely, intermediate cross-sectionsproduce structure lying between the extremes we have simulated.']",['2000-02-18'] +756,['eng'],"['Haiman, Z', 'Mohr, J J', 'Holder, G P']",['Constraints on Quintessence from Future Galaxy Cluster Surveys'],['Astrophysics and Astronomy'],"['galaxy, cluster', 'quintessence', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'photon, cosmic radiation', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']","['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002336', 'http://fnalpubs.fnal.gov/archive/2000/pub/Pub-00-043-A.html']","['We study the expected redshift evolution of galaxy cluster abundance between0^{3/2}$, which for relativistically-decoupled relics isdetermined by particle mass and spin and is insensitive to cosmologicalparameters. Finite $Q$ leads to small-scale filtering of the primordial powerspectrum, which reduces substructure, and limits the maximum central density ofhalos, which eliminates central cusps. The relationship between $Q$ and haloobservables is estimated. The primordial $Q$ may be preserved in the cores ofhalos and if so leads to a predicted relation, closely analogous to that indegenerate dwarf stars, between the central density and velocity dispersion.Classical polytrope solutions are used to model the structure of halos ofcollisional dark matter, and to show that self-interactions in halos today areprobably not significant because they destabilize halo cores via heatconduction. Constraints on masses and self-interactions of dark matterparticles are estimated from halo stability and other considerations.""]",['2000-02-17'] +758,['eng'],"['Bourilkov, D']",['Study of Multi-muon Events from EAS with the L3 Detector at Shallow Depth Underground'],['Astrophysics and Astronomy'],"['talk, Paris 1999/09/06', 'muon, cosmic radiation', 'showers, air', 'muon, multiplicity', 'muon+ muon-, ratio', 'momentum dependence', 'numerical calculations, Monte Carlo', 'magnetic detector, L3', 'experimental results', 'CERN LEP Stor']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002326'],['We present first preliminary data from the L3+Cosmics experiment and resultsfrom Monte Carlo simulations of multi-muon events as observed 30 m underground.'],['2000-02-17'] +759,['eng'],"['Amenomori, M', 'Ayabe, S', 'Cao, P Y', 'Danzengluobu', 'Ding, L K', 'Feng, Z Y', 'Fu, Y', 'Guo, H W', 'He, M', 'Hibino, K', 'Hotta, N', 'Huang, Q', 'Huo, A X', 'Izu, K', 'Jia, H Y', 'Kajino, F', 'Kasahara, K', 'Katayose, Y', 'Labaciren', 'Li Jing Yi', 'Lu, H', 'Lu, S L', 'Luo, G X', 'Meng, X R', 'Mizutani, K', 'Mu, J', 'Nanjo, H', 'Nishizawa, M', 'Ohnishi, M', 'Ohta, I', 'Ouchi, T', 'Ren, J R', 'Saitô, T', 'Sakata, M', 'Sasaki, T', 'Shi, Z Z', 'Shibata, M', 'Shiomi, A', 'Shirai, T', 'Sugimoto, H', 'Taira, K', 'Tan, Y H', 'Tateyama, N', 'Torii, S', 'Utsugi, T', 'Wang, C R', 'Wang, H', 'Xu, X W', 'Yamamoto, Y', 'Yu, G C', 'Yuan, A F', 'Yuda, T', 'Zhang, C S', 'Zhang, H M', 'Zhang, J L', 'Zhang, N J', 'Zhang, X Y', 'Zha Xi Ciren', 'Zhaxi Sang Zhu', 'Zhou, W D']",['Detection of Multi-TeV $\\gamma$ Rays from Markarian 501 during an Unforeseen Flaring State in 1997 with the Tibet Air Shower Array'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'cosmic radiation, energy spectrum', 'shower detector, experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002314'],"['In 1997, the BL Lac Object Mrk 501 entered a very active phase and was thebrightest source in the sky at TeV energies, showing strong and frequentflaring. Using the data obtained with a high density air shower array that hasbeen operating successfully at Yangbajing in Tibet since 1996, we searched forgamma-ray signals from this source during the period from February throughAugust in 1997. Our observation detected multi-TeV $\\gamma$-ray signals at the3.7-Sigma level during this period. The most rapid increase of the excesscounts was observed between April 7 and June 16 and the statisticalsignificance of the excess counts in this period was 4.7-Sigma. Among severalobservations of flaring TeV gamma-rays from Mrk 501 in 1997, this is the onlyobservation using a conventional air shower array. We present the energyspectrum of gamma-rays which will be worthy to compare with those obtained byimaging atmospheric Cerenkov telescopes.']",['2000-02-17'] +760,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Dokuchaev, V I']",['Hidden Source of High-Energy Neutrinos in Collapsing Galactic Nucleus'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, particle source', 'galaxy, AGN', 'black hole, massive', 'n, matter', 'matter, cluster', 'fireball, production', 'shock waves, production', 'particle, acceleration', 'neutrino, production', 'photon, cosmic radiation']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002274'],"['We propose a model of a short-lived extremely powerful source of high energyneutrinos. It is formed as a result of dynamical evolution of a galacticnucleus prior to its collapse into the massive black hole. A dense centralstellar cluster in the galactic nucleus on the late stage of evolution consistsof compact stars (neutron stars and stellar mass black holes). This cluster issinked deep into the massive gas envelope produced in the collisions of theprimary stellar population. The frequent collisions of remaining neutron starsin central stellar cluster result in a creation of ultrarelativistic fireballsand shock waves. They produce the rarefied cavern with external shell andquasi-stationary external shock. The particles are effectively accelerated inthe cavern and, due to pp-collisions in the gas envelope, they produce highenergy neutrinos. All high energy particles, except neutrinos, are absorbed inthe thick envelope. Duration of active stage is $\\sim10$ yr, the number of thesources can be $\\sim 10$ per cosmological horizon. High energy neutrino signalcan be detected by underground neutrino telescope with effective area $S\\sim1$km$^2$.']",['2000-02-15'] +761,['eng'],"['Mayet, F', 'Santos, D', 'Perrin, G', 'Bunkov, Yu M', 'Godfrin, H']","['Design optimization of MACHe3, a project of superfuid $^{3}He$ Detector for direct Dark Matter search']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'supersymmetry', 'counters and detectors, proposed', 'helium, superfluid', 'bolometer', 'n, background', 'photon, background', 'numerical calculations, Monte Carlo']","['http://arXiv.org/ps/astro-ph/0002303', 'http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002303']","['MACHe3 (MAtrix of Cells of superfluid He3) is a project of a new detector fordirect Dark Matter (DM) search. A cell of superfluid He3 has been developed andthe idea of using a large number of such cells in a high granularity detectoris proposed. This paper presents, after a brief description of the superfluidHe3 cell, the simulation of the response of different matrix configurationsallowing to define an optimum design as a function of the number of cells andthe volume of each cell. The background rejection, for several configurations,is presented both for neutrons and gamma-rays of various kinetic energies.']",['2000-02-16'] +762,['eng'],"['Yoshida, S', 'Lee, U']",['Rotational modes of non-isentropic stars and the gravitational radiation driven instability'],['Astrophysics and Astronomy'],"['n, matter', 'matter, rotational', 'model, fluid', 'stability', 'gravitational radiation', 'oscillation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002300'],"['We investigate the properties of r-mode and inertial mode of slowly rotating,non-isentropic, Newtonian stars, by taking account of the effects of theCoriolis force and the centrifugal force. For the non-isentropic models weconsider only two cases, that is, the models with the stable fluidstratification in the whole interior and the models that are fully convective.For simplicity we call these two kinds of models ""radiative"" and ""convective""models in this paper. For both cases, we assume the deviation of the modelsfrom isentropic structure is small. Examining the dissipation timescales due tothe gravitational radiation and several viscous processes for the polytropicneutron star models, we find that the gravitational radiation driveninstability of the r-modes remains strong even in the non-isentropic models.Calculating the rotational modes of the radiative models as functions of theangular rotation frequency $\\Omega$, we find that the inertial modes arestrongly modified by the buoyant force at small $\\Omega$, where the buoyantforce as a dominant restoring force becomes comparable with or stronger thanthe Coriolis force. Because of this property we obtain the mode sequences inwhich the inertial modes at large $\\Omega$ are identified as g-modes or ther-modes with l=|m| at small $\\Omega$. We also note that as $\\Omega$ increasesfrom $\\Omega=0$ the retrograde g-modes become retrograde inertial modes, whichare unstable against the gravitational radiation reaction.']",['2000-02-16'] +763,['eng'],"['Wolter, A', 'Tavecchio, F', 'Caccianiga, A', 'Ghisellini, G', 'Tagliaferri, G']",['X-ray variability and prediction of TeV emission in the HBL 1ES1101-232'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'galaxy', 'magnetic field', 'experimental results, satellite']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002298'],"['1ES1101-232 is a bright BL Lac of the High frequency peak class. We presenthere the results of two BeppoSAX observations in which the source has shown avariation of about 30 0n flux with a corresponding spectral variability. Weinterpret the overall spectral energy distribution in terms of an homogeneousSSC model and, by using also the TeV upper limit from a short Mark 6 pointing,derive constraints on the physical parameters of the source, in particular onthe magnetic field strength. The overall Spectral Energy Distribution makes1ES1101-232 a very promising candidate for TeV detection.']",['2000-02-16'] +764,['eng'],"['Petry, D', 'Böttcher, M', 'Connaughton, V', 'Lahteenmaki, A', 'Pursimo, T', 'Raiteri, C M', 'Schröder, F', 'Sillanpää, A', 'Sobrito, G', 'Takalo, L', 'Terasranta, H', 'Tosti, G', 'Villata, M']",['Multiwavelength observations of Mkn 501 during the 1997 high state'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'electron, jet', 'cosmic radiation, correlation', 'photon electron, Compton scattering', 'electron, injection', 'electron, energy spectrum', 'data analysis method', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002255'],"['During the observation period 1997, the nearby Blazar Mkn 501 showedextremely strong emission and high variability. We examine multiwavelengthaspects of this event using radio, optical, soft and hard X-ray and TeV data.We concentrate on the medium-timescale variability of the broadband spectra,averaged over weekly intervals. We confirm the previously found correlation between soft and hard X-rayemission and the emission at TeV energies, while the source shows only minorvariability at radio and optical wavelengths. The non-linear correlationbetween hard X-ray and TeV fluxes is consistent with a simple analytic estimatebased on an SSC model in which Klein-Nishina effects are important for thehighest-energy electrons in the jet, and flux variations are caused byvariations of the electron density and/or the spectral index of the electroninjection spectrum. The time-averaged spectra are fitted with a Synchrotron Self-Compton (SSC)dominated leptonic jet model, using the full Klein-Nishina cross section andfollowing the self-consistent evolution of relativistic particles along thejet, accounting for gamma-gamma absorption and pair production within thesource as well as due to the intergalactic infrared background radiation. Thecontribution from external inverse-Compton scattering is tightly constrained bythe low maximum EGRET flux and found to be negligible at TeV energies. We findthat high levels of the X-ray and TeV fluxes can be explained by a hardening ofthe energy spectra of electrons injected at the base of the jet, in remarkablecontrast to the trend found for gamma-ray flares of the flat-spectrum radioquasar PKS 0528+134.']",['2000-02-14'] +765,['eng'],"['Sako, T', 'Matsubara, Y', 'Muraki, Y', 'Ramana-Murthy, P V', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, T', 'Hara, S', 'Holder, J', 'Kamei, S', 'Kawachi, A', 'Kifune, T', 'Kita, R', 'Masaike, A', 'Mizumoto, Y', 'Mori, M', 'Moriya, M', 'Muraishi, H', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Rowell, G P', 'Sakurazawa, K', 'Sato, Y', 'Susukita, R', 'Suzuki, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['Very High-Energy $\\gamma$-Ray Observations of PSR B1509-58 with the CANGAROO 3.8 m Telescope'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'pulsar', 'cosmic radiation, flux', 'time variation', 'Cherenkov counter, imaging', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002252'],"[""The gamma-ray pulsar PSR B1509-58 and its surrounding nebulae have beenobserved with the CANGAROO 3.8m imaging atmospheric Cherenkov telescope. Theobservations were performed from 1996 to 1998 in Woomera, South Australia,under different instrumental conditions with estimated threshold energies of4.5 TeV (1996), 1.9 TeV (1997) and 2.5 TeV (1998) at zenith angles of ~30 deg.Although no strong evidence of the gamma-ray emission was found, the lowestenergy threshold data of 1997 showed a marginal excess of gamma-ray--likeevents at the 4.1 sigma significance level. The corresponding gamma-ray flux iscalculated to be (2.9 +/- 0.7) * 10^{-12}cm^{-2}s^{-1} above 1.9 TeV. Theobservations of 1996 and 1998 yielded only upper limits (99.5onfidencelevel) of 1.9 * 10^{-12}cm^{-2}s^{-1} above 4.5 TeV and 2.0 *10^{-12}cm^{-2}s^{-1} above 2.5 TeV, respectively. Assuming that the 1997excess is due to Very High-Energy (VHE) gamma-ray emission from the pulsarnebula, our result, when combined with the X-ray observations, leads to a valueof the magnetic field strength ~5 micro G. This is consistent with theequipartition value previously estimated in the X-ray nebula surrounding thepulsar. No significant periodicity at the 150ms pulsar period has been found inany of the three years' data. The flux upper limits set from our observationsare one order of magnitude below previously reported detections of pulsed TeVemission.""]",['2000-02-14'] +766,['eng'],"['Waxman, E']","['$\\gamma$-Ray Bursts, Cosmic-Rays and Neutrinos']",['Astrophysics and Astronomy'],"['talk, Paris 1999/09/06', 'photon, cosmic radiation', 'gamma ray burst', 'cosmic radiation, particle source', 'fireball, relativistic', 'cosmic radiation, flux', 'neutrino, production', 'p, cosmic radiation', 'p, acceleration', 'energy spectrum', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002243'],"[""The gamma-ray burst (GRB) model for production of ultra-high-energycosmic-rays (UHECRs) is based on the hypothesis that GRBs arise from thedissipation of the kinetic energy of relativistic fireballs at cosmologicaldistances. Recent GRB afterglow observations support the validity of thishypothesis and provide quantitative support for the model. The inferredphysical fireball parameters imply that protons may be accelerated to >10^20eV, and the inferred GRB energy generation rate is similar to that required toaccount for the observed flux of UHECRs. Strong suppression of UHECR flux is expected in this model above 10^19.7 eV,due to proton interaction with CMB photons. Strong deviations from model fluxderived under the assumption of uniform source distribution is expected above10^20 eV, due to source clustering. The flux above 10^20.5 eV is expected to bedominated by few, narrow spectrum sources. While model predictions can not betested (with high confidence level) at present, the predicted signatures shouldbe observed with the planned Auger and Telescope-Array UHECR detectors. A natural consequence of the GRB model of UHECR production is the conversionof a large fraction, ~10, of the fireball energy to accompanying burst of\\~10^14 eV and ~10^18 eV neutrinos. A km^2 neutrino detector would observeseveral tens of events per year correlated with GRBs, and test for neutrinoproperties (e.g. flavor oscillations, for which upward moving tau's would be aunique signature, and coupling to gravity) with an accuracy many orders ofmagnitude better than is currently possible.""]",['2000-02-14'] +767,['eng'],"['Sedrakian, Ara G', 'Dieperink, A E L']",['Coherent neutrino radiation in supernovae at two loops'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'transport theory', 'propagator', 'polarization, tensor', 'cosmic radiation, coherence', 'supernova', 'Feynman graph, higher-order', 'neutrino, bremsstrahlung', 'pseudoparticle, width', 'baryon, off-shell', 'neutral current, axial-vector', 'phase space', 'n, matter', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002228'],"[""We develop a neutrino transport theory, in terms of the real-timenon-equilibrium Green's functions, which is applicable to physical conditionsarbitrary far from thermal equilibrium. We compute the coherent neutrinoradiation in cores of supernovae by evaluating the two-particle-two-hole(2p-2h) polarization function with dressed propagators. The propagator dressingis carried out in the particle-particle channel to all orders in theinteraction. We show that at two loops there are two distinct sources ofcoherence effects in the bremsstrahlung. One is the generically off-shellintermediate state propagation, which leads to the Landau-Pomeranchuk-Migdaltype suppression of radiation. We extend previous perturbative results,obtained in the leading order in quasiparticle width, by deriving the exactnon-perturbative expression. A new contribution due to off-shell finial/initialbaryon states is treated in the leading order in the quasiparticle width. Thelatter contribution corresponds to processes of higher order than second orderin the virial expansion in the number of quasiparticles. At 2p-2h level, thetime component of the polarization tensor for the vector transitions vanishesidentically in the soft neutrino limit. Vector current thereby is conserved.The contraction of the neutral axial vector current with tensor interactionamong the baryons leads to a non-vanishing contribution to the bremsstrahlungrate. These rates are evaluated numerically for finite temperature pure neutronmatter at and above the nuclear saturation density.""]",['2000-02-11'] +768,['eng'],"['Guth, A H']",['Inflation and Eternal Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'space-time', 'statistics', 'regularization']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002156'],"[""The basic workings of inflationary models are summarized, along with thearguments that strongly suggest that our universe is the product of inflation.The mechanisms that lead to eternal inflation in both new and chaotic modelsare described. Although the infinity of pocket universes produced by eternalinflation are unobservable, it is argued that eternal inflation has realconsequences in terms of the way that predictions are extracted fromtheoretical models. The ambiguities in defining probabilities in eternallyinflating spacetimes are reviewed, with emphasis on the youngness paradox thatresults from a synchronous gauge regularization technique. Vilenkin's proposalfor avoiding these problems is also discussed.""]",['2000-02-08'] +769,['eng'],"['De Gouveia dal Pino, E M', 'Lazarian, A']",['Ultra-High-Energy Cosmic Ray Acceleration by Magnetic Reconnection in Newborn Accretion Induced Collapse Pulsars'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'cosmic radiation, acceleration', 'pulsar', 'magnetic field', 'cosmic radiation, flux', 'n, matter', 'astrophysics, white dwarf', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002155'],"['We here investigate the possibility that the ultra-high energy cosmic ray(UHECR) events observed above the GZK limit are mostly protons accelerated inreconnection sites just above the magnetosphere of newborn millisecond pulsarswhich are originated by accretion induced collapse (AIC). We find thatAIC-pulsars with surface magnetic fields $10^{12} G < B_{\\star} \\lesssim10^{15}$ G and spin periods $1 ms \\lesssim P_{\\star} < 60 ms$, are able toaccelerate particles to energies $\\geq 10^{20}$ eV. Because the expected rateof AIC sources in our Galaxy is very small (\\sim 10^{-5} yr^{-1}), thecorresponding contribution to the flux of UHECRs is neglegible, and the totalflux is given by the integrated contribution from AIC sources produced by thedistribution of galaxies located within the distance which is unaffected by theGZK cutoff ($\\sim 50 $ Mpc). We find that the reconnection efficiency factorneeds to be only $ \\xi \\gtrsim 3.6 \\times 10^{-3}$ in order to reproduce theobserved flux of UHECRs.']",['2000-02-08'] +770,['eng'],"['Matos, T', 'Guzmán, F']",['Quintessence at Galactic Level?'],['Astrophysics and Astronomy'],"['galaxy', 'field theory, scalar', 'quintessence', 'astrophysics, missing-mass', 'Einstein equation, solution', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002126'],"[""Recently it has been proposed that the main contributor to the dark energy ofthe Universe is a dynamical, slow evolving, spatially inhomogeneous scalarfield called quintessence. We investigate the behavior of this scalar field atgalactic level by assuming that it is the dark matter compossing the halos ofgalaxies. Using an exact solution of the Einstein's equations we find anexcellent concordance between our results and observations.""]",['2000-02-08'] +771,['eng'],"['Lee, A', 'Bloom, Elliott D', 'Petrosian, V']",['Intrinsic and Cosmological Signatures in Gamma-Ray Burst Time Profiles'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'gamma ray burst', 'data analysis method', 'signal processing', 'time dependence', 'correlation, measure', 'effect, time delay', 'cosmic radiation, flux', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002218'],"['The time profiles of many gamma-ray bursts consist of distinct pulses, whichoffers the possibility of characterizing the temporal structure of these burstsusing a relatively small set of pulse shape parameters. We have used a pulsedecomposition procedure to analyze the Time-to-Spill (TTS) data for all burstsobserved by BATSE up through trigger number 2000, in all energy channels forwhich TTS data is available. We obtain amplitude, rise and decay timescales, apulse shape parameter, and the fluences of individual pulses in all of thebursts. We investigate the correlations between brightness measures (amplitudeand fluence) and timescale measures (pulse width and separation) which mayresult from cosmological time dilation of bursts, or from intrinsic propertiesof burst sources or from selection effects. The effects of selection biases areevaluated through simulations. The correlations between these parameters amongpulses within individual bursts give a measure of the intrinsic effects whilethe correlations among bursts could result both from intrinsic and cosmologicaleffects. We find that timescales tend to be shorter in bursts with higher peakfluxes, as expected from cosmological time dilation effects, but also find thatthere are non-cosmological effects contributing to this inverse correlation. Wefind that timescales tend to be longer in bursts with higher total fluences,contrary to what is expected from cosmological effects. We also find that peakfluxes and total fluences of bursts are uncorrelated, indicating that theycannot both be good distance indicators for bursts.']",['2000-02-11'] +772,['eng'],"['Sambruna, R M']",['Correlated intense X-ray and TeV activity of Mrk~501 in 1998 June'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'blazar', 'cosmic radiation, energy', 'cosmic radiation, flux', 'time variation', 'shower detector', 'counters and detectors, satellite', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002215'],"['We present exactly simultaneous X-ray and TeV monitoring with {\\it RXTE} andHEGRA of the TeV blazar Mrk 501 during 15 days in 1998 June. After an initialperiod of very low flux at both wavelengths, the source underwent a remarkableflare in the TeV and X-ray energy bands, lasting for about six days and with alarger amplitude at TeV energies than in the X-ray band. At the peak of the TeVflare, rapid TeV flux variability on sub-hour timescales is found. Largespectral variations are observed at X-rays, with the 3--20 keV photon index ofa pure power law continuum flattening from $\\Gamma=2.3$ to $\\Gamma=1.8$ on atimescale of 2--3 days. This implies that during the maximum of the TeVactivity, the synchrotron peak shifted to energies $\\gtrsim 50$ keV, a behaviorsimilar to that observed during the longer-lasting, more intense flare in 1997April. The TeV spectrum during the flare is described by a power law withphoton index $\\Gamma=1.9$ and an exponential cutoff at $\\sim$ 4 TeV; anindication for spectral softening during the flare decay is observed in the TeVhardness ratios. Our results generally support a scenario where the TeV photonsare emitted via inverse Compton scattering of ambient seed photons by the sameelectron population responsible for the synchrotron X-rays. The simultaneousspectral energy distributions (SEDs) can be fit with a one-zonesynchrotron-self Compton model assuming a substantial increase of the magneticfield and the electron energy by a factor of 3 and 10, respectively.']",['2000-02-14'] +773,['eng'],"['Asano, K', 'Fukuyama, T']",['Neutrino Pair Annihilation in the Gravitation of Gamma Ray Burst Sources'],['Astrophysics and Astronomy'],"['neutrino, sphere', 'accretion', 'neutrino antineutrino, annihilation', 'gravitation, effect', 'black hole, Schwarzschild', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'energy', 'relativity theory, general', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002196'],"[""We study semianalytically the gravitational effects on neutrino pairannihilation near the neutrinosphere and around the thin accretion disk. Forthe disk case, we assume that the accretion disk is isothermal and that thegravitational field is dominated by the Schwarzschild black hole. Generalrelativistic effects are studied only near the rotation axis. The energydeposition rate is enhanced by the effect of orbital bending toward the center.However, the effects of the redshift and gravitational trapping of thedeposited energy reduce the effective energy of the gamma ray bursts' source.Although each effect is substantial, the effects partly cancel one another. Asa result, the gravitational effects do not substantially change the energydeposition rate for either the spherical symmetric case or the disk case.""]",['2000-02-10'] +774,['eng'],"['Kim, J E']",['A Theoretical Review of Axion'],['Astrophysics and Astronomy'],"['talk, Trieste 1999/09/27', 'strong interaction, CP', 'axion, mass', 'axion, decay constant', 'astrophysics', 'string model', 'supersymmetry', 'axion, search for', 'quintessence', 'quantum chromodynamics, Theta parameter', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002193'],['It is emphasized that the existence of a very light axion is consistent withthe strong CP invariance and cosmological and astrophysical constraints. Theattempt to embed the very light axion in superstring models is discussed.'],['2000-02-10'] +775,['eng'],"['Guth, A H']",['Inflationary Models and Connections to Particle Physics'],['Astrophysics and Astronomy'],"['talk, Chicago 1999/01/29', 'inflationary universe', 'chaos', 'space-time', 'statistics', 'regularization', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002188'],"[""The basic workings of inflationary models are summarized, along with thearguments that strongly suggest that our universe is the product of inflation.The mechanisms that lead to eternal inflation in both new and chaotic modelsare described. Although the infinity of pocket universes produced by eternalinflation are unobservable, it is argued that eternal inflation has realconsequences in terms of the way that predictions are extracted fromtheoretical models. The ambiguities in defining probabilities in eternallyinflating spacetimes are reviewed, with emphasis on the youngness paradox thatresults from a synchronous gauge regularization technique. To clarify (but notresolve) this ambiguity, a toy model of an eternally inflating universe isintroduced. Vilenkin's proposal for avoiding these problems is also discussed,as is the question of whether it is meaningful to discuss probabilities forunrepeatable measurements.""]",['2000-02-09'] +776,['eng'],"['Knox, L']",['The CMB success of adiabatic CDM'],['Astrophysics and Astronomy'],"['talk, Granlibakken 1999/12/10', 'astrophysics, missing-mass', 'model, adiabatic', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'topology, defect', 'astrophysics, fundamental constant', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002163'],"['The inflation-inspired flat, cold dark matter-dominated models of structureformation with adiabatic, nearly scale-invariant initial conditions agree verywell with current CMB anisotropy data. The success of these models ishighlighted by the failure of alternatives; we argue that there are no longerany viable competitors (with the exception of models with more complicatedmatter content which are still flat and which still require inflation). CMBdata will soon be of sufficient quality that, if one {\\it assumes} inflation,one can detect a non-zero cosmological constant by combining a determination ofthe peak location with Hubble constant measurements.']",['2000-02-09'] +777,['eng'],"['Kawasaki, M', 'Kohri, K', 'Sugiyama, N']",['MeV-scale Reheating Temperature and Thermalization of Neutrino Background'],['Astrophysics and Astronomy'],"['inflationary universe', 'entropy, production', 'Boltzmann equation, solution', 'neutrino, spectra', 'light nucleus, production', 'particle, massive', 'particle, decay', 'hadron, injection', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002127'],"['The late-time entropy production by the massive particle decay induces thevarious cosmological effects in the early epoch and modify the standardscenario. We investigate the thermalization process of the neutrinos after theentropy production by solving the Boltzmann equations numerically. We find thatif the large entropy are produced at t $\\sim$ 1 sec, the neutrinos are notthermalized very well and do not have the perfect Fermi-Dirac distribution.Then the freeze-out value of the neutron to proton ratio is alteredconsiderably and the produced light elements, especially He4, are drasticallychanged. Comparing with the observational light element abundances, we findthat $T_R$ < 0.7 MeV is excluded at 95 .L. We also study the case in whichthe massive particle has a decay mode into hadrons. Then we find that $T_R$should be a little higher, i.e. $T_R$ > 2.5 MeV - 4 MeV, for the hadronicbranching ratio $B_h = 10^{-2} - 1$. Possible influence of late-time entropyproduction on the large scale structure formation and temperature anisotropiesof cosmic microwave background is studied. It is expected that the futuresatellite experiments (MAP and PLANCK) to measure anisotropies of cosmicmicrowave background radiation temperature can detect the vestige of thelate-time entropy production as a modification of the effective number of theneutrino species $N_{\\nu}^{\\rm eff}$.']",['2000-02-08'] +778,['eng'],"['Chilingarian, A A', 'Gharagyozyan, G V', 'Kazarian, S', 'Hovsepyan, G G', 'Mamidjanyan, E A', 'Melkumyan, L G', 'Sokhoyan, S H']",['The Dependence of the Age Parameter from EAS Size and Zenith Angle of Incidence'],['Astrophysics and Astronomy'],"['talk, Nor-Amberd 1999/05/25', 'cosmic radiation', 'showers, air', 'showers, spatial distribution', 'parametrization', 'angular dependence', 'time dependence', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002077'],"['The quality of the MAKET-ANI detector installation in view of the uniformityof the registration efficiency is demonstrated. Based on a data samplecollected by the MAKET-ANI array in the period of June 1997 - March 1999, thedependencies of the age parameter on the zenith angle and the EAS size(10^5-10^7) are studied. The variation of the age parameter with the showersize can be approximately related to the elongation rate.']",['2000-02-04'] +779,['eng'],"['Chilingarian, A A', 'Gharagyozyan, G V', 'Kazarian, S', 'Hovsepyan, G G', 'Mamidjanyan, E A', 'Melkumyan, L G', 'Sokhoyan, S H']",['Determination of the EAS Attenuation Length from Data of the ANI Experiment'],['Astrophysics and Astronomy'],"['talk, Nor-Amberd 1999/05/25', 'cosmic radiation, secondary radiation', 'showers, air', 'absorption, length', 'angular dependence', 'cosmic radiation, primary', 'nucleus nucleus, interaction', 'air', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002076'],"['Using the EAS size spectra measured with the MAKET ANI array on Mt. Aragats,Armenia (3200m a.s.l.) in the range of the shower size 10^5 - 10^7 fordifferent angles-of-incidence, the EAS attenuation length has been determinedapplying different analysis methods. The analysis is based on a data sample of2.5*10^6 events collected in the period of June, 97 - April, 99. The resultsare compared with results deduced from data of the EAS TOP and KASCADEexperiments.']",['2000-02-04'] +780,['eng'],"['Kurki-Suonio, H']",['Alternative Solutions to Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'n, diffusion', 'antimatter', 'neutrino, oscillation', 'neutrino/tau, decay', 'energy, density', 'helium, yield', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002071'],"['Standard big bang nucleosynthesis (SBBN) has been remarkably successful, andit may well be the correct and sufficient account of what happened. However,interest in variations from the standard picture come from two sources: First,big bang nucleosynthesis can be used to constrain physics of the earlyuniverse. Second, there may be some discrepancy between predictions of SBBN andobservations of abundances. Various alternatives to SBBN include inhomogeneousnucleosynthesis, nucleosynthesis with antimatter, and nonstandard neutrinophysics.']",['2000-02-04'] +781,['eng'],"['Schneider, R', 'Ferrari, V', 'Matarrese, S', 'Zwart, S F P']",['Gravitational waves from cosmological compact binaries'],['Astrophysics and Astronomy'],"['gravitational radiation, particle source', 'binary', 'n, matter', 'black hole', 'astrophysics, white dwarf', 'background, stochastic', 'counters and detectors', 'interference, laser', 'energy spectrum', 'matter, production', 'numerical calculations', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002055'],"['We consider gravitational waves emitted by various populations of compactbinaries at cosmological distances. We use population synthesis models tocharacterize the properties of double neutron stars, double black holes anddouble white dwarf binaries as well as white dwarf-neutron star, whitedwarf-black hole and black hole-neutron star systems. We use theobservationally determined cosmic star formation history to reconstruct theredshift distribution of these sources and their merging rate evolution. Thegravitational signals emitted by each source during its early-inspiral phaseadd randomly to produce a stochastic background in the low frequency band withspectral strain amplitude between 10^{-18} Hz^{-1/2} and 5 10^{-17} Hz^{-1/2} at frequencies in the interval [5 10^{-6}-5 10^{-5}] Hz.The overall signal which, at frequencies above 10^{-4}Hz, is largely dominatedby double white dwarf systems, might be detectable with LISA in the frequencyrange [1-10] mHz and acts like a confusion limited noise component which mightlimit the LISA sensitivity at frequencies above 1 mHz.']",['2000-02-03'] +782,['eng'],"['Magueijo, J', 'Brandenberger, R H']",['Cosmic defects and cosmology'],['Astrophysics and Astronomy'],"['lectures, Tehran 1999/01/23', 'astrophysics, string', 'topology, defect', 'critical phenomena', 'defect, production', 'scaling', 'cosmic radiation, background', 'spectra, fluctuation', 'correlation function', 'baryon, production', 'domain wall', 'magnetic monopole', 'perturbation, coherence', 'causality', 'energy, density', 'inflationary universe', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002030'],"[""We provide a pedagogical overview of defect models of structure formation. We first introduce the concept of topological defect, and describe how to classify them. We then show how defects might be produced in phase transitions in the Early Universe and approach non-pathological scaling solutions. A very heuristic account of structure formation with defects is then provided, following which we introduce the tool box required for high precision calculations of CMB and LSS power spectra in these theories. The decomposition into scalar vector and tensor modes is reviewed, and then we introduce the concept of unequal-time correlator. We use isotropy and causality to constrain the form of these correlators. We finally show how these correlators may be decomposed into eigenmodes, thereby reducing a defect problem to a series of ``inflation'' problems. We conclude with a short description of results in these theories and how they fare against observations. We finally describe yet another application of topological defects in cosmology: baryogenesis.""]",['2000-02-02'] +783,['eng'],"['Dar, Arnon', 'De Rújula, Alvaro']",['Soft Gamma-Ray repeaters and anomalous x-ray pulsars'],['Astrophysics and Astronomy'],"['pulsar', 'photon, cosmic radiation', 'n, matter', 'jet, relativistic', 'radiation, magnetic', 'magnetic field', 'matter, strangeness', 'quark, matter', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002014'],"[""Recent measurements of the spin-down rates of soft gamma ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) have been interpreted as evidence that these objects are ``magnetars'': neutron stars spinning down by magnetic dipole radiation, but with a magnetic field two orders of magnitude larger than that of ordinary neutron stars. We discuss the evidence disfavouring this interpretation. We argue that, instead, the observations support the hypothesis that SGRs and AXPs are neutron stars that have suffered a transition into a denser form of nuclear matter to become, presumably, strange stars or quark stars.""]",['2000-02-02'] +784,['eng'],"['Olinto, A V']",['Ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'astrophysics, acceleration', 'model, hybrid', 'galaxy, AGN', 'n, matter', 'photon, cosmic radiation', 'p, cosmic radiation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0002006'],['The origin of the highest-energy cosmic rays remains a mystery. The lack of a high energy cutoff in the cosmic ray spectrum together with an apparently isotropic distribution of arrival directions have strongly constrained most models proposed for the generation of these particles. An overview of the present state of theoretical proposals is presented. Astrophysical accelerators as well as top-down scenarios are reviewed along with their most general signatures. The origin and nature of these ultra-high energy particles will be tested by future observations and may indicate as well as constrain physics beyond the standard model of particle physics.'],['2000-02-02'] +785,['eng'],"['Konopelko, A K', 'Plyasheshnikov, A V']",['ALTAI'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'radiation, Cherenkov', 'showers, electromagnetic', 'multiple scattering', 'charged particle, energy loss', 'showers, hadronic', 'nucleus nucleus, nuclear reaction', 'Cherenkov counter, imaging', 'programming, Monte Carlo', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001541'],['Ground-based atmospheric Cherenkov telescopes are proven to be effective instruments for observations of very high energy (VHE) gamma-radiation from celestial objects. For effective use of such technique one needs detailed Monte Carlo simulations of gamma-ray- and proton/nuclei-induced air showers in Earth atmosphere. Here we discuss in detail the algorithms used in the numerical code ALTAI developed particularly for the simulations of Cherenkov light emission from air showers of energy below 50 TeV. The specific scheme of sampling the charged particle transport in the atmosphere allows the performance of very fast and accurate simulations used for interpretation of the VHE gamma-ray observations.'],['2000-02-01'] +786,['eng'],"['Bertou, X', 'Boratav, M', 'Letessier-Selvon, A A']",['Physics of Extremely High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'elements, cosmic radiation', 'cosmic radiation, secondary radiation', 'showers, air', 'counters and detectors', 'neutrino, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'cosmic radiation, anisotropy', 'magnetic field, effect', 'supersymmetry', 'LSP', 'cosmic radiation, acceleration', 'astrophysics', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001516'],"['Over the last third of the century, a few tens of events, detected by ground-based cosmic ray detectors, have opened a new window in the field of high-energy astrophysics. These events have macroscopic energies, unobserved sources, an unknown chemical composition and a production and transport mechanism yet to be explained. With a flux as low as one particle per century per square kilometer, only dedicated detectors with huge apertures can bring in the high-quality and statistically significant data needed to answer those questions. In this article, we review the present status of the field both from an experimental and theoretical point of view. Special attention is given to the next generation of detectors devoted to the thorough exploration of the highest energy ranges']",['2000-02-01'] +787,['eng'],"['Collar, J I', 'Puibasset, J', 'Girard, T A', 'Limagne, D', 'Miley, H S', 'Waysand, G']","['First Dark Matter Limits from a Large-Mass, Low-Background Superheated Droplet Detector']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'search for, missing-mass', 'counters and detectors, droplet', 'WIMP, search for', 'scattering, WIMP p', 'energy spectrum', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001511'],"[""We report on the fabrication aspects and calibration of the first large active mass ($\\sim15$ g) modules of SIMPLE, a search for particle dark matter using Superheated Droplet Detectors (SDDs). While still limited by the statistical uncertainty of the small data sample on hand, the first weeks of operation in the new underground laboratory of Rustrel-Pays d'Apt already provide a sensitivity to axially-coupled Weakly Interacting Massive Particles (WIMPs) competitive with leading experiments, confirming SDDs as a convenient, low-cost alternative for WIMP detection.""]",['2000-01-31'] +788,['eng'],"['Bombaci, I', 'Datta, B']",['Conversion of neutron stars to strange stars as the central engine of $\\gamma$-ray bursts'],['Astrophysics and Astronomy'],"['n, matter', 'matter, strangeness', 'matter, transition', 'photon, cosmic radiation', 'energy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001478'],['We study the conversion of a neutron star to a strange star as a possible energy source for gamma-ray bursts. We use different recent models for the equation of state of neutron star matter and strange quark matter. We show that the total amount of energy liberated in the conversion is in the range of (1-4) 10^{53} ergs (one order of magnitude larger than previous estimates) and is in agreement with the energy required to power gamma-ray burst sources at cosmological distances.'],['2000-01-28'] +789,['eng'],"['Ferrari, V', ""D'Andrea, M"", 'Berti, E']",['Gravitational waves emitted by extrasolar planetary systems'],['Astrophysics and Astronomy'],"['astrophysics, matter', 'gravitational radiation, emission', 'binary', 'amplitude analysis', 'moment, multipole', 'scattering, resonance', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001463'],"['In this paper we consider the Extra-solar Planetary Systems recently discovered in our Galaxy as potential sources of gravitational waves. We estimate the frequency and characteristic amplitude of the radiation they emit due to the orbital motion, using the quadrupole formalism. In addition, we check whether the conditions needed for the resonant excitation of the f- and g-modes of the central star can be fulfilled. By a Roche-lobe analysis, we show that there could exist systems in which the low-order g-modes could be excited, although this does not happen in the systems discovered up to now.']",['2000-01-27'] +790,['eng'],"['Schertler, K', 'Greiner, C', 'Schaffner-Bielich, J', 'Thoma, M H']","['Quark phases in neutron stars and a ""third family"" of compact stars as a signature for phase transitions']",['Astrophysics and Astronomy'],"['n, matter', 'quark, matter', 'mean field approximation, relativistic', 'bag model', 'critical phenomena, confinement', 'transition, quark hadron', 'astrophysics, white dwarf', 'matter, mass', 'proposed experiment', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001467'],"['The appearance of quark phases in the dense interior of neutron stars provides one possibility to soften the equation of state (EOS) of neutron star matter at high densities. This softening leads to more compact equilibrium configurations of neutron stars compared to pure hadronic stars of the same mass. We investigate the question to which amount the compactness of a neutron star can be attributed to the presence of a quark phase. For this purpose we employ several hadronic EOS in the framework of the relativistic mean-field (RMF) model and an extended MIT bag model to describe the quark phase. We find that - almost independent of the model parameters - the radius of a pure hadronic neutron star gets typically reduced by 20-30% if a pure quark phase in the center of the star does exist. For some EOS we furthermore find the possibility of a ""third family"" of compact stars which may exist besides the two known families of white dwarfs and neutron stars. We show how an experimental proof of the existence of a third family by mass and radius measurements may provide a unique signature for a phase transition inside neutron stars.']",['2000-01-27'] +791,['eng'],"['Bassett, B A', 'Liberati, S', 'Molina-Paris, C', 'Visser, M']",['Geometrodynamics of Variable-Speed-of-Light Cosmologies'],['Astrophysics and Astronomy'],"['astrophysics, model', 'heterotic', 'photon, velocity', 'symmetry breaking, Lorentz', 'relativity theory, general', 'tensor, energy-momentum', 'entropy', 'space-time, Robertson-Walker', 'gravitation, lens', 'quintessence', 'space-time, horizon', 'fundamental constant, time variation', 'photon, polarization', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001441'],"[""This paper is dedicated to the memory of Dennis Sciama. Variable-Speed-of-Light (VSL) cosmologies are currently attracting great interest as an alternative to inflation. We investigate the fundamental geometrodynamic aspects of VSL cosmologies and provide several implementations which do not explicitly break Lorentz invariance (no ``hard'' breaking), and answer the question ``VSL with respect to what?''. This large class of VSL cosmologies are compatible with both classical Einstein gravity and low-energy particle physics. These models solve the ``kinematic'' puzzles of cosmology as well as inflation does, but cannot by themselves solve the flatness problem, since in their purest form no violation of the strong energy condition occurs. We also consider a heterotic model (VSL scalar field chi plus inflaton field phi) which provides a number of observational implications for the low-redshift universe if chi contributes to the ``dark energy'' either as CDM or quintessence. These implications include modified gravitational lensing, birefringence, variation of fundamental constants, and rotation of the plane of polarization of light from distant sources.""]",['2000-01-26'] +792,['eng'],"['Billoir, P', 'Letessier-Selvon, A A']",['Note on the Origin of the Highest Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'magnetic field, galaxy', 'p, tracks', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001427'],"['In this note we argue that the galactic model chosen by E.-J. Ahn, G. Medina-Tanco, P.L. Bierman and T. Stanev in their paper discussing the origin of the highest energy cosmic rays, is alone responsible for the focussing of positive particles towards the North galactic pole. We discuss the validity of this model, in particular in terms of field reversals and radial extensions. We conclude that with such a model one cannot retreive any directional information from the observed direction of the cosmic rays. In particular one cannot identify point sources at least up to energies of about 200 EeV. Therefore the apparent clustering of the back-traced highest energy cosmic rays observed to date cannot be interpreted as an evidence for a point source nor for the identification of M87, which happens to be close to the North pole, as being such a source.']",['2000-01-26'] +793,['eng'],"['Montanet, F']",['Design and expected performance of the ANTARES neutrino telescope'],['Astrophysics and Astronomy'],"['talk, Paris 1999/09/06', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'astrophysics, missing-mass', 'Cherenkov counter, water', 'photoelectron, amplifier', 'deep underground detector, ANTARES', 'deep underground detector, performance']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001380'],"['The ANTARES Collaboration is aiming at the construction and the operation of a large undersea neutrino telescope for neutrino astronomy, neutrino oscillation and indirect dark matter searches. Started 3 years ago an intensive R&D program has shown the feasibility of such a detector in the deep waters of the Mediterranean sea. We have now started the design and the construction of a 0.1 km(^{2}) detector for which the expected performance will be briefly described here.']",['2000-01-24'] +794,['eng'],"['Völk, H J']",['HEGRA Observations of Galactic Sources'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'astrophysics', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'supernova', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001301'],"[""In this talk I will first give a summary of the observations of expected Galactic TeV gamma-ray sources with the HEGRA CT-Sytem since the Kruger Park Workshop in 1997. Then I will go into some detail regarding the observations of Supernova Remnants (SNRs), especially those of Tycho's SNR and of Cas A. The emphasis will not be on all aspects of these published data. I will rather review the selection of these observational targets, and discuss some of the physical implications of the results.""]",['2000-01-18'] +795,['eng'],"['Sánchez, N', 'Anez, N']",['Neutrino decay and the thermochemical equilibrium of the interstellar medium'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, decay', 'photon, flux', 'ionization', 'stability', 'pressure', 'neutrino, flux', 'electron, density', 'gas, condensation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001274'],"['We calculate the thermochemical equilibrium of the diffuse interstellar medium, including ionization by a photon flux F_{nu} from neutrino decay. The main heating mechanism considered is photoelectrons from grains and PAHs. For the studied range of F_{nu} values, there always exists two regions of stability (a warm and a cold phase) that can coexist in equilibrium if the thermal interstellar pressure is between a maximum value P_{max} and a minimum value P_{min}. High F_{nu} values (~10^4-10^5 cm^{-2} s^{-1}) can be consistent with observed interstellar pressures only if more efficient sources are heating the gas. It is shown that a neutrino flux increase (due, for example, to an increase in the supernova explosion rate) may stimulate the condensation of cold gas by decreasing P_{max} below the interstellar pressure value.']",['2000-01-18'] +796,['eng'],"['Alcock, C B', 'Allsman, R A', 'Alves, D R', 'Axelrod, T S', 'Becker, A C', 'Bennett, D P', 'Cook, K H', 'Dalal, N', 'Drake, A J', 'Freeman, K C', 'Geha, M', 'Griest, K', 'Lehner, M J', 'Marshall, S L', 'Minniti, D', 'Nelson, C A', 'Peterson, B A', 'Popowski, P A', 'Pratt, M R', 'Quinn, P J', 'Stubbs, C W', 'Sutherland, W', 'Tomaney, A B', 'Vandehei, T', 'Welch, D']",['The MACHO Project'],['Astrophysics and Astronomy'],"['astrophysics', 'gravitation, lens', 'MACHO', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001272'],"['We report on our search for microlensing towards the Large Magellanic Cloud (LMC). Analysis of 5.7 years of photometry on 11.9 million stars in the LMC reveals 13 - 17 microlensing events. This is significantly more than the $\\sim$ 2 to 4 events expected from lensing by known stellar populations. The timescales ($\\that$) of the events range from 34 to 230 days. We estimate the microlensing optical depth towards the LMC from events with $2 < \\that < 400$ days to be 1.2 ^{+0.4}_ {-0.3} \\ten{-7}$, with an additional 20% to 30% of systematic error. The spatial distribution of events is mildly inconsistent with LMC/LMC disk self-lensing, but is consistent with an extended lens distribution such as a Milky Way or LMC halo. Interpreted in the context of a Galactic dark matter halo, consisting partially of compact objects, a maximum likelihood analysis gives a MACHO halo fraction of 20% for a typical halo model with a 95% confidence interval of 8% to 50%. A 100% MACHO halo is ruled out at the 95% C.L. for all except our most extreme halo model. Interpreted as a Galactic halo population, the most likely MACHO mass is between $ 0.15 \\msun$ and $ 0.9 \\msun$, depending on the halo model, and the total mass in MACHOs out to 50 kpc is found to be 9+4-3 10^{10} msun, independent of the halo model. These results are marginally consistent with our previous results, but are lower by about a factor of two. Besides a larger data set, this work also includes an improved efficiency determination, improved likelihood analysis, and more thorough testing of systematic errors, especially with respect to the treatment of potential backgrounds to microlensing, such as supernovae in galaxies behind the LMC. [Abridged]']",['2000-01-18'] +797,['eng'],"['Cline, David B']",['Search for Relic Neutrinos and Supernova Bursts'],['Astrophysics and Astronomy'],"['talk, Venice 1999/02/23', 'supernova', 'astrophysics, model', 'neutrino, cosmic radiation', 'neutrino, mass', 'deep underground detector', 'scintillation counter, proposed', 'neutrino, search for', 'neutrino, flux', 'neutrino, oscillation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001261'],"['We describe the current situation concerning methods to search for relic neutrinos from the Big Bang and from all past supernovae (SNs). The most promising method for Big Bang neutrinos is by the interaction of ultra-high- energy (UHE) neutrinos. For supernova neutrinos, both Super Kamiokande- and ICARUS-type detectors will be important to study both nubar_{e} and nu_{e} fluxes. We also discuss a dedicated supernova burst observatory (OMNIS) being planned for three sites in the world. We also describe the possible analysis of the supernova type-II (SNII) neutrinos, including flavor mixing, that might be carried out in the future.']",['2000-01-17'] +798,['eng'],"['Cormier, D', 'Holman, R']",['Metric Perturbations and Inflationary Phase Transitions'],['Astrophysics and Astronomy'],"['talk, Trieste 1999/09/27', 'inflationary universe', 'critical phenomena', 'space-time, perturbation', 'spectra, perturbation', 'perturbation, adiabatic', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001255'],['We study the out of equilibrium dynamics of inflationary phase transitions and compute the resulting spectrum of metric perturbations relevant to observation. We show that simple single field models of inflation may produce an adiabatic perturbation spectrum with a blue spectral tilt and that the precise spectrum depends on initial conditions at the outset of inflation.'],['2000-01-17'] +799,['eng'],"['Heyl, J S']",['Gravitational Radiation from Strongly Magnetized White Dwarfs'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'astrophysics, white dwarf', 'magnetic field, high', 'moment, multipole', 'interference, laser', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001343'],"['The magnetic fields of white dwarfs distort their shape generating an anisotropic moment of inertia. A magnetized white dwarf which rotates obliquely relative to the symmetry axis has a mass quadrupole moment which varies in time, so it will emit gravitational radiation. LISA may be able to detect the gravitational waves from two nearby, quickly rotating white dwarfs.']",['2000-01-20'] +800,['eng'],"['Völk, H J']",['The Diffusive Galactic GeV/TeV $\\gamma$-Ray Background'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'galaxy', 'supernova', 'cosmic radiation, diffusion', 'transport theory', 'energy, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001331'],"['The diffuse Galactic gamma-ray background, as observed with EGRET on CGRO, exceeds the model predictions significantly above 1 GeV. This is particularly true for the inner Galaxy. We shall discuss here the contribution of the Galactic Cosmic Ray (GCR) sources, considered as unresolved, and in addition the possibility that the transport of the GCRs out of the Galaxy is not uniform over the Galactic disk. In both cases the spectrum of the diffuse gamma-rays is harder than the GCR spectrum in the neighborhood of the Solar system, as observed in situ. The source contribution is a necessary and, as it turns out, significant part of the diffuse background, whereas the transport effect is one of several conceivable additional causes for the hard diffuse gamma-ray spectrum observed.']",['2000-01-20'] +801,['eng'],"['Dubovsky, S L', 'Tinyakov, Peter G', 'Tkachev, Igor I']",['Statistics of clustering of ultra-high energy cosmic rays and the number of their sources'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'energy spectrum', 'cosmic radiation, particle source', 'statistical analysis, cluster', 'astrophysics, model', 'galaxy, AGN', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001317'],"['Observation of clustering of ultra-high energy cosmic rays (UHECR) suggests that they are emitted by compact sources. Assuming small (smaller than ~3 degrees) deflection of UHECR during the propagation, the statistical analysis of clustering allows to estimate the total number of the sources S, including those which have not yet been observed directly. When applied to astrophysical models involving extra-galactic sources, the estimate gives S ~ 400 inside the sphere of the radius ~50 Mpc. This is too large for models which associate the production of UHECR with exceptional galaxies such as AGN, powerful radio-galaxies, dead quasars, and for models based on gamma ray bursts.']",['2000-01-19'] +802,['eng'],"['Medvedev, M V']","['Theory of ""Jitter"" Radiation from Small-Scale Random Magnetic Fields and Prompt Emission from $\\gamma$-Ray Burst Shocks']",['Astrophysics and Astronomy'],"['electron, relativistic', 'radiation, emission', 'magnetic field, random', 'radiation, spectra', 'photon, cosmic radiation', 'shock waves', 'model, composite', 'synchrotron radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001314'],"[""Abridged.-- We demonstrate that the radiation emitted by ultrarelativistic electrons in highly nonuniform, small-scale magnetic fields is different from synchrotron radiation if the electron's transverse deflections in these fields are much smaller than the beaming angle. A quantitative analytical theory of this radiation, which we refer to as jitter radiation, is developed. It is shown that the emergent spectrum is determined by statistical properties of the magnetic field. As an example,we then use the model of a magnetic field in internal shocks of GRBs. The spectral power distribution of radiation produced by the power-law electrons is well described by a sharply broken power-law with indices 1 and -(p-1)/2 and the jitter break frequency is independent of the field strength but depends on the electron density in the ejecta. Since large-scale fields may also be present in the ejecta, we construct a two-component, jitter+synchrotron spectral model of the prompt $\\gamma$-ray emission. Quite surprisingly, this model seems to be readily capable of explaining several properties of time-resolved spectra of some GRBs, such as (i) the violation of the constraint on the low-energy spectral index called the synchrotron ``line of death'', (ii) the sharp spectral break at the peak frequency, inconsistent with the broad synchrotron bump, (iii) the evidence for two spectral sub-components, and (iv) possible existence of emission features called ``GRB lines''. We believe these facts strongly support both the existence of small-scale magnetic fields and the proposed radiation mechanism from GRB shocks. As an example, we use the composite model to analyze GRB 910503 which has two spectral peaks.""]",['2000-01-19'] +803,['eng'],"['Dey, J', 'Ray, S', 'Li, X D', 'Dey, M', 'Bombaci, I']",['Glimpses of a strange star'],['Astrophysics and Astronomy'],"['matter, strangeness', 'quark, matter', 'photon, cosmic radiation', 'n, matter', 'rotator', 'energy, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001305'],"['There are about 2000 gamma ray burst (GRB) events known to us with data pouring in at the rate of one per day. While the afterglows of GRBs in radio, optical and X-ray bands are successfully explained by the fireball model, a significant difficulty with the proposed mechanisms for GRBs is that a small amount ($\\le 10^{-6} M_{\\odot}$) of baryons in the ejecta can be involved. There are very few models that fulfill this criteria together with other observational features, among which are the differentially rotating collapsed object model and the ""supernova"" model. These models generally invoke rapidly rotating neutron stars, and may be subject to uncertainties in the formation mechanisms and the equations of state of neutron stars. According to Spruit, the problem of making a GRB from an X-ray binary is reduced to finding a plausible way to make the star rotate differentially. We suggest that a model of strange star (SS) can naturally explain many of these bursts with not only their low baryon content, but the differential rotation which leads to an enhanced magnetic field that surfaces up and is responsible for GRBs.']",['2000-01-19'] +804,['eng'],"['Aloisio, R', 'Blasi, P', 'Ghia, P L', 'Grillo, A F']",['Probing The Structure of Space-Time with Cosmic Rays'],['Astrophysics and Astronomy'],"['relativity theory, validity test', 'cosmic radiation, scattering', 'radiation, background', 'energy, threshold', 'space-time', 'invariance, Lorentz', 'parametrization', 'photon photon, interaction', 'electron, pair production', 'pi, photoproduction', 'quantum gravity', 'group theory, deformation', 'dispersion relations', 'quantum space', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001258'],"[""The study of the interactions of Cosmic Rays (CR's) with universal diffuse background radiation can provide very stringent tests of the validity of Special Relativity. The interactions we consider are the ones characterized by well defined energy thresholds whose energy position can be predicted on the basis of Special Relativity. We argue that the experimental confirmation of the existence of these thresholds can in principle put very stringent limits on the scale where Special Relativity and/or continuity of space-time may possibly break down.""]",['2000-01-17'] +805,['eng'],"['Cline, David B']",['A WIMP Detector with Two-Phase Liquid Xenon'],['Astrophysics and Astronomy'],"['talk, Paris 1999/09/06', 'astrophysics, missing-mass', 'particle identification, WIMP', 'supersymmetry', 'scintillation counter, liquid', 'xenon, liquid', 'proposed experiment, deep underground detector']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001243'],"['We describe the liquid-xenon dark-matter detector program of the UCLA-Torino team. A two-phase detector, ZEPLIN II, for the Boulby Mine is a good match for the current search for WIMP dark matter.']",['2000-01-14'] +806,['eng'],"['Cline, David B']",['A Novel Supernova Detector'],['Astrophysics and Astronomy'],"['talk, Stony Brook 1999/09/23', 'neutrino, cosmic radiation', 'neutrino, mass', 'fast logic, time-of-flight', 'neutrino/mu', 'neutrino/tau', 'supernova', 'gadolinium', 'lithium', 'scintillation counter, liquid', 'scintillation counter, plastics', 'proposed experiment', 'deep underground detector, Soudan']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001237'],"['We discuss the prospects for detecting nu_{mu,tau} and nu_{tau}neutrinos from Type II supernovas using the novel detector at the Supernova Burst Observatory (SNBO) or OMNIS that is being designed for an underground laboratory in the USA. This detector would collect ~2000 flavor selected events from a Galactic supernova and could probe neutrino mass down to a few eV, as well as the dynamics of the supernova process. We believe this is essential to further our understanding of the neutrino section of elementary particle physics.']",['2000-01-14'] +807,['eng'],"['Wick, S D', 'Kephart, T W', 'Weiler, Thomas J', 'Biermann, P L']",['Signatures for a Cosmic Flux of Magnetic Monopoles'],['Astrophysics and Astronomy'],"['inflationary universe', 'magnetic monopole, flux', 'energy loss, electromagnetic', 'magnetic monopole, mass', 'magnetic field, galaxy', 'showers, air', 'radiation, Cherenkov', 'geophysics', 'cross section', 'magnetic monopole, color', 'magnetic monopole, bound state', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001233'],"[""Any early universe phase transition occurring after inflation has the potential to populate the universe with a flux of magnetic monopoles. Observations of galactic magnetic fields, and models for extragalactic magnetic fields, lead to the conclusion that monopoles of mass $\\lsim 10^{15}$ GeV are accelerated in these fields to relativistic velocities. We explore the possible signatures of a cosmic flux of relativistic monopoles impinging on the earth. The electromagnetically-induced signatures of monopoles are reliable. The hadronically-induced signatures are highly model-dependent. Among our findings are (i) the electromagnetic energy losses of monopoles continuously initiate a protracted shower of small intensity; (ii) monopoles may traverse the earth's diameter, making them a probe of the earth's interior structure; (iii) the best search strategy for monopoles is detection of their radio-Cherenkov signal produced by the coherent charge-excess in the $e^+-e^-$ shower --- in fact, underground radio-detectors have the potential to discover a monopole flux (or limit it) several orders of magnitude below the theoretical Parker limit of $10^{-15}$/$\\rm{cm}^2$/s/sr; (iv) it is conceivable (but not compelling) that bound states of colored monopoles may be the primary particles initiating the air showers observed above the GZK cutoff.""]",['2000-01-14'] +808,['eng'],"['Ioka, K', 'Taniguchi, K']",['Gravitational waves from inspiralling compact binaries with magnetic dipole moments'],['Astrophysics and Astronomy'],"['gravitational radiation', 'n, matter', 'magnetic moment', 'radiation, electromagnetic', 'coupling, magnetic', 'magnetic field, effect', 'photon, cosmic radiation', 'matter, orbit', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001218'],"['We investigate the effects of the magnetic dipole-dipole coupling and the electromagnetic radiation on the frequency evolution of gravitational waves from inspiralling binary neutron stars with magnetic dipole moments. This study is motivated by the discovery of the superstrongly magnetized neutron stars, i.e., magnetar. We derive the contributions of the magnetic fields to the accumulated cycles in gravitational waves as $N_{mag} \\sim 6 \\times 10^{-3} (H/10^{16}{\\rm G})^{2}$, where $H$ denotes the strength of the polar magnetic fields of each neutron star in the binary system. It is found that the effects of the magnetic fields will be negligible for the detection and the parameter estimation of gravitational waves, if the upper limit for magnetic fields of neutron stars are less than $\\sim 10^{16}$G, which is the maximum magnetic field observed in the soft gamma repeaters and the anomalous X-ray pulsars up to date. We also discuss the implications of electromagnetic radiation from the inspiralling binary neutron stars for the precursory X-ray emission prior to the gamma ray burst observed by the Ginga satellite.']",['2000-01-14'] +809,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Hnatyk, B I', 'Vilenkin, A']",['Superconducting cosmic strings as $\\gamma$ Ray Burst engines'],['Astrophysics and Astronomy'],"['astrophysics, string', 'string, superconducting', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'electron, acceleration', 'synchrotron radiation, emission', 'shock waves']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001213'],"['Cusps of superconducting strings can serve as GRB engines. A powerful beamed pulse of electromagnetic radiation from a cusp produces a jet of accelerated particles, whose propagation is terminated by the shock responsible for GRB. A single free parameter, the string scale of symmetry breaking $\\eta \\sim 10^{14} GeV$, successfully explains the typical values of GRB duration, fluence, the rate of bursts, as well as the observed ranges of these quantities. The wiggles on the string can drive the short-time structures of GRB. The model predicts reoccurance of GRBs with a period of about 20 yrs. The cusp mechanism resolves also some problems of GRBs as sources of Ultra High Energy Cosmic Rays.']",['2000-01-13'] +810,['eng'],"['Araya-Gochez, R A']",['An Instability-driven Dynamo for $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['talk, College Park 1999/10/11', 'photon, cosmic radiation', 'accretion', 'stability', 'flux, magnetic', 'energy, magnetic', 'neutrino, luminosity']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001192'],"[""We show that an MHD-instability driven dynamo (IDD) operating in a hot accretion disk is capable of generating energetically adequate magnetic flux deposition rates above and below a mildly advective accretion disk structure. The dynamo is driven by the magnetorotational instability (MRI) of a toroidal field in a shear flow and is limited by the buoyancy of `horizontal' flux and by reconnection in the turbulent medium. The efficiency of magnetic energy deposition is estimated to be comparable to the neutrino losses although an MHD collimation mechanism may deem this process a more viable alternative to neutrino-burst-driven models of gamma ray bursts.""]",['2000-01-12'] +811,['eng'],"['Vergados, J D']",['The modulation effect for supersymmetric dark matter detection with asymmetric velocity dispersion'],['Astrophysics and Astronomy'],"['talk, Dubna 1999/06/28', 'astrophysics, missing-mass', 'search for, missing-mass', 'supersymmetry', 'effect, time variation', 'elastic scattering, nucleus sparticle', 'LSP, mass', 'velocity, dispersion', 'nucleon, form factor', 'amplitude analysis', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001190'],"[""The detection of the theoretically expected dark matter is central to particle physics cosmology. Current fashionable supersymmetric models provide a natural dark matter candidate which is the lightest supersymmetric particle (LSP). Such models combined with fairly well understood physics like the quark substructure of the nucleon and the nuclear form factor and the spin response function of the nucleus, permit the evaluation of the event rate for LSP-nucleus elastic scattering. The thus obtained event rates are, however, very low or even undetectable. So it is imperative to exploit the modulation effect, i.e. the dependence of the event rate on the earth's annual motion. In this review we study such a modulation effect in directional and undirectional experiments. We calculate both the differential and the total rates using symmetric as well as asymmetric velocity distributions. We find that in the symmetric case the modulation amplitude is small, less than 0.07. There exist, however, regions of the phase space and experimental conditions such that the effect can become larger. The inclusion of asymmetry, with a realistic enhanced velocity dispersion in the galactocentric direction, yields the bonus of an enhanced modulation effect, with an amplitude which for certain parameters can become as large as 0.46.""]",['2000-01-12'] +812,['eng'],"['Atoyan, A M', 'Aharonian, F A', 'Tuffs, R J', 'Völk, H J']",['On the $\\gamma$-ray fluxes expected from Cassiopeia A'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, flux', 'electron, acceleration', 'electron, bremsstrahlung', 'supernova', 'pi0, decay', 'cosmic radiation, energy spectrum', 'synchrotron radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001186'],"['Based on the results of our previous study of the broad band synchrotron emission of Cas A in the framework of a spatial inhomogeneous model, we calculate the fluxes of gamma-radiation that can be expected from this supernova remnant in different energy bands. We show that at energies below 10 GeV gamma-ray fluxes detectable by forthcoming space-borne detectors should be produced due to bremsstrahlung of radio emitting electrons. We predict that the power-law index of the photon flux in the GeV region should be hard, close to the index ~2.2 expected for the acceleration spectrum of the electrons. Photon fluxes accessible to future ground-based gamma-ray detectors could also be expected at very high energies. The fluxes to be expected due to bremsstrahlung and inverse Compton radiation of relativistic electrons at TeV energies should be very steep, and strongly dependent on the characteristic magnetic fields in Cas A. We could expect also significant fluxes of pi^0 -decay gamma-rays produced by relativistic protons. These fluxes may extend with a hard spectrum beyond TeV energies as far as the protons would be accelerated to energies beyond 100 TeV. The hardness of the gamma-ray spectrum at TeV energies could in principle allow one to distinguish between electronic and hadronic origins of those gamma-rays. We discuss also other implications, such as relativistic particle content, or physical parameters in the source, that could be derived from future gamma-ray flux measurements in different energy bands.']",['2000-01-12'] +813,['eng'],"['Balkanov, V A']",['The Lake Baikal neutrino experiment'],['Astrophysics and Astronomy'],"['talk, Dubna 1999/06/28', 'muon, cosmic radiation', 'neutrino, cosmic radiation', 'WIMP, annihilation', 'magnetic monopole, search for', 'cosmic radiation, angular distribution', 'flux, upper limit', 'water, monitoring', 'Cherenkov counter, experimental results', 'deep underground detector, Baikal']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001151'],"['We review the present status of the lake Baikal Neutrino Experiment and present selected physical results gained with the consequetive stages of the stepwise increasing detector: from NT-36 to NT-96. Results cover atmospheric muons, neutrino events, very high energy neutrinos, search for neutrino events from WIMP annihilation, search for magnetic monopoles and environmental studies. We also describe an air Cherenkov array developed for the study of angular resolution of NT-200.']",['2000-01-11'] +814,['eng'],"['Baggio, L', 'Cerdonio, M', 'Ortolan, A', 'Vedovato, G', 'Taffarello, L', 'Zendri, J P', 'Bonaldi, M', 'Falferi, P', 'Martinucci, V', 'Mezzena, R', 'Prodi, G A', 'Vitale, S']",['Testing of optimal filters for gravitational wave signals'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'mass, resonance', 'signal processing', 'electronics, background', 'statistical analysis', 'effect, stochastic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001148'],"['We have implemented likelihood testing of the performance of an optimal filter within the online analysis of AURIGA, a sub-Kelvin resonant-bar gravitational wave detector. We demonstrate the effectiveness of this technique in discriminating between impulsive mechanical excitations of the resonant-bar and other spurious excitations. This technique also ensures the accuracy of the estimated parameters such as the signal-to-noise ratio. The efficiency of the technique to deal with non-stationary noise and its application to data from a network of detectors are also discussed.']",['2000-01-11'] +815,['eng'],"['Balkanov, V A']",['The Lake Baikal neutrino experiment'],['Astrophysics and Astronomy'],"['talk, Paris 1999/09/06', 'neutrino, cosmic radiation', 'neutrino, energy', 'neutrino, flux', 'upper limit', 'Cherenkov counter, water', 'experimental results', 'deep underground detector, Baikal']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001145'],['We rewiew the present status of the Baikal Neutrino Project and present the results of a search for high energy neutrinos with the detector intermediate stage NT-96.'],['2000-01-11'] +816,['eng'],"['Ziaeepour, H']",['Searching the Footprint of WIMPZILLAs'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'postulated particle, mass', 'postulated particle, decay', 'postulated particle, lifetime', 'WIMPZILLA', 'Boltzmann equation, solution', 'cross section', 'photon, cosmic radiation', 'p, cosmic radiation', 'cosmic radiation, particle source', 'energy, flux', 'galaxy', 'numerical calculations, Monte Carlo', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001137'],"['We constrain mass, lifetime and contribution of a very slowly decaying Ultra Heavy Dark Matter (UHDM) by simulating the cosmological evolution of its remnants. Most of interactions which participate in energy dissipation are included in the numerical solution of the Boltzmann equation. Cross-sections are calculated either analytically or by using PYTHIA Monte Carlo program. This paper describes in detail our simulation. To show the importance of the distribution of matter in constraining WIMPZILLA characteristics, we consider two extreme cases: a homogeneous universe, and a local halo with uniform distribution. We show that in a homogeneous universe, the decay of UHDM with a mass $\\sim 10^{15} GeV$ and a lifetime $\\sim$ a few times $\\tau_0$ the age of the Universe, can not explain the flux of observed Ultra High Energy Cosmic Rays (UHECRs). This shows the importance of nearby sources, notably galactic halo. In a uniform clump with an over-density of $\\sim 200$ extended to $100 kpc$ or more, the lifetime must be $\\sim 10 - 100 \\tau_0$ or the contribution in the DM must be proportionally smaller. If the model developed by DIRBE group for estimating galactic IR underestimates the Galactic background or there is a significant galactic radio background, the lifetime can approach the lower limit of this range. We also compare our calculation with observed distribution of UHDM with relatively short lifetime.']",['2000-01-11'] +817,['eng'],"['Ushomirsky, G', 'Bildsten, L', 'Cutler, C']",['Gravitational Waves from Low-Mass X-ray Binaries'],['Astrophysics and Astronomy'],"['talk, Pasadena 1999/07/12', 'gravitational radiation, emission', 'n, matter', 'spin', 'matter, accretion', 'moment, multipole', 'counters and detectors', 'interference, laser', 'stability', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001129'],"['We summarize the observations of the spin periods of rapidly accreting neutron stars. If gravitational radiation is responsible for balancing the accretion torque at the observed spin frequencies of ~300 Hz, then the brightest of these systems make excellent gravitational wave sources for LIGO-II and beyond. We review the recent theoretical progress on two mechanisms for gravitational wave emission: mass quadrupole radiation from deformed neutron star crusts and current quadrupole radiation from r-mode pulsations in neutron star cores.']",['2000-01-11'] +818,['eng'],"['Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G', 'Dingus, B L', 'Dorfan, D E', 'Ellsworth, R W', 'Evans, D', 'Falcone, A D', 'Fleysher, L', 'Fleysher, R', 'Gisler, G', 'Goodman, J A', 'Haines, T J', 'Hoffman, C M', 'Hugenberger, S', 'Kelley, L A', 'Leonor, I', 'McConnell, M', 'McCullough, J F', 'McEnery, J E', 'Miller, R S', 'Mincer, A I', 'Morales, M F', 'Némethy, P', 'Ryan, J M', 'Shen, B', 'Shoup, A L', 'Sinnis, C', 'Smith, A J', 'Sullivan, G W', 'Tumer, T O', 'Wang, K', 'Wascko, M O', 'Westerhoff, S', 'Williams, D A', 'Yang, T', 'Yodh, G B']",['Evidence for TeV Emission from GRB 970417a'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'photon, showers', 'Cherenkov counter, water', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001111'],"['Milagrito, a detector sensitive to very high energy gamma rays, monitored the northern sky from February 1997 through May 1998. With a large field of view and a high duty cycle, this instrument was well suited to perform a search for TeV gamma-ray bursts (GRBs). We report on a search made for TeV counterparts to GRBs observed by BATSE. BATSE detected 54 GRBs within the field of view of Milagrito during this period. An excess of events coincident in time and space with one of these bursts, GRB 970417a, was observed by Milagrito. The excess has a chance probability of $2.8 \\times 10^{-5}$ of being a fluctuation of the background. The probability for observing an excess at least this large from any of the 54 bursts is $1.5 \\times 10^{-3}$. No significant correlations were detected from the other bursts.']",['2000-01-10'] +819,['eng'],"['Muraishi, H', 'Tanimori, T', 'Yanagita, S', 'Yoshida, T', 'Moriya, M', 'Kifune, T', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, S', 'Hara, T', 'Kawachi, A', 'Kubo, H', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Patterson, J R', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Tamura, T', 'Yoshikoshi, T']",['Evidence for TeV $\\gamma$-ray emission from the shell type SNR RXJ1713.7-3946'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'cosmic radiation, background', 'microwaves, Compton scattering', 'electron, acceleration', 'shock waves', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001047'],"['We report the results of TeV gamma-ray observations of the shell type SNR RXJ1713.7-3946 (G347.3-0.5). The discovery of strong non-thermal X-ray emission from the northwest part of the remnant strongly suggests the existence of electrons with energies up to 100 TeV in the remnant, making the SNR a good candidate TeV gamma-ray source. We observed RXJ1713.7-3946 from May to August 1998 with the CANGAROO 3.8m atmospheric imaging Cerenkov telescope and obtained evidence for TeV gamma-ray emission from the NW rim of the remnant with the significance of 5.6 sigma. The observed TeV gamma-ray flux from the NW rim region was estimated to be (5.3 +/- 0.9[statistical] +/- 1.6[systematic]) * 10^{-12} photons cm^{-2} s^{-1} at energies >= 1.8 +/- 0.9 TeV. The data indicate that the emitting region is much broader than the point spread function of our telescope. The extent of the emission is consistent with that of hard X-rays observed by ASCA. This TeV gamma-ray emission can be attributed to the Inverse Compton scattering of the Cosmic Microwave Background Radiation by shock accelerated ultra-relativistic electrons. Under this assumption, a rather low magnetic field of 11 micro gauss is deduced for the remnant from our observation.']",['2000-01-06'] +820,['eng'],"['Pal, S', 'Bandyopadhyay, D', 'Greiner, W']",['$\\overline{K}^{0}$ condensation in neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'K-, condensation', 'anti-K0, condensation', 'mean field approximation, relativistic', 'potential, optical', 'coupling constant, (K meson)', 'K nucleon, scattering length', 'K, mass spectrum', 'energy, condensation', 'energy, density', 'pressure', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0001039'],"['We investigate the condensation of charged K^- meson and neutral $\\bar K^0$ meson in dense neutron star matter. Calculations are performed in relativistic mean field models in which both the baryon-baryon and (anti)kaon-baryon interactions are mediated by meson exchange. It is found that $\\bar K^0$ condensation is quite sensitive to the antikaon optical potential and depends more strongly on the nucleonic equation of state. For moderate values of antikaon potential and a rather stiff equation of state, a significant region of maximum mass star will contain $\\bar K^0$ meson. The critical density of the appearance of K^- and $\\bar K^0$ condensates, pairs of p-K^- and $n-\\bar K^0$ are produced with equal proportion leading to a perfectly symmetric matter of nucleons and antikaons in neutron stars. Along with K^- condensate, $\\bar K^0$ condensate makes the equation of state much softer resulting in smaller maximum mass stars compared to the case without any condensate.']",['2000-01-05'] +821,['eng'],"['Morales, A']",['Direct Detection of WIMP Dark Matter'],['Astrophysics and Astronomy'],"['review, Paris 1999/09/06', 'astrophysics, missing-mass', 'cosmic radiation, energy spectrum', 'time variation', 'WIMP, search for', 'elastic scattering, WIMP nucleus', 'cross section, mass', 'semiconductor detector, germanium', 'scintillation counter, sodium-iodide', 'cryogenics', 'experimental results']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912554'],['The status of the recent efforts in the direct search for Weak InteractingMassive Particle (WIMP) Dark Matter is briefly reviewed and the mainachievements illustrated by the contributions presented to TAUP 99. Thestrategies followed in the quest for WIMPs will be first revisited and then thenew results and the future prospects reported.'],['2000-03-01'] +822,['eng'],"['Hogan, C J']",['Warm Dark Matter'],['Astrophysics and Astronomy'],"['talk, Erice 1999/12/05', 'astrophysics, missing-mass', 'decoupling, relativistic', 'velocity, dispersion', 'density, perturbation', 'matter, density', 'quantum chromodynamics', 'weak interaction']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912549'],"[""The Cold Dark Matter paradigm successfully explains many phenomena on scaleslarger than galaxies, but seems to predict galaxy halos which are morecentrally concentrated and have a lumpier substructure than observed. Endowingcosmic dark matter with a small primordial velocity dispersion preserves thesuccessful predictions of the Cold Dark Matter scenario on large scales andimproves the agreement with halo structure. A ``phase density'' $Q$,proportional to the inverse entropy for nonrelativistic matter, is estimatedfor relativistically decoupled thermal or degenerate relic particles of mass$m_X$, with a numerical factor depending on the particle type but nocosmological parameters. Since $Q$ cannot increase for dissipationless,collisionless matter, at a given velocity dispersion there is a maximum spacedensity; this ``phase packing'' constraint eliminates the singular densitypredicted by CDM. The core radius and halo circular velocity scale analogouslyto degenerate dwarf stars. Particle velocities also filter primordialperturbations on a scale depending on $Q$ and on details of particledistributions. Particle candidates for warm matter are briefly discussed; forwarm thermal relics to have the observed mass density requires decoupling priorto the QCD epoch and therefore a superweak interaction with thermal StandardModel particles.""]",['2000-03-01'] +823,['eng'],"['Burdyuzha, V', 'Lalakulich, O', 'Ponomarev, Yu', 'Vereshkov, G M']",['The Forming of the Cosmological Constant'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'vacuum state, condensation', 'energy, density', 'space-time, geometry', 'critical phenomena, relativistic', 'Higgs particle, condensation', 'quantum chromodynamics', 'quantum cosmology']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912542'],"[""The problem of the physical nature and the cosmological constant genesis isdiscussed. This problem can't be solved in terms of the current quantum fieldtheory which operates with Higgs and nonperturbative vacuum condensates andtakes into account the changes of these condensates during relativistic phasetransitions. The problem can't be completely solved also in terms of theconventional global quantum theory: Wheeler-DeWitt quantum geometrodynamicsdoes not describe the evolution of the Universe in time (RPT in particular). Wehave investigated this problem in the context of energies density of differentvacuum subsystems characteristic scales of which pervaid all energetic scale ofthe Universe. At first the phemenological solution of the cosmological constantproblem and then the hypothesis about the possible structure of a new globalquantum theory are proposed. The main feature of this theory is theirreversible evolution of geometry and vacuum condensates in time in the regimeof their selforganization. The transformation of the cosmological constant indynamical variable is inevitably.""]",['2000-03-01'] +824,['eng'],"['Ghosh, T K', 'Chakrabarti, S']",['Can There be Quark Matter Core in a Strongly Magnetized Neutron Star?'],['Astrophysics and Astronomy'],"['n, matter', 'quark, matter', 'quark, droplet', 'magnetic field, effect', 'energy, surface', 'critical phenomena', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912527'],"['The effect of strong quantizing magnetic field on the nucleation of quark matter droplets and on the chemical evolution of nascent quark phase at the core of a neutron star are investigated. The surface energy of quark phase diverges logarithmically. As a consequence there can not be a first order transition to quark phase. However, a metal-insulator type of second order transition is possible unless the field strength exceeds $10^{20}$G. The study of chemical evolution of newborn quark phase shows that in $\\beta$-equilibrium the system becomes energetically unstable.']",['1999-12-29'] +825,['eng'],"['Lessard, R W', 'Bond, I H', 'Bradbury, S M', 'Buckley, J H', 'Burdett, A M', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', ""D'Vali, M"", 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Gillanders, G H', 'Hall, T', 'Hillas, A M', 'Krennrich, F', 'Lang, M J', 'Masterson, C', 'Moriarty, P', 'Quinn, J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Vasilev, V', 'Weekes, T C']",['Search for Pulsed TeV $\\gamma$-ray Emission from the Crab Pulsar'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'pulsar', 'cosmic radiation, energy', 'flux, upper limit', 'Cherenkov counter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912520'],"[""We present the results of a search for pulsed TeV emission from the Crab pulsar using the Whipple Observatory's 10 m gamma-ray telescope. The direction of the Crab pulsar was observed for a total of 73.4 hours between 1994 November and 1997 March. During this period the Whipple 10 m telescope was operated at its lowest energy threshold to date. Spectral analysis techniques were applied to search for the presence of a gamma-ray signal from the Crab pulsar over the energy band 250 GeV to 4 TeV. We do not see any evidence of the 33 ms pulsations present in other energy bands from the Crab pulsar. The 99.9% confidence level upper limit for pulsed emission above 250 GeV is derived to be 4.8x10^-12 cm^-2 s^-1 or <3% of the steady flux from the Crab Nebula. These results imply a sharp cut-off of the power-law spectrum seen by the EGRET instrument on the Compton Gamma-Ray Observatory. If the cut-off is exponential, it must begin at 60 GeV or lower to accommodate these upper limits.""]",['1999-12-28'] +826,['eng'],"['Novosyadlyj, B', 'Durrer, R', 'Gottlöber, S', 'Lukash, V N', 'Apunevych, S']",['Determination of cosmological parameters from a wide set of observational data on large scale structure of the Universe'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'cosmic radiation, background', 'temperature, fluctuation', 'baryon, density', 'neutrino, density', 'spectra, fluctuation', 'Hubble constant', 'astrophysics, fundamental constant', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912511'],"['The possibility of determining cosmological parameters on the basis of a wide set of observational data including the Abell-ACO cluster power spectrum and mass function, peculiar velocities of galaxies, the distribution of Ly-$\\alpha$ clouds and CMB temperature fluctuations is analyzed. Using a $\\chi^2$ minimization method, assuming $\\Omega_{\\Lambda}+\\Omega_{\\rm{matter}} =1 $ and no contribution from gravity waves, we found that a tilted $\\Lambda$MDM model with one sort of massive neutrinos and the parameters $n=1.12\\pm 0.10$, matches observational data best. The 1$\\sigma$ (68.3%) confidence limits on each cosmological parameter, which are obtained by marginalizing over the other parameters, are $0.82\\le $0\\leØmega_{\\nu}\\le 0.17$, $0.021\\le Ømega_b\\le 0.13$ and $0.38\\le h\\le 0.85$ $1.5\\le b_{cl}\\le 3.5$. Here $b_{cl}$ is the cluster bias parameter. The best-fit parameters for 31 models which are inside of $1\\sigma$ range of the best model are presented. It is shown also that observational data set used here rules out the class of CDM models with $h\\ge 0.5$, scale invariant primordial power spectrum, zero cosmological constant and spatial curvature at very high confidence level, $>99.99%$. The corresponding class of MDM models are ruled out at $\\sim 95%$ C.L.']",['1999-12-27'] +827,['eng'],"['Irastorza, I G', 'Cebrian, S', 'García, E', 'González, D', 'Morales, A', 'Morales, J', 'De Solorzano, A O', 'Peruzzi, A', 'Puimedón, J', 'Sarsa, M L', 'Scopel, S', 'Villar, J A']",['Prospects for solar axions searches with crystals via Bragg scattering'],['Astrophysics and Astronomy'],"['talk, Paris 1999/09/06', 'axion, solar', 'axion, search for', 'axion, radiative decay', 'Primakoff effect', 'Bragg scattering', 'solid-state counter, crystal', 'coupling constant, (axion 2photon)', 'axion, mass', 'experimental methods, proposed', 'numerical calculations', 'axion --> 2photon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912491'],['A calculation of the expected signal due to Primakov coherent conversion of solar axions into photons via Bragg scattering in several solid-state detectors is presented and compared with present and future experimental sensitivities. The axion window m_a > 0.03 eV (not accessible at present by other techniques) could be explored in the foreseeable future with crystal detectors to constrain the axion-photon coupling constant below the latest bounds coming from helioseismology. On the contrary a positive signal in the sensitivity region of such devices would imply revisiting other more stringent astrophysical limits derived for the same range of the axion mass. The application of this technique to the COSME germanium detector which is taking data at the Canfranc Underground Laboratory leads to a 95% C.L. limit g_a < 2.8 10^-9 GeV^-1.'],['1999-12-24'] +828,['eng'],"['Loinger, A']",['Vain is the pursuit of gravity waves'],['Astrophysics and Astronomy'],"['gravitational radiation, measurement', 'energy-momentum', 'counters and detectors, interference', 'differential equations', 'relativity theory, general', 'radiation, electromagnetic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912507'],['The modern apparatuses for the detection of the gravity waves are devised with the purpose to exploit the geodesic deviation generated by them. But the pseudo energy-momentum of these waves cannot exert any physical action on the apparatuses.'],['1999-12-24'] +829,['eng'],"['Kurki-Suonio, H', 'Sihvola, E']",['Constraining Antimatter Domains in the Early Universe with Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'antimatter, annihilation', 'antimatter, density', 'upper limit', 'helium, nuclide', 'cosmic radiation, background', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912473'],"['We consider the effect on big bang nucleosynthesis of a small-scale matter-antimatter domain structure (with more matter than antimatter) in the early universe. Depending on the size of the antimatter domains, antimatter annihilates before, during, or after nucleosynthesis. We place upper limits on the amount of antimatter at various domain sizes based on the abundances of light elements. For small domains, which annihilate before nucleosynthesis, the upper limit comes from underproduction of He-4. For larger domains, the limit comes from He-3 overproduction. Most of the He-3 from antiproton-helium annihilation is unable to escape far enough from the annihilation zone, and is annihilated later. The main source of He-3 is photodisintegration of He-4 by the electromagnetic cascades initiated by the high-energy photons and electrons produced by annihilation.']",['1999-12-23'] +830,['eng'],"['Atkins, R']",['Milagrito'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'Cherenkov counter, water', 'photoelectron, amplifier', 'electronics', 'data acquisition', 'calibration', 'performance', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912456'],"[""Milagrito, a large, covered water-Cherenkov detector, was the world's firstair-shower-particle detector sensitive to cosmic gamma rays below 1 TeV. Itserved as a prototype for the Milagro detector and operated from February 1997to May 1998. This paper gives a description of Milagrito, a summary of theoperating experience, and early results that demonstrate the capabilities ofthis technique.""]",['2000-03-01'] +831,['eng'],"['Habig, A']",['SNEWS'],['Astrophysics and Astronomy'],"['talk, College Park 1999/10/11', 'neutrino, cosmic radiation', 'supernova', 'galaxy', 'neutrino, particle identification', 'deep underground detector']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912293'],"['The detection of neutrinos from SN1987A confirmed the core-collapse nature of SN II, but the neutrinos were not noticed until after the optical discovery. The current generation of neutrino experiments are both much larger and actively looking for SN neutrinos in real time. Since neutrinos escape a new SN promptly while the first photons are not produced until the photospheric shock breakout hours later, these experiments can provide an early warning of a coming galactic SN II. A coincidence network between neutrino experiments has been established to minimize response time, eliminate experimental false alarms, and possibly provide some pointing to the impending event from neutrino wave-front timing.']",['1999-12-15'] +832,['eng'],"['Bulik, T', 'Rudak, B', 'Dyks, J']",['Spectral features in $\\gamma$-rays expected from millisecond pulsars'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'pulsar, particle source', 'photon electron, Compton scattering', 'electron, acceleration', 'cosmic radiation, energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912274'],"['In the advent of next generation gamma-ray missions, we present general properties of spectral features of high-energy emission above $1\\MeV$ expected for a class of millisecond, low magnetic field ($\\sim 10^9\\G$) pulsars. We extend polar-cap model calculations of Rudak & Dyks (1999) by including inverse Compton scattering events in ambient field of thermal X-ray photons and by allowing for two models of particle acceleration. In the range between $1\\MeV$ and a few hundred GeV the main spectral component is due to curvature radiation of primary particles. Synchrotron component due to secondary pairs becomes dominant only below $1\\MeV$. The slope of the curvature radiation spectrum in the energy range from $100\\MeV$ to $10\\GeV$ strongly depends on the model of longitudinal acceleration, whereas below $\\sim 100\\MeV$ all slopes converge to a unique value of 4/3 (in a $\\nu {\\cal F}_\\nu$ convention). The thermal soft X-ray photons, which come either from the polar cap or from the surface, are Compton upscattered to a domain of the VHE and form a separate spectral component peaking at $\\sim 1\\TeV$. We discuss observability of millisecond pulsars by future high energy instruments and present two rankings relevant for GLAST and MAGIC. We point to the pulsar J0437-4715 as a promising candidate for observations.']",['1999-12-15'] +833,['eng'],"['Madsen, J']",['Probing strange stars and color superconductivity by r-mode instabilities in millisecond pulsars'],['Astrophysics and Astronomy'],"['matter, strangeness', 'quark, matter', 'stability', 'astrophysics, pulsar', 'superconducting, color', 'flavor, 2', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912418'],"['R-mode instabilities in rapidly rotating quark matter stars (strange stars) lead to specific signatures in the evolution of pulsars with periods below 2.5 msec, and may explain the apparent lack of very rapid pulsars. Existing data seem consistent with pulsars being strange stars with a normal quark matter phase surrounded by an insulating nuclear crust. In contrast, bare strange stars and quark stars in a color-flavor-locked (CFL) phase are ruled out. Two-flavor color superconductivity (2SC) is marginally inconsistent with pulsar data.']",['1999-12-21'] +834,['eng'],"['Poirier, J', 'Carpenter, J', 'Gress, J', 'Lin, T F', 'Rösch, A']",['Composition of UHE Cosmic Ray Primaries'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0005089'],"['Project GRAND presents results on the atomic composition of primary cosmic rays. This is accomplished by determining the average height of primary particles that cause extensive air showers detected by Project GRAND. Particles with a larger cross sectional area, such as iron nuclei, are likely to start an extensive air shower higher in the atmosphere whereas protons, with a smaller cross section, would pass through more air before interacting and thus start showers at lower heights. Such heights can be determined by extrapolating identified muon tracks backward (upward) to determine their height of origin (Gress et al., 1997). Since muons are from the top, hadronic part of the shower, they are a good estimator for the beginning of the shower. The data for this study were taken during the previous year with 20 million shower events.']",['2000-05-05'] +835,['eng'],"['Becattini, F', 'Bottai, S']",['Extreme Energy $\\nu_{\\tau}$ Propagation Through the Earth'],['Astrophysics and Astronomy'],"['neutrino/tau, cosmic radiation', 'neutrino/mu, cosmic radiation', 'matter, effect', 'geophysics', 'neutrino nucleon, deep inelastic scattering', 'charged current', 'neutral current', 'tau, energy loss', 'cross section, energy dependence', 'neutrino, energy spectrum', 'numerical calculations, Monte Carlo']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=0003179'],"[""The propagation of extremely energetic nu_tau's through the Earth is studied by means of a detailed Monte Carlo simulation. All major mechanisms of nu_tau interactions and tau energy loss as well as all its relevant decay modes are properly taken into account. The detection possibility of nu_tau's emerging from Earth in forthcoming neutrino telescopes is addressed""]",['2000-03-14'] +836,['eng'],"['Kaplinghat, M', 'Steigman, G', 'Walker, T P']",['The Supernova Relic Neutrino Background'],['Astrophysics and Astronomy'],"['supernova', 'neutrino, cosmic radiation', 'background, upper limit', 'antineutrino/e, flux', 'metal', 'neutrino, oscillation', 'numerical calculations, KAMIOKANDE', 'numerical calculations, Sudbury']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912391'],"['An upper bound to the supernova relic neutrino background from all past Type II supernovae is obtained using observations of the Universal metal enrichment history. We show that an unambiguous detection of these relic neutrinos by the Super-Kamiokande detector is unlikely. We also analyze the event rate in the Sudbury Neutrino Observatory (where coincident neutrons from nu_e_bar + D --> 2 neutrons + positron, might enhance background rejection), and arrive at the same conclusion. If the relic neutrino flux should be observed to exceed our upper bound and if the observations of the metal enrichment history (for z<1) are not in considerable error, then either the Type II supernova rate does not track the metal enrichment history or some mechanism may be responsible for transforming nu_mu_bar and/or nu_tau_bar --> nu_e_bar.']",['1999-12-20'] +837,['eng'],"['Bilic, N', 'Nikolic, H', 'Viollier, R D']",['Fermion stars as gravitational lenses'],['Astrophysics and Astronomy'],"['gravitation, lens', 'fermion, matter', 'black hole, Schwarzschild', 'boson, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912381'],"['We study in detail gravitational lensing caused by a supermassive fermion star and compare it with lensing by a black hole of the same mass. It is argued that lensing effects, being very distinct, may shed some light on the yet unexplained nature of the compact dark massive object at the Galactic center.']",['1999-12-20'] +838,['eng'],"['Babusci, D', 'Giovannini, M']",['Maximal overlap and sensitivity of a VIRGO pair to graviton backgrounds'],['Astrophysics and Astronomy'],"['gravitational radiation, background', 'counters and detectors, interference', 'graviton, energy spectrum', 'scaling, invariance', 'search for, graviton', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912377'],['The sensitivity of a pair of VIRGO interferometers to gravitational waves backgrounds of cosmological origin is analyzed for the cases of maximal and minimal overlap of the two detectors. The improvements in the detectability prospects of scale-invariant and non-scale-invariant logarithmic energy spectra of relic gravitons are discussed.'],['1999-12-20'] +839,['eng'],"['Liddle, A R', 'Mazumdar, A']",['Perturbation amplitude in isocurvature inflation scenarios'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time, perturbation', 'amplitude analysis', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912349'],"['We make a detailed calculation of the amplitude of isocurvature perturbations arising from inflationary models in which the cold dark matter is represented by a scalar field which acquires perturbations during inflation. We use this to compute the normalization to large-angle microwave background anisotropies. Unlike the case of adiabatic perturbations, the normalization to COBE fixes the spectral index of the perturbations; if adiabatic perturbations are negligible then $n_{iso} \\simeq 0.4$. Such blue spectra are also favoured by other observational data. Although the pure isocurvature models are unlikely to adequately fit the entire observational data set, these results also have implications for models with mixed adiabatic and isocurvature perturbations.']",['1999-12-17'] +840,['eng'],"['Schwarz, Dominik J', 'Hofmann, S']",['Small-scale structure of cold dark matter'],['Astrophysics and Astronomy'],"['talk, Paris 1999/09/06', 'astrophysics, missing-mass', 'axion', 'neutralino', 'black hole', 'energy loss', 'radiation, fluid', 'quantum chromodynamics', 'critical phenomena']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912343'],"['We investigate the clumping of cold dark matter (CDM) at small scales. If the CDM particle is the neutralino, we find that collisional damping during its kinetic decoupling from the radiation fluid and free streaming introduce a small-scale cut-off in the primordial power spectrum of CDM. This cut-off sets the scale for the very first CDM objects in the Universe, which we expect to have a mass of $\\sim 10^{-12} M_\\odot$. For non-thermal CDM candidates, such as axions, wimpzillas, or primordial black holes, the cosmological QCD transition might induce features in the primordial spectrum at similar mass scales.']",['1999-12-17'] +841,['eng'],"['Mao, G', 'Chiba, S', 'Greiner, W', 'Oyamatsu, K']",['Vacuum discharge as a possible source of $\\gamma$-ray bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'vacuum state', 'p, pair production', 'n, matter', 'matter, scattering', 'black hole', 'anti-p p, annihilation', 'energy, production', 'dependence, impact parameter', 'anti-p, spectra', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912303'],['We propose that spontaneous particle--anti-particle pair creations from thedischarged vacuum caused by the strong interactions in dense matter are majorsources of $\\gamma$-ray bursts. Two neutron star collisions or blackhole-neutron star mergers at cosmological distance could produce a compactobject with its density exceeding the critical density for pair creations. Theemitted anti-particles annihilate with corresponding particles at the ambientmedium. This releases a large amount of energy. We discuss the spontaneous$p\\bar{p}$ pair creations within two neutron star collision and estimate theexploded energy from $p\\bar{p}$ annihilation processes. The total energy couldbe around $10^{51} - 10^{53}$ erg depending on the impact parameter ofcolliding neutron stars. This value fits well into the range of the initialenergy of the most energetic $\\gamma$-ray bursts. We suggest to measure theanti-proton spectra from the identical sources of $\\gamma$-ray bursts to testthe scenario.'],['2000-02-28'] +842,['eng'],"['Hannestad, S', 'Janka, H T', 'Raffelt, G G', 'Sigl, G']","['Electron-, $\\mu$-, and $\\tau$-Number Conservation in a Supernova Core']",['Astrophysics and Astronomy'],"['supernova', 'neutrino, mixing angle', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'flavor, conservation law', 'neutrino, diffusion', 'effect, refraction', 'decoherence']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912242'],"['We study if the neutrino mixing parameters suggested by the atmospheric neutrino anomaly imply chemical equilibrium between mu- and tau-flavored leptons in a supernova (SN) core. The initial flavor-conversion rate would indeed be fast if the nu_mu-nu_tau-mixing angle were not suppressed by second-order refractive effects. The neutrino diffusion coefficients are different for nu_mu, anti-nu_mu, nu_tau and anti-nu_tau so that neutrino transport may lead to a situation where the usual first-order refractive effects dominate. Either way, neutrino refraction guarantees the separate conservation of e, mu, and tau lepton number in a SN core, even when neutrino mixing angles are large.']",['1999-12-14'] +843,['eng'],"['Blasi, P', 'Epstein, R I', 'Olinto, A V']",['Ultra-High Energy Cosmic Rays from Young Neutron Star Winds'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'iron, acceleration', 'n, matter', 'magnetic field', 'supernova', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912240'],"['The long-held notion that the highest-energy cosmic rays are of distant extragalactic origin is challenged by observations that events above $\\sim 10^{20}$ eV do not exhibit the expected high-energy cutoff from photopion production off the cosmic microwave background. We suggest that these unexpected ultra-high-energy events are due to iron nuclei accelerated from young strongly magnetized neutron stars through relativistic MHD winds. We find that neutron stars whose initial spin periods are shorter than $\\sim 4 (B_S/10^{13}{\\rm G})^{1/2}$ ms, where $B_S$ is the surface magnetic field, can accelerate iron cosmic rays to greater than $\\sim 10^{20}$ eV. These ions can pass through the remnant of the supernova explosion that produced the neutron star without suffering significant spallation reactions. For plausible models of the Galactic magnetic field, the trajectories of the iron ions curve sufficiently to be consistent with the observed arrival directions of the highest energy events.']",['2000-01-06'] +844,['eng'],"['Nagano, M', 'Heck, D', 'Shinozaki, K', 'Inoue, N', 'Knapp, J']",['Comparison of AGASA data with CORSIKA simulation'],['Astrophysics and Astronomy'],"['cosmic radiation, cascade', 'showers, air', 'cosmic radiation, energy spectrum', 'particle, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912222'],"['An interpretation of AGASA (Akeno Giant Air Shower Array) data by comparing the experimental results with the simulated ones by CORSIKA (COsmic Ray SImulation for KASCADE) has been made. General features of the electromagnetic component and low energy muons observed by AGASA can be well reproduced by CORSIKA. The form of the lateral distribution of charged particles agrees well with the experimental one between a few hundred metres and 2000 m from the core, irrespective of the hadronic interaction model studied and the primary composition (proton or iron). It does not depend on the primary energy between 10^17.5 and 10^20 eV as the experiment shows. If we evaluate the particle density measured by scintillators of 5 cm thickness at 600 m from the core (S_0(600), suffix 0 denotes the vertically incident shower) by taking into account the similar conditions as in the experiment, the conversion relation from S_0(600) to the primary energy is expressed as E [eV] = 2.15 x 10^17 x S_0(600)^1.015, within 10% uncertainty among the models and composition used, which suggests the present AGASA conversion factor is the lower limit. Though the form of the muon lateral distribution fits well to the experiment within 1000 m from the core, the absolute values change with hadronic interaction model and primary composition. The slope of the rho_mu(600) (muon density above 1 GeV at 600 m from the core) vs. S_0(600) relation in experiment is flatter than that in simulation of any hadronic model and primary composition. Since the experimental slope is constant from 10^15 eV to 10^19 eV, we need to study this relation in a wide primary energy range to infer the rate of change of chemical composition with energy. keywords: cosmic ray, extensive air shower, simulation, primary energy estimation PACS number ; 96.40.De, 96.40.Pq']",['2000-01-06'] +845,['eng'],"['Turner, M S']","['Dark Matter, Dark Energy and Fundamental Physics']",['Astrophysics and Astronomy'],"['talk, Ann Arbor 1999/06/24', 'astrophysics, missing-mass', 'dark energy', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'astrophysics, fundamental constant', 'galaxy, cluster', 'astrophysics, history', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912211'],"['More than sixty years ago Zwicky made the case that the great clusters of galaxies are held together by the gravitational force of unseen (dark) matter. Today, the case is stronger and more precise: Dark, nonbaryonic matter accounts for 30% +/- 7% of the critical mass density, with baryons (most of which are dark) contributing only 4.5% +/- 0.5% of the critical density. The large-scale structure that exists in the Universe indicates that the bulk of the nonbaryonic dark matter must be cold (slowly moving particles). The SuperKamiokande detection of neutrino oscillations shows that particle dark matter exists, crossing an important threshold. Over the past few years a case has developed for a dark-energy problem. This dark component contributes about 80% +/- 20% of the critical density and is characterized by very negative pressure (p_X < -0.6 rho_X). Consistent with this picture of dark energy and dark matter are measurements of CMB anisotropy that indicate that total contribution of matter and energy is within 10% of the critical density. Fundamental physics beyond the standard model is implicated in both the dark matter and dark energy puzzles: new fundamental particles (e.g., axion or neutralino) and new forms of relativistic energy (e.g., vacuum energy or a light scalar field). A flood of observations will shed light on the dark side of the Universe over the next two decades; as it does it will advance our understanding of the Universe and the laws of physics that govern it.']",['1999-12-10'] +846,['eng'],"['Chudakov, A E', 'Petkov, V B', 'Poddubny, V Y', 'Voevodsky, A V']",['Around the Knee'],['Astrophysics and Astronomy'],"['talk, Karbardino-Balkaria 1999/04/19', 'cosmic radiation, electromagnetic component', 'muon, cosmic radiation', 'cosmic radiation, energy spectrum', 'showers, air', 'shower detector', 'deep underground detector, Baksan', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912192'],"['We present the experimental data on the knee, as observed in the electromagnatic and high energy muon (E\\mu \\ge 230 Gev) components.']",['1999-12-10'] +847,['eng'],"['Kujat, J', 'Scherrer, R J']",['The Effect of Time Variation in the Higgs Vacuum Expectation Value on the Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['electron, mass', 'Higgs model', 'time variation', 'ionization', 'cosmic radiation, background', 'spectra, fluctuation', 'fundamental constant, fine structure', 'nucleus, mass', 'binding energy', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912174'],"['A time variation in the Higgs vacuum expectation value alters the electron mass and thereby changes the ionization history of the universe. This change produces a measurable imprint on the pattern of cosmic microwave background (CMB) fluctuations. The nuclear masses and nuclear binding energies, as well as the Fermi coupling constant, are also altered, with negligible impact on the CMB. We calculate the changes in the spectrum of the CMB fluctuations as a function of the change in the electron mass. We find that future CMB experiments could be sensitive to |\\Delta m_e/m_e| \\sim |\\Delta G_F/G_F| \\sim 10^{-2} - 10^{-3}. However, we also show that a change in the electron mass is nearly, but not exactly, degenerate with a change in the fine-structure constant. If both the electron mass and the fine-structure constant are time-varying, the corresponding CMB limits are much weaker, particularly for l < 1000.']",['1999-12-09'] +848,['eng'],"['Dermer, C D', 'Chiang, J']",['High Energy Radiation from $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'photon photon, transparency', 'fireball', 'synchrotron radiation', 'energy spectrum', 'hadron, acceleration', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912164'],"['Gamma-ray burst (GRB) engines are probed most intimately during the prompt gamma-ray luminous phase when the expanding blast wave is closest to the explosion center. Using GRBs 990123 and 940217 as guides, we briefly review observations of high-energy emission from GRBs and summarize some problems in GRB physics. \\gamma\\gamma transparency arguments imply relativistic beaming. The parameters that go into the external shock model are stated, and we show numerical simulation results of gamma-ray light curves from relativistic blast waves with different amounts of baryon loading. A distinct component due to the synchrotron self-Compton process produces significant emission at GeV and TeV energies. Predictions for spectral and temporal evolution at these energies are presented for a blast wave expanding into uniform surroundings. Observations of the slow decay of GeV-TeV radiation provide evidence for ultra-high energy cosmic ray acceleration in GRBs.']",['1999-12-09'] +849,['eng'],"['Sumiyoshi, K', 'Suzuki, H', 'Otsuki, K', 'Terasawa, M', 'Yamada, S']",['Hydrodynamical study of neutrino-driven wind as an r-process site'],['Astrophysics and Astronomy'],"['n, matter', 'neutrino, cosmic radiation', 'model, hydrodynamical', 'relativity theory, general', 'light nucleus, production', 'neutrino, luminosity', 'mass, dependence', 'entropy', 'expansion, time', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912156'],"['We study the neutrino-driven wind from the proto-neutron star by the general relativistic hydrodynamical simulations. We examine the properties of the neutrino-driven wind to explore the possibility of the r-process nucleosynthesis. The numerical simulations with the neutrino heating and cooling processes are performed with the assumption of the constant neutrino luminosity by using realistic profiles of the proto-neutron star (PNS) as well as simplified models. The dependence on the mass of PNS and the neutrino luminosity is studied systematically. Comparisons with the analytic treatment in the previous studies are also done. In the cases with the realistic PNS, we found that the entropy per baryon and the expansion time scale are neither high nor short enough for the r-process within the current assumptions. On the other hand, we found that the expansion time scale obtained by the hydrodynamical simulations is systematically shorter than that in the analytic solutions due to our proper treatment of the equation of state. This fact might lead to the increase of the neutron-to-seed ratio, which is suitable for the r-process in the neutrino-driven wind. Indeed, in the case of massive and compact proto-neutron stars with high neutrino luminosities, the expansion time scale is found short enough in the hydrodynamical simulations and the r-process elements up to A ~ 200 are produced in the r-process network calculation.']",['1999-12-09'] +850,['eng'],"['Ormes, J', 'Moiseev, A', 'Wells, J']",['Interstellar Low Energy Antiprotons as a Probe of Dark Matter and Primordial Black Holes'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'astrophysics, missing-mass', 'missing-mass, annihilation', 'quark, production', 'quark, decay', 'anti-p, cosmic radiation', 'anti-p, flux', 'energy dependence', 'black hole', 'magnetic spectrometer, satellite', 'experimental equipment, proposed', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912140'],"['Cosmic ray antiprotons can originate from dark matter annihilating into quarks that subsequently decay into antiprotons. Evaporation of primordial black holes also can produce a significant antiproton flux. Since the spectrum of secondary antiprotons from cosmic ray interactions peaks at ~ 2 GeV and goes down sharply at lower energy, there is a window at energies < 1 GeV in which to look for excess antiprotons as a signature of these exotic antiproton sources. However, in the vicinity of the Earth low energy particles are strongly modulated by the solar wind, which makes any analysis ambiguous. The adverse effects of the solar wind can be avoided by placing a low energy antiproton spectrometer aboard an interstellar probe. The theoretical predictions are reviewed and the preliminary design of a light-weight, low-power instrument to make the measurements and a summary of the anticipated results are given in this paper.']",['1999-12-08'] +851,['eng'],"['Moiseev, A', 'Norris, J', 'Ormes, J', 'Ritz, S', 'Thompson, D']",['Anticoincidence Detector for GLAST'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'background', 'scintillation counter, plastics', 'optics, transformation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912138'],"[""The Gamma-ray Large Area Space Telescope (GLAST) is now being designed by a number of collaborating institutions. It will study the cosmic gamma radiation from 20 MeV to 300 GeV with high precision and sensitivity, greatly expanding on the important EGRET results. One of the key systems of the instrument, the Anticoincidence Detector (ACD), is designed to reject the majority of charged particles, which are the background for any gamma-ray experiment. The ACD of EGRET has suffered from the self-veto effect when the products of the high energy photon interactions in the instrument's calorimeter cause a veto signal in the anticoincidence detector (backsplash effect), resulting in the degradation of the efficiency for high energy (> 5 GeV) gamma rays. To avoid this effect, the ACD for GLAST is divided into many scintillating tiles with wave-shifting fiber readout. The design of this detector along with the beam test and simulation results are given in this paper.""]",['1999-12-08'] +852,['eng'],"['Norris, J P', 'Bonnell, J T', 'Marani, G F', 'Scargle, J D']","['GLAST, GRBs and Quantum Gravity']",['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'quantum gravity, effect', 'dispersion, energy dependence', 'statistics', 'counters and detectors, proposed', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912136'],"['The fast temporal structures and cosmological distances of gamma-ray bursts (GRBs) afford a natural laboratory for testing theories of frequency-dependent propagation of high-energy photons, as predicted for quantum gravity (QG). We calibrate the sensitivity of the proposed Gamma-ray Large Area Space Telescope (GLAST) by performing simulations which include: the response of GLAST to a GRB fluence distribution; a distribution of spectral power-law indices similar to the EGRET sample; and consideration of gamma-gamma attenuation, significant above ~ 10 GeV for redshifts z > 3 - 5. We find that GLAST should detect > 200 GRBs per year, with sensitivity to a few tens of GeV for a few bursts. GLAST could detect the energy- and distance-dependent dispersion (10 ms / GeV / Gpc) predicted by QG with 1 - 2 years of observations. Attribution to QG would require correlation of GRB redshifts with the temporal and energetic signatures.']",['1999-12-08'] +853,['eng'],"['Sambruna, R M']",['Understanding Blazar Jets Through Their Multifrequency Emission'],['Astrophysics and Astronomy'],"['astrophysics, blazar', 'galaxy, AGN', 'jet, relativistic', 'energy spectrum', 'particle, emission', 'cosmic radiation, acceleration', 'quasar', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912129'],"[""Being dominated by non-thermal (synchrotron and inverse Compton) emission from a relativistic jet, blazars offer important clues to the structure and radiative processes in extragalactic jets. Crucial information is provided by blazars' spectral energy distributions from radio to gamma-rays (GeV and TeV energies), their trends with bolometric luminosity, and their correlated variability properties. This review is focussed on recent multiwavelength monitorings of confirmed and candidate TeV blazars and the constraints they provide for the radiative properties of the emitting particles. I also present recent observations of the newly discovered class of ``blue quasars'' and the implications for current blazars' unification schemes.""]",['1999-12-08'] +854,['eng'],"['Anchordoqui, L A', 'Dova, M T', 'McCauley, T P', 'Reucroft, S', 'Swain, J D']",['Unmasking the tail of the cosmic ray spectrum'],['Astrophysics and Astronomy'],"['nucleon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'data analysis method', 'nucleus, cosmic radiation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912081'],"['A re-examination of the energy cosmic ray spectrum above $10^{20}$ eV is presented. The overall data-base provides evidence, albeit still statistically limited, that non-nucleon primaries could be present at the end of the spectrum. In particular, the possible appearance of superheavy nuclei (seldom discussed in the literature) is analysed in detail.']",['1999-12-06'] +855,['eng'],"['Baring, M G']","['Cosmic Ray Origin, Acceleration and Propagation']",['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'cosmic radiation, diffusion', 'astrophysics']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912058'],"['This paper summarizes highlights of the OG3.1, 3.2 and 3.3 sessions of the XXVIth International Cosmic Ray Conference in Salt Lake City, which were devoted to issues of origin/composition, acceleration and propagation.']",['1999-12-03'] +856,['eng'],"['Starobinsky, A A']",['Future and Origin of our Universe'],['Astrophysics and Astronomy'],"['talk, Budapest 1999/07/02', 'astrophysics, fundamental constant', 'inflationary universe', 'space-time, singularity', 'space-time, de Sitter', 'Friedman model', 'Hubble constant', 'cosmic radiation, background', 'quantum gravity, effect']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912054'],"['The existence of a positive and possibly varying Lambda-term opens a much wider field of possibilities for the future of our Universe than it was usually thought before. Definite predictions may be made for finite (though very large) intervals of time only, as well as in other branches of science. In particular, our Universe will continue to expand as far as the Lambda-term remains positive and does not decay to other forms of matter, even if the Universe is closed. Two new effects due to the presence of a constant Lambda-term are discussed: reversal of a sign of the redshift change with time for sufficiently close objects and inaccessibility of sufficiently distant objects in the Universe for us. A number of more distant and speculative possibilities for the future evolution of the Universe is listed including hitting a space-time singularity during an expansion phase. Finally, in fantastically remote future, a part of our Universe surrounding us can become supercurved and superdense due to various quantum-gravitational effects. This returns us to the past, to the origin of our Universe from a superdense state about 14 Gy ago. According to the inflationary scenario, this state was almost maximally symmetric (de Sitter-like). Though this scenario seems to be sufficient for the explanation of observable properties of the present Universe, and its predictions have been confirmed by observations, the question of the origin of the initial de Sitter (inflationary) state itself remains open. A number of conjectures regarding the very origin of our Universe, ranging from ""creation from nothing"" to ""creation from anything"", are discussed.']",['1999-12-03'] +857,['eng'],"['Brax, P', 'Martín, J']",['The Robustness of Quintessence'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'quintessence', 'potential, Kaehler', 'correction, higher-order', 'supersymmetry', 'space-time, effect', 'supergravity, correction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912046'],"['Recent observations seem to suggest that our Universe is accelerating implying that it is dominated by a fluid whose equation of state is negative. Quintessence is a possible explanation. In particular, the concept of tracking solutions permits to adress the fine-tuning and coincidence problems. We study this proposal in the simplest case of an inverse power potential and investigate its robustness to corrections. We show that quintessence is not affected by the one-loop quantum corrections. In the supersymmetric case where the quintessential potential is motivated by non-perturbative effects in gauge theories, we consider the curvature effects and the Kähler corrections. We find that the curvature effects are negligible while the Kähler corrections modify the early evolution of the quintessence field. Finally we study the supergravity corrections and show that they must be taken into account as $Q\\approx m_{\\rm Pl}$ at small red-shifts. We discuss simple supergravity models exhibiting the quintessential behaviour. In particular, we propose a model where the scalar potential is given by $V(Q)=\\frac{\\Lambda^{4+\\alpha }}{Q^{\\alpha}}e^{\\frac{\\kappa}{2}Q^2}$. We argue that the fine-tuning problem can be overcome if $\\alpha \\ge 11$. This model leads to $\\omega_Q\\approx -0.82$ for $\\Omega_{\\rm m}\\approx 0.3$ which is in good agreement with the presently available data.']",['1999-12-03'] +858,['eng'],"['Kosenko, D I', 'Postnov, K A']",['Fluctuations of Gravitational Wave Noise from Unresolved Extragalactic Sources'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'background, fluctuation', 'angular dependence', 'galaxy, cluster', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912045'],['Angular fluctuations of stochastic gravitational wave backgrounds (GWB) produced by extragalactic astrophysical sources are calculated. The angular properties of such backgrounds are determined by the large scale structure of Universe (galaxy clustering). The evolution of star formation rate with redshift is taken into account. Fluctuations of the metric strain amplitude associated with such noises at angular scales of about one degree are found to be of order 5-20% slowly growing toward smaller angular scales. This feature can be potentially used to separate astrophysical GWB from cosmological ones in future experiments.'],['1999-12-03'] +859,['eng'],"['Brax, P', 'Martín, J']",['Cosmological Implications of the Supergravity Tracking Potential'],['Astrophysics and Astronomy'],"['talk, Weimar 1999/09/12', 'supergravity', 'potential, quintessence', 'astrophysics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912005'],"['It is demonstrated that any realistic model of quintessence should be based on Supergravity since, when the scalar field is on tracks today, $Q\\approx m_{\\rm Pl}$. This improves the agreement between theoretical predictions and the current observations. In particular, a generic property is that ratio string-inspired model is proposed where the potential is given by $V(Q)= predicts $ømega_{\\rm Q}\\approx -0.82$, a value less that one sigma from the current likehood value.']",['1999-12-02'] +860,['eng'],"['Kalogera, V']",['Compact Binary Mergers and Accretion-Induced Collapse'],['Astrophysics and Astronomy'],"['review, Pasadena 1999/07/12', 'gravitational radiation', 'n, matter', 'black hole', 'binary, coalescence', 'white dwarf', 'counters and detectors', 'interference, laser', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911532'],"['This paper is a brief review of the topic of binary systems as sources of gravitational-wave emission for both LIGO and LISA. In particular I review the current estimates of the associated Galactic event rates and their implications for expected detection rates. I discuss the estimates for (i) the coalescence of close binaries containing neutron stars or black holes, (ii) white dwarfs going through accretion-induced collapse into neutron stars, and (iii) detached but close binaries containing two white dwarfs. The relevant uncertainties and robustness of the estimates are addressed along with ways of obtaining conservative upper limits.']",['1999-12-01'] +861,['eng'],"['Baccigalupi, C', 'Perrotta, F']",['Effects of inflationary bubbles on the polarization and temperature anisotropies of the cosmic microwave background'],['Astrophysics and Astronomy'],"['inflationary universe, bubble', 'cosmic radiation, background', 'cosmic radiation, polarization', 'temperature, anisotropy', 'density, perturbation', 'perturbation, linear', 'decoupling', 'cosmic radiation, angular distribution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911530'],"[""We predict the imprint of linear bubbly perturbations on the polarization and temperature anisotropies of the cosmic microwave background (CMB). We analytically model a bubbly density perturbation at the beginning of the radiation dominated era and we apply the linear theory of cosmological perturbations to compute its time evolution. At decoupling, it uniquely signs the CMB polarization and temperature anisotropy sky. During evolution the perturbation propagates beyond the size of the bubble and reaches the CMB sound horizon at the time considered. Therefore, its signal appears as a series of concentric rings, each characterized by its own amplitude and sign, on the scale of 1^{o} on the sky, even if the real seed size is much smaller. Polarization and temperature rings are strictly correlated. As expected for linear perturbations with size L and density contrast \\delta at decoupling, the temperature anisotropy. We predict the impact of a distribution of bubbles on the CMB polarization and temperature power spectra. Considering models containing both CDM Gaussian and bubbly non-Gaussian fluctuations, we simulate and analyze 10^{o} x 10^{o} sky patches with angular resolution of about 3.5^{'}. The CMB power associated with the bubbles is entirely on sub-degree angular scales (200<= l<=1000), that will be explored by the forthcoming high resolution CMB experiments with the percent precision. Depending on the parameters of the bubbly distribution we find extra-power with respect to the ordinary CDM Gaussian fluctuations; we infer simple analytical scalings of the power induced by bubbly perturbations and we constrain our parameters with the existing data.""]",['1999-12-01'] +862,['eng'],"['New, K C B', 'Centrella, J M', 'Tohline, J E']",['Gravitational Waves from Long-Duration Simulations of the Dynamical Bar Instability'],['Astrophysics and Astronomy'],"['gravitational radiation', 'n, matter', 'stability, rotational', 'model, hydrodynamical', 'signal processing', 'numerical methods', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911525'],"[""Compact astrophysical objects that rotate rapidly may encounter the dynamical ``bar instability.'' The bar-like deformation induced by this rotational instability causes the object to become a potentially strong source of gravitational radiation. We have carried out a set of long-duration simulations of the bar instability with two Eulerian hydrodynamics codes. Our results indicate that the remnant of this instability is a persistent bar-like structure that emits a long-lived gravitational radiation signal.""]",['1999-12-01'] +863,['eng'],"['Cheng, K S', 'Dai, Z G']",['Energy Sources of Soft $\\gamma$-Ray Repeaters'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'n, matter', 'energy', 'magnetic field', 'pulsar', 'flux tube', 'matter, strangeness', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911516'],"['Quiescence and burst emission and relativistic particle winds of soft gamma-ray repeaters (SGRs) have been widely interpreted to result from ultrastrongly magnetized neutron stars. In this magnetar model, the magnetic energy and gravitational energy of the neutron stars are suggested as the energy sources of all the emission and winds. However, Harding, Contopoulos & Kazanas (1999) have shown that the magnetic field should be only ~ 3 x 10^{13} G in order to match the characteristic spin-down timescale of SGR 1806-20 and its SNR age. Here we argue that if the magnetic field is indeed so weak, the previously suggested energy sources seem problematic. We further propose a plausible model in which SGR pulsars are young strange stars with superconducting cores and with a poloidal magnetic field of ~ 3 x 10^{13} G. In this model, the movement of the flux tubes not only leads to crustal cracking of the stars, giving rise to deconfinement of crustal matter to strange matter, but also to movement of internal magnetic toruses with the flux tubes. The former process will result in burst and quiescence emission and the latter process will produce steady relativistic winds which will power the surrounding supernova remnants.']",['1999-12-01'] +864,['eng'],"['Yoshida, S', 'Eriguchi, Y']",['Influence of the r-mode instability on hypercritically accreting neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'matter, accretion', 'stability', 'matter, mass', 'temperature', 'oscillation, rotational', 'gravitational radiation', 'angular momentum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911513'],"['We have investigated an influence of the r-mode instability on hypercritically accreting (M ~ 10^8 M_Edd) neutron stars in close binary systems during their common envelope phases based on the scenario proposed by Bethe et al. On the one hand neutron stars are heated by the accreted matter at the stellar surface, but on the other hand they are also cooled down by the neutrino radiation. At the same time, the accreted matter transports its angular momentum and mass to the star. We have studied the evolution of the stellar mass, temperature and rotational frequency. The gravitational-wave-driven instability of the r-mode oscillation strongly suppresses spinning-up of the star, whose final rotational frequency is well below the mass-shedding limit, typically as small as 10% of that of the mass-shedding state. On a very short timescale the rotational frequency tends to approach a certain constant value and saturates there as far as the amount of the accreted mass does not exceed a certain limit to collapse to a black hole. This implies that the similar mechanism of gravitational radiation as the so-called Wagoner star may work in this process. The star is spun up by accretion until the angular momentum loss by gravitational radiation balances the accretion torque. However the lifetime of the system is extremely short, roughly one year or so, to be detected by gravitational wave detectors.']",['1999-12-01'] +865,['eng'],"['Mori, M', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, S', 'Hara, T', 'Jinbo, J', 'Kawachi, A', 'Kifune, T', 'Kubo, H', 'Kushida, J', 'Matsubara, Y', 'Mizumoto, Y', 'Moriya, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Sato, Y', 'Susukita, R', 'Tamura, T', 'Tanimori, T', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T', 'Yuki, A']",['The Cangaroo-III Project'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'radiation, Cherenkov', 'imaging', 'optics, reflection', 'photoelectron, amplifier']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911512'],"['The CANGAROO-III project,which consists of an array of four 10 m imaging Cherenkov telescopes,has just started being constructed in Woomera, South Australia,in a collaboration between Australia and Japan. The first stereoscopic observation of celestial high-energy gamma-rays in the 100 GeV region with two telescopes will start in 2002,and the four telescope array will be completed in 2004. The concept of the project and the expected performance are discussed.']",['1999-12-01'] +866,['eng'],"['Sakellariadou, M']",['Cosmic Microwave Background Anisotropies'],['Astrophysics and Astronomy'],"['talk, Bilbao 1999/09/07', 'inflationary universe', 'topology, defect', 'density, perturbation', 'cosmic radiation, background', 'anisotropy', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911497'],"['I present a briefly summary of the current status of inflationary models versus topological defects scenarios, as the mechanisms which could have induced the initial density perturbations, which left an imprint on the cosmic microwave backgound radiation anisotropies.']",['1999-11-30'] +867,['eng'],"['Bahcall, J N', 'Davis, R']",['The Evolution of Neutrino Astronomy'],['Astrophysics and Astronomy'],"['history', 'neutrino, astrophysics', 'neutrino, solar', 'neutrino, particle identification', 'neutrino nucleus, interaction', 'neutrino electron, elastic scattering', 'model, solar', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911486'],['How did neutrino astronomy evolve? Are there any useful lessons for astronomers and physicists embarking on new observational ventures today? We answer the first question; the reader can can decide if there are any useful parallels for other fields.'],['1999-11-30'] +868,['eng'],"['Ellis, Jonathan Richard']",['Particles and cosmology'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'cosmic radiation, background', 'neutrino, mass', 'matter, density', 'LSP, search for', 'postulated particle, heavy', 'crypton', 'string model', 'vacuum state, energy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911440'],"['The density budget of the Universe is reviewed, and then specific particle candidates for non-bayonic dark matter are introduced, with emphasis on the relevance of cosmic-ray physics. The sizes of the neutrino masses indicated by recent atmospheric and solar neutrino experiments may be too small to contribute much hot dark matter. My favoured candidate for the dominant cold dark matter is the lightest supersymmetric particle, which probably weighs between about 50 GeV and about 600 GeV. Strategies to search for it via cosmic rays due to annihilations in the halo, Sun and Earth, or via direct scattering experiments, are mentioned. Possible superheavy relic particles are also discussed, in particular metastable string- or M-theory cryptons, that may be responsible for the ultra-high-energy cosmic rays. Finally, it is speculated that a non-zero contribution to the cosmological vacuum energy might result from incomplete relaxation of the quantum-gravitational vacuum.']",['1999-11-24'] +869,['eng'],"['Waxman, E']",['High energy cosmic-rays and neutrinos from cosmological $\\gamma$-ray burst fireballs'],['Astrophysics and Astronomy'],"['talk, Enkoping 1998/08/20', 'photon, cosmic radiation', 'fireball', 'neutrino, production', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'cosmic radiation, spectra', 'counters and detectors', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911395'],"['The recent detection of delayed, low energy emission from Gamma-Ray Burst (GRB) sources confirmed the cosmological origin of the bursts and provided support for models where GRBs are produced by the dissipation of the kinetic energy of relativistic fireballs. In this review, ultra high energy, >10^{19} eV, cosmic-ray and high energy, 100 TeV, neutrino production in GRBs is discussed in the light of recent GRB and cosmic-ray observations. Emphasis is put on model predictions that can be tested with operating and planned cosmic-ray and neutrino detectors. The predicted neutrino intensity, E^2 dN/dE=3\\times 10^{-9} GeV/(cm^2 s sr) for 10^{14} eV630 GeV and would be highly suppressed for M_x>~150 GeV. Annihilation of captured WIMPs and anti-WIMPs is expected to give rise to neutrinos coming from the Earth's center. The absence of such a neutrino signal has been used to place limits on WIMP parameters. At present, one does not know if typical WIMP orbits are in fact affected by these resonances. Until this question is investigated and resolved, one must (conservatively) assume that they are. Hence, limits on high-mass WIMP parameters are significantly weaker than previously believed.""]",['1999-11-17'] +877,['eng'],"['Seto, O', 'Yokoyama, J', 'Kodama, H']",['What happens when the inflaton stops during inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'spectra, perturbation', 'field theory, scalar', 'potential', 'field equations, solution']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911119'],['The spectrum of adiabatic density perturbation generated during inflation is studied in the case the time derivative of an inflation-driving scalar field (inflaton) vanishes at some time during inflation. It is shown that the nondecaying mode of perturbation has a finite value even in this case and that its amplitude is given by the standard formula with the time derivation of the scalar field replaced by the potential gradient using the slow-roll equation.'],['1999-11-09'] +878,['eng'],"['Abdurashitov, J N', 'Yants, V E', 'Parfenov, C V']",['Primordial Black Hole Binaries as a Source of $\\gamma$-Ray Bursts and of a High-Frequent Gravitational Radiation'],['Astrophysics and Astronomy'],"['black hole, binary', 'gravitational radiation', 'energy, flux', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, missing-mass', 'coalescence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911093'],"[""Ultracompact primordial black hole binaries with masses > 10^{16} g are considered. If PBHB's contribute significant part of the dark matter of the Galaxy one can expect an existence of high-frequent non-thermal diffuse gravitational radiation with flux of ~1 erg cm^{-2} s^{-1}. The possibility of coalescence of the PBHB's in Galaxy's halo to be a source at least of a part of gamma-ray bursts (GRB) observed is discussed. The energy flux of gravitational radiation from those GRB's should exceed the energy flux of gamma-radiation by 7-8 orders of magnitude. The possibility of observation of PBHB through detection of the gravitational radiation burst coincident with GRB is emphasized. The PBHB also can be observed detecting a stationary gravitatonal radiation in the frequency range > 10^4 Hz and observing a high-frequent pulsation of a source's brightness in microlensing effects in the Galaxy's halo.""]",['1999-11-08'] +879,['eng'],"['Kapusta, J I']",['The Last Eight Minutes of a Primordial Black Hole'],['Astrophysics and Astronomy'],"['black hole, decay', 'shell model', 'expansion, hydrodynamical', 'photon, emission', 'photon, energy spectrum']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911309'],"['About eight minutes before a black hole expires it has a decreasing mass of 10^{10} g, an increasing temperature of 1 TeV, and an increasing luminosity of 7x10^{27} erg/s. I show that such a black hole is surrounded by a quasi-stationary shell of matter undergoing radial hydrodynamic expansion. The inner radius of this shell is bounded by ten times the Schwarzschild radius of 1.6x10^{-5} fm and has a temperature about one-tenth that of the black hole. The outer radius, as defined by the photosphere, is about 1000 fm, has a local temperature of 100 keV, and is moving with a Lorentz gamma factor of 10^7. Most of the emitted radiation is in photons with small amounts in gravitons and neutrinos. I calculate the instantaneous photon spectrum and then integrate it over the last eight minutes to obtain the energy distribution dN_{gamma}/dE =']",['1999-11-17'] +880,['eng'],"['Crocker, R M', 'Melia, F', 'Volkas, R R']",['Oscillating Neutrinos from the Galactic Center'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, particle source', 'galaxy', 'neutrino, oscillation', 'Cherenkov counter', 'neutrino, solar', 'cosmic radiation, flux', 'counters and detectors, proposed', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911292'],"[""It has recently been demonstrated that the $\\gamma$-ray emission spectrum of the EGRET-identified, central Galactic source 2EG J1746-2852 can be well fitted by positing that these photons are generated by the decay of $\\pi^0$'s produced in p-p scattering at or near an energizing shock. Such scattering also produces charged pions which decay leptonically.The ratio of $\\gamma$-rays to neutrinos generated by the central Galactic source may be accurately determined and a well-defined and potentially-measurable high energy neutrino flux at Earth is unavoidable. An opportunity, therefore, to detect neutrino oscillations over an unprecedented scale is offered by this source. In this paper we assess the prospects for such an observation with the generation of neutrino \\v{C}erenkov telescopes now in the planning stage. We determine that the next generation of detectors may find an oscillation signature in the Galactic Center (GC) signal, but that such an observation will probably not further constrain the oscillation parameter space mapped out by current atmospheric, solar, reactor and accelerator neutrino oscillation experiments.""]",['1999-11-17'] +881,['eng'],"['Stecker, F W']",['$\\gamma$-Ray Bursts Cannot Produce the Observed Cosmic Rays Above $10^{19} eV$'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911269'],"['Using recent results indicating that the redshift distribution of gamma-ray bursts most likely follows the redshift evolution of the star formation rate, I show that the energy input from these bursts at low redshifts is insufficient to account for the observed flux of ultrahigh energy cosmic rays with energies above $10^{19}$ eV.']",['1999-11-16'] +882,['eng'],"['Bednarek, W']",['Cascades initiated by EHE photons in the magnetic field of the Earth and the Sun'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, primary', 'showers, air', 'magnetic field, solar', 'magnetic field, geophysics', 'cosmic radiation, cascade', 'electron, pair production', 'electron, cosmic radiation', 'cosmic radiation, secondary radiation', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911266'],"[""The content of extremely high energy (EHE) photons in the highest energy cosmic rays can be investigated by analyzing showers arriving from directions where the perpendicular component of the Earth's magnetic field is high or showers arriving from the region surrounding the Sun. We perform Monte Carlo simulations of cascades initiated by photons with parameters of the highest energy showers observed by the past and present detectors (AGASA, Fly's Eye, Yakutsk, Haverah Park). The purpose is to find out which events should cascade with high probability if initiated by photons. It is shown that EHE photons arriving from directions towards the magnetic poles cascade with higher probability. Alternatively, the lowest probabilities of cascading are expected for photons arriving from directions of the equator at the zenith angles equal to the angle between location of the specific observatory and the magnetic pole. We show that very unusual showers should arrive from direction of the Sun due to cascading of photons in the Sun's magnetosphere if EHE photons are numerous at the highest energies. The rate of such showers is estimated on about one per ten years. However extraordinary lateral distribution of secondary particles of such showers in the Earth's atmosphere may help to distinguish them from the ordinary showers arriving isotropically from the sky.""]",['1999-11-16'] +883,['eng'],"['Ramachers, Y']",['Non-baryonic dark matter searches'],['Astrophysics and Astronomy'],"['review, Blois 1999/06/28', 'astrophysics, missing-mass', 'WIMP, search for', 'scattering, nucleon WIMP', 'nucleus, recoil', 'counters and detectors', 'experimental equipment', 'proposed experiment', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911260'],"['The emphasis in this review about non-baryonic dark matter will be on experimental approaches to this fast evolving field of astroparticle physics, especially the direct detection method. The current status of experimental techniques will be reviewed and recent highlights as well as future plans will be introduced.']",['1999-11-16'] +884,['eng'],"['Mereghetti, S', 'Barbiellini, G', 'Budini, G', 'Caraveo, P A', 'Costa, E', 'Cocco, V', 'Cocco, G D', 'Feroci, M', 'Labanti, C', 'Longo, F', 'Morelli, E', 'Morselli, A', 'Pellizzoni, A', 'Perotti, F', 'Picozza, P', 'Prest, M', 'Soffitta, P', 'Soli, L', 'Tavani, M', 'Vallazza, E', 'Vercellone, S']",['The AGILE $\\gamma$-ray Astronomy Mission'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'counters and detectors, satellite', 'semiconductor detector, microstrip', 'tungsten', 'scintillation counter, crystal', 'cesium, iodine', 'angular resolution']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911256'],"['We describe the AGILE gamma-ray astronomy satellite which has recently been selected as the first Small Scientific Mission of the Italian Space Agency. With a launch in 2002, AGILE will provide a unique tool for high-energy astrophysics in the 30 MeV - 50 GeV range before GLAST. Despite the much smaller weight and dimensions, the scientific performances of AGILE are comparable to those of EGRET.']",['1999-11-16'] +885,['eng'],"['Özer, M']","['Fate of the Universe, Age of the Universe, Dark Matter and the Decaying Vacuum Energy']",['Astrophysics and Astronomy'],"['astrophysics, model', 'vacuum state, energy', 'vacuum state, decay', 'gravitation, lens', 'astrophysics, fundamental constant', 'time variation', 'astrophysics, missing-mass', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911246'],"['It is shown that in the cosmological models based on a vacuum energy decaying as a^{-2}, where a is the scale factor of the universe, the fate of the universe in regard to whether it will collapse in future or expand forever is determined not by the curvature constant k but by an effective curvature constant k_{eff}. It is argued that a closed universe with k=1 may expand forever, in other words simulate the expansion dynamics of a flat or an open universe because of the possibility that k_{eff}=0 or -1, respectively. Two such models, in one of which the vacuum does not interact with matter and in another of which it does, are studied. It is shown that the vacuum equation of state p_{vac}= -\\rho_{vac} may be realized in a decaying vacuum cosmology provided the vacuum interacts wuth matter. The optical depths for gravitational lensing as a function of the matter density and other parameters in the models are calculated at a source redshift of 2. The age of the universe is discussed and shown to be compatible with the new Hipparcos lower limit of 11Gyr. The possibility that a time-varying vacuum energy may serve as dark matter is suggested.']",['1999-11-16'] +886,['eng'],"['Battiston, R']",['The Capabilities of the Alpha Magnetic Spectrometer as GeV $\\gamma$-ray detector'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'counters and detectors, satellite', 'magnetic spectrometer', 'angular resolution', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911241'],"['The modeled performance of the Alpha Magnetic Spectrometer (AMS) as a high-energy (0.3 to 100 GeV) gamma-ray detector is described, and its gamma-ray astrophysics objectives are discussed.']",['1999-11-16'] +887,['eng'],"['Martín, J', 'Schwarz, Dominik J']",['The precision of slow-roll predictions for the CMBR anisotropies'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'temperature, fluctuation', 'two-point function', 'moment, multipole', 'density, perturbation', 'gravitational radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911225'],['Inflationary predictions for the anisotropy of the cosmic microwave background radiation (CMBR) are often based on the slow-roll approximation. We study the precision with which the multipole moments of the temperature two-point correlation function can be predicted by means of the slow-roll approximation. We ask whether this precision is good enough for the forthcoming high precision observations (error < 1%) by means of the MAP and PLANCK satellites. The error in the multipole moments due to the slow-roll approximation is demonstrated to be bigger than the error in the power spectrum. For power-law inflation with n_S = 0.9 the error from the leading order slow-roll approximation is ~ 5% for the amplitudes and ~ 20% for the quadrupoles. For the next-to-leading order the errors are within a few percent. The errors increase with |n_S - 1|. To obtain a precision of 1% it is mandatory to use the next-to-leading order. For a general model of inflation the next-to-leading order does not guarantee 1% precision. In the case of power-law inflation this precision is obtained for the spectral indices if |n_S - 1| > 0.02 and for the quadrupoles if |n_S - 1| > 0.15 only. The slow-roll approximation cannot be improved beyond the next-to-leading order in the slow-roll parameters.'],['1999-11-15'] +888,['eng'],"['Krawczynski, H', 'Coppi, P S', 'Maccarone, T J', 'Aharonian, F A']",['X-ray/TeV-$\\gamma$-ray observations of several strong flares of Mkn 501 during 1997 and implications'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'correlation function', 'data analysis method', 'Cherenkov counter', 'photon, emission', 'galaxy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911224'],"['During more than 6 months in 1997, the BL Lac object Mkn 501 was in an exceptionally bright state, both in the X-ray band and in the Very High Energy (VHE) band. In this paper we present a multiwavelength study of Mkn 501 during this extraordinary outburst. We describe the analysis of a data base of X-ray observations acquired with the pointed X-ray telescopes on board the Rossi X-Ray Timing Explorer (RXTE) during April, May, and July, 1997. We combine this data set with detailed VHE spectral information obtained from simultaneous or nearly simultaneous observations with the stereoscopic Cherenkov telescope system of HEGRA. Several strong flares could clearly be resolved in both energy bands, making it possible to perform a detailed correlation analysis of the X-ray and VHE gamma-ray flux levels and spectra. We interpret the results in the framework of a Synchrotron Self Compton models and study the constraints on the model parameters. We show that the emission mechanism produces an Inverse Compton spectrum with a significant curvature in the TeV energy range and discuss the implications for estimates of the intergalactic extinction due to pair production processes of the VHE photons on the Diffuse Extragalactic Background Radiation.']",['1999-11-15'] +889,['eng'],"['Safonova, M V', 'Lohiya, D']",['Gravity balls in induced gravity model'],['Astrophysics and Astronomy'],"['gravitation, induced', 'soliton', 'galaxy, cluster', 'gravitation, lens', 'background field, random', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911210'],"[""In non-minimally coupled effective gravity theories one can have non-topological solitonic solutions. A typical solution is a spherical region with $G_{\\it eff}=0$ outside and having the canonical Newtonian value inside. Such a spherical domain (gravity-ball) is characterized by an effective index of refraction which causes bending of light incident on it. The gravity ball thus acts as a spherical lens. We consider the gravity ball to be of a size of a typical cluster of galaxies and show that even empty (without matter) gravity ball can produce arc-like images of the background source galaxy. In case of background random galaxy field the ball produces distortions (`shear') of that field. We also obtained constraints on the size of the large gravity ball, which can be inferred from the existing observations of clusters with arcs.""]",['1999-11-12'] +890,['eng'],"['Fang, L Z', 'Lee, W', 'Pando, J']",['The origin of scale-scale correlations of the density perturbations during inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'correlation function']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911189'],['We show that scale-scale correlations are a generic feature of slow-roll inflation theories. These correlations result from the long-time tails characteristic of the time dependent correlations because the long wavelength density perturbation modes are diffusion-like. A relationship between the scale-scale correlations and time-correlations is established providing a way to reveal the time correlations of the perturbations during inflation. This mechanism provides for a testable prediction that the scale-scale correlations at two different spatial points will vanish.'],['1999-11-11'] +891,['eng'],"['Stodolsky, L']",['Neutrino Flight Times in Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, expansion', 'neutrino, massive', 'neutrino, cosmic radiation', 'space-time, Robertson-Walker', 'Hubble constant', 'acceleration', 'mass, dependence']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911167'],"['If neutrinos have a small but non-zero mass, time-of-flight effects for neutrino bursts from distant sources can yield information on the large-scale geometry of the universe, the effects being proportional to the integral over time of the cosmological expansion parameter. In principle absolute physical determinations of the Hubble constant and the acceleration parameter are possible. Practical realization of these possibilities would depend on neutrino masses being in a favorable range and the future development of very large detectors.']",['1999-11-11'] +892,['eng'],"['Otsuki, K', 'Tagoshi, H', 'Kajino, T', 'Wanajo, S']","['General relativistic effects on neutrino-driven wind from young, hot neutron star and the r-process nucleosynthesis']",['Astrophysics and Astronomy'],"['n, matter', 'light nucleus, production', 'space-time, Schwarzschild', 'relativity theory, general', 'entropy', 'neutrino, cosmic radiation', 'supernova', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911164'],"['Neutrino-driven wind from young hot neutron star, which is formed by supernova explosion, is the most promising candidate site for r-process nucleosynthesis. We study general relativistic effects on this wind in Schwarzschild geometry in order to look for suitable conditions for a successful r-process nucleosynthesis. It is quantitatively discussed that the general relativistic effects play a significant role in increasing entropy and decreasing dynamic time scale of the neutrino-driven wind. Exploring wide parameter region which determines the expansion dynamics of the wind, we find interesting physical conditions which lead to successful r-process nucleosynthesis. The conditions which we found realize in the neutrino-driven wind with very short dynamic time scale $\\tau_{\\rm dyn} \\sim 6$ ms and relatively low entropy $S \\sim 140$. We carry out the $\\alpha$-process and r-process nucleosynthesis calculation on these conditions by the use of our single network code including over 3000 isotopes, and confirm quantitatively that the second and third r-process abundance peaks are produced in the neutrino-driven wind.']",['1999-11-11'] +893,['eng'],"['Aharonian, F A', 'Atoyan, A M']",['On the origin of TeV radiation of SN 1006'],['Astrophysics and Astronomy'],"['supernova', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'photon electron, Compton scattering', 'magnetic field', 'p, acceleration', 'electron, acceleration', 'pi0, decay', 'synchrotron radiation, flux', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911158'],"['We discuss the link between the nonthermal X-radiation and TeV gamma-ray emission from SN 1006, and study the capabilities of both electronic and nucleonic models for explanation of the TeV flux observed from the northeast rim of SN 1006.']",['1999-11-11'] +894,['eng'],"['Olinto, A V']",['Ultra High Energy Cosmic Ray Accelerators'],['Astrophysics and Astronomy'],"['talk', 'cosmic radiation, spectra', 'cosmic radiation, acceleration', 'n, matter', 'galaxy', 'cosmic radiation, angular distribution', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911154'],"['The surprising lack of a high energy cutoff in the cosmic ray spectrum at the highest energies together with an apparently isotropic distribution of arrival directions have strongly challenged most models proposed for the acceleration of ultra high energy cosmic rays. Young neutron star winds may be able to explain the mystery. We discuss this recent proposal after summarizing the observational challenge and plausible acceleration sites. Young neutrons star winds differ from alternative models in the predictions for composition, spectrum, and angular distribution which will be tested in future experiments.']",['1999-11-10'] +895,['eng'],"['Catanese, M']",['Ground-Based $\\gamma$-Ray Astronomy'],['Astrophysics and Astronomy'],"['talk, Portsmouth 1999/09/15', 'astrophysics', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911150'],"['Ground-based gamma-ray astronomy has become an active astrophysical discipline with four confirmed sources of TeV gamma rays, two plerionic supernova remnants (SNRs) and two BL Lac objects (BL Lacs). An additional nine objects (one plerion, three shell-type SNRs, one X-ray binary, and four BL Lacs) have been detected but have not been confirmed by independent detections. None of the galactic sources require the presence of hadronic cosmic rays, so definitive evidence of their origin remains elusive. Mrk 421 and Mrk 501 are weak EGRET sources but they exhibit extremely variable TeV emission with spectra that extend beyond 10 TeV. They also exhibit correlations with lower energy photons during multi-wavelength campaigns, providing tests of emission models. Next generation telescopes like VERITAS hold the promise of moving this field dramatically forward.']",['1999-11-10'] +896,['eng'],"['Abu-Zayyad, T', 'Belov, K', 'Bird, D J', 'Boyer, J', 'Cao, Z', 'Catanese, M', 'Chen, G F', 'Clay, R W', 'Covault, C E', 'Cronin, J W', 'Dai, H Y', 'Dawson, B R', 'Elbert, J W', 'Fick, B E', 'Fortson, Lucy F', 'Fowler, J W', 'Gibbs, K G', 'Glasmacher, M A K', 'Green, K D', 'Huang, A', 'Jui, C', 'Kidd, M J', 'Kieda, D B', 'Knapp, B C', 'Larsen, C G', 'Lee, W', 'Loh, E C', 'Mannel, E J', 'Matthews, J', 'Matthews, J N', 'Newport, B J', 'Nitz, D F', 'Ong, R A', 'Simpson, K M', 'Smith, J D', 'Sinclair, D', 'Sokolsky, P', 'Sommers, P', 'Song, C', 'Tang, J K K', 'Thomas, S B', 'Van der Velde, J C', 'Wiencke, L R', 'Wilkinson, C R', 'Yoshida, S', 'Zhang, X Z', 'Ko, S', 'Ho, Y']",['A Multicomponent Measurement of the Cosmic Ray Composition between $10^{17}$ eV and $10^{18}$ eV'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'elements, cosmic radiation', 'energy dependence', 'showers, air', 'showers, spatial distribution', 'muon, cosmic radiation', 'muon, density', 'counters and detectors, optical', 'scintillation counter', 'correlation, time', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911144'],"[""The average mass composition of cosmic rays with primary energies between $10^{17}$eV and $10^{18}$eV has been studied using a hybrid detector consisting of the High Resolution Fly's Eye (HiRes) prototype and the MIA muon array. Measurements have been made of the change in the depth of shower maximum, $X_{max}$, and in the change in the muon density at a fixed core location, evaluated in terms of the combination of $X_{max}$ and $\\rho_\\mu(600m)$. The results show that the composition is changing from a heavy to lighter mix as the energy increases.""]",['1999-11-10'] +897,['eng'],"['Blinnikov, S I']",['Cosmic $\\gamma$-ray Bursts'],['Astrophysics and Astronomy'],"['lectures, Moscow 1999/02/16', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'photon, showers', 'photon, flux', 'fireball', 'astrophysics, missing-mass', 'astrophysics, mirror particle', 'neutrino, oscillation', 'neutrino antineutrino, annihilation', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911138'],"['The properties of the cosmic Gamma-ray Bursts (GRBs) are briefly summarized. A detailed bibliography is given with titles of the papers. Two fundamental theoretical problems are pointed out: the problem of the energy source, and the problem of compactness. I demonstrate some inconsistencies in the estimates of the fireball optical thickness that are widely used in the discussion of the latter problem. The possible connection of GRBs with the Dark Matter candidates is mentioned. I argue that GRBs can be produced by collapses or mergers of stars made of one probable Dark Matter candidate, namely the mirror particles. I speculate on the impact that the parameters of the neutrino oscillations might have on the observed properties of GRBs if the latter are the products of mirror star deaths.']",['1999-11-10'] +898,['eng'],"['De la Macorra, A']",['Model Independent Accelerating Universe and the Cosmological Coincidence Problem'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, acceleration', 'energy, density', 'light nucleus, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911079'],"['We show that the evolution of the quintessence energy density $\\Omega_Q$ is model independent in an accelerating universe. The accelerating behaviour has lasted at most 0.5 e-folds of expansion assuming a present day value of percentage given by $r=2\\gm_Q$, with $\\gm_Q=(\\rho_Q+p_Q)/\\rho_Q$. For a small Nucleosynthesis bounds on $\\Omega_Q$ suggest that the model independent solution is valid for at least 12 e-folds of expansion which includes then the scale of radiation and matter equality. We can, therefore, establish model independent conditions on the cosmological parameters at some factor scale $a_i coincidence problem.']",['1999-11-08'] +899,['eng'],"['Kohri, K', 'Nagataki, S']",['Pulsar Kick and Asymmetric Iron Velocity Distribution in SN1987A'],['Astrophysics and Astronomy'],"['supernova', 'pulsar', 'matter, momentum', 'neutrino, momentum', 'n, matter', 'iron, velocity', 'thermodynamics', 'neutrino, flux', 'angular dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911077'],"['We have investigated the relation of the direction of the momentum among the matter, neutrino, and proto-neutron star in a collapse-driven supernova in order to discuss the pulsar kick. In particular, we have investigated the effects of the pulsar motion on the explosion, which are neglected in the previous study. As a result, we have concluded that the direction of the total momentum of the matter and neutrino is opposite to that of the momentum of the proto-neutron star, irrespective of the asymmetric explosion models. So if we assume that the pulsar motion is caused by an asymmetric supernova explosion, the neutron star born in SN 1987A, which has not been found yet, will be moving in the southern part of the remnant. In other words, if we can find the neutron star in SN 1987A on the south part of the remnant, asymmetric explosion models will be strongly supported by the observation than the binary models.']",['1999-11-08'] +900,['eng'],"['Golubkov, Yu A', 'Khlopov, M Ya']",['Diffuse $\\gamma$ Flux from Antiproton Annihilation in our Galaxy'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'anti-p p, annihilation', 'photon, flux', 'photon, energy spectrum', 'astrophysics, galaxy', 'cosmic radiation, primary', 'anti-p p, ratio', 'anti-p, lifetime', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911058'],"['The all-sky survey in high-energy gamma rays (E > 30 MeV) carried out by the Energetic Gamma Ray Experiment Telescope (EGRET) aboard the Compton Gamma-Ray Observatory provides a unique opportunity to examine in detail the diffuse gamma-ray emission. The observed diffuse emission has a Galactic component arising from cosmic-ray interactions with the local interstellar gas and radiation as well an almost uniformly distributed component that is generally believed to originate outside the Galaxy. The results of the observations have been interpreted as the extragalactic high-energy gamma-ray emission arising primarily from unresolved gamma-ray-emitting blazars. We considered another possible origin of the diffuse gamma-ray flux, namely, as originating from the annihilation of the antiprotons with the interstellar medium.']",['1999-11-05'] +901,['eng'],"['Vasilev, V']",['Extragalactic background light absorption signal in the 0.26-10 TeV spectra of blazars'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, spectra', 'energy, density', 'photon, absorption', 'blazar', 'galaxy, AGN', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9911018'],"['Recent observations of the TeV gamma-ray spectra of the two closest active galactic nuclei (AGNs), Markarian 501 (Mrk 501) and Markarian 421 (Mrk 421), by the Whipple and HEGRA collaborations have stimulated efforts to estimate or limit the spectral energy density (SED) of extragalactic background light (EBL) which causes attenuation of TeV photons via pair-production when they travel cosmological distances. In spite of the lack of any distinct cutoff-like feature in the spectra of Mrk 501 and Mrk 421 (in the interval 0.26-10 TeV) which could clearly indicate the presence of such a photon absorption mechanism, we demonstrate that strong EBL attenuation signal (survival probability of 10 TeV photon (~10^{-2}) may still be present in the spectra of these AGNs. This attenuation could escape detection due to a special form of SED of EBL and unknown intrinsic spectra of these blazars. Here we show how the proposed and existing experiments, VERITAS, HESS, MAGIC, STACEE and CELESTE may be able to detect or severely limit the EBL SED by extension of spectral measurements into the critical 100-300 GeV regime.']",['1999-11-03'] +902,['eng'],"['Munyaneza, F', 'Viollier, R D']",['Heavy neutrino dark matter in the solar system'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutrino, heavy', 'neutrino, gas', 'matter, solar', 'gravitation, cluster', 'neutrino, mass', 'neutrino, radiative decay', 'proposed experiment', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910566'],"['We study a simple model of dark matter that is gravitationally clustered around the sun in the form of a spherical halo of a degenerate gas of heavy neutrinos. It is shown that for neutrino masses $m_{\\nu} \\stackrel {\\textstyle <}{\\sim} 16~{\\rm keV}/c^{2}$, the resulting matter distribution is consistent with the constraints on the mass excesses within the orbits of the outer planets, as obtained from astrometrical and the Pioneer 10/11 and Voyager 1/2 (Anderson et al. 1995) ranging data. However, the anomalous acceleration recently detected in the Pioneer 10/11 data that is approximately constant between 40 AU and 60 AU (Anderson et al. 1998; Turyshev et al. 1999) is incompatible with both our model and earlier Pioneer 10/11 ranging data for the outer planets. We then calculate the planetary and asteroidal perihelion shifts generated by such a neutrino halo. For $m_{\\nu} \\stackrel{\\textstyle <}{\\sim}16~{\\rm keV}/c^{2}$, our results are consistent with the observational data on Mercury, Venus, Earth and Icarus.Finally, we propose to detect this neutrino halo directly with a dedicated experiment on Earth, observing the X-rays emitted in the radiative decay of the heavy neutrino into a light neutrino and a photon.']",['1999-11-02'] +903,['eng'],"['McEnery, J E', 'Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G', 'Dingus, B L', 'Dorfan, D E', 'Ellsworth, R W', 'Evans, D', 'Falcone, A D', 'Fleysher, L', 'Fleysher, R', 'Gisler, G', 'Goodman, J A', 'Haines, T J', 'Hoffman, C M', 'Hugenberger, S', 'Kelley, L A', 'Leonor, I', 'McConnell, M', 'McCullough, J F', 'Miller, R S', 'Mincer, A I', 'Morales, M F', 'Némethy, P', 'Ryan, J M', 'Shen, B', 'Shoup, A L', 'Sinnis, C', 'Smith, A J', 'Sullivan, G W', 'Tumer, T O', 'Wang, K', 'Wascko, M O', 'Westerhoff, S', 'Williams, D A', 'Yang, T', 'Yodh, G B']",['First Results of a Study of TeV Emission from GRBs in Milagrito'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'photon, showers', 'cosmic radiation, energy', 'correlation, time', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910549'],"['Milagrito, a detector sensitive to gamma-rays at TeV energies, monitored the northern sky during the period February 1997 through May 1998. With a large field of view and high duty cycle, this instrument was used to perform a search for TeV counterparts to gamma-ray bursts. Within the Milagrito field of view 54 gamma-ray bursts at keV energies were observed by the Burst And Transient Satellite Experiment (BATSE) aboard the Compton Gamma-Ray Observatory. This paper describes the results of a preliminary analysis to search for TeV emission correlated with BATSE detected bursts. Milagrito detected an excess of events coincident both spatially and temporally with GRB 970417a, with chance probability $2.8 \\times 10^{-5}$ within the BATSE error radius. No other significant correlations were detected. Since 54 bursts were examined the chance probability of observing an excess with this significance in any of these bursts is $1.5 \\times 10^{-3}$. The statistical aspects and physical implications of this result are discussed.']",['1999-11-01'] +904,['eng'],"['Piron, F']",['Calibration of the CAT Telescope'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'muon, cosmic radiation', 'showers, air', 'Cherenkov counter, ring imaging', 'calibration']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910518'],"['Due to the lack of test-beams in ground-based gamma-ray astronomy, detector calibration has been a major challenge in this field. However, with the use of Cherenkov ring-images due to cosmic-ray muons and of strong gamma-ray signals, the CAT telescope could be rather well monitored and understood. Here we present a few oustanding aspects of this work.']",['1999-10-29'] +905,['eng'],"['Piron, F']",['VHE gamma-ray spectral properties of the blazars Mrk 501 and Mrk 421 from CAT observations in 1997 and 1998'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'blazar', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910512'],"['The Very High Energy (VHE) gamma-ray emission of the BL Lacertae objects Markarian 501 and Markarian 421 has been observed by the CAT Imaging Atmospheric Cherenkov Telescope in 1997 and 1998. The spectrum extraction method is presented, and the spectral properties of both sources are compared in different activity states. Theoretical implications for jet astrophysics are discussed.']",['1999-10-29'] +906,['eng'],"['Zimdahl, W']","['Cosmological particle production, causal thermodynamics, and inflationary expansion']",['Astrophysics and Astronomy'],"['inflationary universe', 'model, fluid', 'particle, production', 'thermodynamics', 'expansion, acceleration', 'pressure', 'causality', 'vacuum state, decay', 'energy, density', 'field theory, scalar', 'coupling, minimal', 'potential', 'entropy', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910483'],"['Combining the equivalence between cosmological particle creation and an effective viscous fluid pressure with the fact that the latter represents a dynamical degree of freedom within the second-order Israel-Stewart theory for imperfect fluids, we reconsider the possibility of accelerated expansion in fluid cosmology. We find an inherent self-limitation for the magnitude of an effective bulk pressure which is due to adiabatic (isentropic) particle production. For a production rate which depends quadratically on the Hubble rate we confirm the existence of solutions which describe a smooth transition from inflationary to noninflationary behavior and discuss their interpretation within the model of a decaying vacuum energy density. An alternative formulation of the effective imperfect fluid dynamics in terms of a minimally coupled scalar field is given. The corresponding potential is discussed and an entropy equivalent for the scalar field is found.']",['1999-10-28'] +907,['eng'],"['Lampeitl, H', 'Hofmann, W']","['""Convergent observations"" with the stereoscopic HEGRA CT system']",['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'photon, cosmic radiation', 'Cherenkov counter', 'showers, air', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910461'],"[""Observations of air showers with the stereoscopic HEGRA IACT system are usually carried out in a mode where all telescopes point in the same direction. Alternatively, one could take into account the finite distance to the shower maximum and orient the telescopes such that their optical axes intersect at the average height of the shower maximum. In this paper we show that this ``convergent observation mode'' is advantageous for the observation of extended sources and for surveys, based on a small data set taken with the HEGRA telescopes operated in this mode.""]",['1999-10-27'] +908,['eng'],"['Mücke, A', 'Protheroe, R J']",['Modeling the April 1997 flare of Mkn 501'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, acceleration', 'pi, synchrotron radiation', 'pi0, radiative decay', 'pi, leptonic decay', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910460'],"['The April 1997 giant flare of Mkn 501 is modelled by a stationary Synchrotron-Proton-Blazar model. Our derived model parameters are consistent with X-ray-to-TeV-data in the flare state and diffusive shock acceleration of electron and proton in a Kolmogorov/Kraichnan turbulence sprectrum. While the emerging pair-synchrotron cascade spectra initiated by photons from neutral pi-decay and electrons from pi+- --> mu+- --> e+- decay turn out to be relatively featureless, muon and proton synchrotron radiation and their cascade radiation produce a double-humped spectral energy distribution. For the present model we find proton synchrotron radiation to dominate the TeV emission, while the contribution from the synchrotron radiation of the pairs, produced by the high energy hump, is only minor.']",['1999-10-27'] +909,['eng'],"['Coley, A A']",['Qualitative properties of scalar-tensor theories of Gravity'],['Astrophysics and Astronomy'],"['gravitation, scalar', 'gravitation, tensor', 'model, fluid', 'field theory, scalar', 'massless', 'coupling, minimal', 'transformation, conformal', 'relativity theory, general', 'asymptotic behavior']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910395'],"['The qualitative properties of spatially homogeneous stiff perfect fluid and minimally coupled massless scalar field models within general relativity are discussed. Consequently, by exploiting the formal equivalence under conformal transformations and field redefinitions of certain classes of theories of gravity, the asymptotic properties of spatially homogeneous models in a class of scalar-tensor theories of gravity that includes the Brans-Dicke theory can be determined. For example, exact solutions are presented, which are analogues of the general relativistic Jacobs stiff perfect fluid solutions and vacuum plane wave solutions, which act as past and future attractors in the class of spatially homogeneous models in Brans-Dicke theory.']",['1999-10-22'] +910,['eng'],"['Weekes, T C']",['VHE Astronomy before the New Millenium'],['Astrophysics and Astronomy'],"['review, Snowbird 1999/08/13', 'astrophysics', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'galaxy', 'experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910394'],['A report on the observational status of VHE astronomy is given.'],['1999-10-22'] +911,['eng'],"['Weber, F']",['From Boson Condensation to Quark Deconfinement'],['Astrophysics and Astronomy'],"['talk, Ustron 1999/09/15', 'n, matter', 'quark, confinement', 'boson, condensation', 'baryon, matter', 'quark, matter', 'matter, rotational', 'oscillation', 'hyperon, matter', 'baryon resonance, dibaryon', 'H baryon', 'diquark, condensation', 'color, superconducting', 'matter, strangeness', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910371'],"[""Gravity compresses the matter in the cores of neutron stars to densities which are significantly higher than the density of ordinary atomic nuclei, thus providing a high-pressure environment in which numerous particle processes - from the generation of new baryonic particles to quark deconfinement to the formation of Boson condensates and H-matter - may compete with each other. There are theoretical suggestions of even more `exotic' processes inside pulsars, such as the formation of absolutely stable strange quark matter, a configuration of matter even more stable than the most stable atomic nucleus, iron. In the latter event, neutron stars would be largely composed of pure quark matter, eventually enveloped in nuclear crust matter. No matter which physical processes are actually realized inside neutron stars, each one leads to fingerprints, some more pronounced than others though, in the observable stellar quantities. This feature combined with the tremendous recent progress in observational radio and X-ray astronomy, renders neutron stars to nearly ideal probes for a wide range of dense matter studies, complementing the quest of the behavior of superdense matter in terrestrial collider experiments.""]",['1999-10-21'] +912,['eng'],"['Olum, K D', 'Blanco-Pillado, J J']",['Radiation from cosmic string standing waves'],['Astrophysics and Astronomy'],"['astrophysics, string', 'Higgs model, abelian', 'lattice field theory, classical', 'cosmic radiation', 'scaling, network', 'energy, emission', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910354'],"['We have simulated large-amplitude standing waves on an Abelian-Higgs cosmic string in classical lattice field theory. The radiation rate falls exponentially with wavelength, as one would expect from the field profile around a gauge string. Our results agree with those of Shellard and Moore, but not those of Vincent, Antunes, and Hindmarsh. The radiation rate falls too rapidly to sustain a scaling solution via direct radiation of particles from string length. There is thus reason to doubt claims of strong constraints on cosmic string theories from cosmic ray observations.']",['1999-10-20'] +913,['eng'],"['Whitmire, S E', 'Scherrer, R J']",['Inhomogeneous Neutrino Degeneracy and Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'neutrino, density', 'potential, chemical', 'programming, linear', 'energy, density', 'photon baryon, ratio', 'cosmic radiation, background', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910352'],"['We examine Big Bang nucleosynthesis (BBN) in the case of inhomogenous neutrino degeneracy, in the limit where the fluctuations are sufficiently small on large length scales that the present-day element abundances are homogeneous. We consider two representive cases: degeneracy of the electron neutrino alone, and equal chemical potentials for all three neutrinos. We use a linear programming method to constrain an arbitrary distribution of the chemical potentials. For the current set of (highly-restrictive) limits on the primordial element abundances, homogeneous neutrino degeneracy barely changes the allowed range of the baryon-to-photon ratio. Inhomogeneous degeneracy allows for little change in the lower bound on the baryon-to-photon ratio, but the upper bound in this case can be as large as 1.1 \\times 10^{-8} (only electron neutrino degeneracy) or 1.0 \\times 10^{-9} (equal degeneracies for all three neutrinos). For the case of inhomogeneous neutrino degeneracy, we show that there is no BBN upper bound on the neutrino energy density, which is bounded in this case only by limits from structure formation and the cosmic microwave background.']",['1999-10-20'] +914,['eng'],"['Peebles, P J E']",['Dynamics of a Dark Matter Field with a Quartic Self-Interaction Potential'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'field theory, scalar', 'potential', 'energy, density', 'inflationary universe', 'squeezed state', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910350'],"['It may prove useful in cosmology to understand the behavior of the energy distribution in a scalar field that interacts only with gravity and with itself by a pure quartic potential, because if such a field existed it would be gravitationally produced, as a squeezed state, during inflation. It is known that the mean energy density in such a field after inflation varies with the expansion of the universe in the same way as radiation. I show that if the field initially is close to homogeneous, with small energy density contrast delta rho /rho and coherence length L, the energy density fluctuations behave like acoustic oscillations in an ideal relativistic fluid for a time on the order of L/|delta rho /rho|. This ends with the appearance of features that resemble shock waves, but interact in a close to elastic way that reversibly disturbs the energy distribution.']",['1999-10-20'] +915,['eng'],"['Krogh, K']",['Gravitation Without Curved Space-time'],['Astrophysics and Astronomy'],"['gravitation, model', 'quantum mechanics', 'particle, velocity', 'optics', 'potential', 'photon, deflection', 'relativity theory, general', 'matter, orbit', 'mass', 'pulsar, density', 'astrophysics', 'electromagnetic interaction', 'gravitational radiation', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910325'],"[""A quantum-mechanical theory of gravitation is presented, where the motion of particles is based on the optics of de Broglie waves. Here the large-scale geometry of the universe is inherently flat, and its age is not constrained to < 12 billion years. While this theory agrees with the standard experimental tests of Einstein's general relativity, it predicts a different second-order deflection of light, and measurement of the Lense-Thirring effect in the upcoming NASA experiment Gravity Probe B.""]",['1999-10-19'] +916,['eng'],"['Boone, L M', 'Bullock, J S', 'Primack, Joel R', 'Williams, D A']",['The Implications of Galaxy Formation Models for the TeV Observations of Current Detectors'],['Astrophysics and Astronomy'],"['talk, Snowbird 1999/08/13', 'galaxy, production', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910301'],"['This paper represents a step toward constraining galaxy formation models via TeV gamm a ray observations. We use semi-analytic models of galaxy formation to predict a spectral distribution for the intergalactic infrared photon field, which in turn yields information about the absorption of TeV gamma rays from extra-galactic sources. By making predictions for integral flux observations at >200 GeV for several known EGRE T sources, we directly compare our models with current observational upper limits obtained by Whipple. In addition, our predictions may offer a guide to the observing programs for the current population of TeV gamma ray observatories.']",['1999-10-19'] +917,['eng'],"['Riazuelo, A', 'Deruelle, N', 'Peter, P']",['Topological Defects and CMB anisotropies'],['Astrophysics and Astronomy'],"['astrophysics, string', 'topology, defect', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, spectra', 'defect, decay', 'energy, density', 'string, network', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910290'],"['We consider a network of topological defects which can partly decay into neutrinos, photons, baryons, or Cold Dark Matter. We find that the degree-scale amplitude of the cosmic microwave background (CMB) anisotropies as well as the shape of the matter power spectrum can be considerably modified when such a decay is taken into account. We conclude that present predictions concerning structure formation by defects might be unreliable.']",['1999-10-18'] +918,['eng'],"['Contaldi, C R', 'Bean, R', 'Magueijo, J']",['Photographing the wave function of the Universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'inflaton, wave function', 'density, fluctuation', 'energy eigenstate', 'cumulant expansion', 'coherent state', 'decoherence', 'Edgeworth expansion']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910309'],"['We show that density fluctuations in standard inflationary scenarios may take the most general non-Gaussian distribution if the wave function of the Universe is not in the ground state. We adopt the Schrödinger picture to find a remarkable similarity between the most general inflaton wavefunction and the Edgeworth expansion used in probability theory. Hence we arrive at an explicit relation between the cumulants of the density fluctuations and the amplitudes or occupation numbers of the various energy eigenstates. For incoherent superpositions only even cumulants may be non-zero, but coherent superpositions may generate non-zero odd cumulants as well. Within this framework measurements of cumulants in Galaxy surveys directly map the wavefunction of the Universe.']",['1999-10-19'] +919,['eng'],"['Abbas, A']",['Signals of Supersymmetric Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'LSP', 'neutralino, annihilation', 'WIMP', 'geophysics']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910265'],['The Lightest Supersymmetric Particle predicted in most of the supersymmetric scenarios is an ideal candidate for the dark matter of cosmology. Their detection is of extreme significance today. Recently there have been intriguing signals of a 59 Gev neutralino dark matter at DAMA in Gran Sasso. We look at other possible signatures of dark matter in astrophysical and geological frameworks. The passage of the earth through dense clumps of dark matter would produce large quantities of heat in the interior of this planet through the capture and subsequent annihilation of dark matter particles. This heat would lead to large-scale volcanism which could in turn have caused mass extinctions. The periodicity of such volcanic outbursts agrees with the frequency of palaeontological mass extinctions as well as the observed periodicity in the occurrence of the largest flood basalt provinces on the globe. Binary character of these extinctions is another unique aspect of this signature of dark matter. In addition dark matter annihilations appear to be a new source of heat in the planetary systems.'],['1999-10-15'] +920,['eng'],"['Balkanov, V A']",['Search for high energy neutrinos with the BAIKAL underwater detector NT-96'],['Astrophysics and Astronomy'],"['talk, Ringberg Castle 1999/06/06', 'neutrino, cosmic radiation', 'cosmic radiation, flux', 'upper limit', 'Cherenkov counter, water', 'deep underground detector, Baikal', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910133'],"['We present the results of a search for high energy neutrinos with the Baikal underwater Cherenkov detector NT-96. An upper limit to the flux of \\nu_e + GeV is obtained, assuming an E^{-2} behavior of the neutrino spectrum.']",['1999-10-08'] +921,['eng'],"['Ellison, D C', 'Goret, P', 'Baring, M G', 'Grenier, I A', 'Lagage, P O']","['Photons and Particle Production in Cassiopeia ; A, Predictions from Nonlinear Diffusive Shock Acceleration']",['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'supernova', 'cosmic radiation, production', 'cosmic radiation, spectra', 'photon, cosmic radiation', 'cosmic radiation, acceleration', 'ion', 'acceleration, shock waves', 'synchrotron radiation', 'magnetic field, high', 'numerical calculations, Monte Carlo', 'interpretation of experiments']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910125', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_2_09.pdf']","['We calculate particle spectra and continuum photon emission from the Cassiopeia A supernova remnant (SNR). The particle spectra, ion and electron, result from diffusive shock acceleration at the forward SNR shock and are determined with a nonlinear Monte Carlo calculation. The calculation self-consistently determines the shock structure under the influence of ion pressure, and includes a simple parameterized treatment of electron injection and acceleration. Our results are compared to photon observations, concentrating on the connection between the Radio and GeV-TeV gamma-ray range, and to cosmic ray ion observations. We include new upper limits from the Cherenkov Array at Themis (CAT) imaging Cherenkov telescope and the Whipple 10m gamma-ray telescope at > 400 GeV. These new limits support the suggestion (e.g. Cowsik & Sarkar 1980; Allen et. al. 1997) that energetic electrons are emitting synchrotron radiation in an extremely high magnetic field (~ 1000 microGauss), far greater than values routinely assigned to the ISM, and help to constrain our model. The large magnetic field allows acceleration of cosmic ray ions to well above $10^{15}$ eV per nucleon in the ~ 300 yr lifetime of Cas A.']",['1999-10-08'] +922,['eng'],"['Hu, W', 'Peebles, P J E']",['A model for structure formation seeded by gravitationally produced matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'model, fluid', 'field theory, scalar', 'gravitation', 'mass spectrum', 'cosmic radiation, background', 'cosmic radiation, spectra', 'galaxy, production', 'inflationary universe', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910222'],"['This model assumes the baryons, radiation, three families of massless neutrinos, and cold dark matter were mutually thermalized before the baryon number was fixed, primeval curvature fluctuations were subdominant, and homogeneity was broken by scale-invariant fluctuations in a new dark matter component that behaves like a relativistic ideal fluid. The fluid behavior could follow if this new component were a single scalar field that interacts only with gravity and with itself by a pure quartic potential. The initial energy distribution could follow if this component were gravitationally produced by inflation. The power spectra of the present distributions of mass and radiation in this model are not inconsistent with the measurements but are sufficiently different from the adiabatic cold dark matter model to allow a sharp test in the near future.']",['1999-10-14'] +923,['eng'],"['Barreiro, T', 'Copeland, E J', 'Nunes, N J']",['Quintessence arising from exponential potentials'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'potential', 'quintessence', 'astrophysics, model', 'string model', 'Kaluza-Klein model', 'scaling', 'model, attractor', 'coupling constant', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910214'],"['We demonstrate how exponential potentials that could arise in the early Universe as a result of Kaluza-Klein type compactifications of string theory, can lead to cosmological solutions which correspond to the currently observed accelerating Universe. The idea is simple, relying solely on the known scaling properties associated with exponential potentials. In particular we show that the existence of stable attractor solutions implies that the results hold for a wide range of coupling constants and initial conditions.']",['1999-10-13'] +924,['eng'],"['Hettlage, C', 'Mannheim, K', 'Learned, J G']",['The sun as a high energy neutrino source'],['Astrophysics and Astronomy'],"['cosmic radiation', 'model, solar', 'neutrino, solar', 'neutrino, oscillation', 'neutrino, flux', 'WIMP', 'neutrino, particle identification', 'background', 'Cherenkov counter, water', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910208'],['Cosmic ray interactions in the solar atmosphere yield a flux of electron and muon neutrinos with energies greater than 10 GeV. We discuss the influence of neutrino oscillations on the event rates in water-based Cerenkov detectors due to this neutrino flux and comment on the possibility of detecting the sun as a high energy neutrino source.'],['1999-10-13'] +925,['eng'],"['Heiselberg, H']",['Dense matter in neutron stars and phase transitions'],['Astrophysics and Astronomy'],"['talk, Paris 1999/06/16', 'n, matter', 'supernova', 'nuclear matter', 'binary', 'nucleon nucleon, potential', 'critical phenomena, quark hadron', 'hadron, condensation', 'superfluid', 'matter, rotational', 'matter, mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910200'],"[""After a brief history of neutron stars and supernovae recent developments are discussed. Based on modern nucleon-nucleon potentials more reliable equations of state for dense nuclear matter have been constructed. Furthermore, phase transitions such as pion, kaon and hyperon condensation, superfluidity and quark matter can occur in cores of neutron stars. Specifically, the nuclear to quark matter phase transition and its mixed phases with intriguing structures is treated. Rotating neutron stars with and without phase transitions are discussed and compared to observed masses, radii and glitches. The observations of possible heavy $\\sim 2M_\\odot$ neutron stars in X-ray binaries and QPO's require relatively stiff equation of states and restricts strong phase transitions to occur at very high nuclear densities only.""]",['1999-10-13'] +926,['eng'],"['Caldwell, D O', 'Fuller, G M', 'Qian, Y Z']",['Sterile neutrinos and supernova nucleosynthesis'],['Astrophysics and Astronomy'],"['neutrino, sterile', 'neutrino, mass', 'neutrino, mixing angle', 'neutrino, oscillation', 'electron, density', 'light nucleus, production', 'supernova', 'proposed experiment', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910175'],"['A light sterile neutrino species has been introduced to explain simultaneously the solar and atmospheric neutrino puzzles and the results of the LSND experiment, while providing for a hot component of dark matter. Employing this scheme of neutrino masses and mixings, we show how matter-enhanced active-sterile neutrino transformation followed by active-active neutrino transformation can solve robustly the neutron deficit problem encountered by models of r-process nucleosynthesis associated with neutrino-heated supernova ejecta.']",['1999-10-12'] +927,['eng'],"['Maia, J M F', 'Lima, J A S']",['Extended Warm Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'thermodynamics', 'dissipation', 'expansion, strong coupling', 'potential', 'space-time, Robertson-Walker']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910568'],['A bidimensional parameter space of unitary area is introduced to study phenomenologically the dynamic and thermodynamic behavior of inflationary models driven by a scalar field coupled to a thermal component. In this enlarged context the isentropic and warm pictures are just extreme cases of an infinite two-parametric family of possible inflationary scenarios. It is also shown that strong couplings are responsible by an alteration in the standard slow roll conditions which relax the smallness constraint on the first and the second derivatives of the potential.'],['1999-11-02'] +928,['eng'],"['Song, C', 'Cao, Z', 'Dawson, B R', 'Fick, B E', 'Lee, W', 'Sokolsky, P', 'Zhang, X']",['Energy Estimation of UHE Cosmic Rays using the Atmospheric Fluorescence Technique'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'showers, air', 'photon, cosmic radiation', 'energy loss', 'calorimeter, air', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910195'],"['We use the CORSIKA air shower simulation program to review the method for assigning energies to ultra-high energy (UHE) cosmic rays viewed with the air fluorescence technique. This technique uses the atmosphere as a calorimeter, and we determine the corrections that must be made to the calorimetric energy to yield the primary cosmic ray energy.']",['1999-10-12'] +929,['eng'],"['Liddle, A R']",['Observational tests of inflation'],['Astrophysics and Astronomy'],"['talk, Batavia 1999/05/26', 'inflationary universe, validity test', 'perturbation, tensor', 'perturbation, vector', 'potential, inflaton', 'field theory, scalar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910110'],"['We are on the verge of the first precision testing of the inflationary cosmology as a model for the origin of structure in the Universe. I review the key predictions of inflation which can be used as observational tests, in the sense of allowing inflation to be falsified. The most important prediction of this type is that the perturbations will cross inside the Hubble radius entirely in their growing mode, though nongaussianity can also provide critical tests. Spatial flatness and tensor perturbations may offer strong support to inflation, but cannot be used to exclude it. Finally, I discuss the extent to which observations will distinguish between inflation models, should the paradigm survive these key tests, in particular describing a technique for reconstruction of the inflaton potential which does not require the slow-roll approximation.']",['1999-10-07'] +930,['eng'],"['Sahni, V', 'Wang, L']",['A New Cosmological Model of Quintessence and Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'field theory, scalar', 'quintessence', 'astrophysics, missing-mass', 'matter, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910097'],"['We propose a new class of quintessence models in which late times oscillations of a scalar field give rise to an effective equation of state which can be negative: $w_\\phi \\leq -1/3$, and hence drive the observed acceleration of the universe. Currently favoured values $\\Omega_\\phi \\sim 0.7$, can be easily accommodated by our model. A novel feature of our ansatz is that it permits a unified treatment of quintessence and CDM by describing both within the framework of the same class of potentials. Quintessence potentials of the kind discussed in this paper are often encountered in field theory, condensed matter physics and particle physics.']",['1999-10-07'] +931,['eng'],"['Lukash, V N']",['The very early Universe'],['Astrophysics and Astronomy'],"['lectures', 'astrophysics, model', 'potential, perturbation', 'inflationary universe, stochastic', 'chaos', 'validity test', 'field theory, scalar', 'quantization']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910009'],"['In these lectures we dwell upon the cosmological corner-stones of the Very Early Universe (VEU) theory: Parametric Amplification Effect (PAE) responsible for the generation of Primordial Cosmological Perturbations (PCPs), Chaotic and Stochastic Inflation, Principal Tests of VEU, and others.']",['1999-10-04'] +932,['eng'],"['Mannheim, P D']",['Cosmic acceleration as the solution to the cosmological constant problem'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'gravitation, fundamental constant', 'gravitation, conformal', 'astrophysics, model', 'symmetry, spontaneously broken', 'energy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910093'],"[""In this paper we provide both a diagnosis and resolution of the cosmological constant problem, one in which a large (as opposed to a small) cosmological constant $\\Lambda$ can be made compatible with observation. We trace the origin of the cosmological constant problem to the assumption that Newton's constant $G$ sets the scale for cosmology. And then we show that once this assumption is relaxed (so that the local $G$ as measured in a local Cavendish experiment is no longer to be associated with global cosmology), the very same cosmic acceleration which has served to make the cosmological constant problem so very severe instead then serves to provide us with its potential resolution. In addition, we present an alternate cosmology, one based on conformal gravity (a theory which explicitly possesses no fundamental $G$), and show that once given only that there is to be cosmic acceleration in the conformal theory (i.e. once given only that in the theory the sign of $\\Lambda$ is to specifically be the negative one suggested by spontaneous symmetry breaking), then that alone, no matter how big $\\Lambda$ might actually be magnitude, is sufficient to not only make the actually measurable contribution $\\Omega_{\\Lambda}(t_0)$ of $\\Lambda$ to current era cosmology naturally be of order one today, but to even do so in a way which is fully compatible with the recent high $z$ supernovae cosmology data. Cosmology can thus live with either a fundamental $G$ or with the large (and even potentially negative) $\\Lambda$ associated with elementary particle physics phase transitions but not with both.""]",['1999-10-06'] +933,['eng'],"['Xu, R X', 'Qiao, G J', 'Zhang, B']",['High-energy accelerators above pulsar polar caps'],['Astrophysics and Astronomy'],"['talk, Bonn 1999/08/30', 'pulsar, temperature', 'electron, acceleration', 'electron positron, interaction', 'matter, strangeness', 'n, matter']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909485'],"['Similar to the terrestrial collision accelerators of electron-antielectron, another kind of accelerator is above a positively or negatively charged pulsar polar cap. In the case of pulsars with magnetic axis parallel (anti-parallel) to rotational axis, relativistic antielectron (electron) with Lorentz factor about 10^6 hit the electrons in the polar caps. These scenarios are investigated both for pulsars being bare strange stars and for pulsars being neutron stars. Such a study may be valuable to differentiate neutron stars and bare strange stars observationally.']",['1999-09-30'] +934,['eng'],"['Xu, R X', 'Qiao, G J', 'Zhang, B']",['Are pulsars bare strange stars?'],['Astrophysics and Astronomy'],"['talk, Bonn 1999/08/30', 'pulsar', 'matter, strangeness', 'supernova', 'critical phenomena']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909484'],"['It is believed that pulsars are neutron stars or strange stars with crusts. However we suggest here that pulsars may be bare strange stars (i.e., strange stars without crust). Due to rapid rotation and strong emission, young strange stars produced in supernova explosions should be bare when they act as radio pulsars. Because of strong magnetic field, two polar-crusts would shield the polar caps of an accreting strange star. Such a suggestion can be checked by further observations.']",['1999-09-30'] +935,['eng'],"['Einasto, J', 'Einasto, M']",['Dark Matter in Groups and Clusters of Galaxies'],['Astrophysics and Astronomy'],"['talk, Turku 1999/06/13', 'astrophysics, missing-mass', 'galaxy, cluster', 'matter, density', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909437'],"['A short story of dark matter as an example of a scientific revolution is given. The characteristics of stellar populations are compared with those of dark halos. The mean mass-to-luminosity ratio of stellar populations is found to be 4 in Solar units. Dark matter around galaxies, and in groups, clusters and voids is discussed. Modern data suggest that the overall density of matter in the Universe is 0.3 +- 0.1, about 80% of this matter is non-baryonic dark matter, and about 20% is baryonic, mostly in the form of hot intra-cluster and intragroup gas, the rest in stellar populations of galaxies. The Universe is dominated by dark energy (cosmological constant) term.']",['1999-09-28'] +936,['eng'],"['Battiston, R', 'Biasini, M', 'Fiandrini, E', 'Petrakis, J', 'Salamon, M H']",['The Gamma Ray Detection Capabilities of the Alpha Magnetic Spectrometer'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, showers', 'cosmic radiation, particle source', 'magnetic spectrometer, satellite', 'energy resolution', 'neutralino', 'proposed experiment', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909432'],"['The modeled performance of the Alpha Magnetic Spectrometer (AMS) as a high energy (0.3 to 100 GeV) gamma-ray detector is described, and its gamma ray astrophysics objectives are discussed.']",['1999-09-28'] +937,['eng'],"['Bednarz, J', 'Ostrowski, M']",['Efficiency of cosmic ray reflections from an ultrarelativistic shock wave'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, acceleration', 'shock waves, relativistic', 'cosmic radiation, reflection', 'magnetic field, fluctuation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909430'],"['The process of cosmic ray acceleration up to energies in excess of $10^{20}$ eV at relativistic shock waves with large Lorentz factors, $\\Gamma \\gg 1$ requires $\\sim \\Gamma^2$ particle energy gains at single reflections from the shock (cf. Gallant & Achterberg 1999). In the present comment, applying numerical simulations we address an efficiency problem arising for such models. The actual efficiency of the acceleration process is expected to be substantially lower than the estimates of previous authors.']",['1999-09-28'] +938,['eng'],"['Schneider, R', 'Ferrara, A', 'Ciardi, B', 'Ferrari, V', 'Matarrese, S']",['Gravitational Waves Signals from the Collapse of the First Stars'],['Astrophysics and Astronomy'],"['gravitational radiation, emission', 'black hole, massive', 'astrophysics, model', 'matter, mass', 'background, stochastic', 'signal processing', 'counters and detectors', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909419'],"['We study the gravitational wave emission from the first stars which are assumed to be Very Massive Objects (VMOs). We take into account various feedback (both radiative and stellar) effects regulating the collapse of objects in the early universe and thus derive the VMO initial mass function and formation rate. If the final fate of VMOs is to collapse, leaving very massive black hole remnants, then the gravitational waves emitted during each collapse would be seen as a stochastic background. The predicted spectral strain amplitude in a critical density Cold Dark Matter universe peaks in the frequency range \\approx 5 \\times 10^{-4}-5 \\times 10^{-3} Hz where it has a value in the range \\approx 10^{-20}-10^{-19} Hz^{-1/2}, and might be detected by LISA. The expected emission rate is roughly 4000 events/yr, resulting in a stationary, discrete sequence of bursts, i.e. a shot--noise signal.']",['1999-09-27'] +939,['eng'],"['Swordy, S P', 'Kieda, D B']",['Elemental Composition of Cosmic Rays near the Knee by Multiparameter Measurement of Air Showerss'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'showers, air', 'counters and detectors', 'supernova', 'radiation, Cherenkov', 'cosmic radiation, mass', 'correlation', 'experimental results', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909381'],"[""The small change in the spectral slope of the overall intensity of cosmic rays near 1 PeV may be associated with the endpoint energy of supernova shock acceleration. A crucial test of this connection and other ideas of the origin of the spectral `knee' is the reliable determination of the variation of elemental composition in this region. Recent measurements at the DICE/CASA/MIA air shower installation in Dugway, Utah, USA have provided several independent air shower parameters for each event. The derivation of elemental composition from a combination of Cherenkov size, depth of shower maximum in the atmosphere, muon size and electron size at ground level and the reliability of these results are discussed. There is no evidence from these data for a large change in the mean mass of cosmic rays across the `knee'. These measurements show the cosmic rays are composed of ~ 70% protons and alpha-particles near total energies of 10PeV.""]",['1999-09-23'] +940,['eng'],"['Mohapatra, R N', 'Nussinov, S', 'Teplitz, V L']",['TeV Scale Quantum Gravity and Mirror Supernovae as Sources of Gamma Ray Bursts'],['Astrophysics and Astronomy'],"['quantum gravity', 'supernova, mirror', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'fireball', 'neutrino, mirror particle', 'photon, mirror particle']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909376'],"[""Mirror matter models have been suggested recently as an explanation of neutrino puzzles and microlensing anomalies. We show that mirror supernovae can be a copious source of energetic gamma rays if one assumes that the quantum gravity scale is in the TeV range. We show that under certain assumptions plausible in the mirror models, the gamma energies could be degraded to the 10 MeV range (and perhaps even further) so as to provide an explanation of observed gamma ray bursts. This mechanism for the origin of the gamma ray bursts has the advantage that it neatly avoids the ``baryon load problem''.""]",['1999-09-23'] +941,['eng'],"['Spergel, D N', 'Steinhardt, Paul Joseph']",['Observational evidence for self-interacting cold dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'scattering, missing-mass', 'cross section', 'galaxy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909386'],"['Cosmological models with cold dark matter composed of weakly interacting particles predict overly dense cores in the centers of galaxies and clusters and an overly large number of halos within the Local Group compared to actual observations. We propose that the conflict can be resolved if the cold dark matter particles are self-interacting with a large scattering cross-section but negligible annihilation or dissipation. In this scenario, astronomical observations may enable us to study dark matter properties that are inaccessible in the laboratory']",['1999-09-24'] +942,['eng'],"['Cramer, J G', 'Elliott, S R', 'Wilkerson, J F', 'Wilkes, R J', 'Zager, E L']",['The Washington Large Area Time Coincidence Array'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'cosmic radiation', 'showers, air', 'scintillation counter', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909268'],['The number and density of schools in the Seattle area is convenient for the study of distributed particle showers produced at the top of the atmosphere by ultra-high energy (about $10^{20}$ eV) cosmic rays. We are forming a collaboration for the development of a distributed detector network to study air showers from such ultra-high energy cosmic rays. We call the cosmic ray measurement component WALTA (WAshington Large-area Time-coincidence Array). WALTA aims to provide teachers and students the opportunity to become active participants in forefront scientific projects. A cornerstone of the program will be to install a measurement module at each participating school.'],['1999-09-16'] +943,['eng'],"['Guruprasad, V']",['Extreme path accumulation corrections to cosmological and neutrino wave propagation'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'photon, cosmic radiation', 'neutrino, solar', 'diffraction', 'absorption', 'galaxy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909340'],"[""Extremely weak en route losses, due to diffraction and absorption by non-paraxial objects, accumulate sufficiently on the cosmological scale to resolve Olbers' paradox, and could be contributing to dark matter, primeval galaxies and solar neutrino measurements.""]",['1999-09-21'] +944,['eng'],"['Khokhlov, D L']",['The extra high energy cosmic rays spectrum in view of the decay of proton into Planck neutrinos'],['Astrophysics and Astronomy'],"['cosmic radiation, spectra', 'p, decay', 'neutrino, production', 'p, lifetime', 'energy dependence', 'neutrino, cosmic radiation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909322'],['It is assumed that proton decays into Planck neutrinos. The energy of the Planck neutrino is equal to the Planck mass in the preferred rest frame. In the frame moving relative to the preferred rest frame the energy of the Planck neutrino reduces by the corresponding Lorentz factor. The lifetime of proton depends on the kinetic energy of proton relative to the preferred rest frame. The time required for proton travel from the source to the earth defines the limiting energy. Protons with the energies more than the limiting energy decay and do not give contribution in the EHECRs spectrum. It is shown that EHECRs with the energies $E>3 \\times 10^{18} {\\rm eV}$ can be identified with the Planck neutrinos.'],['1999-09-21'] +945,['eng'],"['Huang, W']","['Dark Matter, Mass Scales Sequence, and Superstructure in the Universe']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'fermion, mass', 'boson, mass', 'astrophysics, fundamental constant', 'galaxy', 'cosmic radiation, primary', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909321'],"['There may exist a category of stable non-baryonic dark matter particles in the universe at the present time, they are fermions or bosons with mass extremely high energy primary cosmic ray spectrum at ~10^(-15) eV (""knee"") and shift z~10. The mass scales sequence connected by a large number A, especially the superstructure scale are helpful for us to understand the Hubble constant and the cosmological constant.']",['1999-09-21'] +946,['eng'],"['Abazajian, K N', 'Shi, X', 'Fuller, G M']",['Transformation-Induced Nonthermal Neutrino Spectra and Primordial Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'helium, production', 'neutrino, momentum spectrum', 'neutrino/e, oscillation', 'resonance, oscillation', 'neutrino, sterile', 'lepton number, asymmetry', 'nucleon, semileptonic decay', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909320'],"['We examine in detail the changes in the production of primordial helium resulting from nonthermal neutrino momentum distributions produced by resonant transformation of electron-type neutrinos to steriles. These transformations, anti-nu_e -> anti-nu_s (nu_e->nu_s), amplify a positive (negative) lepton number asymmetry. We find that the resulting supression relative to a thermal distribution of low energy nu_e reduces n -> p conversion to a greater extent than does the enhancement of n -> p from an identical suppression of anti-nu_e. Thus, equal lepton-number asymmetries of opposite sign have unequal effects on the resulting helium yield in primordial nucleosynthesis.']",['1999-09-20'] +947,['eng'],"['Iwasa, N', 'Boué, F', 'Surówka, G', 'Sümmerer, K', 'Baumann, T', 'Blank, B', 'Czajkowski, S', 'Förster, A', 'Gai, M', 'Geissel, H', 'Grosse, E', 'Hellström, M', 'Koczón, P', 'Kohlmeyer, B', 'Kulessa, R', 'Laue, F', 'Marchand, C', 'Motobayashi, T', 'Oeschler, H', 'Ozawa, A', 'Pravikoff, M S', 'Schwab, E', 'Schwab, W', 'Senger, P', 'Speer, J', 'Sturm, C', 'Surowiec, A', 'Teranishi, T', 'Uhlig, F', 'Wagner, A', 'Walús, W', 'Bertulani, C A']",['A Measurement of the Coulomb Dissociation of $^{8}B$ at 254 MeV/nucleon and the $^{8}B$ Solar Neutrino Flux'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'nucleus nucleus, nuclear reaction', 'boron, secondary beam', 'lead', 'dissociation, Coulomb', 'scintillation counter, experimental results', 'Darmstadt SIS', 'photon boron-8 --> beryllium-7 p', '0.254 GeV/nucleon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909317'],"['We have measured the Coulomb dissociation of 8B into 7Be and proton at 254 MeV/nucleon using a large-acceptance focusing spectrometer. The astrophysical S17 factor for the 7Be(p,gamma)8B reaction at E{c.m.} = 0.25-2.78 MeV is deduced yielding S17(0)=20.6 \\pm 1.2 (exp.) \\pm 1.0 (theo.) eV-b. This result agrees with the presently adopted zero-energy S17 factor obtained in direct-reaction measurements and with the results of other Coulomb-dissociation studies performed at 46.5 and 51.2 MeV/nucleon.']",['1999-09-20'] +948,['eng'],"['Hogan, C J']",['Why the Universe is Just So'],['Astrophysics and Astronomy'],"['astrophysics', 'biology', 'space-time', 'grand unified theory', 'gravitation', 'gauge field theory, SU(3) x SU(2) x U(1)', 'quark, mass', 'coupling constant', 'particle, stability', 'fundamental constant', 'nuclear physics', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909295'],"[""Some properties of the universe are fixed by physics derived from mathematical symmetries, others may have been selected from an ensemble of possibilities. Some successes and failures of anthropic reasoning in this context are reviewed in the light of recent developments in astrobiology, cosmology and unification physics. Specific issues raised include our spacetime location (including the reason for the present age of the universe), the timescale of biological evolution, the tuning of global cosmological parameters, the origin of the Large Numbers of astrophysics, and the parameters of the Standard Model. Out of the twenty parameters of the Standard Model,the basic behavior and structures of the world (nucleons, nuclei,atoms, molecules, planets, stars, galaxies) depend mainly on five of them: $m_e,m_u,m_d,\\alpha,\\alpha_G$, three of which are independent in the context of Grand Unified Theories (that is, not related by any known symmetry). These parameters also need to be finely tuned to make stable nucleons and nuclei and abundant carbon, leading to the conjecture that the two light quark masses and one coupling constant are ultimately determined even in the ``Final Theory'' by a choice from a continuous ensemble, and the prediction that the correct unification scheme will not allow calculation of $(m_d-m_u)/m_{proton}$ from first principles.""]",['1999-09-17'] +949,['eng'],"['Tokuhisa, A', 'Kajino, T']",['Meson Synchrotron Emission from Central Engines of Gamma-Ray Bursts with Strong Magnetic Fields'],['Astrophysics and Astronomy'],"['astrophysics, model', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'pi0, cosmic radiation', 'meson, synchrotron radiation', 'pi, charged particle', 'rho(770)0', 'magnetic field, high', 'cosmic radiation, energy spectrum', 'n, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909286'],"['Gamma-ray bursts (GRBs) are presumed to be powered by still unknown central engines for the timescales in the range $1ms \\sim$ a few s. We propose that the GRB central engines would be a viable site for strong meson synchrotron emission if they were the compact astrophysical objects such as neutron stars or rotating black holes with extremely strong magnetic fields $H \\sim10^{12} - 10^{17}G$ and if protons or heavy nuclei were accelerated to ultra-relativistic energies of order $\\sim 10^{12}-10^{22}eV$. We show that the charged scalar mesons like $\\pi^{\\pm}$ and heavy vector mesons like $\\rho$, which have several decay modes onto $\\pi^{\\pm}$, could be emitted with high intensity a thousand times larger than photons through strong couplings to ultra-relativistic nucleons. These meson synchrotron emission processes eventually produce a burst of very high-energy cosmic neutrinos with $10^{12} eV \\leq E_{\\nu}$. These neutrinos are to be detected during the early time duration of short GRBs.']",['1999-09-17'] +950,['eng'],"['Tinyakov, Peter G']",['Ultra-High Energy Cosmic Rays and Diffuse Photon Spectrum'],['Astrophysics and Astronomy'],"['talk, Blois 1999/06/28', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'cosmic radiation, flux', 'astrophysics', 'magnetic field', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909244'],"['It is argued that if extragalactic magnetic fields are smaller than 2x10^{-12} G the flux of ultra-high energy photons of (a few)x10^{-1} eV cm^{-2}s^{-1}sr^{-1} predicted in the top-down models of UHE CR implies similar flux of the diffuse photons in the energy range 10^{15}-10^{17} eV, which is close to the existing experimental limit.']",['1999-09-15'] +951,['eng'],"['Battye, R A', 'Shellard, E P S']",['Axion string cosmology and its controversies'],['Astrophysics and Astronomy'],"['astrophysics, string', 'axion, mass', 'inflationary universe', 'strong interaction, CP', 'critical phenomena', 'axion, decay']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909231'],"['Understanding axion cosmology has important experimental consequences since it constrains the range of allowed values for the axion mass. In the standard thermal scenario, which assumes Peccei-Quinn symmetry restoration after inflation, an axion string network forms at the phase transition $T\\sim\\fa$ and then radiatively decays into a cosmological background of axions. Under standard assumptions for the evolution of this string network and the radiation from it, axions must have a mass of $\\ma\\sim 100\\mu{\\rm eV}$ with large specified uncertainties. We discuss critically the various suggestions in the literature that the axion mass migh be lighter.']",['1999-09-15'] +952,['eng'],"['Shi, X', 'Fuller, G M', 'Abazajian, K N']","['Comments Regarding ""On Neutrino-Mixing-Generated Lepton Asymmetry and the Primordial Helium-4 Abundance""']",['Astrophysics and Astronomy'],"['astrophysics', 'light nucleus, production', 'helium', 'neutrino, interference', 'lepton, asymmetry', 'neutrino, oscillation', 'neutrino, sterile']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909221'],"['This is a reply to the preprint ""On Neutrino-Mixing-Generated Lepton Asymmetry and the Primordial Helium-4 Abundance"" by M. V. Chizhov and D. P. Kirilova (hep-ph/9908525), which criticised our recent publication (X. Shi, G. M. Fuller and K. Abazajian Phys. Rev. D 60, 063002 (1999)). Here we point out factual errors in their description of what our paper says. We also show that their criticisms of our work have no merit.']",['1999-09-15'] +953,['eng'],"['Ahluwalia, D V']",['On Quantum Nature of Black-Hole Spacetime'],['Astrophysics and Astronomy'],"['black hole', 'space-time', 'quantum mechanics', 'radiation, Hawking', 'operator', 'quantum gravity']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909192'],"[""Atoms and the planets acquire their stability from the quantum mechanical incompatibility of the position and momentum measurements. This incompatibility is expressed by the fundamental commutator [x, p_x]=i hbar, or equivalently, via the Heisenberg's uncertainty principle Delta x Delta p_x sim hbar. A further stability-related phenomenon where the quantum realm plays a dramatic role is the collapse of certain stars into white dwarfs and neutron stars. Here, an intervention of the Pauli exclusion principle, via the fermionic degenerate pressure, stops the gravitational collapse. However, by the neutron-star stage the standard quantum realm runs dry. One is left with the problematic collapse of a black hole. This essay is devoted to a concrete argument on why the black-hole spacetime itself should exhibit a quantum nature. The proposed quantum aspect of spacetime is shown to prevent the general-relativistic dictated problematic collapse. The quantum nature of black-hole spacetime is deciphered from a recent result on the universal equal-area spacing [=lambda_P^2 4 ln(3)] for black holes. In one interpretation of the emergent picture, an astrophysical black hole can fluctuate to sqrt{pi/ln(3)} approx 1.7 times its classical size, and thus allow radiation and matter to escape to the outside observers. These fluctuations I conjecture provide a new source, perhaps beyond Hawking radiation, of intense radiation from astrophysical black holes and may be the primary source of observed radiation from those galactic cores what carry black hole(s). The presented interpretation may be used as a criterion to choose black holes from black hole candidates.""]",['1999-09-14'] +954,['eng'],"['Amenomori, M', 'Ayabe, S', 'Cao, P Y', 'Danzengluobu', 'Ding, L K', 'Feng, Z Y', 'Fu, Y', 'Guo, H W', 'He, M', 'Hibino, K', 'Hotta, N', 'Huang, Q', 'Huo, A X', 'Izu, K', 'Jia, H Y', 'Kajino, F', 'Kasahara, K', 'Katayose, Y', 'Labaciren', 'Li Jing Yi', 'Lu, H', 'Lu, S L', 'Luo, G X', 'Meng, X R', 'Mizutani, K', 'Mu, J', 'Nanjo, H', 'Nishizawa, M', 'Ohnishi, M', 'Ohta, I', 'Ouchi, T', 'Ren, J R', 'Saitô, T', 'Sakata, M', 'Sasaki, T', 'Shi, Z Z', 'Shibata, M', 'Shiomi, A', 'Shirai, T', 'Sugimoto, H', 'Taira, K', 'Tan, Y H', 'Tateyama, N', 'Torii, S', 'Utsugi, T', 'Wang, C R', 'Wang, H', 'Xu, X W', 'Yamamoto, Y', 'Yu, G C', 'Yuan, A F', 'Yuda, T', 'Zhang, C S', 'Zhang, H M', 'Zhang, J L', 'Zhang, N J', 'Zhang, X Y', 'Zhaxi Sang Zhu', 'Zha Xi Ciren', 'Zhou, W D']",['Observation of Multi-Tev Gamma Rays from the Crab Nebula Using the Tibet Air Shower Array'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909172'],"['The Tibet experiment, operating at Yangbajing (4,300 m above sea level), is the lowest energy air shower array and the new high density array constructed in 1996 has sensitivity to $\\gamma$-ray air showers at energies as low as 3 TeV. With this new array, the Crab Nebula was observed in multi-TeV obtained the energy spectrum of $\\gamma$-rays in the energy region above 3 TeV which partially overlaps those observed with imaging atmospheric Cherenkov telescopes. This is the first observation of $\\gamma$-ray signals from point sources with a conventional air shower array using scintillation detectors.']",['1999-09-13'] +955,['eng'],"['Hwang, J']",['Conserved quantities in the perturbed Friedmann world model'],['Astrophysics and Astronomy'],"['talk, Seoul 1998/02/21', 'Friedman model', 'gravitation', 'gravitational radiation', 'space-time, perturbation', 'angular momentum', 'invariance, gauge']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909150'],"['The evolutions of linear structures in a spatially homogeneous and isotropic world model are characterized by some conserved quantities: the amplitude of gravitational wave is conserved in the super-horizon scale, the perturbed three-space curvature in the comoving gauge is conserved in the super-sound-horizon scale, and the angular momentum of rotational perturbation is generally conserved.']",['1999-09-10'] +956,['eng'],"['Garriga, J', 'Mukhanov, V F', 'Olum, K D', 'Vilenkin, A']","['Eternal inflation, black holes, and the future of civilizations']",['Astrophysics and Astronomy'],"['talk', 'inflationary universe', 'black hole', 'energy, density', 'field theory, scalar', 'space-time', 'tunneling']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909143'],"['We discuss the large-scale structure of the universe in inflationary cosmology and the implications that it may have for the long-term future of civilizations. Although each civilization is doomed to perish, it may be possible to transmit its accumulated knowledge to future civilizations. We consider several scenarios of this sort. If the cosmological constant is positive, it eventually dominates the universe and bubbles of inflationary phase begin to nucleate at a constant rate. Thermalized regions inside these inflating bubbles will give rise to new galaxies and civilizations. It is possible in principle to send a message to one of them. It might even be possible to send a device whose purpose is to recreate an approximation of the original civilization in the new region. However, the message or device will almost certainly be intercepted by black holes, which nucleate at a much higher rate than inflating bubbles. Formation of new inflating regions can also be triggered by gravitational collapse, but again the probability is low, and the number of attempts required for a positive outcome is enormous. The probability can be higher if the energy scale of inflation is closer to the Planck scale, but a high energy scale produces a tight bound on the amount of information that can be transmitted. One can try to avoid quantum tunneling altogether, but this requires a violation of quantum inequalities which constrain the magnitude of negative energy densities. However, the limits of validity of quantum inequalities are not clear, and future research may show that the required violation is in fact possible. Therein lies the hope for the future of civilizations.']",['1999-09-09'] +957,['eng'],"['Horns, D', 'Schmele, D']",['Anisotropies of Cosmic Rays and Search for Intergalactic Cascades from the direction of the Highest Energetic Cosmic Ray Events with the HEGRA Scintillator Array'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, anisotropy', 'cosmic radiation, particle source', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909125'],"['Data taken with the HEGRA Scintillator Array have been used to search for spatial anisotropies in the arrival directions of cosmic rays above 20 TeV. In this paper results on the search for TeV gamma-ray emission from the Galactic plane and the Gould belt are presented. Furthermore, a search for TeV gamma-ray emission correlated with the arrival directions of cosmic rays with energies well beyond the Greizen-Zatsepin-Kuzmin cutoff has been performed. Such a correlation can be expected from sufficiently high energetic nuclei inducing electromagnetic cascades on the diffuse intergalactic background radiation, eventually producing TeV photons. Interestingly, the direction of the most energetic event yields the highest excess with a chance probability of 1.8%.']",['1999-09-08'] +958,['eng'],"['Baltz, E A', 'Briot, C A A', 'Salati, Pierre', 'Taillet, R', 'Silk, J']",['Detection of Neutralino Annihilation Photons from External Galaxies'],['Astrophysics and Astronomy'],"['neutrino, annihilation', 'galaxy', 'astrophysics, missing-mass', 'photon, cosmic radiation', 'cosmic radiation, secondary radiation', 'cosmic radiation, flux', 'supersymmetry', 'Cherenkov counter', 'signal processing', 'background', 'sparticle, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909112'],"['We consider neutralino annihilation in dense extragalactic systems known to be dominated by dark matter, in particular M87 and several local dwarf spheroidal galaxies. These annihilations can produce energetic gamma rays which may be visible to atmospheric Cerenkov telescopes. We explore the supersymmetric parameter space, and compute the expected flux of gamma--rays coming from these objects. It is shown that some parts of the parameter space lead to a signal observable with the next generation of Cerenkov telescopes, provided the supersymmetric dark matter has a clumpy structure, as may be expected in a hierarchical scenario for structure formation.']",['1999-09-08'] +959,['eng'],"['Atkins, R']",['TeV Observations of Markarian 501 with the Milagrito Water Cherenkov Detector'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'blazar', 'cosmic radiation, time variation', 'Cherenkov counter, water', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909090'],"['The Milagrito water Cherenkov detector near Los Alamos, New Mexico, operated as a sky monitor at energies of a few TeV between February 1997 and May 1998 including the period of the strong, long-lasting 1997 flare of Markarian 501. Milagrito served as a test run for the full Milagro detector. An event excess with a significance of 3.7 sigma from Markarian 501 was observed, in agreement with expectations.']",['1999-09-07'] +960,['eng'],"['Straumann, N']",['The mystery of the cosmic vacuum energy density and the accelerated expansion of the Universe'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'vacuum state', 'energy, density', 'expansion, acceleration', 'supernova', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'temperature, fluctuation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908342'],"['After a short history of the $\\Lambda$-term it is explained why the (effective) cosmological constant is expected to obtain contributions from short-distance-physics, corresponding to an energy scale of at least 100 GeV. The actual tiny value of the cosmological constant in any natural scale of units represents, therefore, one of the deepest mysteries of present day fundamental physics. We also briefly discuss recent astronomical evidence for a cosmologically significant vacuum energy density causing an accelerating expansion of the universe. This arises mainly from the Hubble diagram of type Ia supernovae and from the observed temperature fluctuations of the cosmic microwave background radiation. If this should become an established fact, we are also confronted with a disturbing {\\it cosmic coincidence} problem.']",['1999-09-01'] +961,['eng'],"['Ehrlich, R']",['Lorentz Symmetry-Breaking Formalisms and Tachyonic and Relic Neutrinos'],['Astrophysics and Astronomy'],"['neutrino/e, cosmic radiation', 'cosmic radiation, spectra', 'tachyon', 'cosmic radiation, flux', 'energy dependence', 'proposed experiment', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812336'],['The hypothesis by Coleman and Glashow that Lorentz Symmetry is slightly broken is examined and compared with two other unrelated conjectures in terms of their specific predictions.'],['1998-12-18'] +962,['eng'],"['Hanauske, M', 'Zschiesche, D', 'Pal, S', 'Schramm, S', 'Stöcker, H', 'Greiner, W']",['Neutron star properties in a chiral SU(3) model'],['Astrophysics and Astronomy'],"['n, matter', 'symmetry, chiral', 'symmetry, SU(3) x SU(3)', 'hyperon, effect', 'Lagrangian formalism', 'matter, strangeness', 'mean field approximation', 'matter, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9909052'],"['We investigate various properties of neutron star matter within an effective chiral $SU(3)_L \\times SU(3)_R$ model. The predictions of this model are compared with a Walecka-type model. It is demonstrated that the importance of hyperon degrees are strongly depending on the interaction used, even if the equation of state near saturation density is nearly the same in both models. While the Walecka-type model predicts a strange star core with strangeness fraction $f_S \\approx 4/3$, the chiral model allows only for $f_S \\approx 1/3$ and predicts that $\\Sigma^0$, $\\Sigma^+$ and $\\Xi^0$ will not exist in star, in contrast to the Walecka-type model.']",['1999-09-03'] +963,['eng'],"['Kühne, R W']",['Time-Varying Fine-Structure Constant Requires Cosmological Constant'],['Astrophysics and Astronomy'],"['fundamental constant, fine structure', 'time variation', 'astrophysics, fundamental constant']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908356'],"[""Webb et al. presented preliminary evidence for a time-varying fine-structure constant. We show Teller's formula for this variation to be ruled out within the Einstein-de Sitter universe, however, it is compatible with cosmologies which require a large cosmological constant.""]",['1999-09-01'] +964,['eng'],"['Hwang, J', 'Noh, H']",['COBE constraints on inflation models with a massive non-minimal scalar field'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'massive', 'spectra, scalar', 'spectra, tensor', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation', 'relativity theory, general', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908340'],"['We derive power spectra of the scalar- and tensor-type structures generated in an inflation model based on a massive non-minimally coupled scalar field with the strong coupling assumption. We make analyses in both the original-frame and the conformally transformed Einstein-frame. We derive contributions of both structures to the anisotropy of the cosmic microwave background radiation, and compare the contributions with the four-year COBE-DMR data. Previous study showed that sufficient amount of inflation requires a small coupling parameter. In such a case the spectra become near Zeldovich spectra, and the gravitational wave contribution becomes negligible compared with the scalar-type contribution which is testable in future CMBR experiments.']",['1999-09-01'] +965,['eng'],"['Harwit, M', 'Protheroe, R J', 'Biermann, P L']",['TeV Cherenkov Events as Bose-Einstein Gamma Condensations'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, condensation', 'radiation, Cherenkov', 'cosmic radiation, diffusion', 'cosmic radiation, particle source', 'coherence', 'showers, air', 'photon, fluctuation', 'photon, production', 'electron, relativistic', 'synchrotron radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908338'],"['The recent detection of gamma radiation from Mkn 501 at energies as high as 25 TeV suggests stringent upper bounds on the diffuse, far infrared, extragalactic radiation density. The production of electron-positron pairs through photon-photon collisions would prevent gamma photons of substantially higher energies from reaching us across distances of order 100 Mpc. However, coherently arriving TeV or sub-TeV gammas - Bose-Einstein condensations of photons at these energies - could mimic the Cherenkov shower signatures of extremely energetic gammas. To better understand such events, we describe their observational traits and discuss how they might be generated.']",['1999-09-01'] +966,['eng'],"['Janka, H T', 'Eberl, T', 'Ruffert, M', 'Fryer, C L']",['Black Hole-Neutron Star Mergers as Central Engines of Gamma-Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'black hole', 'n, matter', 'back reaction, hydrodynamical', 'gravitational radiation, emission', 'neutrino, emission', 'matter, mass ratio', 'neutrino antineutrino, annihilation', 'electron, pair production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908290'],"['Hydrodynamic simulations of the merging of stellar mass black hole -- neutron star binaries (BH/NS) are compared with mergers of binary neutron stars (NS/NS). The simulations are Newtonian, but take into account the emission of gravitational waves and their backreaction on the hydrodynamics. The use of a physical nuclear equation of state allowed us to include the effects of neutrino emission by a neutrino trapping scheme. For low neutron star to black hole mass ratios the neutron star transfers mass to the black hole during a few cycles of orbital decay and subsequent widening before finally being disrupted, whereas for ratios near unity the neutron star is already distroyed during its first approach. A gas mass between about 0.3 and about 0.7 solar masses is left in an accretion torus around the black hole and radiates neutrinos at a luminosity of several 10^{53} erg/s. The emitted neutrinos and antineutrinos annihilate into electron-positron pairs with efficiencies of a few percent and rates of up to about 2*10^{52} erg/s, releasing an estimated energy of up to about 10^{51} erg in a pair-plasma fireball, which could give rise to a gamma-ray burst.']",['1999-08-27'] +967,['eng'],"['Allen, G E', 'Gotthelf, E V', 'Petre, R']",['Evidence of 10-100 TeV Electrons in Supernova Remnants'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'supernova', 'photon, cosmic radiation', 'synchrotron radiation', 'electron, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, acceleration', 'numerical calculations, interpretation of experiments']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908209', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_2_12.pdf']","['Analyses of the X-ray data of the five young shell-type supernova remnants Cas A, Kepler, Tycho, SN 1006, and RCW 86 suggest that some of the X-ray emission of these sources is non-thermal. This non-thermal emission is qualitatively consistent with models of the broad-band (radio-to-X-ray) synchrotron spectra of remnants and does not seem to be consistent with other non-thermal X-ray emission processes. If this emission is produced by synchrotron radiation, the radio-to-X-ray synchrotron spectra imply that the electron spectra have differential spectral indices of about 2.2 and exponential cut offs at energies ~ 10 TeV. If the remnants also accelerate cosmic-ray nuclei, the total energies of the cosmic rays in the remnants are estimated to be ~ 1-5 X 10^49 erg. Therefore, the shapes of the cosmic-ray electron spectra, the maximum energies of the cosmic-ray electrons, and the total cosmic-ray energies of the five young remnants seem to be consistent with the idea that Galactic cosmic rays are predominantly accelerated in the shocks of supernova remnants.']",['1999-08-20'] +968,['eng'],"['Uchihori, Y', 'Nagano, M', 'Takeda, M', 'Teshima, M', 'Lloyd-Evans, J', 'Watson, A A']",['Cluster Analysis of Extremely High Energy Cosmic Rays in the Northern Sky'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'galaxy, cluster', 'showers, air', 'cosmic radiation, spatial distribution', 'cosmic radiation, anisotropy', 'showers, multiplet', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908193'],"['The arrival directions of extremely high energy cosmic rays (EHECR) above $4\\times10^{19}$ eV, observed by four surface array experiments in the northern hemisphere,are examined for coincidences from similar directions in the sky. The total number of cosmic rays is 92.A significant number of double coincidences (doublet) and triple coincidences (triplet) are observed on the supergalactic plane within the experimental angular resolution. The chance probability of such multiplets from a uniform distribution is less than 1 % if we consider a restricted region within $\\pm 10^{\\circ}$ of the supergalactic plane. Though there is still a possibility of chance coincidence, the present results on small angle clustering along the supergalactic plane may be important in interpreting EHECR enigma. An independent set of data is required to check our claims.']",['1999-08-19'] +969,['eng'],"['Lloyd, N M', 'Petrosian, V', 'Mallozzi, R S']",['Cosmological versus Intrinsic'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'correlation', 'synchrotron radiation', 'shock waves', 'data analysis method', 'counters and detectors, threshold', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908191'],"[""We present results of correlation studies, examining the association between the peak of the nu F_nu spectrum of gamma ray bursts, E_p, with the burst's energy fluence and photon peak flux. We discuss methods to account for data truncation in E_p and fluence or flux when performing the correlation analyses. However, because bursts near the detector threshold are not usually able to provide reliable spectral parameters, we focus on results for the brightest bursts in which we can better understand the selection effects relevant to E_p and burst strength. We find that there is a strong correlation between total fluence and E_p. We discuss these results in terms of both cosmological and intrinsic effects. In particular, we show that for realistic distributions of the burst parameters, cosmological expansion alone cannot account for the correlation between E_p and total fluence; the observed correlation is likely a result of an intrinsic relation between the burst rest-frame peak energy and the total radiated energy. We investigate this latter scenario in the context of synchrotron radiation from external and internal shock models of GRBs. We find that the internal shock model is consistent with our interpretation of the correlation, while the external shock model cannot easily explain this intrinsic relation between peak energy and burst radiated energy.""]",['1999-08-18'] +970,['eng'],"['Vasilev, V', 'Carter-Lewis, D A', 'Hillas, A M', 'Kertzman, M P', 'Knapp, J', 'Krennrich, F', 'Lessard, R W', 'Rose, H J', 'Sembroski, G H']",['VERITAS'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'showers, air', 'Cherenkov counter, imaging', 'angular resolution', 'energy resolution']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908135', 'http://krusty.physics.utah.edu/~icrc1999/root/vol5/o4_3_35.pdf']","['VERITAS is a proposed major ground-based gamma-ray observatory to be built at the Whipple Observatory in southern Arizona, USA. It will consist of an array of seven 10m imaging Cherenkov telescopes designed to conduct gamma-ray observations in the energy range of 50 GeV - 50 TeV. A description of the baseline VERITAS design and optimization criteria are presented. We provide basic characteristics of the array performance for observations of point sources, such as angular resolution, energy threshold, energy resolution, and integral flux sensitivity. The limiting factors of the VERITAS performance are discussed.']",['1999-08-13'] +971,['eng'],"['Magnussen, N']",['The Physics Potential of Ground-Based Gamma-Ray Astronomy below 50 GeV'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'radiation, Cherenkov', 'supernova', 'pulsar', 'astrophysics, missing-mass', 'quantum gravity, validity test']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908109', 'http://krusty.physics.utah.edu/~icrc1999/root/vol4/o2_4_19.pdf']","['Currently three ground-based Air Cherenkov detectors with energy thresholds below 50 GeV are being commissioned (CELESTE and STACEE) or under construction (MAGIC Telescope). Based on the expected performance of the MAGIC Telescope and with an emphasis on those physics questions which are unique to the energy domain below 50 GeV an overview of the scientific prospects of ground-based high energy Gamma-Ray Astronomy in terms of astrophysics, cosmology and particle physics questions is given.']",['1999-08-11'] +972,['eng'],"['Roberts, M D']",['Cosmic ray composition estimation below the knee of the spectrum from the time structure of Cherenkov light in EAS'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'showers, air', 'radiation, Cherenkov', 'cosmic radiation, primary', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908098'],"['Monte Carlo simulations show that the pulse profile of Cherenkov photons measured near the core of an extensive air shower is sensitive to the secondary muon/electron ratio of the cascade. Cherenkov pulses can easily be measured with a single large area mirror viewed by a photomultiplier tube subtending a small field of view (~1 degree). Even for such a simple experiment, exposed to EAS from a range of core locations and arrival directions, strong statistical differences are shown to exist between the pulse parameter distributions of primary protons and those of heavier primary particles. A range of primary energies can be investigated by varying the zenith angle of observations. In this paper, results from simulations of primaries in the energy range 20TeV to 400TeV are presented, although in principle the technique could be extended to include the knee of the spectrum. At the lower end of this energy range results can be compared to direct measurements of the composition, while measurements at the upper end can augment results from existing ground based experiments.']",['1999-08-10'] +973,['eng'],"['Hofmann, W', 'Lampeitl, H', 'Konopelko, A K', 'Krawczynski, H']",['Improved energy resolution for VHE gamma-ray astronomy with systems of Cherenkov telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'Cherenkov counter, imaging', 'energy resolution', 'statistical analysis']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908092'],"['We present analysis techniques to improve the energy resolution of stereoscopic systems of imaging atmospheric Cherenkov telescopes, using the HEGRA telescope system as an example. The techniques include (i) the determination of the height of the shower maximum, which is then taken into account in the energy determination, and (ii) the determination of the location of the shower core with the additional constraint that the direction of the gamma rays is known a priori. This constraint can be applied for gamma-ray point sources, and results in a significant improvement in the localization of the shower core, which translates into better energy resolution. Combining both techniques, the HEGRA telescopes reach an energy resolution between 9% and 12%, over the entire energy range from 1 TeV to almost 100 TeV. Options for further improvements of the energy resolution are discussed.']",['1999-08-10'] +974,['eng'],"['Vasilev, V']",['Extragalactic background light absorption signal in the TeV $\\gamma$-ray spectra of blazars'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'galaxy, AGN', 'cosmic radiation, background', 'photon, absorption', 'Cherenkov counter', 'blazar', 'experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908088'],"[""Recent observations of the TeV gamma-ray spectra of the two closest active galactic nuclei (AGNs), Markarian 501 (Mrk 501) and Markarian 421 (Mrk 421), by the Whipple and HEGRA collaborations have stimulated efforts to estimate or limit the spectral energy density (SED) of extragalactic background light (EBL) which causes attenuation of TeV photons via pair-production when they travel cosmological distances. In spite of the lack of any distinct cutoff-like feature in the spectra of Mrk 501 and Mrk 421 (in the interval 0.26-10 TeV) which could clearly indicate the presence of such a photon absorption mechanism, we demonstrate that strong EBL attenuation signal (survival probability of 10 TeV photon <10^{-2}) may still be present in the spectra of these AGNs. By estimating the minimal and maximal opacity of the universe to TeV gamma-ray photons, we calculate the visibility range for current and future gamma-ray observatories. Finally, we show that the proposed experiments, VERITAS, HESS, and MAGIC, may even be able to actually measure the EBL SED because their observations extend to the critical 75-150 GeV regime. In this transition region a distinct ``knee-like'' feature should exist in the spectra of blazars, which is invariant with respect to their intrinsic properties. The change of the spectral index and flux amplitude across this knee, if observed for several blazars, will provide missing pieces of information needed to measure EBL in the wavelength range 0.1-30 $\\mu$m.""]",['1999-08-10'] +975,['eng'],"['Wittek, W', 'Kornmayer, H']",['Correlations between parameters of extended air showers and their proper use in analyses'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'showers, air', 'photon, cosmic radiation', 'showers, energy', 'scintillation counter', 'correlation', 'Cherenkov counter', 'data analysis method', 'numerical calculations, Monte Carlo', 'interpretation of experiments']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908029', 'http://krusty.physics.utah.edu/~icrc1999/root/vol1/h2_2_16.pdf']","['In air shower experiments information about the initial cosmic ray particle or about the shower development is obtained by exploiting the correlations between the quantities of interest and the directly measurable quantities. It is shown how these correlations are properly treated in order to obtain unbiased results. As an example, the measurement of the average penetration depth as a function of the shower energy is presented.']",['1999-08-05'] +976,['eng'],"['Cillis, A N', 'Sciutto, S J']",['Air Showers and Geomagnetic Field'],['Astrophysics and Astronomy'],"['charged particle, cosmic radiation', 'showers, air', 'magnetic field, effect', 'muon, cosmic radiation', 'cosmic radiation, spatial distribution', 'cosmic radiation, angular distribution', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908002'],"['The influence of the geomagnetic field on the development of air showers is studied. The well known International Geomagnetic Reference Field was included in the AIRES air shower simulation program as an auxiliary tool to allow calculating very accurate estimations of the geomagnetic field given the geographic coordinates, altitude above sea level and date of a given event. Our simulations indicate that the geomagnetic deflections alter significantly some shower observables like, for example, the lateral distribution of muons in the case of events with large zenith angles (larger than 75 degrees). On the other hand, such alterations seem not to be important for smaller zenith angles. Global observables like total numbers of particles or longitudinal development parameters do not present appreciable dependences on the geomagnetic deflections for all the cases that were studied.']",['1999-08-03'] +977,['eng'],"['Foot, R']",['Have mirror planets been observed?'],['Astrophysics and Astronomy'],"['astrophysics', 'matter, mirror', 'matter, orbit', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908276'],"['Over the last few years, several close orbiting ($\\sim 0.05$ AU) large mass planets ($M \\sim M_{Jupiter}$) of nearby stars have been discovered. Their existence has been inferred from tiny doppler shifts in the light from the star. We suggest that these planets may be made of mirror matter. We also point out that some stars such as our sun may also have a similar amount of mirror matter, which has escaped detection due to the effects of a tiny force such as photon - mirror photon kinetic mixing or something else.']",['1999-08-26'] +978,['eng'],"['Xu, R X', 'Dai, Z G', 'Hong, B H', 'Qiao, G J']",['GRB'],['Astrophysics and Astronomy'],"['talk, Hong Kong 1999/08/03', 'photon, cosmic radiation', 'quark gluon, plasma', 'n, matter', 'matter, strangeness', 'critical phenomena', 'quantum chromodynamics', 'astrophysics, white dwarf', 'black hole', 'supernova']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908262'],"['It is suggested that the inner energetic engine of Gamma ray burst (GRB) may be the result of the transition of normal hadron to quark-gluon plasma (QGP) in rapidly-rotating and spin-down newborn neutron star. When such a nascent neutron star slows down through dipole electromagnetic and quadruple gravitational radiation, the increasing center density may reach the QCD transition density, i.e., 5-10 nuclear density. Such kind of energy release from the phase transition would be responsible for GRB and its possible beaming effect. The relative dense gaseous environment of GRB location and the iron line observed in the X-ray afterglow support this idea. Some predictions in this model are given. keywords: Gamma-ray Bursts, Supernova, Quark-gluon plasma']",['1999-08-25'] +979,['eng'],"['Esposito, S', 'Mangano, G', 'Miele, G', 'Pisanti, O']",['Primordial Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Valencia 1999/05/03', 'astrophysics, model', 'light nucleus, production', 'helium', 'nucleon, weak interaction', 'Born approximation', 'radiative correction', 'nucleon, mass', 'plasma, effect', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907420'],"['A new accurate evaluation of primordial light nuclei abundances is presented. The proton to neutron conversion rates have been corrected to take into account radiative effects, finite nucleon mass, thermal and plasma corrections. The theoretical uncertainty on 4He is so reduced to the order of 0.1%.']",['1999-07-30'] +980,['eng'],"['Esposito, S', 'Mangano, G', 'Miele, G', 'Pisanti, O']",['New results in primordial nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, San Miniato 1999/05/17', 'astrophysics, model', 'light nucleus, production', 'light nucleus, yield', 'helium', 'deuterium', 'lithium', 'nucleus, weak interaction', 'Born approximation', 'radiative correction', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907421'],"['We report the results of a new accurate evaluation of light nuclei yields in primordial nucleosynthesis. The relic densities of 4He, D and 7Li have been numerically obtained via a new updated version of the standard BBN code.']",['1999-07-30'] +981,['eng'],"['Esposito, S', 'Mangano, G', 'Miele, G', 'Pisanti, O']",['A detailed analysis of the neutron to proton ratio at the onset of primordial nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Faro 1998/09/03', 'astrophysics, model', 'light nucleus, production', 'p n, ratio', 'weak interaction', 'Born approximation, correction', 'temperature', 'nucleon, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907422'],"['We report on the results of a recent evaluation of all percent level corrections to weak rates of processes converting n <-> p, which are crucial for the determination of the 4He mass fraction produced during primordial nucleosynthesis.']",['1999-07-30'] +982,['eng'],"['Halzen, Francis', 'Hooper, D W']",['Neutrino Event Rates from Gamma Ray Bursts'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'fireball, relativistic', 'photon, cosmic radiation', 'effect, fluctuation', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908138'],"['We recalculate the diffuse flux of high energy neutrinos produced by Gamma Ray Bursts (GRB) in the relativistic fireball model. Although we confirm that the average single burst produces only ~10^{-2} high energy neutrino events in a detector with 1 km^2 effective area, i.e. about 10 events per year, we show that the observed rate is dominated by burst-to-burst fluctuations which are very large. We find event rates that are expected to be larger by one order of magnitude, likely more, which are dominated by a few very bright bursts. This greatly simplifies their detection.']",['1999-08-13'] +983,['eng'],"['Horowitz, C J', 'Li, G']",['Charge-conjugation violating neutrino interactions in supernovae'],['Astrophysics and Astronomy'],"['supernova', 'neutrino nucleon, interaction', 'antineutrino nucleon, interaction', 'charge conjugation, violation', 'neutrino, transport theory', 'neutrino, energy', 'Boltzmann equation', 'neutrino, current', 'neutrino, path length', 'finite temperature', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908219'],"['The well known charge conjugation violating interactions in the Standard Model increase neutrino- and decrease anti-neutrino- nucleon cross sections. This impacts neutrino transport in core collapse supernovae through ""recoil"" corrections of order the neutrino energy $k$ over the nucleon mass $M$. All $k/M$ corrections to neutrino transport deep inside a protoneutron star are calculated from angular integrals of the Boltzmann equation. We find these corrections significantly modify neutrino currents at high temperatures. This produces a large mu and tau number for the protoneutron star and can change the ratio of neutrons to protons. In addition, the relative size of neutrino mean free paths changes. At high temperatures, the electron anti-neutrino mean free path becomes {\\it longer} than that for mu or tau neutrinos.']",['1999-08-20'] +984,['eng'],"['Arqueros, F']",['Energy Spectrum and Chemical Composition of Cosmic Rays between 0.3 and 10 PeV determined from the Cherenkov-Light and Charged-Particle distributions in Air Showers'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'elements, cosmic radiation', 'photon, cosmic radiation', 'radiation, Cherenkov', 'showers, air', 'showers, angular distribution', 'cosmic radiation, electromagnetic component', 'numerical calculations, Monte Carlo', 'shower detector, experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908202'],"[""Measurements of the lateral distribution of Cherenkov photons with the wide-angle atmospheric Cherenkov light detector array AIROBICC and of the charged particle lateral distribution with the scintillator matrix of the HEGRA air-shower detector complex in air showers are reported. With the atmospheric shower-front sampling technique these detectors measure the electromagnetic component of an extensive air shower via the lateral density distribution of the shower particles and of the Cherenkov photons. The data are compared with events generated with the CORSIKA program package with the QGSJET hadronic-event generator. Consistency checks performed with primary energy-reconstruction methods based on different shower observables indicate satisfactory agreement between these extensive air shower simulations and the experimental data. The energy spectrum features a so called ``knee'' at an energy of E_knee = 3.98 (+4.66) (-0.83) (stat) +- 0.53 (syst) PeV. Power law fits to the differential energy spectrum yield indices of -2.72 (+0.02)(-0.03) (stat) +- 0.07 (syst) below, and -3.22 (+0.47) (-0.59) (stat) +- 0.08 (syst)} above the knee. The best-fit elongation rate for the whole energy range is determined to 78.3 +- 1.0 (stat) +- 6.2 (syst) g/cm^2. At the highest energies it seems to decrease slightly.The best-fit fraction of light nuclei decreases from 37 (+28) (-21) % (combined statistical and systematic) to 8 (+32) (-8) % (combined statistical and systematic) in the energy range discussed here. A detailed study of the systematic errors reveals that a non-changing composition cannot be excluded.""]",['1999-08-19'] +985,['eng'],"['Xu, R X', 'Qiao, G J']",['Electric Character of Strange Stars'],['Astrophysics and Astronomy'],"['matter, strangeness', 'quark, matter', 'electron, density', 'electric field', 'quark, charge', 'charge, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908176'],"['Using the Thomas-Fermi model, we investigated the electric characteristics of a static non-magnetized strange star without crust in this paper. The exact solutions of electron number density and electric field above the quark surface are obtained. These results are useful if we are concerned about physical processes near the quark matter surfaces of strange stars.']",['1999-08-18'] +986,['eng'],"['Kaminker, A D', 'Haensel, P']",['Neutrino emission due to electron bremsstrahlung in superfluid neutron-star cores'],['Astrophysics and Astronomy'],"['n, matter', 'superfluid', 'electron electron, interaction', 'electron p, interaction', 'electron, bremsstrahlung', 'neutrino, emission', 'temperature, dependence', 'energy loss', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908249'],['We study neutrino energy emission rates (emissivities) due to electron bremsstrahlung produced by $ee$ and $ep$ collisions in the superfluid neutron star cores. The neutrino emission due to $ee$ collisions is shown to be the dominant neutrino reaction at not too high temperatures ($T \\la 10^8$ K) in dense matter if all other neutrino reactions involving nucleons are strongly suppressed by neutron and proton superfluidity. Simple practical expressions for the $ee$ and $ep$ neutrino emissivities are obtained. The efficiency of various neutrino reactions in the superfluid neutron-star cores is discussed for the cases of standard neutrino energy losses and the losses enhanced by the direct Urca process.'],['1999-08-24'] +987,['eng'],"['Kohri, K', 'Yokoyama, J']","['Primordial Black Holes and Primordial Nucleosynthesis; 1, Effects of Hadron Injection from Low Mass Holes']",['Astrophysics and Astronomy'],"['astrophysics, model', 'black hole, radiation', 'hadron, emission', 'light nucleus, production', 'jet, emission', 'hadron hadron, interaction', 'black hole, density', 'black hole, lifetime', 'black hole, mass', 'upper limit', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908160'],"[""We investigate the influence of hadron injection from evaporating primordial black holes (PBHs) in the early stage of the primordial nucleosynthesis era (t = 10^{-3} - 10^4 sec). The emitted quark-antiquark pairs or gluons immediately fragment into a lot of hadrons and scatter off the thermal plasma which is constituted by photons, electrons and nucleons. For the relatively low mass holes we point out that the dominant effect is the inter-conversion between ambient proton and neutron through the strong interaction induced by the emitted hadrons. Even after the freeze-out time of the week interactions between neutron and proton, more neutrons are produced and the synthesized light element abundances could be drastically changed. Comparing the theoretical predictions with the observational data, we constrain the PBH's density and their lifetime. We obtain the upper bound for PBH's initial mass fraction, \\beta < 10^{-20} for 10^8 g < M < 10^{10} g, and \\beta < 10^{-22} for 10^{10} g < M < 3 * 10^{10} g.""]",['1999-08-17'] +988,['eng'],"['Huterer, D', 'Turner, M S']",['On the degree of scale invariance of inflationary perturbations'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'spectra, perturbation', 'scaling, invariance', 'potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908157'],"[""Many, if not most, inflationary models predict the power-law index of the spectrum of density perturbations is close to one, though not precisely equal to one, |n-1| \\sim O(0.1), implying that the spectrum of density perturbations is nearly, but not exactly, scale invariant. Some models allow n to be significantly less than one (n \\sim 0.7); a spectral index significantly greater than one is more difficult to achieve. We show that n \\approx 1 is a consequence of the slow-roll conditions for inflation and ``naturalness,'' and thus is a generic prediction of inflation. We discuss what is required to deviate significantly from scale invariance, and then show, by explicit construction, the existence of smooth potentials that satisfy all the conditions for successful inflation and give $n$ as large as 2.""]",['1999-08-17'] +989,['eng'],"['Matos, T', 'Guzmán, F', 'Urena-Lopez, L A']",['Scalar Field as Dark Matter in the Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'field theory, scalar', 'astrophysics, missing-mass', 'supernova', 'cosmic radiation, background', 'mass spectrum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908152'],"['In this letter we investigate the hypothesis that the scalar field is the dark matter and the dark energy in the Cosmos, wich composes about 95% of the matter of the Universe. We show that this hypothesis explains quite well the recent observations on type Ia supernovae. Our results agree with the restrictions impossed by the Cosmic Background Radiation and by the mass power spectrum.']",['1999-08-16'] +990,['eng'],"['Jonauskas, V']",['On the possibility of variation of the fundamental constants of physics in the static universe'],['Astrophysics and Astronomy'],"['space-time, static', 'fundamental constant, fine structure', 'photon, velocity', 'atom, energy levels', 'matter, expansion', 'mass', 'gravitation, fundamental constant', 'fundamental constant, time variation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908082'],"[""A variation of fundamental constants of physics is proposed in a frame of static universe. It is shown when the velocity of light increases (decreases) the Planck's constant increases (decreases) and mass of bodies decreases (increases). This variation of constants leads to the variation of dimensions of bodies and the energy levels of atoms, but a fine structure constant remains unaltered.""]",['1999-08-10'] +991,['eng'],"['Garriga, J', 'Vilenkin, A']",['On likely values of the cosmological constant'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'vacuum state', 'energy, density', 'inflationary universe', 'potential', 'field theory, scalar', 'quantum cosmology', 'quintessence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908115'],"[""We discuss models in which the smallness of the effective vacuum energy density $\\rho_\\L$ and the coincidence of the time of its dominance $t_\\L$ with the epoch of galaxy formation $t_G$ are due to anthropic selection effects. In such models, the probability distribution for $\\rho_\\L$ is a product of an {\\it a priori} distribution ${\\cal P}_*(\\rho_\\L)$ and of the number density of galaxies at a given $\\rho_\\L$ (which is proportional to the number of observers who will detect that value of $\\rho_\\L$). To determine ${\\cal P}_*$, we consider inflationary models in which the role of the vacuum energy is played by a slowly-varying potential of some scalar field. We show that the resulting distribution depends on the shape of the potential and generally has a non-trivial dependence on $\\rho_\\L$, even in the narrow anthropically allowed range. This is contrary to Weinberg's earlier conjecture that the {\\it a priori} distribution should be nearly flat in the range of interest. We calculate the (final) probability distributions for $\\rho_\\L$ and for $t_G/t_\\L$ in simple models with power-law potentials. For some of these models, the agreement with the observationally suggested values of $\\rho_\\L$ is better than with a flat {\\it a priori} distribution. We also discuss quantum-cosmological approach in which $\\rho_\\L$ takes different values in different disconnected universes and argue that Weinberg's conjecture is not valid in this case as well. Finally, we extend our analysis to models of quintessence, with similar conclusions.""]",['1999-08-11'] +992,['eng'],"['Shi, X', 'Fuller, G M', 'Abazajian, K N']",['The Increase to the Primordial $^{4}He$ Yield in the Two-Doublet Four-Neutrino Mixing Scheme'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'helium, yield', 'neutrino, oscillation', 'neutrino, cosmic radiation', 'neutrino, solar', 'neutrino, mixing angle', 'neutrino, multiplet', 'doublet, 2', 'neutrino, beam', 'neutrino, mass difference', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908081'],"[""One current scheme to accommodate simultaneously the Super Kamiokande atmospheric neutrino data, the solar neutrino data and the data from the Los Alamos Scintillation Neutrino Detector (LSND) involves two-doublet neutrino mixing. The upper (heavier) doublet exhibits (near) maximal $\\mutau$ mixing and explains the atmospheric neutrino data, while the $\\es$ mixing (with $\\nu_s$ being a sterile neutrino) of the lower (lighter) doublet accounts for the solar neutrino deficit. The inter-doublet mixing between $\\nu_\\mu$ and $\\nu_e$ can provide an explanation for the LSND results. The inter-doublet mixing between changing the spectrum of $\\nu_e$/$\\bar\\nu_e$ and populating the sterile neutrino sea. Both effects {\\sl increase} the primorial $^4$He yield $Y$. We show that in the two-doublet neutrino scheme $\\Delta Y/Y$ can reach the few percent level, which is in the range subject to observational constraint. The inter-doublet mixing allowed by the constraint from the observationally-inferred $Y$ value is drastically different for the two possible channels for solving the solar neutrino deficit: a matter-enhanced (Mikheyev-Smirnov-Wolfenstein effect) $\\es$ transformation; or a `just-so' vacuum $\\es$ oscillation. If we assume that $\\nu_e$ and $\\nu_s$ mix with the favor a vacuum solution to the solar neutrino problem and effective parameters for LSND of $m^2_{\\nu_\\mu}-m^2_{\\nu_e} \\approx 1$ eV$^2$ and""]",['1999-08-10'] +993,['eng'],"['Albrecht, Andreas', 'Skordis, C']",['Phenomenology of a realistic accelerating universe using only Planck-scale physics'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'field theory, scalar', 'quintessence', 'energy, density', 'matter, density', 'potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908085'],"[""Modern data is showing increasing evidence that the Universe is accelerating. So far, no theoretical account of the acceleration has been satisfactory, particularly because of the need to greatly ``fine tune'' theoretical parameters. We show how a class of scalar field models (which may emerge naturally from superstring theory) can account for acceleration which starts in the present epoch with all the potential parameters O(1) in Planck units.""]",['1999-08-10'] +994,['eng'],"['Horváth, J E']",['Strange stars in low-mass binary pulsar systems'],['Astrophysics and Astronomy'],"['pulsar, binary', 'mass, low', 'matter, strangeness', 'magnetic field, time variation', 'temperature, surface', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908054'],"['Based on observational facts and a variety of theoretical arguments we discuss in this work the possibility that pulsars in Low-Mass Binary Pulsar systems could be strange stars rather than neutron stars. It is shown that, although subject to reasonable uncertainties, the consideration of the physics of the SQM core and thin normal crusts leads to the prediction of several observed features of the magnetic field history of these systems whitin this working hypothesis.']",['1999-08-09'] +995,['eng'],"['Lewin, A', 'Albrecht, Andreas']",['Can inflationary models of cosmic perturbations evade the secondary oscillation test?'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'cosmic radiation, background', 'cosmic radiation, spectra', 'temperature, anisotropy', 'cosmic radiation, polarization', 'spectra, oscillation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908061'],"['We consider the consequences of an observed Cosmic Microwave Background (CMB) temperature anisotropy spectrum containing no secondary oscillations. While such a spectrum is generally considered to be a robust signature of active structure formation, we show that such a spectrum {\\em can} be produced by (very unusual) inflationary models or other passive evolution models. However, we show that for all these passive models the characteristic oscillations would show up in other observable spectra. Our work shows that when CMB polarization and matter power spectra are taken into account secondary oscillations are indeed a signature of even these very exotic passive models. We construct a measure of the observability of secondary oscillations in a given experiment, and show that even with foregrounds both the MAP and \\pk satellites should be able to distinguish between models with and without oscillations. Thus we conclude that inflationary and other passive models can {\\em not} evade the secondary oscillation test.']",['1999-08-09'] +996,['eng'],"['Salmonson, J D', 'Wilson, J R']",['General Relativistic Augmentation of Neutrino Pair Annihilation Energy Deposition Near Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'neutrino antineutrino, annihilation', 'electron, pair production', 'relativity theory, general', 'supernova', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908017'],['General relativistic calculations are made of neutrino-antineutrino annihilation into electron-positron pairs near the surface of a neutron star. It is found that the efficiency of this process is enhanced over the Newtonian values up to a factor of more than 4 in the regime applicable to Type II supernovae and by up to a factor of 30 for collapsing neutron stars.'],['1999-08-04'] +997,['eng'],"['Amendola, L']",['Coupled Quintessence'],['Astrophysics and Astronomy'],"['astrophysics, acceleration', 'field theory, scalar', 'quintessence', 'potential', 'coupling, linear', 'density, perturbation', 'cosmic radiation, background', 'galaxy', 'coupling constant', 'phase space, attractor', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908023'],"[""A new component of the cosmic medium, a light scalar field or ''quintessence '', has been proposed recently to explain cosmic acceleration with a dynamical cosmological constant. Such a field is expected to be coupled explicitely to ordinary matter, unless some unknown symmetry prevents it. I investigate the cosmological consequences of such a coupled quintessence (CQ) model, assuming an exponential potential and a linear coupling. This model is conformally equivalent to Brans-Dicke Lagrangians with power-law potential. I evaluate the density perturbations on the cosmic microwave background and on the galaxy distribution at the present and derive bounds on the coupling constant from the comparison with observational data. A novel feature of CQ is that during the matter dominated era the scalar field has a finite and almost constant energy density. This epoch, denoted as quintessence: the multipole spectrum of the microwave background is tilted at large angles, the acoustic peaks are shifted, their amplitude is changed, and the present 8Mpc$/h$ density variance is diminished. The present data constrain the dimensionless coupling constant to $|\\beta |\\leq 0.1$.""]",['1999-08-04'] +998,['eng'],"['Battye, R A', 'Bucher, M', 'Spergel, D N']",['Domain Wall Dominated Universes'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'domain wall, network', 'matter, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'quintessence', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908047'],"['We consider a cosmogony with a dark matter component consisting of a network of frustrated domain walls. Such a network provides a solid dark matter component with $p=-(2/3)\\rho $ that remains unclustered on small scales and with $\\Omega_{\\rm dw}\\approx 0.7$ can reconcile a spatially flat universe with the many observations indicating $\\Omega_{\\rm m}\\approx 0.3.$ Because of its large negative pressure, this component can explain the recent observations indicating an accelerating universe without recourse to a non-vanishing cosmological constant. We explore the viability of this proposal and prospects for distinguishing it from other kinds of proposed dark matter with significant negative pressure.']",['1999-08-06'] +999,['eng'],"['Rachen, J P', 'Protheroe, R J', 'Mannheim, K']",['The relation of extragalactic cosmic ray and neutrino fluxes'],['Astrophysics and Astronomy'],"['talk, Paris 1998/12/14', 'cosmic radiation', 'neutrino, flux', 'upper limit', 'photon, cosmic radiation', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9908031'],"['In a recent paper, Waxman and Bahcall (PRD 59, 023002) claimed that the present data on ultra-high energy cosmic rays imply a model-independent upper bound on extragalactic neutrino fluxes of 2*10^-8 GeV cm^-2 s^-1 ster^-1, independent of neutrino energy. Mannheim, Protheroe and Rachen (astro-ph/9812398) have repeated this calculation and confirmed the WB-bound, within a factor of 2, only at a very limited energy range of E_\\nu \\sim 10^(16-18) eV, while at other energies the neutrino flux is mainly limited by the extragalactic gamma ray background to a level about two orders of magnitude higher than the WB bound. In this paper we present a simple, (almost) no-math approach to the problem, and discuss under which astrophysical assumptions the WB-bound and the MPR-bound, respectively, apply. Then we discuss to which respect these assumptions apply to presently discussed models of extragalactic neutrino production. We note that, averaged over the observed luminosity function, blazars are sufficiently opaque to ultra-high energy neutrons that there is no conflict of the predicted neutrino fluxes with the cosmic ray data, and that these models are rather constrained by their contributions to the extragalactic gamma ray background. At present, no modifications are implied to the predicted neutrino events from these models in active or planned neutrino detectors.']",['1999-08-05'] +1000,['eng'],"['Wang, L', 'Kamionkowski, M P']",['The Cosmic Microwave Background Bispectrum and Inflation'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'inflationary universe', 'correlation function', 'potential']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907431'],"['We derive an expression for the non-Gaussian cosmic-microwave-background (CMB) statistic $I_l^3$ defined recently by Ferreira, Magueijo, and Górski in terms of the slow-roll-inflation parameters $\\epsilon$ and $\\eta$. This result shows that a nonzero value of $I_l^3$ in COBE would rule out single-field slow-roll inflation. A sharp change in the slope of the inflaton potential could increase the predicted value of $I_l^3$, but not significantly. This further suggests that it will be difficult to account for such a detection in multiple-field models in which density perturbations are produced by quantum fluctuations in the scalar field driving inflation. An Appendix shows how to evaluate an integral that is needed in our calculation as well as in more general calculations of CMB bispectra.']",['1999-08-02'] +1001,['eng'],"['Altmann, M', 'Hillebrandt, W', 'Janka, H T', 'Raffelt, G G']",[],['Astrophysics and Astronomy'],"['conference, Ringberg Castle/Tegernsee 1997/10/20', 'neutrino, astrophysics', 'neutrino, solar', 'supernova', 'photon, cosmic radiation', 'astrophysics, model']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801320'],"['Collection of ""Extended Abstracts"" of talks presented at the SFB-375 workshop NEUTRINO ASTROPHYSICS, Ringberg Castle, Tegernsee, Germany, 20-24 Oct. 1997. Topics include Solar Neutrinos, Supernovae, Gamma-Ray Bursts, High-Energy Neutrinos (atmospheric, astrophysical), Cosmology, and Future Prospects. The focus is on astrophysical and experimental/observational aspects of astrophysical neutrinos while particle theory and neutrino laboratory experiments are not covered.']",['1998-02-16'] +1002,['eng'],"['Protheroe, R J']",['Developments in High Energy Neutrino Astronomy'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, measurement', 'muon, velocity', 'deep underground detector, AMANDA', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907374'],"['Nature produces cosmic ray particles, probably protons, with energies well above $10^{20}$ eV -- how are they produced? Where do they come from? Gamma rays with energies above $10^{13}$ eV are produced in jets of active galaxies -- are these produced by energetic electrons or protons? What is the correct model of Gamma Ray Bursts? These are just some of the fundamental questions in high energy astrophysics to be answered by observations made with large area neutrino telescopes.']",['1999-07-28'] +1003,['eng'],"['Kim, H I']",['Primordial black holes under the double inflationary power spectrum'],['Astrophysics and Astronomy'],"['black hole, production', 'mass, scaling', 'inflationary universe', 'density, fluctuation', 'spectra, perturbation', 'black hole, mass spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907372'],"['Recently, it has been shown that the primordial black holes (PBHs) from the near critical collapse in the expanding universe have a scaling mass relation similar to that of black holes produced in the asymptotically flat spacetime. Distinct from the PBHs with mass about the horizon mass (Type I), the PBHs with the scaling relation (Type II) can be formed with a range of masses at a given time. In general, only the case in which the PBH formation is concentrated at only one epoch has been considered. However, it is expected that the PBH formation epoch is possible in a broad range of period if the density fluctuation has rather large amplitude and smooth scale dependence. So, we study the PBH formation for both types assuming the power spectrum of double inflationary models such that the small scale fluctuations could have large amplitudes independent of the CMBR anisotropy. The mass spectrum of Type II PBHs is newly constructed without limiting the PBH formation period. Under the double inflationary power spectrum, the accumulation of PBHs formed at later times is important and the mass range is significantly broadened. It seems difficult for the PBHs under the assumed power spectrum to generate the observed MACHO spectrum.']",['1999-07-28'] +1004,['eng'],"['Barrau, A']",['Primordial black holes as a source of extremely high energy cosmic rays'],['Astrophysics and Astronomy'],"['black hole', 'cosmic radiation, particle source', 'quark gluon, hadronization', 'cosmic radiation, flux', 'dependence, density', 'hadron, multiplicity', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907347'],['The origin of observed extremely high energy cosmic rays remains an astrophysical enigma. We show that a single evaporating primordial black hole should produce 8.5*10^14 particles over a 10^20 eV threshold. This emission results from direct production of fundamental constituants and from hadronization of quarks and gluons. The induced flux on the Earth is studied as a function of the local density of exploding black holes and compared with experimental data. The discovery potential of future detectors is finally reviewed.'],['1999-07-27'] +1005,['eng'],"['Ellis, Jonathan Richard', 'Farakos, K', 'Mavromatos, Nikolaos E', 'Mitsou, V A', 'Nanopoulos, Dimitri V']",['Astrophysical Probes of the Constancy of the Velocity of Light'],['Astrophysics and Astronomy'],"['photon, velocity', 'photon, cosmic radiation', 'galaxy, AGN', 'pulsar', 'space-time, foam', 'model, fluctuation', 'velocity, energy dependence', 'radiation, electromagnetic', 'recoil, effect', 'quantum gravity', 'data analysis method', 'astrophysics, model', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907340'],"['We discuss possible tests of the constancy of the velocity of light using distant astrophysical sources such as gamma-ray bursters (GRBs), Active Galactic Nuclei (AGNs) and pulsars. This speculative quest may be motivated by some models of quantum fluctuations in the space-time background, and we discuss explicitly how an energy-dependent variation in photon velocity \\delta c/ c \\sim - E / M arises in one particular quantum-gravitational model. We then discuss how data on GRBs may be used to set limits on variations in the velocity of light, which we illustrate using BATSE and OSSE observations of the GRBs that have recently been identified optically and for which precise redshifts are available. We show how a regression analysis can be performed to look for an energy-dependent effect that should correlate with redshift. The present data yield a limit M \\gsim 10^{15} GeV for the quantum gravity scale. We discuss the prospects for improving this analysis using future data, and how one might hope to distinguish any positive signal from astrophysical effects associated with the sources.']",['1999-07-27'] +1006,['eng'],"['Narayan, R']",['Hydrodynamic Drag on a Compact Star Orbiting a Supermassive Black Hole'],['Astrophysics and Astronomy'],"['black hole, massive', 'galaxy, AGN', 'accretion', 'n, matter', 'gravitational radiation, emission', 'matter, orbit', 'model, hydrodynamical', 'relativity theory, general', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907328'],['The proposed Laser Interferometer Space Antenna is expected to detect gravitational waves from neutron stars and stellar-mass black holes spiraling into supermassive black holes in distant galactic nuclei. Analysis of the inspiral events will require careful comparison of the observed signals with theoretical waveform templates. The comparison could be seriously compromised if non-gravitational torques modify the orbit of the star. This paper estimates the torque exerted on an orbiting star as a result of hydrodynamic interactions with an accretion flow around the supermassive black hole. It is argued that the majority of inspiral events will take place in low luminosity galactic nuclei in which the mass accretion rate is low and the accretion occurs via an advection-dominated flow. The hydrodynamic torque is negligibly small in such systems and will have no effect on gravitational wave experiments.'],['1999-07-26'] +1007,['eng'],"['Munyaneza, F', 'Viollier, R D']",['Emission spectrum of Sagittarius $A^{*}$ and the neutrino ball scenario'],['Astrophysics and Astronomy'],"['black hole, massive', 'spectra, emission', 'neutrino, matter', 'neutrino, mass', 'accretion', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907318'],['The emission spectrum of the supermassive compact dark object at the Galactic center is calculated in the framework of standard thin accretion disk theory assuming that the compact object is a neutrino ball of $2.6 \\times 10^{6}M_{\\odot}$ instead of a supermassive black hole. The neutrino ball scenario could explain the observed radio and infrared emission spectrum of the Galactic center for wavelengths between $\\lambda=0.3 {\\rm cm}$ and some constraints.'],['1999-07-26'] +1008,['eng'],"['Amram, P', 'Anvar, S', 'Aslanides, Elie', 'Aubert, Jean-Jacques', 'Azoulay, R', 'Basa, S', 'Benhammou, Ya', 'Bernard, F', 'Bertin, V', 'Billault, M', 'Blanc, P E', 'Blanc, F', 'Bland, R', 'Blondeau, F', 'Bottu, N', 'Boulesteix, J', 'Brooks, B', 'Brunner, J', 'Calzas, A', 'Cârloganu, C', 'Carmona, F E', 'Carr, J', 'Carton, P H', 'Cartwright, S L', 'Cases, R', 'Cassol, F', 'Compere, C', 'Cooper, S', 'Coustillier, G', 'De Botton, N R', 'Deck, P', 'Desages, F E', 'Destelle, J J', 'Dispau, G', 'Drogou, J F', 'Drouhin, F', 'Duval, P Y', 'Feinstein, F', 'Festy, D', 'Fopma, J', 'Fuda, J L', 'Goret, P', 'Gosset, L G', 'Gournay, J F', 'Hernández, J J', 'Herrouin, G', 'Hubaut, F', 'Hubbard, J R', 'Huss, D', 'Jaquet, M', 'Jelley, N A', 'Kajfasz, E', 'Karolak, M', 'Kouchner, A', 'Kudryavtsev, V A', 'Lachartre, D', 'Lafoux, H', 'Lamare, P', 'Languillat, J C', 'Laugier, D', 'Laugier, J P', 'Le Guen, Y', 'Le Provost, H', 'Le Van Suu, A', 'Lemoine, L', 'Liotard, P L', 'Loucatos, S', 'Magnier, P', 'Marcelin, M', 'Martin, L', 'Massol, A', 'Mazeau, B', 'Mazure, A', 'Mazéas, F', 'McMillan, J', 'Millot, C', 'Mols, P', 'Montanet, F', 'Morel, J P', 'Moscoso, L', 'Navas, S', 'Olivetto, C', 'Palanque-Delabrouille, N', 'Pallarès, A', 'Payre, P', 'Perrin, P', 'Pohl, A', 'Poinsignon, J', 'Potheau, R', 'Queinec, Y', 'Racca, C', 'Raymond, M', 'Rolin, J F', 'Sacquin, Yu', 'Schuller, J P', 'Schuster, W', 'Spooner, N', 'Stolarczyk, T', 'Tabary, A', 'Talby, M', 'Tao, Charling', 'Tayalati, Y', 'Thompson, L F', 'Triay, R', 'Tzvetanov, T', 'Valdy, P', 'Vernin, P', 'Vigeolas, E', 'Vignaud, D', 'Vilanova, D', 'Wark, D', 'Zghiche, A', 'Zúñiga, J']",['Background light in potential sites for the ANTARES undersea neutrino telescope'],['Detectors and Experimental Techniques'],"['neutrino, cosmic radiation', 'Cherenkov counter, water', 'photon, background', 'potassium, radiative decay', 'photoelectron, amplifier', 'deep underground detector, ANTARES']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9910170'],"['The ANTARES collaboration has performed a series of {\\em in situ} measurements to study the background light for a planned undersea neutrino telescope. Such background can be caused by $^{40}$K decays or by biological activity. We report on measurements at two sites in the Mediterranean Sea at depths of 2400~m and 2700~m, respectively. Three photomultiplier tubes were used to measure single counting rates and coincidence rates for pairs of tubes at various distances. The background rate is seen to consist of three components: a constant rate due to $^{40}$K decays, a continuum rate that varies on a time scale of several hours simultaneously over distances up to at least 40~m, and random bursts a few seconds long that are only correlated in time over distances of the order of a meter. A trigger requiring coincidences between nearby photomultiplier tubes should reduce the trigger rate for a neutrino telescope to a manageable level with only a small loss in efficiency.']",['1999-10-11'] +1009,['eng'],"['Peterson, J B', 'Carlstrom, J E', 'Cheng, E S', 'Kamionkowski, M P', 'Lange, A E', 'Seiffert, M', 'Spergel, D N', 'Stebbins, A J']",['Cosmic Microwave Background Observations in the Post-Planck Era'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'cosmic radiation, polarization', 'temperature', 'gravitational radiation', 'inflationary universe', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907276'],"['The Microwave Anisotropy Probe and Planck missions will provide low noise maps of the temperature of the cosmic microwave background (CMB). These maps will allow measurement of the power spectrum of the CMB with measurement noise below cosmic variance for l < 1500. It is anticipated that no further all sky CMB temperature observations will be needed after Planck. There are, however, other CMB measurements for which Planck will be not the end but the beginning. Following Planck, precise CMB polarization observations will offer the potential to study physical processes at energies as high as 10^19 GeV. In addition, arcminute scale, multi-frequency observations will allow study of the early phases of the formation of large-scale structure in the universe.']",['1999-07-21'] +1010,['eng'],"['Bradbury, S M', 'Bond, I H', 'Breslin, A C', 'Buckley, J H', 'Carter-Lewis, D A', 'Catanese, M', 'Criswell, S', 'Dingus, B L', 'Fegan, D J', 'Finley, J P', 'Gaidos, J', 'Grindlay, J', 'Hillas, A M', 'Harris, K', 'Hermann, G', 'Kaaret, P E', 'Kieda, D B', 'Knapp, J', 'Krennrich, F', 'Le Bohec, S', 'Lessard, R W', 'Lloyd-Evans, J', 'McKernan, B', 'Müller, D', 'Ong, R', 'Quenby, J J', 'Quinn, J', 'Rochester, G D', 'Rose, H J', 'Salamon, M B', 'Sembroski, G H', 'Sumner, T J', 'Swordy, S', 'Vasilev, V', 'Weekes, T C']",['The Very Energetic Radiation Imaging Telescope Array System (VERITAS)'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'photoelectron, amplifier']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907248', 'http://krusty.physics.utah.edu/~icrc1999/root/vol5/o4_3_28.pdf']","[""We give an overview of the current status and scientific goals of VERITAS, a proposed hexagonal array of seven 10 m aperture imaging Cherenkov telescopes. The selected site is Montosa Canyon (1390 m a.s.l.) at the Whipple Observatory, Arizona. Each telescope, of 12 m focal length, will initially be equipped with a 499 element photomultiplier camera covering a 3.5 degree field of view. A central station will initiate the readout of 500 MHz FADCs upon receipt of multiple telescope triggers. The minimum detectable flux sensitivity will be 0.5% of the Crab Nebula flux at 200 GeV. Detailed simulations of the array's performance are presented elsewhere at this meeting. VERITAS will operate primarily as a gamma-ray observatory in the 50 GeV to 50 TeV range for the study of active galaxies, supernova remnants, pulsars and gamma-ray bursts.""]",['1999-07-20'] +1011,['eng'],"['Gourgoulhon, E', 'Haensel, P', 'Livine, E R', 'Paluch, E', 'Bonazzola, S', 'Marck, J A']",['Fast rotation of strange stars'],['Astrophysics and Astronomy'],"['matter, strangeness', 'matter, rotational', 'quark, matter', 'relativity theory, general', 'bag model', 'baryon, mass', 'susceptibility', 'scaling', 'matter, stability', 'matter, density', 'n, matter', 'pulsar', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907225'],"['Exact models of uniformly rotating strange stars, built of self bound quark matter, are calculated within the framework of general relativity. This is made possible thanks to a new numerical technique capable to handle the strong density discontinuity at the surface of these stars. Numerical calculations are done for a simple MIT bag model equation of state of strange quark matter. Evolutionary sequences of models of rotating strange stars at constant baryon mass are calculated. Maximally rotating configurations of strange stars are determined, assuming that the rotation frequency is limited by the mass shedding and the secular instability with respect to axisymmetric perturbations. Exact formulae which give the dependence of the maximum rotation frequency, and of the maximum mass and corresponding radius of rotating configurations, on the value of the bag constant, are obtained. The values of T/W for rapidly rotating massive strange stars are significantly higher than those for ordinary neutron stars. This might indicate particular susceptibility of rapidly rotating strange stars to triaxial instabilities.']",['1999-07-19'] +1012,['eng'],"['Green, A M', 'Lidsey, J E']",['Assisted dynamics of multi-scalar field cosmologies'],['Astrophysics and Astronomy'],"['astrophysics', 'field theory, scalar', 'potential', 'field equations, solution', 'attractor', 'field theory, action', 'field theory, massless', 'higher-dimensional', 'spontaneous compactification']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907223'],"['We examine the dynamics of an arbitrary number of scalar fields interacting via a series of exponential potentials. In many cases, redefining the fields reduces the system to a single field with a single exponential potential, independent of the background spacetime. We show that this solution is the late--time attractor for an arbitrary number of scalar fields interacting via two exponential potentials. We apply this analysis to a reduced action resulting from a generalized compactification of higher--dimensional fields.']",['1999-07-19'] +1013,['eng'],"['Amendola, L', 'Corasaniti, S', 'Occhionero, F']",['Time variability of the gravitational constant and Type Ia supernovae'],['Astrophysics and Astronomy'],"['gravitation, fundamental constant', 'fundamental constant, time variation', 'supernova', 'astrophysics, fundamental constant', 'matter, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907222'],"['We investigate to which extent a time variation of the gravitational constant or other fundamental constants affects the best fit of the Hubble diagram of type Ia supernovae. In particular, we show that a slow increase of $G$ in the past, below experimental constraints, can reconcile the SNe Ia observations with an open zero-$\\Lambda$ universe.']",['1999-07-19'] +1014,['eng'],"['Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G', 'Delay, R S', 'Dingus, B L', 'Dorfan, D E', 'Ellsworth, R W', 'Evans, D', 'Falcone, A D', 'Fleysher, L', 'Fleysher, R', 'Gisler, G', 'Goodman, J A', 'Haines, T J', 'Hoffman, C M', 'Hugenberger, S', 'Kelley, L A', 'Leonor, I', 'Macri, J R', 'McConnell, M', 'McCullough, J F', 'McEnery, J E', 'Miller, R S', 'Mincer, A I', 'Morales, M F', 'Némethy, P', 'Ryan, J M', 'Schneider, M', 'Shen, B', 'Shoup, A L', 'Sinnis, G', 'Smith, A J', 'Sullivan, G W', 'Thompson, T N', 'Tumer, O T', 'Wang, K', 'Wascko, M O', 'Westerhoff, S', 'Williams, D A', 'Yang, T', 'Yodh, G B']",['Instrumented Water Tanks can Improve Air Shower Detector Sensitivity'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'showers, air', 'Cherenkov counter, water', 'angular resolution', 'spatial resolution', 'photoelectron, amplifier', 'trigger']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=990721', 'http://krusty.physics.utah.edu/~icrc1999/root/vol5/o4_4_06.pdf']","[""Previous works have shown that water Cherenkov detectors have superior sensitivity to those of scintillation counters as applied to detecting extensive air showers (EAS). This is in large part due to their much higher sensitivity to EAS photons which are more than five times more numerous than EAS electrons. Large area water Cherenkov detectors can be constructed relatively cheaply and operated reliably. A sparse detector array has been designed which uses these types of detectors to substantially increase the area over which the Milagro Gamma Ray Observatory collects EAS information. Improvements to the Milagro detector's performance characteristics and sensitivity derived from this array and preliminary results from a prototype array currently installed near the Milagro detector will be presented.""]",['1999-07-16'] +1015,['eng'],"['Gratton, S', 'Hertog, T', 'Turok, Neil G']",['An Observational Test of Quantum Cosmology'],['Astrophysics and Astronomy'],"['quantum cosmology, validity test', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, tensor', 'instanton, symmetry breaking', 'singularity', 'inflationary universe, open', 'amplitude analysis', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907212'],"[""We compute the tensor CMB anisotropy power spectrum for singular and non-singular instantons describing the beginning of the universe according to the no boundary proposal. For the non-singular instantons we use gently sloping potentials with a sharp negative false vacuum added. The surfaces of constant density break the O(4,1) symmetry of perfect de Sitter space. In the nonsingular instantons this breaking is small, but in singular instantons the singularity makes the breaking much stronger. The effect of the singularity is to suppress long wavelength tensor fluctuations usually called bubble wall fluctuation modes. This alleviates the problem of the large low $l$ $C_l$'s which plagues open inflation theories. Thus singular instantons are observationally favoured over non-singular Coleman De Luccia instantons arising from an equivalent potential but with a sharp false vacuum superposed.""]",['1999-07-16'] +1016,['eng'],"['Battiston, R']",['Search for Antimatter in Space with the Alpha Magnetic Spectrometer'],['Astrophysics and Astronomy'],"['talk, La Thuile 1999/02/28', 'antimatter, search for', 'helium, antinucleus', 'yield, (antinucleus nucleus)', 'upper limit', 'magnetic spectrometer, satellite', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907152'],"['The Alpha Magnetic Spectrometer (AMS) is a state of the art particle physics experiment for the extraterrestrial study of antimatter, matter and missing matter. AMS successfully completed the precursor STS91 Discovery flight (June 2nd-12th, 1998), completing 152 orbits at 52 degrees of latitude and about 400 km of height, collecting more than 100 million CR events. In this paper we report on the first flight experience and we present preliminary results on the search for nuclear antimatter. No antimatter nuclei with Z>=2 were detected. We obtain a model dependent upper limit on the anti-He /He flux <1.14 10^^-6 In the rigidity region between 1.6 to 20 GV we obtain a model independent, conservative upper limit on anti-He /He flux <1.7 10^^-6 and <2.8 10^^-5 for Z>2, improving the results of previous published searches performed with stratospheric balloons.']",['1999-07-13'] +1017,['eng'],"['Bludman, Sidney A']",['Vacuum Energy'],['Astrophysics and Astronomy'],"['review', 'astrophysics, fundamental constant', 'vacuum state, energy', 'matter, density', 'radiation, density', 'matter, cluster', 'expansion, acceleration', 'inflationary universe', 'quintessence', 'field theory, scalar', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907168'],"['We review the cosmological evidence for a low matter density universe and a cosmological constant or dynamical vacuum energy and address the cosmolog$ coincidence problem: why is the matter density about one-half the vacuum energy and of Martel, Schapiro & Weinberg.']",['1999-07-14'] +1018,['eng'],"['Volkas, R R', 'Wong, Y Y Y']",['Matter-affected neutrino oscillations in ordinary and mirror stars and their implications for $\\gamma$-ray bursts'],['Astrophysics and Astronomy'],"['astrophysics, model', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'neutrino antineutrino, annihilation', 'neutrino, oscillation', 'matter, effect', 'binding energy, gravitation', 'baryon', 'neutrino, sterile', 'neutrino, mixing angle', 'neutrino, flavor', 'bibliography', 'neutrino antineutrino --> positron electron', 'neutrino antineutrino --> 2photon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907161'],"['It has been proposed that the annihilation process $\\nu\\bar{\\nu} \\to e^{-}e^{+} \\to \\gamma\\gamma$ may be responsible for the generation of gamma-ray bursts (GRBs). The incipient neutrino--antineutrino pairs carry virtually all of the gravitational binding energy available from the central engine. However, gamma-ray bursters proposed to date are inevitably surrounded by an excess of baryons, leading to the ""baryon-loading problem"". In the light of growing evidence for neutrino oscillations, we discuss the implications of matter-affected oscillations for GRB energetics, and on the viability of ""mirror"" stars as GRB progenitors.']",['1999-07-14'] +1019,['eng'],"['Samurovic, S', 'Cirkovic, M M']",['Massive Neutrino Decay and Shape of the Galactic Dark Halo'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutrino, massive', 'neutrino, radiative decay', 'neutrino, lifetime', 'galaxy', 'electron, density', 'particle source, ionization', 'numerical calculations, interpretation of experiments', 'neutrino --> neutrino photon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907142'],"['In this Letter we investigate the basic assumptions of the decaying dark matter (DDM) theory in the light of recent advances in observational and theoretical cosmology and physics, i.e. detection of massive astrophysical compact halo objects (MACHOs) and Super-Kamiokande results. Specifically, the consequences pertaining to the shape of the Milky Way galaxy dark halo are discussed. We find that, by taking into account the values of the main constituent of the mass in DDM theory, massive neutrino, with the mass of 30 eV, and lifetime $\\sim 10^{23}$ s, the initially proposed value of extreme halo flattening $q\\sim 0.2$ is no longer necessary, and that one can easily accommodate a much larger value of $q\\sim 0.6$, that is in accord with all available observational data.']",['1999-07-13'] +1020,['eng'],"['Sicka, C', 'Buchert, T', 'Kerscher, M']",['Backreaction in Cosmological Models'],['Astrophysics and Astronomy'],"['talk, Ringberg Castle 1999/05/30', 'astrophysics, model', 'back reaction', 'astrophysics, fundamental constant', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907137'],"[""Most cosmological models studied today are based on the assumption of homogeneity and isotropy. Observationally one can find evidence that supports these assumptions on very large scales, the strongest being the almost isotropy of the Cosmic Microwave Background radiation after assigning the whole dipole to our proper motion relative to this background. However, on small and on intermediate scales up to several hundreds of Mpcs, there are strong deviations from homogeneity and isotropy. Here the problem arises how to relate the observations with the homogeneous and isotropic models. The usual proposal for solving this problem is to assume that Friedmann-Lemaitre models describe the mean observables. Such mean values may be identified with spatial averages. For Newtonian fluid dynamics the averaging procedure has been discussed in detail in Buchert and Ehlers (1997), leading to an additional backreaction term in the Friedmann equation. We use the Eulerian linear approximation and the `Zel'dovich approximation' to estimate the effect of the backreaction term on the expansion. Our results indicate that even for domains matching the background density in the mean, the evolution of the scale factor strongly deviates from the Friedmann solution, critically depending on the velocity field inside.""]",['1999-07-13'] +1021,['eng'],"['Xu, R X', 'Qiao, G J', 'Zhang, B']",['PSR 0943+10'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'n, matter', 'matter, strangeness', 'binding energy', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907132'],"[""Recent work by Rankin & Deshpande strongly suggests that there exist strong `micro-storms' rotating around the magnetic axis of the 1.1s pulsar PSR 0943+10. Such a feature hints that most probably the large-voltage vacuum gap proposed by Ruderman & Sutherland (RS) does exist in the pulsar polar cap. However, there are severe arguments against the formation of the RS-type gap in pulsars, since the binding energies of both the Fe ions and the electrons in a neutron star's surface layer is too small to prevent thermionic ejection of the particles from the surface. Here we propose that PSR 0943+10 (probably also most of the other `drifting' pulsars) might be bare strange stars rather than normal neutron stars, in which the `binding energy' at the surface is merely infinity either for the case of `pulsar' or `anti-pulsar'. It is further proposed that identifying a drifting pulsar as an anti-pulsar is the key criterion to distinguish strange stars from neutron stars.""]",['1999-07-13'] +1022,['eng'],"['Abdurashitov, J N', 'Bowles, T J', 'Cherry, M L', 'Cleveland, B T', 'Davis, R', 'Elliott, S R', 'Gavrin, V N', 'Girin, S V', 'Gorbachev, V V', 'Ibragimova, T V', 'Kalikhov, A V', 'Knodel, T V', 'Lande, K', 'Mirmov, I N', 'Nico, J S', 'Shikhin, A A', 'Teasdale, W A', 'Veretenkin, E P', 'Vermul, V M', 'Wark, D L', 'Wildenhain, P S', 'Yants, V E', 'Zatsepin, G T', 'Khairnasov, N G', 'Wilkerson, J F']",['Measurement of the solar neutrino capture rate by SAGE and implications for neutrino oscillations in vacuum'],['Astrophysics and Astronomy'],"['neutrino nucleus, capture', 'gallium', 'neutrino, solar', 'neutrino, oscillation', 'neutrino, mass difference', 'neutrino, mixing angle', 'deep underground detector, Baksan', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907131'],"['The Russian-American solar neutrino experiment has measured the capture rate of neutrinos on metallic gallium in a radiochemical experiment at the Baksan Neutrino Observatory. Eight years of measurement give the result 67.2 (+7.2,-7.0) (+3.5,-3.0) SNU, where the uncertainties are statistical and systematic, respectively. The restrictions these results impose on vacuum neutrino oscillation parameters are given.']",['1999-07-13'] +1023,['eng'],"['Abdurashitov, J N', 'Garvin, V N', 'Girin, S V', 'Gorbachev, V V', 'Ibragimova, T V', 'Kalikhov, A V', 'Khairnasov, N G', 'Knodel, T V', 'Mirmov, I N', 'Shikhin, A A', 'Veretenkin, E P', 'Vermul, V M', 'Yants, V E', 'Zatsepin, G T', 'Bowles, T J', 'Teasdale, W A', 'Wark, D L', 'Cherry, M L', 'Nico, J S', 'Cleveland, B T', 'Davis, R', 'Lande, K', 'Wildenhain, P S', 'Elliott, S R', 'Wilkerson, J F']",['Measurement of the solar neutrino capture rate with gallium metal'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino nucleus, capture', 'gallium', 'chemistry', 'experimental methods, efficiency', 'neutrino, mass difference', 'neutrino, mixing angle', 'deep underground detector, Baksan', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907113'],"['The solar neutrino capture rate measured by the Russian-American Gallium Experiment (SAGE) on metallic gallium during the period January 1990 through December 1997 is 67.2 (+7.2-7.0) (+3.5-3.0) SNU, where the uncertainties are statistical and systematic, respectively. This represents only about half of the predicted Standard Solar Model rate of 129 SNU. All the experimental procedures, including extraction of germanium from gallium, counting of 71Ge, and data analysis are discussed in detail.']",['1999-07-12'] +1024,['eng'],"['Moiseev, A', 'Ormes, J', 'Arrighi, H', 'Bloom, Elliott D', 'Chaput, C', 'Digel, S W', 'Engovatov, D', 'Norris, J', 'Silvis, J']",['Detection of Galactic Dark Matter by GLAST'],['Astrophysics and Astronomy'],"['talk, Atlanta 1999/03/20', 'astrophysics, missing-mass', 'WIMP', 'photon, cosmic radiation', 'counters and detectors, satellite', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9912139'],"['The mysterious dark matter has been a subject of special interest to high energy physicists, astrophysicists and cosmologists for many years. According to theoretical models, it can make up a significant fraction of the mass of the Universe. One possible form of galactic dark matter, Weakly Interacting Massive Particles (WIMPs), could be detected by their annihilation into monoenergetic gamma-ray line(s). This paper will demonstrate that the Gamma-ray Large Area Space Telescope (GLAST), scheduled for launch in 2005 by NASA, will be capable of searching for these gamma-ray lines in the energy range from 20 GeV to ~500 GeV and will be sufficiently sensitive to test a number of models. The required instrument performance and its capability to reject backgrounds to the required levels are explicitly discussed.']",['1999-12-08'] +1025,['eng'],"['Bourilkov, D']",['Simulation of Multi-muon Events from EAS at Shallow Depths Underground'],['Astrophysics and Astronomy'],"['talk, Sodankylae 1999/04/24', 'cosmic radiation, primary', 'cosmic radiation, hadronic component', 'muon, cosmic radiation', 'showers, air', 'muon, multiplicity', 'programming, Monte Carlo', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907078'],"['The Monte Carlo program ARROW, based on GEANT and using GHEISHA at energies below 30 GeV, is developed for simulation of the hadron and muon components of extensive air showers with primary energy $10^{12}-10^{17}$ eV. Calculations of the characteristics of multi-muon events as observed underground by the LEP detectors are presented and their dependence on the primary cosmic ray composition and some basic assumptions of the hadronic interaction model is discussed.']",['1999-07-07'] +1026,['eng'],"['Brandt, S', 'Anninos, P']",['Radiation recoil from highly distorted black holes'],['Astrophysics and Astronomy'],"['black hole, Schwarzschild', 'gravitational radiation', 'symmetry, axial', 'radiation, energy', 'velocity, recoil', 'parity, perturbation', 'black hole, horizon', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907075'],"['We present results from numerical evolutions of single black holes distorted by axisymmetric, but equatorially asymmetric, gravitational (Brill) waves. Net radiated energies, apparent horizon embeddings, and recoil velocities are shown for a range of Brill wave parameters, including both even and odd parity distortions of Schwarzschild black holes. We find that a wave packet initially concentrated on the black hole throat, a likely model also for highly asymmetric stellar collapse and late stage binary mergers, can generate a maximum recoil velocity of about 150 (23) km/sec for even (odd) parity perturbations, significantly less than that required to eject black holes from galactic cores.']",['1999-07-07'] +1027,['eng'],"['Achterberg, A', 'Gallant, Y A', 'Norman, C A', 'Melrose, D B']",['Intergalactic Propagation of UHE Cosmic Rays'],['Astrophysics and Astronomy'],"['galaxy', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'magnetic field, random', 'energy loss', 'pi, photoproduction', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907060'],"[""We discuss the intergalactic propagation of ultra-high-energy cosmic rays (UHECRs) with energies E \\geq 10^{18.5} eV. We consider the propagation of UHECRs under the influence of the energy-dependent deflection by a weak random magnetic field in the intergalactic medium and energy losses by photo-pion and pair production. We calculate arrival spectra taking full account of the kinematics of photo-pion production and the Poisson statistics of the photo-pion interaction rate. We give estimates for the deflection of UHECRs from the line of sight to the source, time delays with respect to photons from the same source, arrival spectra and source statistics. These estimates are confirmed by numerical simulations of the propagation in energy evolution of UHECRs. These simulations demonstrate that the often-used continuous approximation in the treatment of energy losses due to photo-pion production on the cosmic microwave background (CMWB) cannot be justified for UHECRs. We discuss the implications of these results for the observed flux of particles above the Greisen-Zatsepin-Kuz'min cut-off in two of the scenarios that have been proposed for the production of these particles: continuous production in the large shock waves associated with powerful radio galaxies, or possibly large-scale structure formation, and the impulsive production at relativistic blast waves associated with cosmological gamma-ray bursts.""]",['1999-07-06'] +1028,['eng'],"['Yamada, S']",['Reduction of neutrino - nucleon scattering rate by nucleon - nucleon collisions'],['Astrophysics and Astronomy'],"['supernova', 'nucleon nucleon, interaction', 'neutrino nucleon, interaction', 'nucleon, propagator', 'nucleon, structure function', 'spectral representation', 'width, finite', 'structure function, spin', 'current, axial-vector', 'Bethe-Salpeter equation, solution', 'propagator, renormalization', 'energy dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907045'],"['We studied possible modifications of the neutrino - nucleon scattering rate due to the nucleon - nucleon collisions in the hot dense matter which we find in the supernova core. We show that the finite width of the nucleon spectral function induced by the nucleon collisions leads to broadening of the dynamical spin structure function of the nucleon, resulting in the reduction of the rate of neutrino - nucleon scattering via the axial vector current and making the energy exchange between neutrinos and nucleons easier. The reduction rate is relatively large (about 0.6) even at density of about 10^{13}g/cm^{3} and could have a significant impact on the dynamics of the collapse-driven supernova as well as the cooling of the proto neutron star.']",['1999-07-06'] +1029,['eng'],"['Yamada, S', 'Toki, H']",['Neutrino-nucleon reaction rates in the supernova core in the relativistic random phase approximation'],['Astrophysics and Astronomy'],"['supernova, opacity', 'neutrino nucleon, interaction', 'neutral current', 'charged current', 'random phase approximation, relativistic', 'mean field approximation', 'thermodynamics', 'pi, exchange', 'rho(770), exchange', 'structure function', 'current, vector', 'current, axial-vector', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907044'],"[""In view of the application to supernova simulations, we calculate neutrino reaction rates with nucleons via the neutral and charged currents in the supernova core in the relativistic random phase approximation (RPA) and study their effects on the opacity of the supernova core. The formulation is based on the Lagrangian employed in the calculation of nuclear equation of state (EOS) in the relativistic mean field theory (RMF). The nonlinear meson terms are treated appropriately so that the consistency of the density correlation derived in RPA with the thermodynamic derivative obtained from EOS by RMF is satisfied in the static and long wave length limit. We employ pion and rho meson exchange interactions together with the phenomenological Landau-Migdal parameters for the isospin-dependent nuclear interactions. We find that both the charged and neutral current reaction rates are suppressed from the standard Bruenn's approximate formula considerably in the high density regime. In the low density regime, on the other hand, the vector current contribution to the neutrino-nucleon scattering rate is enhanced in the vicinity of the boundary of the liquid-gas phase transition, while the other contributions are moderately suppressed there also. In the high temperature regime or in the regime where electrons have a large chemical potential, the latter of which is important only for the electron capture process and its inverse process, the recoil of nucleons cannot be neglected and further reduces the reaction rates with respect to the standard approximate formula which discards any energy transfer in the processes. These issues could have a great impact on the neutrino heating mechanism of collapse-driven supernovae.""]",['1999-07-06'] +1030,['eng'],"['Stanev, T']",['Possible $\\tau$ appearance experiment with atmospheric neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, oscillation', 'showers, air', 'energy spectrum', 'neutrino nucleon, interaction', 'neutrino/tau', 'charged current', 'tau, decay', 'tau, lifetime', 'neutral current', 'neutrino, flux', 'proposed experiment', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9907018'],"[""We suggest an experimental measurement that could detect the appearance of the tau neutrinos in muon to tau neutrino oscillations of atmospheric neutrinos by measuring the energy spectra of neutrino induced showers. Tau neutrinos deposit a large fraction of their energy in showers generated in CC interactions and the subsequent tau--lepton decay. The appearance of tau neutrinos will enhance the spectrum of neutrino induced showers in energy ranges corresponding to the neutrino oscillation parameters. A shower rate lower than the `no oscillation' prediction is an indication for oscillations into sterile neutrinos.""]",['1999-07-02'] +1031,['eng'],"['Catanese, M', 'Weekes, T C']",['Very High Energy $\\gamma$-Ray Astronomy'],['Astrophysics and Astronomy'],"['review, experimental results', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'astrophysics', 'galaxy, AGN', 'pulsar', 'supernova', 'Cherenkov counter, imaging', 'cosmic radiation, flux', 'cosmic radiation, time variation', 'photon, showers', 'cosmic radiation, background', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906501'],['We present a review of the current status of very high energy gamma-ray astronomy. The development of the atmospheric Cherenkov imaging technique for ground-based gamma-ray astronomy has led to a rapid growth in the number of observatories. The detection of TeV gamma rays from Active Galactic Nuclei was unexpected and is providing new insights into the emission mechanisms in the jets. Next generation telescopes are under construction and will increase dramatically the knowledge available at this extreme end of the cosmic electromagnetic spectrum.'],['1999-07-01'] +1032,['eng'],"['Challinor, A D']",['Microwave background anisotropies from gravitational waves'],['Astrophysics and Astronomy'],"['gravitational radiation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'space-time, Robertson-Walker', 'perturbation theory', 'tensor, Weyl', 'cosmic radiation, multipole', 'cosmic radiation, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906474'],"['We present a 1+3 covariant discussion of the contribution of gravitational waves to the anisotropy of the CMB in an almost-Friedmann-Robertson-Walker universe. Our discussion is based in the 1+3 covariant approach to perturbations in cosmology, which provides a physically transparent and gauge-invariant methodology for CMB physics. Applying this approach to linearised gravitational waves, we derive a closed set of covariant equations describing the evolution of the shear and the Weyl tensor, and the angular multipoles of the CMB intensity, valid for an arbitrary matter description and background spatial curvature. A significant feature of the present approach is that the normal mode expansion of the radiation distribution function, which arises naturally here, preserves the simple quadrupolar nature of the anisotropic part of the Thomson scattering source terms, and provides a direct characterisation of the power in the CMB at a given multipole, as in the recently introduced total angular momentum method. We provide the integral solution of the multipole equations, and analytic solutions for the shear and the Weyl tensor, for models with arbitrary spatial curvature. Numerical results for the CMB power spectrum in open models are also presented.']",['1999-06-30'] +1033,['eng'],"['Bahcall, N A', 'Ostriker, J P', 'Perlmutter, S', 'Steinhardt, Paul Joseph']",['The Cosmic Triangle'],['Astrophysics and Astronomy'],['introductory'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906463'],"['The ""cosmic triangle"" is introduced as a way of representing the past, present, and future status of the universe. Our current location within the cosmic triangle is determined by the answers to three questions: How much matter is in the universe? Is the expansion rate slowing down or speeding up? And, is the universe flat? A review of recent observations suggests a universe that is lightweight (matter density about one-third the critical value), is accelerating, and is flat. The acceleration implies the existence of cosmic dark energy that overcomes the gravitational self-attraction of matter and causes the expansion to speed up.']",['1999-06-30'] +1034,['eng'],"['Fargion, D', 'Melé, B']",['Ultrahigh energy neutrinos scattering off relic light neutrinos to explain UHECR above GZK cut off and thin blazars'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'neutrino, cosmic radiation', 'neutrino, cluster', 'galaxy, AGN', 'cosmic radiation, particle source', 'neutrino antineutrino, interaction', 'neutrino/mu', 'neutrino/tau', 'W, pair production', 'Z0, pair production', 'cross section, energy dependence', 'numerical calculations']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906451', 'http://krusty.physics.utah.edu/~icrc1999/root/vol4/o3_2_30.pdf']","[""UHE neutrinos may transfer highest cosmic-rays energies overcoming $2.75K^\\circ$ BBR and radio-waves opacities (the GZK cut off) from most distant AGN sources at the age of the Universe. These UHE $\\nu$ might scatter onto those (light and cosmological) relic neutrinos clustered around our galactic halo or nearby neutrino hot dark halo clustered around the AGN blazar and its jets. The branched chain reactions from a primordial nucleon (via photo production of pions and decay to UHE neutrinos) toward the consequent beam dump scattering on galactic relic neutrinos is at least three order of magnitude more efficient than any known neutrino interactions with Earth atmosphere or direct nucleon propagation. Therefore the rarest cosmic rays (as the 320 EeV event) might be originated at far $(\\tilde{>} 100 Mpc)$ distances (as Seyfert galaxy MCG 8-11-11); its corresponding UHE radiation power is in agreement with the observed one in MeV gamma energies. The final chain products observed on Earth by the Fly's Eye and AGASA detectors might be mainly neutron and anti-neutrons and delayed, protons and anti-protons at symmetric off-axis angles. These hadronic products are most probably secondaries of $W^+ W^-$ or $ZZ$ pair productions and might be consistent with the last AGASA discoveries of doublets and one triplet event.""]",['1999-06-29'] +1035,['eng'],"['Fargion, D', 'Aiello, A', 'Conversano, R']",['Horizontal $\\tau$ air showers from mountains in deep valley'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'neutrino/tau, cosmic radiation', 'neutrino/tau, particle source', 'showers, air', 'showers, angular distribution', 'tau, particle identification', 'muon, background', 'experimental methods, proposed']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906450', 'http://krusty.physics.utah.edu/~icrc1999/root/vol2/h6_1_10.pdf']","['Ultra High Energy (UHE) Tau neutrino may lead to a very peculiar imprint in future underground $Km^3$ detectors in water and ice as well as in air: rarest secondary tau tracks and decay which may exceed the muon ones. Indeed Bremsstrahlung at high energy lead to longer tracks for heavier leptons. Radiation lenght grows nearly with the square of the lepton mass. Indeed electrons are too light and their trace in matter (liquid or rock) is negligible (tens of centimeters); muons are much better observed, while tau are too short life time and too short range to be found. However, because relativistic time expansion, UHE tau traces in matter, above $10^{17} eV$, are relativistically boosted overcoming the corresponding muon tracks, already bounded by bremsstrahlung logarithmic regime. The tau crossing for Kms in water or ice may be confused with common muon tracks; their tau decay may be misunderstood as muonic catastrophic bremsstrahlung interactions. To economize UHE tau discovery, we suggest to look the tau decay in air into the deep valleys mountains, like Canyons or deep in excavation mines where horizontal air showers induce fluorescent or Cerenkov lights. The mountain valley width screens from horizontal secondary muons. The valley height increases the solid angle view. The horizontal air Kms-size gap offer a strong discriminator to filter UHE muons against tau. Tens event a year at PeV (W resonance peak) energies in $Km^3$ excavation gap should be observable . Hunting air shower in the night toward high mountains in Canyons or in a deep excavation may be the best and cheapest way to discover UHE neutrinos, either born by electron anti neutrino scattering on electrons at PeV energies, or by direct tau neutrino possibly relic of muonic flavour oscillation even at EeV energies.']",['1999-06-29'] +1036,['eng'],"['Orito, S', 'Maeno, T', 'Matsunaga, H', 'Abe, K', 'Anraku, K', 'Asaoka, Y', 'Fujikawa, M', 'Imori, M', 'Ishino, M', 'Makida, Y', 'Matsui, N', 'Matsumoto, H', 'Mitchell, J', 'Mitsui, T', 'Moiseev, A', 'Motoki, M', 'Nishimura, J', 'Nozaki, M', 'Ormes, J', 'Saeki, T', 'Sanuki, T', 'Sasaki, M', 'Seo, E S', 'Shikaze, Y', 'Sonoda, T', 'Streitmatter, R', 'Suzuki, J', 'Tanaka, K', 'Ueda, I', 'Yajima, N', 'Yamagami, T', 'Yamamoto, A', 'Yoshida, T', 'Yoshimura, K']",['Precision Measurement of Cosmic-Ray Antiproton Spectrum'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'anti-p, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'anti-p p, ratio', 'magnetic spectrometer, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906426'],"['The energy spectrum of cosmic-ray antiprotons has been measured in the range 0.18 to 3.56 GeV, based on 458 antiprotons collected by BESS in recent solar-minimum period. We have detected for the first time a distinctive peak at 2 GeV of antiprotons originating from cosmic-ray interactions with the interstellar gas. The peak spectrum is reproduced by theoretical calculations, implying that the propagation models are basically correct and that different cosmic-ray species undergo a universal propagation. Future BESS flights toward the solar maximum will help us to study the solar modulation and the propagation in detail and to search for primary antiproton components.']",['1999-06-29'] +1037,['eng'],"['Konopelko, A K', 'Aharonian, F A', 'Hemberger, M', 'Hofmann, W', 'Kettler, J', 'Pühlhofer, G', 'Völk, H J']",['Effectiveness of TeV $\\gamma$-Ray Observations at Large Zenith Angles with a Stereoscopic System of Imaging Atmospheric Cherenkov Telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'cosmic radiation, angular distribution', 'Cherenkov counter, imaging', 'efficiency', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906405'],"['The sensitivity of imaging atmospheric Cherenkov telescopes (IACTs) in TeV gamma-ray observations reachs its maximum at small zenith angles (< 30 degree) which provide the minimum attainable energy threshold of an instrument. However, for a specific telescope site a number of gamma-ray sources, or source candidates, can only be observed at much larger zenith angles (< 60 degree). Moreover the observations at large zenith angles allow to extend the observation time window for any object seen at small zenith angles, as well as to enlarge the dynamic energy range of an instrument towards the highest observable energies of gamma-rays. Based on Monte Carlo simulations we present here the results on the sensitivity of a stereoscopic system of 5 IACTs in observations at large zenith angles. We point out some important parameters of the telescope design which could substantially improve the efficiency of such observations with forthcoming IACT arrays like CANGAROO III, HESS and VERITAS.']",['1999-06-28'] +1038,['eng'],"['Gondolo, P', 'Silk, J']",['Dark matter annihilation at the galactic center'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'galaxy', 'neutralino, annihilation', 'cosmic radiation, production', 'cosmic radiation, particle source', 'luminosity', 'matter, density', 'neutrino, cosmic radiation', 'neutrino, flux', 'black hole', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906391'],"['If cold dark matter is present at the galactic center, as in current models of the dark halo, it is accreted by the central black hole into a dense spike. Particle dark matter then annihilates strongly inside the spike, making it a compact source of photons, electrons, positrons, protons, antiprotons, and neutrinos. The spike luminosity depends on the density profile of the inner halo: halos with finite cores have unnoticeable spikes, while halos with inner cusps may have spikes so bright that the absence of a detected neutrino signal from the galactic center already places interesting upper limits on the density slope of the inner halo. Future neutrino telescopes observing the galactic center could probe the inner structure of the dark halo, or indirectly find the nature of dark matter.']",['1999-06-25'] +1039,['eng'],"['Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G', 'Delay, R S', 'Dingus, B L', 'Dorfan, D E', 'Ellsworth, R W', 'Evans, D', 'Falcone, A D', 'Fleysher, L', 'Fleysher, R', 'Gisler, G', 'Goodman, J A', 'Haines, T J', 'Hoffman, C M', 'Hugenberger, S', 'Kelley, L A', 'Leonor, I', 'Macri, J R', 'McConnell, M', 'McCullough, J F', 'McEnery, J E', 'Miller, R S', 'Mincer, A I', 'Morales, M F', 'Némethy, P', 'Ryan, J M', 'Schneider, M', 'Shen, B', 'Shoup, A L', 'Sinnis, G', 'Smith, A J', 'Sullivan, G W', 'Thompson, T N', 'Tumer, O T', 'Wang, K', 'Wascko, M O', 'Westerhoff, S', 'Williams, D A', 'Yang, T', 'Yodh, G B']",['Study of the Shadows of the Moon and the Sun with VHE Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'cosmic radiation', 'showers, air', 'shadowing, solar', 'shadowing, lunar', 'shower detector, angular resolution', 'numerical calculations, Monte Carlo', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906388', 'http://krusty.physics.utah.edu/~icrc1999/root/vol7/s3_2_39.pdf']","['Milagrito, a prototype for the Milagro detector, operated for 15 months in 1997-8 and collected 8.9 billion events. It was the first extensive air shower (EAS) array sensitive to showers intiated by primaries with energy below 1 TeV. The shadows of the sun and moon observed with cosmic rays can be used to study systematic pointing shifts and measure the angular resolution of EAS arrays. Below a few TeV, the paths of cosmic rays coming toward the earth are bent by the helio- and geo-magnetic fields. This is expected to distort and displace the shadows of the sun and the moon. The moon shadow, offset from the nominal (undeflected) position, has been observed with high statistical significance in Milagrito. This can be used to establish energy calibrations, as well as to search for the anti-matter content of the VHE cosmic ray flux. The shadow of the sun has also been observed with high significance.']",['1999-06-25'] +1040,['eng'],"['Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G', 'Delay, R S', 'Dingus, B L', 'Dorfan, D E', 'Ellsworth, R W', 'Evans, D', 'Falcone, A D', 'Fleysher, L', 'Fleysher, R', 'Gisler, G', 'Goodman, J A', 'Haines, T J', 'Hoffman, C M', 'Hugenberger, S', 'Kelley, L A', 'Leonor, I', 'Macri, J R', 'McConnell, M', 'McCullough, J F', 'McEnery, J E', 'Miller, R S', 'Mincer, A I', 'Morales, M F', 'Némethy, P', 'Ryan, J M', 'Schneider, M', 'Shen, B', 'Shoup, A L', 'Sinnis, G', 'Smith, A J', 'Sullivan, G W', 'Thompson, T N', 'Tumer, O T', 'Wang, K', 'Wascko, M O', 'Westerhoff, S', 'Williams, D A', 'Yang, T', 'Yodh, G B']",['Detection of 6 November 1997 Ground Level Event by Milagrito'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'cosmic radiation, solar', 'cosmic radiation, flux', 'cosmic radiation, time variation', 'shower detector, experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906387', 'http://krusty.physics.utah.edu/~icrc1999/root/vol6/s1_7_02.pdf']","['Solar Energetic Particles from the 6 November 1997 solar flare/CME(coronal mass ejection) with energies exceeding 10 GeV have been detected by Milagrito, a prototype of the Milagro Gamma Ray Observatory. While particle acceleration beyond 1 GeV at the Sun is well established, few data exist for protons or ions beyond 10 GeV. The Milagro observatory, a ground based water Cherenkov detector designed for observing very high energy gamma ray sources, can also be used to study the Sun. Milagrito, which operated for approximately one year in 1997/98, was sensitive to solar proton and neutron fluxes above ~5- 10 GeV. Milagrito operated in a scaler mode, which was primarily sensitive to muons, low energy photons, and electrons, and the detector operated in a mode sensitive to showers and high zenith angle muons. In its scaler mode, Milagrito registered a rate increase coincident with the 6 November 1997 ground level event observed by Climax and other neutron monitors. A preliminary analysis suggests the presence of >10 GeV particles.']",['1999-06-25'] +1041,['eng'],"['Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G', 'Delay, R S', 'Dingus, B L', 'Dorfan, D E', 'Ellsworth, R W', 'Evans, D', 'Falcone, A D', 'Fleysher, L', 'Fleysher, R', 'Gisler, G', 'Goodman, J A', 'Haines, T J', 'Hoffman, C M', 'Hugenberger, S', 'Kelley, L A', 'Leonor, I', 'Macri, J R', 'McConnell, M', 'McCullough, J F', 'McEnery, J E', 'Miller, R S', 'Mincer, A I', 'Morales, M F', 'Némethy, P', 'Ryan, J M', 'Schneider, M', 'Shen, B', 'Shoup, A L', 'Sinnis, G', 'Smith, A J', 'Sullivan, G W', 'Thompson, T N', 'Tumer, O T', 'Wang, K', 'Wascko, M O', 'Westerhoff, S', 'Williams, D A', 'Yang, T', 'Yodh, G B']",['Search for Short Duration Bursts of TeV $\\gamma$ Rays with the Milagrito Telescope'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, time variation', 'cosmic radiation, flux', 'upper limit', 'cosmic radiation, energy', 'data analysis method', 'Cherenkov counter, water', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906386', 'http://krusty.physics.utah.edu/~icrc1999/root/vol4/o2_3_07.pdf']","['The Milagrito water Cherenkov telescope operated for over a year. The most probable gamma-ray energy was ~1 TeV and the trigger rate was as high as 400 Hz. We have developed an efficient technique for searching the entire sky for short duration bursts of TeV photons. Such bursts may result from ""traditional"" gamma-ray bursts that were not in the field-of-view of any other instruments, the evaporation of primordial black holes, or some as yet undiscovered phenomenon. We have begun to search the Milagrito data set for bursts of duration 10 seconds. Here we will present the technique and the expected results. Final results will be presented at the conference.']",['1999-06-25'] +1042,['eng'],"['Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G', 'Delay, R S', 'Dingus, B L', 'Dorfan, D E', 'Ellsworth, R W', 'Evans, D', 'Falcone, A D', 'Fleysher, L', 'Fleysher, R', 'Gisler, G', 'Goodman, J A', 'Haines, T J', 'Hoffman, C M', 'Hugenberger, S', 'Kelley, L A', 'Leonor, I', 'Macri, J R', 'McConnell, M', 'McCullough, J F', 'McEnery, J E', 'Miller, R S', 'Mincer, A I', 'Morales, M F', 'Némethy, P', 'Ryan, J M', 'Schneider, M', 'Shen, B', 'Shoup, A L', 'Sinnis, G', 'Smith, A J', 'Sullivan, G W', 'Thompson, T N', 'Tumer, O T', 'Wang, K', 'Wascko, M O', 'Westerhoff, S', 'Williams, D A', 'Yang, T', 'Yodh, G B']",['Status of the Milagro $\\gamma$ Ray Observatory'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'Cherenkov counter, water', 'photoelectron, amplifier', 'showers, air']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906383', 'http://krusty.physics.utah.edu/~icrc1999/root/vol2/h6_1_02.pdf', 'http://documents.cern.ch/archive/electronic/other/uploader/MORIOND/heg-t13.pdf']","[""The Milagro Gamma Ray Observatory is the world's first large-area water Cherenkov detector capable of continuously monitoring the sky at TeV energies. Located in northern New Mexico, Milagro will perform an all sky survey of the Northern Hemisphere at energies between ~250 GeV and 50 TeV. With a high duty cycle, large detector area (~5000 square meters), and a wide field-of-view (~1 sr), Milagro is uniquely capable of searching for transient and DC sources of high-energy gamma-ray emission. Milagro has been operating since February, 1999. The current status of the Milagro Observatory and initial results will be discussed.""]",['1999-06-25'] +1043,['eng'],"['Atkins, R', 'Benbow, W', 'Berley, D', 'Chen, M L', 'Coyne, D G', 'Delay, R S', 'Dingus, B L', 'Dorfan, D E', 'Ellsworth, R W', 'Evans, D', 'Falcone, A D', 'Fleysher, L', 'Fleysher, R', 'Gisler, G', 'Goodman, J A', 'Haines, T J', 'Hoffman, C M', 'Hugenberger, S', 'Kelley, L A', 'Leonor, I', 'Macri, J R', 'McConnell, M', 'McCullough, J F', 'McEnery, J E', 'Miller, R S', 'Mincer, A I', 'Morales, M F', 'Némethy, P', 'Ryan, J M', 'Schneider, M', 'Shen, B', 'Shoup, A L', 'Sinnis, G', 'Smith, A J', 'Sullivan, G W', 'Thompson, T N', 'Tumer, O T', 'Wang, K', 'Wascko, M O', 'Westerhoff, S', 'Williams, D A', 'Yang, T', 'Yodh, G B']",['An All-Sky Search for Steady VHE Gamma-Ray Sources'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'Cherenkov counter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906369'],"['The Milagrito water Cherenkov detector in the Jemez Mountains near Los Alamos, New Mexico took data from February 1997 to April 1998. Milagrito served as a prototype for the larger Milagro detector, which has just begun operations. Milagrito was the first large-aperture gamma-ray detector with sensitivity to gamma rays below 1 TeV. We report here on a search for steady emission from point sources over most of the northern sky using data from Milagrito.']",['1999-06-24'] +1044,['eng'],"['Alvarez-Muñiz, J', 'Vázquez, R A', 'Zas, E']",['Radiodetection of neutrino interactions in ice'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'neutrino/e, cosmic radiation', 'Cherenkov counter, water', 'solids, water', 'showers']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906348', 'http://krusty.physics.utah.edu/~icrc1999/root/vol2/h6_3_14.pdf']","['We study the Cherenkov radiopulses emitted in PeV and EeV neutrino interactions in ice. We discuss how the rich radiation pattern in the 100 MHz to 1 GHz frequency range, in principle allows the measurement of shower elongation produced in neutrino interactions opening up the possibility of flavor recognition identifying charged current electron neutrino interactions.']",['1999-06-24'] +1045,['eng'],"['Alvarez-Muñiz, J', 'Zas, E']",['EeV Hadronic Showers in Ice'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'cosmic radiation', 'showers, hadronic', 'showers, parametrization', 'water, solids', 'Landau-Pomeranchuk-Migdal effect', 'numerical methods, Monte Carlo', 'Cherenkov counter, water', 'numerical calculations, Monte Carlo']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906347', 'http://krusty.physics.utah.edu/~icrc1999/root/vol1/h2_5_31.pdf']",['We study the longitudinal development of hadronic showers in water and ice for energies up to 100 EeV. We present results of a hybrid Monte Carlo method developed for the purpose of simulating those showers. We show parameterizations of the longitudinal development of hadronic showers in ice and we investigate the implications of the LPM effect on shower development. The results obtained are relevant for the detection of high energy cosmic rays and neutrinos in large scale detectors that use water as Cherenkov medium.'],['1999-06-24'] +1046,['eng'],"['Olinto, A V', 'Epstein, R I', 'Blasi, P']",['Galactic Ultra-High-Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'galaxy', 'iron, acceleration', 'n, matter', 'magnetic field, high', 'pulsar', 'ion, tracks', 'numerical calculations, interpretation of experiments', 'proposed experiment']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906338', 'http://krusty.physics.utah.edu/~icrc1999/root/vol4/o3_3_03.pdf']","['The absence of the expected GZK cutoff strongly challenges the notion that the highest-energy cosmic rays are of distant extragalactic origin. We discuss the possibility that these ultra-high-energy events originate in our Galaxy and propose that they may be due to iron nuclei accelerated from young, strongly magnetic neutron stars. Newly formed pulsars accelerate ions from their surface through relativistic MHD winds. We find that pulsars whose initial spin periods are shorter than $\\sim 4 (B_S/10^{13}{\\rm G})$ ms, where $B_S$ is the surface magnetic field, can accelerate iron ions to greater than $10^{20} eV$. These ions can pass through the remnant of the supernova explosion that produced the pulsar without suffering significant spallation reactions. Depending on the structure of the galactic magnetic field, the trajectories of the iron ions from galactic sources can be consistent with the observed arrival directions of the highest energy events.']",['1999-06-24'] +1047,['eng'],"['Grivell, I J', 'Liddle, A R']",['Inflaton potential reconstruction without slow-roll'],['Astrophysics and Astronomy'],"['inflationary universe', 'potential, inflaton', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'phi**n model, 4', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906327'],"['We describe a method of obtaining the inflationary potential from observations which does not use the slow-roll approximation. Rather, the microwave anisotropy spectrum is obtained directly from a parametrized potential numerically, with no approximation beyond linear perturbation theory. This permits unbiased estimation of the parameters describing the potential, as well as providing the full error covariance matrix. We illustrate the typical uncertainties obtained using the Fisher information matrix technique, studying the $\\lambda \\phi^4$ potential in detail as a concrete example.']",['1999-06-24'] +1048,['eng'],"['Burdett, A M', 'Bond, I H', 'Boyle, P J', 'Bradbury, S M', 'Buckley, J H', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', ""D'Vali, M"", 'Fegan, D J', 'Fegan, S J', 'Finley, J P', 'Gaidos, J A', 'Gillanders, G H', 'Hall, T A', 'Hillas, A M', 'Kildea, J', 'Knapp, J', 'Krennrich, F', 'Lang, M J', 'Le Bohec, S', 'Lessard, R W', 'Masterson, C', 'Moriarty, P', 'Quinn, J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Vasilev, V', 'Weekes, T C']",['A Search for Pulsed TeV $\\gamma$ Ray Emission from the Crab Pulsar'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, time variation', 'cosmic radiation, particle source', 'pulsar', 'cosmic radiation, energy spectrum', 'flux, upper limit', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906318', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_2_02.pdf']","[""We present the results of a search for pulsed TeV emission from the Crab pulsar using the Whipple Observatory's 10m gamma-ray telescope. The direction of the Crab pulsar was observed for a total of 73.4 hours between 1994 November and 1997 March. Spectral analysis techniques were applied to search for the presence of a gamma-ray signal from the Crab pulsar over the energy band 250GeV to 4TeV. At these energies we do not see any evidence of the 33ms pulsations present at lower energies from the Crab pulsar. The 99.9% confidence level upper limit for pulsed emission above 250GeV is derived to be 4.8 10^-12 cm^-2 s^-1 or <3% of the steady flux from the Crab Nebula. These results imply a sharp cut-off of the power-law spectrum seen by the EGRET instrument on the Compton Gamma-Ray Observatory. If the cut-off is exponential, it must begin at 60GeV or lower to accommodate these upper limits.""]",['1999-06-21'] +1049,['eng'],"['Pina-Avelino, P', 'Shellard, E P S']",['The cluster abundance in cosmic string models for structure formation'],['Astrophysics and Astronomy'],"['astrophysics, string', 'density, perturbation', 'photon, cluster', 'photon, cosmic radiation', 'cluster, density', 'energy, density', 'cosmic radiation, background', 'astrophysics, fundamental constant', 'astrophysics, missing-mass', 'mass, temperature', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906313'],"['We use the present observed number density of large X-ray clusters to constrain the amplitude of matter density perturbations induced by cosmic strings on the scale of $8 h^{-1}$Mpc ($\\sigma_8$), in both open cosmologies and flat models with a non-zero cosmological constant. We find a slightly lower value of $\\sigma_8$ than that obtained in the context of primordial Gaussian fluctuations generated during inflation. This lower normalization of $\\sigma_8$ results from the mild non-Gaussianity on cluster scales, where the one point probability distribution function is well approximated by a $\\chi^2$ distribution. We use our estimate of $\\sigma_8$ to constrain the string linear energy density $\\mu$ and show that it is consistent with the COBE normalization.']",['1999-06-21'] +1050,['eng'],"['Baiko, D A', 'Haensel, P']",['Transport properties and neutrino emissivity of dense neutron-star matter with localized protons'],['Astrophysics and Astronomy'],"['n, matter', 'p', 'transport theory', 'neutrino, emission', 'neutrino, bremsstrahlung', 'neutrino, pair production', 'energy loss', 'temperature, dependence', 'astrophysics', 'electron p, interaction', 'electron electron, interaction', 'nucleon nucleon, interaction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906312'],"[""As pointed out by Kutschera and W{ó}jcik, very low concentration of protons combined with a specific density dependence of effective neutron-proton interaction could lead to a localization of ``proton impurities'' in neutron medium at densities exceeding four times normal nuclear matter density. We study consequences of the localization of protons for transport processes in dense neutron star cores, assuming random distribution of proton impurities. Kinetic equations, relevant for the transport of charge, heat and momentum, are solved using variational method. Localization of protons removes a T^{-2} factor from the transport coefficients, which leads, at lower temperatures, to a strong decrease of thermal conductivity, electrical conductivity and shear viscosity of neutron star matter, as compared to the standard case, where protons form a Fermi liquid. Due to the localization of protons a number of conventional neutrino emission processes (including modified URCA process) become inoperative in neutron star cores. On the other hand, the energy loss rate from neutrino-antineutrino pair bremsstrahlung due to electron and neutron scattering off (localized) protons, will have a specific T^6 dependence, which could modify the cooling of the neutron star core, as compared to the standard case. Possible astrophysical implications of the localization of protons for neutron star evolution and dynamics are discussed.""]",['1999-06-21'] +1051,['eng'],"['Mikhailov, A A']",['Search for Sources of Ultrahigh Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, angular distribution', 'pulsar', 'cosmic radiation, flux', 'shower detector, experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906302', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o1_3_08.pdf']","['The connection between the arrival directions of ultrahigh energy cosmic rays by using the EAS array data and point galactic sources of radio-and gamma-radiations, pulsars,is sought. At the mean particle energy of 10^{19} eV the correlation between the particle arrival directions and pulsars located along the magnetic field lines has been found. According to our estimations the chance probability is equal to 2.10^{-4}. The observed particle flux from 16 pulsars inside a circle of radius <6^{\\circ} exceeds the background by 6.3\\sigma (p < 10^{-10}), from PSR 2351+61 - 5\\sigma. A group of 9 pulsars has been found from the direction of which the particle flux in the region 10^{\\circ}\\times60^{\\circ} is in excess of the expected one by 4.4\\sigma. The obtained results are discussed.']",['1999-06-21'] +1052,['eng'],"['Vankov, A']",['On matter-antimatter separation in open relativistic material system'],['Astrophysics and Astronomy'],"['antimatter', 'relativistic', 'matter, interaction', 'radiation, electromagnetic', 'mass spectrum', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906279'],"['An open (having no physical boundaries) baryon symmetric system is considered in a flat space-time. We assume that a space is uniformly filled with electromagnetic radiation and material objects, and the system is isotropic in any inertial reference frame. It means that a coordinate-momentum distribution of radiation and material objects does not depend on a reference frame, and the system should be in a state of chaotic relativistic motion. The dominant interaction processes are like-matter merge, unlike-matter annihilation and pair production. In this approximation we came to the conclusion that matter and antimatter exist in a form of mix of material objects characterized by a stationary baryon symmetric mass distribution in a broad mass range. In other words, a matter-antimatter space separation takes place.']",['1999-06-17'] +1053,['eng'],"['Pal, P B']",['Particle dark matter'],['Astrophysics and Astronomy'],"['talk, Kharagpur 1999/01/04', 'astrophysics, missing-mass', 'neutrino, mass', 'energy, density', 'axion, search for', 'WIMP, search for', 'proposed experiment', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906261'],"['I discuss some compelling suggestions about particles which could be the dark matter in the universe, with special attention to experimental searches for them.']",['1999-06-17'] +1054,['eng'],"['Dzhilkibaev, Z A']",['The Lake Baikal Experiment'],['Astrophysics and Astronomy'],"['talk, Venice 1999/02/23', 'neutrino, cosmic radiation', 'muon, cosmic radiation', 'muon, angular distribution', 'magnetic monopole, search for', 'neutrino/e, flux', 'upper limit', 'antineutrino electron, interaction', 'hadron, multiple production', 'W-', 'Cherenkov counter, water', 'deep underground detector, Baikal', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906255'],"['We review the present status of the Baikal Neutrino Project. The construction and performance of the large deep underwater Cherenkov detector NT-200 with 192 PMTs, which is currently taking data in Lake Baikal, are described. Some results from intermediate detector stages are presented.']",['1999-06-16'] +1055,['eng'],"['Periwal, V']",['Cosmological and astrophysical tests of quantum gravity'],['Astrophysics and Astronomy'],"['quantum gravity, validity test', 'renormalization group, fixed point', 'parametrization', 'fundamental constant, length', 'correlation, length', 'effective action', 'astrophysics, fundamental constant', 'galaxy, rotational']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906253'],"['Physics in the vicinity of an ultraviolet stable fixed point of a quantum field theory is parametrized by a renormalization group invariant macroscopic length scale, the correlation length $\\xi,$ with the quantum effective action a function of this length scale. Numerical simulations of quantum gravity suggest the existence of just such a fixed point. Since the quantum effective action is a function only of $\\xi,$ the cosmological constant must be $k \\xi^{-2}$ with $k$ a pure number. Higher derivative terms are also parametrized by this length scale, so in particular the effective Newtonian dynamics of a test particle is modified at acceleration scales of order $1/\\xi.$ Thus, renormalization group effects in quantum gravity provide a natural link between the phenomenological acceleration scale associated with galactic rotation curves and the value of the cosmological constant favoured by recent supernovae observations.']",['1999-06-16'] +1056,['eng'],"['Sinnis, G']",['Current Status of VHE Astronomy'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'counters and detectors', 'proposed experiment', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906242'],"['Very-high-energy astronomy studies the Universe at energies between 30 GeV and 100 TeV. The past decade has seen enormous progress in this field. There are now at least seven known sources of VHE photons. By studying these objects in the VHE regime one can begin to understand the environments surrounding these objects, and how particle acceleration is realized in nature. In addition the photon beams from the extragalactic gamma-ray sources can be used to study the electromagnetic fields in the intervening space. This recent progress can be traced to the development of a new class of detector with the ability to differentiate between air showers produced by gamma rays and those produced by the much more numerous hadronic cosmic-ray background. Much more sensitive instruments are currently in the design phase and two new types of instruments are beginning to take data. In this paper we will discuss the physics of these sources and describe the existing and planned detectors.']",['1999-06-15'] +1057,['eng'],"['Bowyer, S', 'Korpela, E J', 'Lampton, J E M', 'Morales, C', 'Pérez-Mercader, J', 'Gomes, J F', 'Trapero, J']",['Evidence Against the Sciama Model of Radiative Decay of Massive Neutrinos'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, massive', 'neutrino, radiative decay', 'photon, energy spectrum', 'spectrometer, experimental results', 'satellite']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906241'],"['We report on spectral observations of the night sky in the band around 900 angstroms where the emission line in the Sciama model of radiatively decaying massive neutrinos would be present. The data were obtained with a high resolution, high sensitivity spectrometer flown on the Spanish MINISAT satellite. The observed emission is far less intense than that expected in the Sciama model.']",['1999-06-15'] +1058,['eng'],"['Moskalenko, I V', 'Strong, A W']",['Galactic propagation of positrons from particle dark-matter annihilation'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'astrophysics, missing-mass', 'annihilation, missing-mass', 'positron, propagator', 'positron, flux', 'galaxy', 'cosmic radiation, energy spectrum', 'cosmic radiation, background', 'numerical calculations']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906230', 'http://krusty.physics.utah.edu/~icrc1999/root/vol2/h5_1_15.pdf']","['We have made a calculation of the propagation of positrons from dark-matter particle annihilation in the Galactic halo for different models of the dark matter halo distribution using our 3D code. We show that the Green\'s functions are not very sensitive to the dark matter distribution for the same local dark matter energy density. We compare our predictions with computed cosmic ray positron spectra (""background"") for the ""conventional"" cosmic-ray nucleon spectrum which matches the local measurements, and a modified spectrum which respects the limits imposed by measurements of diffuse Galactic gamma-rays, antiprotons, and positrons. We conclude that significant detection of a dark matter signal requires favourable conditions and precise measurements unless the dark matter is clumpy which would produce a stronger signal. Although our conclusion qualitatively agrees with that of previous authors, it is based on a more realistic model of particle propagation and thus reduces the scope for future speculations. Reliable background evaluation requires new accurate positron measurements and further developments in modelling production and propagation of cosmic ray species in the Galaxy.']",['1999-06-15'] +1059,['eng'],"['Catanese, M', 'Bond, I H', 'Bradbury, S M', 'Breslin, A C', 'Buckley, J H', 'Burdett, A M', 'Carter-Lewis, D A', 'Cawley, M F', 'Dunlea, S', ""D'Vali, M"", 'Fegan, D J', 'Fegan, S J', 'Finley, J P', 'Gaidos, J A', 'Hall, T A', 'Hillas, A M', 'Horan, D', 'Knapp, J', 'Krennrich, F', 'Le Bohec, S', 'Lessard, R W', 'Masterson, C', 'Moriarty, P', 'Quinn, J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Vasilev, V', 'Weekes, T C', 'Maraschi, L', 'Fossati, G', 'Tavecchio, F', 'Chiappetti, L', 'Celotti, A', 'Ghisellini, G', 'Grandi, P', 'Pian, E', 'Tagliaferri, G', 'Treves, A']",['Hour-Scale Multiwavelength Variability in Markarian 421'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'astrophysics, blazar', 'cosmic radiation, time variation', 'correlation, time', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906209', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_03.pdf']","['Markarian 421 was observed for about four days with BeppoSAX and the Whipple Observatory gamma-ray telescope in April 1998. A pronounced, well-defined, flare with hour-scale variability was observed simultaneously in X-rays and very high energy gamma-rays. These data provide the first evidence that the X-ray and TeV intensities are well correlated on time-scales of hours. While the rise of the flare occurred on a similar time-scale in the two wavebands, the decay of the flare was much more rapid in gamma rays, providing the first clear indication that the X-ray and gamma-ray emission may not be completely correlated in Markarian 421.']",['1999-06-14'] +1060,['eng'],"['Spiering, C']",['AMANDA'],['Astrophysics and Astronomy'],"['talk, Venice 1999/02/23', 'neutrino, cosmic radiation', 'Cherenkov counter, water', 'solids, water', 'photoelectron, amplifier', 'muon, tracks', 'search for, magnetic monopole', 'showers, air', 'deep underground detector, AMANDA']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906205'],"['We review the status of the AMANDA neutrino telescope. We present results obtained from the four-string prototype array AMANDA-B4 and describe the methods of track reconstruction and neutrino event separation. We give also first results of the analysis of the 10-string detector AMANDA-B10, in particular on atmospheric neutrinos and the search for magnetic monopoles. We sketch the future schedule on the way to a cube kilometer telescope at the South Pole, ICECUBE']",['1999-06-14'] +1061,['eng'],"['Andrés, E C']",['The AMANDA Neutrino Telescope'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'Cherenkov counter, water', 'solids, water', 'calibration', 'statistical analysis', 'photoelectron, amplifier', 'deep underground detector, AMANDA', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906203'],"['AMANDA is a high-energy neutrino telescope presently under construction at the geographical South Pole. In the Antarctic summer 1995/96, an array of 80 optical modules (OMs) arranged on 4 strings (AMANDA-B4) was deployed at depths between 1.5 and 2 km. In this paper we describe the design and performance of the AMANDA-B4 prototype, based on data collected between February and November 1996. Monte Carlo simulations of the detector response to down-going atmospheric muon tracks show that the global behavior of the detector is understood. We describe the data analysis method and present first results on atmospheric muon reconstruction and separation of neutrino candidates. The AMANDA array was upgraded with 216 OMs on 6 new strings in 1996/97 (AMANDA-B10), and 122 additional OMs on 3 strings in 1997/98.']",['1999-06-14'] +1062,['eng'],"['Piner, B G', 'Unwin, S C', 'Wehrle, A E', 'Edwards, P G', 'Fey, A L', 'Kingham, K A']",['VSOP and Ground-based VLBI Imaging of the TeV Blazar Markarian 421 at Multiple Epochs'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, blazar', 'cosmic radiation, energy', 'cosmic radiation, time variation', 'counters and detectors, satellite', 'imaging', 'experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906202'],"[""We present thirty VLBI images of the TeV blazar Markarian 421 (1101+384) at fifteen epochs spanning the time range from 1994 to 1997, and at six different frequencies from 2.3 to 43 GHz. The imaged observations include a high-resolution 5 GHz VLBI Space Observatory Programme (VSOP) observation with the HALCA satellite on 1997 November 14; full-track VLBA observations from 1994 April, 1996 November, and 1997 May at frequencies between 5 and 43 GHz; six epochs of VLBA snapshot observations at frequencies between 2 and 15 GHz from Radio Reference Frame studies; and five geodetic VLBI observations at 2 and 8 GHz from the archive of the Washington VLBI Correlator Facility located at the U.S. Naval Observatory. The dense time coverage of the images allows us to unambiguously track components in the parsec-scale jet over the observed time range. We measure the speeds of three inner jet components located between 0.5 and 5 mas from the core (0.3 to 3 pc projected linear distance) to be 0.19 +/- 0.27, 0.30 +/- 0.07, and -0.07 +/- 0.07 c (H_{0}=65 km s^{-1} Mpc^{-1}). If the sole 43 GHz image is excluded, all measured speeds are consistent with no motion. These speeds differ from tentative superluminal speeds measured by Zhang & Båå th from three epochs of data from the early 1980's. Possible interpretations of these subluminal speeds in terms of the high Doppler factor demanded by the TeV variability of this source are discussed.""]",['1999-06-14'] +1063,['eng'],"['Bussino, S']",['$\\gamma$-Hadron Discrimination with a Neural Network in the ARGO-YBJ Experiment'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'p, cosmic radiation', 'particle identification, (p photon)', 'neural network', 'drift chamber', 'electrode, impedance']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906201', 'http://krusty.physics.utah.edu/~icrc1999/root/vol1/h2_5_08.pdf']",['The structure of a neural network developed for the gamma hadron separation in the ARGO-YBJ detector is presented. The discrimination power in the full ARGO-YBJ energy range is shown in detail and the improvement in the detector sensitivity is also discussed.'],['1999-06-14'] +1064,['eng'],"['Carson, M J', 'McKernan, B', 'Yaqoob, T', 'Fegan, D J']",['Short-timescale Variability in the Broadband Emission of the Blazars Mkn421 and Mkn501'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'astrophysics, blazar', 'cosmic radiation, energy', 'numerical calculations, interpretation of experiments']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906200', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_39.pdf']","['We analyse ASCA x-ray data and Whipple \\gamma-ray data from the blazars Mkn421 and Mkn501 for short-timescale variability. We find no evidence for statistically significant (>3\\sigma) variability in these data, in either source, on timescales of less than \\sim 10 minutes.']",['1999-06-14'] +1065,['eng'],"['Vernetto, S']",['Study of $\\gamma$-Ray Bursts of energy E > 10 GeV with the ARGO-YBJ detector'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'photon, showers', 'cosmic radiation, energy', 'shower detector, efficiency']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906185'],"['The study of high energy gamma-ray bursts can be performed by large area air shower arrays operating at very high mountain altitudes. ARGO-YBJ is a detector optimized to observe small size air showers, to be constructed at the Yangbajing Laboratory (Tibet, P.R. China) at an altitude of 4300 m. One of the goals of the experiment is the study of Gamma-Ray Bursts of energies E > 10 GeV. This can be achieved using the ""single particle"" technique, more profitable in the energy region E < 50 GeV, and the ""low multiplicity"" technique, suitable to observe GRBs at higher energies. The sensitiviy of ARGO-YBJ allows the detection of GRBs with energy fluences in the range 1--100 GeV as low as F~10^{-6} -- 10^{-5} erg cm^{-2}, depending on the spectral characteristics of the burst.']",['1999-06-11'] +1066,['eng'],"['Breslin, A C', 'Bond, I H', 'Bradbury, S M', 'Buckley, J H', 'Burdett, A M', 'Carson, M J', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Dunlea, S', ""D'Vali, M"", 'Fegan, D J', 'Fegan, S J', 'Finley, J P', 'Gaidos, J A', 'Hall, T A', 'Hillas, A M', 'Horan, D', 'Kildea, J', 'Knapp, J', 'Krennrich, F', 'Le Bohec, S', 'Lessard, R W', 'Masterson, C', 'McKernan, B', 'Quinn, J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Vasilev, V', 'Weekes, T C']",['VHE $\\gamma$-ray observations of Markarian 501'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'Cherenkov counter, imaging', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906150', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_23.pdf']","[""Markarian 501, a nearby (z=0.033) X-ray selected BL Lacertae object, is a well established source of Very High Energy (VHE, E>=300 GeV) gamma rays. Dramatic variability in its gamma-ray emission on time-scales from years to as short as two hours has been detected. Multiwavelength observations have also revealed evidence that the VHE gamma-ray and hard X-ray fluxes may be correlated. Here we present results of observations made with the Whipple Collaboration's 10 m Atmospheric Cerenkov Imaging Telescope during 1999 and discuss them in the context of observations made on Markarian 501 during the period from 1996-1998.""]",['1999-06-09'] +1067,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['Geomagnetic effects on atmospheric Cerenkov images'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'magnetic field, geophysics', 'statistical analysis']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906139', 'http://krusty.physics.utah.edu/~icrc1999/root/vol5/o4_3_11.pdf']",['Atmospheric Cerenkov telescopes are used to detect electromagnetic showers from primary gamma rays of energy > 300 GeV and to discriminate these from cascades due to hadrons using the shape and orientation of the Cerenkov images. The geomagnetic field affects the development of showers and diffuses and distorts the images. When the component of the field normal to the shower axis is sufficiently large (> 0.4 G) the performance of gamma ray telescopes may be affected.'],['1999-06-09'] +1068,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['The energy spectra of TeV sources measured with the Durham Mark 6 Telescope'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'photon, showers', 'Cherenkov counter, imaging', 'trigger, efficiency', 'energy dependence', 'numerical calculations, Monte Carlo']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906138', 'http://krusty.physics.utah.edu/~icrc1999/root/vol5/o4_3_10.pdf']",['A programme of detailed simulations of the response of the Durham Mark 6 atmospheric Cherenkov telescope is in progress. The effective collecting area for triggering by gamma-ray showers after application of selection criteria is derived as a function of energy. An initial result from the larger events in the 1996 and 1997 observations of the BL Lac PKS 2155-304 is that the time averaged flux above 1.5 TeV was (6.7 +/- 2.2) x 10^-8 m^-2 s^-1.'],['1999-06-09'] +1069,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['TeV Gamma Ray Emission from Cen X-3'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'cosmic radiation, energy', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906137', 'http://krusty.physics.utah.edu/~icrc1999/root/vol4/o2_4_09.pdf']","['Cen X-3 is a well-studied high-mass accreting X-ray binary and a variable source of high energy gamma rays from 100 MeV to 1 TeV. The object has been extensively monitored with the University of Durham Mark 6 telescope. Results of observations, including those taken in 1998 and 1999, are reported. There is no evidence for time variability in all the VHE data. There is also no evidence for correlation of the VHE flux with the X-ray flux detected by BATSE and RXTE/ASM. A search for periodic emission, at or close to the X-ray spin period, in the VHE data yielded a 3 sigma upper limit to the pulsed flux of 2.0 x 10^-12 cm^-2 s^-1.']",['1999-06-09'] +1070,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Orford, K J', ""O'Connell, M G G"", 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['TeV Measurements of Young Pulsars and Supernova Remnants'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'pulsar', 'supernova', 'cosmic radiation, flux', 'upper limit', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906136', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_2_21.pdf']","['Observations have been made with the University of Durham Mark 6 telescope of a number of supernova remnants and young pulsars (Vela pulsar, PSR B1055-52, PSR J1105-6107, PSR J0537-6910 and PSR B0540-69). No VHE gamma ray emission, either steady or pulsed, has been detected from these objects.']",['1999-06-09'] +1071,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Murray, J A', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['Measurements of Flux Limits for TeV Emission from AGNs'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'galaxy, AGN', 'cosmic radiation, flux', 'upper limit', 'cosmic radiation, time variation', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906134', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_30.pdf']","['The University of Durham Mark 6 Telescope has been used to make observations of a number of AGNs visible from the Southern Hemisphere. Results are presented for limits to VHE gamma ray emission from 1ES 0323+022, PKS 0829+046, 1ES 1101-232, Cen A, PKS 1514-24, RXJ 10578-275 and 1ES 2316-423, both for steady emission and for outbursts on timescales of ~ 1 day.']",['1999-06-09'] +1072,['eng'],"['Mangalam, A', 'Nityananda, R', 'Sridhar, S']",['Constrained Violent Relaxation to a Spherical Halo'],['Astrophysics and Astronomy'],"['galaxy', 'potential, fluctuation', 'particle, orbit', 'diffusion', 'plasma', 'phase space', 'angular momentum', 'energy, density', 'velocity, dispersion', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906133'],"[""Violent relaxation during the collapse of a galaxy halo is known to be incomplete in realistic cases such as cosmological infall or mergers. We adopt a physical picture of strong but short lived interactions between potential fluctuations and particle orbits, using the broad framework outlined by Tremaine (1987) for incorporating incompleteness of the relaxation. We are guided by results from plasma physics, viz. the quasilinear theory of Landau damping, but allow for significant differences in our case. Crucially, wave particle scattering does not drive the system to an equilibrium distribution function of the exponential type, even in regions of phase space allowed by the constraints. The physical process is mixing without friction in ``action'' space, for which the simplest possible model is a constant phase space density modulated by the constraints. Our distribution function does not use the exponential functions of the energy prevalent in other work, which we regard as inappropriate to collisionless systems. The halo of the self-consistent, parameter-free solutions show an r^(-4) behavior in density at large r, an r^(1/4) surface brightness profile in the region 0.1-8 r_e, and a radially anisotropic velocity dispersion profile outside an isotropic core. The energy distribution seen in simulations N(E) singles out the pericenter cutoff model as the most realistic among the variants we have explored.""]",['1999-06-09'] +1073,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['VHE $\\gamma$ Rays from PKS 2155-304'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'upper limit', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906132', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_13.pdf']",['The X-ray selected BL Lac PKS 2155-304 has been observed using the University of Durham Mark 6 very high energy gamma ray telescope during 1998. We find no evidence for TeV emission during these recent observations when the X-ray flux was observed to be low. We have reconsidered our measurements made in 1997 November when PKS 2155-304 was in a bright X-ray state and extended X-ray and GeV gamma ray observations were made as part of a multiwavelength campaign. Comparisons are made of the VHE emission during this time with the available data from other wavelengths.'],['1999-06-09'] +1074,['eng'],"['Bhatt, N', 'Agarwal, N K', 'Bhat, C K', 'Bhattacharya, S', 'Dhar, V K', 'Goyal, A', 'Goyal, H C', 'Kaul, C L', 'Koul, D K', 'Kaul, I K', 'Kaul, R K', 'Kaul, S K', 'Kaul, S R', 'Koul, M K', 'Koul, R K', 'Kothari, M', 'Rannot, R C', 'Razdan, A K', 'Sahayanathan, S', 'Sapru, M L', 'Satyabhama, N', 'Tickoo, A K', 'Venugopal, N', 'Yadav, K K', 'Bhat, C L']","['Observations of the Crab Nebula, Mkn 501 and Mkn 421 using the TACTIC Imaging Element']",['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'Cherenkov counter, imaging', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906128', 'http://krusty.physics.utah.edu/~icrc1999/root/vol4/o2_4_20.pdf']","[""The results of our observational campaigns on the two extragalactic sources Mkn 501 and Mkn 421, carried out with the Imaging Element of the TACTIC array, during March-May, 1998 and April-May, 1999, are presented. The results indicate that the two BL Lac objects (Mkn 501 and Mkn 421) were in a `low' gamma-ray emission state during both epochs of our observations.""]",['1999-06-09'] +1075,['eng'],"['Lessard, R W', 'Bond, I H', 'Boyle, P J', 'Bradbury, S M', 'Buckley, J H', 'Burdett, A M', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Dunlea, S', ""D'Vali, M"", 'Fegan, D J', 'Fegan, S J', 'Finley, J P', 'Gaidos, J A', 'Hall, T A', 'Hillas, A M', 'Horan, D', 'Knapp, J', 'Krennrich, F', 'Le Bohec, S', 'Masterson, C', 'Quinn, J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Vasilev, V', 'Weekes, T C']",['Search for TeV $\\gamma$-Rays from Shell-Type Supernova Remnants'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'supernova', 'acceleration, shock waves', 'cosmic radiation, flux', 'upper limit', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906118'],"[""If cosmic rays with energies <100 TeV originate in the galaxy and are accelerated in shock waves in shell-type supernova remnants (SNRs), gamma-rays will be produced as the result of proton and electron interactions with the local interstellar medium, and by inverse Compton emission from electrons scattering soft photon fields. We report on observations of two supernova remnants with the Whipple Observatory's 10 m gamma-ray telescope. No significant detections have been made and upper limits on the >500 GeV flux are reported. Non-thermal X-ray emission detected from one of these remnants (Cassiopeia A) has been interpreted as synchrotron emission from electrons in the ambient magnetic fields. Gamma-ray emission detected from the Monoceros/Rosette Nebula region has been interpreted as evidence of cosmic-ray acceleration. We interpret our results in the context of these observations.""]",['1999-06-08'] +1076,['eng'],"['Pina-Avelino, P', 'Martins, C J A P']",['Does a varying speed of light solve the cosmological problems?'],['Astrophysics and Astronomy'],"['relativity theory, general', 'photon, velocity', 'vacuum state', 'gravitation, fundamental constant', 'time variation', 'invariance, Lorentz', 'Einstein equation, solution', 'Friedman model', 'astrophysics, fundamental constant']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906117'],"['We propose a new generalisation of general relativity which incorporates a variation in both the speed of light in vacuum (c) and the gravitational constant (G) and which is both covariant and Lorentz invariant. We solve the generalised Einstein equations for Friedmann universes and show that arbitrary time-variations of c and G never lead to a solution to the flatness, horizon or order to do so, one needs to construct a theory which does not reduce to the standard one for any choice of time, length and energy units. This can be achieved by breaking a number of invariance principles such as covariance and Lorentz invariance.']",['1999-06-08'] +1077,['eng'],"['Barone, F', 'De Rosa, R', 'Eleuteri, A', 'Garufi, F', 'Milano, L', 'Tagliaferri, R']",['A Neural Network-based ARX Model of Virgo Noise'],['Astrophysics and Astronomy'],"['talk, Vietri 1999', 'gravitational radiation, counters and detectors', 'optics, interference', 'laser', 'neural network', 'statistical analysis']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906107'],['In this paper a Neural Network based approach is presented to identify the noise in the VIRGO context. VIRGO is an experiment to detect Gravitational Waves by means of a Laser Interferometer. Preliminary results appear to be very promising for data analysis of realistic Interferometer outputs.'],['1999-06-08'] +1078,['eng'],"['Piron, F']",['Observations of $\\gamma$-ray emission from the blazar Markarian 421 above 250 GeV with the CAT Cherenkov imaging telescope'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'blazar', 'cosmic radiation, energy spectrum', 'Cherenkov counter, imaging', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906102', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_09.pdf']","['The gamma-ray emission of the blazar Markarian 421 above 250 GeV has been observed by the CAT Cherenkov imaging telescope since December, 1996. We report here results on the source variability up to April, 1998, with emphasis on the 1998 campaign. For the flaring periods of this year, the energy spectrum was derived from 330 GeV up to 5.2 TeV: it is very well represented by a simple power law, with a differential spectral index of 2.96 +/- 0.13.']",['1999-06-08'] +1079,['eng'],"['Battye, R A', 'Magueijo, J', 'Weller, J']",['Early structure formation with cold plus hot dark matter'],['Astrophysics and Astronomy'],"['inflationary universe', 'astrophysics, string', 'astrophysics, missing-mass', 'matter, density', 'cosmic radiation, anisotropy', 'density, perturbation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906093'],"['Quantum fluctuations created during inflation can account for the observed matter distribution in the linear regime if the universe has two components of dark matter, one which is cold and collisionless, and the other which is hot and free streams on small scales. However, this free streaming property of the hot component prevents early structure formation, and since objects, such as damped Lyman-$\\alpha$ systems, have been observed at high redshift, it is necessary to produce more power on small scales. Here, we show that the situation can be improved substantially in models where cosmic strings are formed at the end of inflation, and in which both inflation and strings participate in the generation of structure.']",['1999-06-07'] +1080,['eng'],"['Dubovsky, S L', 'Tinyakov, Peter G']",['Generation of $10^{15}$ - $10^{17} eV$ photons by UHE CR in the Galactic magnetic filed'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, spectra', 'magnetic field, galaxy', 'synchrotron radiation', 'cosmic radiation, flux', 'electron, cosmic radiation', 'cosmic radiation, diffusion', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906092'],"['We show that the deep expected in the diffuse photon spectrum above the threshold of e+e- pair production, i.e., at energies 10^15 - 10^17 eV, may be absent due to the synchrotron radiation by the electron component of the extragalactic Ultra-High Energy Cosmic Rays (UHE CR) in the Galactic magnetic filed. The mechanism we propose requires small (less than 10^-11 G) extragalactic magnetic fields and large fraction of photons in the UHE CR. For a typical photon flux expected in top-down scenarios of UHE CR, the predicted flux in the region of the deep is close to the existing experimental limit. The sensitivity of our mechanism to the extragalactic magnetic field may be used to improve existing bounds on the latter by two orders of magnitude.']",['1999-06-07'] +1081,['eng'],"['Nishikawa, D']",['Periodicity in the TeV $\\gamma$ rays and X rays from Markarian 501'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'galaxy, AGN', 'cosmic radiation, time variation', 'experimental results', '> 1000 GeV']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906087', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_17.pdf']","['Historical TeV gamma-ray flares from Markarian 501 was observed using Utah Seven Telescope Array (7TA) from the end of March to the end of July of 1997. The Rossi X-ray Timing Explorer All Sky Monitor (RXTE ASM) has been observing X rays from Mrk 501 since Jan. 5, 1996. We find evidence for periodicities of $23.9^{+2.3}_{-2.0}$ days and $23.9^{+1.6}_{-2.9}$ days from TeV gamma-ray and X-ray light curves using 7TA and RXTE ASM. Their false-alarm probabilities are $8.2 \\times 10^{-3}$ and $5.6 \\times 10^{-5}$, respectively.']",['1999-06-07'] +1082,['eng'],"['Langlois, D']",['Correlated adiabatic and isocurvature perturbations from double inflation'],['Astrophysics and Astronomy'],"['inflationary universe, multiple', 'field theory, scalar', 'massive', 'coupling, minimal', 'perturbation, adiabatic', 'density, perturbation', 'correlation', 'spectra, production', 'cosmic radiation, background', 'anisotropy', 'temperature, fluctuation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906080'],"['It is shown that double inflation (two minimally coupled massive scalar fields) can produce correlated adiabatic and isocurvature primordial perturbations. Depending on the two relevant parameters of the model, the contributions to the primordial perturbations are computed, with special emphasis on the correlation, which can be quantitatively represented by a correlation spectrum. Finally the primordial spectra are evolved numerically to obtain the CMBR anisotropy multipole expectation values. It turns out that the existence of mixing and correlation can alter very significantly the temperature fluctuation predictions.']",['1999-06-07'] +1083,['eng'],"['Tanimori, T', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, S', 'Hara, T', 'Jinbo, J', 'Kawachi, A', 'Kifune, T', 'Kubo, H', 'Kushida, J', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Moriya, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Sato, Y', 'Susukita, R', 'Tamura, T', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T', 'Yuki, A']",['Construction of New 7 m Imaging Air Cerenkov Telescope of CANGAROO'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'optics, reflection', 'photoelectron, amplifier']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906078', 'http://krusty.physics.utah.edu/~icrc1999/root/vol5/o4_3_04.pdf']","['CANGAROO group has constructed the new large imaging Air \\v Cerenkov telescope to exploit hundred GeV region gamma-ray astronomy in March 1999 at Woomera, South Australia. It has a 7m parabolic mirror consisting of 60 small plastic spherical mirrors, and a fine imaging camera with 512 PMTs covering the field of view of 3 degree. Observation will start from July 1999.']",['1999-06-07'] +1084,['eng'],"['Muraishi, H', 'Tanimori, T', 'Yanagita, S', 'Yoshida, T', 'Kifune, T', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, S', 'Hara, T', 'Jinbo, J', 'Kawachi, A', 'Kubo, H', 'Kushida, J', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Moriya, M', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Sato, Y', 'Susukita, R', 'Tamura, T', 'Yoshikoshi, T', 'Yuki, A']",['Search for TeV $\\gamma$-Rays from the SNR RXJ1713.7-3946'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'supernova', 'cosmic radiation, energy', 'cosmic radiation, flux', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906077', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_2_20.pdf']","['The shell type SNR RXJ1713.7-3946 is a new SNR discovered by the ROSAT all sky survey. Recently, strong non-thermal X-ray emission from the northwest part of the remnant was detected by the ASCA satellite. This synchrotron X-ray emission strongly suggests the existence of electrons with energies up to hundreds of TeV in the remnant. This SNR is, therefore, a good candidate TeV gamma ray source, due to the Inverse Compton scattering of the Cosmic Microwave Background Radiation by the shock accelerated ultra-relativistic electrons, as seen in SN1006. In this paper, we report a preliminary result of TeV gamma-ray observations of the SNR RXJ1713.7-3946 by the CANGAROO 3.8m telescope at Woomera, South Australia.']",['1999-06-07'] +1085,['eng'],"['Mori, M', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, S', 'Hara, T', 'Jinbo, J', 'Kawachi, A', 'Kifune, T', 'Kubo, H', 'Kushida, J', 'Matsubara, Y', 'Mizumoto, Y', 'Moriya, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Sato, Y', 'Susukita, R', 'Tamura, T', 'Tanimori, T', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T', 'Yuki, A']",['Data Acquisition System of the CANGAROO-II Telescope'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'photoelectron, amplifier', 'data acquisition', 'signal processing']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906076', 'http://krusty.physics.utah.edu/~icrc1999/root/vol5/o4_3_31.pdf']",['The data acquisition system for the new CANGAROO-II 7m telescope is described.'],['1999-06-07'] +1086,['eng'],"['Kawachi, A', 'Kushida, J', 'Dazeley, S A', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, S', 'Hara, T', 'Jinbo, J', 'Kifune, T', 'Kubo, H', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Moriya, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Sato, Y', 'Susukita, R', 'Tamura, T', 'Tanimori, T', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T', 'Yuki, A']",['An Optical Reflector for the CANGAROO-II Telescope'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'optics, reflection', 'alignment', 'statistical analysis']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906075', 'http://krusty.physics.utah.edu/~icrc1999/root/vol5/o4_3_05.pdf']","['We have been successful in developing light and durable mirrors made of CFRP (Carbon Fiber Reinforced Plastic) laminates for the reflector of the new CANGAROO-II 7 m telescope. The reflector has a parabolic shape (F/1.1) with a 30 m^2 effective area which consists of 60 small spherical mirrors of CFRP laminates. The orientation of each mirror can be remotely adjusted by stepping motors. After the first adjustment work, the reflector offers a point image of about $0.^\\circ 14$ (FWHM) on the optic axis.']",['1999-06-07'] +1087,['eng'],"['Amendola, L']",['Perturbations in a coupled scalar field cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'field theory, scalar', 'coupling, matter', 'density, perturbation', 'spectra, multipole', 'spectra, perturbation', 'model, acoustic', 'galaxy, cluster', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906073'],"['I analyze the density perturbations in a cosmological model with a scalar field coupled to ordinary matter, such as one obtains in string theory and in conformally transformed scalar-tensor theories. The spectrum of multipoles on the last scattering surface and the power spectrum at the present are compared with observations to derive bounds on the coupling constant and on the exponential potential slope. It is found that the acoustic peaks and the power spectrum are strongly sensitive to the model parameters. The models that best fit the galaxy spectrum and satisfy the cluster abundance test have energy density $\\Omega_{\\phi}\\simeq 0.1$ and a scale factor expansion law $a\\sim t^{p}, p\\simeq 0.68$.']",['1999-06-07'] +1088,['eng'],"['Wieringa, M H', 'Kulkarni, S R', 'Frail, D A']",['SN 1998bw'],['Astrophysics and Astronomy'],"['talk, Rome 1998/11/03', 'supernova', 'shock waves', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, emission', 'flux, density', 'plasma, energy', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906070'],"['SN1998bw shot to fame by claims of association with GRB980425. Independent of its presumed association with a GRB, this SN is unusual in its radio properties. A simple interpretation of the unusually bright radio emission leads us to the conclusion that there are two shocks in this SN: a slow moving shock containing most of the ejecta and a relativistic shock (Gamma=2) which is responsible for the radio emission. This is the first evidence for the existence of relativistic shocks in supernovae. It is quite plausible that this shock may produce high energy emission (at early times and by inverse Compton scattering). As with other supernovae, we expect radio emission at much later times powered primarily by the slow moving ejecta. This expectation has motivated us to continue monitoring this unusual SN.']",['1999-06-04'] +1089,['eng'],"['Perrotta, F', 'Baccigalupi, C', 'Matarrese, S']",['Extended Quintessence'],['Astrophysics and Astronomy'],"['quintessence', 'gravitation, scalar', 'gravitation, tensor', 'gravitation, induced', 'field theory, scalar', 'space-time', 'astrophysics, missing-mass', 'perturbation theory, linear', 'cosmic radiation, background', 'cosmic radiation, polarization', 'temperature, anisotropy', 'effective potential', 'matter, density', 'time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906066'],"[""We study Quintessence cosmologies in the context of scalar-tensor theories of gravity, where a scalar field $\\phi$, assumed to provide most of the cosmic energy density today, is non-minimally coupled to the Ricci curvature scalar $R$. Such `Extended Quintessence' cosmologies have the appealing feature that the same field causing the time (and space) variation of the cosmological constant is the source of a varying Newton's constant à la Jordan-Brans-Dicke. We investigate here two classes of models, where the gravitational sector of the Lagrangian is $F(\\phi)R$ with $F(\\phi )=\\xi\\phi^{2}$ (Induced Gravity, IG) and $F(\\phi)=1+\\xi\\phi^{2}$ (Non-Minimal Coupling, NMC). As a first application of this idea we consider a specific model, where the Quintessence field, $\\phi$, obeying the simplest inverse power potential, has $\\Omega_{\\phi}=0.6$ today, in the context of the Cold Dark Matter scenario, with scale-invariant adiabatic initial perturbations. We find that, if $\\xi\\lesssim 5\\times 10^{-4}$ for IG and $\\xi\\lesssim 5\\times 10^{-3}(\\sqrt{G}\\phi_{0})^{-1}$ for NMC ($\\phi_{0}$ is the present Quintessence value) our Quintessence field satisfies the existing solar system experimental constraints. Using linear perturbation theory we then obtain the polarization and temperature anisotropy spectra of the Cosmic Microwave Background (CMB) as well as the matter power-spectrum. The perturbation behavior possesses distinctive features, that we name `QR-effects', regarding acoustic peak location and height, late time integrated Sachs-Wolfe effect, as well as turnover and amplitude in the matter power spectrum. These features could be detected in the upcoming observations on CMB and large-scale structure.""]",['1999-06-04'] +1090,['eng'],"['Djannati-Ataï, A', 'Piron, F', 'Barrau, A', 'Iacoucci, L', 'Punch, M', 'Tavernet, J P', 'Bazer-Bachi, R', 'Cabot, H', 'Chounet, L M', 'Debiais, G', 'Degrange, B', 'Dezalay, J P', 'Dumora, D', 'Espigat, P', 'Fabre, B', 'Fleury, P', 'Fontaine, G', 'Ghesquière, C', 'Goret, P', 'Gouiffes, C', 'Grenier, I A', 'Le Bohec, S', 'Malet, I', 'Meynadier, C', 'Mohanty, G', 'Nuss, E', 'Paré, E', 'Québert, J', 'Ragan, K', 'Renault, C', 'Rivoal, M', 'Rob, L', 'Schahmaneche, K', 'Smith, D A']",['Very High Energy $\\gamma$-ray spectral properties of Mrk 501 from CAT Cerenkov telescope observations in 1997'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906060'],"['The BL Lac object Mrk 501 went into a very high state of activity during 1997, both in VHE gamma-rays and X-rays. We present here results from observations at energies above 250 GeV carried out between March and October 1997 with the CAT Cerenkov imaging Telescope. The average differential spectrum between 30 GeV and 13 TeV shows significant curvature and is well represented by phi_0 * E_TeV^{-(alpha + beta*log10(E_TeV))}, with: phi_0 = 5.19 +/- 0.13 {stat} +/- 0.12 {sys-MC} +1.66/-1.04 {sys-atm} * 10^-11 /cm^2/s/TeV alpha = 2.24 +/- 0.04 {stat} +/- 0.05 {sys} beta = 0.50 +/- 0.07 {stat} (negligible systematics). The TeV spectral energy distribution of Mrk 501 clearly peaks in the range 500 GeV-1 TeV. Investigation of spectral variations shows a significant hardness-intensity correlation with no measurable effect on the curvature. This can be described as an increase of the peak TeV emission energy with intensity. Simultaneous and quasi-simultaneous CAT VHE gamma-ray and BeppoSAX hard X-ray detections for the highest recorded flare on 16th April and for lower-activity states of the same period show correlated variability with a higher luminosity in X-rays than in gamma-rays. The observed spectral energy distribution and the correlated variability between X-rays and gamma-rays, both in amplitude and in hardening of spectra, favour a two-component emission scheme where the low and high energy components are attributed to synchrotron and inverse Compton (IC) radiation, respectively.']",['1999-06-04'] +1091,['eng'],"['Loinger, A']","['The gravitational waves are fictitious entities, 3']",['Astrophysics and Astronomy'],"['gravitational radiation', 'Einstein equation', 'radiation, electromagnetic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906058'],"[""Only Levi-Civita's electromagnetic interpretation of the characteristic hypersurfaces of Einstein field equations is conceptually correct.""]",['1999-06-04'] +1092,['eng'],"['Hayashida, N', 'Honda, K', 'Inoue, N', 'Kadota, K', 'Kakimoto, F', 'Kakizawa, S', 'Kamata, K', 'Kawaguchi, S', 'Kawasaki, Y', 'Kawasumi, N', 'Kusano, E', 'Matsubara, Y', 'Mase, K', 'Minagawa, T', 'Murakami, K', 'Nagano, M', 'Nishikawa, D', 'Ohoka, H', 'Osone, S', 'Sakaki, N', 'Sasaki, M', 'Sasano, M', 'Shinozaki, K', 'Takeda, M', 'Teshima, M', 'Torii, R', 'Tsushima, I', 'Uchihori, Y', 'Yamamoto, T', 'Yoshida, S', 'Yoshii, H']",['The Anisotropy of Cosmic Ray Arrival Direction around $10^{18} eV$'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08', 'cosmic radiation, anisotropy', 'showers, air', 'particle source, galaxy', 'nucleon, cosmic radiation', 'cosmic radiation, primary', 'shower detector, experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906056', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o1_3_04.pdf']","['Anisotropy in the arrival directions of cosmic rays around 10^{18}eV is studied using data from the Akeno 20 km^2 array and the Akeno Giant Air Shower Array (AGASA), using a total of about 216,000 showers observed over 15 years above 10^{17}eV. In the first harmonic analysis, we have found significant anisotropy of $\\sim$ 4 % around 10^{18}eV, corresponding to a chance probability of $\\sim 10^{-5}$ after taking the number of independent trials into account. With two dimensional analysis in right ascension and declination, this anisotropy is interpreted as an excess of showers near the directions of the Galactic Center and the Cygnus region. This is a clear evidence for the existence of the galactic cosmic ray up to the energy of 10^{18}eV. Primary particle which contribute this anisotropy may be proton or neutron.']",['1999-06-04'] +1093,['eng'],"['Yamamoto, T', 'Chamoto, N', 'Chikawa, M', 'Hayashi, S', 'Hayashida, N', 'Hibino, K', 'Hirasawa, H', 'Honda, K', 'Hotta, N', 'Inoue, N', 'Ishikawa, F', 'Ito, N', 'Kabe, S', 'Kajino, F', 'Kashiwagi, T', 'Kakizawa, S', 'Kawakami, Y', 'Kawasumi, N', 'Kitamura, H', 'Kuramochi, K', 'Kusano, E', 'Loch, E C', 'Mase, K', 'Matsuyama, T', 'Morizane, Y', 'Nishikawa, D', 'Nagano, M', 'Nishimura, J', 'Nishiyama, T', 'Nishizawa, M', 'Ouchi, T', 'Ohoka, H', 'Ohnishi, M', 'Osone, S', 'Saitô, T', 'Sakaki, N', 'Sakata, M', 'Sasano, M', 'Shimodaira, H', 'Shiomi, A', 'Sokolsky, P', 'Takahashi, T', 'Taylor, S F', 'Takeda, M', 'Teshima, M', 'Tsukiji, M', 'Uchihori, Y', 'Yamamoto, Y', 'Yasui, K', 'Yochida, S', 'Yoshii, H', 'Yuda, T', 'Torii, R']",['The energy spectrum of high energy $\\gamma$ rays from Mrk501 by the stereoscopic analysis'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'galaxy, AGN', 'showers, air', 'energy resolution', 'Cherenkov counter, experimental results', 'experimental methods']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906055', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_01.pdf']",['We have developed the energy measurement method which based on stereoscopic observation with multiple telescopes for TeV gamma rays. Energy resolution obtained by this method was 23 %. The energy spectrum of the gamma-ray flares of Markarian 501 in 1997 was also obtained using this techniques. We have confirmed the bending or the cutoff of the energy spectrum around several TeV.'],['1999-06-04'] +1094,['eng'],"['Yamamoto, T', 'Chamoto, N', 'Chikawa, M', 'Hayashi, S', 'Hayashida, N', 'Hibino, K', 'Hirasawa, H', 'Honda, K', 'Hotta, N', 'Inoue, N', 'Ishikawa, F', 'Ito, N', 'Kabe, S', 'Kajino, F', 'Kashiwagi, T', 'Kakizawa, S', 'Kawakami, Y', 'Kawasumi, N', 'Kitamura, H', 'Kuramochi, K', 'Kusano, E', 'Loch, E C', 'Mase, K', 'Matsuyama, T', 'Morizane, Y', 'Nishikawa, D', 'Nagano, M', 'Nishimura, J', 'Nishiyama, T', 'Nishizawa, M', 'Ouchi, T', 'Ohoka, H', 'Ohnishi, M', 'Osone, S', 'Saitô, T', 'Sakaki, N', 'Sakata, M', 'Sasano, M', 'Shimodaira, H', 'Shiomi, A', 'Sokolsky, P', 'Takahashi, T', 'Taylor, S F', 'Takeda, M', 'Teshima, M', 'Tsukiji, M', 'Uchihori, Y', 'Yamamoto, Y', 'Yasui, K', 'Yochida, S', 'Yoshii, H', 'Yuda, T', 'Torii, R']",['TeV $\\gamma$-ray observations from nearby AGNs by Utah Seven Telescope Array'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'galaxy, AGN', 'cosmic radiation, time variation', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906054', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_25.pdf']",['We have investigated TeV gamma-ray emissions from nearby X-ray selected BL Lac objects using the Utah Seven Telescope Array for more than two years. These objects can be considered as potential sources of TeV gamma rays with inverse compton model. The gamma-ray flares from Mrk421 and Mrk501 found in these observation will be reported.'],['1999-06-04'] +1095,['eng'],"['Tavernet, J P']",['VHE Spectral Properties of Mrk 501 with the CAT telescope'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'galaxy, AGN', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906043', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_1_08.pdf']","['We report here observations of the active galactic nucleus Mrk 501, at energies above 250 GeV carried out with the CAT atmospheric imaging telescope from March 1997 to Autumn 1998. This source was in a high state of activity at several different wavelengths in 1997, and the observed flux at TeV energies has been seen to change by a factor of ~ 20 from from 1995 and 1996 fluxes. CAT observations also indicate a curved spectrum at TeV energies, and a correlation between the gamma-ray intensity and the spectral hardness. The temporal variability and the TeV spectral properties are examined.']",['1999-06-03'] +1096,['eng'],"['Musquere, A']",['Search for VHE pulsed emission from the Crab with the CAT Telescope'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'cosmic radiation, flux', 'pulsar', 'Cherenkov counter, imaging', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906042', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_2_05.pdf']","['Since 1996, the CAT experiment, operating at the THEMIS site (French Pyrenees), has been collecting Very High Energy (VHE) gamma-ray data from the Crab. The temporal analysis of photon arrival times folded with the pulsar parameters did not reveal any significant pulsation. The upper limit of a steady pulsed flux over the 102.7 hours of observation is 1.5 10^-12 cm^-2.s^-1, 3.0 10^-13 cm^-2.s^-1 and 5.4 10^-14 cm^-2.s^-1 above 250 GeV, 1 TeV and 5 TeV, respectively. These results put stringent constraints on the models of high energy pulsar electrodynamics.']",['1999-06-03'] +1097,['eng'],[],['Large zenith-angle observations with the CAT Cherenkov imaging telescope'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'radiation, Cherenkov', 'statistical analysis', 'numerical calculations, Monte Carlo']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906041', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_2_03.pdf']","['We present here results from large zenith-angle observations with the CAT atmospheric Cherenkov imaging telescope, based on data taken on the Crab Nebula and on the blazar Mk501 from 1996 onwards. From Monte Carlo simulations, the threshold energy of the telescope is expected to vary from about 250 GeV at zenith to about 2 TeV at a zenith angle of 60 degrees. The lower source-fluxes due to the increased threshold energy are partly compensated for by an increase in the effective collection area at large zenith angles, thus allowing a significant extension of the dynamic range of the CAT telescope, with a tolerable loss in sensitivity. We discuss the implications for source detection and energy spectrum measurements.']",['1999-06-03'] +1098,['eng'],"['Goret, P', 'Gouiffes, C', 'Nuss, E', 'Ellison, D C']",['Search for $\\geq 400 GeV$ $\\gamma$-rays from the SNR Cas A'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'photon, cosmic radiation', 'cosmic radiation, energy', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'upper limit', 'supernova', 'acceleration, shock waves', 'magnetic field', 'Cherenkov counter, imaging', 'experimental results']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906040', 'http://krusty.physics.utah.edu/~icrc1999/root/vol3/o2_2_18.pdf']","['The recent detection of a hard X-ray component in the supernova remnant Cassiopeia A is interpreted as synchrotron emission from electrons accelerated to energies up to 40 TeV (Allen et al., 1997). It is therefore tempting to consider TeV gamma-ray emission from this object through : i) bremsstrahlung and inverse Compton radiation from electrons and/or ii) pi0 production from an associated high energy cosmic ray component hitting surrounding material. Cas A was observed by the CAT imaging Cherenkov telescope during the observing season Aug-Nov 1998. An upper limit to the integral flux above 400 GeV of 0.74x10^-11 gamma.cm^-2.s^-1 is derived. This result is used to constrain shock-acceleration models for production of VHE gamma-rays in SNRs.']",['1999-06-03'] +1099,['eng'],"['Bergström, L', 'Edsjö, J', 'Ullio, P']",['Cosmic antiprotons as a probe for neutralino dark matter?'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'astrophysics, missing-mass', 'neutralino, annihilation', 'anti-p, cosmic radiation', 'cosmic radiation, flux', 'electroweak interaction', 'supersymmetry', 'cosmic radiation, background', 'galaxy', 'numerical calculations']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906034', 'http://krusty.physics.utah.edu/~icrc1999/root/vol2/h5_1_05.pdf']","['The flux of cosmic ray antiprotons from neutralino annihilations in the galactic halo is computed for a large sample of models in the Minimal Supersymmetric extension of the Standard Model. We also revisit the problem of estimating the background of low-energy cosmic ray induced secondary antiprotons, taking into account their subsequent interactions (and energy loss) and the presence of nuclei in the interstellar matter. We point out that in some cases the optimal kinetic energy to search for a signal from supersymmetric dark matter is above several GeV, rather than the traditional sub-GeV region. The large astrophysical uncertainties involved do not allow the exclusion of any of the MSSM models we consider, on the basis of current data.']",['1999-06-03'] +1100,['eng'],"['Bergström, L', 'Edsjö, J', 'Gondolo, P']",['Indirect Detection of Dark Matter in km-size Neutrino Telescopes'],['Astrophysics and Astronomy'],"['talk, Salt Lake City 1999/08/17', 'astrophysics, missing-mass', 'WIMP, search for', 'neutralino, annihilation', 'neutrino, pair production', 'neutrino, counters and detectors', 'muon, flux', 'energy, threshold', 'numerical calculations']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906033', 'http://krusty.physics.utah.edu/~icrc1999/root/vol2/h5_1_04.pdf']","['Neutrino telescopes of kilometer size are currently being planned. They will be two or three orders of magnitude larger than presently operating detectors, but they will have a much higher muon energy threshold. We discuss the trade-off between area and energy threshold for indirect detection of neutralino dark matter captured in the Sun and in the Earth and annihilating into high energy neutrinos. We also study the effect of a higher threshold on the complementarity of different searches for supersymmetric dark matter.']",['1999-06-03'] +1101,['eng'],"['Blandford, R D']",['Acceleration of Ultra High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'cosmic radiation, acceleration', 'cosmic radiation, energy spectrum', 'luminosity, density', 'shock waves', 'black hole', 'galaxy, AGN', 'topology, defect', 'energy, density']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906026'],"[""Some general features of cosmic ray acceleration are summarized along with some inferences that can be drawn concerning the origin of the UHE component. The UHE luminosity density is found to be similar to that derived for GeV cosmic rays and its slope suggests a distinct origin. Reports of clustering on small angular scale, if confirmed, would rule out most proposed source models. More generally, it is argued that the highest energy particles can only be accelerated in sites that can induce an EMF ${\\cal E}\\go3\\times10^{20}$ V and an associated power $L_{min} \\go {\\cal E}^2/Z\\sim10^{39}$ W, where $Z$ is the characteristic, electrical impedance, typically $\\lo100\\Omega$. Shock acceleration, unipolar induction and magnetic flares are the three most potent, observed, acceleration mechanisms and radio jet termination shocks, are the least implausible, ``conventional'' manifestations of these mechanisms that have been invoked to explain the UHE cosmic rays. Each of these models presents problems and deciding between these and ``exotic'' origins for UHE cosmic rays, including those involving new particles or defects will require improved statistical information on the energies, arrival times and directions, as should be provided by the Auger project.""]",['1999-06-02'] +1102,['eng'],"['Lindebaum, R J', 'Tupper, G B', 'Viollier, R D']","['Particle Physics, Astrophysics and Cosmology with Forbidden Neutrinos']",['Astrophysics and Astronomy'],"['talk, Cape Town 1999/01/24', 'neutrino, sterile', 'neutrino/tau, mass', 'neutrino, solar', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'astrophysics, model', 'black hole', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9906004'],"['Astrophysical and cosmological consequences of a standard $\\nu_{\\tau}$ of (15 +- 3) keV/c^{2} mass are discussed in the light of the recent results of the solar, atmospheric and LSND neutrino experiments and theoretical prejudices.']",['1999-06-02'] +1103,['eng'],"['Magueijo, J', 'Baskerville, W K']",['Big Bang riddles and their revelations'],['Astrophysics and Astronomy'],"['astrophysics, model', 'inflationary universe', 'string model', 'photon, velocity']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905393'],"[""We describe how cosmology has converged towards a beautiful model of the Universe: the Big Bang Universe. We praise this model, but show there is a dark side to it. This dark side is usually called ``the cosmological problems'': a set of coincidences and fine tuning features required for the Big Bang Universe to be possible. After reviewing these ``riddles'' we show how they have acted as windows into the very early Universe, revealing new physics and new cosmology just as the Universe came into being. We describe inflation, pre Big Bang, and varying speed of light theories. At the end of the millennium, these proposals are seen respectively as a paradigm, a tentative idea, and outright speculation.""]",['1999-06-01'] +1104,['eng'],"['Chen, X', 'Kamionkowski, M P']",['Cosmic Microwave Background Temperature and Polarization Anisotropy in Brans-Dicke Cosmology'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, spectra', 'temperature, anisotropy', 'polarization, anisotropy', 'Brans-Dicke model', 'Boltzmann equation', 'relativity theory, general', 'astrophysics, model', 'astrophysics, missing-mass', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905368'],"['We develop a formalism for calculating cosmic microwave background (CMB) temperature and polarization anisotropies in cosmological models with Brans-Dicke gravity. We then modify publicly available Boltzmann codes to calculate numerically the temperature and polarization power spectra. Results are illustrated with a few representative models. Comparing with the general-relativistic model with the same cosmological parameters, both the amplitude and the width of the acoustic peaks are different in the Brans-Dicke models. We use a covariance-matrix calculation to investigate whether the effects of Brans-Dicke gravity are degenerate with those of variation in other cosmological parameters and to simultaneously determine whether forthcoming CMB maps might be able to distinguish Brans-Dicke and general-relativistic cosmology. Although the predicted power spectra for plausible Brans-Dicke models differ from those in general relativity only slightly, we find that MAP and/or the Planck Surveyor may in principle provide a test of Brans-Dicke theory that is competitive to solar-system tests. For example, if all other parameters except for the CMB normalization are fixed, a value of the Brans-Dicke parameter omega as large as 500 could be identified with MAP, and for Planck, values as large as omega \\simeq3000 could be identified; these sensitivities are decreased roughly by a factor of 3 if we marginalize over the baryon density, Hubble constant, spectral index, and reionization optical depth. In more general scalar-tensor theories, omega may evolve with time, and in this case, the CMB probe would be complementary to that from solar-system tests.']",['1999-05-28'] +1105,['eng'],"['Chaves, M']",['Cosmic Magnetic Fields Exert Negative Pressure and Act as a Cosmological Constant'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'magnetic field', 'pressure', 'astrophysics, acceleration', 'gauge field theory, Yang-Mills', 'coherence']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905367'],"['Recently there has been mounting evidence for the existence of a cosmological constant (CC). Here we show that cosmic magnetic fields act as a CC, having negative pressure and tending to cause cosmological acceleration. However, if present-day estimates of the intensity of these fields are correct, they would be too weak to be the cause of the acceleration. It is pointed out that large-scale coherent Yang-Mills field structures can also act as a CC.']",['1999-05-28'] +1106,['eng'],"['Magueijo, J', 'Sandvik, H B', 'Steer, D']",['The statistical physics of cosmological networks of string loops'],['Astrophysics and Astronomy'],"['astrophysics, string', 'string, network', 'Boltzmann equation, solution', 'statistical mechanics', 'space-time, Minkowski', 'stability', 'perturbation, nonlinear', 'temperature, Hagedorn', 'astrophysics, model', 'scaling', 'energy, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905363'],"['We solve numerically the Boltzmann equation describing the evolution of a cosmic string network which contains only loops. In Minkowski space time the equilibrium solution predicted by statistical mechanics is recovered, and we prove that this solution is stable to non-linear perturbations provided that their energy does not exceed the critical energy for the Hagedorn transition. In expanding Einstein - de Sitter Universes we probe the distribution of loops with length much smaller than the horizon. For these loops we discover stable scaling solutions both in the radiation and matter dominated epochs. The shape of these solutions is very different in the two eras, with much higher energy density in the radiation epoch, and a larger average loop length in the matter epoch. These results suggest that if the conditions for formation of loop networks are indeed satisfied, these could in principle be good candidates for structure formation.']",['1999-05-28'] +1107,['eng'],"['Cline, David B', 'Matthey, C', 'Otwinowski, Stanislas']",['Study of Very Short $\\gamma$-Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, particle source', 'data analysis method', 'event shape analysis', 'spectra, density', 'space-time, Euclidean', 'black hole', 'transition, quark hadron', 'temperature', 'model, shock waves', 'model, fireball', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905346'],"['We have carried out a detailed study of the morphology of gamma-ray bursts (GRBs) with time duration less than 100 ms that includes: (1) a fast-Fourier spectrum analysis, (2) a comparison with the Stern analysis of longer bursts, (3) an inner comparison of the properties of the short bursts, and (4) a comparison of the short burst properties with the bulk of the GRBs from the Burst and Transient Source Experiment (BATSE) 4B catalogue. We have used the time tagged event (TTE) BATSE 3B data, which is available to the public, for part of the analysis. We show that these bursts are very different from the rest of the GRB events. The short bursts appear to be nearly identical, suggesting a separate class of GRBs. We also show that the short bursts have a Euclidean space-time distribution, in sharp contrast to the longer bursts with Finally we compare the bursts with a model of primordial black hole (PBH) evaporation at the quark-gluon (Q-G) phase transition temperature and other shock wave models.']",['1999-05-27'] +1108,['eng'],"['Fiorentini, G', 'Ricci, B']","['Helioseismology, solar models and solar neutrinos']",['Astrophysics and Astronomy'],"['model, solar', 'validity test', 'neutrino, solar', 'neutrino, flux', 'neutrino, production', 'velocity, acoustic', 'axion', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905341'],"['We review recent advances concerning helioseismology, solar models and solar neutrinos. Particularly we shall address the following points: i) helioseismic tests of recent SSMs; ii)the accuracy of the helioseismic determination of the sound speed near the solar center; iii)predictions of neutrino fluxes based on helioseismology, (almost) independent of SSMs; iv)helioseismic tests of exotic solar models.']",['1999-05-27'] +1109,['eng'],"['Khokhlov, D L']",['Generation of density perturbations due to the birth of baryons'],['Astrophysics and Astronomy'],"['astrophysics, model', 'baryon, production', 'density, perturbation', 'adiabatic', 'spectra, fluctuation', 'cosmic radiation, background', 'baryon, asymmetry']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905339'],['Generation of adiabatic density perturbations from fluctuations caused by the birth of baryons is considered. This is based on the scenario of baryogenesis in which the birth of protons takes place at the temperature equal to the mass of electron.'],['1999-05-27'] +1110,['eng'],"['Melchiorri, A', 'Vernizzi, F', 'Durrer, R', 'Veneziano, Gabriele']",['Cosmic Microwave Background anisotropies and extra dimensions in String Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'string model', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, fluctuation', 'axion', 'higher-dimensional', 'space-time', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905327'],"[""A recently proposed mechanism for large-scale structure in string cosmology --based on massless axionic seeds-- is further analyzed and extended to the acoustic-peak region. Existence, structure, and normalization of the peaks turn out to depend crucially on the overall evolution of extra dimensions during the pre-big bang phase: conversely, precise cosmic microwave background anisotropy data in the acoustic-peak region will provide, within the next decade, a window on string-theory's extra dimensions before their eventual compactification.""]",['1999-05-27'] +1111,['eng'],"['Olive, Keith A', 'Steigman, G', 'Walker, T P']",['Primordial Nucleosynthesis'],['Astrophysics and Astronomy'],"['review', 'astrophysics, model', 'light nucleus, production', 'baryon, density', 'neutrino, flavor', 'deuterium', 'helium', 'lithium', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905320'],"['We review the Cosmology and Physics underlying Primordial Nucleosynthesis and survey current observational data in order to compare the predictions of Big Bang Nucleosynthesis with the inferred primordial abundances. From this comparison we report on the status of the consistency of the standard hot big bang model, we constrain the universal density of baryons (nucleons), and we set limits to the numbers and/or effective interactions of hypothetical new ""light"" particles (equivalent massless neutrinos).']",['1999-05-26'] +1112,['eng'],"['Genreith, H']",['A Black Hole emerged Universe'],['Astrophysics and Astronomy'],"['talk, Bonn 1998/09/22', 'astrophysics, model', 'black hole', 'relativity theory, general', 'quantization', 'entropy', 'particle, mass spectrum', 'electromagnetic interaction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905317'],['A simple model of a universe is presented composed of black holes and black branes. It uses the most simplest approximations and models of General Relativity and Quantum Dynamics to offer an idea of an unification and gives a possible answer to the quantization and entropy of Black Holes. It proposes a mass spectra for elementary particles and gives a vivid interpretation of the particle-wave-dualism.'],['1999-05-26'] +1113,['eng'],"['Dar, Arnon']","['High Energy Cosmic Rays, $\\gamma$ Rays And Neutrinos From Jetted GRBs']",['Astrophysics and Astronomy'],"['talk, Venice 1999/02/23', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'cosmic radiation, energy spectrum', 'jet, relativistic', 'galaxy', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905315'],"['Recent observations suggest that gamma ray bursts (GRBs) and their afterglows are produced in star formation regions in distant galaxies by highly relativistic jets that happen to point in our direction. Relativistic beaming collimates the emission from the highly relativistic jets into small solid angles along the jet direction. It implies that we are seeing only a small fraction of the events that produce GRBs. The observed GRB rate then requires an event rate which is comparable to the birth rate of neutron stars (NS). The highly relativistic jets sweep up ambient matter along their trajectories, accelerate it to cosmic ray (CR) energies and disperse it in hot spots which they form when they stop in the galactic halo. With an event rate comparable to the NS birth rate, such events in our Galaxy may be the main source of Galactic cosmic rays at all energies. Internal interactions and/or external interactions of these jets with high column density matter and/or radiation at their production sites or along their trajectories can produce high energy gamma rays and neutrinos that are highly beamed along the jet direction. Jetted GRBs, like blazars, may be much more fluent in high energy gamma rays and neutrinos than in MeV gamma rays. But, TeV gamma rays from large cosmological distances are unobservable because of their attenuation by electron-positron pair creation on the intergalactic infrared background radiation. However, high energy neutrinos from distant GRBs may be observed with large surface/volume telescopes which are under construction. TeV gamma rays and high energy neutrinos may also be detected from relatively nearby GRBs by the existing moderate size detectors, but with a much smaller rate.']",['1999-05-26'] +1114,['eng'],"['Haungs, A', 'Razdan, A K', 'Bhat, C L', 'Rannot, R C', 'Rebel, H']","['First results on characterization of Cerenkov images through combined use of Hillas, fractal and wavelet parameters']",['Astrophysics and Astronomy'],"['p, cosmic radiation', 'photon, cosmic radiation', 'nucleus, cosmic radiation', 'neon', 'iron', 'showers, air', 'radiation, Cherenkov', 'imaging', 'semiconductor detector, pixel', 'statistical analysis', 'transformation, wavelet']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905312'],"['Based on Monte Carlo simulations using the CORSIKA code, it is shown that Cerenkov images produced by ultrahigh energy $\\gamma$-rays and cosmic ray nuclei (proton, Neon and Iron) are fractal in nature. The resulting multifractal and wavelet moments when employed in association with the conventional Hillas parameters as inputs to a properly-trained artificial neural network are found to provide more efficient primary characterization scheme than the one based on the use of Hillas or fractal parameters alone.']",['1999-05-26'] +1115,['eng'],"['Kluzniak, W']",['Is the Universe transparent to TeV photons?'],['Astrophysics and Astronomy'],"['talk, Venice 1999/02/23', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'invariance, Lorentz', 'photon photon, interaction', 'kinematics', 'electron, pair production', 'dispersion relations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905308'],"['If Lorentz invariance is broken at an energy scale Eq, as has recently been suggested in the context of attempts to quantize gravity, the kinematics of photon-photon collisions would be profoundly affected at lower energies. Specifically, electron-positron pair creation on soft photons may be forbidden at photon energies as low as 30 TeV times square root of (Eq/10**17 GeV) and the Universe would then be transparent to high energy photons. The proposition that Lorentz invariance is broken may be falsified by the techniques of TeV astronomy.']",['1999-05-26'] +1116,['eng'],"['Jacobson, T']",['Primordial black hole evolution in tensor-scalar cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'black hole, mass', 'field theory, scalar', 'field theory, tensor', 'black hole, horizon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905303'],"['A perturbative analysis shows that black holes do not remember the value of the scalar field $\\phi$ at the time they formed if $\\phi$ changes in tensor-scalar cosmology. Moreover, even when the black hole mass in the Einstein frame is approximately unaffected by the changing of $\\phi$, in the Jordan-Fierz frame the mass increases. This mass increase requires a reanalysis of the evaporation of primordial black holes in tensor-scalar cosmology. It also implies that there could have been a significant magnification of the (Jordan-Fierz frame) mass of primordial black holes.']",['1999-05-25'] +1117,['eng'],"['Moskalenko, I V', 'Strong, A W']",['Positrons from particle dark-matter annihilation in the Galactic halo'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'annihilation, missing-mass', 'galaxy', 'positron, propagator', 'positron, cosmic radiation', 'positron, flux', 'nucleon, cosmic radiation', 'neutralino', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905283'],"[""We have made a calculation of the propagation of positrons from dark-matter particle annihilation in the Galactic halo in different models of the dark matter halo distribution using our 3D code, and present fits to our numerical propagation Green's functions. We show that the Green's functions are not very sensitive to the dark matter distribution for the same local dark matter energy density. We compare our predictions with computed cosmic ray positron spectra (``background'') for the ``conventional'' CR nucleon spectrum which matches the local measurements, and a modified spectrum which respects the limits imposed by measurements of diffuse Galactic gamma-rays, antiprotons, and positrons. We conclude that significant detection of a dark matter signal requires favourable conditions and precise measurements unless the dark matter is clumpy which would produce a stronger signal. Although our conclusion qualitatively agrees with that of previous authors, it is based on a more realistic model of particle propagation and thus reduces the scope for future speculations. Reliable background evaluation requires new accurate positron measurements and further developments in modelling production and propagation of cosmic ray species in the Galaxy.""]",['1999-05-24'] +1118,['eng'],"['Laming, J M']",['Neutrino Induced Electrostatic Waves in Degenerate Electron Plasmas'],['Astrophysics and Astronomy'],"['electron, plasma', 'neutrino, cosmic radiation', 'neutrino electron, interaction', 'shock waves, electrostatic', 'statistical mechanics', 'supernova', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905268'],"['The plasma theory of electrostatic waves generated collisionlessly when neutrinos pass through degenerate electrons is developed. It is consistent with the results of calculations using quantum statistical field theory in the degenerate limit for kinetic instabilities, and using this formalism reactive instabilities may also be treated. For all neutrino distribution functions that might be appropriate to the neutrino burst during a core collapse supernova, no significant wave growth is found for non-magnetic electrostatic waves. It is speculated that this situation might be different for magnetic fields approaching the values believed to be present on magnetars.']",['1999-05-21'] +1119,['eng'],"['Khokhlov, D L']",['Neutrino flux from the sun in the fractal universe'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'fractals', 'boron', 'beryllium', 'neutrino, capture', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905266'],['The neutrino flux from the sun is estimated within the framework of the fractal universe with a power index of 2. The obtained value of the neutrino flux may provide a solution for the solar neutrino puzzle.'],['1999-05-21'] +1120,['eng'],"['Shi, X', 'Fuller, G M', 'Abazajian, K N']",['Neutrino-Mixing-Generated Lepton Asymmetry and the Primordial $^{4}He$ Abundance'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino/e, asymmetry', 'neutrino, oscillation', 'helium, nuclide', 'helium, yield', 'light nucleus, production', 'neutrino, mixing angle', 'neutrino, sterile', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905259'],"['It has been proposed that an asymmetry in the electron neutrino sector may be generated by resonant active-sterile neutrino transformations during Big Bang Nucleosynthesis (BBN). We calculate the change in the primordial $^4$He yield $Y$ resulting from this asymmetry, taking into account both the time evolution of the $\\nu_e$ and $\\bar\\nu_e$ distribution function and the spectral distortions in these. We calculate this change in two schemes: (1) a lepton asymmetry directly generated by $\\nu_e$ mixing with a lighter right-handed sterile neutrino $\\nu_s$; and (2) a lepton asymmetry generated by a which is subsequently partially converted to an asymmetry in the transformation. In the first scheme, we find that the percentage change in $Y$ is between -1% and 9% (with the sign depending on the sign of the asymmetry), bounded by the Majorana mass limit $m_{\\nu_e}\\la 1$ eV. In the second scheme, the maximal percentage reduction in $Y$ is 2%, if the lepton number asymmetry in neutrinos is positive; Otherwise, the percentage increase in $Y$ is $\\la 5%$ for $m^2_{\\nu_\\mu,\\nu_\\tau}-m^2_{\\nu_s}\\la 10^4$ eV. We conclude that the change in the primordial $^4$He yield induced by a neutrino-mixing-generated lepton number asymmetry can be substantial in the upward direction, but limited in the downward direction.']",['1999-05-21'] +1121,['eng'],"['Hagmann, C']",['Cosmic neutrinos and their detection'],['Astrophysics and Astronomy'],"['talk, Los Angeles 1999/01/05', 'neutrino, cosmic radiation', 'particle identification', 'counters and detectors, torsion', 'background', 'angular resolution', 'stability', 'RF system', 'experimental equipment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905258'],"[""The standard Big-Bang theory predicts a cosmic neutrino background with an average number density of $\\sim 100/cm^3$ per flavor. The most promising way of its detection is measuring the feeble ``neutrino wind'' forces exerted on macroscopic targets. The expected acceleration is $\\sim 10^{-23} cm/s^2$ for Dirac neutrinos with a local number density $\\sim 10^7/cm^3$. A novel torsion balance design is presented, which addresses the sensitivity-limiting factors of existing balances, such as seismic and thermal noise, and angular readout resolution and stability.""]",['1999-05-21'] +1122,['eng'],"['Freedman, W L']",['Determination of Cosmological Parameters'],['Astrophysics and Astronomy'],"['review, Enkoeping 1998/08/20', 'astrophysics, fundamental constant', 'matter, density', 'vacuum state, energy', 'Hubble constant', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'supernova', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905222'],"['Rapid progress has been made recently toward the measurement of cosmological parameters. Still, there are areas remaining where future progress will be relatively slow and difficult, and where further attention is needed. In this review, the status of measurements of the matter density, the vacuum energy density or cosmological constant, the Hubble constant, and ages of the oldest measured objects are summarized. Many recent, independent dynamical measurements are yielding a low value for the matter density of about 1/3 the critical density. New evidence from type Ia supernovae suggests that the vacuum energy density may be non-zero. Many recent Hubble constant measurements appear to be converging in the range of 65-75 km/sec/Mpc. Eliminating systematic errors lies at the heart of accurate measurements for all of these parameters; as a result, a wide range of cosmological parameter space is currently still open. Fortunately, the prospects for accurately measuring cosmological parameters continue to increase.']",['1999-05-19'] +1123,['eng'],"['Sciutto, S J']",['Air Shower Simulations with the AIRES System'],['Astrophysics and Astronomy'],"['showers, air', 'cosmic radiation, spatial distribution', 'photon', 'electron', 'muon', 'numerical calculations, Monte Carlo']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905185', 'http://krusty.physics.utah.edu/~icrc1999/root/vol1/h2_5_02.pdf']",['A report on the characteristics of ultra-high energy air showers simulated with the AIRES program is presented. The AIRES system includes a fast simulating program which is an improved version of the well-known MOCCA program. The AIRES algorithms are briefly described and a series of results coming from the simulations are analyzed.'],['1999-05-17'] +1124,['eng'],"['Mücke, A', 'Rachen, J P', 'Engel, R', 'Protheroe, R J', 'Stanev, T']",['Photomeson production in astrophysical sources'],['Astrophysics and Astronomy'],"['talk, Paris 1998/12/14', 'photon, cosmic radiation', 'galaxy, AGN', 'photon hadron, interaction', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'neutrino, energy spectrum', 'n, energy spectrum', 'antibaryon, photoproduction', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905153'],"['Photomeson production is the main energy loss for relativistic nucleons in dense radiation fields like the cosmic microwave background and the radiation fields in Gamma Ray Bursts (GRB) and jets of Active Galactic Nuclei (AGN). In this paper we study photomeson production in typical GRB and AGN jet radiation fields by using the recently developed Monte Carlo event generator SOPHIA (see these proceedings). We discuss processes that are relevant for the physics of cosmic ray acceleration and the production of neutrinos and gamma rays. We compare our results with widely used approximations, and find significant deviations, particularly for GRBs. The photoproduction of antibaryons as a so far not considered effect in astrophysics is briefly discussed.']",['1999-05-14'] +1125,['eng'],"['Burrows, A', 'Young, T', 'Pinto, P A', 'Eastman, R', 'Thompson, T']",['Supernova Neutrinos and a New Algorithm for Neutrino Transport'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, cosmic radiation', 'transport theory, time dependence', 'neutrino, particle source', 'nucleon nucleon, bremsstrahlung', 'n, matter', 'angular distribution', 'phase space, density', 'neutrino, absorption', 'velocity', 'neutrino nucleon, interaction', 'effect, recoil', 'electron positron, annihilation', 'luminosity', 'numerical methods', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905132'],"['We have developed a new implicit, multi-group, time-dependent, spherical neutrino transport algorithm based on the Feautrier variables, the tangent-ray method, and accelerated ${\\bf \\Lambda}$ iteration. The code achieves high angular resolution, is conceptually equivalent to a Boltzmann solver (without redshifts), and solves the transport equation exactly at all optical depths. We summarize and review the neutrino physics of stellar collapse and supernovae and our formulation of the relevant microphysics. In addition, we derive various useful expressions for neutrino source strengths, including those for nucleon-nucleon bremsstrahlung. With this code, we study character of protoneutron star atmospheres for snapshot post-bounce models, with particular emphasis on their spectra, Eddington factors and angular distributions, phase-space occupancies, and neutrino-matter heating rates. Concerning the latter, we explore the influence of final-state electron blocking, stimulated absorption, velocity terms in the transport equation, neutrino-nucleon scattering asymmetry, and weak magnetism and recoil effects. We also investigate the physical determinants of the $\\nu_{\\mu}$ spectra that emerge from supernova cores and the neutrino heating rates in post-explosion protoneutron star winds. These studies are in preparation for new calculations of spherically symmetric core-collapse supernovae, protoneutron star winds, and neutrino signals, but are also meant to establish a high-accuracy benchmark for future studies of the neutrino atmospheres of evolving protoneutron stars.']",['1999-05-13'] +1126,['eng'],"['Lehner, M J', 'Griest, K', 'Martoff, C J', 'Masek, G E', 'Ohnuki, T', 'Snowden-Ifft, D P', 'Spooner, N J C']",['The DRIFT Project'],['Astrophysics and Astronomy'],"['WIMP, search for', 'drift chamber, time projection', 'xenon', 'carbon, sulfur', 'nucleus, recoil']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905074'],"['A low pressure time projection chamber for the detection of WIMPs is discussed. Discrimination against Compton electron background in such a device should be very good, and directional information about the recoil atoms would be obtainable. If a full 3-D reconstruction of the recoil tracks can be achieved, Monte Carlo studies indicate that a WIMP signal could be identified with high confidence from as few as 30 detected WIMP-nucleus scattering events.']",['1999-05-07'] +1127,['eng'],"['Vasilev, V']",['Flux Sensitivity of VERITAS'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'photon, cosmic radiation', 'galaxy', 'supernova', 'Cherenkov counter, imaging', 'photon, flux']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905044'],"['VERITAS is a new major ground-based gamma-ray observatory with an array of seven 10 m optical reflectors to be built at the Whipple Observatory in southern Arizona, USA. It will consist of an array of imaging Cherenkov telescopes designed to conduct critical measurements of AGNs and SNRs in the energy range of 50 GeV - 50 TeV. The design of the array has been optimized for the highest sensitivity to point sources in the 100 GeV - 10 TeV band when the stereoscopic imaging technique is employed. Maximum versatility of the array has been another major optimization criterion. We present the flux sensitivity of the baseline VERITAS configuration.']",['1999-05-06'] +1128,['eng'],"['Brax, P', 'Martín, J']",['Quintessence and Supergravity'],['Astrophysics and Astronomy'],"['quintessence', 'supergravity', 'potential, scalar', 'astrophysics, density', 'potential, Kaehler']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905040'],"['In the context of quintessence, the concept of tracking solutions allows to address the fine-tuning and coincidence problems. When the field is on tracks today, one has $Q\\approx m_{Pl}$ demonstrating that, generically, any realistic model of quintessence must be based on supergravity. We construct the most simple model for which the scalar potential is positive. The scalar potential deduced from the supergravity model has the form $V(Q)=\\frac{\\Lambda^{4+\\alpha}}{Q^{\\alpha}}e^{\\kappa/2 Q^2}$. We show that despite the appearence of positive powers of the field, the coincidence problem is still solved. If $\\alpha \\ge 11$, the fine-tuning problem can be overcome. Moreover, due to the presence of the exponential term, the value of the equation of state, $\\omega_Q$, is pushed towards the value -1 in contrast to the usual case for which it is difficult to go beyond $\\omega_Q\\approx -0.7$. For $\\Omega_m \\approx 0.3$, the model presented here predicts $\\omega_Q \\approx -0.77$. Finally, we establish the $\\Omega_m-\\omega_Q$ relation for this model.']",['1999-05-06'] +1129,['eng'],"['Aharonian, F A']",['Observations of Mkn 421 during 1997 and 1998 in the energy range above 500 GeV with the HEGRA stereoscopic Cherenkov telescope system'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation', 'Cherenkov counter, imaging', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905032'],"['Since its commissioning in fall 1996, the stereoscopic system of Imaging Atmospheric Cherenkov Telescope (IACTs) of HEGRA with an energy threshold of 500 GeV, an angular resolution of 0.1 degree and an energy resolution of 20% per individual photon, and an energy flux sensitivity nu F_nu at 1 TeV of 1E-11erg/cm**2 s (S/N = 5 sigma) for one hour of observation time has been used to monitor the BL Lac object Mkn 421 on a regular basis. In this letter, we report detailed temporal and spectral information about the TeV characteristics of Mkn 421 in 1997 and 1998. We study the light curve, the shortest time scales of flux variability, the differential spectra on diurnal basis for several days with good gamma-ray statistics and the time averaged energy spectrum. Special emphasis will be put on presenting the data taken during the world-wide April 1997 multiwavelength campaign. We compare the Mkn 421 results with the results obtained for the BL Lac object Mkn 501 and discuss possible implications for the emission mechanism and the Diffuse Intergalactic Background Radiation.']",['1999-05-06'] +1130,['eng'],"['Drell, P S', 'Loredo, T J', 'Wasserman, I M']","['Type Ia Supernovae, Evolution and the Cosmological Constant']",['Astrophysics and Astronomy'],"['supernova', 'matter, density', 'astrophysics, fundamental constant', 'statistics', 'luminosity, dependence', 'data analysis method', 'astrophysics, model', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905027'],"['We explore the possible role of evolution in the analysis of data on SNe Ia at cosmological distances. First, using a variety of simple sleuthing techniques, we find evidence that the properties of the high and low redshift SNe Ia observed so far differ from one another. Next, we examine the effects of including simple phenomenological models for evolution in the analysis. The result is that cosmological models and evolution are highly degenerate with one another, so that the incorporation of even very simple models for evolution makes it virtually impossible to pin down the values of $\\Omega_M$ and cosmological constant, respectively. Moreover, we show that if SNe Ia evolve with time, but evolution is neglected in analyzing data, then, given enough SNe Ia, the analysis hones in on values of $\\Omega_M$ and $\\Omega_\\Lambda$ which are incorrect. Using Bayesian methods, we show that the probability that the cosmological constant is nonzero (rather than zero) is unchanged by the SNe Ia data when one accounts for the possibility of evolution, provided that we do not discriminate among open, closed and flat cosmologies a priori. The case for nonzero cosmological constant is stronger if the Universe is presumed to be flat, but still depends sensitively on the degree to which the peak luminosities of SNe Ia evolve as a function of redshift.']",['1999-05-05'] +1131,['eng'],"['Matos, T']",['From Strings Theory to the Dark Matter in Galaxies'],['Astrophysics and Astronomy'],"['talk, Oaxaca de Juarez 1998/11/20', 'string model', 'effective action', 'field equations, solution', 'velocity, galaxy', 'astrophysics, missing-mass', 'energy, density', 'dilaton', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905024'],"['Starting from the effective action of the low energy limit of superstrings theory, I find an exact solution of the field equations which geodesics behavie exactly as the trajectories of stars arround of a spiral galaxy. Here dark matter is of dilatonic origin. It is remarkable that the energy density of this space-time is the same as the used by astronomers to model galaxy stability. Some remarks about a universe dominated by dilatons are pointed out.']",['1999-05-05'] +1132,['eng'],"['Meng, X H']",['Particle Physics Inflation Model Constrained from Astrophysics Observations'],['Astrophysics and Astronomy'],"['inflationary universe, hybrid', 'potential, inflaton', 'mass, inflaton', 'spectra, perturbation', 'cosmic radiation, background', 'coupling constant', 'supersymmetry']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905017'],"[""The early Universe inflation\\cite{guth} is well known as a promising theory to explain the origin of large scale structure of the Universe, a causal theory for the origin of primordial density fluctuations which may explain the observed density inhomogeneities and cosmic microwave fluctuations in the very early Universe, and to solve the early universe pressing problems for the standard hot big bang theory\\cite{tur}. For a resonable inflation model, the potential during inflation must be very flat in, at least, the direction of the inflaton. To construct a resonable inflation model, or the inflaton potential, all the known related astrophysics observations should be included. For a general tree-level hybrid inflation potential, which is not discussed fully so far for the quartic term, the parameters in it are shown how to be constrained via the astrophysics data observed and to be obtained to the expected accuracy by the soon lauched MAP and PLANCK satellite missions\\cite{mp}, as well as the consistent cosmology requirements. We find the effective inflaton mass parameter is in the TeV range, and the quartic term's self-coupling constant tiny, needs fine-tunning.""]",['1999-05-05'] +1133,['eng'],"['Pal, S', 'Hanauske, M', 'Zakout, I', 'Stöcker, H', 'Greiner, W']",['Neutron star properties in the quark-meson coupling model'],['Astrophysics and Astronomy'],"['n, matter', 'baryon, density', 'hyperon', 'bag model', 'coupling, (meson quark)', 'mean field approximation, relativistic', 'strange meson', 'field theory, scalar', 'quark, strangeness', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9905010'],"['The effects of internal quark structure of baryons on the composition and structure of neutron star matter with hyperons are investigated in the quark-meson coupling (QMC) model. The QMC model is based on mean-field description of nonoverlapping spherical bags bound by self-consistent exchange of scalar and vector mesons. The predictions of this model are compared with quantum hadrodynamic (QHD) model calibrated to reproduce identical nuclear matter saturation properties. By employing a density dependent bag constant through direct coupling to the scalar field, the QMC model is found to exhibit identical properties as QHD near saturation density. Furthermore, this modified QMC model provides well-behaved and continuous solutions at high densities relevant to the core of neutron stars. Two additional strange mesons are introduced which couple only to the strange quark in the QMC model and to the hyperons in the QHD model. The constitution and structure of stars with hyperons in the QMC and QHD models reveal interesting differences. This suggests the importance of quark structure effects in the baryons at high densities.']",['1999-05-04'] +1134,['eng'],"['Kamionkowski, M P']",['The Case of the Curved Universe'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'inflationary universe', 'cosmic radiation', 'space-time', 'proposed experiment', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806347'],"['This is a short article on inflation, the geometry of the Universe, and the cosmic microwave background that appeared as a Perspective in Science magazine.']",['1998-06-26'] +1135,['eng'],"['Peebles, P J E', 'Vilenkin, A']",['Noninteracting dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'matter, density', 'cosmic radiation, background', 'cosmic radiation, fluctuation', 'inflationary universe', 'quintessence', 'field theory, scalar', 'gravitation', 'space-time, de Sitter', 'statistics', 'correlation function', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904396'],"['Since an acceptable dark matter candidate may interact only weakly with ordinary matter and radiation, it is of interest to consider the limiting case where the dark matter interacts only with gravity and itself, the matter originating by the gravitational particle production at the end of inflation. We use the bounds on the present dark mass density and the measured large-scale fluctuations in the thermal cosmic background radiation to constrain the two parameters in a self-interaction potential that is a sum of quadratic and quartic terms in a single scalar dark matter field that is minimally coupled to gravity. In quintessential inflation, where the temperature at the end of inflation is relatively low, the field starts acting like cold dark matter relatively late, shortly before the epoch of equal mass densities in matter and radiation. This could have observable consequences for galaxy formation. We respond to recent criticisms of the quintessential inflation scenario, since these issues also apply to elements of the noninteracting dark matter picture.']",['1999-04-29'] +1136,['eng'],"['Karle, A']",['Observation of Atmospheric Neutrino Events with the AMANDA Experiment'],['Astrophysics and Astronomy'],"['talk, Cape Town 1999/01/24', 'neutrino, cosmic radiation', 'neutrino nucleon, interaction', 'charged current', 'muon, angular distribution', 'background', 'deep underground detector, AMANDA', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904379'],['A first analysis of the AMANDA-B 10-string array data is presented. A total of 113 days of data from its first year of operation in 1997 have been analyzed. High energy neutrinos generate upward moving muons. Cosmic ray muons penetrating the ice sheet to a depth of 2000 m are the major source of background. We discuss the method used to reject the background of approximately 0.5*10^9 downgoing muons and leave 17 upward going events. The neutrino candidates are discussed and compared with expectations.'],['1999-04-28'] +1137,['eng'],"['Christensson, M', 'Hindmarsh, M B']",['Magnetic fields in the early universe in the string approach to MHD'],['Astrophysics and Astronomy'],"['astrophysics', 'string, network', 'magnetic field', 'model, hydrodynamical', 'flux tube, magnetic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904358'],"['There is a reformulation of magnetohydrodynamics in which the fundamental dynamical quantities are the positions and velocities of the lines of magnetic flux in the plasma, which turn out to obey equations of motion very much like ideal strings. We use this approach to study the evolution of a primordial magnetic field generated during the radiation-dominated era in the early Universe. Causality dictates that the field lines form a tangled random network, and the string-like equations of motion, plus the assumption of perfect reconnection, inevitably lead to a self-similar solution for the magnetic field power spectrum. We present the predicted form of the power spectrum, and discuss insights gained from the string approximation, in particular the implications for the existence or not of an inverse cascade.']",['1999-04-27'] +1138,['eng'],"['Vogel, P']",['What might we learn from a future supernova neutrino signal?'],['Astrophysics and Astronomy'],"['talk, Venice 1999/02/23', 'supernova', 'neutrino, cosmic radiation', 'neutral current', 'charged current', 'neutrino/tau, mass', 'neutrino/mu, mass', 'time delay', 'neutrino, interaction', 'channel cross section, energy dependence', 'deep underground detector, experimental methods', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904338'],"['Neutrinos from a future Galactic supernova will be detected by several large underground detectors, in particular by SuperKamiokande (SK) and the Sudbury Neutrino Observatory (SNO). If, as expected, the $\\nu_{\\mu}$ and $\\nu_{\\tau}$ neutrinos have somewhat higher energy on average that the electron neutrinos, they will dominate the neutral current response. The ways to separate the neutral and charged current signals will be discussed, and the best strategy to measure the possible time delay of the neutral current events will be outlined. Given the expected count rates, one will be able to measure in this way the Another application to be discussed is the supernova localization by the neutrino signal, prior to or independently of the electromagnetic signal. The accuracy with which this can be accomplished using the angular distributions of the reactions will be estimated. With two or more detectors one can, in principle, attempt triangulation based on the arrival time of the neutrinos. It will be argued that for realistic parameters this method will be very difficult and likely leads only to crude localization.']",['1999-04-26'] +1139,['eng'],"['Vernetto, S']",['Detection of $\\gamma$-Ray Bursts in the 1 GeV/1 TeV Energy Range by Ground-Based Experiments'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, measurement', 'cosmic radiation, primary', 'showers, air', 'charged particle, cosmic radiation', 'cosmic radiation, secondary radiation', 'signal processing', 'experimental methods, proposed', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904324'],"['Ground based experiments as extensive air showers can observe 1-1000 GeV GRBs using the ""single particle"" techique. The sensitivity to detect a GRB as a function of the burst parameters and the detector characteristics are discussed. The rate of possible observations is evaluated, making reasonable assumptions on the high energy emission, the absorbtion of gamma-rays in the intergalactic space, the distribution of the sources in the universe and the bursts luminosity function. We show that a large area detector located at high mountain altitude has good prospects for positive detections, providing useful informations on the high energy components of GRBs.']",['1999-04-26'] +1140,['eng'],"['Rosenberg, D E']","['Quintessence, Quantum Gravity and the Big Bang']",['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'black hole, rotator', 'density, perturbation', 'energy loss', 'cosmic radiation, background', 'quantum gravity', 'quintessence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904320'],"['A 160 MeV bounce model is utilized for the big bang. In order to prevent a singularity, an energy sink is postulated as the correction to general relativity for quantum gravity. Evidence is presented that quintessence is the net result of quantum gravity applied both to black holes and the universe.']",['1999-04-26'] +1141,['eng'],"['Blanco-Pillado, J J', 'Olum, K D']",['Monopole-antimonopole bound states as a source of ultra-high-energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'bound state, magnetic monopole', 'critical phenomena', 'bound state, decay', 'bound state, annihilation', 'gravitational radiation', 'string model', 'density, upper limit']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904315'],"['The electromagnetic decay and final annihilation of magnetic monopole-antimonopole pairs formed in the early universe has been proposed as a possible mechanism to produce the highest energy cosmic rays. We show that for a monopole abundance saturating the Parker limit, the density of magnetic monopolonium formed is many orders of magnitude less than that required to explain the observed cosmic ray flux. We then propose a different scenario in which the monopoles and antimonopoles are connected by strings formed at a low energy phase transition (~ 100 GeV). The bound states decay by gravitational radiation, with lifetimes comparable with the age of the universe. This mechanism avoids the problems of the standard monopolonium scenario, since the binding of monopoles and antimonopoles is perfectly efficient.']",['1999-04-23'] +1142,['eng'],"['Cardenas, V H', 'Palma, G M']",['Some Remarks on Oscillating Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'model, oscillation', 'field theory, scalar', 'spectra, perturbation', 'energy, density', 'potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904313'],"['In a recent paper Damour and Mukhanov describe a scenario where inflation may continue during the oscillatory phase. This effect is possible because the scalar field spends a significant fraction of each period f oscillation on the upper part of the potential. Such additional period of inflation could push perturbations after the slow roll regime to observable scales. Although we show that the small region of the Damour-Mukhanov parameter q gives the main contribution to oscillating inflation, it remained until now not satisfactory understood. Further, it drives to an expression for the energy density spectrum of perturbations, which is well behaved in the whole physical range of q .']",['1999-04-23'] +1143,['eng'],"['Copeland, E J', 'Mazumdar, A', 'Nunes, N J']",['Generalized Assisted Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'potential', 'supergravity']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904309'],"['We obtain a new class of exact cosmological solutions for multi-scalar fields with exponential potentials. We generalize the assisted inflation solutions previously obtained, and demonstrate how they are modified when there exist cross-couplings between the fields, such as occur in supergravity inspired cosmological models.']",['1999-04-23'] +1144,['eng'],"['Khokhlov, D L']",['Improved scenario of baryogenesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'baryon, production', 'plasma', 'electron p, symmetry', 'interference, (particle antiparticle)', 'p, neutral particle', 'electron, neutral particle', 'electron electron, annihilation', 'photon, electroproduction']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904306'],"['It is assumed that, in the primordial plasma, at the temperatures above the mass of electron, fermions are in the neutral state being the superposition of particle and antiparticle. There exists neutral proton-electron symmetry. Proton-electron equilibrium is defined by the proton-electron mass difference. At the temperature equal to the mass of electron, pairs of neutral electrons annihilate into photons, and pairs of neutral protons and electrons survive as protons and electrons.']",['1999-04-23'] +1145,['eng'],"['Ehrlich, R']",['Is there a 4.5 PeV neutron line in the cosmic ray spectrum?'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'n, cosmic radiation', 'n, flux', 'neutrino/e, tachyon', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904290'],['Recently we presented a model to fit the cosmic ray spectrum using the hypothesis that the electron neutrino is a tachyon. The model predicted the existence of a neutron flux in the cosmic rays in a narrow region centered on $E = 4.5 \\pm 2.2$ PeV. The published literature on Cygnus X-3 reveals just such a $6\\sigma$ spike of neutral particles centered on E = 4.5 PeV. A second prediction of the model concerning integrated neutron fluxes at several energies also is consistent with published data. A specific further test of the model is proposed.'],['1999-04-22'] +1146,['eng'],"['Antoni, T', 'Hörandel, J R']",['Test of high-energy interaction models using the hadronic core of EAS'],['Astrophysics and Astronomy'],"['showers, air', 'hadron, density', 'hadron, interaction', 'cosmic radiation, energy spectrum', 'hadron, spatial distribution', 'showers, hadronic', 'muon, showers', 'calorimeter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904287'],"['Using the large hadron calorimeter of the KASCADE experiment, hadronic cores of extensive air showers have been studied. The hadron lateral and energy distributions have been investigated in order to study the reliability of the shower simulation program CORSIKA with respect to particle transport, decays, treatment of low-energy particles, etc. A good description of the data has been found at large distances from the shower core for several interaction models. The inner part of the hadron distribution, on the other hand, reveals pronounced differences among interaction models. Several hadronic observables are compared with CORSIKA simulations using the QGSJET, VENUS and SIBYLL models. QGSJET reproduces the hadronic distributions best. At the highest energy, in the 10 PeV region, however, none of these models can describe the experimental data satisfactorily. The expected number of hadrons in a shower is too large compared to the observed number, when the data are classified according to the muonic shower size.']",['1999-04-22'] +1147,['eng'],"['Cooray, A R']",['Weighing Neutrinos'],['Astrophysics and Astronomy'],"['neutrino, mass', 'gravitation, lens', 'cosmic radiation, background', 'astrophysics, missing-mass', 'numerical calculations', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904246'],"['We study the possibility for a measurement of neutrino mass using weak gravitational lensing. The presence of non-zero mass neutrinos leads to a suppression of power at small scales and reduces the expected weak lensing signal. The measurement of such a suppression in the weak lensing power spectrum allows a direct measurement of the neutrino mass, in contrast to various other experiments which only allow mass splittings between two neutrino species. Making reasonable assumptions on the accuracy of cosmological parameters, we suggest that a weak lensing survey of 100 sqr. degrees can be easily used to detect neutrinos down to a mass limit of 3.5 eV at the 2 sigma level. This limit is lower than current limits on neutrino mass, such as from the Ly-alpha forest and SN1987A. An ultimate weak lensing survey of pi steradians down to a magnitude limit of 25 can be used to detect neutrinos down to a mass limit of 0.4 eV at the 2 sigma level, provided that other cosmological parameters will be known to an accuracy expected from cosmic microwave background spectrum using the MAP satellite. For much smaller surveys (10 sqr. degrees) that are likely to be first available in the near future with several wide-field cameras, the presence of neutrinos can be safely ignored when deriving conventional cosmological parameters such as the mass density of the Universe. However, armed with cosmological parameter estimates with other techniques, even such small area surveys allow a strong possibility to investigate the presence of non-zero mass neutrinos.']",['1999-04-20'] +1148,['eng'],"['Hofmann, W', 'Jung, I', 'Konopelko, A K', 'Krawczynski, H', 'Lampeitl, H', 'Pühlhofer, G']",['Comparison of techniques to reconstruct VHE $\\gamma$-ray showers from multiple stereoscopic Cherenkov images'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'Cherenkov counter, imaging', 'angular resolution']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904234'],"['For air showers observed simultaneously by more than two imaging atmospheric Cherenkov telescopes, the shower geometry is overconstrained by the images and image information should be combined taking into account the quality of the images. Different algorithms are discussed and tested experimentally using data obtained from observations of Mkn 501 with the HEGRA IACT system. Most of these algorithms provide an estimate of the accuracy of the reconstruction of shower geometry on an event-by-event basis, allowing, e.g., to select higher-quality subsamples for precision measurements.']",['1999-04-20'] +1149,['eng'],"['Bucher, M', 'Moodley, K', 'Turok, Neil G']",['The General Primordial Cosmic Perturbation'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'density, perturbation', 'ratio, (neutrino photon)', 'photon baryon, plasma', 'neutrino, fluid', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904231'],"['We consider the most general primordial cosmological perturbation in a universe filled with photons, baryons, neutrinos, and a hypothetical cold dark matter (CDM) component within the framework of linearized perturbation theory. We give a careful discussion of the different allowed modes, distinguishing modes which are regular at early times, singular at early times, or pure gauge. As well as the familiar growing and decaying adiabatic modes and the baryonic and CDM isocurvature modes we identify two {\\it neutrino isocurvature} modes which do not seem to have been discussed before. In the first, the ratio of neutrinos to photons varies spatially but the net density perturbation vanishes. In the second the photon-baryon plasma and the neutrino fluid have a spatially varying relative bulk velocity, balanced so that the net momentum density vanishes. Possible mechanisms which could generate the two neutrino isocurvature modes are discussed. If one allows the most general regular primordial perturbation, all quadratic correlators of observables such as the microwave background anisotropy and matter perturbations are completely determined by a 5x5, real, symmetric matrix-valued function of co-moving wavenumber. In a companion paper we examine prospects for detecting or constraining the amplitudes of the most general allowed regular perturbations using present and future CMB data.']",['1999-04-20'] +1150,['eng'],"['Zibin, J P', 'Scott, D', 'White, M']",['Gravity waves goodbye'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, polarization', 'density, perturbation', 'potential, inflaton', 'perturbation, scalar', 'perturbation, tensor', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904228'],['The detection of a stochastic background of long-wavelength gravitational waves (tensors) in the cosmic microwave background (CMB) anisotropy would be an invaluable probe of the high energy physics of the early universe. Unfortunately a combination of factors now makes such a detection seem unlikely: the vast majority of the CMB signal appears to come from density perturbations (scalars) - detailed fits to current observations indicate a tensor-to-scalar quadrupole ratio of T/S < 0.5 for the simplest models; and on the theoretical side the best-motivated inflationary models seem to require very small T/S. Unfortunately CMB temperature anisotropies can only probe a gravity wave signal down to T/S \\sim 10% and optimistic assumptions about polarization of the CMB only lower this another order of magnitude.'],['1999-04-20'] +1151,['eng'],"['Halzen, Francis']",['High Energy Neutrino Astronomy'],['Astrophysics and Astronomy'],"['review, Cape Town 1999/01/24', 'neutrino, cosmic radiation', 'cosmic radiation, flux', 'photon, cosmic radiation', 'neutrino, oscillation', 'neutrino, mass', 'Cherenkov counter', 'muon, cosmic radiation', 'deep underground detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904216'],"['Although high energy neutrino astronomy is a multidisciplinary science, gamma ray bursts have become the theoretical focus since recent astronomical observations revealed their potential as cosmic particle accelerators. This spotlight is shared with investigations of the potential of high energy telescopes to observe oscillating atmospheric neutrinos. The Superkamiokande results have boosted atmospheric neutrinos from a calibration tool and a background for doing astronomy, to an opportunity to confirm the evidence for neutrino mass. Nevertheless, the highlights are mostly on the experimental front with the completion of the first-generation Baikal and AMANDA detectors. Neutrino signals from the Lake Baikal detector bode well for the flurry of activities in the Mediterranean. The completed AMANDA telescope announced first light, neutrinos actually, at this meeting.']",['1999-04-19'] +1152,['eng'],"['Basa, S']",['High Energy Cosmic Neutrinos Astronomy'],['Astrophysics and Astronomy'],"['talk, Paris 1998/12/14', 'neutrino, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, particle identification', 'muon, energy spectrum', 'muon, cosmic radiation', 'neutrino, oscillation', 'deep underground detector, proposed', 'Cherenkov counter, water']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904213'],"['Neutrinos may offer a unique opportunity to explore the far Universe at high energy. The ANTARES collaboration aims at building a large undersea neutrino detector able to observe astrophysical sources (AGNs, X-ray binary systems, ...) and to study particle physics topics (neutrino oscillation, ...). After a description of the research opportunities of such a detector, a status report of the experiment will be made.']",['1999-04-19'] +1153,['eng'],"['Abazajian, K N', 'Fuller, G M', 'Shi, X']",['Are $\\gamma$-Ray Bursts Signals of Supermassive Black Hole Formation?'],['Astrophysics and Astronomy'],"['talk, Byurakan 1998/08/17', 'black hole, massive', 'black hole, production', 'photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'fireball', 'time variation', 'baryon, density', 'neutrino, luminosity', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812287'],['The formation of supermassive black holes through the gravitational collapse of supermassive objects ($M \\ga 10^4 M_\\odot$) has been proposed as a source of cosmological gamma-ray bursts. The major advantage of this model is that such collapses are far more energetic than stellar-remnant mergers. The major drawback of this idea is the severe baryon loading problem in one-dimensional models. We can show that the observed log N - log P (number vs. peak flux) distribution for gamma-ray bursts in the BATSE database is not inconsistent with an identification of supermassive object collapse as the origin of the gamma-ray bursts. This conclusion is valid for a range of plausible cosmological and gamma-ray burst spectral parameters.'],['1998-12-16'] +1154,['eng'],"['Chary, R R', 'Wright, E L']",['The High Energy $\\gamma$-Ray Background as a Probe of the Dark Matter in the Galactic Halo'],['Astrophysics and Astronomy'],"['talk, Canberra 1998/08/17', 'astrophysics, missing-mass', 'galaxy', 'photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'upper limit', 'black hole', 'data analysis method', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811324'],"['We present constraints on the density of halo dark matter candidates within the solar circle based on the anisotropy in the high energy gamma-ray background. The known galactic components of the gamma-ray background, in particular the inverse Compton component, have been estimated more accurately. We find the spectrum of the residual emission, after subtracting the galactic component is inconsistent with emission from some of the proposed dark matter candidates. We derive upper limits of 10^8 M_sun for the mass of diffuse gas and 3*10^9 pc^(-3) for the number density of primordial black holes contributing to the gamma-ray background.']",['1998-11-23'] +1155,['eng'],"['Cuesta, H J M']",['Gravitational-Wave Bursts Induced by Neutrino Oscillations'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, oscillation', 'neutrino, sterile', 'supernova', 'asymmetry', 'gravitational radiation, induced', 'relativity theory, general', 'neutrino, flavor']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904200'],"['If neutrino flavor changes really exist, to say: $\\mu$-neutrino oscillating into a sterile neutrino, then, it can be expected that due to neutrino oscillations and non-spherical distortion of the resonance surface induced by the magnetic field, some asymmetric emission of sterile neutrinos can occur during the protoneutron star formation at the onset of a supernova core-collapse. Assuming no strong suppression of the oscillations, the non-spherical huge neutrino energies released, ($\\sim 10^{53-54} erg$), together with the proto-neutron star rapid rotation, may trigger powerful bursts of gravitational waves by the time neutrino flavor conversions ensue. I show here that these bursts are detectable by the new generation of gravitational-wave detectors as LIGO, VIRGO and TIGAs for distance scales $\\sim 10 kpc$. It is also argued that the general relativity requirement of an ellipsoidal axisymmetric core at maximum gravitational-wave emission induced by the oscillations onset. The connection of neutrino oscillations with the supernova asymmetry and bi-polar jets ejecta is shown naturally to appear in this scenario.']",['1999-04-20'] +1156,['eng'],"['Capozziello, S', 'Iovane, G', 'Lambiase, G', 'Stornaiolo, C']",['Fermion Helicity Flip Induced by Torsion Field'],['Astrophysics and Astronomy'],"['gravitation', 'torsion', 'fermion, helicity', 'Dirac equation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904199'],"['We show that in theories of gravitation with torsion the helicity of fermion particles is not conserved and we calculate the probability of spin flip, which is related to the anti-symmetric part of affine connection. Some cosmological consequences are discussed.']",['1999-04-20'] +1157,['eng'],"['Hwang, J', 'Noh, H']",['$COBE$-DMR constraints on a inflation model with non-minimal scalar field'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'field theory, scalar', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation', 'coupling constant', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811069'],"['We derive the power spectra of the scalar- and tensor-type structures generated in a chaotic-type inflation model based on non-minimally coupled scalar field with a self interaction. By comparing contributions of both-structures to the anisotropy of the cosmic microwave background radiation with the four-year COBE-DMR data on quadrupole anisotropy we derive constraints on the ratio of self-coupling and non-minimal coupling constants, and the expansion rate in the inflation era, Eq. (12). The requirement of successful amount of inflation further constrains the relative amount of tensor-type contribution, Eq. (16).']",['1998-11-05'] +1158,['eng'],"['Kataoka, J', 'Mattox, J R', 'Quinn, J', 'Kubo, H', 'Makino, F', 'Takahashi, T', 'Inoue, S', 'Hartman, R C', 'Madejski, G M', 'Sreekumar, P', 'Wagner, S J']",['High-Energy Emission From The TeV Blazar Markarian 501 During Multiwavelength Observations In 1996'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'cosmic radiation, production', 'cosmic radiation, particle source', 'photon, Compton scattering', 'magnetic field', 'experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811014'],"[""We present the results of a multiwavelength campaign for Mrk 501 performed in March 1996 with ASCA, EGRET, Whipple, and optical telescopes. In the X-ray band, a spectral break was observed around 2 keV. We report here for the first time the detection of high-energy gamma-ray flux from Mrk 501 with EGRET with 3.5 sigma significance (E>100 MeV). Higher flux was also observed in April/May 1996, with 4.0 sigma significance for E>100 MeV, and 5.2 sigma significance for E>500 MeV. The gamma-ray spectrum was measured to be flatter than most of the gamma-ray blazars. We find that the multiband spectrum in 1996 is consistent with that calculated from a one-zone SSC model in a homogeneous region. In the context of this model, we investigate the values of the magnetic field strength and the beaming factor allowed by the observational results. We compare the March 1996 multiwavelength spectrum with that in the flare state in April 1997. Between these two epochs, the TeV flux increase is well correlated with that observed in keV range. The keV and TeV amplitudes during the April 1997 flare are accurately reproduced, assuming that the population of synchrotron photons in 1996 are scattered by the newly injected relativistic electrons, having maximum energies of G_max = 6.0e6. However, the TeV spectrum observed during March 1996 campaign is flatter than predicted by our models. We find that this cannot be explained by either higher order Comptonization or the contribution of the `seed' IR photons from the host galaxy for the first-order external radiation Comptonization.""]",['1998-11-03'] +1159,['eng'],"['Albrecht, Andreas']",['Cosmology with a time-varying speed of light'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'inflationary universe', 'photon, velocity', 'velocity, time variation', 'horizon', 'space-time, Robertson-Walker']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904185'],['Cosmic inflation is the only known mechanism with the potential to explain the very special initial conditions which are required at the early stages of the evolution of our universe. This article outlines my work with Joao Magueijo which attempts to construct an alternative mechanism based on a time-varying speed of light.'],['1999-04-20'] +1160,['eng'],"['Lima, J A S', 'Alcaniz, J S']","['On the minimal angular size in open, $\\Lambda$CDM, and scalar field cosmologies']",['Astrophysics and Astronomy'],"['Friedman model', 'space-time, Robertson-Walker', 'astrophysics, fundamental constant', 'astrophysics, missing-mass', 'matter, density', 'field theory, scalar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904182'],"['We propose a simple method for determining the redshift $z_{m}$ at which the angular size of an extragalactic source with fixed proper diameter takes its minimal value. A closed analytical expression, which is often convenient for numerical evaluation is derived. The method is exemplified with the following FRW type expanding universes: the open matter dominated models ($\\Omega_{\\Lambda} = 0$), a critical density model with cosmological constant ($\\Omega_{\\Lambda} \\neq 0$), and the class of scalar field cosmologies proposed by Ratra and Peebles. The influence of systematic evolutionary effects is briefly discussed.']",['1999-04-20'] +1161,['eng'],"['Horowitz, C J', 'Li, G']",['Charge Conjugation Violating Interactions in Supernovae and Nucleosynthesis'],['Astrophysics and Astronomy'],"['supernova', 'light nucleus, production', 'charge conjugation, violation', 'neutrino, energy', 'parity, violation', 'neutrino nucleon, interaction', 'cross section, capture', 'nucleon, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904171'],['Core collapse supernovae are dominated by energy transport from weakly interacting neutrinos. This offers a unique opportunity for large parity and or charge conjugation violation. One charge conjugation violating term in the standard model is of order the neutrino energy over the nucleon mass and increases the $\\nu_e-n$ capture cross section while decreasing that for significantly hinder r-process nucleosynthesis.'],['1999-04-14'] +1162,['eng'],"['Martín, J', 'Riazuelo, A', 'Sakellariadou, M']",['Non-Vacuum Initial States for Cosmological Perturbations of Quantum-Mechanical Origin'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'operator, spectra', 'potential', 'quantum mechanics', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904167'],"['In the context of inflation, non-vacuum initial states for cosmological perturbations that possess a built in scale are studied. It is demonstrated that this assumption leads to a falsifiable class of models. The question of whether they lead to conflicts with the available observations is addressed. For this purpose, the power spectrum of the Bardeen potential operator is calculated and compared with the CMBR anisotropies measurements and the redshift surveys of galaxies and clusters of galaxies. Generic predictions of the model are: a high first acoustic peak, the presence of a bump in the matter power spectrum and non-Gaussian statistics. The details are controlled by the number of quanta in the non-vacuum initial state. Comparisons with observations show that there exists a window for the free parameters such that good agreement between the data and the theoretical predictions is possible. However, in the case where the initial state is a state with a fixed number of quanta, it is shown that this number cannot be greater than a few. On the other hand, if the initial state is a quantum superposition, then a larger class of initial states could account for the observations, even though the state cannot be too different from the vacuum. Planned missions such as the MAP and Planck satellites and the Sloan Survey, will demonstrate whether the new class of models proposed here represents a viable alternative to the standard theory.']",['1999-04-14'] +1163,['eng'],"['Kifune, T']",['Invariance Violation Extends the Cosmic Ray Horizon?'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'conservation law, energy-momentum', 'violation, Lorentz', 'photon, velocity', 'absorption, path length', 'p, cosmic radiation', 'photon photon, interaction', 'cosmic radiation, energy spectrum', 'galaxy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904164'],"['We postulate in the present paper that the energy-momentum relation is modified for very high energy particles to violate Lorentz invariance and the speed of photon is changed from the light velocity c. The violation effect is amplified, in a sensitive way to detection, through the modified kinematical constraints on the conservation of energy and momentum, in the absorption process of gamma-rays colliding against photons of longer wavelengths and converting into an electron-positron pair. For gamma-rays of energies higher than 10 TeV, the minimum energy of the soft photons for the reaction and then the absorption mean free path of gamma-rays are altered by orders of magnitude from the ones conventionally estimated. Consideration is similarly applied to high energy cosmic ray protons. The consequences may require the standard assumptions on the maximum distance that very high energy radiation can travel from to be revised.']",['1999-04-14'] +1164,['eng'],"['Benacquista, M J']",['Gravitational Radiation From Globular Clusters'],['Astrophysics and Astronomy'],"['gravitational radiation, measurement', 'galaxy, cluster', 'signal processing', 'counters and detectors, angular resolution', 'n, matter', 'black hole', 'binary', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810484'],"['Space-based gravitational wave detectors will have the ability to observe continuous low frequency gravitational radiation from binary star systems. They can determine the direction to continuous sources with an angular resolution approaching tens of arcminutes. This resolution should be sufficient to identify binary sources as members of some nearby globular clusters. Thus, gravitational radiation can be used to determine the population of hard binaries in globular clusters. For particularly hard binaries, the orbital period may change as a result of gravitational wave emission. If one of these binaries can be identified with a globular cluster, then the distance to that cluster can be determined. Thus, gravitational radiation may provide reddening-independent distance measurements to globular clusters.']",['1998-10-30'] +1165,['eng'],"['Usov, Yu V', 'Smolsky, M V']",['Particle acceleration and high-frequency (X-ray and $\\gamma$-ray) emission in the jets of active galactic nuclei'],['Astrophysics and Astronomy'],"['galaxy, AGN', 'plasma, jet', 'particle, acceleration', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810410'],"['It is suggested that the outflowing plasma in the jets of active galactic nuclei (AGNs) is inhomogeneous and consists of separate clouds. These clouds are strongly magnetized and move away from the central engine at relativistic speeds. The clouds interact with an ambient medium which is assumed to be at rest. In the process of this interaction, particles of the ambient medium are accelerated to high energies at the cloud front and flow ahead of the front. It is shown that the radiation of the accelerated particles may be responsible for the X-ray and $\\gamma$-ray emission from AGN jets. TeV $\\gamma$-ray emission is generated in the inner parts of AGN jets where the Lorentz factor of the cloud fronts is $\\Gamma_0\\geq 30$, while GeV $\\gamma$-ray emission emanates from the outer parts of AGN jets where $\\Gamma_0$ is $\\sim 10$.']",['1998-10-27'] +1166,['eng'],"['Barabash, O V', 'Shtanov, Yu V']",['Newtonian limit of conformal gravity'],['Astrophysics and Astronomy'],"['gravitation, conformal', 'approximation, weak field', 'symmetry, rotational', 'field theory, scalar', 'symmetry breaking, conformal', 'fermion, mass generation', 'space-time, Schwarzschild', 'space-time, anti-de Sitter']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904144'],"[""We obtain the weak-field limit of the static spherically symmetric solution of the locally conformally invariant theory advocated in the recent past by Mannheim and Kazanas as an alternative to Einstein's General Relativity. In contrast with the previous studies by these authors, we consider the physically relevant case where the scalar field that breaks conformal symmetry and generates fermion masses is nonzero. In the physical gauge, in which this scalar field is constant in space-time, our solution reproduces the weak-field limit of the Schwarzschild--(anti) De Sitter solution modified by an additional term that, depending on the sign of the Weyl term in the action, is either oscillatory or exponential as a function of the radial distance. Such behavior reflects the presence of, correspondingly, either a tachion or a massive ghost in the spectrum, which is a serious drawback of the theory under discussion.""]",['1999-04-13'] +1167,['eng'],"['Drago, A']","['Neutron Stars, Supernova Explosions and the Transition to Quark Matter']",['Astrophysics and Astronomy'],"['talk, Paris 1998/12/14', 'n, matter', 'supernova', 'quark, matter', 'bag model', 'matter, hybrid', 'critical phenomena, confinement', 'finite temperature', 'dependence, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904124'],"[""The transition to quark matter can take place in neutron stars. The structure of a hybrid star, containing a core made of quark matter is discussed. The maximum mass of the non-rotating hybrid star turns out to be 1.6 M_s. Possible signatures of the quark phase as pulsar's timing, cooling rate etc. are briefly analyzed. The deconfinement transition can also take place during the pre-supernova collapse. This possibility is studied by introducing a finite temperature EOS. The dependence of the latter on the proton fraction is shown to be crucial. The softening of the EOS at densities just above nuclear matter saturation density for Z/A = 0.3 helps in obtaining an explosion. At the same time, at larger densities the EOS is stiff enough to support a neutron star compatible with observations.""]",['1999-04-12'] +1168,['eng'],"['Amendola, L']",['Scaling solutions in general non-minimal coupling theories'],['Astrophysics and Astronomy'],"['gravitation', 'field theory, scalar', 'matter, fluid', 'scaling, attractor', 'strong coupling', 'potential', 'energy, density', 'field equations, solution', 'astrophysics', 'critical phenomena', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904120'],"['A class of generalized non-minimal coupling theories is investigated, in search of scaling attractors able to provide an accelerated expansion at the present time. Solutions are found in the strong coupling regime and when the coupling function and the potential verify a simple relation. In such cases, which include power law and exponential functions, the dynamics is independent of the exact form of the coupling and the potential. The constraint from the time variability of $G$, however, limits the fraction of energy in the scalar field to less than 4% of the total energy density, and excludes accelerated solutions at the present.']",['1999-04-12'] +1169,['eng'],"['Barrow, John D', ""O'Toole, C""]",['Spatial Variations of Fundamental Constants'],['Astrophysics and Astronomy'],"['gravitation, fundamental constant', 'fundamental constant, fine structure', 'fundamental constant, time variation', 'fundamental constant, spatial distribution', 'Maxwell equation', 'matter, density']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904116'],"[""We show that observational limits on the possible time variation of constants of Nature are significantly affected by allowing for both space and time variation. Bekenstein's generalisation of Maxwell's equations to allow for cosmological variation of $alpha$ is investigated in a universe containing spherically symmetric inhomogeneities. The time variation of $alpha$ is determined by the local matter density and hence limits obtained in high-density geophysical enviroments are far more constraining than those obtained at high redshift. This new feature is expected to be a property of a wide class of theories for the variation of constants.""]",['1999-04-12'] +1170,['eng'],"['Kamionkowski, M P', 'Kosowsky, A']",['The Cosmic Microwave Background and Particle Physics'],['Astrophysics and Astronomy'],"['review', 'cosmic radiation, background', 'inflationary universe, validity test', 'space-time, geometry', 'density, perturbation', 'temperature, fluctuation', 'gravitational radiation', 'cosmic radiation, polarization', 'topology, defect', 'magnetic field', 'critical phenomena', 'astrophysics, missing-mass', 'particle, decay', 'baryon, asymmetry', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904108'],"['In forthcoming years, connections between cosmology and particle physics will be made increasingly important with the advent of a new generation of cosmic microwave background (CMB) experiments. Here, we review a number of these links. Our primary focus is on new CMB tests of inflation. We explain how the inflationary predictions for the geometry of the Universe and primordial density perturbations will be tested by CMB temperature fluctuations, and how the gravitational waves predicted by inflation can be pursued with the CMB polarization. The CMB signatures of topological defects and primordial magnetic fields from cosmological phase transitions are also discussed. Furthermore, we review current and future CMB constraints on various types of dark matter (e.g. massive neutrinos, weakly interacting massive particles, axions, vacuum energy), decaying particles, the baryon asymmetry of the Universe, ultra-high-energy cosmic rays, exotic cosmological topologies, and other new physics.']",['1999-04-12'] +1171,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Roberts, I D', 'Shaw, S E', 'Turver, K E']",['Geomagnetic effects on atmospheric Cerenkov images'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, electromagnetic', 'showers, hadronic', 'Cherenkov counter', 'magnetic field, geophysics', 'performance', 'experimental results', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904082'],"['Atmospheric Cerenkov telescopes are used to detect electromagnetic showers from primary gamma rays of energy ~300 GeV - ~10 TeV and to discriminate these from cascades due to hadrons using the Cerenkov images. The geomagnetic field affects the development of showers and is shown to diffuse and distort the images. When the component of the field normal to the shower axis is sufficiently large (> 0.4 G) the performance of gamma ray telescopes may be affected, although corrections should be possible.']",['1999-04-08'] +1172,['eng'],"['Ricci, B', 'Villante, F L', 'Lissia, M']",['Helioseismology and Beryllium neutrino'],['Astrophysics and Astronomy'],"['model, solar', 'neutrino, solar', 'beryllium', 'neutrino, flux', 'lower limit', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904072'],"['We derive a lower limit on the Beryllium neutrino flux on earth, by using helioseismic data, the B-neutrino flux measured by Superkamiokande and the hydrogen abundance at the solar center predicted by Standard Solar Model (SSM) calculations. We emphasize that this abundance is the only result of SSMs needed for getting $\\Phi(Be)_{min}$. We also derive lower bounds for the Gallium signal, $G_{min}=(91 \\pm 3) $ SNU, and for the Chlorine signal, $C_{min}=(3.24\\pm 0.14)$ SNU, which are about $3\\sigma$ above their corresponding experimental values, $G_{exp}= (72\\pm 6)$ SNU and $C_{exp}= (2.56\\pm 0.22) $ SNU.']",['1999-04-07'] +1173,['eng'],"['Kim, J E']",['Lifetime Limit of LSP from Cosmological Light Elements'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'astrophysics, light nucleus', 'deuterium', 'supersymmetry', 'R parity, violation', 'LSP, lifetime', 'lower limit', 'sparticle, mass', 'temperature, decoupling', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904067'],"['From the present cosmic abundance of the light elements, one can obtain a lifetime bounds of LSP. From the consideration of deuterium, we obtain']",['1999-04-07'] +1174,['eng'],"['Snowden-Ifft, D P', 'Martoff, C J', 'Burwell, J M']",['Low Pressure Negative Ion Drift Chamber for Dark Matter Search'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP', 'drift chamber, gas', 'ion, drift velocity', 'ion, negative particle', 'carbon, sulfur', 'argon', 'xenon', 'deep underground detector, Gran Sasso']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904064'],"['Weakly Interacting Massive Particles (WIMPs) are an attractive candidate for the dark matter thought to make up the bulk of the mass of our universe. We explore here the possibility of using a low pressure negative ion drift chamber to search for WIMPs. The innovation of drifting ions, instead of electrons, allows the design of a detector with exceptional sensitivity to, background rejection from, and signature of WIMPs.']",['1999-04-06'] +1175,['eng'],"['Konopelko, A K', 'Kirk, J G', 'Stecker, F W', 'Mastichiadis, A']",['Evidence for Intergalactic Absorption in the TeV Gamma-Ray Spectrum of Markarian 501'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'astrophysics, galaxy', 'photon, absorption', 'cosmic radiation, background', 'cosmic radiation, energy spectrum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904057'],"['The recent HEGRA observations of the blazar Mkn 501 show strong curvature in the very high energy gamma-ray spectrum. Applying the gamma-ray opacity derived from an empirically based model of the intergalactic infrared background radiation field (IIRF), to these observations, we find that the intrinsic spectrum of this source is consistent with a power-law: dN/dE~ E^-alpha with alpha=2.00 +/- 0.03 over the range 500 GeV - 20 TeV. Within current synchrotron self-Compton scenarios, the fact that the TeV spectral energy distribution of Mkn 501 does not vary with luminosity, combined with the correlated, spectrally variable emission in X-rays, as observed by the BeppoSAX and RXTE instruments, also independently implies that the intrinsic spectrum must be close to alpha=2. Thus, the observed curvature in the spectrum is most easily understood as resulting from intergalactic absorption.']",['1999-04-06'] +1176,['eng'],"['Abazajian, K N', 'Shi, X', 'Fuller, G M']",['Active-Sterile Neutrino Mixing in the Early Universe and Primordial Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Los Angeles 1999/01/05', 'astrophysics, model', 'neutrino, oscillation', 'resonance, oscillation', 'neutrino, sterile', 'helium, yield', 'neutrino, energy spectrum', 'n, semileptonic decay', 'neutrino, capture', 'neutrino, mixing angle', 'light nucleus, production', 'numerical calculations', 'n --> p electron antineutrino/e']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904052'],"['We investigate the effects of matter-enhanced (MSW) transformation of neutrinos in the Early Universe on the primordial helium yield (Y_p). We find that Y_p is affected much more by the MSW-induced alterations in the neutrino energy spectra than by the associated change in expansion rate. Specifically, the absence due to transformation of low energy electron neutrinos can significantly affect neutron-proton weak interconversion rates through the lifting of Fermi-blocking of neutron decay at low energies and through halting low-energy neutrino capture on neutrons. We find that the change of Y_p within a causal horizon is -0.005\\le \\delta Y_p \\leq 0.013 for m_{\\nu_{\\mu,\\tau}}^2 - m_{\\nu_s}^2 \\le 10^4 eV^2 in the case of \\nu_{\\mu,\\tau}-\\nu_s-\\nu_e mixing, with the lower limit at m_{\\nu_{\\mu,\\tau}}^2 - m_{\\nu_s}^2 \\approx 100 eV^2, and -0.002\\le \\delta Y_p \\leq 0.020 for m_{\\nu_e}^2 - m_{\\nu_s}^2 \\le 1 eV^2 in the case of \\nu_e-\\nu_s mixing.']",['1999-04-06'] +1177,['eng'],"['Vankov, A']",['On the Cosmological Aspects of Observed High Energy Cosmic Phenomena'],['Astrophysics and Astronomy'],"['talk, Atlanta 1999/03/20', 'astrophysics, model', 'cosmic radiation, background', 'antimatter', 'matter, expansion', 'time variation', 'photon, cosmic radiation', 'quasar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904045'],"['Super-high energy corpuscular and gamma rays as well as cosmic high--power density sources are hard to explain in a galaxy model framework. Attempts to include some of those phenomena in the Standard Cosmological Model also encounter serious difficulties. In the present paper an alternative cosmological concept is discussed. There are several features in it. First of all, the whole Universe (Grand Universe) is a multitude of typical universes, like ours, evenly made of either matter or antimatter, hence, there is no violation of the baryon symmetry on the largest scale. Second, high-energy phenomena are the result of matter-antimatter annihilation processes in a typical universe evolution. Finally, the Ground Universe is a self-creating due to a balance of annihilation and pair creation in the inter-universe infinite space. This concept and its consistence with the major observational data are discussed in detail.']",['1999-04-06'] +1178,['eng'],"['Shi, X', 'Fuller, G M']",['Leptonic Domains in the Early Universe and Their Implications'],['Astrophysics and Astronomy'],"['astrophysics, model', 'lepton number, production', 'neutrino, oscillation', 'resonance, oscillation', 'space-time, causality', 'neutrino, sterile', 'neutrino, production', 'light nucleus, production', 'neutrino, mixing angle', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904041'],"['We extend a treatment of the causal structure of space-time to active-sterile neutrino transformation-based schemes for lepton number generation in the early universe. We find that these causality considerations necessarily lead to the creation of spatial domains of lepton number with opposite signs. Lepton number gradients at the domain boundaries can open a new channel for MSW resonant production of sterile neutrinos. The enhanced sterile neutrino production via this new channel allows considerable tightening of Big Bang Nucleosynthesis constraints on active-sterile neutrino mixing, including the proposed $\\nu_\\mu the four-neutrino schemes proposed to simultaneously fit current neutrino experimental results.']",['1999-04-05'] +1179,['eng'],"['Tsiklauri, D']",['On the gravitational stability of a compressed slab of gas in the background of weakly interacting massive particles'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'gas, stability', 'coupling, gravitation', 'WIMP', 'dispersion relations', 'oscillation', 'matter, production', 'perturbation, linear']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904013'],"['Linear stability of an isothermal, pressure-bounded, self-gravitating gas slab which is gravitationally coupled with the background weakly interacting massive particles (WIMPs) is investigated. Analytic dispersion relations describing such a configuration are derived. Two novel, distinct oscillatory modes are found. Astrophysical implications of the results are discussed.']",['1999-04-02'] +1180,['eng'],"['Ma, C P']",['Neutrinos and Dark Matter'],['Astrophysics and Astronomy'],"['lectures, Boulder 1998/05/31', 'astrophysics, missing-mass', 'neutrino, cosmic radiation', 'neutrino, mass', 'temperature', 'neutrino, density', 'velocity', 'neutrino, phase space', 'astrophysics, model', 'energy, density', 'time dependence', 'neutrino, cluster', 'gravitation', 'neutrino, spatial distribution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9904001'],['In these lectures I highlight some key features of massive neutrinos in the context of cosmology. I first review the thermal history and the free-streaming kinematics of the uniform cosmic background neutrinos. I then describe how fluctuations in the phase space distributions of neutrinos and other particles arise and evolve after neutrino decoupling according to the linear perturbation theory of gravitational instability. The different clustering properties of massive neutrinos (aka hot dark matter) and cold dark matter are contrasted. The last part discusses the nonlinear stage of gravitational clustering and highlights the effects of massive neutrinos on the formation of cosmological structure.'],['1999-04-02'] +1181,['eng'],"['Chubarian, E', 'Grigorian, H', 'Poghosyan, G', 'Blaschke, David B']",['Deconfinement phase transition in rotating compact stars'],['Astrophysics and Astronomy'],"['n, matter', 'rotational', 'gravitation', 'field equations', 'symmetry, axial', 'perturbation theory', 'velocity', 'critical phenomena, confinement', 'flavor, 2', 'baryon number', 'charge, electric', 'quark, matter', 'radiation, dipole', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903489'],"['We formulate the selfconsistent set of equations for the gravitational field and its sources for the case of axial symmetry relevant for the application to rotating compact stars. We develop a perturbation theory with respect to angular velocity and define physical quantities such as mass, shape, momentum of inertia and total energy of the star. This method allows an investigation of the change of the internal structure of the star due to rotation as well as a separate evaluation of the angular velocity dependence of the different contributions to the moment of inertia. Numerical solutions have been performed using a two-flavor model equation of state describing the deconfinement phase transition as constrained by the conservation of total baryon number and electric charge. During the spin down evolution of the rotating neutron star, below critical values of angular velocity a quark matter core can appear which might be detected as a characteristic signal in the pulsar timing. We show that in the spin-down scenario due to magnetic dipole radiation the deviation of the braking index from $n=3$ could signal not only the occurence but also the size of a quark core in the pulsar. We propose also another scenario where due to mass accretion onto the star a spin-down to spin-up transition might signal a deconfinement transition in the rapidly rotating compact object.']",['1999-04-01'] +1182,['eng'],"['Green, A M']",['Supersymmetry and primordial black hole abundance constraints'],['Astrophysics and Astronomy'],"['black hole', 'supersymmetry', 'LSP', 'density, perturbation', 'inflationary universe', 'temperature', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903484'],"['We study the consequences of supersymmetry for primordial black hole (PBH) abundance constraints. PBHs with mass less than about 10^{11}g will emit supersymmetric particles when they evaporate. In most models of supersymmetry the lightest of these particles, the lightest supersymmetric particle (LSP), is stable and will hence survive to the present day. We calculate the limit on the initial abundance of PBHs from the requirement that the present day LSP density is less than the critical density. We apply this limit, along with those previously obtained from the effects of PBH evaporation on nucleosynthesis and the present day density of PBHs, to PBHs formed from the collpase of inflationary density perturbations, in the context of supersymmetric inflation models. If the reheat temperature after inflation is low, so as to avoid the overproduction of gravitinos and moduli, then the lightest PBHs which are produced in significant numbers will be evaporating around the present day and there are therefore no constraints from the effects of the evaporation products on nucleosynthesis or from the production of LSPs. We then examine models with a high reheat temperature and a subsequent period of thermal inflation. In these models avoiding the overproduction of LSPs limits the abundance of low mass PBHs which were previously unconstrained. Throughout we incorporate the production, at fixed time, of PBHs with a range of masses, which occurs when critical collapse is taken into account.']",['1999-04-01'] +1183,['eng'],"['Mücke, A', 'Engel, R', 'Rachen, J P', 'Protheroe, R J', 'Stanev, T']",['Monte-Carlo simulations of photohadronic processes in astrophysics'],['Astrophysics and Astronomy'],"['photon hadron, interaction', 'astrophysics', 'photon nucleon, interaction', 'baryon resonance, photoproduction', 'baryon resonance, decay', 'pi, direct production', 'exchange, pomeron', 'Regge poles', 'Feynman graph', 'color, flux', 'cross section, parametrization', 'pi, multiple production', 'kinematics', 'photon, radiation', 'cross section, energy dependence', 'multiplicity, spectra', 'rapidity spectrum', 'programming, Monte Carlo', 'numerical calculations, Monte Carlo', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903478'],"['A new Monte Carlo program for photohadronic interactions of relativistic nucleons with an ambient photon radiation field is presented. The event generator is designed to fulfil typical astrophysical requirements, but can also be used for radiation and background studies at high energy colliders such as LEP2 and HERA, as well as for simulations of photon induced air showers. We consider the full photopion production cross section from the pion production threshold up to high energies. It includes resonance excitation and decay, direct single pion production and diffractive and non-diffractive multiparticle production. The cross section of each individual process is calculated by fitting experimental data, while the kinematics is determined by the underlying particle production process. We demonstrate that our model is capable of reproducing known accelerator data over a wide energy range.']",['1999-04-01'] +1184,['eng'],"['Hannestad, S']",['Probing neutrino decays with the cosmic microwave background'],['Astrophysics and Astronomy'],"['neutrino, massive', 'neutrino, decay modes', 'final state, two-particle', 'final state, (3neutrino)', 'neutrino, lifetime', 'neutrino, mass', 'cosmic radiation, background', 'microwaves', 'Boltzmann equation, solution', 'astrophysics, model', 'neutrino, energy spectrum', 'energy, density', 'neutrino, momentum spectrum', 'numerical calculations', 'neutrino --> 2neutrino antineutrino', 'neutrino --> scalar particle neutrino']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903475'],"['We investigate in detail the possibility of constraining neutrino decays with data from the cosmic microwave background radiation (CMBR). Two generic decays are considered \\nu_H -> \\nu_L \\phi and \\nu_H -> \\nu_L \\nu_L_bar \\nu_L. We have solved the momentum dependent Boltzmann equation in order to account for possible relativistic decays. Doing this we estimate that any neutrino with mass m > 1 eV decaying before the present should be detectable with future CMBR data. Combining this result with other results on stable neutrinos, any neutrino mass of the order 1 eV should be detectable.']",['1999-04-01'] +1185,['eng'],"['Schneider, R', 'Ferrari, V', 'Matarrese, S']",['Stochastic Backgrounds of Gravitational Waves from Cosmological Populations of Astrophysical Sources'],['Astrophysics and Astronomy'],"['talk, Paris 1998/12/14', 'gravitational radiation, spectra', 'background, stochastic', 'matter, production', 'black hole', 'n, matter', 'energy, density', 'signal processing', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903470'],"['Astrophysical sources of gravitational radiation are likely to have been formed since the beginning of star formation. Realistic source rates of formation throughout the Universe have been estimated from an observation-based determination of the star formation rate density evolution. Both the radiation emitted during the collapse to black holes and the spin-down radiation, induced by the r-mode instability, emitted by hot, young rapidly rotating neutron stars have been considered. We have investigated the overall signal produced by the ensemble of sources exploring the parameter space and discussing its possible detectability.']",['1999-04-01'] +1186,['eng'],"['Barwick, S W']",['High Energy Cosmic Neutrinos'],['Astrophysics and Astronomy'],"['talk, Enkoeping 1998/08/20', 'neutrino, cosmic radiation', 'neutrino, energy spectrum', 'neutrino, oscillation', 'neutrino, solar', 'astrophysics, missing-mass', 'WIMP', 'astrophysics, particle source', 'galaxy', 'deep underground detector, AMANDA', 'deep underground detector, proposed', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903467'],"['While the general principles of high-energy neutrino detection have been understood for many years, the deep, remote geographical locations of suitable detector sites have challenged the ingenuity of experimentalists, who have confronted unusual deployment, calibration, and robustness issues. Two high energy neutrino programs are now operating (Baikal and AMANDA), with the expectation of ushering in an era of multi-messenger astronomy, and two Mediterranean programs have made impressive progress. The detectors are optimized to detect neutrinos with energies of the order of 1-10 TeV, although they are capable of detecting neutrinos with energies of tens of MeV to greater than PeV. This paper outlines the interdisciplinary scientific agenda, which span the fields of astronomy, particle physics, and cosmic ray physics, and describes ongoing worldwide experimental programs to realize these goals.']",['1999-04-01'] +1187,['eng'],"['Böttcher, M', 'Dermer, C D']",['Prompt and Delayed High-Energy Emission from Cosmological $\\gamma$-Ray Bursts'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'astrophysics, model', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'photon electron, Compton scattering', 'p, cosmic radiation', 'acceleration', 'synchrotron radiation', 'Cherenkov counter']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812175'],"['In the cosmological blast-wave model for gamma ray bursts (GRBs), high energy (> 10 GeV) gamma-rays are produced either through Compton scattering of soft photons by ultrarelativistic electrons, or as a consequence of the acceleration of protons to ultrahigh energies. We describe the spectral and temporal characteristics of high energy gamma-rays produced by both mechanisms, and discuss how these processes can be distinguished through observations with low-threshold Cherenkov telescopes or GLAST. We propose that Compton scattering of starlight photons by blast wave electrons can produce delayed flares of GeV -- TeV radiation.']",['1998-12-10'] +1188,['eng'],"['Kaaret, P E']",['Pulsar Radiation and Quantum Gravity'],['Astrophysics and Astronomy'],"['quantum gravity', 'photon, velocity', 'energy dependence', 'photon, cosmic radiation', 'pulsar', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903464'],"['Quantum gravity may lead to an energy dependence in the speed of light. The high energy radiation from gamma-ray pulsars can be used to place limits on such effects. We find that emission from the Crab pulsar at energies above 2 GeV trails that at 70-100 MeV by no more than 0.35 ms (95% confidence) and place a lower bound on the energy scale of quantum gravitational effects on the speed of light of 1.8 x 10^15 GeV. This bound might be improved by two orders of magnitude by observation of pulsations from the Crab at higher energies, 50-100 GeV, in the near future.']",['1999-03-31'] +1189,['eng'],"['Aharonian, F A']",['Constraints on BL Lac objects by the HEGRA-system of Cherenkov telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'upper limit', 'astrophysics', 'Cherenkov counter, imaging', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903455'],"[""The HEGRA system of four Imaging Atmospheric Cherenkov Telescopes (IACTs) has been used to extensively observe extragalactic objects. In this paper we describe the search for TeV emission from nine very promising potential TeV sources, i.e. eight ``high frequency'' BL Lac objects (HBLs), and the object ``BL Lac'' itself. The objects were observed between one and 15 hours during 1997 and 1998. No evidence for emission was found and the upper limits on the integral energy flux above ~750 GeV are on the level of a few times 10^-12 erg.cm^-2.s^-1. For the two objects BL Lac and 1ES 2344+51.4, we discuss the astrophysical implications of the TeV flux upper limit, using also information from the X-ray and gamma-ray bands as measured with the RXTE All Sky Monitor (ASM, 1.3-12.0 keV) and with EGRET (30 MeV - 20 GeV).""]",['1999-03-31'] +1190,['eng'],"['Silk, J']",['Seven Paradigms in Structure Formation'],['Astrophysics and Astronomy'],"['talk, Faro 1998/09/03', 'inflationary universe', 'light nucleus, production', 'baryon, density', 'density, fluctuation', 'galaxy, rotational', 'astrophysics, missing-mass', 'luminosity', 'cosmic radiation, background', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903402'],['Have we converged on the definitive model of cosmology? I present a critical assessment of the current paradigms for the evolution of large-scale structure.'],['1999-03-26'] +1191,['eng'],"['Massó, E', 'Toldrà, R']",['Photon Spectrum Produced by the Late Decay of a Cosmic Neutrino Background'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, radiative decay', 'photon, energy spectrum', 'momentum spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903397'],['We obtain the photon spectrum induced by a cosmic background of unstable neutrinos. We study the spectrum in a variety of cosmological scenarios and also we allow for the neutrinos having a momentum distribution (only a critical matter dominated universe and neutrinos at rest have been considered until now). Our results can be helpful when extracting bounds on neutrino electric and magnetic moments from cosmic photon background observations.'],['1999-03-26'] +1192,['eng'],"['Aharonian, F A']",['The time averaged TeV energy spectrum of Mkn 501 of the extraordinary 1997 outburst as measured with the stereoscopic Cherenkov telescope system of HEGRA'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'galaxy, AGN', 'cosmic radiation, energy spectrum', 'astrophysics', 'photon, absorption', 'Cherenkov counter, imaging', 'shower detector, experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903386'],"['During the several months of the outburst of Mkn 501 in 1997 the source has been monitored in TeV gamma-rays with the HEGRA stereoscopic system of imaging atmospheric Cherenkov telescopes. Quite remarkably it turned out that the shapes of the daily gamma-ray energy spectra remained essentially stable throughout the entire state of high activity despite dramatic flux variations during this period. The derivation of a long term time-averaged energy spectrum, based on more than 38,000 detected TeV photons, is therefore physically meaningful. The unprecedented gamma-ray statistics, combined with the 20% energy resolution of the instrument, results in a well-defined, smooth differential energy spectrum extending deeply into the exponential regime. From 500 GeV to 24 TeV the differential spectrum is well approximated by a power-law with an exponential cutoff: dN/dE = N0 (E/1 TeV)^{-alpha} exp(-E/E0), with N0 = (10.8 +-0.2(stat) +-2.1(sys)) 1E-11/cm^2 s TeV, alpha = 1.92 +- 0.03(stat) +-0.20(sys), and E0 = (6.2 +-0.4(stat) (-1.5 +2.9)(syst)) TeV. We summarize the methods for the evaluation of the energy spectrum in a broad dynamical range which covers almost two energy decades, and study in detail the principal sources of systematic errors. We also discuss several important astrophysical implications of the observed result concerning the production and absorption mechanisms of gamma-rays in the emitting jet and the modifications of the initial spectrum of TeV radiation due to its interaction with the diffuse extragalactic background radiation.']",['1999-03-26'] +1193,['eng'],"['Navarro, A', 'Serna, A', 'Alimi, J M']",['Asymptotic and Exact Solutions of Perfect-Fluid Scalar-Tensor Cosmologies'],['Astrophysics and Astronomy'],"['astrophysics, model', 'gravitation, scalar', 'gravitation, tensor', 'fluid', 'field equations, solution', 'asymptotic behavior', 'space-time, Robertson-Walker', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903368'],"['We present a method which enables exact solutions to be found for at homogeneous and isotropic scalar-tensor cosmologies with an arbitrary $P=(\\gamma-1)\\rho c^2$. This method has been used to analyze a wide range of asymptotic analytical solutions at early and late times for different epochs in the cosmic history: false vacuum inflationary models, vacuum and radiation-dominated models, and matter-dominated models. We also describe the qualitative behavior of models at intermediary times and give exact solutions at any time for some particular scalar-tensor theories.']",['1999-03-25'] +1194,['eng'],"['Rudenko, V N', 'Gusev, A V', 'Kravchuk, V K', 'Vinogradov, M P']",['Search for astro-gravity correlations'],['Astrophysics and Astronomy'],"['gravitational radiation', 'counters and detectors', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'background, perturbation', 'correlation, (neutrino graviton)', 'supernova', 'data analysis method', 'experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903365'],['A new approach in the gravitational wave experiment is considered. In addition to the old method of searching for coincident reactions of two separated gravitational antennae it was proposed to seek perturbations of the gravitational detector noise background correlated with astrophysical events such as neutrino and gamma ray bursts which can be relaibly registered by correspondent sensors. A general algorithm for this approach is developed. Its efficiency is demonstrated in reanalysis of the old data concerning the phenomenon of neutrino-gravity correlation registered during of SN1987A explosion.'],['1999-03-25'] +1195,['eng'],"['Vachaspati, T']","['Formation, Interaction and Observation of Topological Defects']",['Astrophysics and Astronomy'],"['talk, Les Houches 1999/02/16', 'astrophysics, string', 'topology, defect', 'defect, production', 'defect, interaction', 'critical phenomena', 'bubble', 'gravitation, lens', 'cosmic radiation, background', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903362'],"['In these lectures, I describe the formation of defect distributions in first-order phase transitions, then briefly discuss the relevance of defect interactions after a phase transition and the observational signatures of cosmic strings. Some open questions are also discussed.']",['1999-03-24'] +1196,['eng'],"['Pogosian, L E', 'Vachaspati, T']",['Cosmic microwave background anisotropy from wiggly strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'string, network', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'density, perturbation', 'astrophysics, fundamental constant', 'tensor, energy-momentum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903361'],"['We investigate the effect of wiggly cosmic strings on the cosmic microwave background radiation anisotropy and matter power spectrum by modifying the string network model used by Albrecht et al.. We employ the wiggly equation of state for strings and the one-scale model for the cosmological evolution of certain network characteristics. For the same choice of simulation parameters we compare the results with and without including wiggliness in the model and find that wiggliness together with the accompanying low string velocities lead to a significant peak in the microwave background anisotropy and to an enhancement in the matter power spectrum. For the cosmologies we have investigated (standard CDM, and, CDM plus cosmological constant), and within the limitations of our modeling of the string network, the anisotropy is in reasonable agreement with current observations but the COBE normalized amplitude of density perturbations is lower than what the data suggests. In the case of a cosmological constant and CDM model, a bias factor of about 2 is required.']",['1999-03-24'] +1197,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['A Search for VHE $\\gamma$ Rays from AGNs Visible from the Southern Hemisphere'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'cosmic radiation, time variation', 'galaxy, AGN', 'Cherenkov counter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903346'],"['Observations have been made, using the University of Durham Mark 6 gamma ray telescope, of the very high energy gamma ray emission from a number of active galactic nuclei visible from the Southern hemisphere. Limits are presented to the VHE gamma ray emission from 1ES 0323+022, PKS 0829+046, 1ES 1101--232, Cen A, PKS 1514-24, RXJ 10578-275, and 1ES 2316-423, both for steady long-term emission and for outbursts of emission on timescales of 1 day.']",['1999-03-24'] +1198,['eng'],"['Ivanov, A A', 'Egorova, V P', 'Kolosov, V A', 'Krasilnikov, A D', 'Pravdin, M I', 'Sleptsov, I Y']",['Azimuthal modulation of the event rate of cosmic ray extensive air showers by the geomagnetic field'],['Astrophysics and Astronomy'],"['cosmic radiation', 'showers, air', 'angular distribution', 'magnetic field, geophysics', 'correction, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903337'],"[""The Earth's magnetic field effect on the azimuthal distribution of extensive air showers (EAS) of cosmic rays has been evaluated using a bulk of the Yakutsk array data. The uniform azimuthal distribution of the EAS event rate is rejected at the significance level 10^(-14). Amplitude of the first harmonics of observed distribution depends on zenith angle as A1=0.2*sin^2(theta) and is almost independent of the primary energy; the phase coincides with the magnetic meridian. Basing upon the value of measured effect, the correction factor has been derived for the particle density depending on a geomagnetic parameter of a shower.""]",['1999-03-24'] +1199,['eng'],"['Croft, R A C', 'Hu, W', 'Davé, R']",['Cosmological Limits on the Neutrino Mass from the Ly$\\alpha$ Forest'],['Astrophysics and Astronomy'],"['neutrino, mass', 'spectra, quasar', 'mass, upper limit', 'mass, fluctuation', 'spectra, fluctuation', 'astrophysics, missing-mass', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903335'],"['The Lya forest in quasar spectra probes scales where massive neutrinos can strongly suppress the growth of mass fluctuations. Using hydrodynamic simulations with massive neutrinos, we successfully test techniques developed to measure the mass power spectrum from the forest. A recent observational measurement in conjunction with a conservative implementation of other cosmological constraints places upper limits on the neutrino mass: m_nu < 5.5 eV for all values of Omega_m, and m_nu < 2.4 (Omega_m/0.17 -1) eV, if 0.2 < Omega_m <0.5 as currently observationally favored (both 95 % C.L.).']",['1999-03-24'] +1200,['eng'],"['Salopek, D S']",['Generating Non-Gaussian Adiabatic Fluctuations from Inflation'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'inflationary universe', 'fluctuation, adiabatic', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'approximation, strong coupling', 'Hamilton-Jacobi equation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903327'],"['As the quality of cosmological data continue to improve, it is natural to test the statistics of primordial fluctuations: are they Gaussian or non-Gaussian? I review a model which generates non-Gaussian adiabatic fluctuations from inflation. Current investigations suggest that there may possibly be a non-Gaussian signal in large angle cosmic microwave background anisotropy data. Statistics of microwave anisotropies could thus serve as a powerful probe of the very early Universe.']",['1999-03-23'] +1201,['eng'],"['Schwarz, Dominik J', 'Schmid, C', 'Widerin, P']",['Clumping of CDM from the cosmological QCD transition'],['Astrophysics and Astronomy'],"['talk, Paris 1998/12/14', 'astrophysics, model', 'density, perturbation', 'quantum chromodynamics', 'critical phenomena', 'radiation, fluid', 'astrophysics, missing-mass', 'neutrino, decoupling', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903319'],"[""The cosmological QCD transition affects primordial density perturbations. If the QCD transition is first order, the sound speed vanishes during the transition and density perturbations fall freely. For scales below the Hubble radius at the transition the primordial Harrison-Zel'dovich spectrum of density fluctuations develops large peaks and dips. These peaks grow with wave number for both the radiation fluid and for cold dark matter (CDM). The peaks in the radiation fluid are wiped out during neutrino decoupling. For cold dark matter that is kinetically decoupled at the QCD transition (e.g. axions) these peaks lead to the formation of CDM clumps of masses $10^{-20} M_\\odot< M < 10^{-10} M_\\odot$.""]",['1999-03-23'] +1202,['eng'],"['Olive, Keith A']",['Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Paris 1998/12/14', 'astrophysics, model', 'light nucleus, production', 'chemistry', 'galaxy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903309'],['A brief review of standard big bang nucleosynthesis theory and the related observations of the light element isotopes is presented. Implications of BBN on chemical evolution and constraints on particle properties will also be discussed.'],['1999-03-22'] +1203,['eng'],"['Novosyadlyj, B', 'Durrer, R', 'Lukash, V N']",['An analytic approximation of MDM power spectra in four dimensional parameter space'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'density, perturbation', 'spectra, perturbation', 'neutrino, flavor', 'neutrino, density', 'baryon, density', 'cosmic radiation, background', 'Hubble constant', 'numerical methods', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811262'],"['An accurate analytic approximation of the transfer function for the power spectra of primordial density perturbations in mixed dark matter models is presented. The fitting formula in a matter-dominated Universe ($\\Omega_0=\\Omega_M=1$) is a function of wavenumber $k$, redshift $z$ and four cosmological parameters: the density of massive neutrinos, $\\Omega_{\\nu}$, the number of massive neutrino species, $N_{\\nu}$, the baryon density, $\\Omega_{b}$ and the dimensionless Hubble constant, $h$. Our formula is accurate in a broad range of parameters: $k\\le 100 h/Mpc$, $z\\le 30$, $\\Omega_{\\nu}\\le 0.5$, $N_{\\nu}\\le 3$, $\\Omega_{b}\\le 0.3$, $0.3\\le h\\le 0.7$. The deviation of the variance of density fluctuations from numerical results obtained with CMBfast is less than 2.5% for $\\Omega_bh^{2/N_{\\nu}}\\le 0.05$ and a Hubble parameter in the most interesting range of $0.5\\le h\\le 0.7$. For the broader interval, $0.3\\le h\\le 0.7$, the accuracy is still better than $\\le 5%$ for the entire range of $\\Omega_b$ if $N_{\\nu}=1$ and for $\\Omega_bh\\le 0.07$ if $N_{\\nu}=2,3$. The performance of the analytic approximation of MDM power spectra proposed here is compared with other approximations found in the literature. Our approximation turns out to be closest to numerical results in the parameter space considered here.']",['1998-11-19'] +1204,['eng'],"['Burles, S M', 'Nollett, K M', 'Turner, M S']",['Big-Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Atlanta 1999/03/20', 'astrophysics, model', 'light nucleus, production', 'history', 'baryon, density', 'astrophysics, missing-mass', 'cosmic radiation, background', 'helium, mass', 'neutrino, flavor', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903300'],"['We summarize the history, theory, observational status, and implications of big-bang nucleosynthesis.']",['1999-03-19'] +1205,['eng'],"['Abramo, L R W']",['Energy density an pressure of long wavelength gravitational waves'],['Astrophysics and Astronomy'],"['gravitational radiation, spectra', 'energy, density', 'perturbation, tensor', 'back reaction', 'inflationary universe', 'pressure']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903270'],"['Inflation leads us to expect a spectrum of gravitational waves (tensor perturbations) extending to wavelengths much bigger than the present observable horizon. Although these gravity waves are not directly observable, the energy density that they contribute grows in importance during the radiation- and dust-dominated ages of the universe. We show that the back reaction of tensor perturbations during matter domination is limited from above, since gravitational waves of wavelength $\\lambda$ have a share of the total energy density $\\Delta \\rho(\\lambda)/\\rho$ during matter domination that is at most equal to the share of the total energy density that they had when the mode be contrasted to that of Sahni, who analyzed the back reaction of gravity waves only insofar as their wavelengths are smaller than $H^{-1}$. Such a cut-off in the spectral energy of gravity waves leads to the breakdown of energy conservation, and we show that this anomaly is eliminated simply by taking into account the energy density and pressure of long wavelength gravitational waves as well as short wavelength ones.']",['1999-03-18'] +1206,['eng'],"['Weekes, T C']",['High Energy Astrophysics'],['Astrophysics and Astronomy'],"['talk, Los Angeles 1999/01/05', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'radiation, Cherenkov', 'imaging', 'photoelectron, amplifier', 'astrophysics', 'supersymmetry', 'quantum gravity', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903263'],"['The development of the atmospheric Cherenkov imaging technique has led to significant advances in gamma-ray detection sensitivity in the energy range from 200 GeV to 50 TeV. The Whipple Observatory 10m reflector has detected the first galactic and extragalactic sources in the Northern Hemisphere; the Crab Nebula has been established as the standard candle for ground-based gamma-ray astronomy. The highly variable Active Galactic Nuclei, Markarian 421 and Markarian 501, have proved to be particularly interesting. A new generation of telescopes with improved sensitivity has the promise of interesting measurements of fundamental phenomena in physics and astrophysics. VERITAS (the Very Energetic Radiation Imaging Telescope Array System) is one such next generation system; it is an array of seven large atmospheric Cherenkov telescopes planned for a site in southern Arizona.']",['1999-03-18'] +1207,['eng'],"['Bartlett, J G']",['The Standard Cosmological Model and CMB Anisotropies'],['Astrophysics and Astronomy'],"[""lectures, L'Aquila 1998/09/02"", 'Friedman model', 'space-time, Robertson-Walker', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'density, perturbation', 'gravitation', 'temperature, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903260'],"[""This is a course on cosmic microwave background (CMB) anisotropies in the standard cosmological model, designed for beginning graduate students and advanced undergraduates. ``Standard cosmological model'' in this context means a Universe dominated by some form of cold dark matter (CDM) with adiabatic perturbations generated at some initial epoch, e.g., Inflation, and left to evolve under gravity alone (which distinguishes it from defect models). The course is primarily theoretical and concerned with the physics of CMB anisotropies in this context and their relation to structure formation. Brief presentations of the uniform Big Bang model and of the observed large--scale structure of the Universe are given. The bulk of the course then focuses on the evolution of small perturbations to the uniform model and on the generation of temperature anisotropies in the CMB. The theoretical development is performed in the (pseudo--)Newtonian gauge because it aids intuitive understanding by providing a quick reference to classical (Newtonian) concepts. The fundamental goal of the course is not to arrive at a highly exact nor exhaustive calculation of the anisotropies, but rather to a good understanding of the basic physics that goes into such calculations.""]",['1999-03-18'] +1208,['eng'],"['Nelemans, G', 'Zwart, S F P', 'Verbunt, F']",['Gravitational waves from double white dwarfs'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1999/01/23', 'white dwarf', 'galaxy', 'gravitational radiation, spectra', 'n, matter', 'black hole', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903255'],"['Double white dwarfs could be important sources for space based gravitational wave detectors like OMEGA and LISA. We use population synthesis to predict the current population of double white dwarfs in the Galaxy and the gravitational waves produced by this population. We simulate a detailed power spectrum for an observation with an integration time of 10^6 s. At frequencies below ~3 mHz confusion limited noise dominates. At higher frequencies a few thousand double white dwarfs are resolved individually. Including compact binaries containing neutron stars and black holes in our calculations yields a further few hundred resolved binaries and some tens which can be detected above the double white dwarf noise at low frequencies. We find that binaries in which one white dwarf transfers matter to another white dwarf are rare, and thus unimportant for gravitational wave detectors. We discuss the uncertainties and compare our results with other authors.']",['1999-03-18'] +1209,['eng'],"['Iwazaki, A']",['A Possible Origin of $\\gamma$ Ray Bursts and Axionic Boson Stars'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'axion, matter', 'boson, matter', 'n, matter', 'matter, scattering', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903251'],"['We indicate a possible mechanism of generating gamma ray bursts. They are generated by a collision between an axionic boson star and a neutron star. The axionic boson star can dissipates its whole energy $10^{50}$ erg in the magnetized conducting medium of the neutron star. This dissipation arises only around envelope of the neutron star so that a fire ball with small baryon contamination is expected. We have evaluated roughly a rate of the collision per year and per galaxy which is consistent with observations, under plausible assumptions. We also point out that cosmic rays with extremely high energy, $10^{21}$eV, can be produced in the similar collisions with the neutron stars with strong magnetic fields $\\sim 10^{14}$G.']",['1999-03-18'] +1210,['eng'],"['Catanese, M']",['The Future of Cherenkov Astronomy'],['Astrophysics and Astronomy'],"['talk, Los Angeles 1999/01/05', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'radiation, Cherenkov', 'imaging', 'photoelectron, amplifier', 'astrophysics', 'supersymmetry', 'quantum gravity', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903244'],"['In the last ten years, the field of Cherenkov astronomy has become an important contributor to high energy astrophysics with the detection of eight objects at energies above 300 GeV. These observations have advanced our understanding of active galactic nuclei, supernova remnants, the extragalactic background light and cosmic-ray acceleration and production. Several efforts are now underway to develop new Cherenkov telescopes which will cover a wider range of energies (10 GeV - 50 TeV), improve the flux sensitivity by at least an order of magnitude and provide more accurate measures of particle energy and direction. I describe some of the new Cherenkov telescopes and discuss their potential to improve our understanding of astrophysics and fundamental physics.']",['1999-03-17'] +1211,['eng'],"['Roy, M F', 'Crawford, H J', 'Trattner, A']",['The Prediction and Detection of UHE Neutrino Bursts'],['Astrophysics and Astronomy'],"['talk, Los Angeles 1999/01/05', 'neutrino, cosmic radiation', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, string model', 'Cherenkov counter, water', 'deep underground detector, proposed']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903231'],"['In this paper we look at \\sim 10^14 eV neutrino bursts which are predicted to be observed in correlation with gamma ray bursts (GRBs). We describe an efficient way of constructing a km^2 effective area detector for these neutrino bursts. The proposed detector will cost <$3M and will operate in the 4-km deep water off St.Croix for at least one year, sufficient time to collect the expected \\sim 20 events in coincidence with satellite measured GRBs provided the fireball model is correct. Coincident gamma ray and neutrino bursts can be used to test the limits of the relativity principles.']",['1999-03-16'] +1212,['eng'],"['Liddle, A R']",['Aspects of inflationary reconstruction'],['Astrophysics and Astronomy'],"['talk, Paris 1998/12/14', 'inflationary universe, open', 'potential, inflaton', 'spectra, perturbation', 'space-time']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903195'],"['I review various aspects of techniques for reconstructing the potential of the inflaton field from observations, with special emphasis on difficulties which might arise. While my view is that if inflation is to prove viable then most likely it will be one of the simplest models, it is important to consider the impact should we need to move to a more complicated model-building realm.']",['1999-03-15'] +1213,['eng'],"['Urry, C M']",['Multiwavelength Properties of Blazars'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'blazar', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, jet', 'luminosity', 'synchrotron radiation', 'Compton scattering', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903189'],"['Blazar spectral energy distributions (SEDs) are double peaked and follow a self-similar sequence in luminosity. The so-called ""blue"" blazars, whose first SED component peaks at X-ray energies, are TeV sources, although with a relatively small fraction of their bolometric luminosities. The ""red"" blazars, with SED peaks in the infrared-optical range, appear to emit relatively more power in the gamma-ray component but at much lower energies (GeV and below). Correlated variations across the SEDs (of both types) are consistent with the picture that a single electron population gives rise to the high-energy parts of both SED components, via synchrotron at low energies and Compton-scattering at high energies. In this scenario, the trends of SED shape with luminosity can be explained by electron cooling on ambient photons. With simple assumptions, we can make some estimates of the physical conditions in blazar jets of each ""type"" and can predict which blazars are the most likely TeV sources. Upper limits from a mini-survey of candidate TeV sources indicate that only ~10% of their bolometric luminosity is radiated in gamma-rays, assuming the two SED components peak near 1 keV and 1 TeV. Finally, present blazar samples are too shallow to indicate what kinds of jets nature prefers, i.e., whether the low-luminosity ""blue"" blazars or the high-luminosity ""red"" blazars are more common.']",['1999-03-12'] +1214,['eng'],"['Castro-Tirado, A J']",['Cosmic gamma-ray bursts'],['Astrophysics and Astronomy'],"['review, experimental results', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'counters and detectors, satellite', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903187'],"['Gamma-Ray Bursts (GRBs) have remained a puzzle for many high-energy astrophysicists since their discovery in 1967. With the advent of the X-ray satellites BeppoSAX and RossiXTE, it has been possible to carry out deep multi-wavelength observations of the counterparts associated with the GRBs just within a few hours of occurence, thanks to the observation of the fading X-ray emission that follows the more energetic gamma-ray photons once the GRB event has ended. The fact that this emission (the afterglow) extends at longer wavelengths, has led to the discovery of the first optical/IR/radio counterparts in 1997-98, greatly improving our understanding of these sources. Now it is widely accepted that GRBs originate at cosmological distances but while the observed afterglow satisfies the predictions of the relativistic fireball models, the central engines that power these extraordinary events remain still unknown. Detailed results for nine selected GRBs are presented as well as a summary of the GRB counterparts and GRB host galaxies found so far.']",['1999-03-12'] +1215,['eng'],"['Morley, P D', 'Dib, C O', 'Schmidt, I']",['Neutrino scattering off spin-polarized particles in supernovae'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino electron, elastic scattering', 'antineutrino electron, elastic scattering', 'neutrino nucleon, elastic scattering', 'antineutrino nucleon, elastic scattering', 'electron, polarization', 'nucleon, polarization', 'magnetic field', 'temperature', 'n, matter', 'neutrino, emission', 'neutrino, flux', 'asymmetry', 'transport theory', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903186'],"['We calculate neutrino and antineutrino scattering off electrons and nucleons in supernovae using a detailed Monte Carlo transport code incorporating realistic equations of state. The goal is to determine whether particles in a neutron star core, partially spin-aligned by the local magnetic field, can give rise to asymmetric neutrino emission via the standard parity breaking weak force. We conclude that electron scattering in a very high magnetic field does indeed give a net asymmetry, but that nucleon scattering, if present, removes the asymmetry.']",['1999-03-12'] +1216,['eng'],"['Sarkar, S']",['Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Heidelberg 1998/07/20', 'astrophysics, model', 'light nucleus, production', 'astrophysics, missing-mass', 'baryon, matter', 'neutrino, flavor', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903183'],"['Recent observational and theoretical developments concerning the primordial synthesis of the light elements are reviewed, and the implications for dark matter mentioned.']",['1999-03-12'] +1217,['eng'],"['Medina-Tanco, G A', 'Watson, A A']",['Dark matter halos and the anisotropy of ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, anisotropy', 'cosmic radiation, particle source', 'particle, massive', 'particle, decay', 'astrophysics, missing-mass', 'galaxy', 'amplitude analysis', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903182'],['Several explanations for the existence of Ultra High Energy Cosmic Rays invoke the idea that they originate from the decay of massive particles created in the reheating following inflation. It has been suggested that the decay products can explain the observed isotropic flux of cosmic rays. We have calculated the anisotropy expected for various models of the dark matter distribution and find that at present data are too sparse above $4 \\times 10^{19}$ eV to discriminate between different models. However we show that with data from three years of operation of the southern section of the Pierre Auger Observatory significant progress in testing the proposals will be made.'],['1999-03-12'] +1218,['eng'],"['Graff, D S', 'Freese, Katherine', 'Walker, T', 'Pinsonneault, M H']",['Constraining the cosmic abundance of stellar remnants with multi-TeV $\\gamma$-rays'],['Astrophysics and Astronomy'],"['astrophysics, model', 'galaxy', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'photon photon, fusion', 'electron, pair production', 'astrophysics, missing-mass', 'baryon', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903181'],"['If galactic halos contain stellar remnants, the infra-red flux from the remnant progenitors would contribute to the opacity of multi-TeV gamma-rays. The multi-TeV gamma-ray horizon is established to be at a redshift z>0.034 by the observation of the blazar Mkn501 . By requiring that the optical depth due to \\gamma \\gamma ---> e+ e- be less than one for a source at z=0.034 we limit the cosmological density of stellar remnants, Omega_rm \\le (2-4) x 10^-3 h_70^-1 (h_70 is the Hubble constant in units of 70 km sec-1 Mpc-1) and thus strongly constrain stellar remnants as a cosmologically significant source of dark matter.']",['1999-03-12'] +1219,['eng'],"['Copeland, E J', 'Magueijo, J', 'Steer, D A']",['Cosmological parameter dependence in local string theories of structure formation'],['Astrophysics and Astronomy'],"['astrophysics, string', 'string, network', 'gravitation, back reaction', 'cosmic radiation, background', 'astrophysics, missing-mass', 'spectra, fluctuation', 'baryon, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903174'],"[""We perform the most accurate study to date of the dependence on cosmological parameters of structure formation with local cosmic strings. The crucial new ingredients are the inclusion of the effects of gravitational backreaction on the evolution of the network, and the accurate evolution of the network through the radiation to matter transition. Our work re-iterates the fact that expanding Universe numerical simulations only probe a transient regime, and we incorporate our results into the unequal time correlators recently measured. We then compute the CMB and CDM fluctuations' power spectra for various values of the Hubble constant $H_0$ and baryon fraction $\\Omega_b$. We find that, whereas the dependence on $\\Omega_b$ is negligible, there is still a strong dependence on $H_0$.""]",['1999-03-12'] +1220,['eng'],"['Jones, A W']",['Application of novel analysis techniques to Cosmic Microwave Background astronomy'],['Astrophysics and Astronomy'],['Thesis'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903173'],['The data from Cosmic Microwave Background (CMB) experiments are becoming more complex with each new experiment. A consistent way of analysing these data sets is required so that direct comparison is possible between the various experimental results. This thesis presents several techniques that can be used to analyse CMB data.'],['1999-03-12'] +1221,['eng'],"['Bieber, J W', 'Burger, R A', 'Engel, R', 'Gaisser, T K', 'Roesler, S', 'Stanev, T']",['Antiprotons at Solar Maximum'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'anti-p, cosmic radiation', 'anti-p, flux', 'p, flux', 'flux, ratio', 'time variation', 'model, solar', 'p, interaction', 'gas', 'anti-p, energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903163'],"['New measurements with good statistics will make it possible to observe the time variation of cosmic antiprotons at 1 AU through the approaching peak of solar activity. We report a new computation of the interstellar antiproton spectrum expected from collisions between cosmic protons and the interstellar gas. This spectrum is then used as input to a steady-state drift model of solar modulation, in order to provide predictions for the antiproton spectrum as well as the antiproton/proton ratio at 1 AU. Our model predicts a surprisingly large, rapid increase in the antiproton/proton ratio through the next solar maximum, followed by a large excursion in the ratio during the following decade.']",['1999-03-11'] +1222,['eng'],"['Aharonian, F A', 'Coppi, P S']",['Understanding the Spectra of TeV Blazars'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'astrophysics, balazar', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'energy spectrum', 'cosmic radiation, background', 'synchrotron radiation', 'Compton scattering', 'absorption', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903160'],"[""With the arrival of powerful, ground-based gamma-ray detectors, we can now begin to seriously probe, via simultaneous X-ray/TeV observations, the origin of the gamma-ray emission in the blazars Mrk 421 and 501. If the synchrotron-Compton emission model turns out to work, then we know that the same electrons are responsible for both the X-ray and the gamma-ray emission of these objects. In this case, we show that we can use their observed X-ray spectra to robustly estimate their intrinsic gamma-ray spectra. Among blazars, Mrk 421/501 are particularly well-suited for this task because the Compton scattering which produces their TeV gamma-rays is likely to be in the Klein-Nishina limit, where the outgoing photon has an energy insensitive to the incoming photon energy. With a better handle on their intrinsic TeV spectra, we can then begin to search for evidence of absorption due to gamma-ray pair production on diffuse infrared background radiation. We discuss some of the pitfalls that arise when one attempts to do this without knowing the intrinsic spectrum. Although Mrk 421/501 are very nearby, the emission of these sources extends to sufficiently high energies (> 20 TeV in Mrk 501) that we may nevertheless be able to derive interesting constraints on the infrared background. If correct, the combination of the COBE 140 micron detection and the measurement of Mrk 501's spectrum out to 20 TeV and perhaps beyond rules out conventional galaxy evolution and star formation scenarios, implying that much of the star formation in the Universe indeed occurs at early times in highly obscured sources that have been missed until now.""]",['1999-03-11'] +1223,['eng'],"['Anchordoqui, L A', 'Romero, G E', 'Combi, J A']",['Heavy nuclei at the end of the cosmic ray spectrum?'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, acceleration', 'astrophysics, galaxy', 'iron, energy loss', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903145'],"['We provide an account of the possible acceleration of iron nuclei up to energies $\\sim300$ EeV in the nearby, metally-rich starburst galaxy NGC 253. It is suggested that particles can escape from the nuclear region with energies of galactic superwind generated by the starburst, avoiding in this way the photodisintegration expected if the nuclei were accelerated in the central region of high photon density. We have also made estimates of the expected arrival spectrum, which display a strong dependency with the energy cutoff at the source.']",['1999-03-11'] +1224,['eng'],"['Khokhlov, D L']",['Internal structure of the star in the fractal universe and solar neutrino puzzle'],['Astrophysics and Astronomy'],"['astrophysics, matter', 'astrophysics, model', 'fractals', 'temperature', 'neutrino, solar', 'neutrino, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903134'],"['The internal structure of the Newton star with the uniform density is considered within the framework of the fractal universe with a power index of 2. The temperature profile in the star follows the law of 4/3. With the use of this profile, the neutrino flux from the sun is estimated. The obtained value of the neutrino flux may provide a solution for the solar neutrino puzzle.']",['1999-03-24'] +1225,['eng'],"['Takahashi, T', 'Madejski, G M', 'Kubo, H']",['X-ray Observations of TeV Blazars and Multi-Frequency Analysis'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, blazar', 'synchrotron radiation', 'Compton scattering', 'magnetic field', 'electron, relativistic', 'galaxy', 'quasar', 'cosmic radiation, jet', 'experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903099'],"['The non-thermal spectra of blazars, observed from radio to GeV/TeV gamma-rays, reveal two pronounced components, both produced by radiation by energetic particles. One peaks in the IR - to soft X-ray band, radiating via the synchrotron process; the other, peaking in the high-energy gamma-rays, is produced by the Compton process. These spectra -- and, in particular, the \\asca data -- suggest that the origin of the seed photons for Comptonization is diverse. In the High-energy peaked BL Lac objects (HBLs), the dominant seed photons for Comptonization appear to be the synchrotron photons internal to the jet (SSC process). In the quasar-hosted blazars (QHBs), on the other hand, the X-ray band emission is still dominated by the SSC process, while the MeV to GeV range is produced by Comptonization of external photons such as the emission line light. In the context of this three-component model, we derive the magnetic field of 0.1 - 1 Gauss for all classes of blazars. Lorentz factors gamma_{peak} of electrons radiating at each peak of the nuFnu spectra are estimated to be ~10^{5}$ for HBLs; this is much higher than ~10^{3}$ for QHBs. This difference is consistent with the fact that the four sources that are known to emit TeV gamma-rays (TeV blazars) are all classified as HBLs. Among the TeV blazars, Mkn 421 is one of the brightest and most variable emitters from ultraviolet (eV) to hard gamma-ray (TeV) energies.The multi-frequency observations including TeV energy band provide the best opportunity to understand high-energy emission from blazar jets. In this paper, we discuss results of multi-frequency analysis and review the results of intensive campaigns for Mkn 421 from 1994 to 1998']",['1999-03-09'] +1226,['eng'],"['Biswas, S', 'Shaw, A', 'Modak, B']",['Decoherence In Starobinsky Model'],['Astrophysics and Astronomy'],"['inflationary universe', 'Wheeler-DeWitt equation', 'space-time, fluctuation', 'Schroedinger equation', 'decoherence', 'quantum gravity']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903097'],"[""Starobinsky described an inflationary scenario in which quantum corrections to vacuum Einstein's equations drive the inflation. The quantum cosmology of the model is studied by solving Wheeler-DeWitt equation. A connection between uncertainty requirement, randomness in initial states as well as curvature fluctuation is studied with a Schroedinger-type equation through a time parameter prescription. The result so obtained is applied to understand the decoherence mechanism in quantum gravity in Starobinsky description.""]",['1999-03-09'] +1227,['eng'],"['Balkanov, V A']",['In situ measurements of optical parameters in Lake Baikal with the help of a Neutrino Telescope'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'Cherenkov counter, water', 'photoelectron, amplifier', 'optics, absorption', 'radiation, laser', 'calibration', 'deep underground detector, Baikal']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903342'],"['We present results of an experiment performed in Lake Baikal at a depth of about 1 km. The photomultipliers of an underwater neutrino telescope under construction at this site have been illuminated by a distant laser. The experiment not only provided a useful cross-check of the time calibration of the detector, but also allowed to determine inherent optical parameters of the water in a way complementary to standard methods. In 1997, we have measured an absorption length of 22 m and an asymptotic attenuation length of 18 m. The effective scattering length was measured as 480 m. Using = 0.95 (0.90) for the average scattering angle, this corresponds to a geometrical scattering length of 24 (48) m.']",['1999-03-24'] +1228,['eng'],"['Khanna, R']",['Generation and evolution of magnetic fields in the gravitomagnetic field of a Kerr Black Hole'],['Astrophysics and Astronomy'],"['talk, Rome 1998/06/29', 'black hole, Kerr', 'black hole, rotational', 'electron, plasma', 'magnetic field, production', 'potential', 'current', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903091'],"[""I study the generation and evolution of magnetic fields in the plasma surrounding a rotating black hole. Attention is focused on effects of the gravitomagnetic potential. The gravitomagnetic force appears as battery term in the generalized Ohm's law. The generated magnetic field should be stronger than fields generated by the classical Biermann battery. The coupling of the gravitomagnetic potential with electric fields appears as gravitomagnetic current in Maxwell's equations. In the magnetohydrodynamic induction equation, this current re-appears as source term for the poloidal magnetic field, which can produce closed magnetic structures around an accreting black hole. In principle, even self-excited axisymmetric dynamo action is possible, which means that Cowling's anti dynamo theorem does not hold in the Kerr metric. Finally, the structure of a black hole driven current is studied.""]",['1999-03-08'] +1229,['eng'],"['Fargion, D', 'Golubkov, Yu A', 'Khlopov, M Ya', 'Konoplich, R V', 'Mignani, R P']",['Possible Effects of the Existence of the 4th Generation Neutrino'],['Astrophysics and Astronomy'],"['neutrino, massive', 'family, 4', 'neutrino, mass', 'string model, heterotic', 'astrophysics, model', 'astrophysics, missing-mass', 'neutrino antineutrino, annihilation', 'galaxy', 'cosmic radiation, background', 'electron positron, annihilation', 'lepton, pair production', 'neutrino, pair production', 'photon, associated production', 'neutralino, annihilation', 'photon, flux', 'channel cross section, energy dependence', 'positron, flux', 'anti-p, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903086'],"['The 4th generation of fermions predicted by the phenomenology of heterotic string models can possess new strictly conserved charge, which leads, in particular, to the hypothesis of the existence of the 4th generation massive stable neutrino. The compatibility of this hypothesis with the results of underground experiment DAMA searching for weakly interactive particles of dark matter and with the EGRET measurements of galactic gamma--background at energies above 1 GeV fixes the possible mass of the 4th neutrino at the value about 50 GeV. The possibility to test the hypothesis in accelerator experiments is considered. Positron signal from the annihilation of relic massive neutrinos in the galactic halo is calculated and is shown to be accessible for planned cosmic ray experiments.']",['1999-03-08'] +1230,['eng'],"['Capozziello, S', 'Iovane, G']",['On-Line Selection and Quasi-On-Line Analysis of Data using the Pixel Lensing Technique'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'relativity theory, general', 'gravitation, lens', 'semiconductor, optical', 'semiconductor detector, pixel']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903085'],"['Pixel lensing is a technique for searching baryonic components of dark matter, (MACHOs), in any part of galaxies. This method is very efficient, since it avoids to resolve each source star and so it has the advantage to provide an high statistic. Taking into account the fact that this technique is very time expensive in data analysis phase and the present technology, we propose a new method to perform a data selection on-line by using two levels of trigger and a quasi-on-line data analysis. The implementation of the project provides to obtain soon results since, due to a new database technology, all physical information are stored for a complementary and secondary analysis to perform off-line.']",['1999-03-08'] +1231,['eng'],"['Biswas, S', 'Modak, B', 'Shaw, A']",['Wormhole Dominance Proposal and Wave Function Discord'],['Astrophysics and Astronomy'],"['wormhole', 'astrophysics, wave function', 'WKB approximation, correction', 'tunneling', 'black hole']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903082'],"['Using the wormhole dominance proposal, it is shown that quantum corrections to the usual WKB ansatz for the wave function of the universe ably circumvent many of the drawbacks present in the current proposals. We also find that the recent criticism by Hawking and Turok does not apply to the tunneling proposal.']",['1999-03-08'] +1232,['eng'],"['Baccigalupi, C']",['Cosmic microwave background'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'temperature, anisotropy', 'polarization, anisotropy', 'symmetry, sphere', 'symmetry, cylinder', 'spectra, perturbation', 'numerical calculations']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811176', 'http://www-lib.fnal.gov/archive/1999/pub/Pub-98-204-A.html']","['I explore the undulatory properties of the cosmic microwave background (CMB) physics. I consider the cases of spherical and cylindrical symmetry of the perturbation source, or seed. Such structures could have been left by high energy symmetries breaking in the early universe. I give suitable analytic expressions for the polarization and temperature linear perturbations from this kind of seeds and I show how to get their appearence on the CMB sky. This treatment highlights the undulatory properties of the CMB. I show with numerical examples how the polarization and temperature perturbations propagate beyond the size of their seeds, reaching the CMB sound horizon at the time considered. Just like the waves from a pebble thrown in a pond, the CMB anisotropy appears as a series of temperature and polarization waves surrounding the seed, extending on the scale of the CMB sound horizon at decoupling, roughly $1^{o}$ in the sky. Each wave is characterized by its own value of the CMB perturbation, with the same mean amplitude of the signal coming from the seed interior. These waves could allow to distinguish relics of the very early universe from point-like astrophysical sources, because of their angular extension and amplitude. Also, the analogy between the polarization and temperature CMB signals offers cross correlation possibilities for the future detection instruments like the Planck Surveyor satellite.']",['1998-11-12'] +1233,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Mikhailov, A A']",['Anisotropy of ultra high energy cosmic rays in the dark matter halo model'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'cosmic radiation, anisotropy', 'cosmic radiation, particle source', 'postulated particle, heavy', 'postulated particle, decay', 'galaxy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810277'],['The harmonic analysis of anisotropy of Ultra High Energy Cosmic Rays is performed for the halo model. In this model the relic superheavy particles comprise the part of Dark Matter and are concentrated in the Galactic halo. The Ultra High Energy Cosmic Rays are produced at the decays of these particles. Anisotropy is caused by asymmetric position of the Sun in the Galactic halo. The maximum anisotropy reaches 40% and in this case some versions of the halo model can be excluded by the AGASA data.'],['1998-10-20'] +1234,['eng'],"['Hertog, T', 'Turok, Neil G']",['Gravity Waves from Instantons'],['Astrophysics and Astronomy'],"['gravitational radiation, spectra', 'inflationary universe, open', 'space-time', 'saddle-point approximation, instanton', 'path integral', 'fluctuation, tensor', 'two-point function', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'propagator, Euclidean', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903075'],['We perform a first principles computation of the spectrum of gravity waves produced in open inflationary universes. The background spacetime is taken to be the continuation of an instanton saddle point of the Euclidean no boundary path integral. The two-point tensor correlator is computed directly from the path integral and is shown to be unique and well behaved in the infrared. We discuss the tensor contribution to the cosmic microwave background anisotropy and show how it may provide an observational discriminant between different types of primordial instantons.'],['1999-03-09'] +1235,['eng'],"['Magueijo, J', 'Contaldi, C', 'Hindmarsh, M B']",['Structure formation with strings plus inflation'],['Astrophysics and Astronomy'],"['talk, Rome 1998/10/05', 'inflationary universe', 'astrophysics, string', 'density, perturbation', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'topology, defect', 'spectra, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903050'],"['Recent developments in inflation model building, based on supersymmetry, have produced compelling models in which strings are produced at the end of inflation. In such models the cosmological perturbations are seeded both by the defects and by the quantum fluctuations. We show that such models produce qualitatively new and desirable predictions for CMB anisotropies and the CDM power spectrum. This remark should put an end to the long term animosity between defect and inflationary scenarios of structure formation.']",['1999-03-03'] +1236,['eng'],"['Vachaspati, T']",['Remarks on Inflation'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'inflationary universe', 'quantum cosmology', 'Friedman model']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903039'],['It has been shown that sub-Planckian models of inflation require initial homogeneity on super-Hubble scales under certain commonly held assumptions. Here I remark on the possible implications of this result for inflationary cosmology.'],['1999-03-03'] +1237,['eng'],"['Hannestad, S']",['Non-equilibrium effects on particle freeze-out in the early universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'particle, massive', 'statistical mechanics', 'Boltzmann equation, solution', 'particle, Dirac', 'particle, Majorana', 'particle, decoupling', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903034'],"['We investigate the possible effects that deviations from kinetic equilibrium can have on massive particles as they decouple from chemical equilibrium. Different methods of solving the Boltzmann equation yield significantly different relic number densities of such particles. General considerations concerning the Dirac or Majorana structure of the particles are discussed. It is shown that non-equilibrium effects are small for particles decoupling while strongly non-relativistic, as will be the case for most cold dark matter candidates.']",['1999-03-03'] +1238,['eng'],"['Ziaeepour, H']",['Initial Data Set For Cosmology'],['Astrophysics and Astronomy'],"['astrophysics', 'gravitation', 'boundary condition', 'space-time, conformal', 'Einstein equation, linear', 'critical phenomena', 'perturbation theory, higher-order']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903033'],"['In Einstein theory of gravity the initial configuration of metric field and its time derivative are related to matter configuration by four equations called constraints. We use the method of conformal metrics (York Method) to solve constraints and find an analytic set of consistent initial data for linearized Einstein field equations in a perturbed constant curvature space-time. As an application example, we use this method to determine matching conditions during a phase transition. The results are explicitly covariant and more compact than decomposition of quantities to scalar, vector and tensor. This method is independent of type and physics of matter fields and is extendable to higher-order perturbative calculations.']",['1999-03-03'] +1239,['eng'],"['Lykken, J D']",['New and Improved Superstring Phenomenology'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'inflationary universe', 'string model', 'supersymmetry', 'astrophysics, fundamental constant', 'space-time, singularity', 'astrophysics, missing-mass', 'moduli space', 'membrane model']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903026'],"['Recent developments in string theory have important implications for cosmology. Topics discussed here are inflation, the cosmological constant, smoothing of cosmological singularities, and dark matter from parallel universes. Talk presented at the International Workshop on Particle Physics and the Early Universe (COSMO-98), 15-20 Nov, Asilomar, Monterey, CA.']",['1999-03-03'] +1240,['eng'],"['Morales, A']",['Particle Dark Matter and its Detection'],['Astrophysics and Astronomy'],"['review, Rome 1996/11/04', 'astrophysics, missing-mass', 'search for, missing-mass', 'baryon, matter', 'neutrino', 'WIMP', 'axion', 'proposed experiment', 'counters and detectors, missing-mass', 'deep underground detector', 'experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810341'],"['The status and prospects of the experimental efforts in the detection of Particle Dark Matter is reviewed. Emphasis is put in the direct searches for WIMPs (Weakly Interacting Massive Particles), outlining the various strategies and techniques currently followed and sumarizing the results. A briefing of the indirect methods of WIMP detection is also presented.']",['1998-10-22'] +1241,['eng'],"['Ioka, K', 'Tanaka, T', 'Nakamura, T']",['Density Distribution and Shape of Galactic Dark Halo Can be Determined by Low Frequency Gravitational Waves?'],['Astrophysics and Astronomy'],"['black hole, MACHO', 'galaxy', 'mass, density', 'gravitational radiation', 'counters and detectors, interference', 'astrophysics, missing-mass', 'gravitation, lens', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903011'],"[""Under the assumption that the Milky Way's dark halo consists of primordial black hole MACHOs (PBHMACHOs), the mass density of the halo can be measured by the low frequency gravitational waves ($10^{-3} Hz \\siml \\nu_{gw} \\siml 10^{-1}$ Hz) from PBHMACHO binaries whose fraction is $\\sim 10^{-6}$. We find that ten years observation by LISA will detect $\\sim 700$ PBHMACHO binaries and enable us to determine the power index of the density profile within 10% (20%) and the core radius within 25% (50%) in about 90% (99%) confidence level, respectively. The axial ratios of the halo may also be determined within $\\sim 10%$. LISA and OMEGA may give us an unique observational method to determine the density profile and the shape of the dark halo to open a new field of observational astronomy.""]",['1999-03-02'] +1242,['eng'],"['Giovannini, M']",['Production and detection of relic gravitons in quintessential inflationary models'],['Astrophysics and Astronomy'],"['inflationary universe', 'quintessence', 'gravitational radiation', 'graviton, energy spectrum', 'graviton, production', 'energy, density', 'graviton, particle identification', 'counters and detectors', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903004'],"['A large class of quintessential inflationary models, recently proposed by Peebles and Vilenkin, leads to post-inflationary phases whose effective equation of state is stiffer than radiation. The expected gravitational waves logarithmic energy spectra are tilted towards high frequencies and characterized by two parameters: the inflationary curvature scale at which the transition to the stiff phase occurs and the number of (non conformally coupled) scalar degrees of freedom whose decay into fermions triggers the onset of a gravitational reheating of the Universe. Depending upon the parameters of the model and upon the different inflationary dynamics (prior to the onset of the stiff evolution) the relic gravitons energy density can be much more sizeable than in standard inflationary models, for frequencies larger than 1 Hz. We estimate the required sensitivity for detection of the predicted spectral amplitude and show that the allowed region of our parameter space leads to a signal smaller (by one 1.5 orders of magnitude) than the advanced LIGO sensitivity at a frequency of 0.1 KHz. The maximal signal, in our context, is expected in the GHz region where the energy density of relic gravitons in critical units (i.e. $h_0^2 \\Omega_{GW}$) is of the order of $10^{-6}$, roughly eight orders of magnitude larger than in ordinary inflationary models. Smaller detectors (not necessarily interferometers) can be relevant for detection purposes in the GHz frequency window. We suggest/speculate that future measurements through microwave cavities can offer interesting perspectives.']",['1999-03-02'] +1243,['eng'],"['Ellis, Jonathan Richard']",['Limits on Sparticle Dark Matter'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'astrophysics, missing-mass', 'supersymmetry', 'neutralino', 'electroweak interaction', 'vacuum state', 'stability', 'sparticle, annihilation', 'LSP, mass', 'electron positron, annihilation', 'sparticle, search for', 'mass, constraint', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9903003'],"['Arguments are given that the lightest supersymmetric particle should be a neutralino $\\chi$. Minimizing the fine tuning of the gauge hierarchy favours space of the MSSM from the stability of the electroweak vacuum. Co-annihilation with the next-to-lightest supersymmetric particle is potentially significant. Incorporating the latest accelerator constraints from LEP and elsewhere, we find that 50 GeV $\\lappeq m_\\chi \\lappeq$ 600 GeV and $\\tan\\beta \\gappeq$ 2.5, if soft supersymmetry breaking parameters are assumed to be universal.']",['1999-03-02'] +1244,['eng'],"['Glendenning, N K', 'Schaffner-Bielich, J']",['First Order Kaon Condensate'],['Astrophysics and Astronomy'],"['nuclear matter', 'isospin, asymmetry', 'n, matter', 'K, condensation', 'thermodynamics', 'potential, chemical', 'charge, density', 'critical phenomena', 'Lagrangian formalism', 'mean field approximation, relativistic', 'energy, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810290'],"['First order Bose condensation in asymmetric nuclear matter and in neutron stars is studied, with particular reference to kaon condensation. We demonstrate explicitly why the Maxwell construction fails to assure equilibrium in multicomponent substances. Gibbs conditions and conservation laws require that for phase equilibrium, the charge density must have opposite sign in the two phases of isospin asymmetric nuclear matter. The mixed phase will therefore form a Coulomb lattice with the rare phase occupying lattice sites in the dominant phase. Moreover, the kaon condensed phase differs from the normal phase, not by the mere presence of kaons in the first, but also by a difference in the nucleon effective masses. The mixed phase region, which occupies a large radial extent amounting to some kilometers in our model neutron stars, is thus highly heterogeneous. It should be particularly interesting in connection with the pulsar glitch phenomenon as well as transport properties.']",['1998-10-20'] +1245,['eng'],"['Scopel, S', 'Irastorza, I G', 'Cebrian, S', 'García, E', 'González, D', 'Morales, A', 'Morales, J', 'De Solorzano, A O', 'Puimedón, J', 'Salinas, A', 'Sarsa, M L', 'Villar, J A']",['Theoretical expectations and experimental prospects for solar axions searches with crystal detectors'],['Astrophysics and Astronomy'],"['talk, Buxton 1998/09/07', 'axion, solar', 'axion, flux', 'axion, search for', 'transition, axion photon', 'Primakoff effect', 'solid-state counter, crystal', 'coupling constant, (axion 2photon)', 'axion, mass', 'time, correlation', 'background', 'experimental methods, proposed', 'numerical calculations', 'axion --> 2photon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810308'],['A calculation of the expected signal due to Primakov coherent conversion of solar axions into photons via Bragg scattering in several solid--state detectors is presented and compared with present and future experimental sensitivities. The axion window m_a>~0.03 eV (not accessible at present by other techniques) could be explored in the foreseeable future with crystal detectors to constrain the axion--photon coupling constant below the latest bounds coming from helioseismology. On the contrary a positive signal in the sensitivity region of such devices would imply revisiting other more stringent astrophysical limits derived for the same range of the axion mass.'],['1998-10-21'] +1246,['eng'],"['De Garcia-Maia, M R', 'Carvalho, J C', 'Neto, C S C']",['Quantum corrections to Maxwell electrodynamics in a homogeneous and isotropic universe with cosmological constant'],['Astrophysics and Astronomy'],"['Maxwell equation', 'quantization, correction', 'magnetic field, time dependence', 'astrophysics, fundamental constant', 'effective Lagrangian', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902380'],"['Some cosmological consequences of first order quantum corrections to Maxwell electrodynamics are investigated in the context of a spatially flat homogeneous and isotropic universe driven by a magnetic field plus a cosmological term corresponding to the particular one recently found by Novello et al. [gr-qc/9806076]. We also find a general solution for the case when $\\Lambda$ is a non-vanishing constant. Both solutions describe a non-singular, bouncing universe. However, we show that the first order correction to the electromagnetic Lagrangean density, in which the analysis is based, fails to describe the dynamics near $a_{min}$. The time range where the first order approximation can be used is explicitly evaluated. These problems my be circumvented through the use of higher order terms in the effective Lagrangean, as numerical calculations performed by Novello et al. [gr-qc/9809080], for the vanishing $\\Lambda$ case, have indicated. A third general solution corresponding to a constant magnetic field sustained by a time dependent cosmic history and describes a universe that, although with vanishing curvature (K=0), has a scale factor that reaches a maximum and then contracts back to an arbitrarilly small size. The cosmological term decays during the initial expansion phase and increases during the late contraction phase, so as to keep $B$ constant throughout.']",['1999-03-01'] +1247,['eng'],"['Schlattl, H', 'Bonanno, A', 'Paternò, L']",['Signature of the efficiency of solar nuclear reactions in the neutrino experiments'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, oscillation', 'model, solar', 'nuclear reaction', 'neutrino, mixing angle', 'neutrino, flux', 'angular dependence', 'neutrino electron, elastic scattering', 'neutrino deuteron, nuclear reaction', 'electron, energy spectrum', 'electron, recoil', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902354'],"['In the framework of the neutrino oscillation scenario, we discuss the influence of the uncertainty on the efficiency of the neutrino emitting reactions 1H(p,e+ \\nu_e)2H and 7Be(p,\\gamma)8B for the neutrino oscillation parameters. We consider solar models with zero-energy astrophysical S-factors S_11 and S_17 varied within nuclear physics uncertainties, and we test them by means of helioseismic data. We then analyse the neutrino mixing parameters and recoil electron spectra for the presently operating neutrino experiments and we predict the results which can be obtained from the recoil electron spectra in SNO and Borexino experiments. We suggest that it should be possible to determine tight bounds to S_17 from the results of the future neutrino experiment, in the case of matter-enhanced oscillations of active neutrinos.']",['1999-02-26'] +1248,['eng'],"['Boldt, E A', 'Ghosh, P']",['Cosmic rays from remnants of quasars?'],['Astrophysics and Astronomy'],"['quasar', 'black hole', 'cosmic radiation, acceleration', 'cosmic radiation, flux', 'p, cosmic radiation', 'galaxy, AGN', 'showers, air', 'magnetic field', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902342'],"['Considerations of the collision losses for protons traversing the 2.7 K black body microwave radiation field have led to the conclusion that the highest energy cosmic rays, those observed at $\\geq 10^{20}$ eV, must come from sources within the present epoch. In light of this constraint, it is here suggested that these particles may be accelerated near the event horizons of spinning supermassive black holes associated with presently inactive quasar remnants. The required emf is generated by the black hole induced rotation of externally supplied magnetic field lines threading the horizon. Producing the observed flux of the highest energy cosmic rays would constitute a negligible drain on the black hole dynamo. Observations with upcoming air shower arrays and space missions may lead to the identification of candidate dormant galaxies which harbor such black holes. Although the highest energy events observed so far are accounted for within the context of this scenario, a spectral upper bound at to be precluded, on general grounds.']",['1999-02-25'] +1249,['eng'],"['Grarcia De Maia, M R', 'Carvalho, J C', 'Alcaniz, J S']",['Cosmological gravitons and the expansion dynamics during the matter age'],['Astrophysics and Astronomy'],"['astrophysics, model', 'graviton', 'back reaction', 'perturbation, tensor', 'gravitational radiation', 'matter, density', 'light nucleus, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902338'],"['Extending previous results [Phys. Rev.D {\\bf 56}, 6351 (1997)], we estimate the back reaction of cosmological gravitons in the expansion dynamics, during the matter age. Tensor perturbations with scales larger than the Hubble radius are created due to the inequivalence of vacua at different times. During noninflationary phases these perturbations become effective gravitational waves as they enter the Hubble radius, adding new contributions to the energy density of the subhorizon waves. During the radiation epoch the creation of these effective gravitons may lead to a departure from the standard behaviour $a(t)\\propto t^{1/2}$, with possible consequences to several cosmic processes, such as primordial nucleosynthesis. We examine the implications of this phenomenom during the matter dominated era, assuming an initial inflationary period. The dynamical equation obeyed by the scale factor is derived and numerically solved for different values of the relevant parameters involved.']",['1999-02-24'] +1250,['eng'],"['Fargion, D', 'Konoplich, R V', 'Grossi, M', 'Khlopov, M Ya']",['On the Heavy Relic Neutrino'],['Astrophysics and Astronomy'],"['talk, Buxton 1998/09/07', 'neutrino, cosmic radiation', 'photon, cosmic radiation', 'galaxy', 'neutrino, heavy', 'flavor, 4', 'neutrino, mass', 'neutrino, annihilation', 'electron, pair production', 'photon, production', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902327'],"['A halo model with heavy relic neutrinos N belonging to a fourth generation and their annihilations in galactic halo may explain the recent evidence of diffused gamma (GeV) radiation around galactic plane. We considered a neutrino mass in the narrow range ($M_Z/2 < m_N < M_Z$) and two main processes as source of gamma rays. A first one is ICS of ultrarelativistic electron pair on IR and optical galactic photons and a second due to prompt gammas by $\\pi^0$ decay, leading to a gamma flux ($10^{-7} - 10^{-6} /(cm^2 s sr)$) comparable to EGRET detection. Our predictions are also compatible with the narrow window of neutrino mass $45 GeV < m_N < 60 GeV$, required to explain the recent underground DAMA positive signals.']",['1999-02-24'] +1251,['eng'],"['Blanco-Pillado, J J', 'Vázquez, R A', 'Zas, E']",['High Energy Cosmic Rays from Neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, flux', 'showers, air', 'neutrino, density', 'galaxy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902266'],"['We discuss recent models in which neutrinos, which are assumed to have mass in the eV range, originate the highest energy cosmic rays by interaction with the enhanced density in the galactic halo of the relic cosmic neutrino background. We make an analytical calculation of the required neutrino fluxes to show that the parameter space for these models is constrained by horizontal air shower searches and by the total number of background neutrinos, so that only models which have fairly unnatural halo sizes and enhanced densities are allowed.']",['1999-02-23'] +1252,['eng'],"['Gratton, S', 'Turok, Neil G']",['Cosmological Perturbations from the No Boundary Euclidean Path Integral'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'path integral, Euclidean', 'relativity theory, general', 'field theory, scalar', 'vacuum state, fluctuation', 'instanton', 'two-point function', 'propagator, Euclidean', 'propagator, Lorentz', 'analytic properties']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902265'],"['We compute, from first principles, the quantum fluctuations about instanton saddle points of the Euclidean path integral for Einstein gravity coupled to a scalar field. The Euclidean two-point correlator is analytically continued into the Lorentzian region where it describes the quantum mechanical vacuum fluctuations in the state described by no boundary proposal initial conditions. We concentrate on the density perturbations in open inflationary universes produced from cosmological instantons, describing the differences between non-singular Coleman-De Luccia and singular Hawking-Turok instantons. We show how the Euclidean path integral uniquely specifies the fluctuations in both cases.']",['1999-02-23'] +1253,['eng'],"['Faraoni, V', 'Gunzig, E']",['Tales of tails in cosmology'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, massive', 'field theory, scalar', 'space-time', 'gravitational radiation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902262'],"['Late time mild inflation (LTMI) proposes to solve the age of the universe problem and the discrepancy between locally and globally measured values of the Hubble parameter. However, the mechanism proposed to achieve LTMI is found to be physically pathological by applying the theory of tails for the solutions of wave equations in curved spaces. Alternative mechanisms for LTMI are discussed, and the relevance of scalar wave tails for cosmology is emphasized.']",['1999-02-23'] +1254,['eng'],"['Ellis, Jonathan Richard']",['Learning Physics from the Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['talk, Villa Olmo 1998/10/05', 'cosmic radiation, background', 'microwaves', 'quantum gravity', 'grand unified theory', 'supersymmetry', 'astrophysics, model', 'astrophysics, missing-mass', 'sparticle, mass', 'LSP', 'neutrino, oscillation', 'neutrino, mass difference', 'neutrino, mixing angle', 'numerical calculations', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902242'],"['The Cosmic Microwave Background (CMB) provides a precious window on fundamental physics at very high energy scales, possibly including quantum gravity, GUTs and supersymmetry. The CMB has already enabled defect-based rivals to inflation to be discarded, and will be able to falsify many inflationary models. In combination with other cosmological observations, including those of high-redshift supernovae and large-scale structure, the CMB is on the way to providing a detailed budget for the density of the Universe, to be compared with particle-physics calculations for neutrinos and cold dark matter. Thus CMB measurements complement experiments with the LHC and long-baseline neutrino beams.']",['1999-02-18'] +1255,['eng'],"['Takeda, M', 'Hayashida, N', 'Honda, K', 'Inoue, N', 'Kadota, K', 'Kakimoto, F', 'Kamata, K', 'Kawaguchi, S', 'Kawasaki, Y', 'Kawasumi, N', 'Kusano, E', 'Matsubara, Y', 'Murakami, K', 'Nagano, M', 'Nishikawa, D', 'Ohoka, H', 'Osone, S', 'Sakaki, N', 'Sasaki, M', 'Shinozaki, K', 'Souma, N', 'Teshima, M', 'Torii, R', 'Tsushima, I', 'Uchihori, Y', 'Yamamoto, T', 'Yoshida, S', 'Yoshii, H']",['Small-scale anisotropy of cosmic rays above $10^{19}$eV observed with the Akeno Giant Air Shower Array'],['Astrophysics and Astronomy'],"['cosmic radiation, angular distribution', 'cosmic radiation, anisotropy', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902239'],"['With the Akeno Giant Air Shower Array (AGASA), 581 cosmic rays above 10^19eV, 47 above 4 x 10^19eV, and 7 above 10^20eV are observed until August 1998. Arrival direction distribution of these extremely high energy cosmic rays has been studied. While no significant large-scale anisotropy is found on the celestial sphere, some interesting clusters of cosmic rays are observed. Above 4 x 10^19eV, there are one triplet and three doublets within separation angle of 2.5^o and the probability of observing these clusters by a chance coincidence under an isotropic distribution is smaller than 1 %. Especially the triplet is observed against expected 0.05 events. The cos(\\theta_GC) distribution expected from the Dark Matter Halo model fits the data as well as an isotropic distribution above 2 x 10^19eV and 4 x 10^19eV, but is a poorer fit than isotropy above 10^19eV. Arrival direction distribution of seven 10^20eV cosmic rays is consistent with that of lower energy cosmic rays and is uniform. Three of seven are members of doublets above about 4 x 10^19eV.']",['1999-02-18'] +1256,['eng'],"['Medvedev, M V']",['Thermodynamics of photons in relativistic $e^{+}e^{-}\\gamma$ plasmas'],['Astrophysics and Astronomy'],"['plasma, relativistic', 'coupling, (positron electron photon)', 'photon, gas', 'thermodynamics', 'photon, mass', 'universality', 'energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902235'],"['Thermodynamic and spectral properties of a photon gas in $e^+e^-\\gamma$ plasmas are studied. The effect of a finite effective mass of a photon, associated with the plasma frequency cutoff, is self-consistently included. In the ultra-relativistic plasma, the photon spectrum turns out to be universal with the temperature normalized plasma frequency cutoff being a fundamental constant independent of plasma parameters. Such a universality does not hold in the non-relativistic plasma.']",['1999-02-17'] +1257,['eng'],"['Maraschi, L', 'Fossati, G', 'Tavecchio, F', 'Chiappetti, L', 'Celotti, A', 'Ghisellini, G', 'Grandi, P', 'Pian, E', 'Tagliaferri, G', 'Treves, A', 'Breslin, A C', 'Buckley, J H', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Fegan, D J', 'Fegan, S J', 'Finley, J', 'Gaidos, J', 'Hall, T', 'Hillas, A M', 'Krennrich, F', 'Lessard, R W', 'Masterson, C', 'Moriarty, P', 'Quinn, J', 'Rose, J', 'Samuelson, F', 'Weekes, T C', 'Weekes, T C']",['Correlated variability of Mkn 421 at X-ray and TeV wavelengths on timescales of hours'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'time variation', 'energy spectrum', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902224'],"[""Mkn 421 was observed for about two days with BeppoSAX, prior to and partly overlapping the start of a 1 week continuous exposure with ASCA in April 1998, as part of a world-wide multiwavelength campaign. A pronounced, well defined, flare observed in X-rays was also observed simultaneously at TeV energies by the Whipple Observatory's 10 m gamma-ray telescope. These data provide the first evidence that the X-ray and TeV intensities are well correlated on time-scales of hours.""]",['1999-02-17'] +1258,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Fiorentini, G', 'Lissia, M']",['Solar neutrino fluxes with arbitrary $^{3}He$ mixing'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'nucleus nucleus, nuclear reaction', 'helium, nuclide', 'boron', 'beryllium', 'neutrino, production', 'parametrization', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902222'],"['The He3 abundance is not constrained by helioseismic data. Mixing of He3 inside the solar core by processes not included in the solar standard model (SSM) has been recently proposed as possible solution to the solar neutrino problem. We have performed a model independent analysis of solar neutrino fluxes using practically arbitrary He3 abundance. In addition, we have been simultaneously varying within very wide ranges the temperature in the neutrino production zone and the astrophysical factors, S17 and S34, of the p+Be7 and He3+He4 cross sections. Seismic data are used as constraints, but the solar- luminosity constraint is not imposed. It is demonstrated that even allowing He3 abundances higher by factors up to 16 than in the SSM, temperatures 5% (or more) lower, the astrophysical factor S17 up to 40% higher, and varying S34 in the range (-20% ,+40%), the best fit is still more than 5 sigmas away from the observed fluxes. We conclude that practically arbitrary He3 mixing combined with independent variations of temperature and cross-sections cannot explain the observed solar neutrino fluxes.']",['1999-02-17'] +1259,['eng'],"['Konar, S']",['Whither Strange Pulsars ?'],['Astrophysics and Astronomy'],"['pulsar, strangeness', 'matter, strangeness', 'magnetic field', 'n, matter']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902220'],"['Both neutron stars and strange stars are capable of supporting fast rotations observed in pulsars. On the basis of this it has been argued that some of the pulsars could be strange stars. We investigate whether strange stars can sustain characteristic pulsar magnetic fields ($10^8 - 10^{13.5} Gauss$) over astronomically significant time-scales. Furthermore, we check whether strange stars fit into the general scenario of field evolution of pulsars. It is found that as far as the evolution of the magnetic field is concerned the strange pulsar hypothesis runs into serious difficulties to explain the observational data.']",['1999-02-17'] +1260,['eng'],"['Gerbier, G', 'Mallet, J', 'Mosca, L', 'Tao, Charling']","['Note about a second ""evidence"" for a WIMP annual modulation']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP', 'cosmic radiation, time variation', 'counters and detectors', 'data analysis method']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902194'],"['This note, with its five questions, is intended to contribute to a clarification about a claimed ""evidence"" by the DAMA group of an annual modulation of the counting rate of a Dark Matter NaI(Tl) detector as due to a neutralino (SUSY-LSP) Dark Matter candidate.']",['1999-02-15'] +1261,['eng'],"['Alvarez-Muñiz, J', 'Zas, E']",['EeV Neutrinos'],['Astrophysics and Astronomy'],"['talk, Faro 1998/09/03', 'neutrino, cosmic radiation', 'neutrino, particle identification', 'neutrino, flux', 'shower detector', 'deep underground detector', 'Cherenkov counter, water', 'water, solids', 'showers, electromagnetic', 'showers, hadronic', 'Landau-Pomeranchuk-Migdal effect', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902187'],['We discuss the recent developments in the study of alternative detection possibilites offered by the radio technique and air shower arrays.'],['1999-02-15'] +1262,['eng'],"['Mannheim, K']",['Frontiers in High-Energy Astroparticle Physics'],['Astrophysics and Astronomy'],"['galaxy, AGN', 'cosmic radiation, background', 'photon, cosmic radiation', 'cosmic radiation, cascade', 'p, blazar', 'p, cosmic radiation', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902185'],"['With the discovery of evidence for neutrino mass, a vivid gamma ray sky at multi-TeV energies, and cosmic ray particles with unexpectedly high energies, astroparticle physics currently runs through an era of rapid progress and moving frontiers. The non-vanishing neutrino mass establishes one smooth component of dark matter which does not, however, supply a critical mass to the Universe. Other dark matter particles are likely to be very massive and should produce high-energy gamma rays, neutrinos, and protons in annihilations or decays. The search for exotic relics with new gamma ray telescopes, extensive air shower arrays, and underwater/-ice neutrino telescopes is a fascinating challenge, but requires to understand the astrophysical background radiations at high energies. Among the high-energy sources in the Universe, radio-loud active galactic nuclei seem to be the most powerful accounting for at least a sizable fraction of the extragalactic gamma ray flux. They could also supply the bulk of the observed cosmic rays at ultrahigh energies and produce interesting event rates in neutrino telescopes aiming at the kubic kilometer scale such as AMANDA and ANTARES. It is proposed that the extragalactic neutrino beam can be used to search for tau lepton appearance thus allowing for a proof of the neutrino oscillation hypothesis. Furthermore, a new method for probing the era of star formation at high redshifts using gamma rays is presented which requires new-generation gamma ray telescopes operating in the 10-100 GeV regime such as MAGIC and GLAST.']",['1999-02-15'] +1263,['eng'],"['Bergström, L']",['Indirect detection of neutralino dark matter'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'astrophysics, missing-mass', 'search for, missing-mass', 'neutralino, LSP', 'neutralino, annihilation', 'positron, cosmic radiation', 'anti-p, cosmic radiation', 'photon, cosmic radiation', 'photon, energy spectrum', 'flux, energy dependence', 'neutrino', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902172'],"['Dark matter detection experiments are getting ever closer to the sensitivity needed to detect the primary particle physics candidates for nonbaryonic dark matter. Indirect detection methods include searching for antimatter and gamma rays, in particular gamma ray lines, in cosmic rays and high-energy neutrinos from the centre of the Earth or Sun caused by accretion and annihilation of dark matter particles. A review is given of recent progress, both on the theoretical and experimental sides.']",['1999-02-12'] +1264,['eng'],"['Coutu, S', 'Barwick, S W', 'Beatty, J J', 'Bhattacharya, A', 'Bower, C', 'Chaput, C J', 'De Nolfo, G A', 'Duvernois, M A', 'Labrador, A W', 'McKee, S', 'Müller, D', 'Musser, J A', 'Nutter, S L', 'Schneider, E', 'Swordy, S P', 'Tarlé, G', 'Tomasch, A D', 'Torbet, E']",['Cosmic-Ray Positrons'],['Astrophysics and Astronomy'],"['positron, cosmic radiation', 'cosmic radiation, primary', 'cosmic radiation, particle source', 'electron, cosmic radiation', 'astrophysics, missing-mass', 'sparticle, annihilation', 'cosmic radiation, secondary radiation', 'cosmic radiation, production', 'WIMP', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902162'],"['Cosmic rays at the Earth include a secondary component originating in collisions of primary particles with the diffuse interstellar gas. The secondary cosmic rays are relatively rare but carry important information on the Galactic propagation of the primary particles. The secondary component includes a small fraction of antimatter particles, positrons and antiprotons. In addition, positrons and antiprotons may also come from unusual sources and possibly provide insight into new physics. For instance, the annihilation of heavy supersymmetric dark matter particles within the Galactic halo could lead to positrons or antiprotons with distinctive energy signatures. With the High-Energy Antimatter Telescope (HEAT) balloon-borne instrument, we have measured the abundances of positrons and electrons at energies between 1 and 50 GeV. The data suggest that indeed a small additional antimatter component may be present that cannot be explained by a purely secondary production mechanism. Here we describe the signature of the effect and discuss its possible origin.']",['1999-02-11'] +1265,['eng'],"['Bergström, L', 'Iguri, S', 'Rubinstein, H R']",['Constraints on the Variation of the Fine Structure Constant from Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['fundamental constant, fine structure', 'astrophysics, model', 'light nucleus, production', 'lithium', 'helium', 'nucleus nucleus, nuclear reaction', 'p nucleus, nuclear reaction', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902157'],"['We put bounds on the variation of the value of the fine structure constant elements up to $^7$Li. We correct a previous upper limit on $|\\Delta \\alpha / potential limits (depending on the value of the baryon-to-photon ratio) from $^7$Li, whose production is governed to a large extent by Coulomb barriers. The presently unclear observational situation concerning the primordial abundances preclude a better limit than $|\\Delta \\alpha/\\alpha| \\lsim 2\\cdot 10^{-2}$, two orders of magnitude less restrictive than previous bounds. In fact, each of the (mutually exclusive) scenarios of standard Big Bang nucleosynthesis proposed, one based on a high value of the measured deuterium primordial abundance and one based on a low value, may describe some aspects of data better if a change in $\\alpha$ of this magnitude is assumed.']",['1999-02-11'] +1266,['eng'],"['Dar, Arnon', 'Plaga, R']",['Galactic Gamma-Ray Bursters'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'galaxy', 'hadron, cosmic radiation', 'jet, relativistic', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902138'],"['We propose a new paradigm for the origin of nonsolar hadronic cosmic rays (CRs) at all energies: Highly relativistic, narrowly collimated jets from the birth or collapse of neutron stars in our Galaxy accelerate ambient disk and halo matter to CR energies and disperse it in hot spots which they form when they stop in the Galactic halo. Such events, seen as cosmological gamma-ray bursts in other galaxies when their beamed radiation happens to point towards Earth, account for many observed properties of the main hadronic component of CRs in a more natural way than all previously discussed CR sources.']",['1999-02-10'] +1267,['eng'],"['Biswas, S', 'Modak, B', 'Shaw, A']",['The Complex Time WKB Approximation And Particle Production'],['Astrophysics and Astronomy'],"['space-time, Minkowski', 'space-time, de Sitter', 'WKB approximation', 'particle, production', 'invariance, gauge', 'time dependence', 'electric field, high', 'dependence, space', 'black hole', 'charge, conservation law', 'current, rotator']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902135'],"['The complex time WKB (CWKB) approximation has been an effective technique to understand particle production in curved as well as in flat spacetime. Earlier we obtained the standard results on particle production in time dependent gauge in various curved spacetime. In the present work we generalize the technique of CWKB to the equivalent problems in space dependent gauge. Using CWKB, we first obtain the gauge invariant result for particle production in Minkowski spacetime in strong electric field. We then carry out particle production in de-Sitter spacetime in space dependent gauge and obtain the same result that we obtained earlier in time dependent gauge. The results obtained for de-Sitter spacetime has a obvious extension to particle production in black hole spacetime. It is found that the origin of Planckian spectrum is due to repeated reflections between the turning points. As mentioned earlier, it is now explicitly shown that particle production is accompanied by rotation of currents.']",['1999-02-10'] +1268,['eng'],"['Fredriksson, S', 'Enström, D', 'Hansson, J', 'Ekelin, S', 'Nicolaidis, A']",['Is Dark Matter made up of Massive Quark Objects?'],['Astrophysics and Astronomy'],"['talk, Heidelberg 1998/07/20', 'astrophysics, missing-mass', 'quark, matter', 'stability', 'critical phenomena', 'matter, hadronic', 'photon, cosmic radiation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810389'],"[""We suggest that dark matter is made up of massive quark objects that have survived from the Big Bang, representing the ground state of ``baryonic'' matter. Hence, there was no overall phase transition of the original quark matter, but only a split-up into smaller objects. We speculate that normal hadronic matter comes about through enforced phase transitions when such objects merge or collide, which also gives rise to the cosmic gamma-ray bursts.""]",['1998-10-26'] +1269,['eng'],"['Hagmann, C']",['A Relic Neutrino Detector'],['Astrophysics and Astronomy'],"['talk, Asilomar 1998/11/15', 'neutrino, cosmic radiation', 'neutrino electron, elastic scattering', 'neutrino nucleon, elastic scattering', 'measurement, recoil', 'gravitation, acceleration', 'counters and detectors, superconducting', 'magnet, superconducting', 'niobium, titanium', 'optics, readout']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902102'],"['Probably the most promising way of detecting cosmic neutrinos is measuring the mechanical force exerted by elastic scattering of cosmic neutrinos from macroscopic targets. The expected acceleration is $\\sim 10^{-23} cm/s^2$ for Dirac neutrinos of mass $\\sim 10 eV$ and local density $\\sim 10^7/ cm^3$. A novel torsion balance design is presented. which addresses the sensitivity-limiting factors of existing balances, such as seismic and thermal noise, and angular readout resolution and stability.']",['1999-02-09'] +1270,['eng'],"['Bell, N F', 'Volkas, R R']",['Mirror matter and primordial black holes'],['Astrophysics and Astronomy'],"['matter, mirror', 'black hole', 'density, perturbation', 'critical phenomena']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812301'],"['A consequence of the evaporation of primordial black holes in the early universe may be the generation of mirror matter. This would have implications with regard to dark matter, and number of light particle species in equilibrium at the time of big bang nucleosynthesis. The possibilities for the production of mirror matter by this mechanism are explored.']",['1998-12-17'] +1271,['eng'],"['Mohapatra, R N', 'Teplitz, V L']",['Mirror Matter MACHOs'],['Astrophysics and Astronomy'],"['matter, mirror', 'MACHO', 'baryon, matter', 'neutrino, sterile', 'mass, scaling', 'matter, lifetime', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902085'],"[""We propose that the massive compact halo objects (MACHOs) observed in the recent microlensing experiments with an apparent best fit mass of about $0.5 M_{\\odot}$ are objects made out of ``mirror'' baryonic matter rather than familiar baryons. Such a possibility arises naturally within the framework of mirror matter models proposed recently to accomodate the sterile neutrinos that seem necessary to solve all the neutrino puzzles simultaneusly. We show that for mirror matter parameters that fit the neutrino observations, the maximum mass of mirror stars are of order $0.5 M_{\\odot}$ and their main sequence lifetime is much less than the age of the universe. They are therefore likely to be black holes. Mirror matter machos have the advantage that they do not suffer from the problems encountered in the conventional red, brown or white dwarf interpretation. The calculations also apply to the question of how the world of familiar matter would be different if all fundamental mass parameters were.""]",['1999-02-05'] +1272,['eng'],"['Rivin, Y R', 'Obridko, V N']",['Time variations of solar neutrino'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'time variation', 'magnetic field, solar', 'neutrino, magnetic moment', 'interpretation of experiments, Homestake']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902074'],['The paper contains some arguments in support of time variations of the high-speed flux of solar neutrino'],['1999-02-05'] +1273,['eng'],"['Foot, R']",['Have mirror stars been observed?'],['Astrophysics and Astronomy'],"['matter, mirror', 'astrophysics, missing-mass', 'supernova, mirror', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'MACHO', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902065'],"[""Observations by the MACHO collaboration suggest that a significant proportion of the galactic halo dark matter is in the form of compact objects with typical masses $M\\sim 0.5M_{\\odot}$. One of the current mysteries is the nature and origin of these objects. We suggest that these objects are stars composed of mirror matter. This interpretation provides a plausible explanation for the inferred masses and abundance of the MACHO events. We also comment on the possibility of inferring the existence of mirror supernova's by detecting the neutrino burst in existing underground detectors such as SuperKamiokande.""]",['1999-02-05'] +1274,['eng'],"['Allen, R E']",['Four Testable Predictions of Instanton Cosmology'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'astrophysics, model', 'instanton', 'gauge field theory, SU(2) x U(1)', 'Einstein equation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902042'],"['A new cosmological model makes the following predictions: (1) The deceleration parameter $q_{0}$ is approximately zero. (2) The mass density parameter $\\Omega_{m}$ is less than 1. (3) The universe is spatially closed, but is asymptotically flat as $t\\to\\infty$, regardless of its matter content. (4) The age of the universe is approximately 15 Gyr if the Hubble parameter $h$ is approximately 0.65.']",['1999-02-03'] +1275,['eng'],"['Alvarez-Muñiz, J', 'Halzen, Francis']",['Muon Detection of TeV $\\gamma$ Rays from $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy', 'photon, showers', 'muon, secondary radiation', 'muon, yield', 'threshold', 'deep underground detector, efficiency', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902039'],"[""Because of the limited size of the satellite-borne instruments, it has not been possible to observe the flux of gamma ray bursts (GRB) beyond GeV energy. We here show that it is possible to detect the GRB radiation of TeV energy and above, by detecting the muon secondaries produced when the gamma rays shower in the Earth's atmosphere. Observation is made possible by the recent commissioning of underground detectors (AMANDA, the Lake Baikal detector and MILAGRO) which combine a low muon threshold of a few hundred GeV or less, with a large effective area of 10^3 m^2 or more. Observations will not only provide new insights in the origin and characteristics of GRB, they also provide quantitative information on the diffuse infrared background.""]",['1999-02-03'] +1276,['eng'],"['Fargion, D', 'Melé, B']",['Scattering of Ultrahigh Energy (UHE) Extragalactic Neutrinos onto Light Relic Neutrinos in Galactic HDM Halo Overcoming the GZK Cut off'],['Astrophysics and Astronomy'],"['talk, Buxton 1998/09/07', 'neutrino, cosmic radiation', 'neutrino neutrino, interaction', 'neutrino antineutrino, interaction', 'neutrino/tau', 'antineutrino/tau', 'W, pair production', 'Z0, neutrinoproduction', 'hadron, production', 'cross section, energy dependence', 'galaxy', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902024'],"[""The rarest cosmic rays above the GZK cut'off $(E_{CR} \\tilde{>} 10^{19} \\div 10^{20} eV)$ are probably born at cosmic distances ($\\tilde{>}$ tens Mpc) by AGNs (QSRs, BLac, Blazars...). Their puzzling survival over $2.75 K^o$ BBR radio waves opacities (the ``GZK cut off'') might find a natural explanation if the traveling primordial cosmic rays were UHE neutrinos (born by UHE photopion decay) which are transparent to $\\gamma$ or $\\nu$ BBR. These UHE$% \\nu$ might scatter onto those (light and cosmological) relic neutrinos clustered around our galactic halo. The branched chain reactions from a primordial nucleon (via photoproduction of pions and decay to UHE neutrinos) toward the consequent beam dump scattering on galactic relic neutrinos is at least three order of magnitude more efficient than any known neutrino interactions with Earth atmosphere or direct nucleon propagation. Therefore the rarest cosmic rays (as the 320 EeV event) might be originated at far $(\\tilde{>} 100 Mpc)$ distances (as Seyfert galaxy MCG 8-11-11). The needed UHE radiation power is in rough agreement with the NCG 8-11-11 observed in MeV gamma energy total output power. The final chain products observed on Earth by the Fly's Eye detector might be mainly neutron and antineutrons as well as, at later stages, protons and antiprotons. These hadronic products are most probably secondaries of $W^+ W^-$ or $ZZ$ pair productions and might be consistent with the last AGASA discoveries of 6 doublet and one triplet event.""]",['1999-02-02'] +1277,['eng'],"['Bergström, L', 'Edsjö, J', 'Ullio, P']",['Cosmic antiprotons as a probe for supersymmetric dark matter?'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutralino, annihilation', 'anti-p, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, background', 'galaxy', 'energy loss', 'diffusion, model', 'supersymmetry', 'anti-p, yield', 'parametrization', 'anti-p, energy spectrum', 'anti-p, lifetime', 'numerical calculations, Monte Carlo', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902012'],"[""The flux of cosmic ray antiprotons from neutralino annihilations in the galactic halo is computed for a large sample of models in the MSSM (the Minimal Supersymmetric extension of the Standard Model). We also revisit the problem of estimating the background of low-energy cosmic ray induced secondary antiprotons, taking into account their subsequent interactions (and energy loss) and the presence of nuclei in the interstellar matter. We consider a two-zone diffusion model, with and without a galactic wind. We find that, given the uncertainties in the background predictions, there is no need for a primary (exotic) component to explain present data. However, allowing for a signal by playing with the uncertainties in the background estimate, we discuss the characteristic features of the supersymmetric models which give a satisfactory description of the data. We point out that in some cases the optimal kinetic energy to search for a signal from supersymmetric dark matter is above several GeV, rather than the traditional sub-GeV region. The large astrophysical uncertainties involved do not, one the other hand, allow the exclusion of any of the MSSM models we consider, on the basis of data. We present besides numerical results also convenient parameterizations of the antiproton yields of all `basic' two-body final states. We also give examples of the yield and differential energy spectrum for a set of supersymmetric models with high rates. We also remark that it is difficult to put a limit on the antiproton lifetime from present measurements, since the injection of antiprotons from neutralino annihilation can compensate the loss from decay.""]",['1999-02-02'] +1278,['eng'],"['Roberts, M D', 'McGee, P', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Holder, J', 'Kawachi, A', 'Kifune, T', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Osaki, T', 'Patterson, J R', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['TeV $\\gamma$-Ray Observations of Three-X-Ray Selected BL Lacs'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'flux, upper limit', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9902008'],"['Despite extensive surveys of extragalactic TeV gamma-ray candidates only 3 sources have so far been detected. All three are northern hemisphere objects and all three are low-redshift X-ray selected BL Lacs (XBLs). In this paper we present the results of observations of the three nearest southern hemisphere XBLs (PKS0548-322, PKS2005-489 and PKS2155-304) with the CANGAROO 3.8m imaging telescope. During the period of observation we estimate that the threshold of the 3.8m telescope was around 1.5TeV. Searches for both steady and short timescale emission have been performed for each source. Additionally, we are able to monitor the X-ray state of each source on a daily basis and we have made contemporaneous measurements of optical activity for PKS0548-322 and PKS2155-304.']",['1999-02-02'] +1279,['eng'],"['Starkman, G D', 'Trodden, M', 'Vachaspati, T']",['Observation of Cosmic Acceleration and Determining the Fate of the Universe'],['Astrophysics and Astronomy'],"['supernova', 'astrophysics, acceleration', 'inflationary universe', 'vacuum state, energy', 'energy, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901405'],"['Current observations of Type Ia supernovae provide evidence for cosmic acceleration out to a redshift of z \\lsim 1, leading to the possibility that the universe is entering an inflationary epoch. However, inflation can take place only if vacuum-energy (or other sufficiently slowly redshifting source of energy density) dominates the energy density of a region of physical radius 1/H. We argue that for the best-fit values of Ømega_\\Lambda and Ømega_m inferred from the supernovae data, one must confirm cosmic acceleration out to at least z \\simeq 1.8 to infer that the universe is inflating.']",['1999-01-29'] +1280,['eng'],"['Vestrand, W T', 'Sreekumar, P']",['RXTE Observations of PKS 2155-304 during the November 1997 $\\gamma$-Ray Outburst'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'energy spectrum', 'time variation', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901404'],['We present x-ray observations of the nearby BL Lac PKS 2155-304 taken when it was undergoing a GeV/TeV gamma-ray outburst. During the outburst we measured x-ray fluxes in the 2-10 keV band that are the largest ever observed for PKS 2155-304. Comparison of these November 1997 measurements and other x-ray observations made contemporaneously with GeV or TeV gamma-ray observations indicate that x-ray and gamma-ray emissions are correlated. Measurements with x-ray all-sky monitors such as the ASM/RXTE and MOXE can therefore signal the presence of outbursts at gamma-ray energies from PKS 2155-304.'],['1999-01-29'] +1281,['eng'],"['Blasi, P']",['$\\gamma$ Rays from Super Heavy Relic Particles in the Halo'],['Astrophysics and Astronomy'],"['astrophysics, model', 'postulated particle, heavy', 'photon, cosmic radiation', 'cosmic radiation, production', 'astrophysics, missing-mass', 'galaxy, cluster', 'electron, emission', 'electron, cosmic radiation', 'magnetic field, galaxy', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901390'],"['Superheavy (SH) quasistable particles generated in the Early Universe could be responsable for Ultra High Energy Cosmic Rays (UHECR) and be a component of Cold Dark Matter (CDM) in the universe. These particles are likely to cluster in the galactic halo, so that the main part of UHECR are gamma rays produced in the decay of neutral pions. Charged pions are also produced in the same decay and result in high energy electrons. We consider here the production of gamma rays by synchrotron emission of these electrons in the galactic magnetic field. The gamma ray fluxes are above the detectability level of current and proposed experiments (e.g. EGRET, GLAST, STACEE and WHIPPLE) in the energy range $0.1-10^4$ GeV and are compatible with the existing upper limits at $10^5-10^8$ GeV. The detection of this flux of gamma rays would be of key relevance to determine the importance of SH relic particles as sources of UHECR and give a clue on the physics of the Early Universe.']",['1999-01-29'] +1282,['eng'],"['Konopelko, A K']",['On design studies for the future 50 GeV arrays of imaging air Cherenkov telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'semiconductor detector, pixel', 'angular resolution', 'electronics, background']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901365'],"['Arrays of imaging air Cherenkov telescopes (IACTs) like VERITAS, HESS have been recently proposed as the instruments of the next generation for ground based very high energy gamma-ray astronomy invading into 50-100 GeV energy range. Here we present results of design studies for the future IACT arrays which have been performed by means of Monte Carlo simulations. We studied different trigger strategies, abilities of cosmic ray rejection for arrays of 4 and 16 telescopes with 10 m reflectors, equipped with cameras comprising 271 and 721 pixels of 0.25 and 0.15 degree, respectively. The comparative analysis of the performance of such telescope arrays has been done for both camera options, providing almost the same field of view of 4.3 degree. An important issue is the choice of the optimum spacing between the telescopes in such an array. In order to maximize the signal-to-noise ratio in observations at the small zenith angles of 20 degree as well as at large zenith angles of 60 degree, different arrangements of IACT array have been examined. Finally, we present a major recommendations regarding the optimum configuration.']",['1999-01-27'] +1283,['eng'],"['Metcalf, R B', 'Silk, J']",['A Fundamental Test of the Nature of Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'gravitation, lens', 'statistical analysis', 'supernova', 'luminosity', 'matter, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901358'],"['Dark matter may consist of weakly interacting elementary particles or of macroscopic compact objects. We show that the statistics of the gravitational lensing of high redshift supernovae strongly discriminate between these two classes of dark matter candidates. We develop a method of calculating the magnification distribution of supernovae, which can be interpreted in terms of the properties of the lensing objects. With simulated data we show that ~ 50 well measured type Ia supernovae (\\Delta m ~ 0.16 mag) at redshifts ~ 1 can clearly distinguish macroscopic from microscopic dark matter.']",['1999-01-27'] +1284,['eng'],"['Pen, U L']",['Broken Defects'],['Astrophysics and Astronomy'],"['talk, Garching 1998/08/02', 'astrophysics, missing-mass', 'topology, defect', 'space-time', 'astrophysics, fundamental constant', 'cosmic radiation, background', 'neutrino, mass', 'cluster, galaxy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901357'],"['Recent indications of a neutrino mass raise the possibility that the dark matter may be hot, which would be a severe challenge for structure formation theory. We argue that generic defect theories fare very well in hot dark matter cosmologies, and also work in the presence of curvature or a cosmological constant. If this model is correct, then the MAP and PLANCK missions will not measure what people expect them to (oscillations); rather, they will measure a broad hump.']",['1999-01-27'] +1285,['eng'],"['Krennrich, F']",['New Generation Atmospheric Cherenkov Detectors'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'radiation, Cherenkov', 'angular resolution', 'energy resolution', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901354'],"['High energy gamma-ray astronomy has been established during the last decade through the launch of the Compton Gamma Ray Observatory (CGRO) and the success of its ground-based counterpart, the imaging atmospheric Cherenkov technique. In the aftermath of their important and surprising scientific results a worldwide effort developing and designing new generation atmospheric Cherenkov detectors is underway. These novel instruments will have higher sensitivity at E > 250 GeV, but most importantly, will be able to close the unexplored energy gap between 20 GeV and 250 GeV. Several ground-based detectors are proposed or under construction. Aspects of the techniques used and sensitivity are discussed in this overview paper. The instruments cover largely complementary energy ranges and together are expected to explore the gamma-ray sky between 20 GeV and 100 TeV with unprecedented sensitivity.']",['1999-01-26'] +1286,['eng'],"['Kranich, D', 'Mirzoian, R M', 'Petry, D', 'Raubenheimer, B C']",['TeV $\\gamma$-ray Observations of the Crab and Mkn 501 during Moonshine and Twilight'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'Cherenkov counter, imaging', 'efficiency, time dependence', 'experimental methods']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901330'],"['TeV Gamma-ray signals from the Crab Nebula and Mkn 501 were detected with the HEGRA CT1 imaging Cerenkov telescope during periods when the moon was shining and during twilight. This was accomplished by lowering the high voltage supply of the photomutipliers in fixed steps up to 13%. No other adjustments were made and no filters were used. Laser runs could not establish any non-linearity in the gain of the individual pixels, and the trigger rate was uniform over the whole camera. The energy threshol was increased by up to a factor of two, depending on the amount of HV reduction. In a series of observations lasting 11.7 hours, a signal with a 3.4 sigma significance was detected from the Crab. During the 1997 multiple flare episode of Mkn 501 a 26 sigma combined excess has been recorded during 134 hours of observations under various moonshine/twilight conditions. The results show that this technique can easily be adapted to increase the exposure of a source, which is important for sources showing rapid time variability such as AGNs or GRBs. Observations can be made up to ~20 deg. angular separation from the moon and until the moon is 85% illuminated (ten to eleven days before and after new moon), as well as during 20 to 40 minutes during twilight, before the commencement of astronomical darkness.']",['1999-01-25'] +1287,['eng'],"['Dermer, C D']",['Variability in Blazars'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'astrophysics, blazar', 'galaxy', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'plasma, relativistic', 'synchrotron radiation, flux', 'jet, particle source', 'plasma, deceleration', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901324'],"['The kinetic energy of bulk relativistic plasma ejected from the central engine of blazars is converted into nonthermal particle energy in the comoving frame through a process of sweeping up material from the surrounding medium. The resulting deceleration of the bulk plasma introduces a number of effects which must be included in blazar modeling. For example, the varying Doppler factor means that model fits must employ time integrations appropriate to the observing times of the detectors. We find that the ratio of the peak synchrotron fluxes reached at two different photon energies is largest when viewing along the jet axis, and becomes smaller at large angles to the jet axis. This effect is important in studies of the statistics of jet sources. Variability due either to bulk plasma deceleration or radiative cooling must be distinguished in order to apply recently proposed tests for beaming from correlated X-ray and TeV observations. The blast-wave physics developed to analyze these problems implies that most of the energy injected in the comoving frame is originally in the form of nonthermal hadrons. Because plasmoid deceleration can produce rapid variability due to a changing Doppler factor, arguments against hadronic blazar models related to the long radiative cooling time scale of hadrons are not compelling.']",['1999-01-25'] +1288,['eng'],"['Dolgov, A D']",['Neutrino Degeneracy and Chemically Inhomogeneous Universe'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'astrophysics, model', 'lepton, asymmetry', 'deuterium', 'helium', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, energy spectrum', 'neutrino/e, potential', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901318'],"['A possibility that the universe may be strongly inhomogeneous chemically, while very smooth energetically, is considered. A possible mechanism which could lead to such a picture is a large and inhomogeneous lepton asymmetry. The model may explain possibly observed variation of primordial deuterium by an order of magnitude and predicts helium-rich and possibly helium-poor regions where the helium mass fraction differs from the observed 25% by a factor of 2 in either direction. Helium variation can be observed by a different dumping rate of CMB angular spectrum at small angles at different patches of the sky.']",['1999-01-25'] +1289,['eng'],"['Rowell, G P', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, T', 'Holder, J', 'Kawachi, A', 'Kifune, T', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Roberts, M D', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['TeV Observations of Centaurus A'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'cosmic radiation, flux', 'upper limit', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901316'],"[""We have searched for TeV gamma-rays from Centaurus A and surrounding region out to +/- 1.0 deg using the CANGAROO 3.8m telescope. No evidence for TeV gamma-ray emission was observed from the search region, which includes a number of interesting features located away from the tracking centre of our data. The 3 sigma upper limit to the flux of gamma-rays above 1.5 TeV from an extended source of radius 14' centred on Centaurus A is 4.66e-12 photons cm^-2 s^-1.""]",['1999-01-25'] +1290,['eng'],"['Farrar, Glennys R S', 'Biermann, P L']","['Reply to ""Comment on ""Correlation between Compact Radio Quasars and Ultra-High Energy Cosmic Rays""""']",['Astrophysics and Astronomy'],"['quasar', 'photon, cosmic radiation', 'correlation', 'cosmic radiation, energy spectrum', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901315'],"['We discuss the rationale for the energy cuts used in the previous study of directional correlation of the five highest energy cosmic ray events with compact, radio quasars. We check the consistency of the next three most energetic events which just missed those cuts, with the correlation hypothesis. Agreement between expected and observed properties of these events is good.']",['1999-01-25'] +1291,['eng'],"['Jedamzik, K', 'Niemeyer, J C']",['Primordial Black Hole Formation during First-Order Phase Transitions'],['Astrophysics and Astronomy'],"['astrophysics, model', 'black hole, production', 'density, fluctuation', 'adiabatic', 'critical phenomena', 'model, hydrodynamical', 'relativity theory, general', 'energy, density', 'mass spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901293'],"['Primordial black holes (PBHs) may form in the early universe when pre-existing adiabatic density fluctuations enter into the cosmological horizon and recollapse. It has been suggested that PBH formation may be facilitated when fluctuations enter into the horizon during a strongly first-order phase transition which proceeds in approximate equilibrium. We employ general-relativistic hydrodynamics numerical simulations in order to follow the collapse of density fluctuations during first-order phase transitions. We find that during late stages of the collapse fluctuations separate into two regimes, an inner part existing exclusively in the high-energy density phase with energy density $\\epsilon_{\\rm h}$, surrounded by an outer part which exists exclusively in the low-energy density phase with energy density $\\epsilon_{\\rm h}-L$, where $L$ is the latent heat of the transition. We confirm that the fluctuation density threshold $\\delta\\epsilon /\\epsilon$ required for the formation of PBHs during first-order transitions decreases with increasing $L$ and falls below that for PBH formation during ordinary radiation dominated epochs. Our results imply that, in case PBHs form at all in the early universe, their mass spectrum is likely dominated by the approximate horizon masses during epochs when the universe undergoes phase transitions.']",['1999-01-22'] +1292,['eng'],"['Kim, H I', 'Lee, B H', 'Lee, C H']",['Relics of cosmological quark-hadron phase transition'],['Astrophysics and Astronomy'],"['astrophysics, model', 'critical phenomena', 'quark hadron, transition', 'density, fluctuation', 'quark gluon, plasma', 'quark, matter', 'astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'light nucleus, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901286'],"['We propose that the amplified density fluctuations by the vanishing sound velocity effect during the cosmological quark-hadron phase transition lead to quark-gluon plasma lumps decoupled from the expansion of the universe, which may evolve to quark nuggets (QNs). Assuming power-law spectrum of density fluctuations, we investigate the parameter ranges for the QNs to play the role of baryonic dark matter and give inhomogeneities which could affect big-bang nucleosynthesis within the observational bounds of CMBR anisotropy. The QNs can give the strongest constraint ever found on the spectral index.']",['1999-01-22'] +1293,['eng'],"['Mannheim, K']",['Neutrino Oscillations and Blazars'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, flux', 'p, cosmic radiation', 'electron, cosmic radiation', 'cosmic radiation, acceleration', 'cosmic radiation, energy spectrum', 'blazar', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812407'],"['Three independent predictions follow from postulating the existence of protons co-accelerated with electrons in extragalactic jets (i) multi-TeV gamma ray emission from nearby blazars, (ii) extragalactic cosmic ray protons up to ray observations of Mrk 421 and Mrk 501 employing the air-Cerenkov technique are consistent with the predicted gamma ray spectrum, if one corrects for pair attenuation on the infrared background. Prediction (ii) is consistent with cosmic ray data, if one requires that jets are responsible for the extragalactic gamma ray background above 100 MeV. With kubic kilometer neutrino telescopes, it will be possible to test (iii), although the muon event rates are rather low. Neutrino oscillations can increase the event rate by inducing tau-cascades removing the Earth shadowing effect.']",['1998-12-23'] +1294,['eng'],"['Kuiper, L', 'Hermsen, W', 'Verbunt, F', 'Belloni, T', 'Lyne, A']",['High-Energy Observations of the Binary Millisecond Pulsar PSR J0218+4232'],['Astrophysics and Astronomy'],"['talk, Taormina 1998/09/14', 'astrophysics, pulsar', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, time variation', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812408'],"['We report the detection of pulsed X-ray emission ($4.9\\sigma$) from the binary millisecond pulsar PSR J0218+4232 in a 100 ks ROSAT HRI observation. The pulse profile shows a sharp main pulse and an indication for a second weaker pulse at $\\sim$ 0.47 phase separation. The pulsed fraction is 37 \\pm 13%. PSR J0218+4232 was several times in the field of view of the high-energy pulsar was detected above 100 MeV. Spatial and timing analyses of EGRET data indicate that the source is probably multiple: Between 0.1 GeV and 1 GeV PSR J0218+4232 is the most likely counterpart, while the BL Lac 3C66A is the best candidate above 1 GeV. If part of the EGRET signal truly belongs to the pulsar, then this would be the first millisecond $\\gamma$-ray pulsar.']",['1998-12-23'] +1295,['eng'],"['Hess, M']",['The time structure of Cherenkov images generated by TeV gamma-rays and by cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation', 'photon, showers', 'showers, air', 'time dependence', 'Cherenkov counter, imaging']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812341'],"['The time profiles of Cherenkov images of cosmic-ray showers and of gamma-ray showers are investigated, using data gathered with the HEGRA system of imaging atmospheric Cherenkov telescopes during the 1997 outbursts of Mrk 501. Photon arrival times are shown to vary across the shower images. The dominant feature is a time gradient along the major axis of the images. The gradient varies with the distance between the telescope and the shower core, and is maximal for large distances. The time profiles of cosmic-ray showers and of gamma-ray showers differ in a characteristic fashion. The main features of the time profiles can be understood in terms of simple geometrical models. Use of the timing information towards improved shower reconstruction and cosmic-ray suppression is discussed.']",['1998-12-21'] +1296,['eng'],"['Sawyer, R F']",['On some singularities of the correlation functions that determine neutrino opacities'],['Astrophysics and Astronomy'],"['supernova', 'neutrino, scattering', 'neutrino, opacity', 'spin, correlation function', 'time dependence', 'perturbation theory, singularity']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812362'],"['Certain perturbation graphs in the calculation of the effects of the medium on neutrino scattering in supernova matter have a nonintegrable singularity in a physical region. A number of papers have addressed the apparent pathology through an ansatz that invokes higher order (rescattering) effects. Taking the Gamow-Teller terms as an example, we display an expression for the spin-spin correlation function that determines the cross-sections. It is clear from the form that there are no pathologies in the order by order perturbation expansion. Explicit formulae are given for a simple case, leading to an answer that is very different from one given by other authors.']",['1998-12-21'] +1297,['eng'],"['Alvarez-Muñiz, J', 'Vázquez, R A', 'Zas, E']",['Characterization of neutrino signals with radiopulses in dense media through the LPM effect'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino nucleon, interaction', 'charged current', 'showers, electromagnetic', 'radiation, Cherenkov', 'coherence', 'angular distribution', 'Landau-Pomeranchuk-Migdal effect', 'particle identification, flavor', 'Cherenkov counter, water', 'water, solids', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901278'],"['We discuss the possibilities of detecting radio pulses from high energy showers in ice, such as those produced by PeV and EeV neutrino interactions. It is shown that the rich radiation pattern structure in the 100 MHz to few GHz allows the separation of electromagnetic showers induced by photons or electrons above 100 PeV from those induced by hadrons. This opens up the possibility of measuring the energy fraction transmitted to the electron in a charged current electron neutrino interaction with adequate sampling of the angular distribution of the signal. The radio technique has the potential to complement conventional high energy neutrino detectors with flavor information.']",['1999-01-29'] +1298,['eng'],"['Sreekumar, P', 'Bertsch, D L', 'Hartman, R C', 'Nolan, P L', 'Thompson, D J']",['GeV emission from the nearby radio galaxy Centaurus A'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'galaxy, AGN', 'astrophysics', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901277'],"['EGRET has detected 67 sources associated with active galactic nuclei. With the exception of radio galaxy Cen A, all are classified as belonging to the blazar class of active galactic nuclei. The cumulative exposure from multiple EGRET observations has provided the first clear detection of Centaurus A. Unlike the \\gr blazars seen by EGRET which are believed to exhibit near-alignment of the central jet along the line-of-sight, Cen A provides the first evidence for $>$100 MeV emission from a source with a confirmed large-inclination jet. Although the high-energy emission represents a lower luminosity than most EGRET blazars, with the advent of new more sensitive instruments such as GLAST and VERITAS, the detection of off-axis high-energy emission from more distant radio galaxies is an exciting possibility.']",['1999-01-29'] +1299,['eng'],"['Yakovlev, D G', 'Kaminker, A D', 'Levenfish, K P']",['Neutrino emission due to Cooper pairing of nucleons in cooling neutron stars'],['Astrophysics and Astronomy'],"['astrophysics, model', 'n, matter', 'superfluid', 'neutrino, emission', 'temperature, dependence', 'neutrino, luminosity', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812366'],"['The neutrino energy emission rate due to formation of Cooper pairs of neutrons and protons in the superfluid cores of neutron stars is studied. The cases of singlet-state pairing with isotropic superfluid gap and triplet-state pairing with anisotropic gap are analysed. The neutrino emission due to singlet-state pairing of protons is found to be greatly suppressed with respect to the cases of singlet- and triplet-state pairings of neutrons. The neutrino emission due to pairing of neutrons is shown to be very important in the superfluid neutron-star cores with the standard neutrino luminosity and with the luminosity enhanced by the direct Urca process. It can greatly accelerate both, standard and enhanced, cooling of neutron stars with superfluid cores. This enables one to interpret the data on surface temperatures of six neutron stars, obtained by fitting the observed spectra with the hydrogen atmosphere models, by the standard cooling with moderate nucleon superfluidity.']",['1998-12-22'] +1300,['eng'],"['Bullock, J S', 'Somerville, R S', 'MacMinn, D', 'Primack, Joel R']",['Constraining the IMF using TeV gamma ray absorption'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, flux', 'photon photon, interaction', 'electron, pair production', 'energy dependence', 'astrophysics, model', 'galaxy, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812370'],"['Gamma rays of ~TeV energies from distant sources suffer attenuation due to pair production off of ~1 micron EBL photons. We may exploit this process in order to indirectly measure the EBL and constrain models of galaxy formation. Here, using semi-analytic models of galaxy formation, we examine how gamma ray absorption may be used as an indirect probe of the stellar initial mass function (IMF), although there is a degeneracy with dust modeling. We point out that with the new generation of gamma ray telescopes including STACEE, MAGIC, HESS, VERITAS, and Milagro, we should soon possess a wealth of new data and a new method for probing the nature of the IMF.']",['1998-12-22'] +1301,['eng'],"['Mannheim, K', 'Protheroe, R J', 'Rachen, J P']",['On the cosmic ray bound for models of extragalactic neutrino production'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, production', 'galaxy, AGN', 'photon, cosmic radiation', 'p, cosmic radiation', 'photon p, interaction', 'pi, photoproduction', 'cosmic radiation, flux', 'cosmic radiation, spectra', 'cosmic radiation, particle source', 'energy loss, adiabatic', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812398'],"['We obtain the maximum diffuse neutrino intensity predicted by hadronic photoproduction models of active galactic nuclei, and other sources such as gamma ray bursts, that is consistent with the observed cosmic ray spectrum and diffuse extragalactic gamma ray background. For this, we compare the contributions to the cosmic ray intensity of extragalactic neutrino sources with the experimental data at energies above 10^15 eV, employing a transport calculation of energetic protons traversing cosmic photon backgrounds. We take into account source evolution, optical depth effects in the sources, and adiabatic losses of protons in magnetic fields on scales of galaxy clusters. The strongest cosmic ray bound applies to photoproduction sources which are optically thin for the emission of neutrons, and for which adiabatic losses of the protons resulting from neutron decay can be neglected. We find that our upper bound is strongly energy dependent, and is much higher than the bound obtained by Waxman and Bahcall at most energies, agreeing only at a neutrino energy of ~10^18 eV. As a corollary of our work we find that the present-day flux of cosmic rays from gamma ray bursts falls short of explaining the observed cosmic rays above 10^19 eV, if the gamma ray burst luminosity density evolves similarly to that of galaxies or active galactic nuclei and if they emit equal fluxes of gamma rays and protons. We also confirm that hadronically emitting active galactic nuclei can produce both the extragalactic gamma ray background and cosmic rays at highest energies, implying interesting event rates in large underwater or deep-ice neutrino detectors.']",['1998-12-22'] +1302,['eng'],"['Kuznetsov, O A', 'Prokhorov, M E', 'Sazhin, M V', 'Chechetkin, V M']",['Orbital evolution of a binary neutron star and gravitational radiation'],['Astrophysics and Astronomy'],"['n, matter', 'binary', 'gravitational radiation', 'energy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812400'],"['We consider the dependence of the internal structure of a neutron star in a close binary system on the semi-major axis of the binary orbit, focusing on the case when the Roche lobes of the components are nearly filled. We adopt a polytropic equation of state. The temporal evolution of the semi-major axis and its dependence on the mass ratio of the binary components and the polytropic index are determined. The calculation are carried out right up to the moment of contact, when quasi-stationary model becomes invalid. We analyze differences in the shapes of the pulses of gravitational radiation emitted by a pair of point masses and by a binary neutron star, taking into account its internal structure and tidal deformations.']",['1998-12-23'] +1303,['eng'],"['Mukherjee, R']",['High Energy Gamma-Ray Emission From Blazars'],['Astrophysics and Astronomy'],"['talk, Calcutta 1998/01/11', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'luminosity, high', 'time variation', 'jet, relativistic', 'energy spectrum', 'data analysis method', 'experimental results', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901222'],"['We will present a summary of the observations of blazars by the Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory (CGRO). EGRET has detected high energy gamma-ray emission at energies greater than 100 MeV from more that 50 blazars. These sources show inferred isotropic luminosities as large as $3\\times 10^{49}$ ergs s$^{-1}$. One of the most remarkable characteristics of the EGRET observations is that the gamma-ray luminosity often dominates the bolometric power of the blazar. A few of the blazars are seen to exhibit variability on very short time-scales of one day or less. The combination of high luminosities and time variations seen in the gamma-ray data indicate that gamma-rays are an important component of the relativistic jet thought to characterize blazars. Currently most models for blazars involve a beaming scenario. In leptonic models, where electrons are the primary accelerated particles, gamma-ray emission is believed to be due to inverse Compton scattering of low energy photons, although opinions differ as to the source of the soft photons. Hardronic models involve secondary production or photomeson production followed by pair cascades, and predict associated neutrino production.']",['2000-10-05'] +1304,['eng'],"['Melchiorri, A', 'Sazhin, M V', 'Shulga, V V', 'Vittorio, N']",['The Gravitational-Wave contribution to the CMB anisotropies'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'statistical analysis', 'inflationary universe', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901220'],['We study the possible contribution of a stochastic gravitational wave background to the anisotropy of the cosmic microwave background (CMB) in cold and mixed dark matter (CDM and MDM) models. We test this contribution against recent detections of CMB anisotropy at large and intermediate angular scales. Our likelihood analysis indicates that models with blue power spectra ($n that by including the possibility of such background in CMB data analysis it can drastically alter the conclusion on the remaining cosmological parameters.'],['1999-01-19'] +1305,['eng'],"['Mannheim, P D']",['Conformal gravity and a naturally small cosmological constant'],['Astrophysics and Astronomy'],"['gravitation, conformal', 'astrophysics, fundamental constant', 'Friedman model', 'matter, density', 'talk, Austin 2000/12/10']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901219'],"['We show that within conformal gravity an assumption regarding only the sign of the cosmological constant, namely that $\\Lambda$ be negative, is sufficient, no matter what its magnitude, to not only make its contribution to current era cosmology naturally be of order one today, but to even do so in a way which is fully compatible with the recent high $z$ supernovae cosmology data.']",['1999-01-19'] +1306,['eng'],"['Roy, M F']",['Ultra High Energy Neutrinos from Supernova Remnants'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, emission', 'neutrino, cosmic radiation', 'p p, interaction', 'photon, cosmic radiation', 'cosmic radiation, flux', 'nuclear reaction', 'neutrino, energy spectrum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901215'],"['In this paper we discuss possible ultra high energy ($\\ge$ TeV) neutrino emission from Supernova Remnants (SNRs), specifically the hadronic gamma ray production models. Recent very high energy (VHE) $\\gamma$ ray observation from SNRs is the main motivation behind this study.']",['1999-01-18'] +1307,['eng'],"['Maartens, R', 'Triginer, J']",['Backreaction effects of dissipation in neutrino decoupling'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, decoupling', 'back reaction', 'temperature', 'entropy', 'transport theory', 'model, hydrodynamical', 'effect, dissipation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901211'],"['Dissipative effects during neutrino decoupling in the early universe create a small backreaction on the Hubble rate, and lead to a small rise in temperature and entropy. We use a simplified thermo-hydrodynamic model, which provides a causal approximation to kinetic theory, in order to estimate the backreaction effects and the entropy production.']",['1999-01-18'] +1308,['eng'],"['Konopelko, A K', 'Hemberger, M', 'Aharonian, F A']",['Performance of the Stereoscopic System of the HEGRA Imaging Air Cherenkov Telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'Cherenkov counter, imaging', 'angular resolution', 'energy resolution']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901199'],"['Based on the Monte Carlo simulations we have studied the performance of the HEGRA system of imaging air Cherenkov telescopes (IACTs) in its present configuration of 4 IACTs as well as in its future final configuration of 5 IACTs. Here we present the results on the basic characteristics of the IACT system which are used in the standard data analysis procedure, i.e., the collection areas, the detection rates, the angular resolution, the energy resolution, and the gamma/hadron-separation efficiency. By comparing several key Monte Carlo predictions with experimental results it is possible to check the accuracy of the simulations. The Monte Carlo results concerning hadron-nuclear showers are tested with the recorded cosmic ray events and the results concerning photon-induced showers are tested with a large data sample of gamma-rays observed from BL Lac object Mkn 501 during its high flaring activity in 1997. Summarizing the simulations and current observations we give the basic recommendations of using the instrument and the major values of its sensitivity.']",['1999-01-18'] +1309,['eng'],"['Shi, X', 'Fuller, G M']",['A New Dark Matter Candidate'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutrino, sterile', 'neutrino, oscillation', 'astrophysics, model', 'neutrino, mixing angle', 'lepton number, asymmetry', 'light nucleus, production', 'energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810076'],"['We suggest \\sim 100 eV to \\sim keV sterile neutrinos produced non-thermally in the early universe through lepton number-driven active-sterile neutrino mixing as a dark matter candidate. The initial lepton number asymmetry required in this scenario is, serendipitously, roughly that required to solve the Big Bang Nucleosynthesis ""crisis"" in discrepant $^4$He and $^2$H yields. The active-sterile neutrino conversion process here favors the production of lower energy sterile neutrinos, yielding a comoving neutrino free-streaming length as small as sub-Mpc. We deem these sterile neutrinos to be ""Cool Dark Matter"": behaving as ""cold"" above the dwarf galaxy scales; and as ""hot"" on smaller scales.']",['1998-10-07'] +1310,['eng'],"['Lee, W', 'Fang, L Z']",['Mass Density Perturbations from Inflation with Thermal Dissipation'],['Astrophysics and Astronomy'],"['inflationary universe', 'mass, density', 'spectra, perturbation', 'density, perturbation', 'cosmic radiation, background', 'temperature, fluctuation', 'field theory, scalar', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901195'],"[""We study the power spectrum of the mass density perturbations in an inflation scenario that includes thermal dissipation. We show that the condition on which the thermal fluctuations dominate the primordial density perturbations can easily be realized even for weak dissipation, i.e., the rate of dissipation is less than the Hubble expansion. We find that our spectrum of primordial density perturbations follows a power law behavior, and exhibits a ``thermodynamical'' feature -- the amplitude and power index of the spectrum depend mainly on the thermodynamical variable $M$, the inflation energy scale. Comparing this result with the observed temperature fluctuations of the cosmic microwave background, we find that both amplitude and index of the power spectrum can be fairly well fitted if $M \\sim 10^{15}-10^{16}$ GeV.""]",['1999-01-15'] +1311,['eng'],"['Kamae, T', 'Ohsugi, T', 'Thompson, D J', 'Watanabe, K']",['Studying the High-Energy $\\gamma$-Ray Sky with Glast'],['Astrophysics and Astronomy'],"['talk, Nagoya 1998/07/12', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'photon, showers', 'astrophysics', 'counters and detectors, proposed', 'semiconductor detector, microstrip', 'computer']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901187'],"['Building on the success of the Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory, the Gamma-ray Large Area Space Telescope (GLAST) will make a major step in the study of such subjects as blazars, gamma-ray bursts, the search for dark matter, supernova remnants, pulsars, diffuse radiation, and unidentified high-energy sources. The instrument will be built on new and mature detector technologies such as silicon strip detectors, low-power low-noise LSI, and a multilevel data acquisition system. GLAST is in the research and development phase, and one full tower (of 25 total) is now being built in collaborating institutes. The prototype tower will be tested thoroughly at SLAC in the fall of 1999.']",['1999-01-15'] +1312,['eng'],"['Bertolami, O']","['$\\gamma$-ray bursts, axion emission and string theory dilaton']",['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'supernova', 'axion, emission', 'string model', 'dilaton', 'radiation, electromagnetic', 'coupling, (axion dilaton)', 'fireball, expansion', 'energy, exchange']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901184'],"['The emission of axions from supernovae is an interesting possibility to account for the Gamma-Ray Bursts provided their energy can be effectively converted into electromagnetic energy elsewhere. The connection between supernova and gamma-ray bursts has been recently confirmed by the observed correlation between the burst of April 25, 1998 and the supernova SN1998bw. We argue that the axion convertion into photons can be more efficient if one considers the coupling between an intermediate scale axion and the string theory dilaton along with the inclusion of string loops. We also discuss the way dilaton dynamics may allow for a more effective energy exchange with electromagnetic radiation in the expansion process of fireballs.']",['1999-01-15'] +1313,['eng'],"['Morselli, A', 'Perrino, A', 'Picozza, P', 'Severson, S A', 'Caraveo, P A', 'Mereghetti, S', 'Tavani, M', 'Barbiellini, Guido', 'Vacchi, A']",['The AGILE $\\gamma$-ray detector'],['Astrophysics and Astronomy'],"['talk, Rome 1998/05/18', 'photon, cosmic radiation', 'counters and detectors, satellite', 'electron, pair production', 'semiconductor detector, microstrip', 'scintillation counter', 'angular resolution', 'energy resolution', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901183'],"['The gamma-ray detector AGILE, operating in the energy range from 30 MeV to 50 GeV, is composed by a tracking part, a light imaging calorimeter and an anticoincidence system. Here we describe the detector and its capabilities to determine the arrival direction and energy of the detected photons.']",['1999-01-15'] +1314,['eng'],"['Turner, M S']",['Cosmology Update 1998'],['Astrophysics and Astronomy'],"['talk, Santa Fe 1998/06/14', 'inflationary universe', 'astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'neutrino, cosmic radiation', 'light nucleus, production', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901168'],"['For two decades the hot big-bang model has been referred to as the standard cosmology -- and for good reason. For just as long cosmologists have known that there are fundamental questions that are not addressed by the standard cosmology and point to a grander theory. The best candidate for that grander theory is inflation + cold dark matter. It holds that the Universe is flat, that slowly moving elementary particles left over from the earliest moments provide the cosmic infrastructure, and that the primeval density inhomogeneities that seed all large-scale structure arose from quantum fluctuations. There is now prima facie evidence that supports two basic tenets of this paradigm, and an avalanche of high-quality cosmological observations will soon make this case stronger or will break it. Key questions remain to be answered; foremost among them are: identification and detection of the cold dark matter particles and elucidation of the mysterious dark-energy component. These are exciting times in cosmology!']",['1999-01-14'] +1315,['eng'],"['Gondek-Rosinska, D', 'Zdunik, J L']",['Avoided crossings in radial pulsations of neutron and strange stars'],['Astrophysics and Astronomy'],"['n, matter', 'matter, strangeness', 'nuclear matter', 'oscillation, adiabatic', 'bag model', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901167'],"['Radial pulsations of neutron stars and strange quark stars with nuclear crust are studied. The avoided crossing phenomenon occurring for the radial modes is found and discussed. Neutron star models are constructed using a realistic equation of state of dense matter and strange star models using a phenomenological bag model of quark matter. The eigenfrequencies of the three lowest modes of linear, adiabatic pulsations are calculated, using the relativistic equations for the radial oscillations.']",['1999-01-14'] +1316,['eng'],"['Aharonian, F A']",['The Cosmic Ray Proton Spectrum determined with the Imaging Atmospheric Cherenkov-Technique'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'cosmic radiation, energy spectrum', 'showers, air', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901160'],"['The HEGRA system of 4 Imaging Atmospheric Cherenkov Telescopes (IACTs) has been used to determine the flux and the spectrum of cosmic ray protons over a limited energy range around 1.5 TeV. Although the IACT system is designed for the detection of gamma-rays with energies above 500 GeV, it has also a large detection area of $ \\simeq 10^6 m^2 \\cdot 3 msr$ for primary protons of energies above 1 TeV and the capability to reconstruct the primary proton energy with a reasonable accuracy $\\Delta$E/E of 50% near this threshold. Furthermore, the principle of stereoscopic detection of air showers permits the effective suppression of air showers induced by heavier primaries already on the trigger level, and in addition on the software level by analysis of the stereoscopic images. The combination of both capabilities permits a determination of the proton spectrum almost independently of the cosmic ray chemical composition. The accuracy of our estimate of the spectral index at 1.5 TeV is limited by systematic uncertainties and is comparable to the accuracy achieved with recent balloon and space borne experiments. In this paper we describe in detail the analysis tools, namely the detailed Monte Carlo simulation, the analysis procedure and the results. We determine the local (i.e. in the range of 1.5 to 3 TeV) differential spectral index to be $\\gamma_p = 2.72\\pm 0.02_{stat.}{\\pm 0.15}_{syst.}$ and obtain an integral flux above 1.5 TeV of $F(> 1.5 TeV) =3.1\\pm 0.6_{stat.}\\pm 1.2_{syst.} 10^{-2}/s sr m^2$.']",['1999-01-14'] +1317,['eng'],"['Schertler, K', 'Leupold, S', 'Schaffner-Bielich, J']",['Neutron stars and quark phases in the NJL model'],['Astrophysics and Astronomy'],"['astrophysics', 'n, matter', 'quark, matter', 'critical phenomena, confinement', 'Jona-Lasinio-Nambu model', 'quark, momentum', 'bag model', 'baryon number, density', 'quark, mass', 'energy, density', 'potential, chemical', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901152'],['We study the possible existence of deconfined quark matter in the interior of neutron stars using the Nambu-Jona-Lasinio model to describe the quark phase. We find that typical neutron stars with masses around 1.4 solar masses do not possess any deconfined quark matter in their center. This can be traced back to the property of the NJL model which suggests a large constituent strange quark mass over a wide range of densities.'],['1999-01-13'] +1318,['eng'],"['Futagami, T']",['Observation of the east-west anisotropy of the atmospheric neutrino flux'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, anisotropy', 'cosmic radiation, energy spectrum', 'cosmic radiation, primary', 'magnetic field, geophysics', 'neutrino nucleon, interaction', 'charged current', 'angular distribution', 'Cherenkov counter, experimental results', 'deep underground detector, KAMIOKANDE']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901139'],"[""The east-west anisotropy, caused by the deflection of primary cosmic rays in the Earth's magnetic field, is observed for the first time in the flux of atmospheric neutrinos. Using a 45 kt-year exposure of the Super-Kamiokande detector, 552 e-like and 633 mu-like horizontally-going events are selected in the momentum range between 400 and 3000 MeV/c. The azimuthal distribution of e-like and mu-like events agrees with the expectation from atmospheric neutrino flux calculations that account for the geomagnetic field, verifying that the geomagnetic field effects in the production of atmospheric neutrinos in the GeV energy range are well understood.""]",['1999-01-13'] +1319,['eng'],"['Linde, Andrei D', 'Sasaki, M', 'Tanaka, T']",['CMB in Open Inflation'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'tunneling', 'bubble, production', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, perturbation', 'perturbation, scalar', 'perturbation, tensor', 'effective potential', 'instanton', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901135'],"['The possibility to have an infinite open inflationary universe inside a bubble of a finite size is one of the most interesting realizations extensively discussed in the literature. The original idea was based on the theory of tunneling and bubble formation in the theories of a single scalar field. However, for a long time we did not have any consistent models of this type, so it was impossible to compare predictions of such models with the observational data on the CMB anisotropy. The first semi-realistic model of this type was proposed only very recently, in hep-ph/9807493. Here we present the results of our investigation of the scalar and tensor perturbation spectra and the resulting CMB anisotropy in such models. In all models which we have studied there are no supercurvature perturbations. The spectrum of scalar CMB anisotropies has a minimum at small l and a plateau at l > O(10) for low Omega_0. Meanwhile tensor CMB anisotropies are peaked at l=2. Relative magnitude of the scalar CMB spectra versus tensor CMB spectra at small l depends on the parameters of the models.']",['1999-01-13'] +1320,['eng'],"['Padovani, P']",['High Energy Emission from AGN and Unified Schemes'],['Astrophysics and Astronomy'],"['talk, Vulcano 1998/05/25', 'galaxy, AGN', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901130'],"['Active Galactic Nuclei (AGN) are now known to be strong gamma-ray emitters. After briefly describing AGN classification and the main ideas behind unified schemes, I summarize the main properties of blazars (that is BL Lacs and flat-spectrum radio quasars) and their connection with relativistic beaming. Finally, I address the question of why blazars, despite being extreme and very rare objects, are the only AGN detected at high (E > 100 MeV) energies, and touch upon the relevance of TeV astronomy for AGN research.']",['1999-01-12'] +1321,['eng'],"['Komatsu, E', 'Futamase, T']",['Complete constraints on a nonminimally coupled chaotic inflationary scenario from the cosmic microwave background'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'density, perturbation', 'gravitational radiation', 'perturbation, scalar', 'perturbation, tensor', 'spectra', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901127'],"['We present complete constraints imposed from observations of the cosmic microwave background radiation (CMBR) on the chaotic inflationary scenario with a nonminimally coupled inflaton field proposed by Fakir and Unruh (FU). Our constraints are complete in the sense that we investigate both the scalar density perturbation and the tensor gravitational wave in the Jordan frame, as well as in the Einstein frame. This makes the constraints extremely strong without any ambiguities due to the choice of frames. We find that the FU scenario generates tiny tensor contributions to the CMBR relative to chaotic models in minimal coupling theory, in spite of its spectral index of scalar perturbation being slightly tilted. This means that the FU scenario will be excluded if any tensor contributions to CMBR are detected by the forthcoming satellite missions. Conversely, if no tensor nature is detected despite the tilted spectrum, a minimal chaotic scenario will be hard to explain and the FU scenario will be supported.']",['1999-01-12'] +1322,['eng'],"['Liddle, A R']",['An introduction to cosmological inflation'],['Astrophysics and Astronomy'],"['lectures, Trieste 1998/06/29', 'inflationary universe', 'density, perturbation', 'gravitational radiation', 'cosmic radiation, background', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901124'],"[""An introductory account is given of the inflationary cosmology, which postulates a period of accelerated expansion during the Universe's earliest stages. The historical motivation is briefly outlined, and the modelling of the inflationary epoch explained. The most important aspect of inflation is that it provides a possible model for the origin of structure in the Universe, and key results are reviewed, along with a discussion of the current observational situation and outlook.""]",['1999-01-12'] +1323,['eng'],"['Turner, M S', 'Tyson, J A']",['Cosmology at the Millennium'],['Astrophysics and Astronomy'],"['review', 'inflationary universe', 'astrophysics, missing-mass', 'particle physics', 'cosmic radiation, background', 'galaxy', 'spectra, fluctuation', 'light nucleus, production', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901113'],"['One hundred years ago we did not know how stars generate energy, the age of the Universe was thought to be only millions of years, and our Milky Way galaxy was the only galaxy known. Today, we know that we live in an evolving and expanding Universe comprising billions of galaxies, all held together by dark matter. With the hot big-bang model, we can trace the evolution of the Universe from the hot soup of quarks and leptons that existed a fraction of a second after the beginning to the formation of galaxies a few billion years later, and finally to the Universe we see today 13 billion years after the big bang, with its clusters of galaxies, superclusters, voids, and great walls. The attractive force of gravity acting on tiny primeval inhomogeneities in the distribution of matter gave rise to all the structure seen today. A paradigm based upon deep connections between cosmology and elementary particle physics -- inflation + cold dark matter -- holds the promise of extending our understanding to an even more fundamental level and much earlier times, as well as shedding light on the unification of the forces and particles of nature. As we enter the 21st century, a flood of observations is testing this paradigm.']",['1999-01-12'] +1324,['eng'],"['Turner, M S']",['Dark Matter and Energy in the Universe'],['Astrophysics and Astronomy'],"['talk, Enkoping 1998/08/20', 'inflationary universe', 'astrophysics, missing-mass', 'energy, density', 'baryon', 'astrophysics, fundamental constant', 'field theory, scalar', 'matter, density', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901109'],"['For the first time, we have a plausible and complete accounting of matter and energy in the Universe. Expressed a fraction of the critical density it goes like this: neutrinos, between 0.3% and 15%; stars, between 0.3% and 0.6%; baryons (total), 5% +/- 0.5%; matter (total), 40% +/- 10%; smooth, dark energy, 80% +/- 20%; totaling to the critical density (within the errors). This accounting is consistent with the inflationary prediction of a flat Universe and defines three dark-matter problems: Where are the dark baryons? What is the nonbaryonic dark matter? What is the nature of the dark energy? The leading candidate for the (optically) dark baryons is diffuse hot gas; the leading candidates for the nonbaryonic dark matter are slowly moving elementary particles left over from the earliest moments (cold dark matter), such as axions or neutralinos; the leading candidates for the dark energy involve fundamental physics and include a cosmological constant (vacuum energy), a rolling scalar field (quintessence), and a network of light, frustrated topological defects.']",['1999-01-12'] +1325,['eng'],"['Konopelko, A K']",['Energy Spectrum of TeV $\\gamma$-Rays from Crab Nebula'],['Astrophysics and Astronomy'],"['talk, Madrid 1998/07/20', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'Cherenkov counter, imaging', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901094'],"['The Crab Nebula has been observed by the HEGRA stereoscopic system of 4 imaging air Cherenkov telescopes (IACTs) for about 100 hours from 1997 September to 1998 March. The recent detailed studies on the system performance give an energy threshold and an energy resolution for gamma-rays of 500 GeV and very broad energy range from 500 GeV to 25 TeV, using the observations at zenith angles up to 50 degree. The pure power-law spectrum in TeV gamma-rays constrains the physics parameters of the nebula environment as well as the models of photon emission.']",['1999-01-11'] +1326,['eng'],"['Konopelko, A K']",['The TeV spectrum of Mkn 501 as measured during the high state in 1997 by the HEGRA stereoscopic system of imaging air Cherenkov telescopes'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation', 'Cherenkov counter, imaging', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901093'],"['The BL Lac object Mkn 501 has shown very high emission in TeV gamma-rays from March to October, 1997. During this period the source was continuously monitored with the HEGRA stereoscopic system of 4 imaging air Cherenkov telescopes for a total exposure time of 110 hours. The unprecedented statistics of about 38,000 TeV photons, combined with the good energy resolution of ~20 % over the entire energy range and with detailed simulations of the detector response, allowed a determination of the average energy spectrum from 500 GeV to 24 TeV. Although the gamma-ray flux varied strongly with time, the daily energy spectra remained rather constant in their shape. Therefore it is justified to derive a time averaged spectrum and thus to extend, for the first time, the spectral measurement well beyond 10 TeV. This TeV spectrum of Mkn 501 shows a gradual steepening which could be caused by a number of physical processes, such as a limited energy range of the radiating particles, intrinsic gamma-ray absorption inside the source, the Klein-Nishina effect (in the case of an inverse Compton origin of the radiation) and finally, an absorption of the TeV gamma-rays propagating in the intergalactic medium.']",['1999-01-11'] +1327,['eng'],"['Krawczynski, H']",['Study of the TeV Emission from Mkn 501 with the Stereoscopic Cherenkov Telescope System of HEGRA'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation', 'correlation, time', 'Cherenkov counter, imaging', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901086'],"['The HEGRA system of 4 Imaging Atmospheric Cherenkov Telescopes (IACTs) has been used since March 1997 for a comprehensive study of the gamma-ray emission from the BL Lac object Mkn 501 in the energy range above 500 GeV. Taking advantage of the unique capabilities of the IACT system, i.e. an unprecedented flux sensitivity in the TeV energy range and an unique energy resolution of better than 20% for individual TeV photons, detailed information about the temporal and spectral characteristics of the source during its spectacular bright phase in 1997 is reported. Further more, using the large HEGRA and Rossi X-Ray Timing Explorer All Sky Monitor (RXTE ASM) data bases, the correlation of the X-ray and the TeV activity of the source is discussed. Finally, an outlook over present and future activities is given.']",['1999-01-11'] +1328,['eng'],"['Sarazin, C L']",['The Energy Spectrum of Primary Cosmic Ray Electrons in Clusters of Galaxies and Inverse Compton Emission'],['Astrophysics and Astronomy'],"['electron, cosmic radiation', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'galaxy, cluster', 'energy loss', 'photon, Compton scattering', 'synchrotron, emission', 'bremsstrahlung', 'luminosity', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901061'],"['Models for the evolution of the integrated energy spectrum of primary cosmic ray electrons in clusters of galaxies have been calculated, including the effects of losses due to inverse Compton (IC), synchrotron, and bremsstrahlung emission, and Coulomb losses to the intracluster medium (ICM). The combined time scale for these losses reaches a maximum of ~3e9 yr for electrons with a Lorentz factor ~300. Only clusters in which there has been a substantial injection of relativistic electrons since z <~ 1 will have any significant population of primary cosmic ray electrons at present. In typical models, there is a broad peak in the electron energy distribution extending to gamma~300, and a steep drop in the electron population beyond this. In clusters with current particle injection, there is a power-law tail of higher energy electrons with an abundance determined by the current rate of injection. A significant population of electrons with gamma~300, associated with the peak in the particle loss time, is a generic feature of the models. The IC and synchrotron emission from these models was calculated. In the models, EUV and soft X-ray emission are nearly ubiquitous. This emission is produced by electrons with gamma~300. The spectra are predicted to drop rapidly in going from the EUV to the X-ray band. The IC emission also extends down the UV, optical, and IR bands with a fairly flat spectrum. Hard X-ray (HXR) and diffuse radio emission due to high energy electrons (gamma~10e4) is present only in clusters which have current particle acceleration. Assuming that the electrons are accelerated in ICM shocks, one would only expect diffuse HXR/radio emission in clusters which are currently undergoing a large merger.']",['1999-01-07'] +1329,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'McQueen, S', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['Correlation between the TeV $\\gamma$-ray and X-ray emission from an accreting X-ray binary'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'photon, cosmic radiation', 'cosmic radiation, energy', 'cosmic radiation, particle source', 'cosmic radiation, correlation', 'cosmic radiation, flux', 'time dependence', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812123'],['The signal strength of TeV gamma rays from the accreting X-ray binary Cen X-3 shows evidence for correlation with both the RXTE/ASM and the BATSE X-ray signal strengths. The time scale for the variability of the gamma rays may be similar to that of X-rays and as short as a day.'],['1998-12-08'] +1330,['eng'],"['Rhode, W', 'Ensslin, T A', 'Biermann, P L']",['Cosmic Rays in the Galactic Center Region'],['Astrophysics and Astronomy'],"['galaxy', 'photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, injection', 'supernova', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811361'],"['EGRET data on the Gamma ray emission from the inner Galaxy have shown a rather flat spectrum, extending to about 50 GeV. It is usually assumed that these gamma-rays arise from the interactions of cosmic ray nuclei with ambient matter. Cosmic Ray particles have been observed up to 3 10^20 eV, with many arguments suggesting, that up to about 3 10^18 eV they are of Galactic origin. Cosmic ray particles get injected by supernova explosions. Their injected spectrum is steepened by diffusive losses from the Galaxy to yield the observed spectrum. As cosmic ray particles roam around in the Galactic disk, they encounter molecular clouds and through p-p collisions produce gamma rays from pion decay. The flux and spectrum of these gamma rays is then a clear signature of cosmic rays throughout the Galaxy. Star formation activity peaks in the central region of the Galaxy, around the Galactic Center. Looking then at the gamma ray spectrum of the central region of our Galaxy yields clues as to where the cosmic ray particles interact, and with what spectrum. Using the FLUKA Monte-Carlo, we have modelled this spectrum, and find a best fit for a powerlaw spectral index of 2.34, rather close to the suggested injection spectrum for supernovae which explode into their own winds. This suggests that most cosmic ray interaction happens near the sources of injection; this is consistent with the spectrum of cosmic ray nuclei derived from spallation. One consequence is that cosmic ray heating and ionization should be strong in the Galactic Center region.']",['1998-11-24'] +1331,['eng'],"['Arras, P', 'Lai, D']",['Neutrino-Nucleon Interactions in Magnetized Neutron-Star Matter'],['Astrophysics and Astronomy'],"['astrophysics', 'neutrino nucleon, interaction', 'neutral current', 'charged current', 'neutrino/e, absorption', 'antineutrino/e, absorption', 'nuclear matter', 'magnetic field', 'parity, violation', 'Boltzmann equation', 'neutrino, flux', 'moment', 'thermodynamics', 'nucleon, polarization', 'differential cross section', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811371'],"['We study neutrino-nucleon scattering and absorption in a dense, magnetized nuclear medium. These are the most important sources of neutrino opacity governing the cooling of a proto-neutron star in the first tens of seconds after its formation. Because the weak interaction is parity violating, the absorption and scattering cross-sections depend asymmetrically on the directions of the neutrino momenta with respect to the magnetic field. We develop the moment formalism of neutrino transport in the presence of such asymmetric opacities and derive explicit expressions for the neutrino flux and other angular moments of the Boltzmann transport equation. For a given neutrino species, there is a drift flux of neutrinos along the magnetic field in addition to the usual diffusive flux. This drift flux depends on the deviation of the neutrino distribution function from thermal equilibrium. Hence, despite the fact that the neutrino cross-sections are asymmetric throughout the star, asymmetric neutrino flux can be generated only in the outer region of the proto-neutron star where the neutrino distribution deviates significantly from thermal equilibrium. In addition to the asymmetric absorption opacity arising from nucleon polarization, we find the contribution of the electron (or positron) ground state Landau level. For neutrinos of energy less than a few times the temperature, this is the dominant source of asymmetric opacity. Lastly, we discuss the implication of our result to the origin of pulsar kicks: in order to generate kick velocity of a few hundred km/s from asymmetric neutrino emission using the parity violation effect, the proto-neutron star must have a dipole magnetic field of at least $10^{15}-10^{16}$ G.']",['1998-11-24'] +1332,['eng'],"['Cebrian, S', 'García, E', 'González, D', 'Irastorza, I G', 'Morales, A', 'Morales, J', 'De Solorzano, A O', 'Puimedón, J', 'Salinas, A', 'Sarsa, M L', 'Scopel, S', 'Villar, J A']",['Prospects of solar axion searches with crystal detectors'],['Astrophysics and Astronomy'],"['axion, search for', 'axion, solar', 'transition, axion photon', 'Primakoff effect', 'coupling, (axion 2photon)', 'axion, mass', 'solid-state counter, crystal', 'efficiency', 'time, correlation', 'experimental methods, proposed', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811359'],"['A calculation of the expected signal due to Primakoff coherent conversion of solar axions into photons via Bragg scattering in several crystal detectors is presented. The results are confronted with the experimental sensitivities of present and future experiments concluding that the sensitivity of crystal detectors does not challenge the globular cluster limit on the axion-photon coupling g_a. In particular, in the axion mass window m_a ~> 0.03 eV explored with this technique (not accessible at present by other methods) g_a might be constrained down to 10^-9 GeV^-1 (the recent helioseismological bound) provided that significant improvements in the parameters and performances of these detectors be achieved and large statistics accumulated. This bound should be considered as a minimal goal for the sensitivity of future crystal experiments. Consequently, finding a positive signal at this level of sensitivity would necessarily imply revisiting other more stringent astrophysical limits derived for the same range of m_a values.']",['1998-11-24'] +1333,['eng'],"['Tavani, M', 'Barbiellini, Guido', 'Caraveo, P A', 'Pippo, S D', 'Mereghetti, S', 'Pellizzoni, A', 'Perrino, A', 'Picozza, P', 'Schiavon, R P', 'Severson, S A', 'Tavecchio, F', 'Vacchi, A', 'Vercellone, S']",['AGILE'],['Astrophysics and Astronomy'],"['talk, Rome 1998/05/18', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'counters and detectors, satellite', 'semiconductor detector', 'astrophysics, galaxy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812096'],"[""AGILE is an innovative, cost-effective gamma-ray mission proposed to the ASI Program of Small Scientific Missions. It is planned to detect gamma-rays in the 30 MeV - 50 GeV energy band and operate as an {\\bf Observatory} open to the international community. Primary scientific goals include the study of AGNs, gamma-ray bursts, Galactic sources, unidentified gamma-ray sources, solar flares, and diffuse gamma-ray emission. AGILE is planned to be operational during the year 2001 for a 3-year mission. It will ideally `fill the gap' between EGRET and GLAST, and support ground-based multiwavelength studies of high-energy sources.""]",['1998-12-07'] +1334,['eng'],"['Krennrich, F', 'Biller, S D', 'Bond, I H', 'Boyle, P J', 'Bradbury, S M', 'Breslin, A C', 'Buckley, J H', 'Burdett, A M', 'Bussons-Gordo, J', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hall, T', 'Hillas, A M', 'Lamb, R C', 'Lessard, R W', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Moriarty, P', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Vasilev, V', 'Weekes, T C']",['Tev Blazars'],['Astrophysics and Astronomy'],"['talk, Taormina 1998/09/14', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'energy spectrum', 'cosmic radiation, flux', 'upper limit', 'correlation', 'astrophysics, blazar', 'galaxy, AGN', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812029'],['The close relation between ground-based TeV observations and satellite borne The observations which involve the TeV component in blazar studies are reviewed.'],['1998-12-02'] +1335,['eng'],"['Wu, J H P', 'Pina-Avelino, P', 'Shellard, E P S', 'Allen, B']","['Cosmic Strings, Loops, and Linear Growth of Matter perturbations']",['Astrophysics and Astronomy'],"['astrophysics, string', 'string, network', 'topology, defect', 'correlation', 'matter, perturbation', 'energy, density', 'astrophysics, missing-mass', 'density, fluctuation', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812156'],"['We describe the detailed study and results of high-resolution numerical simulations of string-induced structure formation in open universes and those with a non-zero cosmological constant. The effect from small loops generated from the string network has also been investigated. We provide a semi-analytical model which can reproduce these simulation results. A detailed study of cosmic string network properties regarding structure formation is also given, including the correlation time, the topological analysis of the source spectrum, the correlation between long strings and loops, and the evolution of long-string and loop energy densities. For models with $\\Gamma=\\Omega h=0.1--0.2 and a cold dark matter background, we show that the linear density fluctuation power spectrum induced by cosmic strings has both an amplitude at $8 h^{-1}$Mpc, $\\sigma_8$, and an overall shape which are consistent within uncertainties with those currently inferred from galaxy surveys. The cosmic string scenario with hot dark matter requires a strongly scale-dependent bias in order to agree with observations.']",['1998-12-09'] +1336,['eng'],"['Lue, A', 'Wang, L', 'Kamionkowski, M P']",['Cosmological Signature of New Parity-Violating Interactions'],['Astrophysics and Astronomy'],"['parity, violation', 'cosmic radiation, background', 'cosmic radiation, temperature', 'cosmic radiation, polarization', 'inflationary universe', 'gravitational radiation', 'field theory, scalar', 'proposed experiment', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812088'],"['Does Nature yield any manifestations of parity violation other than those observed in weak interactions? A map of the cosmic microwave background (CMB) temperature and polarization will provide a new signature of P violation. We give two examples of new P violating interactions, which may have something to do with Planck-scale physics, inflation, and/or quintessence, that would give rise to such a signature. Although these effects would most likely elude detection by MAP and the Planck Surveyor, they may be detectable with a future dedicated CMB polarization experiment.']",['1998-12-07'] +1337,['eng'],"['Moffat, J W']",['Varying Light Velocity as a Solution to the Problems in Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'photon, velocity', 'time dependence', 'invariance, Lorentz', 'field equations, solution', 'astrophysics, fundamental constant', 'entropy', 'critical phenomena', 'cosmic radiation, background', 'cosmic radiation, fluctuation', 'space-time, symmetry', 'symmetry, spontaneously broken', 'density, perturbation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811390'],"['In earlier published work, it was proposed that light speed was larger in the early Universe by 30 orders of magnitude compared to its presently observed value. This change in the speed of light is associated with a spontaneous breaking of local Lorentz invariance in the early Universe, associated with a first order phase transition at a critical time $t=t_c$. This solves the horizon problem, leads to a mechanism of monopole suppression in cosmology and can resolve the flatness problem. After the critical time $t_c$, local Lorentz (and diffeomorphism) invariance is restored and light travels at its presently measured speed. We investigate solutions of the field equations in the spontaneously broken phase and study further the flatness problem and the cosmological constant problem. The entropy is shown to undergo a large increase as the light velocity goes through a phase transition. A scale invariant prediction for microwave background fluctuations originating at the time of the phase transition is discussed.']",['1998-11-25'] +1338,['eng'],"['Baccigalupi, C', 'Perrotta, F']",['Perturbations in Quintessential Inflation'],['Astrophysics and Astronomy'],"['inflationary universe, quintessence', 'cosmic radiation, background', 'cosmic radiation, polarization', 'temperature, anisotropy', 'astrophysics, missing-mass', 'spectra, perturbation', 'energy, density', 'field theory, scalar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811385'],['Recently Peebles and Vilenkin proposed and quantitatively analyzed the fascinating idea that a substantial fraction of the present cosmic energy density could reside in the vacuum potential energy of the scalar field responsible for inflation (quintessential inflation). Here we compute the signature of this model in the cosmic microwave background polarization and temperature anisotropies and in the large scale structure.'],['1998-11-25'] +1339,['eng'],"['Turner, M S']",['Cosmology Solved? Maybe'],['Astrophysics and Astronomy'],"['talk, Gainesville 1998/03/13', 'inflationary universe', 'astrophysics, missing-mass', 'astrophysics, model', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, fluctuation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811366'],"['For two decades the hot big-bang model as been referred to as the standard cosmology -- and for good reason. For just as long cosmologists have known that there are fundamental questions that are not answered by the standard cosmology and point to a grander theory. The best candidate for that grander theory is inflation + cold dark matter. It holds that the Universe is flat, that slowly moving elementary particles left over from the earliest moments provide the cosmic infrastructure, and that the primeval density inhomogeneities that seed all the structure arose from quantum fluctuations. There is now prima facie evidence that supports two basic tenets of this paradigm. An avalanche of high-quality cosmological observations will soon make this case stronger or will break it. Key questions remain to be answered; foremost among them are: identification and detection of the cold dark matter particles and elucidation of the dark-energy component. These are exciting times in cosmology!']",['1998-11-24'] +1340,['eng'],"['Turner, M S']",['Cosmology Solved? Quite Possibly!'],['Astrophysics and Astronomy'],"['talk, Washington 1998/10/04', 'astrophysics, model', 'cosmic radiation, background', 'inflationary universe', 'astrophysics, missing-mass', 'light nucleus, production', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811364'],"[""The discovery of the cosmic microwave background (CMB) in 1964 by Penzias and Wilson led to the establishment of the hot big-bang cosmological model some ten years later. Discoveries made in 1998 may ultimately have as profound an effect on our understanding of the origin and evolution of the Universe. Taken at face value, they confirm the basic tenets of Inflation + Cold Dark Matter, a bold and expansive theory that addresses all the fundamental questions left unanswered by the hot big-bang model and holds that the Universe is flat, slowly moving elementary particles provide the cosmic infrastructure, and quantum fluctuations seeded all the structure seen in the Universe today. Just as it took a decade to establish the hot big-bang model after the discovery of the CMB, it will likely take another ten years to establish the latest addition to the standard cosmology and make the answer to ``Cosmology Solved?'', ``YES!'' Whether or not 1998 proves to be a cosmic milestone, the coming avalanche of high-quality cosmological data promises to make the next twenty years an extremely exciting period for cosmology.""]",['1998-11-24'] +1341,['eng'],"['Starobinsky, A A']",['Beyond the Simplest Inflationary Cosmological Models'],['Astrophysics and Astronomy'],"['talk, Moscow 1997/12/08', 'inflationary universe', 'density, perturbation', 'spectra, perturbation', 'effective potential', 'astrophysics, missing-mass', 'critical phenomena', 'cosmic radiation, background', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811360'],"['Though predictions of the simplest inflationary cosmological models with cold dark matter, flat space and approximately flat initial spectrum of adiabatic perturbations are remarkably close to observational data, we have to go beyond them and to introduce new physics not yet discovered in laboratories to account for all data. Two extensions of these models which seem to be the most actual at present time are discussed. The first one is the possibility that we are living at the beginning of a new inflation-like era. Then classical cosmological tests, like the luminosity distance or the angular size of distant objects as functions of redshift, as well as the behaviour of density perturbations in a dustlike matter component including baryons as a function of redshift, can provide information sufficient for the unambiguous determination of an effective potential of a corresponding present inflaton scalar field. The second, unrelated extension is a possibility of broken-scale-invariant cosmological models which have localized steps or spikes in the primordial perturbation spectrum. These features can be produced by fast phase transitions in physical fields other than an inflaton field in the early Universe during inflation and not far from the end of it. At present, it seems that the only scale in the spectrum around which we might see something of this type is $k=0.05 h Mpc^{-1}$.']",['1998-11-24'] +1342,['eng'],"['Ziaeepour, H']",['Can Dark Matter be Ultra Heavy Particles?'],['Astrophysics and Astronomy'],"['talk, Buxton 1998/09/07', 'cosmic radiation, background', 'astrophysics, missing-mass', 'decay, missing-mass', 'postulated particle, heavy', 'Boltzmann equation, solution', 'baryon, energy', 'photon, energy', 'energy, flux', 'jet, hadronization', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811312'],"['The detection of High Energy Cosmic Rays (HECR) with energies around and beyond GZK expected cutoff has introduced the idea of existence of a decaying Ultra Heavy Dark Matter (UHDM). If this type of particles make a substantial part of the CDM, their decay can have important implications for evolution of the large structures and high energy backgrounds. Here we present preliminary results of numerical solution of Boltzmann equations in presence of a decaying CDM. The evolution of baryons and photons energy are calculated. We find that in a homogeneous universe, UHDM can not have a large contribution to the CDM. However, this hypothesis can probably survive if one takes into account the clumsiness of the matter in the Universe.']",['1998-11-20'] +1343,['eng'],"['Bucher, M', 'Spergel, D N']",['Is the Dark Matter a Solid?'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'density, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'pressure', 'coupling, gravitation', 'potential', 'time, conformal', 'tensor, energy-momentum', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812022'],"['A smooth unclustered dark matter component with negative presure could reconcile a flat universe with the many observations that find a density in ordinary, clustered matter well below the critical density and also explain the recent high redshift supernova data suggesting that the expansion of the universe is now accelerating. For a perfect fluid negative presure leads to instabilities that are most severe on the shortest scales. However, if instead the dark matter is a solid, with an elastic resistance to pure shear deformations, an equation of state with negative presure can avoid these short wavelength instabilities. Such a solid may arise as the result of different kinds of microphysics. Two possible candidates for a solid dark matter component are a frustrated network of non-Abelian cosmic strings or a frustrated network of domain walls. If these networks settle down to an equilibrium configuration that gets carried along and stretched by the Hubble flow, equations of state result with $w=-1/3$ and $w=-2/3,$ respectively. One expects the sound speeds for the solid dark matter component to comprise an appreciable fraction of the speed of light. Therefore, the solid dark matter does not cluster, expect on the very largest scales, accessible only through observing the large-angle CMB anisotropy. In this paper we develop a generally-covariant, continuum description for the dynamics of a solid dark matter component. We derive the evolution equations for the cosmological perturbations in a flat universe with CDM+(solid) and compute the resulting large-angle CMB anisotropy. The formalism presented here applies to any generalized dark matter with negative pressure and a non-dissipative resistance to shear.']",['1998-12-02'] +1344,['eng'],"['Turner, M S']",['Dark Matter and Dark Energy in the Universe'],['Astrophysics and Astronomy'],"['talk, Canberra 1998/08/17', 'astrophysics, missing-mass', 'matter, density', 'energy, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'baryon', 'inflationary universe', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811454'],"['For the first time, we have a plausible, complete accounting of matter and energy in the Universe. Expressed a fraction of the critical density it goes like this: neutrinos, between 0.3% and 15%; stars, 0.5%; baryons (total), 5%; matter (total), 40%; smooth, dark energy, 60%; adding up to the critical density. This accounting is consistent with the inflationary prediction of a flat Universe and defines three dark-matter problems: Where are the dark baryons? What is the nonbaryonic dark matter? What is the nature of the dark energy? The leading candidate for the (optically) dark baryons is diffuse hot gas; the leading candidates for the nonbaryonic dark matter are slowly moving elementary particles left over from the earliest moments (cold dark matter), such as axions or neutralinos; the leading candidates for the dark energy involve fundamental physics and include a cosmological constant (vacuum energy), a rolling scalar field (quintessence), and light, frustrated topological defects.']",['1998-12-01'] +1345,['eng'],"['Medina-Tanco, G A', 'De Gouveia dal Pino, E M', 'Horváth, J E']",['Origin and Propagation of Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'magnetic field', 'p, cosmic radiation', 'iron', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901053'],"['The existence of cosmic ray particles up to the ultra-high energy limit (> 10^20 eV) is now beyond any doubt. The detection of cosmic particles with such energies imposes a challenge for the comprehension of their sources and nature. On one side, particles with such high energies are difficult to be produced by any astrophysical source. On the other side, the interactions of these particles with photons of the cosmic microwave background cause substantial losses of energy which constraint the maximum distances that the particles are able to travel from the sources to the detectors. Aiming to help to elucidate the problem of UHECR source identification, we have performed 3-D simulations of particle trajectories propagated through the stochastic intergalactic and an extended Galactic halo magnetic fields. Going further, we have also performed simulations of proton and Fe nuclei through the spiral Galactic magnetic field (GMF) and built full-sky maps of their arrival direction distribution in both the detector (after deflection in the GMF) and just outside the Galaxy. In this work we summarize the main results of these investigations.']",['1999-01-06'] +1346,['eng'],"['Henri, G', 'Pelletier, G', 'Petrucci, P O', 'Renaud, N']",['Active Galactic Nuclei as High Energy Engines'],['Astrophysics and Astronomy'],"['galaxy, AGN', 'photon, cosmic radiation', 'cosmic radiation, acceleration', 'cosmic radiation, particle source', 'p, cosmic radiation', 'electron, cosmic radiation', 'neutrino, flux']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901051'],"['Active Galactic Nuclei are considered as possible sites of cosmic ray acceleration and some of them have been observed as high energy gamma ray emitters (Blazars). There naturally comes an appealing idea that the acceleration of the highest energy cosmic rays in the AGNs has a signature in the form of gamma ray emission and high energy neutrino emission through the collisions of very high energy protons with soft photons. Moreover it is often said that electrons cannot reach enough energy through Fermi acceleration to account for the highest energy photons observed with ground Cerenkov telescopes. In this paper, we discussed these points and show that the fast variability of the flares recently observed rules out the assumption of a Fermi acceleration of protons. We show that Fermi acceleration of electrons is enough to account for the gamma spectra, their shape, cut-off and their variability. Moreover the spectral break is nicely explained by invoking an gamma-ray photosphere. Nevertheless we give estimates of the high energy cosmic ray generation in AGNs and of the resultant neutrino flux, that turns out to be very sensitive to the spectral index of the proton distribution.']",['1999-01-06'] +1347,['eng'],"['Barrow, John D', 'Magueijo, J']",['Solving the Flatness and Quasi-flatness Problems in Brans-Dicke Cosmologies with a Varying Light Speed'],['Astrophysics and Astronomy'],"['astrophysics, model', 'Brans-Dicke model', 'photon, velocity', 'field equations, solution', 'perturbation theory', 'nonperturbative', 'asymptotic behavior', 'astrophysics, fundamental constant', 'gravitation, fundamental constant', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901049'],"['We define the flatness and quasi-flatness problems in cosmological models. We seek solutions to both problems in homogeneous and isotropic Brans-Dicke cosmologies with varying speed of light. We formulate this theory and find perturbative, non-perturbative, and asymptotic solutions using both numerical and analytical methods. For a particular range of variations of the speed of light the flatness problem can be solved. Under other conditions there exists a late-time attractor with a constant value of Ømega that is smaller than, but of order, unity. Thus these theories may solve the quasi-flatness problem, a considerably more challenging problem than the flatness problem. We also discuss the related \\Lambda and quasi-\\Lambda problem in these theories. We conclude with an appraisal of the difficulties these theories may face.']",['1999-01-06'] +1348,['eng'],"['Baccigalupi, C']",['Throwing pebbles in the primordial pond'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, perturbation', 'symmetry breaking', 'polarization', 'temperature, fluctuation', 'decoupling', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901040'],"['We consider anisotropies in the Cosmic Microwave Background (CMB) generated by spatially limited seeds; these objects could correspond to relics of high energy symmetry breaking in the early universe. It is shown how the CMB perturbation propagate beyond the size of the seed in the form of waves traveling with the CMB sound velocity. Moreover, these waves are the substantial part of the signal, both for polarization and temperature. The explanation of this phenomenology in terms of the CMB equations is given. Observationally, this effect is threefold promising. First, it enlarges the signal from a seed intersecting the last scattering surface to the scale of the CMB sound horizon at decoupling, that is roughly one degree in the sky. Second, it offers cross correlation possibilities between the polarization and temperature signals. Third, it allows to unambiguously distinguish these structures from point-like astrophysical sources.']",['1999-01-06'] +1349,['eng'],"['Kim, H I', 'Lee, C H', 'MacGibbon, J H']",['Diffuse $\\gamma$-ray background and primordial black hole constraints on the spectral index of density fluctuations'],['Astrophysics and Astronomy'],"['astrophysics, model', 'black hole, radiation', 'photon, cosmic radiation', 'photon, flux', 'photon, diffusion', 'density, fluctuation', 'spectra, fluctuation', 'black hole, mass spectrum', 'effect, fragmentation', 'quantum chromodynamics', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901030'],"[""We calculate the flux of $\\gamma$-rays emitted from primordial black holes (PBHs) which are formed by a ``blue'' power-law spectrum of density fluctuations in the early universe. Gamma-ray emission from such PBHs may contribute significantly to the observed extragalactic diffuse $\\gamma$-ray background (DGB). Using the observed DGB flux from the imaging Compton Telescope (COMPTEL) and the Energetic Gamma Ray Experiment Telescope (EGRET) as the upper limit of $\\gamma$-ray flux from PBHs, we derive the upper limit on the spectral index $n$ of the density fluctuations. The range of initial PBH masses which can contribute to the DGB is $2\\times 10^{13}\\g - 5\\times 10^{14}\\g$, corresponding to a cosmic reheating temperature of $7\\times 10^{7}\\gev - 4\\times 10^{8} \\gev$. In this range, we find the upper limit to be $n \\lsim 1.23-1.25$. This limit is stronger than those derived from the energy density in PBHs or PBH relics and matches the value of $n$ required to explain the cosmic microwave background anisotropy.""]",['1999-01-06'] +1350,['eng'],"['Rachen, J P', 'Mészáros, P']",['Cosmic Rays and Neutrinos from $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['talk, Huntsville 1997/09/15', 'photon, cosmic radiation', 'p, cosmic radiation', 'p, acceleration', 'p, ejection', 'photon hadron, interaction', 'n, production', 'neutrino, production', 'neutrino, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811266'],"['We review the hypothesis that the acceleration of protons at internal shocks in Gamma Ray Bursts (GRB) could be the origin of the ultra-high energy cosmic rays (UHECR) observed at earth, E_max > 10^19 eV. We find that, even though protons may be accelerated to such energies, their ejection into the interstellar/intergalactic medium is problematic because it is likely to be accompanied by considerable adiabatic losses in the expanding shell. The problem is circumvented by neutrons produced in photohadronic interactions, which are not magnetically bound and thus effectively ejected in the moment of their production. They can be both produced in sufficient number and be able to leave the emission region if the optical depth of the emission region to photohadronic interactions is of order 1. We show that this requirement can be fulfilled under the same conditions which allow acceleration of protons to the highest energies. The production of neutrinos in this process correlates the fluxes of cosmic rays and neutrinos, and makes the hypothesis of UHECR origin in GRBs testable.']",['1998-11-19'] +1351,['eng'],"['Caldwell, D O']",['Neutrino Mass and Dark Matter'],['Astrophysics and Astronomy'],"['talk, Buxton 1998/09/07', 'neutrino, mass', 'astrophysics, missing-mass', 'neutrino, solar', 'neutrino, flux', 'neutrino, beam', 'neutrino, mass difference', 'neutrino, mixing angle', 'neutrino, flavor', 'galaxy', 'light nucleus, production', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812026'],"['Despite direct observations favoring a low mass density, a critical density universe with a neutrino component of dark matter provides the best existing model to explain the observed structure of the universe over more than three orders of magnitude in distance scale. In principle this hot dark matter could consist of one, two, or three species of active neutrinos. If all present indications for neutrino mass are correct, however, only the two-species (muon neutrino and tau neutrino) possibility works. This requires the existence of at least one light sterile neutrino to explain the solar electron neutrino deficit via nu(e)->nu(s), leaving nu(mu)->nu(tau) as the explanation for the anomalous nu(mu)/nu(e) ratio produced by atmospheric neutrinos, and having the LSND experiment demonstrating via anti-nu(mu)-> anti-nu(e) the mass difference between the light nu(e)-nu(s) pair and the heavier nu(mu)-nu(tau) pair required for dark matter. Other experiments do not conflict with the LSND results when all the experiments are analyzed in the same way, and when analyzed conservatively the LSND data is quite compatible with the mass difference needed for dark matter. Further support for this mass pattern is provided by the need for a sterile neutrino to rescue heavy-element nucleosynthesis in supernovae, and it could even aid the concordance in light element abundances from the early universe.']",['1998-12-02'] +1352,['eng'],"['Ghosh, T K', 'Chakrabarti, S']",['Chemical Evolution of Strongly Magnetized Quark Core in a Newborn Neutron Star'],['Astrophysics and Astronomy'],"['n, matter', 'quark, matter', 'magnetic field, high', 'quark, strangeness', 'quark, production', 'critical phenomena, confinement', 'neutrino, confinement', 'potential, chemical', 'nuclear matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811243'],['The chemical evolution of nascent quark matter core in a newborn compact neutron star is studied in presence of a strong magnetic field. The effective rate of strange quark production in degenerate quark matter core in presence of strong magnetic fields is obtained. The investigations show that in presence of strong magnetic fields a quark matter core becomes energetically unstable and hence a deconfinement transition to quark matter at the centre of a compact neutron star under such circumstances is not possible. The critical strength of magnetic field at the central core to make the system energetically unstable with respect to dense nuclear matter is found to be $\\sim 4.4\\times 10^{13}$G. This is the typical strength at which the Landau levels for electrons are populated. The other possible phase transitions at such high density and ultra strong magnetic field environment are discussed.'],['1998-11-19'] +1353,['eng'],"['Chikashige, Y', 'Kamoshita, J I']",['On Spectrum of Extremely High Energy Cosmic Rays through Decay of Superheavy Particles'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'postulated particle, decay', 'postulated particle, mass', 'postulated particle, lifetime', 'Boltzmann equation', 'neutrino, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812483'],"['We propose a formula for flux of extremely high energy cosmic rays (EHECR) through decay of superheavy particles. It is shown that EHECR spectrum reported by AGASA is reproduced by the formula. The presence of EHECR suggests, according to this approach, the existence of superheavy particles with mass of about $7 \\times 10^{11}$GeV and the lifetime of about $10^9$ years. Possibility to obtain a knowledge of $\\Omega_0$ of the universe from the spectrum of EHECR is also pointed out.']",['1999-01-01'] +1354,['eng'],"['Anchordoqui, L A']",['From 3K to $10^{20} eV$'],['Astrophysics and Astronomy'],"['thesis', 'cosmic radiation, energy spectrum', 'cosmic radiation, primary', 'energy loss', 'dependence, mass number', 'nucleus, cosmic radiation', 'differential equations, solution', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'showers, air', 'hadron, interaction', 'muon, spatial distribution', 'photon, spatial distribution', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812445'],['The problem of predicting the upper cut-off of the cosmic ray spectrum is re-examined. Some aspects of extremely high energy interactions and their implications for the interpretation of giant air showers are also discussed.'],['1998-12-25'] +1355,['eng'],"['De Vega, H J', 'Ramírez, J', 'Sánchez, N']",['Generation of gravitational waves by generic sources in de Sitter space-time'],['Astrophysics and Astronomy'],"['gravitational radiation, production', 'space-time, de Sitter', 'space-time, Minkowski', 'gravitation, perturbation', 'graviton, propagator', 'coupling, minimal', 'field theory, scalar', 'invariance, gauge', 'spectral representation', 'tensor, energy-momentum']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812465'],"[""We study the generation of gravitational radiation by sources moving in the de Sitter background. Exploiting the maximal symmetry and the conformal flatness of de Sitter space-time we prove that the derivation of this gravitational radiation can be done along the same lines as in Minkowski space-time. A gauge is chosen in which all the physical and unphysical modes of the graviton are those of a minimally coupled massless scalar field in de Sitter space-time and a massless field in Minkowski space-time. The graviton retarded Green's function and the Schwinger commutator function are computed in this gauge using Quantum Field Theory techniques. We obtain closed formulae for the spectral decomposition in frequencies of the linaearized gravitational field produced by the source, in terms of a suitable spectral decomposition of the source energy-momentum tensor. This spectral decomposition is dictated by the free (sourceless) gravitational wave modes in the de Sitter background""]",['1998-12-30'] +1356,['eng'],"['Semelin, B', 'De Vega, H J', 'Sánchez, N', 'Combes, F']",['Renormalization Group Flow and Fragmentation in the Self-Gravitating Thermal Gas'],['Astrophysics and Astronomy'],"['gas, nonrelativistic', 'finite temperature', 'gravitation, potential', 'perturbation theory, higher-order', 'correlation function', 'renormalization group', 'coupling constant', 'gas, density', 'gas, fragmentation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812467'],"[""The self-gravitating thermal gas (non-relativistic particles of mass m at temperature T) is exactly equivalent to a field theory with a single scalar field phi(x) and exponential self-interaction. We build up perturbation theory around a space dependent stationary point phi_0(r) in a finite size domain delta \\leq r \\leq R ,(delta << R), which is relevant for astrophysical applica- tions (interstellar medium,galaxy distributions).We compute the correlations of the gravitational potential (phi) and of the density and find that they scale; the latter scales as 1/r^2. A rich structure emerges in the two-point correl- tors from the phi fluctuations around phi_0(r). The n-point correlators are explicitly computed to the one-loop level.The relevant effective coupling turns out to be lambda=4 pi G m^2 / (T R). The renormalization group equations (RGE) for the n-point correlator are derived and the RG flow for the effective coupling lambda(tau) [tau = ln(R/delta), explicitly obtained.A novel dependence on tau emerges here.lambda(tau) vanishes each time tau approaches discrete values tau=tau_n = 2 pi n/sqrt7-0, n=0,1,2, ...Such RG infrared stable behavior [lambda(tau) decreasing with increasing tau] is here connected with low density self-similar fractal structures fitting one into another.For scales smaller than the points tau_n, ultraviolet unstable behaviour appears which we connect to Jeans' unstable behaviour, growing density and fragmentation. Remarkably, we get a hierarchy of scales and Jeans lengths following the geometric progression R_n=R_0 e^{2 pi n /sqrt7} = R_0 [10.749087...]^n . A hierarchy of this type is expected for non-spherical geometries,with a rate different from e^{2 n/sqrt7}.""]",['1998-12-30'] +1357,['eng'],"['Roberts, M D', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Hayami, Y', 'Holder, J', 'Kakimoto, F', 'Kamei, S', 'Kawachi, A', 'Kifune, T', 'Kita, R', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Matsuoka, T', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Nishijima, K', 'Oda, S', 'Ogio, S', 'Patterson, J R', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Suzuki, A', 'Suzuki, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['TeV $\\gamma$-ray observations of southern BL Lacs with the CANGAROO 3.8 m Imaging Telescope'],['Astrophysics and Astronomy'],"['astrophysics', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'cosmic radiation, flux', 'upper limit', 'numerical calculations, Monte Carlo', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811260'],"['Observational and theoretical results indicate that low-redshift BL Lacertae objects are the most likely extragalactic sources to be detectable at TeV energies. In this paper we present the results of observations of 4 BL Lacertae objects (PKS0521-365, EXO0423.4-0840, PKS2005-489 and PKS2316-423) made between 1993 and 1996 with the CANGAROO 3.8m imaging Cherenkov telescope. During the period of these observations the gamma-ray energy threshold of the 3.8m telescope was ~2TeV. Searches for steady long-term emission have been made, and, inspired by the TeV flares detected from Mkn421 and Mkn501, a search on a night-by-night timescale has also been performed for each source. Comprehensive Monte Carlo simulations are used to estimate upper limits for both steady and short timescale emission.']",['1998-11-19'] +1358,['eng'],"['Protheroe, R J']",['Acceleration and Interaction of Ultra High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'cosmic radiation, acceleration', 'cosmic radiation, interaction', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'topology, defect', 'model, shock waves', 'cosmic radiation, background', 'showers, electromagnetic', 'path length', 'magnetic field', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812055'],"['In this chapter I give an overview of shock acceleration, including a discussion of the maximum energies possible and the shape of the spectrum near cut-off, interactions of high energy cosmic rays with, and propagation through, the background radiation, and the resulting electron-photon cascade. Possible sources of the highest energy cosmic rays are discussed including active galaxies, gamma ray bursts and topological defects. I argue that while the origin of the highest energy cosmic rays is still uncertain, it is not necessary to invoke exotic models such as emission by topological defects to explain the existing data. It seems likely that shock acceleration at Fanaroff-Riley Class II radio galaxies can account for the existing data. However, new cosmic ray data, as well as better estimates of the extragalactic radiation fields and magnetic fields will be necessary before we will be certain of the origin of the highest energy particles occurring in nature.']",['1998-12-03'] +1359,['eng'],"['Huber, H', 'Weigel, M K', 'Weber, F']",['Compatibility of neutron star masses and hyperon coupling constants'],['Astrophysics and Astronomy'],"['n, matter', 'mass, lower limit', 'hyperon, coupling constant', 'nuclear matter', 'binding energy', 'Hartree approximation, relativistic', 'Hartree-Fock approximation, relativistic', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811463'],"['It is shown that the modern equations of state for neutron star matter based on microscopic calculations of symmetric and asymmetric nuclear matter are compatible with the lower bound on the maximum neutron-star mass for a certain range of hyperon coupling constants, which are constrained by the binding energies of hyperons in symmetric nuclear matter. The hyperons are included by means of the relativistic Hartree-- or Hartree--Fock approximation. The obtained couplings are also in satisfactory agreement with hypernuclei data in the relativistic Hartree scheme. Within the relativistic Hartree--Fock approximation hypernuclei have not been investigated so far.']",['1998-12-01'] +1360,['eng'],"['Turner, M S']",['Cosmology Solved?'],['Astrophysics and Astronomy'],"['talk, Kyoto 1998/04/07', 'astrophysics, model', 'astrophysics, missing-mass', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811447'],"['For two decades the hot big-bang model as been referred to as the standard cosmology -- and for good reason. For just as long cosmologists have known that there are fundamental questions that are not answered by the standard cosmology and point to a grander theory. The best candidate for that grander theory is inflation + cold dark matter; it can extend our understanding of the Universe back to 10^-32 sec. There is now prima facie evidence for the two basic tenets of this new paradigm: flat Universe and scale-invariant spectrum of Gaussian density perturbations, and an avalanche of telling cosmological observations is coming. If inflation + cold dark matter is correct, then there are new, fundamental questions to be answered, most notably the nature of the dark energy that seems to account for 60% of the critical density and how inflation fits into a unified theory of the forces and particles. These are exciting times in cosmology!']",['1998-11-30'] +1361,['eng'],"['Abramo, L R W', 'Woodard, R P']",['One Loop Back Reaction On Power Law Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'background, classical', 'quantum mechanics, correction', 'effect, graviton', 'potential, inflaton', 'Feynman graph, higher-order', 'back reaction', 'propagator', 'infrared problem', 'quantization, canonical']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811431'],"['We consider quantum mechanical corrections to a homogeneous, isotropic and spatially flat geometry whose scale factor expands classically as a general power of the co-moving time. The effects of both gravitons and the scalar inflaton are computed at one loop using the manifestly causal formalism of Schwinger with the Feynman rules recently developed by Iliopoulos {\\it et al.} We find no significant effect, in marked contrast with the result obtained by Mukhanov {\\it et al.} for chaotic inflation based on a quadratic potential. By applying the canonical technique of Mukhanov {\\it et al.} to the exponential potentials of power law inflation, we show that the two methods produce the same results, within the approximations employed, for these backgrounds. We therefore conclude that the shape of the inflaton potential can have an enormous impact on the one loop back-reaction.']",['1998-11-30'] +1362,['eng'],"['Abramo, L R W', 'Woodard, R P']",['One Loop Back Reaction On Chaotic Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'background, perturbation theory', 'Feynman graph, higher-order', 'potential, scalar', 'back reaction', 'graviton', 'inflaton', 'propagator', 'infrared problem', 'n-point function, 1']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811430'],"['We extend, for the case of a general scalar potential, the inflaton-graviton Feynman rules recently developed by Iliopoulos {\\it et al.} As an application we compute the leading term, for late co-moving times, of the one loop back reaction on the expansion rate for $V(\\phi) = \\frac12 m^2 \\phi^2$. This is expressed as the logarithmic time derivative of the scale factor in the coordinate system for which the expectation value of the metric has the form: $<0 | g_{\\mu\\nu}({\\bar t},{\\vec x}) | 0 > dx^{\\mu} dx^{\\nu} = - d{\\bar t}^2 + a^2({\\bar t}) d{\\vec x} \\cdot d{\\vec x}$. This quantity should be a gauge independent observable. Our result for it agrees exactly with that inferred from the effect previously computed by Mukhanov {\\it et al.} using canonical quantization. It is significant that the two calculations were made with completely different schemes for fixing the gauge, and that our computation was done using the standard formalism of covariant quantization. This should settle some of the issues recently raised by Unruh.']",['1998-11-30'] +1363,['eng'],"['Dar, Arnon']","['Comment on ""Cosmological $\\gamma$ Ray Bursts and the Highest Energy Cosmic Rays""']",['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'cosmic radiation, primary']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811196'],"['In a letter with the above title, published some time ago in PRL, Waxman made the interesting suggestion that cosmological gamma ray bursts (GRBs) are the source of the ultra high energy cosmic rays (UHECR). This has also been proposed independently by Milgrom and Usov and by Vietri. However, recent observations of GRBs and their afterglows and in particular recent data from the Akeno Great Air Shwoer Array (AGASA) on UHECR rule out extragalactic GRBs as the source of UHECR.']",['1998-11-13'] +1364,['eng'],"['Engel, R']",['Implications of HERA results for very high energy cosmic ray physics'],['Astrophysics and Astronomy'],"['talk, Assergi 1998/07/12', 'electron p, deep inelastic scattering', 'p, structure function', 'momentum spectrum, parton', 'small-x', 'gluon, momentum spectrum', 'scaling, violation', 'electron p, inclusive reaction', 'photon p, inclusive reaction', 'jet, electroproduction', 'hadron, multiple production', 'multiplicity, spectra', 'transverse momentum, spectra', 'p p, inclusive reaction', 'charged particle, multiple production', 'quantum chromodynamics, perturbation theory', 'unitarity', 'cosmic radiation, energy spectrum', 'numerical calculations', 'interpretation of experiments, DESY HERA Stor']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811225'],"['Experimental results obtained with the HERA collider and recent progress in their theoretical interpretation are reviewed. After a short introduction to HERA physics, deep inelastic scattering and photoproduction are discussed as (virtual) photon-proton scattering. It is shown that the measurement and theoretical understanding of both photoproduction as well as low-x deep inelastic scattering are essential for obtaining reliable high energy extrapolations within hadron-hadron interaction models. Limitations of the predictive power of hadron interaction models due to the interplay of perturbative QCD and unitarity effects are discussed.']",['1998-11-16'] +1365,['eng'],"['Garriga, J', 'Montes, X', 'Sasaki, M', 'Tanaka, T']",['Spectrum of Cosmological Perturbations in the One-Bubble Open Universe'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'bubble, production', 'density, perturbation', 'spectra, perturbation', 'space-time, fluctuation', 'energy, density', 'field theory, action', 'perturbation, scalar', 'perturbation, tensor', 'WKB approximation', 'quantum mechanics, supersymmetry']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811257'],"['The spectrum of cosmological perturbations in the context of the one-bubble open inflation model is discussed, taking into account fluctuations of the metric. We find that, quite generically,thin wall single field models have no supercurvature modes. However, single field models with supercurvature modes do exist. In these models the density parameter $\\Omega$ becomes a random variable taking a range of values inside of each bubble. We also show that the model dependence of the continuous spectrum for both scalar and tensor-type perturbations is small as long as the kinetic energy density of the background field does not dominate the total energy density. We conclude that the spectrum of the density perturbation predicted in the single-field model of the one-bubble open inflation is rather robust. We also consider the spectrum of scalar and tensor perturbations in a model of the Hawking-Turok type, without a false vacuum.']",['1998-11-19'] +1366,['eng'],"['Berezinsky, Veniamin Sergeevich']",['Ultra high energy cosmic rays from cosmological relics'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1998/07/12', 'astrophysics, model', 'photon, cosmic radiation', 'topology, defect', 'postulated particle, heavy', 'postulated particle, decay', 'p, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811268'],"['Ultra High Energy Cosmic Rays (UHECR) can be a signal from very early (post-inflationary) Universe. At this cosmological epoch Topological Defects (TD) and long-lived suprheavy (SH) particles are expected to be naturally and effectively produced. Both of these relics can produce now the particles, such as protons and photons, with energies in a great excess of what is observed in UHECR, $E \\sim 10^{10} - 10^{11} GeV$. The Topological Defects as the UHECR sources are critically reviewed and cosmic necklaces and monopolonia are identified as most plausible sources. The relic superheavy particles and monopolonia are shown to be clustering in the halo of our Galaxy and their decays produce UHECR without the GZK cutoff. The observational signature of both models are discussed.']",['1998-11-19'] +1367,['eng'],"['Chechin, L M', 'Omarov, T B']",['Gravitational Field and Equations of Motion of Nonlinear Cosmic String'],['Astrophysics and Astronomy'],"['gravitation', 'astrophysics, string', 'nonlinear', 'dimension, 2', 'tensor, energy-momentum', 'particle, orbit', 'field equations, solution']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811254'],"['For the case of tension tensor containing nonlinear terms in $l^{\\alpha}$, we give generalization of Vilenkin metrics and equations of motion of cosmic string. Dynamics of nonlinear string in (1+1)-dimensional universe is discussed.']",['1998-11-19'] +1368,['eng'],"['Reddy, S', 'Prakash, M', 'Lattimer, J M', 'Pons, J A']",['Effects of Strong and Electromagnetic Correlations on Neutrino Interactions in Dense Matter'],['Astrophysics and Astronomy'],"['neutrino n, interaction', 'nuclear matter', 'n, matter', 'neutral current', 'charged current', 'n, path length', 'strong interaction, correlation', 'electromagnetic interaction, correlation', 'model, nonrelativistic', 'model, relativistic', 'astrophysics, supernova', 'thermodynamics', 'nuclear reaction, model', 'differential cross section', 'temperature, dependence', 'dependence, density', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811294'],"['An extensive study of the effects of correlations on both charged and neutral current weak interaction rates in dense matter is performed. Both strong and electromagnetic correlations are considered.The propagation of particle-hole interactions in the medium plays an important role in determining the neutrino mean free paths. The effects due to Pauli-Blocking and density, spin, and isospin correlations in the medium significantly reduce the neutrino cross sections. Due to the lack of experimental information at high density, these correlations are necessarily model dependent. For example, spin correlations in nonrelativistic models are found to lead to larger suppressions of neutrino cross sections compared to those of relativistic models. This is due to the tendency of the nonrelativistic models to develop spin instabilities. Notwithstanding the above caveats, and the differences between nonrelativistic and relativistic approaches such as the spin- and isospin-dependent interactions and the nucleon effective masses, suppressions of order 2--3, relative to the case in which correlations are ignored, are obtained. Neutrino interactions in dense matter are especially important for supernova and early neutron star evolution calculations. The effects of correlations for protoneutron star evolution are calculated. Large effects on the internal thermodynamic properties of protoneutron stars, such as the temperature, are found. These translate into significant early enhancements in the emitted neutrino energies and fluxes, especially after a few seconds. At late times, beyond about 10 seconds, the emitted neutrino fluxes decrease more rapidly compared to simulations without the effects of correlations, due to the more rapid onset of neutrino transparency in the protoneutron star']",['1998-11-19'] +1369,['eng'],"['Malik, K A', 'Wands, D']",['Dynamics of Assisted Inflation'],['Astrophysics and Astronomy'],"['inflationary universe, hybrid', 'field theory, scalar', 'potential', 'mean field approximation', 'scaling', 'model, attractor', 'vacuum state, energy', 'spectra, perturbation', 'vacuum state, fluctuation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812204'],"['We investigate the dynamics of the recently proposed model of assisted inflation. In this model an arbitrary number of scalar fields with exponential potentials evolve towards an inflationary scaling solution, even if each of the individual potentials is too steep to support inflation on its own. By choosing an appropriate rotation in field space we can write down explicitly the potential for the weighted mean field along the scaling solution and for fields orthogonal to it. This demonstrates that the potential has a global minimum along the scaling solution. We show that the potential close to this attractor in the rotated field space is analogous to a hybrid inflation model, but with the vacuum energy having an exponential dependence upon a dilaton field. We present analytic solutions describing homogeneous and inhomogeneous perturbations about the attractor solution without resorting to slow-roll approximations. We discuss the curvature and isocurvature perturbation spectra produced from vacuum fluctuations during assisted inflation.']",['1998-12-11'] +1370,['eng'],"['Ellis, Jonathan Richard']",['Particle Candidates for Dark Matter'],['Astrophysics and Astronomy'],"['review, Haga Slott 1998/08/20', 'astrophysics, missing-mass', 'neutrino, massive', 'neutrino, solar', 'LSP', 'neutralino', 'postulated particle, heavy', 'string model', 'M-theory', 'vacuum state, energy', 'quantum gravity', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812211'],"['Some particle candidates for dark matter are reviewed in the light of recent experimental and theoretical developments. Models for massive neutrinos are discussed in the light of the recent atmospheric-neutrino data, and used to motivate comments on the plausibility of different solutions to the solar neutrino problem. Arguments are given that the lightest supersymmetric particle should be a neutralino \\chi, and accelerator and astrophysical constraints used to suggest that 50 GeV \\lappeq m_\\chi \\lappeq 600 GeV. Minimizing the fine tuning of the gauge hierarchy favours Ømega_\\chi h^2 \\sim 0.1. The possibility of superheavy relic particles is mentioned, and candidates from string and $M$ theory are reviewed. Finally, the possibility of non-zero vacuum energy is discussed: its calculation is a great opportunity for a quantum theory of gravity, and the possibility that it is time dependent should not be forgotten.']",['1998-12-11'] +1371,['eng'],"['Zibin, J P', 'Scott, D', 'White, M']",['Limits on the gravity wave contribution to microwave anisotropies'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'perturbation, tensor', 'perturbation, scalar', 'correlation, galaxy', 'galaxy, cluster', 'inflationary universe', 'gravitational radiation', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901028'],"['We present limits on the fraction of large angle microwave anisotropies which could come from tensor perturbations. We use the COBE results as well as smaller scale CMB observations, measurements of galaxy correlations, abundances of galaxy clusters, and Lyman alpha absorption cloud statistics. Our aim is to provide accurate limits on the tensor-to-scalar ratio for standard inflationary models. For power-law inflation, for example, we find T/S<0.51 at 95% confidence, with a similar constraint for phi^p potentials. However, for models with tensor amplitude unrelated to the scalar spectral index it is still currently possible to have T/S>1.']",['1999-01-05'] +1372,['eng'],"['Lichtensteiger, L', 'Durrer, R']",['Are there static texture?'],['Astrophysics and Astronomy'],"['field theory, scalar', 'field equations, solution', 'space-time', 'topology', 'symmetry, rotational', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901024'],"['We consider harmonic maps from Minkowski space into the three sphere. We are especially interested in solutions which are asymptotically constant, i.e. converge to the same value in all directions of spatial infinity. Physical 3-space can then be compactified and can be identified topologically (but not metrically!) with a three sphere. Therefore, at fixed time, the winding of the map is defined. We investigate whether static solutions with non-trivial winding number exist. The answer which we can proof here is only partial: We show that within a certain family of maps no static solutions with non-zero winding number exist. We discuss the existing static solutions in our family of maps. An extension to other maps or a proof that our family of maps is sufficiently general remains an open problem.']",['1999-01-05'] +1373,['eng'],"['Malyshkin, L M', 'Kulsrud, R M']",['MSW time variations of the solar neutrino flux'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'time variation', 'neutrino, oscillation', 'neutrino, mass', 'Dirac equation, solution', 'WKB approximation', 'neutrino, mass difference', 'neutrino, mixing angle', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901015'],"['We consider the possibility of MSW time variations of the solar neutrino flux due to the radial motion of the Earth and neutrino interference effects. We have calculated the time variations of the detected neutrino flux including collisional decoherence and all other significant physical decoherence effects. Exact results for the detected neutrino flux and its time variations are presented for both the case of a solar neutrino line, and the case of a continuous neutrino spectrum with a Gaussian shape of the energy response function of the neutrino detector. We obtain constraints on the neutrino masses and the vacuum mixing angle required for significant flux time variations to be observed. Pac(s): 14.60.Pq, 26.65.+t, 96.60.Jw']",['1999-01-05'] +1374,['eng'],"['Dar, Arnon']",['Are extragalactic $\\gamma$ ray bursts the source of the highest energy cosmic rays?'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'showers, air', 'astrophysics, supernova', 'astrophysics, galaxy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901005'],"['Recent observations with the large air shower arrays of ultra high energy cosmic rays (UHECR) and recent measurements/estimates of the redshifts of gamma ray bursts (GRBs) seem to rule out extragalactic GRBs as the source of the cosmic rays that are observed near Earth, including those with the highest energies.']",['1999-01-05'] +1375,['eng'],"['Dar, Arnon', 'De Rújula, Alvaro', 'Antoniou, N G']",['A common origin of all the species of high energy cosmic rays?'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'nucleus, cosmic radiation', 'electron, cosmic radiation', 'photon, cosmic radiation', 'astrophysics, galaxy', 'cosmic radiation, acceleration', 'Compton scattering', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901004'],"['The cosmic ray nuclei with energy above a few GeV, the cosmic ray electrons of energy above a few MeV and the diffuse gamma-ray background above a few MeV, could all predominantly originate from our galaxy {\\it and its halo}. The mechanism accelerating hadrons and electrons is the same, the electron spectrum is modulated by inverse Compton scattering on the microwave background radiation, and the $\\gamma$-rays are the resulting recoiling photons. The spectra calculated on this basis agree with observations.']",['1999-01-05'] +1376,['eng'],"['Shi Xiang Dong', 'Fuller, G M']","['A Reply to ""Comment on Big Bang Nucleosynthesis and Active-Sterile Neutrino Mixing']",['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'neutrino, oscillation', 'neutrino, mixing angle', 'neutrino, mass difference', 'neutrino/mu', 'neutrino/tau', 'neutrino, sterile', 'tau, flavor', 'flavor, asymmetry', 'temperature, dependence', 'numerical calculations', 'interpretation of experiments, KAMIOKANDE']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812232'],"['In the paper ""Big Bang Nucleosynthesis and Active-Sterile Neutrino Mixing: Evidence for Maximal Muon-Neutrino/Sterile-Neutrino Mixing in Super Kamiokande"" (astro-ph/9810075), we suggested that to evade the Big Bang Nucleosynthesis exclusion of the muon neutrino to sterile neutrino oscillation explanation of the Super Kamiokande data, the tau neutrino must have a mass over about 15 eV and it must mix with a lighter sterile neutrino. A stable tau neutrino with this mass is inconsistent with cosmological structure formation. In a comment on our paper (astro-ph/9811067), Foot and Volkas argued that our result is incorrect and that the required tau neutrino mass should be much lower. Here we back up our original result with a more detailed calculation. We show that the argument of Foot and Volkas is invalid, most likely due to an insufficient energy resolution in the low energy part of the neutrino spectrum.']",['1998-12-14'] +1377,['eng'],"['Kwiecinski, J', 'Martin, A D', 'Stasto, A M']",['Penetration of the Earth by ultrahigh energy neutrinos predicted by low $\\chi$ QCD'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, energy spectrum', 'neutrino nucleus, nuclear reaction', 'neutrino nucleon, interaction', 'small-x', 'quantum chromodynamics', 'cross section', 'transport theory', 'geophysics', 'neutrino, flux', 'matter, effect', 'effect, shadowing', 'antineutrino nucleon, interaction', 'charged current', 'neutral current', 'astrophysics, particle source', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812262'],"['We calculate the cross sections for neutrino interactions with (isoscalar) nuclear targets in the energy domain all the way up to 10^12 GeV. Small x QCD effects are included by using a unified BFKL/DGLAP formalism which embodies non-leading log(1/x) contributions. The few free parameters which specify the input parton distributions are determined by fitting to HERA deep inelastic data. The attenuation of neutrinos transversing the Earth at different nadir angles is calculated for a variety of energy spectra for neutrinos originating from different sources (from Active Galactic Nuclei, Gamma ray bursts, top-down models), as well as for atmospheric neutrinos. For this purpose we solve the transport equation which includes regeneration due to neutral current neutrino interactions, besides attenuation.']",['1998-12-15'] +1378,['eng'],"['Stecker, F W']",['Intergalactic Extinction of High Energy $\\gamma$-Rays'],['Astrophysics and Astronomy'],"['talk, Cambridge 1998/10/23', 'photon, cosmic radiation', 'photon, absorption', 'energy spectrum', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812286'],"['We discuss the determination of the intergalactic pair-production absorption coefficient (Stecker & De Jager 1998) making use of an empirically based calculation of the IR background spectrum (Malkan & Stecker 1998) which agrees well with recent data and constraints on the IR background. While the Whipple observations of Mrk421 hint at extragalactic absorption, the new HEGRA observations of Mrk501 appear to strongly indicate such absorption. We discuss the determination of absorption at higher redshifts (Salamon & Stecker 1998). We also give a predicted spectrum, with absorption included, for PKS2155-304, which, at a redshift of 0.12, is the highest redshift TeV source yet observed.']",['1998-12-16'] +1379,['eng'],"['Abazajian, K N', 'Fuller, G M']",['Baryon/antibaryon inhomogeneity and big bang nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1998/02/18', 'astrophysics, model', 'baryon antibaryon, ratio', 'light nucleus, production', 'n, diffusion', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812288'],"['We investigate the effects of baryon/anti-baryon inhomogeneity on primordial nucleosynthesis. Recent work claims that electroweak baryogenesis could give rise to distinct regions of net baryon and anti-baryon number, which could survive until the nucleosynthesis epoch. We discuss neutron diffusion effects on nucleosynthesis yields in these models and speculate on the prospects for obtaining constraints.']",['1998-12-16'] +1380,['eng'],"['Wang, Y', 'Spergel, D N', 'Strauss, M A']",['Model-Independent Measurement of the Primordial Power Spectrum'],['Astrophysics and Astronomy'],"['talk, Monterey 1998/11/15', 'inflationary universe', 'density, fluctuation', 'spectra, fluctuation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812291'],"['In inflationary models with minimal amount of gravity waves, the primordial power spectrum of density fluctuations, $A_S^2(k)$, together with the basic cosmological parameters, completely specify the predictions for the cosmic microwave background (CMB) anisotropy and large scale structure. Here we show how we can strongly constrain both $A_S^2(k)$ and the cosmological parameters by combining the data from the Microwave Anisotropy Probe (MAP) and the galaxy redshift survey from the Sloan Digital Sky Survey (SDSS). We allow $A_S^2(k)$ to be a free function, and thus probe features in the primordial power spectrum on all scales. MAP and SDSS have scale-dependent measurement errors that decrease in opposite directions on astrophysically interesting scales; they complement each other and allow the measurement of the primordial power spectrum independent of inflationary models, giving us valuable information on physics in the early Universe, and providing clues to the correct inflationary model.']",['1998-12-16'] +1381,['eng'],"['Kim, J E']",['Axion Theory Review'],['Astrophysics and Astronomy'],"['review, Buxton 1998/09/07', 'axion, mass', 'axion, coupling', 'coupling, Yukawa', 'string model', 'supersymmetry', 'astrophysics, missing-mass', 'strong interaction, CP']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812257'],['I review the axion physics with emphases on the couplings of the very light axion and a possible realization in superstring models.'],['1998-12-15'] +1382,['eng'],"['Geer, S H', 'Kennedy, Dallas C']",['A New Limit on the Antiproton Lifetime'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'anti-p, cosmic radiation', 'anti-p p, ratio', 'anti-p, lifetime', 'lower limit', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9812025'],"['Measurements of the cosmic ray pbar/p ratio are compared to predictions from an inhomogeneous leaky disk model of pbar production and propagation within the Galaxy, combined with a calculation of the modulation of the interstellar cosmic ray spectra as the particles propagate through the heliosphere to the Earth. The predictions agree with the observed pbar/p spectrum. Adding a finite pbar lifetime to the model, we obtain the limit tau(pbar) > 0.8 Myr (90% C.L.).']",['1998-12-02'] +1383,['eng'],"['Arbab, A I']",['Primordial Black Holes With Gravitational Memory'],['Astrophysics and Astronomy'],"['black hole, radiation', 'gravitation, fundamental constant', 'viscosity', 'baryon, asymmetry', 'gravitation, strong interaction']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811422'],"[""We have studied the evolution of primordial black holes (PBHs) in a universe with variable gravitational constant and bulk viscosity. We have found that the gravitational constant attained its maximum value at a time $10^{-23}$ sec and its value at Planck's time is equal to its value today.. The proton formed at the time $10^{-23}$ sec would become a black hole that would have been evaporated by now and that may account for the observed baryon-to-photon ratio.""]",['1998-11-27'] +1384,['eng'],"['De Paolis, F', 'Ingrosso, G', 'Jetzer, Philippe', 'Roncadelli, Marco']",['$\\gamma$ ray astronomy and baryonic dark matter'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'astrophysics, galaxy', 'astrophysics, missing-mass', 'baryon, matter', 'p, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901033'],"['Recently, Dixon et al. have re-analyzed the EGRET data, finding a statistically significant diffuse $\\gamma$-ray emission from the galactic halo. We show that this emission can naturally be explained within a previously-proposed model for baryonic dark matter, in which $\\gamma$-rays are produced through the interaction of high-energy cosmic-ray protons with cold $H_2$ clouds clumped into dark clusters - these dark clusters supposedly populate the outer galactic halo and can show up in microlensing observations. Our estimate for the halo $\\gamma$-ray flux turns out to be in remarkably good agreement with the discovery by Dixon et al. We also address future prospects to test our predictions.']",['1999-01-06'] +1385,['eng'],"['Beacom, J F', 'Vogel, P']",['Can a supernova be located by its neutrinos?'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino electron, forward scattering', 'neutrino nucleus, nuclear reaction', 'angular dependence', 'triangulation', 'deep underground detector', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811350'],"['A future type-II supernova in our Galaxy will be detected by several neutrino detectors around the world. The neutrinos escape from the supernova core over several seconds from the time of collapse, unlike the electromagnetic radiation, emitted from the envelope, which is delayed by a time of order hours. In addition, the electromagnetic radiation can be obscured by dust in the intervening interstellar space. The question therefore arises whether a supernova can be located by its neutrinos alone. The early warning of a supernova and its location might allow greatly improved astronomical observations. The theme of the present work is a careful and realistic assessment of this question, taking into account the statistical significance of the various neutrino signals. Not surprisingly, neutrino-electron forward scattering leads to a good determination of the supernova direction, even in the presence of the large and nearly isotropic background from other reactions. Even with the most pessimstic background assumptions, SuperKamiokande (SK) and the Sudbury Neutrino Observatory (SNO) can restrict the supernova direction to be within circles of radius $5^\\circ$ and $20^\\circ$, respectively. Other reactions with more events but weaker angular dependence are much less useful for locating the supernova. Finally, there is the oft-discussed possibility of triangulation, i.e., determination of the supernova direction based on an arrival time delay between different detectors. Given the expected statistics we show that, contrary to previous estimates, this technique does not allow a good determination of the supernova direction.']",['1998-11-24'] +1386,['eng'],"['Amelino-Camelia, G', 'Ellis, Jonathan Richard', 'Mavromatos, Nikolaos E', 'Nanopoulos, Dimitri V', 'Sarkar, S']",['Sensitivity of Astrophysical Observations to Gravity-Induced Wave Dispersion in Vacuo'],['Astrophysics and Astronomy'],"['quantum gravity', 'photon, velocity', 'energy dependence', 'dispersion relations', 'photon, cosmic radiation', 'birefringence', 'galaxy', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810483'],"['We discuss possible signatures of quantum gravity for the propagation of light, including an energy-dependent velocity (refractive index), dispersion in velocity at a given energy, and birefringence. We also compare the sensitivities of different astrophysical observations, including BATSE data on GRB 920229, BeppoSAX data on GRB 980425, the possible HEGRA observation of GRB 920925c, and Whipple observations of the active galaxy Mrk 421. Finally, we discuss the prospective sensitivities of AMS and GLAST.']",['1998-10-30'] +1387,['eng'],"['Peebles, P J E', 'Vilenkin, A']",['Quintessential inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'entropy', 'radiation', 'matter', 'particle, production', 'potential, inflaton', 'gravitational radiation', 'astrophysics, fundamental constant', 'quintessence']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810509'],"['We present an explicit observationally acceptable model for evolution from inflation to the present epoch under the assumption that the entropy and matter of the familiar universe are from gravitational particle production at the end of inflation. This eliminates the problem of finding a satisfactory coupling of the inflaton and matter fields. Since the inflaton potential $V(\\phi)$ may be a monotonic function of the inflaton $\\phi$, the inflaton energy could produce an observationally significant effective cosmological constant, as in quintessence.']",['1998-11-02'] +1388,['eng'],"['Contaldi, C R', 'Hindmarsh, M B', 'Magueijo, J']",['CMB and LSS Power Spectra From Local Cosmic String Seeded Struture Formation'],['Astrophysics and Astronomy'],"['talk, Santander 1998/06/22', 'astrophysics, string', 'cosmic radiation, background', 'cosmic radiation, spectra', 'two-point function', 'tensor, energy-momentum', 'astrophysics, missing-mass', 'topology, defect', 'correlation function', 'energy, decay', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810411'],['We evaluate the two point functions of the stress energy from the largest string simulations carried out so far. The two point functions are used to calculate the cosmic microwave background (CMB) and cold dark matter (CDM) power spectra from local cosmic string models for structure formation. We find that our spectra differ significantly from those previously calculated for both global and local defects. We find a higher Doppler peak at $l=400-600$ and a less severe bias problem than for global defects. Spectra were obtained for a variety of network energy-decay mechanisms.'],['1998-10-27'] +1389,['eng'],"['De van Bruck, C']",['Cosmic Strings and Structure Formation'],['Astrophysics and Astronomy'],"['talk, Buxton 1998/09/07', 'astrophysics, string', 'astrophysics, missing-mass', 'velocity, galaxy', 'galaxy, cluster', 'string, network', 'matter, density', 'mass, fluctuation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810409'],"['We discuss structure formation in cosmic string theories. Emphasis is laid on the properties of the peculiar velocity field, non-gaussian features and clusters of galaxies. It is found that the predicted peculiar velocity field is quiet ($v<150$ km/s for $L>30 h^{-1}$ Mpc) for models with ($\\Omega_0 h \\leq 0.2$) which is in disagreement with the results from POTENT at large scales ($>30h^{-1}$ Mpc), consistent, however, with the analysis of the peculiar velocity field of spiral galaxies by Giovannelli et al.. Using the Press-Schechter formalism we calculate the abundances of X-ray clusters. It is found that in CDM models a mass fluctuation $\\sigma_8 = 0.6...0.7$ is needed with $\\Omega_0 h =0.1...0.2$ in order to explain the current data.']",['1998-10-27'] +1390,['eng'],"['Pina-Avelino, P', 'Shellard, E P S', 'Allen, B']",['Cosmic string loops and large-scale structure'],['Astrophysics and Astronomy'],"['astrophysics, string', 'density, perturbation', 'spectra, perturbation', 'correlation', 'matter, density', 'radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810439'],['We investigate the contribution made by small loops from a cosmic string network as seeds for large-scale structure formation. We show that cosmic string loops are highly correlated with the long-string network on large scales and therefore contribute significantly to the power spectrum of density perturbations if the average loop lifetime is comparable to or above one Hubble time. This effect further improves the large-scale bias problem previously identified in earlier studies of cosmic string models.'],['1998-10-28'] +1391,['eng'],"['Bhattacharjee, P', 'Sigl, G']",['Origin and Propagation of Extremely High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['review', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'astrophysics, model', 'topology, defect', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'galaxy', 'supersymmetry', 'hadron, cosmic radiation', 'astrophysics, string', 'baryon, asymmetry', 'postulated particle, massive', 'grand unified theory', 'quantum chromodynamics', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811011'],"['Cosmic ray particles with energies in excess of 10**20 eV have been detected. The sources as well as the physical mechanism(s) responsible for endowing cosmic ray particles with such enormous energies are unknown. This report gives a review of the physics and astrophysics associated with the questions of origin and propagation of these EHE cosmic rays in the Universe. After a brief review of the observed cosmic rays in general and their possible sources and acceleration mechanisms, a detailed discussion is given of possible ""top-down"" (non-acceleration) scenarios of origin of EHE cosmic rays through decay of sufficiently massive particles originating from processes in the early Universe. The massive particles can come from collapse and/or annihilation of cosmic topological defects (such as monopoles, cosmic strings, etc.) associated with grand unified theories or they could be some long-lived metastable supermassive relic particles that were created in the early Universe and are decaying in the current epoch. The highest energy end of the cosmic ray spectrum can thus be used as a probe of new fundamental physics beyond Standard Model. We discuss the role of existing and proposed cosmic ray, gamma-ray and neutrino experiments in this context. We also discuss how observations with next generation experiments of images and spectra of EHE cosmic ray sources can be used to obtain new information on Galactic and extragalactic magnetic fields and possibly their origin.']",['1998-11-03'] +1392,['eng'],"['Foot, R', 'Volkas, R R']","['Comment on ""Big Bang Nucleosynthesis and Active-Sterile Neutrino Mixing']",['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'neutrino, interference', 'neutrino/mu', 'neutrino/tau', 'neutrino, sterile', 'neutrino, oscillation', 'neutrino, cosmic radiation', 'neutrino, air', 'numerical calculations', 'interpretation of experiments, KAMIOKANDE']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811067'],"['The paper ""Big Bang Nucleosynthesis and Active-Sterile Neutrino Mixing: Evidence for Maximal $\\nu_\\mu \\leftrightarrow \\nu_\\tau$ Mixing in Super Kamiokande?"" by X. Shi and G. M. Fuller (astro-ph/9810075) discusses the cosmological implications of the $\\nu_\\mu \\to \\nu_s$ solution to the atmospheric neutrino anomaly. It incorrectly concludes that a lower bound on the $\\nu_\\tau$ mass of 15 eV is needed in order for the $\\nu_\\mu \\to \\nu_s$ oscillations to be consistent with a Big Bang Nucleosynthesis upper bound on the effective number of flavours of 3.3. Since such a large $\\nu_\\tau$ mass is disfavoured from large scale structure formation considerations, the strong, but incorrect, conclusion is made that cosmology favours the $\\nu_\\mu \\to of the error. We conclude that cosmology is, at present, consistent with both the $\\nu_\\mu \\to \\nu_s$ and $\\nu_\\mu \\to \\nu_\\tau$ possibilities.']",['1998-11-05'] +1393,['eng'],"['Plaga, R']",['Cosmic very high-energy $\\gamma$ rays'],['Astrophysics and Astronomy'],"['talk, Frascati 1998/06/17', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'astrophysics, model', 'bremsstrahlung', 'synchrotron radiation', 'Compton scattering', 'supernova', 'cosmic radiation, acceleration', 'neutrino, massive', 'supersymmetry', 'LSP', 'astrophysics, missing-mass', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811081'],"['The article gives a brief overview, aimed at nonspecialists, about the goals and selected recent results of the detection of very-high energy gamma-rays (energies above 100 GeV) with ground based detectors. The stress is on the physics questions, especially the origin of Galactic Cosmic Rays and the emission of TeV gamma-radiation from active galaxies. Moreover some particle-physics questions which are addressed in this area are discussed.']",['1998-11-05'] +1394,['eng'],"['Nunokawa, H', 'Tomás, R', 'Valle, José W F']",['Type-II Supernovae and Neutrino Magnetic Moment'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, magnetic moment', 'magnetic moment, transition', 'neutrino/e', 'neutrino, sterile', 'antineutrino', 'light nucleus, production', 'magnetic field', 'Schroedinger equation', 'neutrino, mass difference', 'spin, flavor', 'neutrino, oscillation', 'matter, effect', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811181'],"['The present solar and atmospheric neutrino data together with the LSND results and the presence of hot dark matter (HDM) suggest the existence of a sterile neutrino at the eV scale. We have reanalysed the effect of resonant type-II supernova. We analyse the implications of $\\nu_e-\\nu_s$ and the supernova shock re-heating, the detected $\\bar\\nu_e$ signal from SN1987A and the $r$-process nucleosynthesis hypothesis. Using reasonable magnetic field profiles we determine the sensitivity of these three arguments to the relevant neutrino parameters, i.e. the value of the transition magnetic moment and the']",['1998-11-12'] +1395,['eng'],"['Guzmán, F', 'Matos, T', 'Villegas-Brena, H']",['Dilatonic dark matter in spiral galaxies'],['Astrophysics and Astronomy'],"['gravitation, dilaton', 'gravitation, missing-mass', 'galaxy', 'Einstein equation, solution', 'symmetry, axial', 'field theory, scalar', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811143'],"['An exact, axially symmetric solution to the Einstein-dilaton field equations is employed to model the dark matter in spiral galaxies. The extended rotation curves from a previous analysis are used to fit the model, and a very good agreement is found. A comparison is made with the corresponding fits from three parameter dark-halo and one parameter modified newtonian dynamics (MOND) models. It is argued that, although our model posseses three parameters to be fitted, it is better than the non-relativistic alternatives in the sense that it is not of a phenomenological nature, since the dark matter would consist entirely of the scalar field.']",['1998-11-10'] +1396,['eng'],"['Perrotta, F', 'Baccigalupi, C']",['Early time perturbations behaviour in scalar field cosmologies'],['Astrophysics and Astronomy'],"['astrophysics, model', 'field theory, scalar', 'time, perturbation', 'Einstein equation, solution', 'model, fluid', 'approximation, adiabatic', 'entropy', 'gauge, conformal', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'space-time, horizon', 'boundary condition', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811156'],"['We consider the problem of the initial conditions and behaviour of the perturbations in scalar field cosmology with general potential. We use the general definition of adiabatic and isocurvature conditions to set the appropriate initial values for the perturbation in the scalar field and in the ordinary matter and radiation components. In both the cases of initial adiabaticity and isocurvature, we solve the Einstein and fluid equation at early times and on superhorizon scales to find the initial behaviour of the relevant quantities. In particular, in the isocurvature case, we consider models in which the initial perturbation arises from the matter as well as from the scalar field itself, provided that the initial value of the gauge invariant curvature is zero. We extend the standard code to include all these cases, and we show some results concerning the power spectrum of the cosmic microwave background temperature anisotropies. In particular, it turns out that the acoustic peaks follow opposite behaviours in the adiabatic and isocurvature regimes: in the first case their amplitude is higher than in the corresponding pure cold dark matter model, while they make the opposite thing for pure isocurvature initial perturbations.']",['1998-11-11'] +1397,['eng'],"['Sciama, D W']",['Are Neutrino Oscillations Compatible with the Decaying Neutrino Theory for the Ionisation of Hydrogen in the Interstellar Medium?'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, oscillation', 'neutrino, decay', 'hydrogen, ionization', 'neutrino/mu', 'neutrino, sterile', 'astrophysics, fundamental constant', 'neutrino, solar', 'neutrino, flux', 'neutrino/tau', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811172'],"['Recent Super-Kamiokande data have greatly strengthened the hypothesis that the atmospheric neutrino anomaly is mainly due to nearly maximal oscillations between $\\nu_{\\mu}$ and either $\\nu_{\\tau}$ or a sterile neutrino the ionisation of hydrogen in the interstellar medium, in conjunction with the assumption that the cosmological constant $\\lambda$ is zero, requires these oscillations to be between $\\nu_{\\mu}$ and $\\nu^s_{\\mu}$. This requirement can be tested by forthcoming Super-Kamiokande measurements. A further requirement can be derived if the solar neutrino deficit is energy dependent and if both it and the LSND data are also due to neutrino oscillations. In that case the decaying neutrino theory alone (without any assumption about the value of are between $\\nu_e$ and a second sterile neutrino $\\nu^s_e$. This latter requirement can be tested by forthcoming SNO and BOREXINO measurements. If these are also $\\nu_{\\tau}-\\nu^s_{\\tau}$ oscillations the decay line would be split into two lines of nearly equal intensity and spacing less than $\\sim$ 0.2 eV.']",['1998-11-12'] +1398,['eng'],"['Vankov, A']",['On an Alternative Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'matter, expansion', 'relativistic', 'quasar', 'cosmic radiation, background', 'cosmic radiation, spectra']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811165'],"['The suggested alternative cosmology is based on the idea of barion symmetric universe, in which our home universe is a representative of multitude of typical matter and antimatter universes. This alternative concept gives a physically reasonable explanation of all major problems of the Standard Cosmological Model. Classification Code MSC: Cosmology 524.8 Key words: standard cosmological model, alternative cosmology, barionic symmetry, typical universe, quasars, cosmic rays.']",['1998-11-11'] +1399,['eng'],"['Kosowsky, A']",['Seeing Sound Waves in the Early Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'cosmic radiation, background', 'spectra, temperature', 'spectra, polarization', 'coherence, oscillation', 'acoustic', 'density, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811163'],"['Temperature and polarization power spectra of the cosmic microwave background can provide essentially incontrovertible evidence for coherent acoustic oscillations in the early universe. A simple model calculation demonstrates explicitly how polarization couples to velocities at the surface of last scatter and is nearly independent of gravitational or density perturbations. For coherent acoustic oscillations, peaks in the temperature and polarization power spectra are precisely interleaved. If observed, such a signal would provide strong support for initial density perturbations on scales larger than the horizon, and thus for inflation.']",['1998-11-11'] +1400,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'McQueen, S', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E']",['Correlation between the X-ray and TeV Gamma Ray Emission from an Accreting X-ray Binary'],['Astrophysics and Astronomy'],"['astrophysics', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'time variation', 'correlation', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811094'],['Measurements of the signal strength of TeV gamma rays from the accreting X-ray binary Cen X-3 show evidence for correlation with both the RXTE/ASM and the BATSE X-ray signal strengths. There are indications that the time scale for the variability of the gamma rays may be similar to that of X-rays and as short as a day. These features of the X-ray and TeV emission from an accreting binary show many similarities with the recently discovered high energy behaviour of X-ray selected BL Lacs.'],['1998-11-06'] +1401,['eng'],"['Khlopov, M Ya', 'Konoplich, R V', 'Mignani, R P', 'Rubin, S G', 'Sakharov, A S']","['Physical Origin, Evolution and Observational Signature of Diffused Antiworld']",['Astrophysics and Astronomy'],"['baryon, asymmetry', 'matter, diffusion', 'antimatter, diffusion', 'photon, cosmic radiation', 'cosmic radiation, flux']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810228'],"['The existence of macroscopic regions with antibaryon excess in the baryon asymmetric Universe with general baryon excess is the possible consequence of practically all models of baryosynthesis. Diffusion of matter and antimatter to the border of antimatter domains defines the minimal scale of the antimatter domains surviving to the present time. A model of diffused antiworld is considered, in which the density within the surviving antimatter domains is too low to form gravitationally bound objects. The possibility to test this model by measurements of cosmic gamma ray fluxes is discussed. The expected gamma ray flux is found to be acceptable for modern cosmic gamma ray detectors and for those planned for the near future.']",['1998-10-16'] +1402,['eng'],"['Vázquez, R A']",['Diffuse Extragalactic $\\gamma$ Rays and $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'n, matter', 'critical phenomena', 'baryon number, violation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810231'],"[""If gamma ray bursts produce a total energy of 10^54 ergs and this energy is concentrated on the high energy tail of the spectrum E> 1 TeV, then they may account for the observed diffuse extragalactic gamma ray emission for energies > 100 MeV. Such an energy could be released if the GRB's are produced by the burning of the total mass of a neutron star in a phase transition which violates baryon number.""]",['1998-10-16'] +1403,['eng'],"['Arbab, A I']",['Cosmological implications of the bulk viscous model with variable G and $\\Lambda$'],['Astrophysics and Astronomy'],"['astrophysics, model', 'gravitation, fundamental constant', 'astrophysics, fundamental constant', 'effect, viscosity', 'inflationary universe', 'field equations', 'time', 'luminosity', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810239'],['We have investigated the cosmological implications of the bulk viscous cosmological model with variable G and $\\Lambda$. These results are found to be compatible with the present observations. The classical cosmological tests for this model encompass the Freese et al ones. The model has some sprits of the Standard Model. The inflationary solution which solves the Standard Model problems is obtained as a special solution. The influence of viscosity is shown to affect the past and the future of the Universe.'],['1998-10-16'] +1404,['eng'],"['Medina-Tanco, G A']",['The energy spectrum observed by the AGASA experiment and the spatial distribution of the sources of ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'spatial distribution', 'showers, air', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810366'],"['Seven and a half years of continuous monitoring of giant air showers triggered by ultra high-energy cosmic rays have been recently summarized by the AGASA collaboration. The resulting energy spectrum indicates clearly that the cosmic ray spectrum extends well beyond the Greisen-Zatsepin-Kuzmin (GZK) cut-off at $\\sim 5 \\times 10^{19}$ eV. Furthermore, despite the small number statistics involved, some structure in the spectrum may be emerging. Using numerical simulations, it is demonstrated in the present work that these features are consistent with a spatial distribution of sources that follows the distribution of luminous matter in the local Universe. Therefore, from this point of view, there is no need for a second high-energy component of cosmic rays dominating the spectrum beyond the GZK cut-off.']",['1998-10-23'] +1405,['eng'],"['Balberg, S', 'Lichtenstadt, J', 'Cook, G B']",['Roles of Hyperons in Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'hyperon, effect', 'coupling, superfluid', 'density, high', 'nuclear matter', 'meson, condensation', 'critical phenomena', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810361'],"['We examine the roles the presence of hyperons in the cores of neutron stars may play in determining global properties of these stars. The study is based on estimates that hyperons appear in neutron star matter at about twice the nuclear saturation density, and emphasis is placed on effects that can be attributed to the general multi-species composition of the matter, hence being only weakly dependent on the specific modeling of strong interactions. Our analysis indicates that hyperon formation not only softens the equation of state but also severely constrains its values at high densities. Correspondingly, the valid range for the maximum neutron star mass is limited to about 1.5-1.8 $M_\\odot$, which is a much narrower range than available when hyperon formation is ignored. Effects concerning neutron star radii and rotational evolution are suggested, and we demonstrate that the effect of hyperons on the equation of state allows a reconciliation of observed pulsar glitches with a low neutron star maximum mass. We discuss the effects hyperons may have on neutron star cooling rates, including recent results which indicate that hyperons may also couple to a superfluid state in high density matter. We compare nuclear matter to matter with hyperons and show that once hyperons accumulate in neutron star matter they reduce the likelihood of a meson condensate, but increase the susceptibility to baryon deconfinement, which could result in a mixed baryon-quark matter phase.']",['1998-10-23'] +1406,['eng'],"['Halzen, Francis']",['Lectures on Neutrino Astronomy'],['Astrophysics and Astronomy'],"['lectures, Boulder 1998/05/31', 'neutrino, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, acceleration', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'black hole', 'counters and detectors, water', 'astrophysics, missing-mass', 'cosmic radiation, flux', 'deep underground detector', 'Cherenkov counter', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810368'],['1. Overview of neutrino astronomy: multidisciplinary science. 2. Cosmic accelerators: the highest energy cosmic rays. 3. Neutrino beam dumps: supermassive black holes and gamma ray bursts. 4. Neutrino telescopes: water and ice. 5. Indirect dark matter detection. 6. Towards kilometer-scale detectors.'],['1998-10-23'] +1407,['eng'],"['Eichler, D', 'Seidov, Z F']",['Planck Scale Mixing and Neutrino Puzzles'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, solar', 'neutrino/e, flux', 'neutrino/mu, flux', 'flux, ratio', 'neutrino, massless', 'neutrino, interference', 'neutrino, flavor', 'symmetry breaking, Lorentz', 'grand unified theory', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810372'],"['It is hypotesized that neutrinos are massles and mixed among three (muon, electron and tau) flavors with a mixing length proportional to (E_nu/E_Planck)^-2. It is suggested that this hypothesis mostly reconciles the standard solar models with the observations of the solar Boron and pp neutrinos, and the atmospheric muon-to-electron neutrinos ratio.']",['1998-10-23'] +1408,['eng'],"['Richstone, D O']",['Supermassive Black Holes Then and Now'],['Astrophysics and Astronomy'],"['talk, Pasadena 1998/07/06', 'black hole, massive', 'galaxy', 'statistics', 'luminosity', 'quasar', 'interference, laser', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810379'],"['Recent surveys suggest that most or all normal galaxies host a massive black hole with 1/100 to 1/1000 of the visible mass of the spheroid of the galaxy. Various lines of argument suggest that these galaxies have merged at least once in our past lightcone, and that the black holes have also merged. This leads to a merger rate of massive black holes of about 1/\\yrs.']",['1998-10-26'] +1409,['eng'],"['Richstone, D O', 'Ajhar, E A', 'Bender, R', 'Bower, G', 'Dressler, A', 'Faber, S M', 'Filippenko, A V', 'Gebhardt, K', 'Green, R', 'Ho, L C', 'Kormendy, J', 'Lauer, T R', 'Magorrian, J', 'Tremaine, S']",['Supermassive Black Holes and the Evolution of Galaxies'],['Astrophysics and Astronomy'],"['black hole, massive', 'galaxy', 'quasar', 'luminosity', 'gravitational radiation', 'interference, laser', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810378'],"['Black holes, an extreme consequence of the mathematics of General Relativity, have long been suspected of being the prime movers of quasars, which emit more energy than any other objects in the Universe. Recent evidence indicates that supermassive black holes, which are probably quasar remnants, reside at the centers of most galaxies. As our knowledge of the demographics of these relics of a violent earlier Universe improve, we see tantalizing clues that they participated intimately in the formation of galaxies and have strongly influenced their present-day structure.']",['1998-10-26'] +1410,['eng'],"['Kusenko, A', 'Segrè, G']",['Pulsar kicks from neutrino oscillations'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'neutrino, oscillation', 'n, matter', 'neutrino, emission']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9811144'],"['Neutrino oscillations can explain the observed motion of pulsars. We show that two different models of neutrino emission from a cooling neutron star are in good quantitative agreement and predict the same order of magnitude for the pulsar kick velocity, consistent with the data.']",['1998-11-10'] +1411,['eng'],"['Fargion, D', 'Khlopov, M Ya', 'Konoplich, R V', 'Mignani, R P']",['Signature of relic heavy stable neutrinos in underground experiments'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, stability', 'neutrino, density', 'neutrino, heavy', 'neutrino, condensation', 'family, 4', 'WIMP', 'neutral current', 'elastic scattering, nucleus WIMP', 'cross section', 'neutrino, mass', 'astrophysics, missing-mass', 'deep underground detector', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810048'],['Considering heavy stable neutrinos of 4th generation we calculate the relic density of such neutrinos in the Universe. Taking into account the condensation of heavy neutrinos in the Galaxy and applying the results of calculations to experimental data from underground experiments on search for WIMPs in elastic neutral current scattering on nuclei we found an exclusion region of neutrino mass 60 GeV < m < 290 GeV. The bounds obtained from present underground experiments while confirming the previous bounds derived from analysis of cosmic ray spectra are more relible ones. We discuss also the first indication of elastic scattering induced by WIMP in DAMA experiment finding a very narrow window of neutrino mass 45 GeV < m < 50 GeV compatible with the possible signal rate in the detector.'],['1998-10-07'] +1412,['eng'],"['Janka, H T', 'Ruffert, M', 'Eberl, T']",['Merging Neutron Stars and Black Holes as Sources of $\\gamma$-Ray Bursts and Heavy Elements'],['Astrophysics and Astronomy'],"['talk, Volos 1998/07/06', 'n, matter', 'black hole', 'gravitational radiation, emission', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'model, hydrodynamical', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810057'],"['Hydrodynamic simulations were performed of the dynamical phase of the merging of binary neutron stars (NS-NS) and of neutron star black hole binaries (NS-BH), using the physical nuclear equation of state of Lattimer and Swesty (1991) and taking into account the emission of gravitational waves and neutrinos.']",['1998-10-07'] +1413,['eng'],"['Shi, X', 'Fuller, G M']",['Big Bang Nucleosynthesis and Active-Sterile Neutrino Mixing'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'neutrino, interference', 'neutrino/mu', 'neutrino/tau', 'neutrino, sterile', 'neutrino, oscillation', 'neutrino, flavor', 'lepton, asymmetry', 'helium, nuclide', 'deuterium', 'numerical calculations', 'interpretation of experiments, KAMIOKANDE']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810075'],"['We discuss Big Bang Nucleosynthesis constraints on maximal oscillation has been proposed as one possible explanation of the Super Kamiokande atmospheric neutrino data. Based on the most recent primordial abundance measurements, we find that the effective number of neutrino species for Big Bang Nucleosynthesis (BBN) is $N_\\nu\\la 3.3$. Assuming that all three active neutrinos are light (with masses $\\ll 1$ MeV), we examine BBN constraints on $\\nu_\\mu\\leftrightarrow\\nu_s$ mixing in two scenarios: (1) a negligible lepton asymmetry (the standard picture); (2) the presence of a large lepton asymmetry which has resulted from an amplification by or another sterile neutrino species). The latter scenario has been proposed recently to reconcile the BBN constraints and large-angle $N_\\nu\\approx 4$, is ruled out as an explanation of the Super Kamiokande data. It is conceivably possible for the $\\nu_\\mu\\leftrightarrow\\nu_s$ solution to evade BBN bounds in the second scenario, but only if 300 eV$^2\\la m^2_{\\nu_\\tau}-m^2_{\\nu_{s^\\prime}}\\la 10^4$ eV$^2$ is satisfied, and if mass-squared difference implies 15 eV$\\la m_{\\nu_\\tau}\\la 100$ eV if']",['1998-10-07'] +1414,['eng'],"['Fiorentini, G', 'Berezinsky, Veniamin Sergeevich', ""Degl'Innocenti, S"", 'Ricci, B']",['Bounds on hep neutrinos'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, oscillation', 'neutrino, flux', 'luminosity, solar', 'neutrino, production', 'upper limit', 'model, solar', 'helium, density', 'numerical calculations, KAMIOKANDE']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810083'],"['The excess of highest energy solar-neutrino events recently observed by Superkamiokande can be in principle explained by anomalously high $hep$-neutrino flux $\\Phi_{\\nu}(hep)$. Without using SSM calculations, from the solar luminosity constraint we derive that $\\Phi_\\nu(hep)/S_{13}$ cannot exceed the SSM estimate by more than a factor three. If one makes the additional hypothesis that $hep$ neutrino production occurs where the $^3$He concentration is at equilibrium, helioseismology gives an upper bound which is (less then) two times the SSM prediction. We argue that the anomalous $hep$-neutrino flux of order of that observed by Superkamiokande cannot be explained by astrophysics, but rather by a large production cross-section.']",['1998-10-07'] +1415,['eng'],"['Bond, J R', 'Kofman, L A', 'Pogosian, D Y', 'Wadsley, J']",['Theoretical Tools for Large Scale Structure'],['Astrophysics and Astronomy'],"['review, Paris 1998/05/26', 'astrophysics, model', 'inflaton', 'spectra, fluctuation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'perturbation theory, nonlinear', 'gas', 'galaxy, cluster', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810093'],"['We review the main theoretical aspects of the structure formation paradigm which impinge upon wide angle surveys: the early universe generation of gravitational metric fluctuations from quantum noise in scalar inflaton fields; the well understood and computed linear regime of CMB anisotropy and large scale structure (LSS) generation; the weakly nonlinear regime, where higher order perturbation theory works well, and where the cosmic web picture operates, describing an interconnected LSS of clusters bridged by filaments, with membranes as the intrafilament webbing. Current CMB+LSS data favour the simplest inflation-based $\\Lambda$CDM models, with a primordial spectral index within about 5% of scale invariant and $\\Omega_\\Lambda \\approx 2/3$, similar to that inferred from SNIa observations, and with open CDM models strongly disfavoured. The attack on the nonlinear regime with a variety of N-body and gas codes is described, as are the excursion set and peak-patch semianalytic approaches to object collapse. The ingredients are mixed together in an illustrative gasdynamical simulation of dense supercluster formation.']",['1998-10-07'] +1416,['eng'],"['Hannestad, S']",['Possible Constraints on the Time Variation of the Fine Structure Constant from Cosmic Microwave Background Data'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'fundamental constant, fine structure', 'fundamental constant, time variation', 'spectra, fluctuation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810102'],"['The formation of the cosmic microwave background radiation (CMBR) provides a very powerful probe of the early universe at the epoch of recombination. Specifically, it is possible to constrain the variation of fundamental physical constants in the early universe. We have calculated the effect of a varying electromagnetic coupling constant (\\alpha) on the CMBR and find that new satellite experiments should provide a tight constraint on the value of \\alpha at recombination which is complementary to existing constraints. An estimate of the obtainable precision is |(d\\alpha/dt)/\\alpha| < 7 x 10^-14 y^-1 in a realistic experiment.']",['1998-10-08'] +1417,['eng'],"['Bilic, N', 'Viollier, R D']",['Thermodynamic instability of self-gravitating heavy neutrino matter'],['Astrophysics and Astronomy'],"['talk, Heidelberg 1998/07/20', 'neutrino, matter', 'neutrino, heavy', 'stability, thermodynamical', 'critical phenomena', 'gravitation', 'astrophysics, missing-mass', 'neutrino, mass', 'energy, density', 'entropy', 'Thomas-Fermi model', 'finite temperature', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810108'],"['It is shown, in the framework of the Thomas-Fermi model at finite temperature, that a cooling non-degenerate gas of massive neutrinos will, at a certain temperature, become unstable and undergo a first-order phase transition in which quasi-degenerate supermassive neutrino stars are formed through gravitational collapse. For neutrinos in the mass range of 10 to 25 keV/c$^{2}$, these compact dark objects could mimic the role of supermassive black holes that are reported to exist at the centres of galaxies and quasi-stellar objects.']",['1998-10-08'] +1418,['eng'],"['Chadwick, P M', 'Lyons, K', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Shaw, S E', 'Turver, K E', 'Wieczorek, G J']",['VHE Gamma Rays from PKS 2155-304'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'energy spectrum', 'cosmic radiation, flux', 'correlation', 'galaxy', 'data analysis method', 'cosmic radiation, time variation', 'Cherenkov counter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810209'],"['The close X-ray selected BL Lac PKS 2155-304 has been observed using the University of Durham Mark 6 very high energy (VHE) gamma ray telescope during 1996 September/October/November and 1997 October/November. VHE gamma rays with energy > 300 GeV were detected from this object with a time-averaged integral flux of (4.2 +/- 0.7 (stat) +/- 2.0 (sys)) x 10^(-11) per cm2 per s. There is evidence for VHE gamma ray emission during our observations in 1996 September and 1997 October/November, with the strongest emission being detected in 1997 November, when the object was producing the largest flux ever recorded in high-energy X-rays and was detected in > 100 MeV gamma-rays. The VHE and X-ray fluxes show evidence of a correlation.']",['1998-10-15'] +1419,['eng'],"['Barger, V', 'Learned, J G', 'Pakvasa, S', 'Weiler, Thomas J']",['Neutrino Decay as an Explanation of Atmospheric Neutrino Observations'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, angular dependence', 'neutrino, decay modes', 'flavor, 3', 'neutrino, mixing angle', 'light nucleus, production', 'neutrino, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810121'],"['We show that the observed zenith angle dependence of the atmospheric neutrinos can be accounted for by neutrino decay. Furthermore, it is possible to account for all neutrino anomalies with just three flavors.']",['1998-10-09'] +1420,['eng'],"['Brodin, G', 'Marklund, M']",['Parametric excitation of plasma waves by gravitational radiation'],['Astrophysics and Astronomy'],"['plasma, excited state', 'radiation, electromagnetic', 'gravitational radiation', 'space-time, Minkowski', 'coupling constant', 'stability', 'Vlasov equation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810128'],"['We consider the parametric excitation of a Langmuir wave and an electromagnetic wave by gravitational radiation, in a thin plasma on a Minkowski background. We calculate the coupling coefficients starting from a kinetic description, and the growth rate of the instability is found. The Manley-Rowe relations are fulfilled only in the limit of a cold plasma. As a consequence, it is generally difficult to view the process quantum mechanically, i.e. as the decay of a graviton into a photon and a plasmon. Finally we discuss the relevance of our investigation to realistic physical situations.']",['1998-10-09'] +1421,['eng'],"['Loinger, A']",['The gravitational waves are fictitious entities'],['Astrophysics and Astronomy'],"['gravitational radiation', 'Einstein equation', 'radiation, electromagnetic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810137'],"['The gravitational waves are non-physical sinuosities generated, in the last analysis, by undulating reference frames.']",['1998-10-09'] +1422,['eng'],"['Bulik, T', 'Gondek-Rosinska, D', 'Kluzniak, W']",['Kilohertz QPOs and strange stars'],['Astrophysics and Astronomy'],"['talk, Taormina 1998/09/14', 'matter, strangeness', 'photon, cosmic radiation', 'n, matter', 'matter, orbit', 'matter, density', 'lower limit', 'upper limit', 'thermodynamics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810141'],"['The kilohertz quasi periodic oscillations (QPOs) discovered in several low mass X-ray binaries (LMXBs) by the Rossi X-ray Timing Explorer (XTE) are thought to occur at the orbital frequency in accretion discs whose inner edge corresponds to the innermost (marginally) stable orbit allowed by general relativity. These ideas have been applied to constrain the equation of state (e.o.s.) of the central neutron star. Here we discuss another possibility, that the central object is a strange star, and show how kHz QPOs constrain the e.o.s. of strange matter.']",['1998-10-09'] +1423,['eng'],"['Ivanchik, A V', 'Potekhin, A Yu', 'Varshalovich, D A']",['The fine-structure constant'],['Astrophysics and Astronomy'],"['fundamental constant, fine structure', 'fundamental constant, time variation', 'astrophysics, quasar', 'spectra, absorption', 'data analysis method', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810166'],"['Endeavours of the unification of the four fundamental interactions have resulted in a development of theories having cosmological solutions in which low-energy limits of fundamental physical constants vary with time. The validity of such theoretical models should be checked by comparison of the theoretical predictions with observational and experimental bounds on possible time-dependences of the fundamental constants. Based on high-resolution measurements of quasar spectra, we obtain the following direct limits on the average rate of the cosmological time variation of the fine-structure constant limit, and |\\dot{\\alpha}/\\alpha| < 3.1 \\times 10^{-14} yr^{-1} is the most conservative limit. Analogous estimates published previously, as well as other contemporary tests for possible variations of \\alpha (those based on the ""Oklo phenomenon"", on the primordial nucleosynthesis models, and others) are discussed and compared with the present upper limit. We argue that the present result is the most conservative one.']",['1998-10-13'] +1424,['eng'],"['Battye, R A', 'Weller, J']",['Cosmic structure formation in Hybrid Inflation models'],['Astrophysics and Astronomy'],"['inflationary universe, hybrid', 'topology, defect', 'grand unified theory', 'cosmic radiation, background', 'perturbation, adiabatic', 'spectra, fluctuation', 'cosmic radiation, anisotropy', 'supergravity', 'string model', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810203'],"['A wide class of inflationary models, known as Hybrid Inflation models, may produce topological defects during a phase transition at the end of the inflationary epoch. We point out that, if the energy scale of these defects is close to that of Grand Unification, then their effect on cosmic structure formation and the generation of microwave background anisotropies cannot be ignored. Therefore, it is possible for structure to be seeded by a combination of the adiabatic perturbations produced during inflation and active isocurvature perturbations produced by defects. Since the two mechanisms are uncorrelated the power spectra can be computed by a weighted average of the individual contributions. We investigate the possible observational consequences of this with reference to general Hybrid Inflation models and also a specific model based on Supergravity. These mixed perturbation scenarios have some novel observational consequences and these are discussed qualitatively.']",['1998-10-14'] +1425,['eng'],"['Primack, Joel R', 'Gross, M A K']",['Cold + Hot Dark Matter After Super-Kamiokande'],['Astrophysics and Astronomy'],"['talk, Blois 1998/06/28', 'astrophysics, missing-mass', 'matter, density', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'neutrino, mass', 'astrophysics, model', 'cosmic radiation, background', 'spectra, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810204'],"['The recent atmospheric neutrino data from Super-Kamiokande provide strong evidence of neutrino oscillations and therefore of non-zero neutrino mass. These data imply a lower limit on the hot dark matter (i.e., light neutrino) contribution to the cosmological density $\\Omega_\\nu >~ 0.001$ --- almost as much as that of all the stars in the universe --- and permit higher But adding to CDM neutrinos with mass of about 5 eV, corresponding to galaxy and cluster distribution. Indeed, the resulting Cold + Hot Dark Matter (CHDM) cosmological model is arguably the most successful $\\Omega_m=1$ model for structure formation. However, other recent data has begun to make the case for $\\Omega_m <~ 0.6$ fairly convincing. In light of all this new data, we reconsider whether cosmology still provides evidence favoring neutrino mass of a few eV in flat models with cosmological constant $Ømega_\\Lambda = 1 - (LCDM) cosmological models with the addition of light neutrinos appears to be rather limited.']",['1998-10-14'] +1426,['eng'],"['Totani, T']","['$\\gamma$-Ray Bursts, Ultra High Energy Cosmic Rays, and Cosmic $\\gamma$-Ray Background']",['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'cosmic radiation, flux', 'background', 'p, cosmic radiation', 'synchrotron radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810207'],"['We argue that ultra high energy cosmic rays (UHECRs) accelerated in gamma-ray bursts (GRBs) can escape from GRBs only when their energy is around the acceleration limit. This effect may compensate the GZK cutoff and gives an explanation of the UHECR events beyond the cutoff. Furthermore, most of the energy carried by ultra high energy protons can be emitted as proton synchrotron photons around TeV range rather than as UHECRs, and cascade of the TeV photons can explain the extragalactic gamma-ray background observed in the GeV range. The predicted flux and spectrum of the GeV background radiation are in good agreement with the recent observation.']",['1998-10-15'] +1427,['eng'],"['Bulik, T', 'Rudak, B']",['Broad-Band Model Spectra of $\\gamma$-Ray Emission from Millisecond Pulsars'],['Astrophysics and Astronomy'],"['talk, Taormina 1998/09/14', 'photon, cosmic radiation', 'pulsar', 'electron, acceleration', 'cosmic radiation, energy spectrum', 'magnetic field', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810007'],"['We present spectra of pulsed gamma-ray emission expected from millisecond pulsars within the framework of polar-cap models. The spectra are a superposition of three components due to curvature (CR), synchrotron (SR), and Compton upscattering (ICS) processes. The CR component dominates below $100 $GeV and the ICS component exhibits a peak at $\\sim 1 $TeV. The CR component should be observable from J0437-4715 with the next generation gamma-ray telescopes, like e.g. GLAST.']",['1998-10-16'] +1428,['eng'],"['Koyama, K', 'Soda, J']",['Bryon Isocurvature Perturbation in the Affleck-Dine Baryogenesis Mechanism'],['Astrophysics and Astronomy'],"['baryon, production', 'condensation', 'fluctuation, spectra', 'inflationary universe', 'baryon, asymmetry', 'coupling']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9810006'],['We propose a primeval baryon isocurvature model in the context of the Affleck-Dine (AD) baryogenesis. Quantum fluctuations of the AD field during inflation produce fluctuations in the baryon number. We obtain a model which gives both the appropriate baryon to entropy ratio of the order $10^{-11}$ and the gaussian baryon isocurvature perturbation of the order $10^{-3}$ at the break of the spectrum 1 Mpc with the steep spectrum $n=-1.5$ on large scales >1 Mpc.'],['1998-10-16'] +1429,['eng'],"['Cillis, A N', 'Fanchiotti, H', 'Canal-Garcia, C A', 'Sciutto, S J']",['Influence of the LPM effect and dielectric suppression on particle air showers'],['Astrophysics and Astronomy'],"['showers, air', 'Landau-Migdal-Pomeranchuk effect', 'bremsstrahlung', 'multiple scattering', 'effect, dielectric', 'electron, pair production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809334'],"[""An analysis of the influence of the Landau-Migdal-Pomeranchuk (LPM) effect on the development of air showers initiated by astroparticles is presented. The theory of Migdal is studied and compared with other theoretical methods. By means of computer simulations and using algorithms that emulate Migdal's theory, including also the so-called dielectric suppression, we study the behavior of the relevant observables in the case of ultra-high energy primaries. We find that the LPM effect can significantly modify the development of high energy electromagnetic showers in certain cases.""]",['1998-09-28'] +1430,['eng'],"['Matsunaga, H', 'Orito, S', 'Matsumoto, H', 'Yoshimura, K', 'Moiseev, A', 'Anraku, K', 'Golden, R L', 'Imori, M', 'Makida, Y', 'Mitchell, J', 'Motoki, M', 'Nishimura, J', 'Nozaki, M', 'Ormes, J', 'Saeki, T', 'Sanuki, T', 'Streitmatter, R E', 'Suzuki, J', 'Tanaka, K', 'Ueda, I', 'Yajima, N', 'Yamagami, T', 'Yamamoto, A', 'Yoshida, T']",['Measurement of Low-Energy Cosmic-Ray Antiprotons at Solar Minimum'],['Astrophysics and Astronomy'],"['anti-p, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'magnetic spectrometer, satellite', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809326'],"[""The absolute fluxes of the cosmic-ray antiprotons at solar minimum are measured in the energy range 0.18 to 1.4 GeV, based on 43 events unambiguously detected in BESS '95 data. The resultant energy spectrum appears to be flat below 1 GeV, compatible with a possible admixture of primary antiproton component with a soft energy spectrum, while the possibility of secondary antiprotons alone explaining the data cannot be excluded with the present accuracy. Further improvement of statistical accuracy and extension of the energy range are planned in future BESS flights.""]",['1998-09-28'] +1431,['eng'],"['Hähnelt, M G']",['Supermassive black holes as sources for LISA'],['Astrophysics and Astronomy'],"['talk, Pasadena 1998/07/06', 'gravitational radiation, emission', 'black hole, massive', 'black hole, production', 'galaxy', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809328'],['Some issues relevant for the formation of supermassive black holes are discused and estimates of the event rates for the emission of gravitational waves by coalescing supermassive black hole binaries are given. The models take into account recent improvements in our knowledge of galaxy and star formation in the high-redshift universe. Estimated event rates range from a few to a hundred per year. Typical events will occur at redshift three or larger in galaxies lying at the (very) faint end of the luminosity function at these redshifts.'],['1998-09-28'] +1432,['eng'],"['Cen, R', 'Ostriker, J P']",['Most of Ordinary Matter in the Universe is in Warm/Hot Gas'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, galaxy', 'astrophysics, missing-mass', 'baryon, density', 'temperature, time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806281'],"['New, high resolution, large-scale, cosmological hydrodynamic galaxy formation simulations of a standard %COBE and cluster normalized cold dark matter model (with a cosmological constant) are utilized to predict the distribution of baryons at the present and at moderate redshift. It is found that the average temperature of baryons is an increasing function of time, with most of the baryons at the present time having a temperature in the range $10^{5-7}$K. Thus, not only the universe is dominated by dark matter, but more than one half of the normal matter is yet to be detected. Detection of this warm/hot gas poses an observational challenge, requiring sensitive EUV and X-ray satellites. Signatures include a soft cosmic X-ray background, apparent warm components in hot clusters due to both intrinsic, warm, intra-cluster gas and inter-cluster gas projected onto clusters along the line of sight, absorption lines in X-ray and UV quasar spectra due to various highly ionized metal species, various strong metal emission lines, and low redshift, broad, low column density $\\lya$ absorption lines.']",['1998-06-23'] +1433,['eng'],"['Ostrowski, M']",['Cosmic Ray Acceleration at Relativistic Plasma Flows'],['Astrophysics and Astronomy'],"['talk, Vulcano 1998/05/25', 'cosmic radiation, acceleration', 'time dependence', 'plasma, relativistic', 'model, shock waves', 'Fokker-Planck equation', 'magnetic field', 'particle, density', 'cosmic radiation, energy spectrum', 'astrophysics, pulsar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808233'],"[""Theoretical concepts ofn cosmic ray particle acceleration at relativistic plasma flows -- shocks and shear layers -- are reviewed. We begin with a discussion of mildly relativistic shock waves. The role of oblique field configurations and field perturbations in forming the particle energy spectrum and changing the acceleration time scale is considered. Then, we report on two interesting attempts to consider particle acceleration at ultra-relativistic shocks. Finally, in contrast to the compressive shock discontinuities, we discuss the acceleration processes acting in the boundary layer at the tangential velocity transition. The second-order Fermi acceleration as well as the cosmic ray `viscous' acceleration provide the mechanisms generating energetic particles there.""]",['1998-08-25'] +1434,['eng'],"['Pina-Avelino, P', 'Caldwell, R R', 'Martins, C J A P']",['Cosmological Consequences of String-forming Open Inflation Models'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'astrophysics, string', 'space-time, horizon', 'astrophysics, missing-mass', 'spectra, perturbation', 'model, hybrid', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809130'],"['We present a study of open inflation cosmological scenarios in which cosmic strings form betwen the two inflationary epochs. It is shown that in these models strings are stretched outside the horizon due to the inflationary expansion but must necessarily re-enter the horizon before the epoch of equal matter and radiation densities. We determine the power spectrum of cold dark matter perturbations in these hybrid models, finding good agreement with observations for values of $\\Gamma=\\Omega_0h\\sim0.3$ and comparable contributions from the active and passive sources to the CMB. Finally, we briefly discuss other cosmological consequences of these models.']",['1998-09-11'] +1435,['eng'],"['Protheroe, R J']",['High energy neutrino astrophysics'],['Astrophysics and Astronomy'],"['talk, Takayama 1998/06/04', 'neutrino, cosmic radiation', 'neutrino, particle source', 'neutrino, flux', 'astrophysics', 'cosmic radiation, background', 'microwaves', 'galaxy, AGN', 'photon, showers', 'topology, defect', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809144'],"['I give a brief discussion of possible sources of high energy neutrinos of astrophysical origin over the energy range from $\\sim 10^{12}$ eV to $\\sim 10^{25}$ eV. In particular I shall review predictions of the diffuse neutrino intensity. Neutrinos from interactions of galactic cosmic rays with interstellar matter are guaranteed, and the intensity can be reliably predicted to within a factor of 2. Somewhat less certain are intensities in the same energy range from cosmic rays escaping from normal galaxies or active galactic nuclei (AGN) and interacting with intracluster gas. At higher energies, neutrinos will definitely be produced by interactions of extragalactic cosmic rays with the microwave background. With the discovery that gamma ray bursts (GRB) are extragalactic, and therefore probably the most energetic phenomena in the Universe, it seems likely that they will be copious sources of high energy neutrinos. Other sources, such as AGN and topological defects, are more speculative. However, searches for neutrinos from all of these potential sources should be made because their detection would have important implications for high energy astrophysics and cosmology.']",['1998-09-14'] +1436,['eng'],"['Fuller, G M', 'Haxton, W C', 'McLaughlin, G C']",['Prospects for Detecting Supernova Neutrino Flavor Oscillations'],['Astrophysics and Astronomy'],"['neutrino, oscillation', 'neutrino, mass', 'supernova', 'MSW effect', 'neutrino nucleus, nuclear reaction', 'charged current', 'neutral current', 'n, particle identification', 'channel cross section, mass number', 'lead', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809164'],"['The neutrinos from a Type II supernova provide perhaps our best opportunity to probe cosmologically interesting muon and/or tauon neutrino masses. This is because matter enhanced neutrino oscillations can lead to an anomalously hot nu_e spectrum, and thus to enhanced charged current cross sections in terrestrial detectors. Two recently proposed supernova neutrino observatories, OMNIS and LAND, will detect neutrons spalled from target nuclei by neutral and charged current neutrino interactions. As this signal is not flavor specific, it is not immediately clear whether a convincing neutrino oscillation signal can be extracted from such experiments. To address this issue we examine the responses of a series of possible light and heavy mass targets, 9Be, 23Na, 35Cl, and 208Pb. We find that strategies for detecting oscillations which use only neutron count rates are problematic at best, even if cross sections are determined by ancillary experiments. Plausible uncertainties in supernova neutrino spectra tend to obscure rate enhancements due to oscillations. However, in the case of 208Pb, a signal emerges that is largely flavor specific and extraordinarily sensitive to the nu_e temperature, the emission of two neutrons. This signal and its flavor specificity are associated with the strength and location of the first-forbidden responses for neutral and charge current reactions, aspects of the 208Pb neutrino cross section that have not been discussed previously. Hadronic spin transfer experiments might be helpful in confirming some of the nuclear structure physics underlying our conclusions.']",['1998-09-15'] +1437,['eng'],"['Horváth, J E', 'Vucetich, H']",['Neutrino sparking and the neutron to strange stars conversion'],['Astrophysics and Astronomy'],"['n, matter', 'matter, strangeness', 'matter, production', 'neutrino nucleon, interaction', 'quark gluon, plasma', 'neutrino, flux', 'cross section']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809385'],"['We address the production of strangelets inside neutron stars by means of high-energy neutrino interactions (sparking). Requiring that neutron stars remain as such along their lifetimes, we obtain a bound on the probability of a strangelet in the final state and compare it with existing laboratory limits. It turns out that this mechanism is not likely to drive a neutron $\\to$ strange stars conversion for realistic values of the minimum center-mass-energy necessary to produce the quark-gluon plasma, a necessary precondition for the formation of the strangelet.']",['1998-09-30'] +1438,['eng'],"['Kennett, M P', 'Melrose, D']",['Neutrino emission via the plasma process in a magnetized plasma'],['Astrophysics and Astronomy'],"['plasma', 'magnetic field', 'neutrino, emission', 'quantum electrodynamics', 'weak interaction, model', 'coupling, axial-vector', 'thermodynamics', 'Feynman graph, higher-order', 'vertex function, (neutrino antineutrino photon)', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9901156'],"['Neutrino emission via the plasma process using the vertex formalism for QED in a strongly magnetized plasma is considered. A new vertex function is introduced to include the axial vector part of the weak interaction. Our results are compared with previous calculations, and the effect of the axial vector coupling on neutrino emission is discussed. The contribution from the axial vector coupling can be of the same order as or greater than the vector vector coupling under certain plasma conditions.']",['1999-01-14'] +1439,['eng'],"['Abriola, D', 'Avignone, F T', 'Brodzinski, R L', 'Collar, J I', 'Gregorio, D E D', 'Farach, H A', 'García, E', 'Gattone, A O', 'Guérard, C K', 'Hasenbalg, F', 'Huck, H', 'Miley, H S', 'Morales, A', 'Morales, J', 'De Solorzano, A O', 'Puimedón, J', 'Reeves, J H', 'Salinas, A', 'Sarsa, M L', 'Villar, J A']",['Search for an annual modulation of dark-matter signals with a germanium spectrometer at the Sierra Grande Laboratory'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'search for, WIMP', 'time variation', 'semiconductor detector, germanium', 'deep underground detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809018'],"['Data collected during three years with a germanium spectrometer at the Sierra Grande underground laboratory have been analyzed for distinctive features of annual modulation of the signal induced by WIMP dark matter candidates. The main motivation for this analysis was the recent suggestion by the DAMA/NaI Collaboration that a yearly modulation signal could not be rejected at the 90% confidence level when analyzing data obtained with a high-mass low-background scintillator detector. We performed two different analyses of the data: First, the statistical distribution of modulation-significance variables (expected from an experiment running under the conditions of Sierra Grande) was compared with the same variables obtained from the data. Second, the data were analyzed in energy bins as an independent check of the first result and to allow for the possibility of a crossover in the expected signal. In both cases no statistically significant deviation from the null result was found, which could support the hypothesis that the data contain a modulated component. A plot is also presented to enable the comparison of these results to those of the DAMA collaboration.']",['1999-02-18'] +1440,['eng'],"['Natarajan, P']",['Accretion history of super-massive black holes'],['Astrophysics and Astronomy'],"['black hole, massive', 'mass, density', 'luminosity, galaxy', 'luminosity, quasar', 'model, accretion', 'astrophysics, missing-mass', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809250'],"['We show that the luminosity function of the actively star-forming Lyman break galaxies and the B-band quasar luminosity function at $z = 3$ can be fit reasonably well with the mass function of collapsed galaxy scale dark matter haloes predicted by viable variants of hierarchical cold dark matter dominated cosmological models for lifetimes $t_Q$ of the optically bright phase of QSOs in the range $10^{6}$ to $10^{8}$ yr. There is a strong correlation between $t_Q$ and the required degree of non-linearity in the relation between black hole and host halo mass. Such a non-linear relation is motivated by suggesting that the mass of supermassive black holes may be limited by the back-reaction of the emitted energy on the accretion flow in a self-gravitating disc. This would imply a relation of black hole to halo mass of the form $M_{\\rm bh} the optically bright QSO phase of the order of the Salpeter time, $\\sim 10^{7}$ yr. The high integrated local mass density of black holes inferred from recent kinematic determinations of black hole masses in nearby galaxies seem to indicate that the overall efficiency of supermassive black holes for producing blue light is lower than was previously assumed. We discuss three possible accretion modes with low optical emission efficiency: (i) accretion well above the Eddington rate, (ii) accretion obscured by dust, and (iii) accretion below the critical rate leading to an advection dominated accretion flow lasting for a Hubble time. We further argue that accretion with low optical efficiency might be closely related to the origin of the hard X-ray background.']",['1998-09-22'] +1441,['eng'],"['Fargion, D', 'Konoplich, R V', 'Grossi, M', 'Khlopov, M Ya']",['Galactic $\\gamma$ Halo by Heavy Neutrino annihilations?'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'particle source, galaxy', 'neutrino, heavy', 'neutrino, annihilation', 'electron, pair production', 'photon electron, Compton scattering', 'cosmic radiation, flux', 'neutrino, mass', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809260'],"['The diffused gamma halo around our Galaxy recently discovered by EGRET could be produced by annihilations of relic neutrinos N (of fourth generation), whose mass is within a narrow range (Mz /2 < M < Mz). Neutrino annihilations in the halo may lead to either ultrarelativistic electron pairs whose inverse Compton Scattering on infrared or optical galactic photons could be the source of the observed GeV gamma rays, or to prompt 100 MeV- 1 GeV photons (due to neutral pion secondaries) born by N - anti N --> Z--> quark pairs reactions. The consequent gamma flux (10 ^(-7)- 10^(-6) cm ^(-2) s^(-1) sr^(-1)) is well comparable to the EGRET observed one and it is also compatible with the narrow window of neutrino mass : 45 GeV < M < 50 GeV recently required to explain the underground DAMA signals. The presence of heavy neutrinos of fourth generation do not contribute much to solve the dark matter problem of the Universe, but it may be easily detectable by outcoming LEP II data.']",['1998-09-22'] +1442,['eng'],"['Xu, R X', 'Qiao, G J']",['A strange star model for GRO J1744-28'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'matter, strangeness', 'magnetic field, high', 'critical phenomena', 'luminosity', 'photon, energy', 'photon, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809048'],"['A model is suggested for the bursting x-ray pulsar, GRO J1744-28, where the compact object of the pulsar is proposed to be a strange matter star with crusts. It is suggested that two envelope crusts shield the two polar caps of an accreting strange stars owing to strong polar-cap magnetic fields. GRO J1744-28 might not have a unified crust, but two polar crusts. Bursts are the result of phase transition of polar crusts if one accreting crust is heavier than that the Coulomb force can support. It is shown that there should be phase-lags when bursting crust is expanded about one hundred meters. Many calculated properties of this model, such as the phase-lags, the bursting luminosity and the characteristic photon energy, are in agreement with observations.']",['1998-09-07'] +1443,['eng'],"['Tavecchio, F', 'Maraschi, L', 'Ghisellini, G']",['Constraints on the Physical Parameters of TeV Blazars'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'blazar', 'electron, spectra', 'Compton scattering', 'cosmic radiation, flux', 'magnetic field', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809051'],"['We consider the constraints on the physical parameters of a homogeneous SSC model that can be derived from the spectral shape and variability of TeV blazars. Assuming that the relativistic electron spectrum is a broken power law, where the break energy $\\gamma_b$ is a free parameter, we write the analytical formulae that allow to connect the physical parameters of the model to observable quantities. The constraints can be summarized in a plane where the coordinates are the Doppler factor and the magnetic field. The consistency between the break energy and the balance between cooling and escape and the interpretation of the soft photon lags measured in some sources as radiative cooling times are treated as additional independent constraints. We apply themethod to the case of three well known blazars, PKS 2155-304, Mrk 421 and Mrk 501.']",['1998-09-07'] +1444,['eng'],"['Baltz, E A', 'Edsjö, J']",['Positron Propagation and Fluxes from Neutralino Annihilation in the Halo'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'supersymmetry', 'neutralino', 'sparticle, annihilation', 'astrophysics, galaxy', 'positron, production', 'positron, flux', 'energy loss', 'diffusion', 'model, solar', 'background', 'positron, energy spectrum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808243'],"['Supersymmetric neutralinos are one of the most promising candidates for the dark matter in the Universe. If they exist, they should make up some fraction of the Milky Way halo. We investigate the fluxes of positrons expected at the Earth from neutralino annihilation in the halo. Positron propagation is treated in a diffusion model including energy loss. The positron source function includes contributions from both continuum and monochromatic positrons. We find that, for a ""canonical"" halo model and propagation parameters, the fluxes are generally too low to be visible. Given the large uncertainties in both propagation and halo structure, it is however possible to obtain observable fluxes. We also investigate the shapes of the positron spectra, including fits to a feature indicated by the results of the HEAT experiment.']",['1998-08-25'] +1445,['eng'],"['Raffelt, G G']",['Comment on Neutrino Radiative Decay Limits from the Infrared Background'],['Astrophysics and Astronomy'],"['neutrino, radiative decay', 'astrophysics, galaxy', 'cosmic radiation, background', 'neutrino, width', 'decay, electric moment', 'decay, magnetic moment', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808299'],['Recent observations of TeV gamma rays from distant sources provide new limits on the cosmic infrared background and thus on radiative decays of background neutrinos. I translate these limits into bounds on transition dipole moments and compare them with limits from the energy-loss of globular-cluster stars. The latter are more restrictive for neutrino masses below 1-2 eV.'],['1998-08-27'] +1446,['eng'],"['Liddle, A R', 'Scherrer, R J']",['A classification of scalar field potentials with cosmological scaling solutions'],['Astrophysics and Astronomy'],"['field theory, scalar', 'potential', 'astrophysics, fundamental constant', 'energy, density', 'scaling', 'model, fluid', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809272'],"['An attractive method of obtaining an effective cosmological constant at the present epoch is through the potential energy of a scalar field. Considering models with a perfect fluid and a scalar field, we classify all potentials for which the scalar field energy density scales as a power-law of the scale factor when the perfect fluid density dominates. There are three possibilities. The first two are well known; the much-investigated exponential potentials have the scalar field mimicking the evolution of the perfect fluid, while for negative power-laws, introduced by Ratra and Peebles, the scalar field density grows relative to that of the fluid. The third possibility is a new one, where the potential is a positive power-law and the scalar field energy density decays relative to the perfect fluid. We provide a complete analysis of exact solutions and their stability properties, and investigate a range of possible cosmological applications.']",['1998-09-23'] +1447,['eng'],"['Krennrich, F', 'Biller, S D']",['Measurement of the Multi-TeV $\\gamma$-ray Flare-Spectra of Markarian 421 and Markarian 501'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'photon, emission', 'photon, absorption', 'astrophysics, blazar', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808333'],"['The energy spectrum of Markarian~421 in flaring states has been measured from 0.3 to 10 TeV using both small zenith angle and large zenith angle observations with the Whipple Observatory 10 m imaging telescope. The large zenith angle technique is useful for extending spectra to high energies, and the extraction of spectra with this technique is discussed. The resulting spectrum of Markarian~421 is fit reasonably well by a simple power-law. This is in contrast to our recently reported spectrum of Markarian 501 which, over a similar energy range, has substantial curvature. The differences in TeV energy spectra of gamma-ray blazars reflect both the physics of the gamma-ray production mechanism and possibly differential absorption effects at the source or in the intergalactic medium. Since Markarian~421 and Markarian~501 have almost the same redshift (0.031 and 0.033 respectively), the difference in their energy spectra must be intrinsic to the sources and not due to intergalactic absorption, assuming the intergalactic infrared background is uniform.']",['1998-08-31'] +1448,['eng'],"['Ioka, K', 'Tanaka, T', 'Nakamura, T']",['Low frequency gravitational waves from black hole MACHO binaries'],['Astrophysics and Astronomy'],"['gravitational radiation, background', 'black hole', 'MACHO, binary', 'statistics', 'galaxy', 'amplitude analysis, background', 'counters and detectors, interference', 'astrophysics, white dwarf', 'spectra, density', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809395'],"['The intensity of low frequency gravitational waves from black hole MACHO binaries is studied. First we estimate the gravitational wave background produced by black hole MACHO binaries in the Milky Way halo as well as the cosmological gravitational wave background produced by the extragalactic black hole MACHO binaries. It is found that the cosmological gravitational wave background due to black hole MACHO binaries is larger than the halo background unless an extreme model of the halo is assumed, while it is smaller than the background due to close white dwarf binaries at $\\nu_{gw} \\siml 10^{-2.5}$ Hz if the actual space density of white dwarfs is maximal. This cosmological background due to black hole MACHO binaries is well below the observational constraints from the pulsar timing, quasar proper motions and so on. We find that one year observation by LISA will be able to detect gravitational waves from at least several hundreds of nearby independent black hole MACHO binaries whose amplitudes exceed these backgrounds. This suggests that LISA will be able to pin down various properties of primordial black hole MACHOs together with the results of LIGO-VIRGO-TAMA-GEO network. Furthermore, it may be possible to draw a map of the mass distribution of our halo, since LISA can determine the position and the distance to individual sources consisted of black hole MACHO binaries. Therefore, LISA may open a new field of the gravitational wave astronomy.']",['1998-10-01'] +1449,['eng'],"['Chiba, M', 'Yoshii, Y']",['New limits on a cosmological constant from statistics of gravitational lensing'],['Astrophysics and Astronomy'],"['gravitation, lens', 'statistics', 'astrophysics, fundamental constant', 'luminosity, galaxy', 'quasar', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808321'],"['We present new limits on cosmological parameters from the statistics of gravitational lensing, based on the recently revised knowledge of the luminosity function and internal dynamics of E/S0 galaxies that are essential in lensing high-redshift QSOs. We find that the lens models using updated Schechter parameters for such galaxies, derived from the recent redshift surveys combined with morphological classification, are found to give smaller lensing probabilities than earlier calculated. Inconsistent adoption of these parameters from a mixture of various galaxy surveys gives rise to systematic biases in the results. We also show that less compact dwarf-type galaxies which largely dominate the faint part of the Schechter-form luminosity function contribute little to lensing probabilities, so that earlier lens models overestimate incidents of small separation lenses. Applications of the lens models to the existing lens surveys indicate that reproduction of both the lensing probability of optical sources and the image separations of optical and radio lenses is significantly improved in the revised lens models. The likelihood analyses allow us to conclude that a flat universe with Omega=0.3(+0.2-0.1) and Omega+Lambda=1 is most preferable, and a matter-dominated flat universe with Lambda=0 is ruled out at 98 % confidence level. These new limits are unaffected by inclusion of uncertainties in the lens properties.']",['1998-08-31'] +1450,['eng'],"['Glück, M', 'Kretzer, S', 'Reya, E']",['Dynamical QCD Predictions for Ultrahigh Energy Neutrino Cross Sections'],['Astrophysics and Astronomy'],"['astrophysics', 'neutrino, cosmic radiation', 'neutrino nucleon, deep inelastic scattering', 'antineutrino nucleon, deep inelastic scattering', 'charged current', 'neutral current', 'nucleon, structure function', 'total cross section, energy dependence', 'quantum chromodynamics', 'momentum spectrum, parton', 'small-x', 'numerical calculations', '< 10**12 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809273'],"['Neutrino-nucleon total cross sections for neutrino energies up to ultrahigh energies (UHE), E_\\nu=10^12 GeV, are evaluated within the framework of the dynamical (radiative) parton model. The expected uncertainties of these predictions do not exceed the level of about 20 % at the highest energies where contributions of parton distributions in the yet unmeasured region around estimated uncertainties of about 2^+-1 due to ad hoc extrapolations of parton distributions to x<10^-5 required for calculating UHE cosmic neutrino event rates.']",['1998-09-23'] +1451,['eng'],"['Kamionkowski, M P']",['Possible Relics from New Physics in the Early Universe'],['Astrophysics and Astronomy'],"['review, Beijing 1998/06/22', 'inflationary universe', 'cosmic radiation, background', 'astrophysics, missing-mass', 'density, perturbation', 'spectra, perturbation', 'gravitational radiation', 'background, stochastic', 'cosmic radiation, polarization', 'axion', 'WIMP', 'sparticle, search for', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809214'],"['I review two different connections between particle theory and early-Universe cosmology: (1) Cosmic-microwave-background (CMB) tests of inflation and (2) particle dark matter. The inflationary predictions of a flat Universe and a nearly scale-invariant spectrum of primordial density perturbations will be tested precisely with forthcoming maps of the CMB temperature. A stochastic gravitational-wave background may be probed with a map of the CMB polarization. I also discuss some other uses of CMB maps. Particle theory has produced two very well-motivated candidates for the dark matter in the Universe: an axion and a supersymmetric particle. In both cases, there are a variety of experiments afoot to detect these particles. I review the properties of these dark-matter candidates and these detection techniques. Much of the material here has appeared before in astro-ph/9712215 and hep-ph/9710467, but the article here is updated and also expanded considerably.']",['1998-09-17'] +1452,['eng'],"['Dar, Arnon']",['Cosmic Rays and $\\gamma$ Ray Bursts From Microblazars'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'jet, relativistic', 'astrophysics, galaxy', 'luminosity', 'energy spectrum', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809163'],"['Highly relativistic jets from merger and accretion induced collapse of compact stellar objects, which may produce the cosmological gamma ray bursts (GRBs), are also very efficient and powerful cosmic ray accelerators. The expected luminosity, energy spectrum and chemical composition of cosmic rays from Galactic GRBs, most of which do not point in our direction, can explain the observed properties of Galactic cosmic rays.']",['1998-09-15'] +1453,['eng'],"['Madsen, J']",['Physics and Astrophysics of Strange Quark Matter'],['Astrophysics and Astronomy'],"['quark, matter', 'matter, strangeness', 'scattering, heavy ion', 'astrophysics, model', 'cosmic radiation', 'hadron, ground state', 'n, matter', 'shell model', 'model, droplet', 'neutrino, emission', 'photon, cosmic radiation', 'pulsar', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809032'],"['3-flavor quark matter (strange quark matter; SQM) can be stable or metastable for a wide range of strong interaction parameters. If so, SQM can play an important role in cosmology, neutron stars, cosmic ray physics, and relativistic heavy-ion collisions. As an example of the intimate connections between astrophysics and heavy-ion collision physics, this Chapter gives an overview of the physical properties of SQM in bulk and of small-baryon number strangelets; discusses the possible formation, destruction, and implications of lumps of SQM (quark nuggets) in the early Universe; and describes the structure and signature of strange stars, as well as formation and detection of strangelets in cosmic rays. It is concluded, that astrophysical and laboratory searches are complementary in many respects, and that both should be pursued to test the intriguing possibility of a strange ground state for hadronic matter, and (more generally) to improve our knowledge of the strong interactions.']",['1998-09-07'] +1454,['eng'],"['Meyer, B S', 'McLaughlin, G C', 'Fuller, G M']",['Neutrino Capture and r-Process Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics', 'n, matter', 'neutrino nucleus, nuclear reaction', 'neutrino, capture', 'neutrino/e', 'light nucleus, production', 'charged current', 'model, fluid', 'neural network', 'thermodynamics', 'temperature', 'entropy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809242'],"['We explore neutrino capture during r-process nucleosynthesis in neutrino-driven ejecta from nascent neutron stars. We focus on the interplay between charged-current weak interactions and element synthesis, and we delineate the important role of equilibrium nuclear dynamics. During the period of coexistence of free nucleons and light and/or heavy nuclei, electron neutrino capture inhibits the r-process. At all stages, capture on free neutrons has a larger impact than capture on nuclei. However, neutrino capture on heavey nuclei by itself, if it is very strong, is also detrimental to the r-process until large nuclear equilibrium clusters break down and the classical neutron-capture phase of the r-process begins. The sensitivity of the r-process to neutrino irradiation means that neutrino-capture effects can strongly constrain the r-process site, neutrino physics, or both. These results apply also to r-process scenarios other than neutrino-heated winds.']",['1998-09-21'] +1455,['eng'],"['Bednarz, J']",['Acceleration time scale at ultrarelativistic shock waves'],['Astrophysics and Astronomy'],"['talk, Alcala de Henares 1998/07/20', 'cosmic radiation, acceleration', 'shock waves, relativistic', 'magnetic field', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808297'],['The first-order cosmic ray acceleration at ultrarelativistic shocks is investigated using the Monte Carlo method. We apply a method of discrete particle momentum scattering as a model of particle pitch angle diffusion to reproduce highly anisotropic conditions at the shock wave. Shocks with Lorentz factors $\\gamma$ up to 320 and varying magnetic field inclinations $\\psi$ are considered. Values of diffusion coefficients upstream in the point where energy spectral indices stabilize to the limit 2.2 were calculated. The obtained acceleration time does not depend on shock conditions.'],['1998-08-27'] +1456,['eng'],"['Geer, S H', 'Kennedy, Dallas C']",['The Cosmic Ray Antiproton Spectrum and a Limit on the Antiproton Lifetime'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'anti-p, cosmic radiation', 'anti-p p, ratio', 'anti-p, spectra', 'anti-p, production', 'anti-p, lifetime', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809101'],"['Measurements of the cosmic ray pbar/p ratio are compared to predictions from an inhomogeneous leaky box model of Galactic secondary pbar production combined with an updated heliospheric model that modulates the predicted fluxes measured at the Earth. The heliospheric corrections are crucial for understanding the low-energy part of the spectrum. The pbar production- propagation-modulation model agrees with observations. Adding a finite pbar lifetime to the model, we obtain the limit tau(pbar) > 1.7 Myr (90% C.L.). Restrictions on heliospheric properties and the cutoff of low-energy interstellar cosmic rays are discussed.']",['1998-09-09'] +1457,['eng'],"['Zimdahl, W', 'Pavón, D']",['Cosmic evolution during primordial black hole evaporation'],['Astrophysics and Astronomy'],"['black hole, radiation', 'model, fluid', 'nonrelativistic', 'astrophysics, model', 'model, hydrodynamical', 'entropy, production', 'pressure', 'energy, density', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809045'],['Primordial black holes with a narrow mass range are regarded as a nonrelativistic fluid component with an equation of state for dust. The impact of the black hole evaporation on the dynamics of the early universe is studied by resorting to a two-fluid model. We find periods of intense radiation reheating in the initial and final stages of the evaporation.'],['1998-09-07'] +1458,['eng'],"['Contaldi, C', 'Hindmarsh, M B', 'Magueijo, J']",['Cosmic Microwave Background and Density Fluctuations from Strings plus Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'astrophysics, string', 'spectra, perturbation', 'density, fluctuation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809053'],"['In cosmological models where local cosmic strings are formed at the end of a period of inflation, the perturbations are seeded both by the defects and by the quantum fluctuations. In a subset of these models, for example those based on $D$-term inflation, the amplitudes are similar. Using our recent calculations of structure formation with cosmic strings, we point out that in a flat cosmology with zero cosmological constant and 5% baryonic component, strings plus inflation fits the observational data much better than each component individually. The large-angle CMB spectrum is mildly tilted, for Harrison-Zeldovich inflationary fluctuations. It then rises to a thick Doppler bump, covering $\\ell=200-600$, modulated by soft secondary undulations. The standard CDM anti-biasing problem is cured, giving place to a slightly biased scenario of galaxy formation.']",['1998-09-07'] +1459,['eng'],"['Torres, D F']",['Precision cosmology as a test for statistics'],['Astrophysics and Astronomy'],"['astrophysics, model', 'matter', 'radiation', 'background, statistical', 'neutrino, temperature', 'photon, temperature', 'galaxy', 'cosmic radiation, background']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809035'],['We compute the shift in the epoch of matter-radiation equality due to the possible existence of a different statistical (non-extensive) background. The shift is mainly caused by a different neutrino-photon temperature ratio. We then consider the prospects to use future large galaxy surveys and cosmic microwave background measurements to constrain the degree of non-extensivity of the universe.'],['1998-09-07'] +1460,['eng'],"['Mücke, A', 'Rachen, J P', 'Engel, R', 'Protheroe, R J', 'Stanev, T']",['On photohadronic processes in astrophysical environments'],['Astrophysics and Astronomy'],"['astrophysics', 'p, cosmic radiation', 'photon, cosmic radiation', 'microwaves, background', 'photon p, interaction', 'baryon resonance, photoproduction', 'baryon resonance, decay', 'nucleon resonance, Delta', 'pi, photoproduction', 'diffraction', 'multiple production', 'string model, fragmentation', 'astrophysics, galaxy', 'photon, particle source', 'cross section, energy dependence', 'photon, energy spectrum', 'p, energy spectrum', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808279'],"[""We discuss the first applications of our newly developed Monte Carlo event generator SOPHIA to multiparticle photoproduction of relativistic protons with thermal and power law radiation fields. The measured total cross section is reproduced in terms of excitation and decay of baryon resonances, direct pion production, diffractive scattering, and non-diffractive multiparticle production. Non--diffractive multiparticle production is described using a string fragmentation model. We demonstrate that the widely used `$\\Delta$--approximation' for the photoproduction cross section is reasonable only for a restricted set of astrophysical applications. The relevance of this result for cosmic ray propagation through the microwave background and hadronic models of active galactic nuclei and gamma-ray bursts is briefly discussed.""]",['1998-08-26'] +1461,['eng'],"['Battye, R A', 'Shellard, E P S']",['Spectrum of radiation from axion strings'],['Astrophysics and Astronomy'],"['talk, Gainesville 1998/03/13', 'astrophysics, string', 'axion, string', 'string, network', 'string model, oscillation', 'axion, radiative decay', 'mass, axion', 'axion, production', 'radiation, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808221'],"['In the wide variety of axion cosmologies in which axion strings form, their radiative decay is the dominant mechanism for the production of axions, imposing a tight constraint on the axion mass. Here, we focus on the mechanism by which axions are produced in this scenario and, in particular, the key issue of the axion spectrum emitted by an evolving network of strings.']",['1998-08-21'] +1462,['eng'],"['Shellard, E P S', 'Battye, R A']",['On the origin of dark matter axions'],['Astrophysics and Astronomy'],"['talk, Gainesville 1998/03/13', 'astrophysics, string', 'astrophysics, missing-mass', 'axion, string', 'axion, mass', 'axion, radiative decay', 'inflationary universe', 'strong interaction, CP', 'critical phenomena']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808220'],"[""We discuss the possible sources of dark matter axions in the early universe. In the standard thermal scenario, an axion string network forms at the Peccei-Quinn phase transition $T\\sim \\fa$ and then radiatively decays into a cosmological background of axions; to be the dark matter, these axions must have a mass $\\ma \\sim 100 \\mu eV$ with specified large uncertainties. An inflationary phase with a reheat temperature below the PQ-scale $T_{reh} provided that the Hubble parameter during inflation is large $H_1 \\gapp \\fa$; this case again implies a dark matter axion mass $\\ma \\sim 100 \\mu eV$. For a smaller Hubble parameter during inflation $H_1 \\lapp \\fa$, `anthropic tuning' allows dark matter axions to have any mass in a huge range below $\\ma\\lapp 1 meV$.""]",['1998-08-21'] +1463,['eng'],"['Damour, Thibault Marie Alban Guillaume', 'Pichon, B']",['Big Bang nucleosynthesis and tensor-scalar gravity'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'gravitation, scalar', 'gravitation, tensor', 'light nucleus, yield', 'baryon, density', 'upper limit', 'electron positron, annihilation', 'coupling, scalar', 'relativity theory, general', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807176'],"[""Big Bang Nucleosynthesis (BBN) is studied within the framework of a two-parameter family of tensor-scalar theories of gravitation, with nonlinear scalar-matter coupling function a(phi). We run a BBN code modified by tensor-scalar gravity, and impose that the theoretically predicted BBN yields of Deuterium, Helium and Lithium lie within some conservative observational ranges. It is found that large initial values of a(phi) (corresponding to initial cosmological expansion rates much larger than standard) are compatible with observed BBN yields. However, the BBN-inferred upper bound on the cosmological baryon density is insignificantly modified by considering tensor-scalar gravity. Taking into account the effect of e^+ e^- annihilation together with the subsequent effect of the matter-dominated era (which both tend to decouple phi from matter), we find that the present value of the scalar coupling, i.e. the present level of deviation from Einstein's theory, must be, for compatibility with BBN, smaller than alpha_0^2 < 10^{-6.5} beta^{-1} (Omega_{matter} h^2 / 0.15)^{-3/2} when beta > 0.5.""]",['1998-07-17'] +1464,['eng'],"['Zimdahl, W', 'Balakin, A B']",['Inflation in a self-interacting gas universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time, de Sitter', 'Einstein equation, solution', 'gas, relativistic', 'vector, Killing', 'model, fluid']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9809002'],"[""We show that a de Sitter spacetime is a solution of Einstein's field equations with the energy momentum tensor of a self-interacting, classical Maxwell-Boltzmann gas in collisional equilibrium. The self-interaction is described by a four-force which is quadratic in the (spatially projected) particle four-momenta. This force does not preserve the particle number and gives rise to an exponential increase in the comoving entropy of the universe while the temperature of the latter remains constant. These properties of a gas universe are related to the existence of a ``projector-conformal'' timelike Killing vector representing a symmetry which is ``in between'' the symmetries characterized by a Killing vector and those characterized by a conformal Killing vector.""]",['1998-09-02'] +1465,['eng'],"['Grandpierre, A']",['A Dynamic Solar Core model'],['Astrophysics and Astronomy'],"['model, solar', 'astrophysics', 'nuclear physics', 'thermodynamics', 'stability', 'neutrino, solar', 'neutrino, flux']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808348'],"['I point out that the all the arguments against an astrophysical solution do not exclude a yet not recognised class of solar models, in which an explosive energy source is present in the solar core besides the standard pp and CNO cycle. It is shown from first principle physics that stars have a non-pp,CNO source: local thermonuclear runaways. I derive a model independent inequality, which shows that the problem of the missing beryllium neutrinos lies in that the SuperKamiokande contains a term arising from neutrinos from a runaway source which can produce high-energy electrons and high-energy axions, and muon and tau neutrinos. I point out, that the temperature dependence of the individual neutrino fluxes is related to pure nuclear physics but the usual luminosity constraint is model dependent and actually is a questionable assumption. Allowing non-pp,CNO reaction chains a new approach arises to interpret the neutrino detector data. The explicit temperature dependence leads to $\\Phi_{pp} \\propto T^4$ instead of the usual $\\Phi_{pp} \\propto T^{-1/2}$ for the SSM luminosity constraint. I assume a Sun analogue to the SSM with a different $T_c$. The separate neutrino detector equations lead to separate detector-related temperatures with the neutrino detector data. The results show a slightly lower than standard central temperature. I attempt to show that helioseismology is not in a necessary conflict with the dynamic solar model presented here. The results of the calculations may propose solutions to the problems of solar and atmospheric neutrino oscillations without an ad hoc introduction of sterile neutrinos and present predictions to Borexino and SNO measurements. {\\it PACS numbers}: 26.65+t, 26.30.+k, 96.60Jw, 95.30.Cq']",['1998-09-01'] +1466,['eng'],"['Kinkhabwala, A', 'Kamionkowski, M P']",['A New Constraint to Open Cold-Dark-Matter Models'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, temperature', 'photon, background', 'correlation', 'cosmic radiation, spectra', 'density, perturbation', 'adiabatic', 'matter, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808320'],"[""We calculate the large-angle cross-correlation between the cosmic-microwave-background (CMB) temperature and the x-ray-background (XRB) intensity expected in an open Universe with cold dark matter (CDM) and a nearly scale-invariant spectrum of adiabatic density perturbations. Using a recent experimental upper limit to the amplitude of this cross-correlation, we find that the matter density (in units of the critical density) in an open Universe must be $\\Omega_0\\gtrsim0.7$. Although there are some effects that might weaken this bound, we conclude that open-CDM models with $\\Omega_0 \\simeq 0.3-0.4$, and the ``open inflation'' theories that produce them, are likely incompatible with CMB/XRB data. This provides additional, albeit indirect, evidence for a cosmological constant.""]",['1998-08-31'] +1467,['eng'],"['Edery, A', 'Paranjape, M B']",['A study of the spherically symmetric vacuum solution to Conformal (Weyl) Gravity'],['Astrophysics and Astronomy'],"['gravitation, conformal', 'vacuum state', 'space-time, singularity', 'photon, scattering', 'photon, tracks', 'tensor, Weyl', 'symmetry, rotational']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808345'],['We study in detail the static spherically symmetric vacuum solution to conformal (Weyl) gravity. One of the more striking aspects of the solution is the presence of a physical singularity at $r=0$ due to the linear term in the metric. Using Penrose diagrams we determine which conformally flat space-times allow light to scatter from infinity and calculate the trajectories and deflection of light for these space-times.'],['1998-09-01'] +1468,['eng'],"['Bahcall, J N']",['Standard Solar Models'],['Astrophysics and Astronomy'],"['talk, Takayama 1998/06/04', 'model, solar', 'nuclear reaction, screening', 'fusion', 'neutrino nucleus, nuclear reaction', 'neutrino, absorption', 'neutrino, solar', 'neutrino, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808162'],['I review recent developments that affect standard solar model predictions of solar neutrino fluxes.'],['1998-08-18'] +1469,['eng'],"['Esposito, S', 'Mangano, G', 'Miele, G', 'Pisanti, O']",['Precision Rates for Nucleon Weak Interactions in Primordial Nucleosynthesis and $^{4}He$ abundance'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'nucleon, weak interaction', 'nucleon, density', 'Born approximation', 'radiative correction, electromagnetic', 'n, lifetime', 'nucleon, mass', 'mass, correction', 'neutrino, temperature', 'helium', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808196'],"['We report the results of a detailed calculation of nucleon weak interactions relevant for the neutron to proton density ratio at the onset of primordial nucleosynthesis. Radiative electromagnetic corrections, finite nucleon mass terms, thermal radiative effects on weak processes and on neutrino temperature are taken into account to reduce the theoretical uncertainty on $n mass fraction $Y_p$ prediction up to $10^{-4}$. We find a positive total correction to the Born prediction $\\delta Y_p \\simeq 0.004$.']",['1998-08-20'] +1470,['eng'],"['Zioutas, Konstantin', 'Thompson, D J', 'Paschos, E A']",['Search for energetic cosmic axions utilizing terrestrial/celestial magnetic fields'],['Astrophysics and Astronomy'],"['search for, axion', 'astrophysics', 'magnetic field, geophysics', 'magnetic field, solar', 'transition, axion photon', 'Primakoff effect', 'numerical calculations', 'proposed experiment', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808113'],"[""Orbiting $\\gamma$-detectors combined with the magnetic field of the Earth or the Sun can work parasitically as cosmic axion telescopes. The relatively short field lengths allow the axion-to-photon conversion to be coherent for $m_{axion} \\sim 10^{-4}$ eV, if the axion kinetic energy is above $\\sim 500$ keV (Earth's field), or, $\\sim 50$ MeV (Sun's field), allowing thus to search for axions from $e^+e^-$ annihilations, from supernova explosions, etc. With a detector angular resolution of $\\sim 1^o$, a more efficient sky survey for energetic cosmic axions passing {\\it through the Sun} can be performed. Axions or other axion-like particles might be created by the interaction of the cosmic radiation with the Sun, similarly to the axion searches in accelerator beam dump experiments; the enormous cosmic energy combined with the built-in coherent Primakoff effect might provide a sensitive detection scheme, being out of reach with accelerators. The axion signal will be an excess in $\\gamma$-rays coming either from a specific celestial place behind the Sun, e.g. the Galactic Center, or, from any other direction in the sky being associated with a violent astrophysical event, e.g. a supernova. Earth bound detectors are also of potential interest. The axion scenario also applies to other stars or binary systems in the Universe, in particular to those with superstrong magnetic fields.""]",['1998-08-13'] +1471,['eng'],"['Roy, M F', 'Crawford, H J']",['Sources of UHE Neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, particle source', 'galaxy, AGN', 'neutrino, emission', 'supernova', 'pulsar', 'photon, cosmic radiation', 'neutrino, flux', 'topology, defect', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808170'],['In this paper we give a brief systematic study of different models of astrophysical point sources of ultra high energy (\\ge 1 TeV) neutrinos.'],['1998-08-18'] +1472,['eng'],"['Turner, M S']",['Large-scale Structure from Quantum Fluctuations in the Early Universe'],['Astrophysics and Astronomy'],"['talk', 'inflationary universe', 'astrophysics, missing-mass', 'quark', 'vacuum state, fluctuation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808149'],"[""A better understanding of the formation of large-scale structure in the Universe is arguably the most pressing question in cosmology. The most compelling and promising theoretical paradigm, Inflation + Cold Dark Matter, holds that the density inhomogeneities that seeded the formation of structure in the Universe originated from quantum fluctuations arising during inflation and that the bulk of the dark matter exists as slowing moving elementary particles (`cold dark matter') left over from the earliest, fiery moments. Large redshift surveys (such as the SDSS and 2dF) and high-resolution measurements of CBR anisotropy (to be made by the MAP and Planck Surveyor satellites) have the potential to decisively test Inflation + Cold Dark Matter and to open a window to the very early Universe and fundamental physics.""]",['1998-08-17'] +1473,['eng'],"['Widerin, P', 'Schmid, C']",['Primordial Black Holes from the QCD Transition?'],['Astrophysics and Astronomy'],"['quantum chromodynamics, critical phenomena', 'black hole, production', 'density, perturbation', 'relativity theory, general', 'pressure', 'fluid, acceleration', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808142'],"['Can a violent process like sudden reheating after supercooling at the onset of a first-order QCD transition improve the possibility of primordial black hole formation? Underdensities reheat earlier than overdensities, there is a short period of huge pressure differences, hence fluid acceleration. Density perturbations on scales far below the Hubble radius $\\lambda\\ll R_{\\rm H} $ get an amplification which grows quadratically in wavenumber, the amplifications at the horizon scale are small. Primordial black hole formation cannot be sufficiently amplified by the QCD transition unless the initial spectrum is fine tuned.']",['1998-08-14'] +1474,['eng'],"['Contaldi, C', 'Hindmarsh, M B', 'Magueijo, J']",['The power spectra of CMB and density fluctuations seeded by local cosmic strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'cosmic radiation, background', 'cosmic radiation, spectra', 'astrophysics, missing-mass', 'density, fluctuation', 'tensor, energy-momentum', 'two-point function', 'topology, defect', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808201'],"[""We compute the power spectra in the cosmic microwave background and cold dark matter (CDM) fluctuations seeded by strings, using the largest string simulations performed so far to evaluate the two-point functions of their stress energy tensor. We find that local strings differ from global defects in that the scalar components of the stress-energy tensor dominate over vector and tensor components. This result has far reaching consequences. We find that cosmic strings exhibit a single Doppler peak of acceptable height at high although the CDM power spectrum in the ``standard'' cosmology (flat geometry, zero cosmological constant, 5% baryonic component) is the wrong shape to fit large scale structure data.""]",['1998-08-20'] +1475,['eng'],"['Starobinsky, A A']",['Inflation for Large Scale Structure'],['Astrophysics and Astronomy'],"['talk, Potsdam 1997/09/15', 'inflationary universe', 'critical phenomena', 'effective potential, inflaton', 'spectra, perturbation', 'field theory, scalar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808152'],"['Two extensions of ideas lying in the basis of the inflationary scenario of the early Universe and their effect on the large scale structure of the present-day Universe are discussed. The first of them is the possibility of fast phase transitions in physical fields other than an inflaton scalar field during inflation and nor far from the end of it. This results in the appearance of specific features in the inflaton effective potential which, in turn, lead to the generation of localized spikes in the primordial perturbation spectrum. At present, there seems to exist one scale in the spectrum, $k=0.05h$ Mpc$^{-1}$, around which we might see something of this type. The second one is the possibility that we are living at the beginning of a new inflation-like era now. Then observations of clustering of high-redshift objects can provide information sufficient for the unambiguous determination of the effective potential of a corresponding present inflaton scalar field.']",['1998-08-17'] +1476,['eng'],"['Kirk, J G', 'Ball, L', 'Skjaeraasen, O']",['Inverse Compton Emission of TeV Gamma Rays from PSR B1259-63'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'photon, emission', 'Compton scattering', 'photon, flux', 'time dependence', 'energy spectrum', 'Cherenkov counter, threshold', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808112'],"['We derive light curves for the hard gamma-ray emission, at energies up to several TeV, expected from the unique pulsar/Be-star binary system PSR B1259-63. This is the only known system in our galaxy in which a radio pulsar is orbiting a main sequence star. We show that inverse Compton emission from the electrons and positrons in the shocked pulsar wind, scattering target photons from the Be star, produces a flux of hard gamma-rays that should be above the sensitivity threshold of present day atmospheric Cerenkov detectors. Furthermore, we predict that the flux of hard gamma-rays produced via this mechanism has a characteristic variation with orbital phase that should be observable, and which is not expected from any other mechanism.']",['1998-08-13'] +1477,['eng'],"['Janka, H T', 'Raffelt, G G']",['No Pulsar Kicks from Deformed Neutrinospheres'],['Astrophysics and Astronomy'],"['neutrino, sphere', 'deformation', 'supernova', 'neutrino, cosmic radiation', 'emission, anisotropy', 'neutrino, flux', 'n, matter', 'astrophysics, pulsar', 'transport theory', 'luminosity, scaling', 'neutrino, oscillation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808099'],"['In a supernova core, magnetic fields cause a directional variation of the neutrino refractive index so that resonant flavor oscillations would lead to a deformation of the ""neutrinosphere"" for, say, tau neutrinos. The associated anisotropic neutrino emission was proposed as a possible origin of the observed pulsar proper motions. We argue that this effect was vastly overestimated because the variation of the temperature over the deformed neutrinosphere is not an adequate measure for the anisotropy of neutrino emission. The neutrino flux is generated inside the neutron star core and is transported through the atmosphere at a constant luminosity, forcing the temperature gradient in the atmosphere to adjust to the inflow of energy from below. Therefore, no emission anisotropy is caused by a deformation of the neutrinosphere to lowest order. An estimate of the higher-order corrections must take into account the modified atmospheric temperature profile in response to the deformation of the neutrinosphere and the corresponding feedback on the core. We go through this exercise in the framework of a simplified model which can be solved analytically.']",['1998-08-12'] +1478,['eng'],"['Collar, J I']",['Solar-bound weakly interacting massive particles'],['Astrophysics and Astronomy'],"['WIMP, search for', 'WIMP, mass', 'phase space, density', 'recoil, energy', 'orbit, solar', 'counters and detectors', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808058'],"[""The case for a stable population of solar-bound Earth-crossing Weakly Interacting Massive Particles (WIMPs) is reviewed. A practical general expression for their speed distribution in the laboratory frame is derived under basic assumptions. If such a population exists -even with a conservative phase-space density-, the next generation of large-mass, low-threshold underground bolometers should bring about a sizable enhancement in WIMP sensitivity. Finally, a characteristic yearly modulation in their recoil signal, arising from the ellipticity of the Earth's orbit, is presented.""]",['1998-08-10'] +1479,['eng'],"['Seidov, Z F']",['Isotope Separation and Solar Neutrino Experiments'],['Astrophysics and Astronomy'],"['nuclide, particle identification', 'neutrino, solar', 'neutrino nucleus, nuclear reaction']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808078'],['The isotope composition of target chemical elements in the Solar Neutrino Experiments is discussed and the possibility of improving this isotope composition is speculated.'],['1998-08-11'] +1480,['eng'],"['Medina-Tanco, G A']",['The effect of highly structured cosmic magnetic fields on ultra-high energy cosmic ray propagation'],['Astrophysics and Astronomy'],"['p, cosmic radiation', 'magnetic field', 'cosmic radiation, flux', 'p, tracks', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808073'],"['The possibility that the magnetic field is strongly correlated with the large-scale structure of the universe has been recently considered in the literature. In this scenario the intergalactic magnetic field has a strong ($\\mu$G) regular component spanning tens of Mpc but localized in sheets and filaments, while the vast voids in between are almost free of magnetic field. If true, this could have important consequences on the propagation of ultra-high energy cosmic rays, and severely affect our capacity of doing astronomy with charged particles. A quantitative discussion of these effects is given in the present work.']",['1998-08-10'] +1481,['eng'],"['Moskalenko, I V', 'Strong, A W', 'Reimer, O']","['Diffuse Galactic gamma rays, cosmic-ray nucleons and antiprotons']",['Astrophysics and Astronomy'],"['p, cosmic radiation', 'nucleon, cosmic radiation', 'anti-p, cosmic radiation', 'fragmentation', 'energy loss', 'acceleration', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808084'],"['The excess of continuum gamma-ray emission from the Galaxy above 1 GeV is an unsolved puzzle. It may indicate that the interstellar nucleon or electron spectra are harder than local direct measurements, as could be the case if a local source of cosmic rays were to dominate the nearby flux. It is however difficult to distinguish between the two cases. Cosmic-ray secondary antiprotons provide a way to resolve this issue. We have made a calculation of the cosmic-ray secondary antiproton spectrum in our model, which computes self-consistently propagation of primary and secondary nucleons, and electrons. Fragmentation and energy losses are computed using realistic distributions for the interstellar gas and radiation fields, and diffusive reacceleration is also incorporated. Our study shows that accurate measurements of the antiproton flux, especially at high energies, could provide a diagnostic of the interstellar nucleon spectrum allowing us to test the hard nucleon spectrum hypothesis. Present antiproton data above 3 GeV indicate that it can already be excluded at the few sigma level.']",['1998-08-11'] +1482,['eng'],"['Dar, Arnon', 'Shaviv, G']",['The Solar Neutrino Problem'],['Astrophysics and Astronomy'],"['talk, Haifa 1998/01/12', 'neutrino, solar', 'neutrino, flux', 'boron', 'luminosity, sum rule', 'beryllium', 'model, solar', 'neutrino, oscillation', 'electroweak interaction', 'nucleus nucleus, nuclear reaction', 'chlorine', 'gallium', 'deep underground detector', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808098'],"['The $^8$B solar neutrino flux as measured by Super-Kamiokande is consistent with the $^{37}$Ar production rate in $^{37}$Cl at Homestake. GALLEX and SAGE, continue to observe $^{71}$Ge production rates in $^{71}$Ga that are consistent with the minimal signal expected from the solar luminosity. The observed $^8$B solar neutrino flux is in good agreement with that predicted by the standard solar model of Dar and Shaviv with nuclear reaction rates that are supported by recent measurements of nuclear fusion cross sections at low energies. The measurements of Super-Kamiokande, SAGE and GALLEX suggest that the expected the pep, $^7$Be and NO solar neutrino fluxes are strongly suppressed. This can be explained by neutrino oscillations and the Mikheyev-Smirnov-Wolfenstein effect. Since neither a flavor change, nor a terrestrial variation, nor a spectral distortion of the $^8$B solar neutrino flux has been observed yet, the solar neutrino problem does not provide conclusive evidence for neutrino properties beyond the standard electroweak model. The deviations of the experimental results from those predicted by the standard solar models may reflect the approximate nature of of solar models and of our knowledge of nuclear reaction rates, radiation transport and particle diffusion in dense stellar plasmas. Only future observations of spectral distortions, or terrestrial modulation or flavor change of solar neutrinos in solar neutrino experiments, such as Super-Kamiokande, SNO, Borexino and HELLAZ will be able to establish that neutrino properties beyond the minimal standard electroweak model are responsible for the solar neutrino problem.']",['1998-08-12'] +1483,['eng'],"['Stecker, F W', 'Salamon, M H']",['Photodisintegration of Ultrahigh Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['nucleus, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, background', 'flux, energy', 'photon nucleus, nuclear reaction', 'nucleus, photofission', 'iron', 'galaxy', 'energy loss', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808110'],"['We present the results of a new calculation of the photodisintegration of ultrahigh energy cosmic ray (UHCR) nuclei in intergalactic space. The critical interactions for energy loss and photodisintegration of UHCR nuclei occur with photons of the 2.73K cosmic background radiation (CBR) and with photons of the infrared background radiation (IBR). We have reexamined this problem making use of a new determination of the IBR based on empirical data, primarily from IRAS galaxies, consistent with direct measurements and upper limits from TeV gamma- ray observations. We have also improved the calculation by including the specific threshold energies for the various photodisintegration interactions in our Monte Carlo calculation. With the new smaller IBR flux, the steepness of the Wien side of the now relatively more important CBR makes their inclusion essential for more accurate results. Our results indicate a significant increase in the propagation time of UHCR nuclei of a given energy over previous results. We discuss the possible significance of this for UHCR origin theory.']",['1998-08-12'] +1484,['eng'],"['Epele, L N', 'Roulet, Esteban']",['On the propagation of the highest energy cosmic ray nuclei'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'nucleus, cosmic radiation', 'energy spectrum, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, background', 'nucleus, photofission', 'iron', 'energy loss', 'mass number, time dependence', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808104'],"['We study the propagation of ultra-high energy cosmic ray nuclei through the background of cosmic microwave and intergalactic infrared photons, using recent re-estimates for the density of the last ones. We perform a detailed Monte Carlo simulation to follow the disintegration histories of nuclei starting as Fe and reaching the Earth from extragalactic sources. We obtain the maximum energies of the arriving nuclear fragments as well as the mass composition as a function of the distance traveled. Cosmic rays with energies in excess of $2\\times 10^{20}$ eV cannot originate from Fe nuclei produced in sources beyond 10 Mpc.']",['1998-08-12'] +1485,['eng'],"['Medina-Tanco, G A', 'Watson, A A']",['The photodisintegration of cosmic ray nuclei by solar photons'],['Astrophysics and Astronomy'],"['nucleus, cosmic radiation', 'nucleus, photofission', 'iron', 'photon, solar', 'magnetic field', 'showers, air', 'cross section, energy dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808033'],"['The interesting possibility of measuring the masses of high energy cosmic ray particles by observing pairs of extensive air showers arriving at the earth nearly simultaneously was proposed some years ago by Gerasimova and Zatsepin (1960). Such showers would be created by the nuclear fragments originating as a result of the photodisintegration of massive nuclei interacting with the solar radiation field. In this paper we re-visit this possibility in the context of existing and proposed detectors of high and ultra-high energy cosmic rays considering a simple, yet realistic, model of the interplanetary magnetic field. The possibilty of observing the mass fragmentation of cosmic rays directly, however, remains challenging.']",['1998-08-07'] +1486,['eng'],"['Ray, R D']",['Can gluon condensate in pulsar cores explain pulsar glitches ?'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'gluon, condensation', 'n, matter', 'vortex', 'superfluid', 'glueball']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807333'],"['Making use of the possibility that gluon condensate can be formed in neutron star core, we study the vortex pinning force between the crust and the interior of the neutron star. Our estimations indicate an increase in pinning strength with the age of the neutron star. This helps in explaining observed pulsar glitches and removes some difficulties faced by vortex creep model.']",['1998-08-03'] +1487,['eng'],"['Caldwell, R R', 'Kamionkowski, M P', 'Wadley, L']",['The First Space-Based Gravitational-Wave Detectors'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'counters and detectors, satellite', 'mass, resonance', 'astrophysics, plasma', 'cosmic radiation, background', 'cosmic radiation, polarization']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807319'],"['Gravitational waves provide a laboratory for general relativity and a window to energetic astrophysical phenomena invisible with electromagnetic radiation. Several terrestrial detectors are currently under construction, and a space-based interferometer is envisioned for launch early next century to detect test-mass motions induced by waves of relatively short wavelength. Very-long-wavelength gravitational waves can be detected using the plasma in the early Universe as test masses; the motion induced in the plasma by a wave is imprinted onto the cosmic microwave background (CMB). While the signature of gravitational waves on the CMB temperature fluctuations is not unique, the polarization pattern can be used to unambiguously detect gravitational radiation. Thus, forthcoming CMB polarization experiments, such as MAP and Planck, will be the first space-based gravitational-wave detectors.']",['1998-07-31'] +1488,['eng'],"['Ehrlich, R']",['Implications for the Cosmic Ray Spectrum of a Negative Electron Neutrino $(Mass)^{2}$'],['Astrophysics and Astronomy'],"['neutrino/e, cosmic radiation', 'neutrino/e, mass', 'neutrino/e, tachyon', 'cosmic radiation, anisotropy', 'cosmic radiation, energy loss', 'cosmic radiation, flux', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807324'],"['Evidence is presented that the electron neutrino may be a tachyon with mass^2 = -4 eV^2/c^4 -- a value consistent with results from tritium beta decay experiments. The evidence consists of an explanation of certain properties of the observed cosmic ray spectrum, including: the existence of a ""knee"" at 10^15 eV, the E^{-3} power law after the knee, the dip at 10^19 eV, the changes in composition above the knee, and the change in anisotropy at the knee.']",['1998-07-31'] +1489,['eng'],"['Ma, F']","['Comment on ""Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down""']",['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'critical phenomena, quark hadron', 'quark, confinement', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807330'],"['This is a comment on a paper by Glendenning, Pei, and Weber (Phys. Rev. Lett., 79, 1603, 1997), where the authors gave an incorrect estimate of the event rate and neglected the important gravitational energy release. Previous work on the same subject is reviewed, and a new suggestion is made to link quark-hadron phase transitions with soft gamma-ray repeaters.']",['1998-08-03'] +1490,['eng'],"['Padilla, L', 'Funk, B', 'Krawczynski, H', 'Contreras, J L', 'Moralejo, A', 'Aharonian, F A', 'Akhperjanian, A G', 'Barrio, J A', 'Beteta, J G', 'Cortina, J', 'Deckers, T', 'Fonseca, V', 'Gebauer, H J', 'González, J C', 'Heinzelmann, G', 'Horns, D', 'Kornmayer, H', 'Lindner, A', 'Lorenz, E', 'Magnussen, N', 'Meyer, H', 'Mirzoian, R M', 'Petry, D', 'Plaga, R', 'Prahl, J', 'Prosch, C', 'Rauterberg, G', 'Rhode, W', 'Röhring, A', 'Sahakian, V V', 'Samorski, M', 'Schmele, D', 'Stamm, W', 'Wiebel-Sooth, B', 'Willmer, M', 'Wittek, W']",['Search for gamma-ray bursts above 20 TeV with the HEGRA AIROBICC Cherenkov array'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, showers', 'photon, energy', 'flux, upper limit', 'Cherenkov counter', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807342'],"['A search for gamma-ray bursts (GRBs) above 20 TeV within the field of view (1 sr) of the HEGRA AIROBICC Cherenkov array (29N, 18W, 2200 m a.s.l.) has been performed using data taken between March 1992 and March 1993. The search is based on an all-sky survey using four time scales, 10 seconds, 1 minute, 4 minutes and 1 hour. No evidence for TeV-emission has been found for the data sample. Flux upper limits are given. A special analysis has been performed for GRBs detected by BATSE and WATCH. Two partially and two fully contained GRBs in our field of view (FOV) were studied. For GRB 920925c which was fully contained in our FOV, the most significant excess has a probability of 7.7 10**-8 (corresponding to 5.4 sigmas) of being caused by a background fluctuation. Correcting this probability with the appropriate trial factor, yields a 99.7% confidence level for this excess to be related to the GRB (corresponding to 2.7 sigmas). This result is discussed within the framework of the WATCH detection.']",['1998-08-03'] +1491,['eng'],"['Gondolo, P']",['The Gamma-Ray Halo from Dark Matter Annihilations'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'WIMP, annihilation', 'astrophysics, missing-mass', 'Higgs particle', 'fermion, Majorana', 'elastic scattering, fermion p', 'cross section', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807347'],"['A sophisticated analysis of EGRET data has found evidence for gamma-ray emission from the galactic halo. I entertain the possibility that part of the EGRET signal is due to WIMP annihilations in the halo. I show that a viable candidate with the required properties exists in a model with an extended Higgs sector. The candidate has a mass of 2--4 GeV, a relic density $\\Omega \\sim 0.1$ (for a Hubble constant of 60 km/s/Mpc), and a scattering cross section off nucleons in the range $10^{-5}$--$10^{-1}$ pb. The model satisfies present observational and experimental constraints, and makes strict predictions on the gamma-ray spectrum of the halo emission.']",['1998-08-03'] +1492,['eng'],"['Kamionkowski, M P']",['New Tests of Inflation'],['Astrophysics and Astronomy'],"['talk, Boston 1998/03/22', 'inflationary universe, validity test', 'cosmic radiation, background', 'temperature, anisotropy', 'density, perturbation', 'spectra, perturbation', 'polarization, tensor', 'gravitational radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808004'],"['Slow-roll inflation generically makes several predictions: a flat Universe, primordial adiabatic density perturbations, and a stochastic gravity-wave background. Each inflation model will further predict specific relations between the amplitudes and shapes of the spectrum of density perturbations and gravity waves. There are now excellent prospects for testing precisely these predictions with forthcoming cosmic microwave background (CMB) temperature and polarization maps.']",['1998-08-04'] +1493,['eng'],"['Capuzzo-Dolcetta, R', 'Miocchi, P']",['Gravitational waves from collapsing globular cluster systems'],['Astrophysics and Astronomy'],"['talk', 'gravitational radiation', 'cluster, galaxy', 'galaxy, AGN', 'black hole', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807102'],"['The evolution of globular cluster systems in some galaxies can be cause of merging of globulars in the very central regions. This high stellar density favours the growth of a central nucleus via swallowing of surrounding stars. The infall of stars into a nuclear black hole is here shown to be, under certain conditions, not only source of electromagnetic radiation but also a significant source of gravitational waves.']",['1998-07-13'] +1494,['eng'],"['López, R E', 'Turner, M S']",['An Accurate Calculation of the Big-Bang Prediction for the Abundance of Primordial Helium'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'helium', 'electron nucleon, interaction', 'radiative correction, finite temperature', 'correction, Coulomb', 'nucleon, mass', 'mass, correction', 'plasma, density', 'electron, mass', 'neutrino, temperature', 'neutrino, decoupling', 'quantum electrodynamics, correction', 'numerical calculations', 'bibliography', 'electron nucleon --> nucleon neutrino']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807279'],"['Within the standard model of particle physics and cosmology we have calculated the big-bang prediction for the primordial abundance of Helium to a theoretical uncertainty of $0.1 \\pct$ $(\\delta Y_P = \\pm 0.0002)$. At this accuracy the uncertainty in the abundance is dominated by the experimental uncertainty in the neutron mean lifetime, $\\tau_n = 885.3 \\pm 2.0 \\rm{sec}$. The following physical effects were included in the calculation: the zero and finite-temperature radiative, Coulomb and finite-nucleon mass corrections to the weak rates; order-$\\alpha$ quantum-electrodynamic correction to the plasma density, electron mass, and neutrino temperature; and incomplete neutrino decoupling. New results for the finite-temperature radiative correction and the QED plasma correction were used. In addition, we wrote a new and independent nucleosynthesis code to control numerical errors to less than 0.1\\pct. Our predictions for the \\EL[4]{He} abundance are summarized with an accurate fitting formula. Summarizing our work in one number, $ Y_P(\\eta = 5\\times 10^{-10}) = 0.2460 \\pm 0.0004 ({\\rm expt}) \\pm < 0.0002 ({\\rm theory})$.']",['1998-07-29'] +1495,['eng'],"['Hannestad, S']",['Post freeze-out annihilations in the early universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'particle, heavy', 'particle, annihilation', 'astrophysics, missing-mass', 'Boltzmann equation, solution', 'light nucleus, production', 'fermion, Majorana', 'neutrino', 'WIMP']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807302'],['We investigate the possible effect of the residual annihilations of heavy particles after freeze-out from equilibrium in the early universe. An error in previous work on this subject is pointed out and the correct method of solving the Boltzmann equation for this case is developed. For Majorana particles there are significant differences relative to previous work.'],['1998-07-30'] +1496,['eng'],"['Kainulainen, K', 'Kurki-Suonio, H', 'Sihvola, E']",['Inhomogeneous Big-Bang Nucleosynthesis in Light of Recent Observations'],['Astrophysics and Astronomy'],"['light nucleus, production', 'helium', 'deuterium', 'lithium', 'baryon, density', 'electroweak interaction, critical phenomena', 'quantum chromodynamics', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807098'],"['We consider inhomogeneous big bang nucleosynthesis in light of the present observational situation. Different observations of He-4 and D disagree with each other, and depending on which set of observations one uses, the estimated primordial He-4 corresponds to a lower baryon density in standard big bang nucleosynthesis than what one gets from deuterium. Recent Kamiokande results rule out a favorite particle physics solution to this tension between He-4 and D. Inhomogeneous nucleosynthesis can alleviate this tension, but the more likely solution is systematics in the observations. The upper limit to Omega_b from inhomogeneous nucleosynthesis is higher than in standard nucleosynthesis, given that the distance scale of the inhomogeneity is near the optimal value, which maximizes effects of neutron diffusion. Possible sources of baryon inhomogeneity include the QCD and electroweak phase transitions. The distance scale of the inhomogeneities arising from the electroweak transition is too small for them to have a large effect on nucleosynthesis, but the effect may still be larger than some of the other small corrections recently incorporated to SBBN codes.']",['1998-07-10'] +1497,['eng'],"['Damour, Thibault Marie Alban Guillaume', 'Krauss, L M']",['A New WIMP Population in the Solar System and New Signals for Dark-Matter Detectors'],['Astrophysics and Astronomy'],"['WIMP, density', 'matter, solar', 'astrophysics, missing-mass', 'supersymmetry', 'WIMP, capture', 'counters and detectors', 'signal processing', 'scattering, nucleon WIMP', 'cross section', 'numerical calculations', 'tables']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807099'],"[""We describe in detail how perturbations due to the planets can cause a sub-population of WIMPs captured by scattering in surface layers of the Sun to evolve to have orbits which no longer intersect the Sun. We argue that such WIMPs, if their orbit has a semi-major axis less than 1/2 of Jupiter's, can persist in the solar system for cosmological timescales. This leads to a new, previously unanticipated WIMP population intersecting the Earth's orbit. The WIMP-nucleon cross sections required for this population to be significant are precisely those in the range predicted for SUSY dark matter, lying near the present limits obtained by direct underground dark matter searches using cyrogenic detectors. Thus, if a WIMP signal is observed in the next generation of detectors, a potentially measurable signal due to this new population must exist. This signal, lying in the keV range for Germanium detectors, would be complementary to that of galactic halo WIMPs. A comparison of event rates, anisotropies, and annual modulations would not only yield additional confirmation that any claimed signal is indeed WIMP-based, but would also allow one to gain information on the nature of the underlying dark matter model.""]",['1998-07-13'] +1498,['eng'],"['Majumdar, D', 'Kar, K', 'Ray, A K', 'Raychaudhuri, A K', 'Sutaria, F K']",['Oscillation Effects On Neutrinos From The Early Phase Of a Nearby Supernova'],['Astrophysics and Astronomy'],"['neutrino/e, oscillation', 'astrophysics, supernova', 'neutrino, mass difference', 'flavor, 2', 'flavor, 3', 'neutrino, mixing angle', 'charged current', 'neutral current', 'neutrino, energy', 'deep underground detector', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807100'],"['Neutrinos emitted during stellar core collapse leading to a supernova are primarily of the electron neutrino type at source which may undergo oscillation between flavor eigenstates during propagation to an earth-bound detector. Although the number of neutrinos emitted during the pre-bounce collapse phase is much smaller than that emitted in the post-bounce phase (in which all flavors of neutrinos are emitted), a nearby supernova event may nevertheless register a substantial number of detections from the pre-bounce phase at SuperKamiokande (SK) and the Sudbury Neutrino Observatory (SNO). The calorimetric measurement of the supernova neutrino fluence from this stage via the charge current and neutral current detection channels in SNO and the corresponding distortion of detected spectrum in SK over the no-oscillation spectrum, can probe information about neutrino mass difference and mixing which are illustrated here in terms of two- and three-flavor oscillation models.']",['1998-07-13'] +1499,['eng'],"['Takeda, M', 'Hayashida, N', 'Honda, K', 'Inoue, N', 'Kadota, K', 'Kakimoto, F', 'Kamata, K', 'Kawaguchi, S', 'Kawasaki, Y', 'Kawasumi, N', 'Kitamura, H', 'Kusano, E', 'Matsubara, Y', 'Murakami, K', 'Nagano, M', 'Nishikawa, D', 'Ohoka, H', 'Sakaki, N', 'Sasaki, M', 'Shinozaki, K', 'Souma, N', 'Teshima, M', 'Torii, R', 'Tsushima, I', 'Uchihori, Y', 'Yamamoto, T', 'Yoshida, S', 'Yoshii, H']","[""Extension of the Cosmic-Ray Energy Spectrum Beyond the Predicted Greisen-Zatsepin-Kuz'min Cutoff""]",['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'showers, air', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807193'],['The cosmic-ray energy spectrum above 10^{18.5} eV is reported using the updated data set of the Akeno Giant Air Shower Array (AGASA) from February 1990 to October 1997. The energy spectrum extends beyond 10^{20} eV and the energy gap between the highest energy event and the others is being filled up with recently observed events. The spectral shape suggests the absence of the 2.7 K cutoff in the energy spectrum or a possible presence of a new component beyond the 2.7 K cutoff.'],['1998-07-21'] +1500,['eng'],"['Dolgov, A D']",['Nonequilibrium cosmic neutrinos and nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Kyoto 1998/04/07', 'light nucleus, production', 'neutrino/tau, cosmic radiation', 'neutrino/tau, mass', 'upper limit', 'neutrino, oscillation', 'neutrino, sterile', 'cosmic radiation, anisotropy', 'lepton, asymmetry', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807134'],['The neutrino role in primordial nucleosynthesis is reviewed. The importance of nonequilibrium effects is emphasized both for the standard massless and possibly massive neutrinos. The upper bound on tau neutrino mass is presented. A spatial variation of primordial abundances and a possibility of observing them by precise measurements of the CMB anisotropy are considered.The nucleosynthesis bounds on the parameters of neutrino oscillations into sterile neutrinos are discussed.'],['1998-07-15'] +1501,['eng'],"['Mannheim, P D']",['How We Got Into The Dark Matter Fix And How We Can Get Out'],['Astrophysics and Astronomy'],"['talk, Boston 1998/03/22', 'astrophysics, missing-mass', 'gravitation, conformal', 'matter, density', 'relativity theory, general']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807122'],"['The recent discovery of cosmic repulsion represents a major challenge to standard gravity, adding an apparent missing energy problem to its still not yet adequately resolved missing mass one, while simultaneously requiring the current universe to be a very special, fine-tuned one. We suggest that the resolution of these difficulties lies not in the existence of more and more exotic gravitational sources, but rather in the lack of reliability of the extrapolation of standard gravity from its solar system origins to the altogether larger distance scales associated with cosmology. We suggest a very different such extrapolation, namely that associated with conformal gravity, to find that all of these issues are then readily and naturally resolved.']",['1998-07-14'] +1502,['eng'],"['Brüggen, M']",['Neutrino spin-flips in curved space-time'],['Astrophysics and Astronomy'],"['neutrino, Dirac', 'neutrino, oscillation', 'spin, flavor', 'effect, relativistic', 'supernova', 'magnetic field', 'space-time', 'matter, static', 'matter, rotational', 'effect, resonance', 'effect, adiabatic', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807183'],"['The general relativistic effects on spin-flavor oscillations above the core of type II supernovae are investigated. The evolution equation is derived and the relative magnitudes of the terms in the Hamiltonian, which arise from the weak, electromagnetic and gravitational interaction, are compared. The effects on the resonance position and the adiabaticity are studied. Explicit calculations are presented for non-rotating and slowly rotating stars.']",['1998-07-20'] +1503,['eng'],"['Krauss, L M']",['New Signatures and Sources for the Detection of WIMP Dark Matter in the Solar System'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1998/02/18', 'astrophysics, missing-mass', 'search for, WIMP', 'capture, solar', 'angular distribution, anisotropy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807146'],"['I first outline new results on the angular modulation of WIMP dark matter scattering on targets in terrestrial laboratories, based on our uncertainties of the WIMP halo distribution, I then outline an exciting new result which indicates that for the high end of allowed SUSY WIMP scattering cross sections there exists a new distribution of WIMP dark matter in our solar system which could produce a dramatically different signal from halo WIMP dark matter in terrestrial detectors.']",['1998-07-15'] +1504,['eng'],"['Kluzniak, W']",['Neutrino oscillations and $\\gamma$-ray bursts'],['Astrophysics and Astronomy'],"['neutrino, oscillation', 'photon, cosmic radiation', 'baryon, density', 'neutrino, sterile', 'cosmic radiation, particle source', 'neutrino, annihilation', 'geometry', 'deep underground detector, KAMIOKANDE', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807224'],"[""If the ordinary neutrinos oscillate into a sterile flavor in a manner consistent with the Super-Kamiokande data on the zenith-angle dependence of atmospheric mu-neutrino flux, an energy sufficient to power a typical cosmic gamma-ray burst (GRB) (about 10^{52} erg) can be carried by sterile neutrinos away from the source and deposited in a region relatively free of baryons. Hence, ultra-relativistic bulk motion (required by the theory of and observations of GRBs and their afterglows) can easily be achieved in the vicinity of plausible sources of GRBs. Oscillations between sterile and ordinary neutrinos would thus provide a solution to the ``baryon-loading problem'' in the theory of GRBs.""]",['1998-07-23'] +1505,['eng'],"['Aharonian, F A']",['Measurement of the radial distribution of Cherenkov light generated by TeV $\\gamma$-ray air showers'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'showers, energy', 'radiation, Cherenkov', 'angular distribution', 'Cherenkov counter', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807119'],"['Using air showers induced by TeV gamma-rays from Mrk 501, the radial distribution of Cherenkov light is investigated. The shower geometry is reconstructed from the stereoscopic shower images obtained with the telescopes of the HEGRA IACT system. We observe a change in the shape of the light pool with shower energy, and with zenith angle. Data are well reproduced by Monte-Carlo air shower simulations.']",['1998-07-14'] +1506,['eng'],"['Nadyozhin, D K', 'Panov, I V', 'Blinnikov, S I']",['The neutrino-induced neutron source in helium shell and r-process nucleosynthesis'],['Astrophysics and Astronomy'],"['neutrino nucleus, nuclear reaction', 'helium', 'n, hadroproduction', 'n, flux', 'light nucleus, production', 'supernova', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807056'],"['The huge neutrino pulse that occurs during the collapse of a massive stellar core, is expected to contribute to the origination of a number of isotopes both of light chemical elements and heavy ones. It is shown that, in general, the heating of stellar matter due to the neutrino scattering off electrons and the heat released from the neutrino-helium breakup followed by the thermonuclear reactions should be taken into account. On the base of kinetic network, using all the important reactions up to Z=8, the main features and the time-dependent character of the neutrino- driven neutron flux are investigated. The time-dependent densities of free neutrons produced in helium breakup, Y_n(t), were used to calculate the r-process nucleosynthesis with another full kinetic network for 3200 nuclides. It was found that in the case of metal-deficient stars, Z < 0.01 Z(solar), the resulting density of free neutrons seems to be high enough to drive the r-process efficiently under favorable conditions. But it is impossible to obtain a sufficient amount of heavy nuclei in neutrino-induced r-process in a helium shell at radii R > R_cr \\approx 10^9 cm. We speculate that to make the neutrino-induced r-process work efficiently in the shell, one has to invoke nonstandard presupernova models in which helium hopefully is closer to the collapsed core owing, for instance, to a large scale mixing or/and rotation and magnetic fields. Apart from this exotic possibility, the neutrino-induced nucleosynthesis in the helium shell is certainly not strong enough to explain the observed solar r-process abundances.']",['1998-07-07'] +1507,['eng'],"['Lai, D']",['Secular Instability of g-Modes in Rotating Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'rotational', 'matter, stability', 'matter, oscillation', 'gravitational radiation', 'energy loss', 'model, hydrodynamical', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806378'],"['Gravitational radiation tends to drive gravity modes in rotating neutron stars unstable. For an inviscid star, the instability sets in when the rotation frequency is about 0.68 times the corresponding mode frequency of the nonrotating star. Neutron stars with spin frequencies $\\go 100$ Hz are susceptible to this instability, with growth time of order years. However, viscous dissipation suppresses the instability except for a narrow range of temperatures around $10^9$ K. We also show that the viscosity driven instability of g-modes is absent.']",['1998-06-30'] +1508,['eng'],"['Gleiser, Marcello', 'Roberts, R']",['Gravitational Waves from Collapsing Vacuum Domains'],['Astrophysics and Astronomy'],"['gravitational radiation', 'critical phenomena', 'domain wall, network', 'domain wall, decay', 'background, stochastic', 'approximation, linear', 'counters and detectors', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807260'],"['The breaking of an approximate discrete symmetry, the final stages of a first order phase transition, or a post-inflationary biased probability distribution for scalar fields are possible cosmological scenarios characterized by the presence of unstable domain wall networks. Combining analytical and numerical techniques, we show that the non-spherical collapse of these domains can be a powerful source of gravitational waves. We compute their contribution to the stochastic background of gravitational radiation and explore their observability by present and future gravitational wave detectors.']",['1998-07-27'] +1509,['eng'],"['Schmid, C', 'Schwarz, Dominik J', 'Widerin, P']",['Amplification of cosmological inhomogeneities by the QCD trasition'],['Astrophysics and Astronomy'],"['astrophysics, model', 'quantum chromodynamics', 'critical phenomena', 'density, perturbation', 'spectra, perturbation', 'astrophysics, missing-mass', 'model, fluid', 'bubble, production', 'bag model', 'neutrino, decoupling', 'black hole, production', 'axion', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807257'],"[""The cosmological QCD transition affects primordial density perturbations. If the QCD transition is first order, the sound speed vanishes during the transition and density perturbations fall freely. For scales below the Hubble radius at the transition the primordial Harrison-Zel'dovich spectrum of density fluctuations develops large peaks and dips. These peaks grow with wave number for both the hadron-photon-lepton fluid and for cold dark matter. At the horizon scale the enhancement is small. This by itself does not lead to the formation of black holes at the QCD transition. The peaks in the hadron-photon-lepton fluid are wiped out during neutrino decoupling. For cold dark matter that is kinetically decoupled at the QCD transition (e.g., axions or primordial black holes) these peaks lead to the formation of CDM clumps of masses $10^{-20} M_\\odot< M_{\\rm clump} < 10^{-10} M_\\odot$.""]",['1998-07-27'] +1510,['eng'],"['Lesgourgues, Julien', 'Polarski, D', 'Starobinsky, A A']",['How large can be the primordial gravitational wave background in inflationary models?'],['Astrophysics and Astronomy'],"['gravitational radiation, background', 'inflationary universe', 'astrophysics, missing-mass', 'astrophysics, fundamental constant', 'spectra, perturbation', 'perturbation, adiabatic', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807019'],"['We consider the primordial gravitational wave (GW) background in a class of spatially-flat inflationary cosmological models with cold dark matter (CDM), a cosmological constant, and a broken-scale-invariant (BSI) steplike primordial (initial) spectrum of adiabatic perturbations produced in an exactly solvable inflationary model where the inflaton potential has a rapid change of its first derivative at some point. In contrast to inflationary models with a scale-free initial spectrum, these models may have a GW power spectrum whose amplitude (though not its shape) is arbitrary for a fixed amplitude of the power spectrum of adiabatic perturbations. In the presence of a positive cosmological constant, the models possess the striking property that a significant part of the large-angle CMB temperature anisotropy observed in the COBE experiment is due to primordial GW. Confronting them with existing observational data on CMB angular temperature fluctuations, galaxy clustering and peculiar velocities of galaxies, we find that for the best parameter values $\\Omega_{\\Lambda}\\approx 0.7$ and $h=0.7$, the GW contribution to the CMB anisotropy can be as large as that of the scalar fluctuations.']",['1998-07-03'] +1511,['eng'],"['Pons, J A', 'Reddy, S', 'Prakash, M', 'Lattimer, J M', 'Miralles, J A']",['Evolution of Protoneutron Stars'],['Astrophysics and Astronomy'],"['astrophysics, model', 'n, matter', 'neutrino, transport theory', 'relativity theory, general', 'thermodynamics', 'effective Lagrangian', 'partition function', 'neutrino, interaction', 'matter', 'neutrino, path length', 'entropy', 'supernova', 'deep underground detector', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807040'],"['We study the thermal and chemical evolution during the Kelvin-Helmholtz phase of the birth of a neutron star, employing neutrino opacities that are consistently calculated with the underlying equation of state (EOS). Expressions for the diffusion coefficients appropriate for general relativistic neutrino transport in the equilibrium diffusion approximation are derived. The diffusion coefficients are evaluated using a field-theoretical finite temperature EOS that includes the possible presence of hyperons. The variation of the diffusion coefficients is studied as a function of EOS and compositional parameters. We present results from numerical simulations of protoneutron star cooling for internal stellar properties as well as emitted neutrino energies and luminosities. We discuss the influence of the initial stellar model, the total mass, the underlying EOS, and the addition of hyperons on the evolution of the protoneutron star and upon the expected signal in terrestrial detectors.']",['1998-07-06'] +1512,['eng'],"['Bullock, J S', 'Primack, Joel R']",['Comments on non-Gaussian density perturbations and the production of primordial black holes'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1998/02/18', 'inflationary universe', 'density, perturbation', 'black hole, production', 'field theory, fluctuation', 'space-time, perturbation', 'perturbation, nonlinear', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806301'],"[""We review the basic arguments for the likelihood of non-Gaussian density perturbations in inflation models with primordial black hole (PBH) production. We discuss our derived distributions of field fluctuations and their implications, specifically commenting on the fine-tuning problem. We also discuss how the derived distributions may be affected when linked to metric perturbations. While linking the metric perturbations to field fluctuations in a nonlinear way may be important for determining exact probability distributions, the correct mapping is not self-evident. The calculation of P. Ivanov, which yields skew positive distribution, is based on an ansatz for the behavior of the nonlinear metric perturbation. We note that the ``natural'' generalization of the gauge-invariant formalism favored by Bond and Salopek yields an effective linear link between the distribution of field fluctuations and metric perturbations during inflation.""]",['1998-06-23'] +1513,['eng'],"['Nakamura, T']",['A Model for Non High Energy $\\gamma$ Ray Bursts and Sources of Ultra High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'n, matter', 'black hole', 'astrophysics, pulsar', 'magnetic field, high', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807087'],"['As a progenitor of NHE (Non High Energy) GRBs, we propose a (C+O) star and a neutron star (black hole) close binary system. Since the (C+O) star is tidally locked, a new born pulsar should be a milli second pulsar (MSP). Dynamo will generate a superstrong magnetic field(SSM). The beam of the energy from the super strongly magnetized milli second pulsar can punch a hole in the supernova ejecta . Then the beam of gamma rays flows out of the ejecta. If we observe this beam from the lateral direction, it will be NHE-GRB. In this model the pulsar with the spin period about 1sec should exist in SN1998bw so that the searches for this pulsar in all the wave length are urgent. SSM-MSPs can accelerate protons up to Ultra High Energy. If a few percent of the beam energy of SSM-MSP in NHE-GRB event is in the form of UHECRs, the flux of the observed UHECRs can be explained. Then along the direction of each UHECR, a supernova remnant should be found. It is suggested that NHE-GRB is the progenitor of the soft gamma ray repeater which has also the superstrong magnetic field and is in the supernova remnant.']",['1998-07-10'] +1514,['eng'],"['Lu, T']",['Observational Effects of Strange Stars'],['Astrophysics and Astronomy'],"['talk, Hong Kong 1997/08/13', 'astrophysics, model', 'n, matter', 'matter, strangeness', 'critical phenomena', 'neutrino, production', 'supernova', 'gravitational radiation', 'photon, showers']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807052'],"['In this talk, after briefly reviewing some historical remarks concerning strange stars, the achievements in physics and dynamical behavior of strange stars are discussed. Especially, various observational effects in distinguishing strange stars from neutron stars such as mechanical effects, cooling effects, phase transition and related interesting phenomena are stressed.']",['1998-07-07'] +1515,['eng'],"['Blasi, P', 'Olinto, A V']",['A Magnetized Local Supercluster and the Origin of the Highest Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'galaxy, cluster', 'magnetic field', 'cosmic radiation, energy spectrum', 'cosmic radiation, angular distribution', 'transport theory', 'diffusion', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806264'],['A sufficiently magnetized Local Supercluster can explain the spectrum and angular distribution of ultra-high energy cosmic rays. We show that the spectrum of extragalactic cosmic rays with energies below $\\sim 10^{20}$ eV may be due to the diffusive propagation in the Local Supercluster with fields of in an almost rectilinear way which is evidenced by the change in shape of the spectrum at the highest energies. The fit to the spectrum requires that at least one source be located relatively nearby at $\\sim 10-15$ Mpc away from the Milky Way. We discuss the origin of magnetic fields in the Local Supercluster and the observable predictions of this model.'],['1998-06-22'] +1516,['eng'],"['Battistoni, G', 'Carboni, M', 'Ferrari, A', 'Patera, V']",['Monte Carlo Study of the Arrival Time Distribution of Particles in Extensive Air Showers in the Energy Range 1-100 TeV'],['Astrophysics and Astronomy'],"['showers, air', 'cosmic radiation, primary', 'photon, cosmic radiation', 'p, cosmic radiation', 'cosmic radiation, energy spectrum', 'time dependence', 'time delay', 'moment, fluctuation', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806265'],"['A detailed simulation of vertical showers in atmosphere produced by primary gammas and protons, in the energy range 1-100 TeV, has been performed by means of the FLUKA Monte Carlo code, with the aim of studying the time structure of the shower front at different detector heights. It turns out that the time delay distribution can be fitted using few parameters coincident with the distribution central moments. Such parameters exhibit a smooth behaviour as a function of energy. These results can be used both for detector design and for the interpretation of the existing measurements. Differences in the time structure between gamma and proton induced showers are found and explained in terms of the non-relativistic component of extensive air showers.']",['1998-06-22'] +1517,['eng'],"['Isaac, M C P', 'Chan, Y D', 'Clark, R', 'Deleplanque, M A', 'Dragowsky, M R', 'Fallon, P', 'Goldman, I D', 'Larimer, R M', 'Lee, I Y', 'Macchiavelli, A O', 'MacLeod, R W', 'Nishiizumi, K', 'Norman, E B', 'Schröder, L S', 'Stephens, F S']",['Search for Strange Matter by Heavy Ion Activation'],['Astrophysics and Astronomy'],"['matter, strangeness', 'search for', 'scattering, heavy ion', 'nickel', 'matter, lunar', 'astrophysics', 'photon, emission', 'solid-state counter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806147'],"['We present the results of an experimental search for stable strange matter using the heavy ion activation technique. We studied samples of a meteorite, terrestrial nickel ore, and lunar soil. Our search improved the existing experimental limit on the strange matter content in normal matter by 2 to 3 orders of magnitude, and allowed us to probe for the first time the flux of low mass strangelets on the lunar surface.']",['1998-06-11'] +1518,['eng'],"['Adelberger, E G', 'Austin, S M', 'Bahcall, J N', 'Balantekin, A B', 'Bogaert, G', 'Brown, L S', 'Buchmann, L R', 'Cecil, F E', 'Champagne, A E', 'De Braeckeleer, L', 'Duba, C A', 'Elliott, S R', 'Freedman, S J', 'Gai, M', 'Goldring, G', 'Gould, C R', 'Gruzinov, A V', 'Haxton, W C', 'Heeger, K M', 'Henley, E', 'Johnson, C W', 'Kamionkowski, M P', 'Kavanagh, R W', 'Koonin, S E', 'Kubodera, K', 'Langanke, K']",['Solar Fusion Cross Sections'],['Astrophysics and Astronomy'],"['review', 'model, solar', 'fusion', 'cross section', 'neutrino, solar', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805121'],"['We review and analyze the available information for nuclear fusion cross sections that are most important for solar energy generation and solar neutrino production. We provide best values for the low-energy cross-section factors and, wherever possible, estimates of the uncertainties. We also describe the most important experiments and calculations that are required in order to improve our knowledge of solar fusion rates.']",['1998-05-12'] +1519,['eng'],"['Hayashida, N', 'Honda, K', 'Inoue, N', 'Kadota, K', 'Kakimoto, F', 'Kamata, K', 'Kawaguchi, S', 'Kawasaki, Y', 'Kawasumi, N', 'Kitamura, H', 'Kusano, E', 'Matsubara, Y', 'Murakami, K', 'Nagano, M', 'Nishikawa, D', 'Ohoka, H', 'Sakaki, N', 'Sasaki, M', 'Shinozaki, K', 'Souma, N', 'Takeda, M', 'Teshima, M', 'Torii, R', 'Tsushima, I', 'Uchihori, Y', 'Yamamoto, T', 'Yoshida, S', 'Yoshii, H']",['The Anisotropy of Cosmic Ray Arrival Directions around $10^{18} eV$'],['Astrophysics and Astronomy'],"['cosmic radiation, anisotropy', 'showers, air', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9807045'],"['Anisotropy in the arrival directions of cosmic rays with energies above 10$^{17}$eV is studied using data from the Akeno 20 km$^2$ array and the Akeno Giant Air Shower Array (AGASA), using a total of about 117,000 showers observed during 11 years. In the first harmonic analysis, we have found strong anisotropy of $\\sim$ 4% around 10$^{18}$eV, corresponding to a chance probability of 0.005%. With two dimensional analysis in right ascension and declination, this anisotropy is interpreted as an excess of showers near the directions of the Galactic Center and the Cygnus region.']",['1998-07-07'] +1520,['eng'],"['Ferreira, P G']",['The impact on cosmology of a primordial scaling field'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1998/02/18', 'astrophysics, model', 'field theory, scalar', 'light nucleus, production', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806373'],"['A scalar field with an exponential potential has the particular property that it is attracted into a solution in which its energy scales as the dominant component (radiation or matter) of the Universe, contributing a fixed fraction of the total energy density. We briefly discuss the dynamics of such a scalar field and its impact on Big Bang nucleosynthesis, the growth of large scale structure and abundance of damped Lyman$-\\alpha$ systems at high redshift. Given the simplicity of the model, its theoretical motivation, and its success in matching observations, we argue that it should be taken on par with other currently viable models of structure formation.']",['1998-06-30'] +1521,['eng'],"['Messer, B', 'Mezzacappa, A', 'Bruenn, S W', 'Guidry, M']",['A Comparison of Boltzmann and Multigroup Flux-Limited Diffusion Neutrino Transport During the Postbounce Shock Reheating Phase in Core Collapse Supernovae'],['Astrophysics and Astronomy'],"['supernova', 'neutrino, diffusion', 'transport theory', 'flavor, 3', 'Boltzmann equation', 'neutrino/e, luminosity', 'antineutrino/e, luminosity', 'neutrino, energy', 'neutrino, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805276'],"[""We compare Newtonian three-flavor multigroup Boltzmann (MGBT) and (Bruenn's) multigroup flux-limited diffusion (MGFLD) neutrino transport in postbounce core collapse supernova environments. We focus our study on quantities central to the postbounce neutrino heating mechanism for reviving the stalled shock. Stationary-state three-flavor neutrino distributions are developed in thermally and hydrodynamically frozen time slices obtained from core collapse and bounce simulations that implement Lagrangian hydrodynamics and MGFLD neutrino transport. Most important, we find, for a region above the gain radius, net heating rates for MGBT that are as much as ~2 times the corresponding MGFLD rates, and net cooling rates below the gain radius that are typically ~0.8 times the MGFLD rates. These differences stem from differences in the neutrino luminosities and mean inverse flux factors, which can be as much as 11% and 24%, respectively. They are greatest at earlier postbounce times for a given progenitor mass and, for a given postbounce time, greater for greater progenitor mass. We discuss the ramifications these new results have for the supernova mechanism.""]",['1998-06-15'] +1522,['eng'],"['Cheng, K S', 'Dai, Z G', 'Wei, D M', 'Lu, T']",['Is GRO J1744-28 a Strange Star?'],['Astrophysics and Astronomy'],"['introductory', 'matter, strangeness', 'fireball, energy', 'photon, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806024'],"['The unusal hard x-ray burster GRO J1744-28 recently discovered by the Compton Gamma-ray Observatory (GRO) can be modeled as a strange star with a dipolar magnetic field $\\le 10^{11} $Gauss. When the accreted mass of the star exceeds some critical mass, its crust may break, resulting in conversion of the accreted matter into strange matter and release of energy. Subsequently, a fireball may form and expand relativistically outward. The expanding fireball may interact with the surrounding interstellar medium, causing its kinetic energy to be radiated in shock waves, producing a burst of x-ray radiation. The burst energy, duration, interval and spectrum derived from such a model are consistent with the observations of GRO J1744-28.']",['1998-06-03'] +1523,['eng'],"['Madsen, J']",['How to identify a Strange Star'],['Astrophysics and Astronomy'],"['astrophysics', 'matter, strangeness', 'n, matter', 'pulsar', 'quark, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806032'],"['Contrary to young neutron stars, young strange stars are not subject to the r-mode instability which slows rapidly rotating, hot neutron stars to rotation periods near 10 ms via gravitational wave emission. Young millisecond pulsars are therefore likely to be strange stars rather than neutron stars, or at least to contain significant quantities of quark matter in the interior.']",['1998-06-03'] +1524,['eng'],"['Tsiklauri, D', 'Viollier, R D']","['Heavy neutrino ball as a possible solution to the ""blackness problem"" of the galactic center']",['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'matter, mass', 'neutrino, heavy', 'astrophysics, missing-mass', 'radiation, spectra', 'black hole', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805272'],"['It has been recently shown (Tsiklauri & Viollier, 1998a) that the matter concentration inferred from observed stellar motion at the galactic center (Eckart & Genzel, 1997, MNRAS, 284, 576 and Genzel et al., 1996, ApJ, 472, 153) is consistent with a supermassive object of $2.5 \\times 10^6$ solar masses, composed of self-gravitating, degenerate heavy neutrinos. It has been furthermore suggested (Tsiklauri & Viollier, 1998a) that the neutrino ball scenario may have the distinct advantage that it could naturally explain the so-called ""blackness problem"" of the galactic center. Here, we present a quantitative proof of this statement, by calculating the emitted spectrum of Sgr A$^*$ in the framework of standard accretion disk theory.']",['1998-06-15'] +1525,['eng'],"['Liddle, A R', 'Mazumdar, A']",['Inflation during oscillations of the inflaton'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, inflaton', 'oscillation', 'potential', 'density, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806127'],"['Damour and Mukhanov have recently devised circumstances in which inflation may continue during the oscillatory phase which ensues once the inflaton field reaches the minimum of its potential. We confirm the existence of this phenomenon by numerical integration. In such circumstances the quantification of the amount of inflation requires particular care. We use a definition based on the decrease of the comoving Hubble length, and show that Damour and Mukhanov overestimated the amount of inflation occurring. We use the numerical calculations to check the validity of analytic approximations.']",['1998-06-11'] +1526,['eng'],"['Schwarz, Dominik J', 'Martín, J']",['Predictions of inflation'],['Astrophysics and Astronomy'],"['talk, Potsdam 1998/03/30', 'inflationary universe', 'density, perturbation', 'perturbation, tensor', 'cosmic radiation, background', 'cosmic radiation, anisotropy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805313'],"['Inflation predicts the generation of cosmological perturbations. Usually, the power spectra for the scalar and tensor modes are calculated with help of the slow roll approximation. In the case of power law inflation an exact result is available. We compare the predictions for the cosmic microwave background anisotropies from the slow roll approximation with the exact results from power law inflation. We find that the so-called consistency check from the slow roll approximation, $C_2^T/C_2^S \\approx -6.93 n_T$, may differ considerably from the exact result.']",['1998-05-26'] +1527,['eng'],"['Alvarez-Muñiz, J', 'Zas, E']",['The LPM effect for EeV hadronic showers in ice'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'showers, hadronic', 'spatial distribution', 'water', 'radiation, Cherenkov', 'Landau-Pomeranchuk-Migdal effect', 'neutrino, cosmic radiation', 'tracks, length', 'pi0, energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806098'],"[""We study the longitudinal development of hadronic showers in ice for energies up to 100 EeV and its implications for radio and optical Cherenkov emission. A small fraction of showers induced by primaries of energy above 1 EeV is shown to display the characteristic elongation associated to the Landau Pomeranchuck Migdal (LPM) effect. The rest look like ordinary showers because the highest energy $\\pi^0$'s interact instead of decaying in two photons. The LPM effect observed in this fraction of the showers is mainly due to $\\eta$ and $\\eta '$ production and decay. We give parameterizations for the total and excess charge tracklengths and for the amplitude and angular spread of the electric field spectrum in the Cherenkov direction. Implications for neutrino detection are briefly addressed.""]",['1998-06-10'] +1528,['eng'],"['Pierpaoli, E', 'Bonometto, S A']",['CMB and Large Scale Structure as a test of Mixed Models with n > 1'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'neutrino, cosmic radiation', 'neutrino, massive', 'astrophysics, missing-mass', 'particle, decay', 'matter, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806037'],"['We compute CBR anisotropies in mixed models with different hot components, including neutrinos or volatile HDM arising from the decay of heavier particles. The CBR power spectra of these models exhibit a higher doppler peak than CDM, and the discrepancy is even stronger in volatile models when the decay gives rise also to a neutral scalar. CBR experiments, together with Large Scale Structure (LSS) data, are then used to constrain the space parameter of mixed models, when values of the primeval spectral index n > 1 are also considered. Even if n>1 is allowed, however, LSS alone prescribes that Ømega_h redshift z_der (down to \\simeq 600) and a high n, while CBR data from baloon--borne experiment cause a severe selection on this part of the parameter space. In fact, while late derelativization and $n>1$ have opposite effects on the fluctuation spectrum P(k), they sum their action on the angular spectrum C_l. Henceforth n \\magcir 1.3 seems excluded by baloon--borne experiment outputs, while a good fit of almost all CBR and LSS data is found for Omega_h values between 0.11 and 0.16, n \\sim 1.1 and z_der \\sim 2000--5000. A smaller n is allowed, but z_der should never be smaller than \\simeq 1200.']",['1998-06-03'] +1529,['eng'],"['Dai, H Y', 'Dawson, B R', 'Elbert, J W', 'Huang, M A', 'Kieda, D B', 'Ko, S', 'Loh, E C', 'Luo, M', 'Smith, J D', 'Sokolsky, P', 'Sommers, P', 'Thomas, S B']","[""Study of Broad Scale Anisotropy of Cosmic Ray Arrival Directions from $2 x 10^{17} eV$ to $10^{20} eV$ from Fly's Eye Data""]",['Astrophysics and Astronomy'],"['astrophysics', 'cosmic radiation, anisotropy', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'showers, air', 'shower detector, experimental results', 'tables', 'bibliography', '2x10**8 - 10**11 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806096'],"[""We report results on the broad scale anisotropy of cosmic ray arrival directions in the energy rage from $2 \\times 10^{17} eV$ to $10^{20} eV$. The data was taken by the Fly's Eye detector in both monocular and stereo modes of operation. We look for dependence on galactic latitude or supergalactic latitude by fitting the data to a Wdowczyk and Wolfendale plane enhancement function and a N-S gradient functional form. We report a small but statistically significant galactic plane enhancement in the energy range between $2\\times 10^{17}eV$ and $3.2 \\times 10^{18} eV$. The probability that this anisotropy is due to fluctuations of an isotropic distribution is less than 0.06%. The most significant galactic plane enhancement factor $f_{E} = 0.104 \\pm 0.036$ is in the energy range $0.4-1.0 \\times 10^{18} eV$. No statistically significant evidence for a N-S gradient is found. There is no sign of significant deviation from isotropic background when the data is analyzed in terms of supergalactic latitude distributions""]",['1998-06-10'] +1530,['eng'],"['Ferrari, V', 'Matarrese, S', 'Schneider, R J']","['Stochastic background of gravitational waves generated by a cosmological population of young, rapidly rotating neutron stars']",['Astrophysics and Astronomy'],"['gravitational radiation, emission', 'background, stochastic', 'spectra, density', 'n, matter', 'rotator', 'background, measurement', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806357'],"['We estimate the spectral properties of the stochastic background of gravitational radiation emitted by a cosmological population of hot, young, rapidly rotating neutron stars. Their formation rate as a function of redshift is deduced from an observation-based determination of the star formation history in the Universe, and the gravitational energy is assumed to be radiated during the spin-down phase associated to the newly discovered r-mode instability. We calculate the overall signal produced by the ensemble of such neutron stars, assuming various cosmological backgrounds. We find that the spectral strain amplitude has a maximum $\\approx (2-4)\\times 10^{-26} {Hz}^{-1/2}$, at frequencies $\\approx (30-60)$ Hz, while the corresponding closure density, $h^2 \\Omega_{GW}$, has a maximum amplitude plateau of $\\approx (2.2-3.3) \\times 10^{-8}$ in the frequency range $(500-1700)$ Hz. We compare our results with a preliminary analysis done by Owen et al. (1998), and discuss the detectability of this background.']",['1998-06-29'] +1531,['eng'],"['Fatuzzo, M', 'Melia, F']",['The Hard X-ray to Gamma-ray Spectrum in the EGRET Active Galactic Nuclei'],['Astrophysics and Astronomy'],"['galaxy, AGN', 'photon, cosmic radiation', 'electron, cosmic radiation', 'black hole', 'Compton scattering', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'electromagnetic field', 'acceleration', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806358'],"['EGRET (20 MeV to 30 GeV) on board the Compton GRO has observed high-energy emission from about 40-50 Active Galactic Nuclei. Theoretical models of this emission based on the upscattering of thermal disk photons by cooling, relativistic electrons can successfully account for the EGRET observations, but they predict a considerably greater X-ray flux than that actually observed in a majority of these sources. This inconsistency may be an indication that the particles are energized during the Compton scattering process, since the X-ray emission is produced by the lowest energy electrons, whose density may be relatively small due to the acceleration. Such a situation may arise as a result of resistive field generation in electromagnetic acceleration schemes, which we here explore. A key feature of this model is the assumed existence of a current associated with the azimuthal component B_phi of the underlying magnetic field by a slight imbalance in the energy distributions of outwardly moving, relativistic electrons and protons produced at the disk surface via shock acceleration. The generation of an electric field (via magnetic field line reconnection) is thus required to maintain the current in the presence of a resistivity induced by the radiative drag on the relativistic electrons. We show that the resulting spectrum can exhibit a significant deficit of X-rays compared with gamma-rays. In addition, due to the uni-directional flow of the current associated with B_phi, this model would predict that the electrons are energized relative to the protons in the outflow only on one side of the disk. They should be decelerated on the reverse side. As such, we would anticipate that any given blazar should have a ~50% probability of being gamma-bright, which appears to be consistent with the observed ratio.']",['1998-06-29'] +1532,['eng'],"['Sigl, G', 'Lemoine, M', 'Biermann, P L']",['Ultra-High Energy Cosmic Ray Propagation in the Local Supercluster'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'nucleon, cosmic radiation', 'astrophysics, cluster', 'magnetic field, turbulence', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806283'],"['We present detailed numerical simulations and analytical approximations of the propagation of nucleons above 10**(19) eV in the Local Supercluster, assuming that the ambient magnetic field is turbulent, and its strength 0.01 < B_rms < 1 micro-Gauss. In such strong magnetic fields, protons in the low energy part of the spectrum, 10**(19) eV < E < E_C diffuse, while the higher energy particles, with E > E_C propagate along nearly straight lines. The magnitude of the transition energy E_C depends mainly on the strength of the magnetic field, the coherence length, and the distance to the source; for B_rms=0.1 micro-Gauss, a largest eddy of length 10 Mpc, and a distance to the source of 10 Mpc, E_C=100 EeV. Our numerical treatment substantially improves on previous analytical approximations, as it allows to treat carefully the transition between the two propagation regimes, as well as the effects due to inhomogeneities expected on scales of a few Mpc. We show that a turbulent magnetic field B_rms=0.1 micro-Gauss, close to equipartition, would allow to reproduce exactly the observed spectrum of ultra high energy cosmic rays, up to the highest energy observed, for a distance to the source below 10 Mpc, for the geometry of the Local Supercluster, i.e. a sheet of thickness 10 Mpc. Diffusion, in this case, allows to reproduce the high flux beyond the Greisen Zatsepin Kuzmin cut-off, with a soft injection spectrum proportional to E**(-2.4). Moreover, the large deflection angles at the highest energies observed, typically 10 degrees for the above values, would explain why no close-by astrophysical counterpart could be associated with these events.']",['1998-06-23'] +1533,['eng'],"['Umeda, H', 'Iwamoto, N', 'Tsuruta, S', 'Qin, L', 'Nomoto, K']",['Axion Mass Limits from Cooling Neutron Stars'],['Astrophysics and Astronomy'],"['talk, Tokyo 1997/11/17', 'n, matter', 'axion, emission', 'energy loss', 'nucleon, superfluid', 'axion, mass', 'upper limit', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806337'],"['The thermal evolution of a neutron star is studied by including the energy loss due to axion emission. Two axion models and three types of neutron-star matter equation of state are used with the effects of nucleon superfluidity properly taken into account. In comparison with the observational data of PSR0656+14 from ROSAT, the upper limits on the axion mass are found to be $m_a < 0.06 - 0.3$ eV and 0.08$ -$ 0.8 eV for the KSVZ and DFSZ axion models, respectively, with the soft equation of state giving the most stringent limits.']",['1998-06-26'] +1534,['eng'],"['Arras, P', 'Lai, D']",['Can Parity Violation in Neutrino Transport Lead to Pulsar Kicks?'],['Astrophysics and Astronomy'],"['n, matter', 'astrophysics, pulsar', 'neutrino, cosmic radiation', 'flux, asymmetry', 'transport theory', 'parity, violation', 'velocity, pulsar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806285'],"['In magnetized proto-neutron stars, neutrino cross sections depend asymmetrically on the neutrino momenta due to parity violation. However, these asymmetric opacities do not induce any asymmetric flux in the bulk interior of the star where neutrinos are nearly in thermal equilibrium. Consequently, parity violation in neutrino absorption and scattering can only give rise to asymmetric neutrino flux above the neutrino-matter decoupling layer. The kick velocity is substantially reduced from previous estimates, requiring a dipole field $B \\sim 10^{16}$~G to get $v_{kick}$ of order a few hundred km~s$^{-1}$.']",['1998-06-23'] +1535,['eng'],"['De Paola, G O', 'Kozameh, C N', 'Tiglio, M H']",['A method to determine the polarization of high energy $\\gamma$-rays'],['Astrophysics and Astronomy'],"['astrophysics', 'photon, cosmic radiation', 'photon, polarization', 'polarization, linear', 'electron, pair production', 'matter', 'differential cross section, angular dependence', 'spatial distribution', 'differential cross section, asymmetry', 'counters and detectors, angular resolution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806302'],"['A method to determine the polarization direction of a very high energy (50 MeV - 30 GeV), linearly polarized gamma ray is analyzed and discussed. We study the differential cross section for pair production and show that the only relevant piece of information comes from the reconstruction of the pair trajectory. In particular the polarization information is coded in the azimuthal distribution of the created pair. We show that the Azimuthal Ratio (AR), defined as the ratio of produced pairs parallel to the polarization vector to pairs perpendicular to this vector, yields a very practical method to determine incoming polarization. We investigate the behavior of this function for different angular resolutions of the measuring apparatus and different energies of the incoming pairs.']",['1998-06-23'] +1536,['eng'],"['Masperi, L', 'Orsaria, M']",['Baryogenesis through gradual collapse of vortons'],['Astrophysics and Astronomy'],"['astrophysics, string', 'baryon, production', 'particle antiparticle, asymmetry', 'decay, vorton', 'velocity', 'potential, chemical', 'electroweak interaction, critical phenomena', 'grand unified theory', 'fermion, emission', 'magnetic field', 'tunneling']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806309'],"['We evaluate the matter-antimatter asymmetry produced by emission of fermionic carriers from vortons which are assumed to be destabilized at the electroweak phase transition.The velocity of contraction of the vorton, calculated through the decrease of its magnetic energy, originates a chemical potential which allows a baryogenesis of the order of the observed value. This asymmetry is not diluted by reheating if the collapse of vortons is distributed along an interval of ~ 10^-9 sec.']",['1998-06-24'] +1537,['eng'],"['Farrar, Glennys R S', 'Biermann, P L']",['Correlation between Compact Radio Quasars and Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'astrophysics, quasar', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806242'],"['Some proposals to account for the highest energy cosmic rays predict that they should point to their sources. We study the five highest energy events (E>10^20 eV) and find they are all aligned with compact, radio-loud quasars. The probability that these alignments are coincidental is 0.005, given the accuracy of the position measurements and the rarity of such sources. The source quasars have redshifts between 0.3 and 2.2. If the correlation pointed out here is confirmed by further data, the primary must be a new hadron or one produced by a novel mechanism.']",['1998-06-18'] +1538,['eng'],"['Bednarz, J', 'Ostrowski, M']",['Energy spectra of cosmic rays accelerated at ultrarelativistic shock waves'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'cosmic radiation, acceleration', 'shock waves, relativistic', 'photon, plasma', 'magnetic field', 'angular distribution', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806181'],"['Energy spectra of particles accelerated by the first-order Fermi mechanism are investigated at ultrarelativistic shock waves, outside the range of Lorentz factors considered previously. For particle transport near the shock a numerical method involving small amplitude pitch-angle scattering is applied for flows with Lorentz factors $\\gamma$ from 3 to 243. For large $\\gamma$ shocks a convergence of derived energy spectral indices up to the value amplitudes and magnetic field configurations. Recently the same index was derived for $\\gamma$-ray bursts by Waxman [Astrophys. J. Lett. 485, L5 (1997)].']",['1998-06-15'] +1539,['eng'],"['Kinney, W H']",['Constraining Inflation with Cosmic Microwave Background Polarization'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, polarization', 'cosmic radiation, anisotropy', 'field theory, scalar', 'density, fluctuation', 'statistics', 'cosmic radiation, temperature', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806259'],"['Observations of the polarization of the cosmic microwave backround (CMB) have the potential to place much tighter constraints on cosmological parameters than observations of the fluctuations in temperature alone. We discuss using CMB polarization to constrain parameters relevant for distinguishing among popular models for cosmological inflation, using the MAP and Planck satellite missions as example cases. Of particular interest is the ability to detect tiny contributions to the CMB anisotropy from tensor modes, which is fundamentally limited by cosmic variance in temperature-only observations. The ability to detect a tensor/scalar ratio $r \\sim 0.01$ would allow precision tests of interesting inflation models, and is possible with a modest increase in sensitivity over that planned for the Planck satellite, or potentially by ground-based experiments.']",['1998-06-19'] +1540,['eng'],"['Epele, L N', 'Roulet, Esteban']","['Comment on ""On the Origin of the Highest Energy Cosmic Rays""']",['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'nucleus, cosmic radiation', 'photon, cosmic radiation', 'energy loss', 'cosmic radiation, background', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806251'],"['We show that the photodisintegration of heavy cosmic ray nuclei with energies above 10^20 eV is dominated by interactions with photons from the cosmic microwave background radiation, rather than from infrared ones. This implies that the observed air shower events with energies 2-3 10^20 eV cannot originate from Fe nuclei coming from distances beyond 10 Mpc']",['1998-06-19'] +1541,['eng'],"['Carroll, S M']",['Quintessence and the Rest of the World'],['Astrophysics and Astronomy'],"['field theory, scalar', 'energy, density', 'coupling, matter', 'symmetry, nonlocal', 'electromagnetic field', 'polarization, vector', 'forces, long-range', 'fundamental constant, time variation', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806099'],"['A nearly-massless, slowly-rolling scalar field $\\phi$ may provide most of the energy density of the current universe. One potential difficulty with this idea is that couplings to ordinary matter, even if suppressed by the Planck scale, should lead to observable long-range forces and time dependence of the constants of nature. I explore the possibility that an approximate global symmetry serves to suppress such couplings even further. Such a symmetry would allow a coupling of $\\phi$ to the pseudoscalar $F_{\\mu\\nu}\\widetilde F^{\\mu\\nu}$ of electromagnetism, which would rotate the polarization state of radiation from distant sources. This effect is fairly well constrained, but it is conceivable that future improvements could lead to a detection of a cosmological scalar field.']",['1998-06-10'] +1542,['eng'],"['Gawiser, E', 'Silk, J']",['Extracting Primordial Density Fluctuations'],['Astrophysics and Astronomy'],"['introductory', 'cosmic radiation, anisotropy', 'density, fluctuation', 'astrophysics, missing-mass', 'neutrino, massive', 'galaxy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806197'],"['The combination of detections of anisotropy in the Cosmic Microwave Background radiation and observations of the large-scale distribution of galaxies probes the primordial density fluctuations of the universe on spatial scales varying by three orders of magnitude. These data are found to be inconsistent with the predictions of several popular cosmological models. Agreement between the data and the Cold + Hot Dark Matter model, however, suggests that a significant fraction of the matter in the universe may consist of massive neutrinos.']",['1998-06-16'] +1543,['eng'],"['Hasenbalg, F']",['Annual modulation sensitivity in cold dark matter searches'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'search for, missing-mass', 'signal processing', 'WIMP', 'background', 'counters and detectors, performance', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806198'],"['The sensitivity of experiments looking for annual modulated signals is discussed and analyzed. The choice of energy intervals for rate integration and enhancing the signal-to-noise ratio of the predicted WIMP signal is addressed. Special emphasis is placed on quantifying the minimum required exposure, MT, under experimental conditions. The difficulty reduces to establish the proper separation between the rate due to the unmodulated part of the WIMP signal and the rate of spurious background present in any experiment. The problem is solved by placing an upper bound to the unmodulated part of the signal using the best exclusion plot. We find that the lowest backgrounds achieved result in exposures in the range MT ~ 5 - 100 kg yr for masses m_{\\chi} > 100 GeV depending on the energy threshold of the detector. While our results are valid for Ge and NaI detectors, the formulae derived apply to other elements as well. Prescriptions are given to estimate exposures for higher background experiments.']",['1998-06-16'] +1544,['eng'],"['Kusenko, A', 'Segrè, G', 'Vilenkin, A']",['Neutrino transport'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'transport theory', 'flux, asymmetry', 'scattering amplitude, anisotropy', 'parity, violation', 'thermodynamics', 'velocity, pulsar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806205'],"[""A small asymmetry in the flux of neutrinos emitted by a hot newly-born neutron star could explain the observed motions of pulsars. However, even in the presence of parity-violating processes with anisotropic scattering amplitudes, no asymmetry is generated in thermal equilibrium. We explain why this no-go theorem stymies some of the proposed explanations for the pulsar ``kick'' velocities.""]",['1998-06-16'] +1545,['eng'],"['Barshay, S', 'Kreyerhoff, G']",['The Decay of Dark-Matter Inflatons Can Produce Very Energetic Cosmic Rays'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'decay, inflaton', 'neutrino, pair production', 'cosmic radiation, energy spectrum', 'showers, air', 'neutrino, cosmic radiation', 'neutrino, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806237'],"['We have shown that inflatons with a mass which is calculated to be of the order of $10^{10}\\GeV$ can constitute a dominant part of dark matter. They can decay uniquely into a neutrino and antineutrino with a lifetime calculated to be greater than the present age of the universe. We show here that these neutrinos can give rise to a localized bump in the primary energy spectrum of extensive air showers. The structure would appear above the sharply-falling spectrum at the expected GZK cut-off energy for primary protons $\\sim 5\\times 10^{19}\\GeV$. The flux which is necessary to compensate for the small cross section is, in principle, attainable, with distant structures also as possible significant sources, and such events might be observed in present experiments.']",['1998-06-18'] +1546,['eng'],"['Pohl, M', 'Esposito, J A']",['Electron acceleration in SNR and diffuse $\\gamma$-rays above 1 GeV'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'electron, cosmic radiation', 'electron, acceleration', 'cosmic radiation, energy spectrum', 'time dependence', 'photon, cosmic radiation', 'electron, injection', 'synchrotron, radiation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806160'],"['The recently observed X-ray synchrotron emission from four supernova remnants (SNR) has strengthened the evidence that cosmic ray electrons are accelerated in SNR. We show, that if this is indeed the case, the local electron spectrum will be strongly time-dependent, at least above roughly 30 GeV. The time dependence stems from the Poisson fluctuations in the number of SNR within a certain volume and within a certain time interval. As far as cosmic ray electrons are concerned, the Galaxy looks like actively bubbling swiss cheese rather than a steady, homogeneously filled system. Our finding has important consequences for studies of the Galactic diffuse gamma-ray emission, for which a strong excess over model predictions above 1 GeV has been reported recently. While these models were relying on an electron injection spectrum with index 2.4 -- chosen to fit the local electron flux up to 1 TeV -- we show that an electron injection index of around 2.0 would a) be consistent with the expected Poisson fluctuations in the locally observable electron spectrum and b) explain the above mentioned gamma-ray excess above 1 GeV. An electron injection index around 2 would also correspond to the average radio synchrotron spectrum of individual SNR. We use a three-dimensional propagation code to calculate the spectra of electrons throughout the Galaxy and show that the longitude and latitude distribution of the leptonic gamma-ray production above 1 GeV is in accord with the respective distributions for the gamma-ray excess. We finally point out that our model implies a strong systematic uncertainty in the determination of the spectrum of the extragalactic gamma-ray background.']",['1998-06-12'] +1547,['eng'],"['Kotok, E V', 'Naselsky, P D']",['Blue spectra and induced formation of primordial black holes'],['Astrophysics and Astronomy'],"['black hole, production', 'statistical analysis', 'spectra, perturbation', 'adiabatic', 'inflationary universe', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806139'],['We investigate the statistical properties of primordial black hole (PBH) formation in the very early Universe. We show that the high level of inhomogeneity of the early Universe leads to the formation of the first generation PBHs. %The existence of these PBHs This causes later the appearance of a dust-like phase of the cosmological expansion. We discuss here a new mechanism for the second generation of PBH formation during the dust-like phase. This mechanism is based on the coagulation process. We demonstrate that the blue power spectrum of initial adiabatic perturbations after inflation leads to overproduction of primordial black holes with $10^9$g$\\le'],['1998-06-11'] +1548,['eng'],"['Sidharth, B G']",['Cosmic Background Radiation Due to Photon Condensation'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'photon, condensation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806142'],"['It is shown that a collection of photons with nearly the same frequency exhibits a Bose ""condensation"" type of phenomenon at about 3 degrees K corresponding to a peak intensity at a wave length of about 0.4cm. This could give a mechanism for the observed Cosmic Background Radiation, and also explain some curious features.']",['1998-06-11'] +1549,['eng'],"['Klein, J R', 'Mann, A K']",['Prototype Detector for Ultrahigh Energy Neutrino Detection'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, counters and detectors', 'neutrino nucleon, interaction', 'charged current', 'muon, flux', 'background', 'angular distribution', 'angular resolution', 'energy resolution', 'deep underground detector']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806152'],"['Necessary technical experience is being gained from successful construction and deployment of current prototype detectors to search for UHE neutrinos in Antarctica, Lake Baikal in Russia, and the Mediterranean. The prototype detectors have also the important central purpose of determining whether or not UHE neutrinos do in fact exist in nature by observation of at least a few UHE neutrino-induced leptons with properties that are not consistent with expected backgrounds. We discuss here the criteria for a prototype detector to accomplish that purpose in a convincing way even if the UHE neutrino flux is substantially lower than predicted at present.']",['1998-06-11'] +1550,['eng'],"['Medvedev, M V']",['The Photino Induced Distortion of the CMBR Blackbody Spectrum'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'spectra, fluctuation', 'transition, photon photino', 'mass, photino', 'lower limit', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806136'],"['It is shown that photon--photino inter-conversions (if exist) may result in a detectable CMBR spectrum distortion which amplitude depends on photino properties, such as its mass. An upper bound on the distortion parameter determined from the recent COBE-FIRAS data, hence, sets a lower bound on the photino mass, $m_{\\tilde\\gamma} \\gtrsim 300 eV$.']",['1998-06-11'] +1551,['eng'],"['Damour, Thibault Marie Alban Guillaume', 'Krauss, L M']",['A New Solar System Population of WIMP Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP, orbit', 'matter, solar', 'gravitation, potential', 'scattering, nucleon WIMP', 'cross section, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806165'],"[""Perturbations due to the planets combined with the non-Coulomb nature of the gravitational potential in the Sun imply that WIMPs that are gravitationally captured by scattering in surface layers of the Sun can evolve into orbits that no longer intersect the Sun. For orbits with a semi-major axis $ < 1/2$ of Jupiter's orbit, such WIMPs can persist in the solar system for $ > 10^9$ years, leading to a previously unanticipated population intersecting Earth's orbit. For WIMPs detectable in the next generation of detectors, this population can provide a complementary signal, in the keV range, to that of galactic halo dark matter.""]",['1998-06-12'] +1552,['eng'],"['Zaldarriaga, M']",['Fluctuations in the Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['thesis', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, fluctuation', 'temperature, fluctuation', 'correlation function, polarization', 'ionization', 'gravitational radiation', 'background, stochastic', 'causality', 'statistical analysis', 'error', 'numerical methods', 'proposed experiment, satellite', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806122'],['In this thesis we investigate several aspects related to the theory of fluctuations in the Cosmic Microwave Background. We develop a new algorithm to calculate the angular power spectrum of the anisotropies which is two orders of magnitude faster than the standard Boltzmann hierarchy approach (Chapter 3). The new algorithm will become essential when comparing the observational results of the next generation of CMB experiments with theoretical predictions. The parameter space of the models is so large that an exhaustive exploration to find the best fit model will only be feasible with this new type of algorithm. We also investigate the polarization properties of the CMB field. We develop a new formalism to describe the statistics of the polarization variables that takes into account their spin two nature (Chapter 2). In Chapter 4 we explore several physical effects that create distinct features in the polarization power spectrum. We study the signature of the reionization of the universe and a stochastic background of gravitational waves. We also describe how the polarization correlation functions can be used to test the causal structure of the universe. Finally in Chapter 5 we quantify the amount of information the next generation of satellites can obtain by measuring both temperature and polarization anisotropies. We calculate the expected error bars on the cosmological parameters for the specifications of the MAP and Planck satellite missions.'],['1998-06-10'] +1553,['eng'],"['López, R E', 'Dodelson, S', 'Scherrer, R J', 'Turner, M S']",['Probing Unstable Massive Neutrinos with Current Cosmic Microwave Background Observations'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'microwaves', 'cosmic radiation, anisotropy', 'neutrino, mass', 'neutrino, decay', 'neutrino, lifetime', 'neutrino, flavor', 'Majoron', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806116'],"['The pattern of anisotropies in the Cosmic Microwave Background depends upon the masses and lifetimes of the three neutrino species. A neutrino species of mass greater than 10 eV with lifetime between 10^{13} sec and 10^{17} sec leaves a very distinct signature (due to the integrated Sachs-Wolfe effect): the anisotropies at large angles are predicted to be comparable to those on degree scales. Present data exclude such a possibility and hence this region of parameter space. For $m_\\nu \\simeq 30$ eV, $\\tau \\simeq 10^{13}$ sec, we find an interesting possibility: the Integrated Sachs Wolfe peak produced by the decaying neutrino in low-$\\Omega$ models mimics the acoustic peak expected in an $\\Omega = 1$ model.']",['1998-06-10'] +1554,['eng'],"['Battye, R A']",['Cosmic strings in a universe with non-critical matter density'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1998/01/17', 'astrophysics, string', 'matter, density', 'astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, polarization', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806115'],"['In the light of recent work which suggests that structure formation by cosmic strings in a critical matter density universe requires large biases, we discuss the effects of reducing the matter density. Using a full linear Einstein-Boltzmann solver, we com pute the cold dark matter density field and the microwave background anisotropies/polarization in a flat universe with a non-zero cosmological constant. We find that universes with distribution, albeit with a bias of around 2. This has interesting implications for the anisotropy and polarization of the microwave background. Finally, we discuss the effects of relaxing the assumption that the universe is flat.']",['1998-06-10'] +1555,['eng'],"['Vietri, M']",['On the energy of neutrinos from $\\gamma$ ray bursts'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'pi, semileptonic decay', 'muon, semileptonic decay', 'neutrino, cosmic radiation', 'model, shock waves', 'fireball', 'time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806110'],"['Ultra high energy protons accelerated at the shocks causing gamma ray bursts photoproduce pions, and then neutrinos in situ. I consider here the sources of losses in this process, namely adiabatic and synchrotron losses by both pions and muons. When the shocks under consideration are external, i.e., those between the ejecta and the surrounding interstellar medium, I show that neutrinos produced by pion decay are unaffected by losses; those produced by muon decay, in the strongly beamed emission required by afterglow observations of GRB 971214, are limited in energy, but still exceed 10^19 eV. In particular, this means that ultra high energy neutrinos will be produced through afterglows.']",['1998-06-10'] +1556,['eng'],"['Winitzki, S']",['Non-Gaussian signature of weak gravitational lensing in the CMB'],['Astrophysics and Astronomy'],"['gravitation, lens', 'cosmic radiation, background', 'cosmic radiation, temperature', 'inflationary universe', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806105'],"['Inflationary cosmologies predict Gaussian primordial fluctuations, but subsequent gravitational lensing of the CMB disturbs its Gaussianity. Knowledge of the specific signature of lensing is necessary to distinguish a lensed Gaussian sky from an intrinsically non-Gaussian one. In this paper we investigate the pattern of non-Gaussian features in the CMB resulting from gravitational lensing, both analytically and numerically. We describe the lensed CMB temperature distribution using the formalism of generating functionals and obtain the complete picture of emerging non-Gaussian effects. To test for the signature of lensing in practice, we propose a scale-dependent statistic based on cumulants of the CMB temperature, and we compute that statistic numerically for typical inflationary models. The effect is expected to be most significant at angular scales $\\sim 10^\\prime$ and its magnitude is within observational capabilities of future satellite missions.']",['1998-06-10'] +1557,['eng'],"['Khosroshahi, H G', 'Sobouti, Y']",['Angular momentum transfer to a star by gravitational waves'],['Astrophysics and Astronomy'],"['talk, Pune 1997/12/16', 'gravitational radiation', 'background, stochastic', 'angular momentum, momentum transfer', 'matter, rotator']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806102'],"['Interaction of a stochastic background of gravitational radiation with celestial systems changes their dynamical elements in a random manner and give rise to secular changes in time. In this spirit we study the angular momentum transfer from a random background of radiation either to a rotating star or to an oscillating one. The angular momentum transferred to such objects by a continuous plane wave is proportional to time, $t$, and by an stochastic background is proportional to $t^{1/2}$.']",['1998-06-10'] +1558,['eng'],"['Bergström, L', 'Edsjö, J', 'Gondolo, P', 'Ullio, P']",['Clumpy Neutralino Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'galaxy', 'supersymmetry', 'neutralino, mass', 'sparticle, annihilation', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'anti-p, flux', 'photon, flux', 'neutrino, flux', 'positron, flux', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806072'],"['We investigate the possibility to detect neutralino dark matter in a scenario in which the galactic dark halo is clumpy. We find that under customary assumptions on various astrophysical parameters, the antiproton and continuum gamma-ray signals from neutralino annihilation in the halo put the strongest limits on the clumpiness of a neutralino halo. We argue that indirect detection through neutrinos from the Earth and the Sun should not be much affected by clumpiness. We identify situations in parameter space where the gamma-ray line, positron and diffuse neutrino signals from annihilations in the halo may provide interesting signals in upcoming detectors.']",['1998-06-05'] +1559,['eng'],"['Durrer, R', 'Gasperini, M', 'Sakellariadou, M', 'Veneziano, Gabriele']",['Massless (pseudo-)scalar seeds of CMB anisotropy'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'perturbation, scalar', 'massless', 'background, stochastic', 'tensor, energy-momentum', 'tensor, fluctuation', 'energy spectrum', 'axion']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9806015'],"[""A primordial stochastic background of very weakly coupled massless (pseudo-)scalars can seed CMB anisotropy, when large-scale fluctuations of their stress-tensor re-enter the horizon during the matter-dominated era. A general relation between multipole coefficients of the CMB anisotropy and the seed's energy spectrum is derived. Magnitude and tilt of the observed anisotropies can be reproduced for the nearly scale-invariant axion spectra that are predicted in a particularly symmetric class of string cosmology backgrounds.""]",['1998-06-02'] +1560,['eng'],"['Suh, I S', 'Mathews, G J']",['Finite temperature effects on cosmological baryon diffusion and inhomogeneous Big-Bang nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'baryon, diffusion', 'cross section, correction', 'finite temperature', 'transport theory', 'electron, mass', 'light nucleus, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805179'],['We have studied finite temperature corrections to the baryon transport cross sections and diffusion coefficients. These corrections are based upon recently computed renormalized electron mass and modified density of states due to the background thermal bath. It is found that the optimum nucleosynthesis yields computed using our diffusion coefficients shift to longer distance scales by a factor of about 3. We also found that the minimum value of $^4 He$ abundance decreases by $\\Delta Y_p \\simeq 0.01$. Effects of these results on constraints from primordial nucleosynthesis are discussed.'],['1998-05-14'] +1561,['eng'],"['Jedamzik, K']",['Non-Standard Big Bang Nucleosynthesis Scenarios'],['Astrophysics and Astronomy'],"['talk, Tegernsee 1997/10/24', 'astrophysics, model', 'light nucleus, production', 'antimatter', 'neutrino, massive', 'neutrino, oscillation', 'particle, decay']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805156'],"['A brief overview of non-standard big bang nucleosynthesis (BBN) scenarios is presented. Trends and results of the light-element nucleosynthesis in BBN scenarios with small-scale or large-scale inhomogeneity, the presence of antimatter domains, stable or unstable massive neutrinos, neutrino oscillations, neutrino degeneracy, or massive decaying particles are summarized.']",['1998-05-13'] +1562,['eng'],"['Adams, J A', 'Sarkar, S', 'Sciama, D W']",['CMB Anisotropy in the Decaying Neutrino Cosmology'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'neutrino, radiative decay', 'temperature, fluctuation', 'spectra, fluctuation', 'astrophysics, missing-mass', 'ionization', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805108'],['It is attractive to suppose for several astrophysical reasons that the universe has close to the critical density in light ($\\sim30$~eV) neutrinos which decay radiatively with a lifetime of $\\sim10^{23}$~sec. In such a cosmology the universe is reionized early and the last scattering surface of the cosmic microwave background significantly broadened. We calculate the resulting angular power spectrum of temperature fluctuations in the cosmic microwave background. As expected the acoustic peaks are significantly damped relative to the standard case. This would allow a definitive test of the decaying neutrino cosmology with the forthcoming MAP and PLANCK surveyor missions.'],['1998-05-11'] +1563,['eng'],"['Schäfer, G', 'Sauerbrey, R']",['Probing Black-Hole Physics in the Laboratory Using High Intensity Femtosecond Lasers'],['Astrophysics and Astronomy'],"['astrophysics', 'black hole, horizon', 'radiation, laser', 'photon, emission', 'gravitation, acceleration', 'plasma, surface', 'equivalence principle']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805106'],"[""It is shown how laboratory experiments performed with high intensity femtosecond lasers can probe the physics of black holes in the near-horizon regime. The acceleration generated by the high intensity laser ranging from $10^{13}$g to more than $10^{18}$g is identified with the gravitational acceleration at stretched horizons. In the black-hole's asymptotic region, the stretched-horizon-reflected light shows a measurable universal phase acceleration of $c^4/4GM$. PACS numbers: 04.70.Bw, 97.60.Lf, 52.40.Nk, 52.50.Jm""]",['1998-05-11'] +1564,['eng'],"['Tsiklauri, D', 'Viollier, R D']",['Dark matter concentration in the galactic center'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'galaxy', 'neutrino, heavy', 'neutrino, mass', 'lower limit', 'gravitation', 'photon, emission', 'velocity, dispersion', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805273'],"['It is shown that the matter concentration observed through stellar motion at the galactic center (Eckart & Genzel, 1997, MNRAS, 284, 576 and Genzel et al., 1996, ApJ, 472, 153) is consistent with a supermassive object of $2.5 \\times 10^6$ solar masses composed of self-gravitating, degenerate heavy neutrinos, as an alternative to the black hole interpretation. According to the observational data, the lower bounds on possible neutrino masses are $m_\\nu \\geq 12.0$ keV$/c^2$ for $g=2$ or $m_\\nu \\geq 14.3$ keV$/c^2$ for $g=1$, where $g$ is the spin degeneracy factor. The advantage of this scenario is that it could naturally explain the low X-ray and gamma ray activity of Sgr A$^*$, i.e. the so called ""blackness problem"" of the galactic center.']",['1998-06-15'] +1565,['eng'],"['Pacheco, J A F']",['Do Soft $\\gamma$ Repeaters Emit Gravitational Waves?'],['Astrophysics and Astronomy'],"['n, matter', 'gravitational radiation, emission', 'photon, cosmic radiation', 'counters and detectors, interference', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805321'],"['Soft gamma repeaters are identified as highly magnetized (B$\\approx 10^{14}$ Gauss) neutron stars. Magnetic stresses induce tectonic activity, and field annihilation in faults is the ultimate energy source for the observed elastic energy is converted into high frequency (kHz) shear waves, that excite nonradial oscillation modes damped by gravitational wave emission. This class of objects should certainly be considered as potential sources of gravitational waves that could be detected by the present planned interferometric antennas like VIRGO or LIGO.']",['1998-05-27'] +1566,['eng'],"['Kanazawa, T', 'Kawasaki, M', 'Sugiyama, N', 'Yanagida, T']",['Observational Implications of Axionic Isocurvature Fluctuations'],['Astrophysics and Astronomy'],"['axion, fluctuation', 'adiabatic', 'inflationary universe, hybrid', 'cosmic radiation, background', 'density, fluctuation', 'M-theory', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805102'],"['Axion is the most attractive candidate to solve the strong CP problem in QCD. If it exists, the inflationary universe produces axion fluctuations which are mixture of isocurvature and adiabatic fluctuations in general. We investigate how large isocurvature fluctuations are allowed or favored in order to explain observations of the large scale structure of the present universe. Generic flat universe models with the mixed (isocurvature$+$adiabatic) density fluctuations are studied. It is found that the observations are consistent with the mixed fluctuation model if ratio $\\alpha$ of the power spectrum of isocurvature fluctuations to that of adiabatic fluctuations is less than $\\sim 0.1$. In particular, the mixed fluctuation model with $\\alpha \\sim 0.05$, total matter density $\\Omega =0.4$ and Hubble parameter $H_0=70$km/s/Mpc gives a very good fit to the observational data. Since the height of the acoustic peak in the angular power spectrum of the cosmic microwave background (CMB) radiation decreases significantly when the isocurvature fluctuations are present, the mixed fluctuation model can be tested in future satellite experiments. Ratios of the amplitude at the peak location to the one at the COBE normalization scale for various models are shown. Furthermore we also obtain the amplitude of isocurvature fluctuations as a function of axion parameters and the Hubble parameter during the inflation. We discuss the axion fluctuations in a hybrid inflation model and find that a significant amount of the isocurvature fluctuations are produced if the axion decay constant $F_{a} \\simeq 10^{15}-10^{16}$GeV. We also briefly discuss a possible connection with the M-theory axion model.']",['1998-05-11'] +1567,['eng'],"['Jedamzik, K']",['Could MACHOS be Primordial Black Holes formed during the QCD Epoch?'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1998/02/18', 'black hole, production', 'MACHO', 'density, fluctuation', 'quantum chromodynamics', 'astrophysics, missing-mass', 'mass, solar', 'gravitational radiation', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805147'],"['Observations by the MACHO collaboration indicate that a significant fraction of the galactic halo dark matter may be in form of compact objects with masses $M\\sim 0.5M_{\\odot}$. Identification of these objects as red or white dwarfs is problematic due to stringent observational upper limits on such dwarf populations. Primordial black hole (PBH) formation from pre-existing density fluctuations is facilitated during the cosmic QCD transition due to a significant decrease in pressure forces. For generic initial density perturbation spectra this implies that essentially all PBHs may form with masses close to the QCD-horizon scale, $M_h^{QCD}\\sim 1M_{\\odot}$. It is possible that such QCD PBHs contribute significantly to the closure density today. I discuss the status of theoretical predictions for the properties of QCD PBH dark matter. Observational signatures of and constraints on a cosmic solar mass PBH population are also discussed.']",['1998-05-13'] +1568,['eng'],"['Totani, T']",['Very Strong TeV Emission as $\\gamma$-Ray Burst Afterglows'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'fireball, relativistic', 'cosmic radiation, acceleration', 'p, synchrotron radiation', 'magnetic field, confinement']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805264'],"['Gamma-ray bursts (GRBs) and following afterglows are considered to be produced by dissipation of kinetic energy of a relativistic fireball and radiation process is widely believed as synchrotron radiation or inverse Compton scattering of electrons. We argue that the transfer of kinetic energy of ejecta into electrons may be inefficient process and hence the total energy released by a GRB event is much larger than that emitted in soft gamma-rays, by a factor of \\sim (m_p/m_e). We show that, in this case, very strong emission of TeV gamma-rays is possible due to synchrotron radiation of protons accelerated up to \\sim 10^{21} eV, which are trapped in the magnetic field of afterglow shock and radiate their energy on an observational time scale of \\sim day. This suggests a possibility that GRBs are most energetic in TeV range and such TeV gamma-rays may be detectable from GRBs even at cosmological distances, i.e., z gives a quantitative explanation for the famous long-duration GeV photons detected from GRB940217. If TeV gamma-ray emission which is much more energetic than GRB photons is detected, it provides a strong evidence for acceleration of protons up to \\sim 10^{21} eV.']",['1998-06-15'] +1569,['eng'],"['Quilis, V', 'Ibáñez, J M', 'Sáez, D']",['Gravitational waves from galaxy clusters'],['Astrophysics and Astronomy'],"['gravitational radiation', 'cluster, galaxy', 'model, hydrodynamical', 'astrophysics, missing-mass', 'Gauss model', 'baryon, gas', 'matter, density', 'amplitude analysis', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805301'],"['A rich galaxy cluster showing strong resemblance with the observed ones is simulated. Cold dark matter spectrum, Gaussian statistics, flat universe, and two components -- baryonic gas plus dark matter particles -- are considered. We have calculated the gravitational-wave output during the epoch of the fully nonlinear and nonsymmetric cluster evolution. The amplitudes and frequencies of the resulting gravitational waves are estimated. Since frequencies are very small --of the order of $10^{-17} Hz$ -- a complete pulse cannot be observed during an admissible integration time; nevertheless, it is proved that these waves can produce an interesting secular effect which appears to be observable with current technology.']",['1998-06-03'] +1570,['eng'],"['Stompor, R', 'Efstathiou, G P']",['Gravitational lensing of CMB anisotropies and cosmological parameters estimation'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'gravitation, lens', 'temperature, anisotropy', 'polarization, anisotropy', 'astrophysics, fundamental constant', 'numerical calculations, interpretation of experiments', 'proposed experiment, satellite']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805294'],"['Gravitational lensing, caused by matter perturbations along the line-of-sight to the last scattering surface, can modify the shape of the cosmic microwave background (CMB) anisotropy power spectrum. We discuss the detectability of lensing distortions to both the temperature and polarisation anisotropy power spectra and we analyse how lensing might affect the estimation of cosmological parameters. For cold dark matter-like models with present-day matter power spectra normalised to match the abundances of rich clusters of galaxies, gravitational lensing causes detectable distortions to cosmic variance limited CMB experiments sampling high multipoles (higher than 1000). Gravitational lensing of the CMB, although a small effect, allows independent determinations of the curvature of the universe and the cosmological constant, i.e. breaking the so-called geometrical degeneracy in CMB parameter estimation discussed by Bond, Efstathiou, Tegmark (1997) and Zaldarriaga, Spergel, Seljak (1997). Gravitational lensing of the CMB temperature and polarisation patterns should be detectable by the Planck Surveyor satellite leading to useful independent constraints on the cosmological constant and spatial curvature.']",['1998-05-25'] +1571,['eng'],"['Magnussen, N']",['The MAGIC telescope project for the study of cosmic rays above 10 GeV'],['Astrophysics and Astronomy'],"['talk, Erice 1997/11/01', 'photon, cosmic radiation', 'showers, air', 'Cherenkov counter, air', 'optics, reflection', 'photoelectron, amplifier', 'semiconductor, optical', 'analog-to-digital converter']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805184'],"['A project to construct a 17 m diameter imaging air Cherenkov telescope, called the MAGIC Telescope, is described. The aim of the project is to close the observation gap in the gamma-ray sky extending from 10 GeV as the highest energy measurable by space-borne experiments to 300 GeV, the lowest energy measurable by the current generation of ground-based Cherenkov telescopes. The MAGIC Telescope will incorporate several new features in order to reach the very low energy threshold. At the same time the new technology will yield an improvement in sensitivity in the energy region where current Cherenkov telescopes are measuring by about an order of magnitude.']",['1998-05-15'] +1572,['eng'],"['Kaplinghat, M', 'Steigman, G', 'Tkachev, Igor I', 'Walker, T P']",['Observational Constraints On Power-Law Cosmologies'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'supernova', 'light nucleus, production', 'deuterium, density', 'helium, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805114'],"['In a class of models designed to solve the cosmological constant problem by coupling scalar or tensor classical fields to the space-time curvature, the universal scale factor grows as a power law in the age, $a \\propto t^\\alpha$, regardless of the matter content or cosmological epoch. We investigate constraints on such ""power-law cosmologies"" from the present age of the Universe, the magnitude-redshift relation, and from primordial nucleosynthesis. Constraints from the current age of the Universe and from the high-redshift supernovae data require ""large"" $\\alpha$ ($\\approx 1$), while consistency with the inferred primordial abundances of deuterium and helium-4 forces $\\alpha$ to lie in a very narrow range around a lower value ($\\approx 0.55$). Inconsistency between these independent cosmological constraints suggests that such power-law cosmologies are not viable.']",['1998-05-11'] +1573,['eng'],"['Shi, X', 'Fuller, G M', 'Halzen, Francis']",['Observing the Birth of Supermassive Black Holes with the ICECUBE Neutrino Detector'],['Astrophysics and Astronomy'],"['black hole, massive', 'black hole, production', 'astrophysics, cluster', 'neutrino, emission', 'luminosity', 'Cherenkov counter, water', 'solids, water', 'deep underground detector, proposed', 'proposed experiment', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805242'],"['Supermassive black holes with masses $\\ga{10}^6 M_\\odot$ are inferred to be the central engines of Active Galactic Nuclei and quasars, and are known to exist in the centers of nearby galaxies observed with the Hubble Space Telescope. It has been suggested that these black holes form as a result of the evolution of relativistic star clusters, in which stellar collisions and tidal disruption could build-up a supermassive star. The Feynman-Chandrasekhar instability could cause such stars to collapse to black holes, accompanied by prodigious thermal neutrino/anti-neutrino emission. We explore the possibility of detecting these neutrino bursts with ICECUBE, a planned 1 km$^3$ neutrino detector in Antarctica (and an expanded version of the current AMANDA - Antarctic Muon and Neutrino Detector Array). Assuming that the formation rate of these black holes tracks that of the quasars, we show that it could be possible for ICECUBE in its supernova-watching mode to detect the neutrino bursts from supermassive collapse events at redshift $z\\la 0.2$ with a rate of the formation of structure in the universe, especially when correlated with gravitational radiation signatures or even gamma-ray bursts.']",['1998-05-20'] +1574,['eng'],"['López-Suarez, J', 'Canal, R']",['Light-Element Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Ringberg Castle 1998/03/23', 'astrophysics, model', 'light nucleus, production', 'postulated particle, heavy', 'postulated particle, decay', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805257'],"['We present a model for big bang nucleosynthesis which combines baryon inhomogeneities with the effects of the decays of massive particles (masses higher than a few GeV). Those particles, with half-lives longer than the standard nucleosynthesis epoch, give rise to both electromagnetic and hadron cascades which modify the abundances of the light nuclides resulting from the previous, inhomogeneous thermonuclear nucleosynthesis stage. We find a region in the parameter space of this composite model where there is agreement with currently inferred primordial abundances for values of $\\Omega_{b}h^{2}_{50}$ as high as 0.35 ($\\Omega_{b}$ being the baryon fraction of the closure density and $h_{50}$ the Hubble constant in units of 50 km/s/Mpc). Possible improvements of the model are pointed out.']",['1998-05-20'] +1575,['eng'],"['Vilenkin, A']","['Open universes, inflation, and the anthropic principle']",['Astrophysics and Astronomy'],"['talk, Kyoto 1998/04/07', 'inflationary universe, open', 'matter, density', 'vacuum state, bubble', 'density, fluctuation', 'instanton']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805252'],['Models of open inflation with a variable density parameter $\\Omega$ provide the most natural way to reconcile an open universe with inflation. The use of anthropic principle is essential to derive observational predictions of such models. I discuss how this principle can be used in a quantitative way to determine the most probable value of $\\Omega$. I also comment on recent work by Hawking and Turok on quantum creation of open universes from nothing.'],['1998-05-20'] +1576,['eng'],"['Burrows, A', 'Sawyer, R F']",['Many-Body Corrections to Charged-Current Neutrino Absorption Rates in Nuclear Matter'],['Astrophysics and Astronomy'],"['neutrino nucleon, interaction', 'charged current', 'nuclear matter', 'many-body problem, correction', 'nucleon nucleon, correlation', 'fermion, statistics', 'nuclear force', 'neutrino, path length', 'differential cross section', 'energy, momentum transfer', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804264'],"['Including nucleon--nucleon correlations due to both Fermi statistics and nuclear forces, we have developed a general formalism for calculating the charged--current neutrino--nucleon absorption rates in nuclear matter. We find that at one half nuclear density many--body effects alone suppress the rates by a factor of two and that the suppression factors increase to $\\sim$5 at $4\\times10^{14}$ g cm$^{-3}$. The associated increase in the neutrino--matter mean--free--paths parallels that found for neutral--current interactions and opens up interesting possibilities in the context of the delayed supernova mechanism and protoneutron star cooling.']",['1998-04-27'] +1577,['eng'],"['Hannestad, S', 'Raffelt, G G']",['Imprint of Sterile Neutrinos in the Cosmic Microwave Background Radiation'],['Astrophysics and Astronomy'],"['neutrino, sterile', 'neutrino, solar', 'neutrino, cosmic radiation', 'cosmic radiation, background', 'spectra, fluctuation', 'astrophysics, missing-mass', 'flavor, 4', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805223'],"['The existence of low-mass sterile neutrinos is suggested by the current status of solar and atmospheric neutrinos together with the LSND experiment. In typical four-flavor scenarios, neutrinos would contribute to a cosmic hot dark matter component and to an increased radiation content at the epoch of matter-radiation equality. These effects leave their imprint in sky maps of the cosmic microwave background radiation (CMBR) and may thus be detectable with the precision measurements of the upcoming MAP and PLANCK missions.']",['1998-05-19'] +1578,['eng'],"['Andersson, N', 'Kokkotas, K D', 'Schutz, B F']",['Gravitational radiation limit on the spin of young neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'spin, upper limit', 'gravitational radiation, effect', 'perturbation, linear', 'matter, stability', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805225'],"[""A newly discovered instability in rotating neutron stars, driven by gravitational radiation reaction acting on the stars' $r$-modes, is shown here to set an upper limit on the spin rate of young neutron stars. We calculate the timescales for growth of linear perturbations due to gravitational radiation reaction, and for dissipation by shear and bulk viscosity, working to second order in a slow-rotation expansion within a Newtonian polytropic stellar model. The results are very temperature-sensitive: in hot neutron stars ($T>10^9$ K), the lowest-order $r$-modes are unstable, while in colder stars they are damped by viscosity. These calculations have a number of interesting astrophysical implications. First, the $r$-mode instability will spin down a newly born neutron star to a period close to the initial period inferred for the Crab pulsar, probably between 10 and 20 ms. Second, as an initially rapidly rotating star star spins down, an energy equivalent to roughly 1% of a solar mass is radiated as gravitational waves, which makes the process an interesting source for detectable gravitational waves. Third, the $r$-mode instability rules out the scenario whereby millisecond pulsars are formed by accretion-induced collapse of a white dwarf: the new star would be hot enough to spin down to much slower rates.""]",['1998-05-19'] +1579,['eng'],"['Magnussen, N']",['Selected Results from Ground-Based Cosmic Ray and $\\gamma$-Ray Experiments'],['Astrophysics and Astronomy'],"['talk, Hirschegg 1998/01/11', 'photon, cosmic radiation', 'elements, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805165'],['Selected results from the HEGRA experiment on charged Cosmic Rays and on very high energy gamma-rays are presented. The MAGIC Telescope is presented as an outlook to the future of Gamma-Ray astronomy.'],['1998-05-14'] +1580,['eng'],"['Bahcall, J N', 'Basu, S', 'Pinsonneault, M H']",['How Uncertain Are Solar Neutrino Predictions?'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'fusion', 'model, solar', 'velocity, acoustic', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805135'],['Solar neutrino fluxes and sound speeds are calculated using a systematic reevaluation of nuclear fusion rates. The largest uncertainties are identified and their effects on the solar neutrino fluxes are estimated.'],['1998-05-12'] +1581,['eng'],"['Blasi, P', 'Colafrancesco, Sergio']",['High Energy Phenomena in Clusters of Galaxies'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'astrophysics', 'galaxy, cluster', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'energy, density', 'electron, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9805109'],"['Several phenomena in high energy astrophysics have been recently related to clusters of galaxies and to cosmic ray interactions occurring inside these structures. In many of these phenomena the observable effects depend on the energy density of cosmic rays confined in the Intra Cluster (IC) medium, which is a poorly known quantity. We propose here that useful indications about this quantity can be obtained from present and future observations of galaxy clusters in the radio and hard X-ray frequency ranges.']",['1998-05-11'] +1582,['eng'],"['Bernardeau, F']","[""Cosmologie, la formation des grandes structures de l'Univers""]",['Astrophysics and Astronomy'],"['astrophysics, model', 'relativity theory, general', 'Einstein equation', 'thermodynamics', 'inflationary universe', 'field theory, space-time', 'fluctuation', 'gravitation', 'astrophysics, missing-mass', 'field equations, Liouville', 'field equations, nonlinear', 'perturbation theory', 'cumulant expansion', 'matter, density', 'astrophysics, galaxy', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804230'],"[""Sujets qui sont plus particulierement abordes dans ce cours: 1. Elements de cosmologie, l'Univers homogene Les principes cosmologiques et leurs verifications observationnelles Histoire thermique de l'Univers Inflation, motivations et principe de base 2. Elements de cosmologie, l'Univers inhomogene La croissance des fluctuations Pourquoi un modele avec de la Matiere Noire Froide ? Evidences de l'existence de matiere noire 3. La dynamique gravitationnelle, les theories lineaires L'approximation Newtonnienne avec un seul flot Description Eulerienne ou description Lagrangienne Vers la dynamique non-lineaire: l'effondrement spherique 4. Le regime quasilineaire Effet du couplage de mode: la skewness La hierarchie des correlations en regimes quasi-lineaire Les termes sous-dominants du developpement perturbatif 5. Application aux proprietes statistiques des champs de distorsions gravitationnelles La relation entre convergence locale et densite projetee Variance et skewness de la convergence locale 6. Vers le regime fortement non-lineaire Les solutions auto-similaires et les modeles hierarchiques Distribution de matiere et distribution de lumiere""]",['1998-04-23'] +1583,['eng'],"['Frampton, Paul H']",['Highest Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Boston 1998/03/22', 'cosmic radiation, primary', 'p, cosmic radiation', 'particle, heavy', 'particle, decay', 'grand unified theory, SU(15)', 'model, composite']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804219'],"['It is proposed that the highest energy $\\sim 10^{20}$eV cosmic ray primaries are protons, decay products of a long-lived progenitor whose high kinetic energy arises from decay of a distant (cosmological) superheavy particle, G. Such a scenario can occur in e.g. SU(15) grand unification and in some preon models, but is more generic; if true, these unusual cosmic rays provide a window into new physics.']",['1998-04-23'] +1584,['eng'],"['Armstrong, P', 'Chadwick, P M', 'Cottle, P J', 'Dickinson, J E', 'Dickinson, M R', 'Dipper, N A', 'Hilton, S E', 'Hogg, W R', 'Holder, J', 'Kendall, T R', 'McComb, T J L', 'Moore, C M', 'Orford, K J', 'Rayner, S M', 'Roberts, I D', 'Roberts, M D', 'Robertshaw, M', 'Shaw, S E', 'Tindale, K', 'Tummey, S P', 'Turver, K E']",['The University of Durham Mark 6 $\\gamma$ Ray Telescope'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'Cherenkov counter, air', 'optics, reflection', 'photoelectron, amplifier', 'semiconductor, optical', 'electronics', 'performance']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804212'],"[""The design, construction and operation of the University of Durham ground-based gamma ray telescope is discussed. The telescope has been designed to detect gamma rays in the < 200 GeV region and to achieve good discrimination between gamma ray and hadron initiated showers in the higher energy region (> 300 GeV). The telescope was commissioned in 1995 and a description of its design and operation is presented, together with a verification of the telescope's performance""]",['1998-04-22'] +1585,['eng'],"['Xu, R X', 'Qiao, G J']",['A Strange Star Model for Pulsars'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'matter, strangeness', 'n, matter', 'sphere, magnetic', 'photon, cosmic radiation', 'photon, emission', 'binding energy', 'electric field', 'charge, density', 'quark, matter', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804278'],"[""It is suggested in this paper that the `bare' strange star might be not bare, and there could be a magnetosphere around it. As a strange star might be an intensely magnetized rotator, the induced unipolar electric field would be large enough to construct a magnetosphere around the strange matter core. This kind of magnetosphere is very similar to that of the rotating magnetized neutron stars discussed by many authors. A magnetosphere will be established very soon through pair production by gamma-B or two photon processes after a strange star was born in a supernova explosion. It is emphasized that the fact that the strange star surface can not supply charged particles does not stop the formation of a space charge separated magnetosphere around the bare strange star. An accretion crust is quite difficult to come into being around an isolated strange star. Therefore the observed radio signals of an rotation-powered pulsar may come from a bare strange stars rather than a neutron stars or a strange star with an accretion crust. The idea, that the radio pulsars are the strange stars without crusts, is supported by some observations. The fact, that the iron emission lines have been observed in many X-ray pulsars but never been reported in X-ray emission of radio pulsars, is difficult to be understood if the radio pulsars are the neutron stars or strange star with crust where the surface binding energy of iron ions is too low to avoid a ion free-flow from the surface.""]",['1998-04-28'] +1586,['eng'],"['Potekhin, A Yu', 'Ivanchik, A V', 'Varshalovich, D A', 'Lanzetta, K M', 'Baldwin, J A', 'Williger, G M', 'Carswell, R F']",['Testing cosmological variability of the proton-to-electron mass ratio using the spectrum of PKS 0528-250'],['Astrophysics and Astronomy'],"['astrophysics, quasar', 'space-time, higher-dimensional', 'fundamental constant, time variation', 'mass ratio, (p electron)', 'spectra, moment', 'hydrogen, molecule', 'hydrogen, absorption', 'data analysis method', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804116'],"['Multidimensional cosmologies allow for variations of fundamental physical constants over the course of cosmological evolution, and different versions of the theories predict different time dependences. In particular, such variations could manifest themselves as changes of the proton-to-electron mass ratio high-redshift QSO spectra. Here we analyze a new, high-resolution spectrum of the z=2.81080 molecular hydrogen absorption system toward the quasar PKS 0528-250 to derive a new observational constraint to the time-averaged variation rate of the proton-to-electron mass ratio. We find |\\dot{\\mu} / \\mu| < 1.5 \\times 10^{-14}/year, which is much tighter than previously measured limits.']",['1998-04-14'] +1587,['eng'],"['Suh, I S', 'Lee, C H']",['Axion Emissivity from the Conversion of a Neutron Star into a Strange Star'],['Astrophysics and Astronomy'],"['n, matter', 'matter, strangeness', 'weak interaction, hadronic', 'energy loss', 'axion, emission', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804091'],"['The conversion of neutron matter into strange matter in a neutron star occurs through the non-leptonic weak-interaction process. We study the energy loss of the neutron star by the emission of axions in that process. Owing to that process, the neutron star will liberate the energy which can in no way be negligible as an axion burst.']",['1998-04-09'] +1588,['eng'],"['Bildsten, L']",['Gravitational Radiation and Rotation of Accreting Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'rotational', 'angular momentum', 'gravitational radiation, measurement', 'electron, capture', 'temperature, asymmetry', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804325'],"['Recent discoveries by the Rossi X-Ray Timing Explorer indicate that most of the rapidly accreting and weakly magnetic neutron stars in the Galaxy are rotating at spin frequencies greater than 250 Hz. Remarkably, they all rotate in a narrow range of frequencies. I suggest that these stars rotate fast enough so that, on average, the angular momentum added by accretion is lost to gravitational radiation. The strong spin frequency dependence of the angular momentum loss rate from gravitational radiation then provides a natural reason for similar spin frequencies. Provided that the interior temperature has a large scale asymmetry misaligned from the spin axis, then the temperature sensitive electron captures in the deep crust can provide the quadrupole needed to reach this limiting situation at 300 Hz. This quadrupole is only present during accretion and makes it difficult to form radio pulsars spinning more rapidly than 600-800 Hz via rapid accretion. The gravity wave strength is <10^{-26} from most neutron stars and >2 X 10^{-26} for Sco X-1. Prior knowledge of the position, spin frequency and orbital periods will allow for deep searches for these periodic signals with gravitational wave interferometers (LIGO, VIRGO and the dual-recycled GEO 600 detector) and experimenters need to take such sources into account. Sco X-1 will most likely be detected first.']",['1998-04-30'] +1589,['eng'],"['Wichoski, U F', 'MacGibbon, J H', 'Brandenberger, R H']",['Astrophysical Constraints on Primordial Black Hole Formation from Collapsing Cosmic Strings'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1998/02/18', 'black hole, production', 'astrophysics, string', 'mass spectrum', 'scaling', 'cosmic radiation, flux', 'photon, cosmic radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804341'],['Primordial Black Holes (PBH) may have formed from the collapse of cosmic string loops. The spectral shape of the PBH mass spectrum can be determined by the scaling argument for string networks. Limits on the spectral amplitude derived from extragalactic gamma-ray and galactic gamma-ray and cosmic ray flux observations as well as constraints from the possible formation of stable black holes remnants are reanalyzed. The new constraints are remarkably close to those derived from the normalization of the cosmic string model to the cosmic microwave background anisotropies.'],['1998-05-01'] +1590,['eng'],"['Cohn, J D']",['Fluctuations in the Hawking Turok model'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'gravitational radiation, fluctuation', 'cosmic radiation, background', 'perturbation, scalar', 'tunneling', 'background, instanton']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804289'],['Scalar and gravity wave subcurvature fluctuations are calculated for a background approximating the Hawking and Turok open universe model. The gravity wave cosmic microwave background contribution is finite and it appears that a normalizable scalar supercurvature mode is possible in some regions of parameter space.'],['1998-04-28'] +1591,['eng'],"['Freese, Katherine', 'Krasteva, E']",['A Bound on the Flux of Magnetic Monopoles from Catalysis of Nucleon Decay in White Dwarfs'],['Astrophysics and Astronomy'],"['astrophysics, white dwarf', 'nucleon, decay', 'Rubakov effect', 'flux, magnetic monopole', 'upper limit', 'mass, dependence', 'n, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804148'],"['Catalysis of nucleon decay in white dwarfs is used to constrain the abundance of magnetic monopoles arising from Grand Unified Theories. Recent discoveries of the dimmest white dwarf ever observed, WD 1136-286 with $L = 10^{-4.94} L_{\\odot}$, place limits on the monopole flux. An abundance of monopoles greater than the new bound would heat this star to a luminosity higher than what is observed. The new bound is $(F/$cm $^{-2}$ s$^{-1}$ sr$^{-1}$) $(\\sigma monopoles captured by the main-sequence progenitor of the white dwarf: $(F/$cm $^{-2}$ s$^{-1}$ sr$^{-1}$) $(\\sigma \\upsilon /10^{-28} cm^2) < 3.5(26) \\times 10^{-21}$ for $10^{17}$ ($10^{16}$) GeV monopoles. We also note that the dependence on monopole mass of flux bounds due to catalysis in neutron stars with main sequence accretion has previously been calculated incorrectly (previously the bound has been stated as $F (\\sigma \\upsilon/10^{-28} cm^2) < 10^{-28} $ cm $^{-2}$ s$^{-1}$ sr$^{-1}$). We show that the correct bounds are somewhat weaker for monopole mass other than $10^{17}$ GeV.']",['1998-04-16'] +1592,['eng'],"['Kusenko, A']",['Resonant production of $\\gamma$ rays in jolted cold neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'shock waves, acoustic', 'photon, cosmic radiation', 'critical phenomena, superconducting', 'p, condensation', 'oscillation, coherence', 'photon, production', 'resonance, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804134'],"['Acoustic shock waves passing through colliding cold neutron stars can cause repetitive superconducting phase transitions in which the proton condensate relaxes to its equilibrium value via coherent oscillations. As a result, a resonant non-thermal production of gamma rays in the MeV energy range with power up to 10^(52) erg/s can take place during the short period of time before the nuclear matter is heated by the shock waves.']",['1998-04-15'] +1593,['eng'],"['Fornengo, N']",['Supersymmetric candidates for dark matter'],['Astrophysics and Astronomy'],"['talk, Trieste 1997/12/15', 'astrophysics, missing-mass', 'electroweak interaction', 'supersymmetry', 'neutralino, search for', 'scattering, neutralino nucleon', 'neutralino, annihilation', 'signal processing', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804295'],['Direct and indirect detection rates of relic neutralinos are reviewed in the framework of the Minimal Supersymmetric Standard Model. The theoretical estimates are compared with the most recent experimental limits from low-background detectors and neutrino telescopes. The properties of neutralino under the hypothesis that preliminary experimental results of the DAMA/NaI Collaboration may be indicative of a yearly modulation effect are examined.'],['1998-04-29'] +1594,['eng'],"['Challinor, A D', 'Lasenby, A N']",['Cosmic microwave background anisotropies in the CDM model'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'invariance, gauge', 'Boltzmann equation', 'astrophysics, missing-mass', 'temperature, anisotropy', 'perturbation, scalar', 'perturbation, adiabatic', 'boundary condition', 'space-time, Robertson-Walker', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804301'],"['We present a fully covariant and gauge-invariant calculation of the evolution of anisotropies in the Cosmic Microwave Background (CMB) radiation. We use the physically appealing covariant approach to cosmological perturbations, which ensures that all variables are gauge-invariant and have a clear physical interpretation. We derive the complete set of frame-independent linearised equations describing the (Boltzmann) evolution of anisotropy and inhomogeneity in an almost Friedmann-Robertson-Walker (FRW) Cold Dark Matter (CDM) universe. These equations include the contributions of scalar, vector and tensor modes in a unified manner. Frame-independent equations describing scalar perturbations, which are valid for any value of the background curvature, are obtained by placing appropriate covariant restrictions on the gauge-invariant variables. We derive the analytic solution of these equations in the early radiation dominated universe, and present the results of a numerical simulation of the standard CDM model. Our results confirm those obtained by other groups, who have worked carefully with non-covariant methods in specific gauges, but are derived here in a completely transparent fashion.']",['1998-04-29'] +1595,['eng'],"['Li, L X', 'Gott, J R']",['Inflation in Kaluza-Klein Theory'],['Astrophysics and Astronomy'],"['Kaluza-Klein model', 'dimension, 5', 'inflationary universe', 'energy', 'fundamental constant, fine structure', 'astrophysics, fundamental constant', 'astrophysics, wave function', 'tunneling', 'effect, Casimir', 'Einstein equation, solution', 'space-time, de Sitter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804311'],"['In this paper we investigate a model of an inflationary universe in Kaluza-Klein theory, which is a four-dimensional de Sitter space plus a one-dimensional compactified internal space. We find that the energy scale for inflation can be predicted from the fine-structure constant in a self-consistent solution of the semi-classical Einstein equations including the Casimir effect. From the observed value of the fine-structure constant, we obtain an energy scale for inflation of $\\epsilon=1.84\\times 10^{16}g_*^{1/4}$ Gev, where $g_*$ is a dimensionless number depending on the spin and number of matter fields existing in the universe. This value is consistent with the values often discussed for inflation and grand unification. The wave function for this model predicts a high probability for forming such universes, independent of the value of the cosmological constant. The tunneling probability favors the creation of inflationary universes with a compactified dimension, over those with all macroscopic dimensions.']",['1998-04-29'] +1596,['eng'],"['Bhat, C M', 'Bhat, P C', 'Paterno, M', 'Prosper, H B']",['Study of the Solar Neutrino Survival Probability'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'neutrino, energy', 'model, solar', 'neutrino, oscillation', 'deep underground detector', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804252'],"['We present a study of the recent solar neutrino data using a Bayesian approach. The survival probability for neutrinos as a function of the energy has been extracted by two independent methods. The results of our analysis, assuming that only electron neutrinos are observed in the Super-Kamiokande experiment, show a distinct supression of the survival probability at about 1 MeV, in good agreement with previous chi-square-based analyses. When the detection of muon neutrinos by Super-Kamiokande is taken into account, assuming electron neutrino to muon neutrino oscillations, we find a significant suppression in survival probability at about 8.5 MeV.']",['1998-04-27'] +1597,['eng'],"['Wells, J D']",['Astrophysical search strategies for accelerator blind dark matter'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1998/02/18', 'astrophysics, missing-mass', 'search for, missing-mass', 'supersymmetry', 'supergravity', 'LSP, annihilation', 'quark, truth', 'quark, pair production', 'photon, pair production', 'Higgsino, LSP']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9808052'],"['A weakly interacting dark-matter particle may be difficult to discover at an accelerator because it either (1) is too massive, (2) has no standard-model gauge interactions, or (3) is almost degenerate with other states. In each of these cases, searches for annihilation products in the Galactic halo are useful probes of dark-matter properties. Using the example of supersymmetric dark matter, I discuss how astrophysical searches for dark matter may provide discovery and mass information inaccessible to collider physics programs such as the Tevatron and LHC.']",['1998-08-07'] +1598,['eng'],"['Liddle, A R', 'Mazumdar, A', 'Schunck, F E']",['Assisted inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'potential', 'density, perturbation', 'spectra, perturbation', 'scaling']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804177'],"['In inflationary scenarios with more than one scalar field, inflation may proceed even if each of the individual fields has a potential too steep for that field to sustain inflation on its own. We show that scalar fields with exponential potentials evolve so as to act cooperatively to assist inflation, by finding solutions in which the energy densities of the different scalar fields evolve in fixed proportion. Such scaling solutions exist for an arbitrary number of scalar fields, with different slopes for the exponential potentials, and we show that these solutions are the unique late-time attractors for the evolution. We determine the density perturbation spectrum produced by such a period of inflation, and show that with multiple scalar fields the spectrum is closer to the scale-invariant than the spectrum that any of the fields would generate individually.']",['1998-04-20'] +1599,['eng'],"['López-Suarez, J', 'Canal, R']",['Inhomogeneous big bang nucleosynthesis with late-decaying massive particles'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'baryon, density', 'nucleon, diffusion', 'postulated particle, decay', 'energy, density', 'entropy', 'astrophysics, missing-mass', 'nucleus nucleus, nuclear reaction', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804235'],"['We investigate the possibility of accounting for the currently inferred primordial abundances of D, 3He, 4He, and 7Li by big bang nucleosynthesis in the presence of baryon density inhomogeneities plus the effects of late-decaying massive particles (X), and we explore the allowed range of baryonic fraction of the closure density Omega_b in such context. We find that, depending on the parameters of this composite model (characteristic size and density contrast of the inhomogeneities; mass-density, lifetime, and effective baryon number in the decay of the X-particles), values as high as abundances of the light nuclides. We include diffusion of neutrons and protons at all stages, and we consider the contribution of the X particles to the energy density, the entropy production by their decay, the possibility that the X-products could photodissociate the light nuclei produced during the previous stages of nucleosynthesis, and also the possibility that the decay products of the X-particles would include a substantial fraction of hadrons. Specific predictions for the primordial abundance of Be are made.']",['1998-04-23'] +1600,['eng'],"['Chadwick, P M', 'Dickinson, M R', 'Dipper, N A', 'Holder, J', 'Kendall, T R', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Roberts, I D', 'Shaw, S E', 'Turver, K E']",['TeV gamma rays from PSR 1706-44'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, pulsar', 'cosmic radiation, time variation', 'cosmic radiation, energy', 'Cherenkov counter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804224'],"['Observations made with the University of Durham Mark 6 atmospheric Cerenkov telescope confirm that PSR B1706-44 is a very high energy gamma-ray emitter. There is no indication from our dataset that the very high energy gamma-rays are pulsed, in contrast to the findings at < 20 GeV, which indicate that more than 80% of the flux is pulsed. The flux at E > 300 GeV is estimated to be (3.9 +/- 0.7 (statistical)) x 10^-11 cm^-2 s^-1.']",['1998-04-23'] +1601,['eng'],"['Stecker, F W', 'De Jager, O C']",['Absorption of Very High Energy $\\gamma$-Rays by Intergalactic Infrared Radiation'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'photon, energy spectrum', 'photon, absorption', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804196'],"['We present a new calculation of the intergalactic gamma-ray absorption coefficient as a function of both energy and redshift. In reexamining this problem, we make use of a new, empirically based calculation (as opposed to previous model calculations) of the intergalactic infrared radiation field. We find smaller opacities than those given previously (Stecker & De Jager 1997). We apply our results to the new observations of the flaring gamma-ray spectra of Mrk421 and Mrk501, both at a redshift of apx. 0.03. Our new calculations indicate that there should be no significant curvature in the spectra of these sources for energies below 10 TeV, as indicated by recent observations. However, the intrinsic spectra of these sources should be harder by apx. 0.2 to 0.45 in the spectral index in the 1 to 10 TeV range with an intergalactic absorption cutoff above apx. 20 TeV.']",['1998-04-21'] +1602,['eng'],"['Challinor, A D', 'Lasenby, A N']",['A covariant and gauge-invariant analysis of cosmic microwave background anisotropies from scalar perturbations'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'temperature, anisotropy', 'perturbation, scalar', 'invariance, gauge', 'Boltzmann equation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804150'],"['We present a new, fully covariant and manifestly gauge-invariant expression for the temperature anisotropy in the cosmic microwave background radiation resulting from scalar perturbations. We pay particular attention to gauge issues such as the definition of the temperature perturbation and the placing of the last scattering surface. In the instantaneous recombination approximation, the expression may be integrated up to a Rees-Sciama term for arbitrary matter descriptions in flat, open and closed universes. We discuss the interpretation of our result in the baryon-dominated limit using numerical solutions for conditions on the last scattering surface, and confirm that for adiabatic perturbations the dominant contribution to the anisotropy on intermediate scales (the location of the Doppler peaks) may be understood in terms of the spatial inhomogeneity of the radiation temperature in the baryon rest frame. Finally, we show how this term enters the usual Sachs-Wolfe type calculations (it is rarely seen in such analyses) when subtle gauge effects at the last scattering surface are treated correctly.']",['1998-04-17'] +1603,['eng'],"['Kajino, T', 'Orito, M']",['Neutrinos and Big-Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'helium, nuclide', 'neutrino', 'lepton, asymmetry', 'deuterium, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804170'],['Observations of clusters and super clusters of galaxies have indicated that the Universe is more dominated by baryons than ever estimated in the homogeneous cosmological model for primordial nucleosynthesis. Recent detections of possibly low deuterium abundance in Lyman-$\\alpha$ clouds along the line of sight to high red-shift quasars have raised another potential difficulty that \\he4 is overproduced in any cosmological models which satisfy the low deuterium abundance constraint. We show that the inhomogeneous cosmological model with degenerate electron-neutrino can resolve these two difficulties.'],['1998-04-20'] +1604,['eng'],"['Park, T S', 'Kubodera, K', 'Min, D P', 'Rho, M']",['The Solar Proton Burning Process Revisited In Chiral Perturbation Theory'],['Astrophysics and Astronomy'],"['matter, solar', 'nucleus nucleus, nuclear reaction', 'p p, fusion', 'perturbation theory, chiral', 'effective Lagrangian', 'wave function', 'charged current', 'neutral current', 'channel cross section, energy dependence', 'numerical calculations, interpretation of experiments', 'p p --> deuteron positron neutrino/e']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804144'],"['The proton burning process p + p -> d + e(+) + \\nu(e), important for the stellar evolution of main-sequence stars of mass equal to or less than that of the Sun, is computed in effective field theory using chiral perturbation expansion to the next-to-next-to leading chiral order. This represents a model-independent calculation consistent with low-energy effective theory of QCD comparable in accuracy to the radiative np capture at thermal energy previously calculated by first using very accurate two-nucleon wavefunctions backed up by an effective field theory technique with a finite cut-off. The result obtained thereby is found to support within theoretical uncertainties the previous calculation of the same process by Bahcall and his co-workers.']",['1998-04-16'] +1605,['eng'],"['Ruffert, M', 'Janka, H T']",['Colliding neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'scattering', 'model, hydrodynamical', 'dimension, 3', 'gravitational radiation, emission', 'back reaction', 'neutrino, emission', 'luminosity', 'photon, cosmic radiation', 'neutrino antineutrino, annihilation', 'thermodynamics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804132'],"['Three-dimensional hydrodynamical simulations are presented for the direct head-on or off-center collision of two neutron stars, employing a basically Newtonian PPM code but including the emission of gravitational waves and their back-reaction on the hydrodynamical flow. A physical nuclear equation of state is used that allows us to follow the thermodynamical evolution of the stellar matter and to compute the emission of neutrinos. Predicted gravitational wave signals, luminosities and waveforms, are presented. The models are evaluated for their implications for gamma-ray burst scenarios. We find an extremely luminous outburst of neutrinos with a peak luminosity of more than 4E54 erg/s for several milliseconds. This leads to an efficiency of about 1% for the annihilation of neutrinos with antineutrinos, corresponding to an average energy deposition rate of more than 1E52 erg/s and a total energy of about 1E50 erg deposited in electron-positron pairs around the collision site within 10ms. Although these numbers seem very favorable for gamma-ray burst scenarios, the pollution of the $e^\\pm$ pair-plasma cloud with nearly 0.1$M_{\\odot}$ of dynamically ejected baryons is 5 orders of magnitude too large. Therefore the formation of a relativistically expanding fireball that leads to a gamma-ray burst powered by neutrino emission from colliding neutron stars is definitely ruled out.']",['1998-04-15'] +1606,['eng'],"['Le Bohec, S', 'Degrange, B', 'Punch, M', 'Barrau, A', 'Bazer-Bachi, R', 'Cabot, H', 'Chounet, L M', 'Debiais, G', 'Dezalay, J P', 'Djannati-Ataï, A', 'Dumora, D', 'Espigat, P', 'Fabre, B', 'Fleury, P', 'Fontaine, G', 'George, R', 'Ghesquière, C', 'Goret, P', 'Gouiffes, C', 'Grenier, I A', 'Iacoucci, L', 'Malet, I', 'Meynadier, C', 'Munz, F', 'Palfrey, T A', 'Paré, E', 'Pons, Y', 'Québert, J', 'Ragan, K', 'Renault, C', 'Rivoal, M', 'Rob, L', 'Schovanek, P', 'Smith, D', 'Tavernet, J P', 'Vrana, J']",['A new analysis method for very high definition Imaging Atmospheric Cherenkov Telescopes as applied to the CAT telescope'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'Cherenkov counter, imaging', 'Cherenkov counter, air', 'showers, spectra', 'angular dependence', 'energy resolution']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804133'],"['A new method of shower-image analysis is presented which appears very powerful as applied to those Cherenkov Imaging Telescopes with very high definition imaging capability. It provides hadron rejection on the basis of a single cut on the image shape, and simultaneously determines the energy of the electromagnetic shower and the position of the shower axis with respect to the detector. The source location is also reconstructed for each individual gamma-ray shower, even with one single telescope, so for a point source the hadron rejection can be further improved. As an example, this new method is applied to data from the CAT (Cherenkov Array at Themis) imaging telescope, which has been operational since Autumn, 1996.']",['1998-04-15'] +1607,['eng'],"['Bottino, A', 'Donato, F', 'Fornengo, N', 'Salati, Pierre']",['Which fraction of the measured cosmic-ray antiprotons might be due to neutralino annihilation in the galactic halo?'],['Astrophysics and Astronomy'],"['anti-p, cosmic radiation', 'energy spectrum, cosmic radiation', 'cosmic radiation, flux', 'neutralino, annihilation', 'anti-p, production', 'astrophysics, galaxy', 'astrophysics, missing-mass', 'electron positron, annihilation', 'anti-p, production', 'sparticle, search for', 'model, solar', 'time dependence', 'mass, neutralino', 'neutralino, density', 'correlation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804137'],"['We analyze the data of low-energy cosmic-ray antiproton spectrum, recently published by the BESS Collaboration, in terms of newly calculated fluxes for secondary antiprotons and for a possible contribution of an exotic signal due to neutralino annihilation in the galactic halo. We single out the relevant supersymmetric configurations and discuss their explorability with experiments of direct search for particle dark matter and at accelerators. We discuss how future measurements with the Alpha Magnetic Spectrometer (AMS) on the Shuttle flight may disentangle the possible neutralino-induced contribution from the secondary one.']",['1998-04-15'] +1608,['eng'],"['Rezania, V', 'Sobuti, Y']","[""Integrals and static solutions of general relativistic Liouville's equation in post Newtonian approximation""]",['Astrophysics and Astronomy'],"['relativity theory, general', 'field equations, Liouville', 'field equations, solution', 'energy', 'angular momentum', 'space-time, oscillation', 'model, hydrodynamical']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804120'],"[""The post-Newtonian approximation of general relativistic Liouville's equation is presented. Two integrals of it, generalizations of the classical energy and angular momentum, are obtained. Polytropic models are constructed as an application.""]",['1998-04-14'] +1609,['eng'],"['Hayashida, N']",['Observations of TeV gamma ray flares from Markarian 501 with the Telescope Array Prototype'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation', 'Cherenkov counter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804043'],"['We will report the observations of TeV gamma ray flares from Markarian 501 using Telescope Array Prototype. The observation were carried out continuously from the end of March to the end of July in 1997. The energy spectrum, and the time variation of the gamma ray intensities are shown. The intensity has been changed by the order of magnitude in this period and the possible quasi periodic oscillation of 12.7days were discovered.']",['1998-04-07'] +1610,['eng'],"['Giebels, B', 'Bazer-Bachi, R', 'Bergeret, H', 'Cordier, A', 'Debiais, G', 'De Naurois, M', 'Dezalay, J P', 'Dumora, D', 'Eschstruth, P T', 'Espigat, P', 'Fabre, B', 'Fleury, P', 'Ghesquière, C', 'Herault, N', 'Malet, I', 'Merkel, B', 'Meynadier, C', 'Palatka, M', 'Paré, E', 'Procureur, J', 'Punch, M', 'Québert, J', 'Ragan, K', 'Rob, L', 'Schovanek, P', 'Smith, D A', 'Vrana, J']",['Prototype Tests for the CELESTE Solar Array $\\gamma$-Ray Telescope'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'Cherenkov counter, air', 'optics, reflection', 'photoelectron, amplifier', 'trigger', 'background', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803198'],"['The CELESTE experiment will be an Atmospheric Cherenkov detector designed to bridge the gap in energy sensitivity between current satellite and ground-based gamma-ray telescopes, 20 to 300 GeV. We present test results made at the former solar power plant, Themis, in the French Pyrenees. The tests confirm the viability of using a central tower heliostat array for Cherenkov wavefront sampling.']",['1998-03-18'] +1611,['eng'],"['Messer, O E B', 'Mezzacappa, A', 'Bruenn, S W', 'Guidry, M W']",['Neutrino-driven supernovae'],['Astrophysics and Astronomy'],"['talk, Oak Ridge 1997/12/02', 'astrophysics', 'supernova', 'neutrino, diffusion', 'neutrino, flux', 'transport theory', 'neutrino, luminosity', 'Boltzmann equation', 'neutrino, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804080'],"['Core-collapse supernovae are, despite their spectacular visual display, neutrino events. Virtually all of the 10^53 ergs of gravitational binding energy released in the formation of the nascent neutron star is carried away in the form of neutrinos and antineutrinos of all three flavors, and these neutrinos are primarily responsible for powering the explosion. This mechanism depends sensitively on the neutrino transport between the neutrinospheres and the shock. In light of this, we have performed a comparison of multigroup Boltzmann neutrino transport (MGBT) and multigroup flux-limited diffusion (MGFLD) in post-core bounce environments. Differences in the mean inverse flux factors, luminosities, and RMS energies translate to heating rates that are up to 2 times larger for Boltzmann transport, with net cooling rates below the gain radius that are typically 0.8 times the MGFLD rates. These differences are greatest at earlier postbounce times for a given progenitor mass, and for a given postbounce time, greater for greater progenitor mass. The increased differences with increased progenitor mass suggest that the net heating enhancement from MGBT is potentially robust and self-regulated.']",['1998-04-08'] +1612,['eng'],"['Hannestad, S']",['Constraining neutrino decays with CMBR data'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, background', 'neutrino/tau, decay', 'neutrino, mass', 'neutrino, lifetime', 'neutrino, massless', 'neutrino, flavor', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804075'],['The decay of massive neutrinos to final states containing only invisible particles is poorly constrained experimentally. In this letter we describe the constraints that can be put on neutrino mass and lifetime using CMBR measurements. We find that very tight lifetime limits on neutrinos in the mass range 10 eV - 100 keV can be derived using CMBR data from upcoming satellite measurements.'],['1998-04-08'] +1613,['eng'],"['Hannestad, S']",['Decay-Produced Neutrino Hot Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutrino, heavy', 'neutrino, decay modes', 'neutrino, production', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'numerical calculations, interpretation of experiments', 'neutrino --> scalar particle neutrino']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804053'],"['We investigate different types of neutrino hot dark matter with respect to structure formation and anisotropies in the cosmic microwave background radiation (CMBR). The possibility of neutrino hot dark matter produced through the decay of a heavier neutrino by the process nu_H -> nu_L + phi, where phi is a scalar particle, is discussed in detail. This type of dark matter can possibly be distinguished observationally from the standard neutrino dark matter by using new CMBR data from the upcoming satellite missions MAP and PLANCK.']",['1998-04-07'] +1614,['eng'],"['Barrau, A', 'Bazer-Bachi, R', 'Beyer, E', 'Cabot, H', 'Cerutti, M', 'Chounet, L M', 'Debiais, G', 'Degrange, B', 'Delchini, H', 'Denance, J P', 'Descotes, G', 'Dezalay, J P', 'Djannati-Ataï, A', 'Dumora, D', 'Espigat, P', 'Fabre, B', 'Fleury, P', 'Fontaine, G', 'George, R', 'Ghesquière, C', 'Gilly, J', 'Goret, P', 'Gouiffes, C', 'Gouillaud, J C', 'Gregory, C', 'Grenier, I A', 'Iacoucci, L', 'Kalt, L', 'Le Bohec, S', 'Malet, I', 'Meynadier, C', 'Mols, J P', 'De Freitas, P M', 'Morano, R', 'Morinaud, G', 'Munz, F', 'Palatka, M', 'Palfrey, T A', 'Paré, E', 'Pons, Y', 'Punch, M', 'Québert, J', 'Ragan, K', 'Renault, C', 'Rivoal, M', 'Rob, L', 'Schovanek, P', 'Smith, D', 'Tabary, A', 'Tavernet, J P', 'Toussenel, F', 'Vrana, J']",['The CAT Imaging Telescope for Very-High-Energy Gamma-Ray Astronomy'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'Cherenkov counter, imaging', 'optics, reflection', 'photoelectron, amplifier', 'electronics', 'data acquisition', 'programming']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804046'],"['The CAT (Cherenkov Array at Themis) imaging telescope, equipped with a very-high-definition camera (546 fast phototubes with 0.12 degrees spacing surrounded by 54 larger tubes in two guard rings) started operation in Autumn 1996 on the site of the former solar plant Themis (France). Using the atmospheric Cherenkov technique, it detects and identifies very high energy gamma-rays in the range 250 GeV to a few tens of TeV. The instrument, which has detected three sources (Crab nebula, Mrk 421 and Mrk 501), is described in detail.']",['1998-04-07'] +1615,['eng'],"['Pen, U L']",['Topological Defects with Broken Scale Invariance'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1998/01/17', 'topology, defect', 'scaling, violation', 'temperature, cluster', 'galaxy', 'gravitation, coupling', 'astrophysics, fundamental constant', 'cosmic radiation, background', 'fluctuation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804083'],"['Defect models have recently been declared dead (Watson 1997), because they predict microwave background and matter fluctuations grossly out of line with what we see. In this talk we apply the fact that many defects are automatically destroyed at the time of radiation-matter transition, thus resurrecting the defects model. Moreover, the resurrected version predicts a cosmological constant, explains the apparent excess of hot clusters and the non-Gaussianity observed in galaxy surveys. If this model is correct, then the MAP and PLANCK missions will not measure what people expect them to (oscillations); rather, they will measure a broad hump.']",['1998-04-09'] +1616,['eng'],"['Suh, I S', 'Mathews, G J']",['Finite Temperature effects on baryon transport scattering in the early Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'electron hadron, interaction', 'total cross section, correction', 'finite temperature, effect', 'transport theory', 'electron, mass spectrum', 'baryon, diffusion', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804090'],"['We have computed finite temperature corrections to the electron-hadron scattering cross sections. These are based upon the renormalized electron mass and the modified density of states due to the presence of a background thermal bath. It is found that the electron-hadron thermal transport scattering cross section can be much larger than the zero temperature one. In the case of electron-neutron transport scattering, we find \\sigma_{ne}(T) / \\sigma_{ne} (T=0) \\simeq 5 at T \\simeq 0.1 MeV.']",['1998-04-09'] +1617,['eng'],"['Waxman, E']",['Can high energy neutrino annihilation on relic neutrinos generate the observed highest energy cosmic-rays?'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'neutrino, cosmic radiation', 'neutrino antineutrino, annihilation', 'astrophysics, model', 'astrophysics, galaxy', 'Z0, hadronic decay', 'cosmic radiation, flux', 'neutrino, background', 'neutrino, mass', 'neutrino, density', 'cosmic radiation, particle source', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804023'],"['Annihilation of high energy, $\\sim 10^{21}$eV, neutrinos on big bang relic neutrinos of $\\sim 1$eV mass, clustered in the Galactic halo or in a nearby galaxy cluster halo, has been suggested to generate, through hadronic Z decay, high energy nucleons and photons which may account for the detected flux of >10^{20}eV cosmic-rays. We show that the flux of high energy nucleons and photons produced by this process is dominated by annihilation on the uniform, non-clustered, neutrino background, and that the energy generation rate of 10^{21}eV neutrinos required to account for the detected flux of >10^{20}eV particles is >10^{48} erg/Mpc^3 yr. This energy generation rate, comparable to the total luminosity of the universe, is 4 orders of magnitude larger than the rate of production of high energy nucleons required to account for the flux of >10^{19}eV cosmic-rays. Thus, in order for neutrino annihilation to contribute significantly to the detected flux of >10^{20}eV cosmic-rays, the existence of a new class of high-energy neutrino sources, likely unrelated to the sources of >10^{19}eV cosmic-rays, must be invoked.']",['1998-04-03'] +1618,['eng'],"['Kinney, W H', 'Dodelson, S', 'Kolb, E W']",['Cosmic Microwave Background Observations as a Way to Discriminate Among Inflation Models'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1998/01/17', 'cosmic radiation, background', 'spectra, fluctuation', 'inflationary universe', 'parametrization', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9804034'],['The upcoming satellite missions MAP and Planck will measure the spectrum of fluctuations in the Cosmic Microwave Background with unprecedented accuracy. We discuss the prospect of using these observations to distinguish among proposed models of inflationary cosmology.'],['1998-04-06'] +1619,['eng'],"['Magueijo, J']",['Summary of GR15 session B.3 - Physics of the Early Universe'],['Astrophysics and Astronomy'],"['conference, review', 'inflationary universe', 'topology, defect', 'astrophysics, string', 'black hole']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803116'],"['Session B.3, on physics of the early Universe, of GR15 is briefly summarized.']",['1998-03-11'] +1620,['eng'],"['Ostrowski, M']",['Acceleration of UHE Cosmic Ray Particles at Relativistic Jets in Extragalactic Radio Sources'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, acceleration', 'astrophysics, jet', 'relativistic', 'model, shock waves', 'momentum spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803299'],"[""A mechanism of ultra-high energy cosmic ray acceleration in extragalactic radio sources, at the interface between the relativistic jet and the surrounding medium, is discussed as a supplement to the shock acceleration in `hot spots'. Due to crossing the tangential discontinuity of the velocity the particle can gain an amount of energy comparable to the energy gain at the shock crossing. However, the spectrum of particles accelerated at the jet side boundary is expected to be much flatter than the one formed at the shock. Due to this fact, particles accelerated at the boundary can dominate the overall spectrum at highest energies. In conditions characteristic to extragalactic jets' terminal shocks, the mechanism naturally provides the particles with E ~ 10^20 eV and complies with the efficiency requirements. The spectrum formation near the cut-off energy due to action of both the shock acceleration and the tangential discontinuity acceleration is modelled with the Monte Carlo particle simulations. It confirms that the upper energy limit can surpass the shock acceleration estimate.""]",['1998-03-26'] +1621,['eng'],"['Perivolaropoulos, L']",['Searching for Long Strings in CMB Maps'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'statistics', 'temperature, coherence', 'astrophysics, string', 'random field', 'numerical methods, Monte Carlo', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803292'],"['Using analytical methods and Monte Carlo simulations, we analyze new statistics designed to detect isolated step-like discontinuities which are coherent over large areas of Cosmic Microwave Background (CMB) pixel maps. Such coherent temperature discontinuities are predicted by the Kaiser-Stebbins effect to form due to long cosmic strings present in our present horizon. The background of the coherent step-like seed is assumed to be a scale invariant Gaussian random field which could have been produced by a superposition of seeds on smaller scales and/or by inflationary quantum fluctuations. We find that the proposed statistics can detect the presense of a coherent discontinuity at a sensitivity level almost an order of magnitude better compared to more conventional statistics like the skewness or the kurtosis.']",['1998-03-26'] +1622,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Blasi, P', 'Vilenkin, A']",['Ultra High Energy Gamma Rays as signature of Topological Defects'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'topology, defect', 'p, flux', 'photon, flux', 'showers, air', 'bound state, (2magnetic monopole)', 'superconducting, string', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803271'],"['We argue that due to various restrictions only necklaces and monopolonia survive as potential sources of ultra-high energy cosmic rays, among the topological defects studied so far. Other promising sources which are similar to topological defects are relic superheavy particles. All these sources have an excess of pions (and thus photons) over nucleons at production. We demonstrate that in the case of necklaces the diffuse proton flux can be larger than photon flux, while monopolonia and relic particles are concentrated in the Galactic halo, and the photon flux dominates. In all cases considered so far, including necklaces, photons must be present in ultra-high energy radiation observed from topological defects, and experimental discrimination between photon-induced and proton-induced extensive air showers can give a clue to the origin of ultra-high energy cosmic rays.']",['1998-03-24'] +1623,['eng'],"['Mannheim, K']",['Possible Production of High-Energy Gamma Rays from Proton Acceleration in the Extragalactic Radio Source Markarian 501'],['Astrophysics and Astronomy'],"['introductory', 'cosmic radiation, secondary radiation', 'p, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, acceleration', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803241'],"['The active galaxy Markarian 501 was discovered with air-Cerenkov telescopes at photon energies of 10 tera-electron volts. Such high energies may indicate that the gamma rays from Markarian 501 are due to the acceleration of protons rather than electrons. Furthermore, the observed absence of gamma ray attenuation due to electron-positron pair production in collisions with cosmic infrared photons implies a limit of 2 to 4 nanowatt per squaremeter per steradian for the energy flux of an extragalactic infrared radiation background at a wavelength of 25 micrometers. This limit provides important clues on the epoch of galaxy formation.']",['1998-03-23'] +1624,['eng'],"['Perivolaropoulos, L', 'Simatos, N']",['Hints of Cosmic String Induced Discontinuities in the COBE Data?'],['Astrophysics and Astronomy'],"['astrophysics, string', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'temperature', 'coherence', 'statistical analysis', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803321'],['We apply new statistical tests on the four year 53 GHz DMR data and show that there is significant probability for the existence of coherent temperature discontinuities hidden in the CMB maps around the Galactic Poles. Comparing Monte Carlo simulations with the DMR maps we find that the probability for the existence of a coherent discontinuity with amplitude $0.2 \\times ({{\\delta T} than the corresponding probability when no discontinuity is present. This result is consistent with the existence of a horizon size long cosmic string with mass per unit length $\\mu$ given by $G\\mu v_s \\gamma_s \\simeq 10^{-6}/\\pi$ where $v_s$ is the string velocity and $\\gamma_s$ is the corresponding Lorentz factor.'],['1998-03-31'] +1625,['eng'],"['Pal, P B']",['Neutrino astrophysics and cosmology'],['Astrophysics and Astronomy'],"['talk, Allahabad 1998/01/04', 'velocity, pulsar', 'supernova, shock waves', 'neutrino, cosmic radiation', 'deuterium, density', 'counters and detectors', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803312'],"['In this talk, I have discussed some issues of recent interest and activity in the field of neutrino astrophysics and cosmology. The topics are: (1)~The origin of high peculiar velocities of pulsars; (2)~Energization of the supernova shock wave; (3)~Ultra-high energy neutrino astronomy; (4)~Possible implications of the recent measurements of low deuterium abundance.']",['1998-03-30'] +1626,['eng'],"['Funk, B', 'Magnussen, N', 'Meyer, H', 'Rhode, W', 'Westerhoff, S', 'Wiebel-Sooth, B']",['An Upper Limit on the Infrared Background Density from HEGRA data on Mkn501'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'astrophysics, model', 'photon, absorption', 'photon, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802308'],"['The energy spectrum of Mkn501 in the TeV energy regime, as measured by the HEGRA (High Energy Gamma Ray Astronomy) Cerenkov telescopes during its low state in 1995/96 and during a fraction of the 1997 outburst in the TeV energy regime, is shown to place stringent upper limits on the still unknown infrared photon density in the energy region between 3 x 10**(-3) and 3 xt 10**(-1) eV. Assuming two different shapes for the unknown infrared photon spectrum in this energy range we calculate upper limits on the infrared photon density on the basis of the power-law fit obtained for the observed spectrum up to the maximum energy.']",['1998-02-25'] +1627,['eng'],"['Glendenning, N K', 'Schaffner-Bielich, J']",['Neutron Star Constraints on the H Dibaryon'],['Astrophysics and Astronomy'],"['astrophysics', 'n, matter', 'potential, chemical', 'mean field approximation', 'effective Lagrangian', 'baryon resonance, condensation', 'meson baryon, interaction', 'baryon resonance, interaction', 'baryon resonance, dibaryon', 'mass, H baryon', 'thermodynamics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803232'],"['We study the influence of a possible H dibaryon condensate on the equation of state and the overall properties of neutron stars whose population otherwise contains nucleons and hyperons. In particular, we are interested in the question of whether neutron stars and their masses can be used to say anything about the existence and properties of the H dibaryon. We find that the equation of state is softened by the appearance of a dibaryon condensate and can result in a mass plateau for neutron stars. If the limiting neutron star mass is about that of the Hulse-Taylor pulsar a condensate of H dibaryons of vacuum mass 2.2 GeV and a moderately attractive potential in the medium could not be ruled out. On the other hand, if the medium potential were even moderately repulsive, the H, would not likely exist in neutron stars. If neutron stars of about 1.6 solar mass were known to exist, attractive medium effects for the H could be ruled out.']",['1998-03-20'] +1628,['eng'],"['Ribeiro, M B', 'Miguelote, A Y']",['Fractals and the Distribution of Galaxies'],['Astrophysics and Astronomy'],['review'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803218'],"[""This paper presents a review of the fractal approach for describing the large scale distribution of galaxies. We start by presenting a brief, but general, introduction to fractals, which emphasizes their empirical side and applications rather than their mathematical side. Then we discuss the standard correlation function analysis of galaxy catalogues and many observational facts that brought increasing doubts about the reliability of this method, paying special attention to the standard analysis implicit assumption of an eventual homogeneity of the distribution of galaxies. Some new statistical concepts for analysing this distribution is presented, and without the implicit assumption of homogeneity they bring support to the hypothesis that the distribution of galaxies does form a fractal system. The Pietronero-Wertz's single fractal (hierarchical) model is presented and discussed, together with the implications of this new approach for understanding galaxy clustering.""]",['1998-03-19'] +1629,['eng'],"['Qian, Y Z']",['Some nuclear physics aspects of core-collapse supernovae'],['Astrophysics and Astronomy'],"['review, Oak Ridge 1997/12/02', 'nuclear physics', 'nuclear matter', 'astrophysics', 'supernova', 'neutrino, cosmic radiation', 'neutrino, emission', 'neutrino, opacity', 'parity, violation', 'velocity, pulsar', 'neutrino, energy spectrum', 'nucleus, heavy', 'nucleus, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802259'],"['Here I review some nuclear physics aspects of core-collapse supernovae concerning neutrinos. Studies of neutrino emission and interactions in supernovae are crucial to our understanding of the explosion mechanism, the heavy element nucleosynthesis, and pulsar proper motions. I discuss the effects of reduced neutrino opacities in dense nuclear matter on supernova neutrino emission and their implications for the delayed supernova explosion mechanism and the synthesis of neutron-rich heavy elements. I also discuss the effects of parity violation in weak interactions on supernova neutrino emission and their implications for pulsar proper motions.']",['1998-02-20'] +1630,['eng'],"['Glendenning, N K']",['Pulsar Signal of Deconfinement'],['Astrophysics and Astronomy'],"['talk, Tsukuba 1997/12/01', 'n, matter', 'astrophysics, pulsar', 'signal processing', 'critical phenomena, confinement', 'moment', 'spin', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803067'],"[""A solitary millisecond pulsar, if near the mass limit, and undergoing a phase transition, either first or second order, provided the transition is to a substantially more compressible phase, will emit a blatantly obvious signal---spontaneous spin-up. Normally a pulsar spins down by angular momentum loss to radiation. The signal is trivial to detect and is estimated to be ``on'' for 1/50 of the spin-down era of millisecond pulsars. Presently about 25 solitary millisecond pulsars are known. The phenomenon is analogous to ``backbending'' observed in high spin nuclei in the 1970's.""]",['1998-03-09'] +1631,['eng'],"['Glendenning, N K']",['Spin-up of Solitary Pulsars'],['Astrophysics and Astronomy'],"['talk, Tokyo 1997/11/17', 'astrophysics, model', 'nuclear matter', 'spin, effect', 'radiation', 'thermodynamics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803070'],"['A phase transition in the nature of matter in the core of a neutron star, such as quark deconfinement or Bose condensation, can cause the spontaneous spin-up of a solitary millisecond pulsar. The spin-up epoch for our model lasts for $2\\times 10^7$ years or 1/50 of the spin-down time.']",['1998-03-09'] +1632,['eng'],"['Unruh, W G']",['Cosmological long wavelength perturbations'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'potential', 'perturbation', 'astrophysics, fundamental constant']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802323'],"['This paper presents an exact solution to the long wavelength perturbations for the scalar modes and for a scalar field theory with arbitrary potential. Locally these modes are coordinate transformations of the homogeneous background solutions (although non-locally they are not). These solutions are then used to discuss a couple of recent papers in which such perturbations play a role. Abramo, Brandenberger, and Mukhanov have recently argued that long wavelength perturbations have the effect of driving the cosmological constant to zero if the higher order perturbation equation are examined. I argue that this effect is invisible to any local observer, and thus does not constitute a relaxation of the cosmological constant in the normal sense of the term. Grishchuk has argues that the standard lore on the strength of the perturbations at the end of inflation is wrong. I discuss the disagreement in light of the exact long wavelength solutions, and emphasise the importance of the initial conditions in resolving the disagreement.']",['1998-02-26'] +1633,['eng'],"['Reddy, S', 'Pons, J', 'Prakash, M', 'Lattimer, J M']",['Neutrino Opacities at High Density and the Protoneutron Star Evolution'],['Astrophysics and Astronomy'],"['talk, Oak Ridge 1997/12/02', 'n, matter', 'neutrino, path length', 'density, high', 'scattering, neutrino baryon', 'cross section', 'relativistic', 'effect, correlation', 'strong interaction', 'charged current', 'neutral current', 'transport theory', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802312'],['The early evolution of a protoneutron star depends both on the equation of state and neutrino interactions at high density. We identify the important sources of neutrino opacity and through model calculations show that in-medium effects play an important role in determining the neutrino mean free paths. The effects due to Pauli-blocking and many-body correlations due to strong interactions reduce the neutrino cross sections by large factors compared to the case in which these effects are ignored. We discuss these results in the context of neutrino transport in a protoneutron star.'],['1998-02-25'] +1634,['eng'],"['Reddy, S', 'Pons, J', 'Prakash, M', 'Lattimer, J M']",['Neutrinos from Protoneutron Stars'],['Astrophysics and Astronomy'],"['talk, Hirschegg 1998/01/11', 'n, matter', 'neutrino, diffusion', 'transport theory', 'energy', 'lepton number', 'temperature', 'potential, chemical', 'time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802310'],['We study the diffusive transport of neutrinos in a newly born neutron star to explore its sensitivity to dense matter properties. Energy and lepton number which are trapped during the catastrophic implosion diffuse out on the time scale of a few tens of seconds. Results for different dense matter models are presented.'],['1998-02-25'] +1635,['eng'],"['Wang, Y', 'Spergel, D N', 'Strauss, M A']",['Cosmology in the Next Millennium'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, fluctuation', 'spectra, measurement', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, galaxy', 'error', 'matter, density', 'astrophysics, fundamental constant', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802231'],"['The existence of primordial adiabatic Gaussian random-phase density fluctuations is a generic prediction of inflation. The properties of these fluctuations are completely specified by their power spectrum A_S^2(k). The basic cosmological parameters and the primordial power spectrum together completely specify predictions for the cosmic microwave background radiation anisotropy and large scale structure. Here we show how we can strongly constrain both A_S^2(k) and the cosmological parameters by combining the data from the Microwave Anisotropy Probe (MAP) and the galaxy redshift survey from the Sloan Digital Sky Survey (SDSS). We allow A_S^2(k) to be a free function, and thus probe features in the primordial power spectrum on all scales. If we assume that the cosmological parameters are known a priori, the primordial power spectrum in 20 steps in log k to k\\leq 0.5hMpc^{-1} can be determined to 0.1hMpc^{-1}. The uncertainty in the primordial power spectrum increases by less than a factor of 2 if we solve simultaneously for h, \\Lambda, Ømega_b, galaxy redshift density field b_{eff}. Thus, combining the MAP and SDSS data allows the independent measurement of important cosmological parameters, and a model-independent measurement of the primordial power spectrum, giving us valuable information on physics in the early Universe, and providing clues to the correct inflationary model.(abridged)']",['1998-02-18'] +1636,['eng'],"['Kofman, L A']",['Aspects of Preheating after Inflation'],['Astrophysics and Astronomy'],"['talk, Ambleside 1997/09/15', 'inflationary universe', 'potential, inflaton', 'resonance', 'particle, production', 'particle, scattering', 'critical phenomena', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802221'],"[""In inflationary cosmology, the particles constituting the Universe are created after inflation in the process of reheating due to the interaction with the oscillating inflaton field. We briefly review the basics of the slow reheating, and the stage of fast preheating, when the particles are created explosively in the regime of parametric resonance. The non-perturbative, out-of-equilibrium character of the parametric resonance changes many features of reheating. For these proceedings, we will highlight a few aspects of preheating: the structural dependence of the parametric resonance on the inflationary model, including $V(\\phi)={m^2 \\over 2}\\phi^2$, ${\\lambda\\over 4}\\phi^4$, $1-\\cos {\\phi \\over f}$; ``rescattering'' of created particles; and phase transitions after inflation.""]",['1998-02-18'] +1637,['eng'],"['Copeland, E J', 'Grivell, I J', 'Kolb, E W', 'Liddle, A R']",['On the reliability of inflaton potential reconstruction'],['Astrophysics and Astronomy'],"['inflationary universe', 'potential, inflaton', 'cosmic radiation, background', 'spectra, perturbation', 'error', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802209'],"['If primordial scalar and tensor perturbation spectra can be inferred from observations of the cosmic background radiation and large-scale structure, then one might hope to reconstruct a unique single-field inflaton potential capable of generating the observed spectra. In this paper we examine conditions under which such a potential can be reliably reconstructed. For it to be possible at all, the spectra must be well fit by a Taylor series expansion. A complete reconstruction requires a statistically-significant tensor mode to be measured in the microwave background. We find that the observational uncertainties dominate the theoretical error from use of the slow-roll approximation, and conclude that the reconstruction procedure will never insidiously lead to an irrelevant potential.']",['1998-02-17'] +1638,['eng'],"['Enqvist, Kari']",['Primordial Magnetic Fields'],['Astrophysics and Astronomy'],"['magnetic field, galaxy', 'astrophysics, model', 'critical phenomena', 'correlation, length', 'energy, magnetic', 'fluctuation', 'coherence', 'shell model', 'field theory, Higgs', 'vacuum state, condensation', 'turbulence', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803196'],"['The explanation of the observed galactic magnetic fields may require the existence of a primordial magnetic field. Such a field may arise during the early cosmological phase transitions, or because of other particle physics related phenomena in the very early universe reviewed here. The turbulent evolution of the initial, randomly fluctuating microscopic field to a large-scale macroscopic field can be described in terms of a shell model, which provides an approximation to the complete magnetohydrodynamics. The results indicate that there is an inverse cascade of magnetic energy whereby the coherence of the magnetic field is increased by many orders of magnitude. Cosmological seed fields roughly of the order of $10^{-20}$ G at the scale of protogalaxy, as required by the dynamo explanation of galactic magnetic fields, thus seem plausible.']",['1998-03-18'] +1639,['eng'],"['Fiorentini, G', 'Lisi, E', 'Sarkar, S', 'Villante, F L']",['Quantifying uncertainties in primordial nucleosynthesis without Monte Carlo simulations'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'nucleus nucleus, nuclear reaction', 'ratio, (nucleon photon)', 'cross section', 'statistics', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803177'],"['We present a simple method for determining the (correlated) uncertainties of the light element abundances expected from big bang nucleosynthesis, which avoids the need for lengthy Monte Carlo simulations. Our approach helps to clarify the role of the different nuclear reactions contributing to a particular elemental abundance and makes it easy to implement energy-independent changes in the measured reaction rates. As an application, we demonstrate how this method simplifies the statistical estimation of the nucleon-to-photon ratio through comparison of the standard BBN predictions with the observationally inferred abundances.']",['1998-03-17'] +1640,['eng'],"['Glashow, Sheldon Lee']",['Cosmological Searches for Photon Velocity Oscillations'],['Astrophysics and Astronomy'],"['photon, postulated particle', 'photon, massless', 'velocity, oscillation', 'symmetry breaking, Lorentz', 'cosmic radiation, background', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803202'],"['We posit a second massless photon, uncoupled to known forms of matter but undergoing Lorentz non-invariant velocity mixing with ordinary photons. Our speculation within a speculation suffers from the sin of implausibility but enjoys the virtue of verifiability. To avoid unacceptable distortion of the well-measured microwave background spectrum, the velocity difference of the photons cannot exceed $\\sim10^{-32} c$. Stronger constraints (or observable effects!) can arise from optical measurements of distant sources.']",['1998-03-18'] +1641,['eng'],"['Webb, J K', 'Flambaum, V V', 'Churchill, C W', 'Drinkwater, M J', 'Barrow, John D']",['Search for Time Variation of the Fine Structure Constant'],['Astrophysics and Astronomy'],"['fundamental constant, fine structure', 'fundamental constant, time variation', 'spectra, quasar', 'astrophysics, redshift', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803165'],"['A method offering an order of magnitude sensitivity gain is described for using quasar spectra to investigate possible time or space variation in the fine structure constant $\\alpha$. Applying the technique to a sample of 30 absorption systems, spanning redshifts $0.51$, where $\\Delta \\alpha /\\alpha =-2.6\\pm 0.4\\times 10^{-5}$. For $z<1$, $\\Delta \\alpha /\\alpha =+0.2\\pm 0.4\\times 10^{-5}$, consistent with other known limits. Whilst we cannot rule out either a systematic error in the data, or some different physical explanation, we cannot reliably identify any such mechanism. These results are consistent with a time-varying $\\alpha $.']",['1998-03-17'] +1642,['eng'],"['Abramo, L R W', 'Tsamis, N C', 'Woodard, R P']",['Cosmological Density Perturbations From A Quantum Gravitational Model Of Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'quantum gravity', 'density, perturbation', 'perturbation, scalar', 'perturbation, tensor', 'potential, scalar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803172'],"[""We derive the implications for anisotropies in the cosmic microwave background following from a model of inflation in which a bare cosmological constant is gradually screened by an infrared process in quantum gravity. The model predicts that the amplitude of scalar perturbations is $A_S = (2.0 \\pm .2) \\times 10^{-5}$, that the tensor-to-scalar ratio is $r \\approx 1.7 \\times 10^{-3}$, and that the scalar and tensor spectral indices are $n \\approx .97$ and $n_T \\approx -2.8 \\times 10^{-4}$, respectively. By comparing the model's power spectrum with the COBE 4-year RMS quadrupole, the mass scale of inflation is determined to be $M = (.72 \\pm .03) \\times 10^{16}~{\\rm GeV}$. At this scale the model produces about $10^8$ e-foldings of inflation, so another prediction is $\\Omega = 1$.""]",['1998-03-17'] +1643,['eng'],"['Lipari, P', 'Gaisser, T K', 'Stanev, T']",['Geomagnetic Effects on Atmospheric Neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, air', 'cosmic radiation, energy spectrum', 'magnetic field, effect', 'geophysics', 'neutrino, angular distribution', 'neutrino, flux', 'neutrino, oscillation', 'neutrino, mass difference', 'muon, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803093'],"['Geomagnetic effects distort the zenith angle distribution of sub--GeV and few--GeV atmospheric neutrinos, breaking the up--down symmetry that would be present in the absence of neutrino oscillations and without a geomagnetic field. The geomagnetic effects also produce a characteristic azimuthal dependence of the $\\nu$--fluxes, related to the well known east--west effect, that should be detectable in neutrino experiments of sufficiently large mass. We discuss these effects quantitatively. Because the azimuthal dependence is in first order independent of any oscillation effect, it is a useful diagnostic tool for studying possible systematic effects in the search for neutrino oscillations.']",['1998-03-10'] +1644,['eng'],"['Glendenning, N K']",['Phase Transition Signal in Pulsar Timing'],['Astrophysics and Astronomy'],"['talk, Hirschegg 1998/01/11', 'astrophysics, pulsar', 'n, matter', 'nuclear matter', 'critical phenomena', 'quark, confinement', 'boson, condensation', 'quark, matter', 'astrophysics, spin', 'energy, density', 'moment', 'time dependence', 'thermodynamics', 'forces', 'charge, density', 'spatial distribution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803074'],"[""A phase transition in the nature of matter in the core of a neutron star, such as quark deconfinement or Bose condensation, can cause the spontaneous spin-up of a solitary millisecond pulsar. The spin-up epoch for our model lasts for $2\\times 10^7$ years or 1/50 of the spin-down time (Glendenning, Pei and Weber in Ref. \\cite{glen97:a}). The possibility exists also for future measurements on X-ray neutron stars with low-mass companions for mapping out the tell-tale ``backbending'' behavior of the moment of inertia. Properties of phase transitions in substances such as neutron star matter, which have more than one conserved charge, are reviewed.""]",['1998-03-09'] +1645,['eng'],"['Allen, R E']",['Instanton Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, instanton', 'Einstein equation', 'space-time']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803079'],"['A new cosmological model provides solutions for the flatness, smoothness, monopole, and classical singularity problems, with no adjustment of parameters. The prediction of a scale factor R(t) which is proportional to t (rather than $t^{2/3}$) yields a comfortably large age for the universe, and also implies that the deceleration parameter $q_{0}$ is exactly zero.']",['1998-03-10'] +1646,['eng'],"['López, R E', 'Dodelson, S', 'Heckler, A F', 'Turner, M S']",['Precision Detection of the Cosmic Neutrino Background'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, density', 'photon, density', 'cosmic radiation, background', 'quantum electrodynamics, finite temperature', 'electron positron, annihilation', 'temperature, anisotropy', 'moment, multipole', 'electric field, polarization', 'polarization, anisotropy', 'proposed experiment, satellite', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803095'],"[""In the standard Big Bang cosmology the canonical value for the ratio of relic neutrinos to CMB photons is 9/11. Within the framework of the Standard Model of particle physics there are small corrections, in sum about 1%, due to slight heating of neutrinos by electron/positron annihilations and finite-temperature QED effects. We show that this leads to changes in the predicted cosmic microwave background (CMB) anisotropies that might be detected by future satellite experiments. NASA's MAP and ESA's PLANCK should be able to test the canonical prediction to a precision of 1% or better and could confirm these corrections.""]",['1998-03-10'] +1647,['eng'],"['Liddle, A R']",['Inflation and the microwave background'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1998/01/17', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803152'],"['I discuss the interplay between inflation and microwave background anisotropies, stressing in particular the accuracy with which inflation predictions need to be made, and the importance of inflation as an underlying paradigm for cosmological parameter estimation.']",['1998-03-16'] +1648,['eng'],"['Steigman, G']",['Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Oak Ridge 1997/12/02', 'astrophysics, model', 'light nucleus, production', 'light nucleus, density', 'nucleon, density', 'photon, density', 'deuterium', 'helium, nuclide', 'energy, density', 'neutrino, flavor', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803055'],"['During its hot, dense, early evolution the Universe was a primordial nuclear reactor, synthesizing the light nuclides D, 3He, 4He and 7Li in the first thousand seconds. The presently observed abundances of these relic nuclides provide a unique window on the early Universe. The implications of current observations for cosmology (the universal density of nucleons) and for particle physics (new particles beyond the standard model) will be reviewed. The present data appear to be in rough agreement with the predictions of the standard, hot big bang model for three species of light neutrinos, and a nucleon-to-photon ratio restricted to a narrow range of 3-4 parts in 10 billion. On closer inspection, however, a tension is revealed between the inferred primordial abundances of deuterium and helium-4. Although observations of deuterium in nearly primordial, high-redshift QSO absorbers may help to relieve this tension, current data appear to exacerbate the crisis. Resolution of this conflict may lie with the data (statistical uncertainties?), with the analysis of the data (systematic uncertainties?), or with the fundamental physics (massive, unstable, and/or degenerate neutrinos?). Independent (non-BBN) evidence from cosmological observations of large-scale dynamics and structure may be useful in deciding among the current options.']",['1998-03-06'] +1649,['eng'],"['Haubold, H J']",['Wavelet Analysis of the New Solar Neutrino Capture Rate Data for the Homestake Experiment'],['Astrophysics and Astronomy'],"['talk, Orsay 1997/11/13', 'neutrino, solar', 'neutrino, flux', 'flux, time variation', 'neutrino nucleus, capture', 'chlorine', 'transformation, wavelet', 'numerical calculations, interpretation of experiments', 'deep underground detector, Homestake']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803136'],"[""Wavelet analysis offers an alternative to Fourier based time-series analysis and is particularly useful when spectral features are time dependent. We analyze the solar neutrino capture rate of the radiochemical Homestake chlorine experiment with abbreviated Morlet wavelets, using Foster's (AJ, 111, 1709 (1996)) rescaled wavelet technique. We emphasize the complementarity of wavelet analysis to Fourier analysis. The Homestake data seem to contain a harmonic content with periodicities of 4.76 yr, 1.89 yr, 0.85 yr, and 0.51 yr. Wavelet analysis reveals that the 4.76 yr and 1.89 yr periods show an almost constant behavior over the 25 yr Homestake data record, while the 0.85 yr and 0.51 yr periods exhibit a transient phenomenon. The analysis does not show strong evidence for a period of the solar 11 yr cycle.""]",['1998-03-12'] +1650,['eng'],"['Pina-Avelino, P', 'Shellard, E P S', 'Allen, B']",['Non-gaussian Features of Linear Cosmic String Models'],['Astrophysics and Astronomy'],"['astrophysics, string', 'density, perturbation', 'model, linear', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803120'],"['We investigate the non-gaussian properties of cosmic-string-seeded linear density perturbations with cold and hot dark matter backgrounds. These perturbations are computed using high-resolution numerical simulations with a dynamic range extending from before the radiation-matter transition through to deep into the matter era. We compute the one-point probability density function of the resulting density field, its skewness, kurtosis, and genus curves for different smoothing scales. A semi-analytic model is then invoked to provide a physical interpretation of our results. We conclude that on scales smaller than $1.5{(\\Omega h^2)}^{-1}$Mpc, perturbations seeded by cosmic strings are very non-gaussian. These scales may still be in a linear or mildly non-linear regime in an open or $\\Lambda$-universe with $\\Gamma=\\Omega h \\lsim 0.2$.']",['1998-03-11'] +1651,['eng'],"['Lukash, V N', 'Mikheeva, E V']",['Generation of Gravitational Waves and Scalar Perturbations in Inflation with Effective $\\Lambda$-term and T/S Story'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'inflationary universe, hybrid', 'gravitational radiation, production', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'density, perturbation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803064'],['We argue that gravitational wave contribution to the cosmic microwave background anisotropy at angular scale $\\sim 10^0$ may exceed 50% for some models of hybrid inflation producing standard cosmology with the density perturbation slope $n \\simeq 1$.'],['1998-03-09'] +1652,['eng'],"['Chitnis, V R', 'Bhat, P N']",['Cerenkov Photon Density Fluctuations in Extensive Air Showers'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'p, cosmic radiation', 'electron, secondary radiation', 'showers, air', 'radiation, Cherenkov', 'fluctuation, density', 'moment', 'energy dependence', 'spatial distribution', 'electron, energy spectrum', 'scaling, Coulomb', 'magnetic field, geophysics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802201'],"['The details of Cerenkov light produced by a gamma ray or a cosmic ray incident at the top of the atmosphere is best studied through systematic simulations of the extensive air showers. Recently such studies have become all the more important in view of the various techniques resulting from such studies, to distinguish gamma ray initiated showers from those generated by much more abundant hadronic component of cosmic rays. We have carried out here such systematic simulation studies using CORSIKA package in order to understand the Cerenkov photon density fluctuations for 5 different energies at various core distances both for gamma ray and proton primaries incident vertically at the top of the atmosphere. Such a systematic comparison of shower to shower density fluctuations for gamma ray and proton primaries is carried out for the first time here. It is found that the density fluctuations are significantly non-Poissonian. Such fluctuations are much more pronounced in the proton primaries than gamma ray primaries at all energies. The processes that contribute significantly to the observed fluctuations have been identified. It has been found that significant contribution to fluctuations comes from photons emitted after shower maximum. The electron number fluctuations and correlated emission of Cerenkov photons are mainly responsible for the observed fluctuations.']",['1998-02-17'] +1653,['eng'],"['Chadwick, P M', 'Dickinson, M R', 'Dipper, N A', 'Kendall, T R', 'McComb, T J L', 'Orford, K J', 'Osborne, J L', 'Rayner, S M', 'Roberts, I D', 'Shaw, S E', 'Turver, K E']",['Centaurus X-3'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'time dependence', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802338'],"['Centaurus X-3 is a well-studied high-mass accreting X-ray binary and a variable source of high energy gamma rays with energies from 100 MeV to 1 TeV. Previous results have suggested that the origin of the gamma rays is not the immediate vicinity of the neutron star but is sited in the accretion disc, perhaps in an accretion wake. The Durham Mark 6 gamma ray telescope has been used to measure the gamma ray flux from Centaurus X-3 with much higher sensitivity than previous ground-based measurements. The flux above ~ 400 GeV was measured to be (2 +/- 0.3) x 10^-11 cm^-2 s^-1 and appears constant over a period of 2 - 3 months. In 10 hours of observations there is no evidence for periodicity in the detected gamma rays at the X-ray spin period either from a site in the region of the neutron star, or from any other potential site in the orbit.']",['1998-02-27'] +1654,['eng'],"['Grasso, D', 'Nunokawa, H', 'Valle, José W F']",['Pulsar Velocities without Neutrino Mass'],['Astrophysics and Astronomy'],"['velocity, pulsar', 'neutrino, emission', 'anisotropy', 'neutrino, massless', 'neutrino, transition', 'resonance, transition', 'magnetic field, high', 'universality, violation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803002'],['We show that pulsar velocities may arise from anisotropic neutrino emission induced by resonant conversions of massless neutrinos in the presence of a strong magnetic field. The main ingredient is a small violation of weak universality and neither neutrino masses nor magnetic moments are required.'],['1998-03-03'] +1655,['eng'],"['Baron, E A', 'Cowan, J J', 'Rogers, T', 'Gutíerrez, K']",['R-process in Low Entropy Neutrino Driven Winds'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'n, matter', 'nuclear reaction', 'light nucleus, production', 'neutrino', 'entropy', 'model, hydrodynamical', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802360'],"['We present a parameter study which examines the r-process expected from the ejecta produced by a neutrino driven wind from the accretion induced collapse (AIC) of a white dwarf to a neutron star. The ejecta from this environment is different than that expected from the neutrino driven wind that follows the formation of a neutron star in the core collapse of a massive star which produces a Type II (or Type Ib/c) supernova. The entropy and electron fraction Ye are significantly lower than in the shock driven supernova case. Using the results of hydrodynamical calculations as guidance, we find that for a narrow range of conditions (S approx 3-5 and 0.36 < Ye < 0.41) an r-process distribution that approximates the solar system abundances. The amount of material ejected in AIC is naturally limited to be low, M_{ejecta} approx 0.01-0.0001 solar masses, an amount that would be sufficient to synthesize the Galactic r-process abundances. Also there are no worries that the material will fall back onto the neutron star in AIC.']",['1998-03-02'] +1656,['eng'],"['Lai, D', 'Qian, Y Z']","['Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks; 2, The Effect of Asymmetric Magnetic Field Topology']",['Astrophysics and Astronomy'],"['astrophysics, supernova', 'n, matter', 'astrophysics, pulsar', 'magnetic field, asymmetry', 'neutrino, transport theory', 'neutrino, absorption', 'cross section, energy dependence', 'antineutrino, absorption', 'neutrino/e', 'thermodynamics', 'neutrino, flux', 'neutrino, energy spectrum', 'antineutrino, energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802345'],"['In proto-neutron stars with strong magnetic fields, the cross section for magnetic field strength due to the quantization of energy levels for the $e^-$ ($e^+$) produced in the final state. If the neutron star possesses an asymmetric magnetic field topology in the sense that the magnitude of magnetic field in the north pole is different from that in the south pole, then asymmetric neutrino emission may be generated. We calculate the absorption cross sections of $\\nue$ and $\\bnue$ in strong magnetic fields as a function of the neutrino energy. These cross sections exhibit oscillatory behaviors which occur because new Landau levels for the $e^-$ ($e^+$) become accessible as the neutrino energy increases. By evaluating the appropriately averaged neutrino opacities, we demonstrate that the change in the local neutrino flux due to the modified opacities is rather small. To generate appreciable kick velocity ($\\sim 300$ km/s$) to the newly-formed neutron star, the difference in the field strengths at the two opposite poles of the star must be at least $10^{16}$ G. We conclude that this is a much less efficient mechanism to produce pulsar kicks than the one based on parity violation effect in weak interactions. We also consider the magnetic field effect on the spectral neutrino energy fluxes. The oscillatory features in the absorption opacities give rise to modulations in the emergent spectra of $\\nu_e$ and $\\bar\\nu_e$.']",['1998-02-27'] +1657,['eng'],"['Lai, D', 'Qian, Y Z']","['Neutrino Transport in Strongly Magnetized Proto-Neutron Stars and the Origin of Pulsar Kicks; 1, The Effect of Parity Violation in Weak Interactions']",['Astrophysics and Astronomy'],"['astrophysics, supernova', 'astrophysics, pulsar', 'n, matter', 'matter, density', 'magnetic field', 'parity, violation', 'neutrino nucleon, elastic scattering', 'nucleon, polarization', 'neutrino, absorption', 'neutrino electron, elastic scattering', 'thermodynamics', 'multiple scattering', 'time dependence', 'neutrino, transport theory', 'neutrino, flux', 'antineutrino, flux', 'neutrino, flavor', 'energy, density', 'potential, chemical', 'neutrino, path integral', 'neutrino, luminosity', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802344'],"['In proto-neutron stars with strong magnetic fields, the neutrino-nucleon scattering/absorption cross sections depend asymmetrically on the direction of neutrino momentum with respect to the magnetic field axis, a manifestation of parity violation in weak interactions. We develop the moment formalism of neutrino transport in the presence of such asymmetric neutrino opacities. For a given neutrino species, there is a drift flux of neutrinos along the magnetic field in addition to the usual diffusive flux. Although the drift flux of crossing symmetry in the scattering matrix element, there is a net drift flux associated with $\\nu_e$ and $\\bar\\nu_e$ since a proto-neutron star contains more $\\nu_e$ than $\\bar\\nu_e$. This net drift flux induces globally asymmetric temperature and composition profiles in the star, and leads to asymmetric neutrino emission from the star. We demonstrate that significant asymmetry in neutrino emission can be obtained due to multiple neutrino-nucleon scatterings. We also show that in the bulk interior of the neutron star, the asymmetry associated with neutrino absorption is cancelled by the asymmetry associated with neutrino emission. We numerically evolve the asymmetric profiles of temperature and lepton number fractions of a newly-formed, magnetized neutron star through the deleptonization and thermal cooling phases. For an ordered magnetic field threading the neutron star interior, the fractional asymmetry in the total neutrino emission is about $0.006(B/10^{14}G)$, corresponding to a pulsar kick velocity of about $200(B/10^{14}G)$ km/s for a total radiated neutrino energy of $3\\times 10^{53}$ erg.']",['1998-02-27'] +1658,['eng'],"['Mitra, A']","['Comments on the paper ""Bare Quark Surfacees of Strange Stars and Electron-Positron Pair Emission""']",['Astrophysics and Astronomy'],"['astrophysics, model', 'temperature', 'quark, matter', 'matter, strangeness', 'electron, pair production', 'luminosity', 'electric field, electrostatic', 'baryon, plasma']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802331'],"['In a recent paper (Ushov, PRL, 80, 230, 1998), it has been claimed that the bare surface of a strange star can emit electron-positron pairs of luminosity ~10^{51} ergs/s for about 10s. If true, obviously, this mechanism may explain the origin of cosmic Gamma Ray Bursts. However, we point out that such a mechanism is unlikely to work because (i) if pair production really occurs the supposed pre-existing supercritical electric field will be quenched and this discharge process may at best release ~10^{24} ergs of electromagnetic energy, and (ii) there is no way by which the trapped core thermal energy of few 10^{52} ergs can be transmitted electromagnetically on a time scale of ~10s or even on a much larger time scale. The only way the hot core can cool on a time scale of ~10 s or much shorter is by the well known process of emission of nu-antinu pairs.']",['1998-02-27'] +1659,['eng'],"['Pons, J A', 'Miralles, J A', 'Ibáñez, J M']",['Legendre expansion of the neutrino-antineutrino annihilation kernel'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'n, matter', 'thermodynamics', 'neutrino antineutrino, annihilation', 'electron, pair production', 'electron positron, annihilation', 'neutrino, pair production', 'neutrino, transport theory', 'energy', 'momentum', 'expansion, Legendre', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802333'],['We calculate the Legendre expansion of the rate of the process $\\nu + of other authors which only consider the 0th and 1st order terms. Using different closure relations for the moment equations of the radiative transfer equation we discuss the physical implications of taking into account quadratic and cubic terms on the energy deposition outside the neutrinosphere in a simplified model. The main conclusion is that 2nd order is necessary in the semi-transparent region and gives good results if an appropriate closure relation is used.'],['1998-02-27'] +1660,['eng'],"['Belyaev, V B', 'Monakhov, D E', 'Naumov, D V', 'Penkov, F M']",['Electron Screening in $^{7}Be+p \\rightarrow ^{8}B+ \\gamma$ photon reaction'],['Astrophysics and Astronomy'],"['p nucleus, nuclear reaction', 'beryllium', 'photon, emission', 'electron, screening', 'three-body problem', 'effective potential', 'neutrino, solar', 'fusion', 'numerical calculations', 'p beryllium --> boron photon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803003'],"['We evaluate the effect of screening by bound electron in (7Be,e) + p --> (8B,e) + photon transition in the framework of the adiabatic representation of the three particle problem. Comparison with two approaches (united nucleus and static) is presented. We discuss possible applications of this effect both for Solar Neutrinos and low energy fusion experiments.']",['1998-03-03'] +1661,['eng'],"['Castro-Tirado, A J']",['Multiwavelength observations of $\\gamma$-ray bursts'],['Astrophysics and Astronomy'],['review'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803007'],"['Since their discovery in 1973, Gamma-Ray Bursts (GRBs) have remained for many years one of the most elusive mysteries in High Energy-Astrophysics. The main problem regarding the nature of GRBs has usually been the lack of knowledge of their distance scale. About 300 GRBs are detected annually by BATSE in the full sky, but only a few of them can be localized accurately to less than half a degree. For many years, follow-up observations by other satellites and ground-based telescopes were conducted, but no counterparts at other wavelengths were found. The breakthrough took place in 1997, thanks to the observation by BeppoSAX and RossiXTE of the fading X-ray emission that follows the more energetic gamma-ray photons once the GRB event has ended. This emission (the afterglow) extends at longer wavelengths, and the good accuracy in the position determination by BeppoSAX has led to the discovery of the first optical counterparts -for GRB 970228, GRB 970508, and GRB 971214-, greatly improving our understanding of these puzzling sources. Now it is widely accepted that most bursts originate at cosmological distances but the final solution of the GRB problem is still far away.']",['1998-03-03'] +1662,['eng'],"['Vucetich, H', 'Horváth, J E']",['Strangelet spectra from type II supernovae'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'matter, strangeness', 'spectra', 'oxygen', 'fragmentation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802363'],"['We study in this work the fate of strangelets injected as a contamination in the tail of a ""strange matter-driven"" supernova shock. A simple model for the fragmentation and braking of the strangelets when they pass through the expanding oxygen shell is presented and solved to understand the reprocessing of this component. We find that the escaping spectrum is a scaled-down version of the one injected at the base of the oxygen shell. The supernova source is likely to produce low-energy particles of $A \\sim 100-1000$ quite independently of the initial conditions. However, it is difficult that ultrarrelativistic strangelets (such as the hypothetical Centauro primaries) can have an origin in those explosive events.']",['1998-03-02'] +1663,['eng'],"['Dokuchaev, V I', 'Eroshenko, Y N', 'Ozernoy, L M']",['$\\gamma$ Ray Bursts from the Evolved Galactic Nuclei'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'photon, cosmic radiation', 'nucleus, galaxy', 'cluster, compact', 'matter, scattering', 'n, matter', 'black hole', 'coalescence', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802358'],"['A new cosmological scenario for the origin of gamma ray bursts (GRBs) is proposed. In our scenario, a highly evolved central core in the dense galactic nucleus is formed containing a subsystem of compact stellar remnants (CSRs), such as neutron stars and black holes. Those subsystems result from the dynamical evolution of dense central stellar clusters in the galactic nuclei through merging of stars, thereby forming (as has been realized by many authors) the short-living massive stars and then CSRs. We estimate the rate of random CSR collisions in the evolved galactic nuclei by taking into account, similar to Quinlan & Shapiro (1987), the dissipative encounters of CSRs, mainly due to radiative losses of gravitational waves, which results in the formation of intermediate short-living binaries, with further coalescence of the companions to produce GRBs. We also consider how the possible presence of a central supermassive black hole, formed in a highly evolved galactic nucleus, influences the CSR binary formation. This scenario does not postulate ad hoc a required number of tight binary neutron stars in the galaxies. Instead, it gives, for the most realistic parameters of the evolved nuclei, the expected rate of GRBs consistent with the observed one, thereby explaining the GRB appearance in a natural way of the dynamical evolution of galactic nuclei. In addition, this scenario provides an opportunity for a cosmological GRB recurrence, previously considered to be a distinctive feature of GRBs of a local origin only. We also discuss some other observational tests of the proposed scenario.']",['1998-03-02'] +1664,['eng'],"['Yokoyama, J']",['Chaotic new inflation and formation of primordial black holes'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'potential, scalar', 'density, fluctuation', 'black hole, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802357'],"['It is shown that, in a number of scalar potentials with an unstable local maximum at the origin, chaotic inflation is followed by new inflation if model parameters are appropriately chosen. In this model density fluctuation can have a large-amplitude peak on the comoving Hubble scale at the onset of the slow-roll new inflation and can result in formation of appreciable amount of primordial black holes on astrophysically interesting mass scales.']",['1998-03-02'] +1665,['eng'],"['Bhattacharjee, P']",['Ultrahigh Energy Cosmic Rays from Topological Defects'],['Astrophysics and Astronomy'],"['talk, College Park 1997/11/13', 'astrophysics, string', 'topology, defect', 'cosmic radiation, particle source', 'postulated particle, massive', 'postulated particle, decay', 'magnetic monopole', 'symmetry breaking', 'critical phenomena', 'particle, spectra', 'particle, flux', 'particle, production', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9803029'],"['The topological defect scenario of origin of the observed highest energy cosmic rays is reviewed. Under a variety of circumstances, topological defects formed in the early Universe can be sources of very massive particles in the Universe today. The decay products of these massive particles may be responsible for the observed highest energy cosmic ray particles above $10^{20}$ eV. Some massive particle production processes involving cosmic strings and magnetic monopoles are discussed. We also discuss the implications of results of certain recent numerical simulations of evolution of cosmic strings. These results (which remain to be confirmed by independent simulations) seem to show that massive particle production may be a generic feature of cosmic strings, which would make cosmic strings an inevitable source of extremely high energy cosmic rays with potentially detectable flux. At the same time, cosmic strings are severely constrained by the observed cosmic ray flux above $10^{20}$ eV, if massive particle radiation is the dominant energy loss mechanism for cosmic strings.']",['1998-03-04'] +1666,['eng'],"['Frontera, F']",['Recent Results on $\\gamma$-Ray Bursts with the Bepposax Satellite'],['Astrophysics and Astronomy'],['review'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802157'],"['Recent results on Gamma-Ray Bursts obtained with the X-ray Astronomy satellite BeppoSAX are reviewed. Main emphasis is given to the GRBs simultaneously detected with the Gamma-Ray Burst Monitor (40-700 keV) and the Wide Field Cameras (1.5-26 keV). These bursts were rapidly localized with high precision, which permitted a prompt pointing of their error boxes with the Narrow Field Instruments aboard the same satellite. In three cases of bursts, these prompt observations led to the discovery of an X-ray afterglow. For two events also an optical transient was discovered. We review these results and their implications.']",['1998-02-15'] +1667,['eng'],"['Van Paradijs, J']",['Neutron Stars and Black Holes in X-Ray Binaries'],['Astrophysics and Astronomy'],['review'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802177'],"['Galactic accretion driven stellar X-ray sources can be divided into groups in different ways. An important division, which covers almost all known X-ray binaries, can be made according to the mass of the donor star: high-mass X-ray binaries and low-mass X-ray binaries. Another distinction (partially overlapping with the previous one) can be made on the basis of the nature of the accreting object: a strongly magnetized neutron star, a neutron star with a weak magnetic field, or a black hole. In this review I describe the properties of these different types of X-ray binaries, and discuss the mass determinations which are the basis for distinguishing accreting neutron stars from black holes.']",['1998-02-23'] +1668,['eng'],"['Shellard, E P S', 'Battye, R A']",['Cosmic Axions'],['Astrophysics and Astronomy'],"['talk, Ambleside 1997/09/15', 'astrophysics, missing-mass', 'inflationary universe', 'strong interaction, CP', 'mass, axion', 'quantization, fluctuation', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802216'],"[""The current cosmological constraints on a dark matter axion are reviewed. We describe the basic mechanisms by which axions are created in the early universe, both in the standard thermal scenario in which axion strings form and in inflationary models. In the thermal scenario, the dominant process for axion production is through the radiative decay of an axion string network, which implies a dark matter axion of mass m_a ~ 100 microeV with specified large uncertainties. An inflationary phase does not affect this string bound if the reheat temperature is high T_reh > f_a or, conversely, for T_reh < f_a, if the Hubble parameter during inflation is large H_1 > f_a; in both cases, strings form and we return to the standard picture with a m_a ~ 100 microeV dark matter axion. Inflationary models with f_a > H_1 > T_reh face strong CMBR constraints and require `anthropic misalignment' fine-tuning in order to produce a dark matter axion; in this case, some inflation models are essentially incompatible with a detectable axion, while others can be engineered to allow a dark matter axion anywhere in a huge mass range below m_a < 1 meV. We endeavour to clarify the sometimes confusing and contradictory literature on axion cosmology.""]",['1998-02-17'] +1669,['eng'],"['Kubis, S', 'Kutschera, M', 'Stachniewicz, S']",['Neutron Stars in Relativistic Mean Field Theory with Isovector Scalar Meson'],['Astrophysics and Astronomy'],"['n, matter', 'mean field approximation, relativistic', 'a0(980)', 'scalar meson, isovector', 'p, density', 'nucleon, energy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802303'],"['We study the equation of state of beta-stable dense matter and models of neutron stars in the relativistic mean field theory with the isovector scalar mean field corresponding to the delta-meson [a_0(980)]. A range of values of the delta-meson coupling compatible with the Bonn potentials is explored. Parameters of the model in the isovector sector are constrained to fit the nuclear symmetry energy, E_s=30 MeV. We find that the quantity most sensitive to the delta-meson coupling is the proton fraction of neutron star matter. It increases significantly in the presence of the delta-field. The energy per baryon also increases but the effect is smaller. The equation of state becomes slightly stiffer and the maximum neutron star mass increases for stronger delta-meson coupling.']",['1998-02-25'] +1670,['eng'],"['Yoshida, S', 'Dai, H']",['The Extremely High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['review, experimental results', 'cosmic radiation, energy spectrum', 'cosmic radiation, angular distribution', 'astrophysics, model', 'astrophysics, galaxy', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'hadron hadron, interaction', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802294'],"[""Experimental results from Haverah Park, Yakutsk, AGASA and Fly's Eye are reviewed. All these experiments work in the energy range above 0.1 EeV. The 'dip' structure around 3 EeV in the energy spectrum is well established by all the experiments, though the exact position differs slightly. Fly's Eye and Yakutsk results on the chemical composition indicate that the cosmic rays are getting lighter over the energy range from 0.1 EeV to 10 EeV, but the exact fraction is hadronic interaction model dependent, as indicated by the AGASA analysis. The arrival directions of cosmic rays are largely isotropic, but interesting features may be starting to emerge. Most of the experimental results can best be explained with the scenario that an extragalactic component gradually takes over a galactic population as energy increases and cosmic rays at the highest energies are dominated by particles coming from extragalactic space. However, identification of the extragalactic sources has not yet been successful because of limited statistics and the resolution of the data.""]",['1998-02-24'] +1671,['eng'],"['Bednarek, W', 'Protheroe, R J']",['$\\gamma$-ray and neutrino flares produced by protons accelerated on an accretion disk surface in AGN'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'neutrino, cosmic radiation', 'astrophysics, galaxy', 'p, acceleration', 'astrophysics, quasar', 'cosmic radiation, energy spectrum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802288'],"['We discuss the consequences of almost rectilinear acceleration of protons to extremely high energies in a reconnection region on the surface of an accretion disk which surrounds a central black hole in an active galaxy. The protons produce $\\gamma$-rays and neutrinos in interactions with the disk radiation as considered in several previous papers. However, in this model the secondary the disk. We compute the spectra of $\\gamma$-rays and neutrinos emerging from regions close to the disk surface. Depending on the parameters of the reconnection regions, this model predicts the appearance of $\\gamma$-ray and neutrino flares if protons takes most of the energy from the reconnection region. In contrast, if leptons take most of the energy, they produce pure cascading is compared with the spectrum observed during the flare in June 1991 from 3C 279. The neutrino flares which should accompany these gamma-ray flares may be detected by future large scale neutrino telescopes sensitive at $\\sim 10^{5}$ TeV.']",['1998-02-24'] +1672,['eng'],"['Rachen, J P', 'Mészáros, P']",['Photohadronic Neutrinos from Transients in Astrophysical Sources'],['Astrophysics and Astronomy'],"['astrophysics, particle source', 'neutrino, cosmic radiation', 'cosmic radiation, energy spectrum', 'photon p, interaction', 'neutrino, production', 'neutrino, flux', 'cosmic radiation, acceleration', 'showers, hadronic', 'pi, leptonic decay', 'muon, leptonic decay', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802280'],"['We investigate the spectrum of photohadronically produced neutrinos at very high energies (VHE, >10^14 eV) in astrophysical sources whose physical properties are constrained by their variability, in particular jets in AGN (blazars) and Gamma-Ray Bursts (GRB). We discuss in detail the various competing cooling processes for energetic protons, as well as the cooling of pions and muons in the hadronic cascade, which impose limits on both the efficiency of neutrino production and the maximum neutrino energy. If the proton acceleration process is of the Fermi type, we can derive a model independent upper limit on the neutrino energy from the observed properties of any cosmic transient, which depends only on the assumed total energy of the transient. For standard energetic constraints, we can rule out major contributions above 10^19 eV from current models of both blazars and GRBs; and in most models much stronger limits apply in order to produce measurable neutrino fluxes. For GRBs, we show that the cooling of pions and muons in the hadronic cascade imposes the strongest limit on the neutrino energy, leading to cutoff energies of the electron and muon neutrino spectrum at the source differing by about one order of magnitude. We also discuss the relation of maximum cosmic ray energies to maximum neutrino energies and fluxes in GRBs, and find that the production of both the highest energy cosmic rays and observable neutrino fluxes can only be realized under extreme conditions; a test implication of this joint scenario would be the existence of strong fluxes of muon neutrinos up to energies >~10^18 eV. Secondary particle cooling also leads to slightly revised estimates for the neutrino fluxes from (non-transient) AGN cores.']",['1998-02-24'] +1673,['eng'],"['Dodelson, S']",['Anisotropies in the Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'astrophysics, model', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, fundamental constant', 'inflationary universe', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702134'],"['Anisotropies in the Cosmic Microwave Background (CMB) contain a wealth of information about the past history of the universe and the present values of cosmological parameters. I ouline some of the theoretical advances of the last few years. In particular, I emphasize that for a wide class of cosmological models, theorists can accurately calculate the spectrum to better than a percent. The specturm of anisotropies today is directly related to the pattern of inhomogeneities present at the time of recombination. This recognition leads to a powerful argument that will enable us to distinguish inflationary models from other models of structure formation. If the inflationary models turn out to be correct, the free parameters in these models will be determined to unprecedented accuracy by the upcoming satellite missions.']",['1997-02-17'] +1674,['eng'],"['Torres, D F', 'Romero, G E', 'Anchordoqui, L A']",['Might some $\\gamma$ Ray Bursts be an observable signature of natural wormholes?'],['Astrophysics and Astronomy'],"['wormhole, lens', 'photon, cosmic radiation', 'galaxy, AGN', 'matter, density', 'upper limit', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802106'],"['The extragalactic microlensing scenario for natural wormholes is examined. It is shown that the main features of wormhole lensing events upon the light of distant Active Galactic Nuclei (AGNs) are similar to some types of already observed Gamma Ray Bursts (GRBs). Using recent satellite data on GRBs, an upper limit to the negative matter density under the form of wormhole-like objects is presented.']",['1998-02-10'] +1675,['eng'],"['Fryer, C L', 'Woosley, S E']",['$\\gamma$-Ray Bursts From Neutron Star Phase Transitions'],['Astrophysics and Astronomy'],"['n, matter', 'critical phenomena', 'matter, strangeness', 'photon, cosmic radiation', 'neutrino, density', 'velocity, relativistic', 'energy', 'light nucleus, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802112'],"[""The phase-transition induced collapse of a neutron star to a more compact configuration (typically a ``strange'' star) and the subsequent core bounce is often invoked as a model for gamma-ray bursts. We present the results of numerical simulations of this kind of event using realistic neutrino physics and a high density equation of state. The nature of the collapse itself is represented by the arbitrary motion of a piston deep within the star, but if any shock is to develop, the transition, or at least its final stages, must occur in less than a sonic time. Fine surface zoning is employed to adequately represent the acceleration of the shock to relativistic speeds and to determine the amount and energy of the ejecta. We find that these explosions are far too baryon-rich (ejected Mass > 0.01 solar masses) and have much too low an energy to explain gamma-ray bursts. The total energy of the ejecta having relativistic lorentz factors > 40 is less than 10^46 erg even in our most optimistic models (deep bounce, no neutrino losses or photodisintegration). However, the total energy of all the ejecta, mostly mildly relativistic, is roughly 10^51 erg and, if they occur, these events might be observed. They would also contribute to Galactic nucleosynthesis, especially the r-process, even though the most energetic layers are composed of helium and nucleons, not heavy elements.""]",['1998-02-13'] +1676,['eng'],"['Postnov, K A', 'Prokhorov, M E']",['Galactic Binary Gravitational Wave Noise within LISA Frequency Band'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'astrophysics, binary', 'astrophysics, galaxy', 'n, matter', 'counters and detectors, interference', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801034'],"['Gravitational wave noise associated with unresolved binary stars in the Galaxy is studied with the special aim of determining the upper frequency at which it stops to contribute at the rms noise level of the proposed space-born interferometer (LISA). The upper limit to this background is derived from the statistics of SN Ia explosions, part of which can be triggered by binary white dwarf coalescences. The upper limiting frequency at which binary stochastic noise crosses LISA rms sensitivity is found to lie within the range 0.03-0.07 Hz, depending on the galactic binary white dwarf coalescence rate. To be reliably detectable by LISA, the energy density of relic cosmological background per logarithmic frequency interval should be Omega_{GW}h_{100}^2>10^{-8} at f>0.03 Hz.']",['1998-01-08'] +1677,['eng'],"['Faraoni, V', 'Gunzig, E']",['Lensing by gravitational waves in scalar-tensor gravity'],['Astrophysics and Astronomy'],"['gravitational radiation, lens', 'photon, beam', 'gravitation, scalar', 'gravitation, tensor', 'relativity theory, general', 'space-time, background', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801172'],['The amplification of a light beam due to intervening gravitational waves is studied. The previous Jordan frame result according to which the amplification is many orders of magnitude larger in scalar-tensor gravity than in general relativity does not hold in the Einstein conformal frame. Lensing by gravitational waves is discussed in relation to the ongoing and proposed VLBI observations aimed at detecting the scintillation effect.'],['1998-01-20'] +1678,['eng'],"['Baumgarte, T W', 'Shapiro, S L']",['Radiation of Angular Momentum by Neutrinos from Merged Binary Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'neutrino, emission', 'neutrino, angular momentum', 'coalescence', 'time', 'gravitational radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801294'],"['We study neutrino emission from the remnant of an inspiraling binary neutron star following coalescence. The mass of the merged remnant is likely to exceed the stability limit of a cold, rotating neutron star. However, the angular momentum of the remnant may also approach or even exceed the Kerr limit, J/M^2 = 1, so that total collapse may not be possible unless some angular momentum is dissipated. We find that neutrino emission is very inefficient in decreasing the angular momentum of these merged objects and may even lead to a small increase in J/M^2. We illustrate these findings with a post-Newtonian, ellipsoidal model calculation. Simple arguments suggest that the remnant may form a bar mode instability on a timescale similar to or shorter than the neutrino emission timescale, in which case the evolution of the remnant will be dominated by the emission of gravitational waves.']",['1998-01-29'] +1679,['eng'],"['De Vega, H J', 'Sánchez, N', 'Combes, F']",['The fractal structure of the universe'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'thermodynamics', 'critical phenomena', 'scaling, finite size', 'gravitation', 'fractals', 'density, fluctuation', 'mass, density', 'correlation function', 'renormalization group', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801224'],"['While the universe becomes more and more homogeneous at large scales, statistical analysis of galaxy catalogs have revealed a fractal structure at small-scales (\\lambda < 100 h^{-1} Mpc), with a fractal dimension D=1.5-2 (Sylos Labini et al 1996). We study the thermodynamics of a self-gravitating system with the theory of critical phenomena and finite-size scaling and show that gravity provides a dynamical mechanism to produce this fractal structure. We develop a field theoretical approach to compute the galaxy distribution, assuming them to be in quasi-isothermal equilibrium. Only a limited, (although large), range of scales is involved, between a short-distance cut-off below which other physics intervene, and a large-distance cut-off, where the thermo- dynamic equilibrium is not satisfied. The galaxy ensemble can be considered at critical conditions, with large density fluctuations developping at any scale. From the theory of critical phenomena, we derive the two independent critical exponents nu and eta and predict the fractal dimension D = 1/nu to be either 1.585 or 2, depending on whether the long-range behaviour is governed by the Ising or the mean field fixed points, respectively. Both set of values are compatible with present observations. In addition, we predict the scaling behaviour of the gravitational potential to be r^{-(1 + eta)/2}. That is, r^{-0.5} for mean field or r^{- 0.519} for the Ising fixed point. The theory allows to compute the three and higher density correlators without any assumption or Ansatz. We find that the N-points density scales as r_1^{(N-1)(D-3)}, when r_1 >> r_i, 2 leq i leq N . There are no free parameters in this theory.']",['1998-01-26'] +1680,['eng'],"['Enström, D', 'Fredriksson, S', 'Hansson, J', 'Nicolaidis, A', 'Ekelin, S']",['A Quark-Matter Dominated Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'quark, matter', 'stability', 'astrophysics, missing-mass', 'galaxy, production', 'black hole', 'photon, cosmic radiation', 'quark gluon, plasma', 'critical phenomena', 'hadronization', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802236'],"['We present a new scenario for the development of the Universe after the Big Bang, built on the conjecture that a vast majority of the primordial quark matter did not undergo a phase transition to normal nuclear matter, but rather split up into massive quark objects that remained stable. Hence, such primordial quark matter would make up the so-called dark matter. We discuss, mostly in qualitative terms, the consequences for galaxy formation, the origin of normal matter, the occurrence of massive black-holes in galactic centres and the cosmic gamma-ray bursts.']",['1998-02-19'] +1681,['eng'],"['Schunck, F E']",['A scalar field matter model for dark halos of galaxies and gravitational redshift'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'Einstein equation, solution', 'field theory, scalar', 'massless', 'scaling', 'mass, density', 'energy, density', 'pressure', 'astrophysics, missing-mass', 'gravitation, redshift', 'velocity, rotational', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802258'],"['We analyze the spherically symmetric Einstein field equation with a massless complex scalar field. We can use the Newtonian solutions to fit the rotation curve data of spiral and dwarf galaxies. From the general relativistic solutions, we can derive high gravitational redshift values.']",['1998-02-20'] +1682,['eng'],"['Rehm, J B', 'Jedamzik, K']",['Big Bang Nucleosynthesis with Matter/Antimatter Domains'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'antimatter', 'n, diffusion', 'helium', 'lithium', 'electroweak interaction', 'baryon, production', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802255', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=capp98&id=rehm']","['We investigate Big Bang nucleosynthesis (hereafter, BBN) in a cosmic environment characterized by a distribution of small-scale matter/antimatter domains. Production of antimatter domains in a baryo-asymmetric universe is predicted in some electroweak baryogenesis scenarios. We find that cosmic antimatter domains of size exceeding the neutron-diffusion length at temperature T approx. 1 MeV significantly affect the light-element production. Annihilation of antimatter preferentially occurs on neutrons such that antimatter domains may yield a reduction of the He-4 abundance relative to a standard BBN scenario. In the limiting case, all neutrons will be removed before the onset of light-element production, and a universe with net baryon number but without production of light elements results. In general, antimatter domains spoil agreement between BBN abundance yields and observationally inferred primordial abundances limits which allows us to derive limits on their presence in the early universe. However, if only small amounts of antimatter are present, BBN with low deuterium and low He-4, as seemingly favored by current observational data, is possible.']",['1998-02-20'] +1683,['eng'],"['Vietri, M']",['Ultra high energy neutrinos from $\\gamma$ ray bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'neutrino, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'p, acceleration', 'model, shock waves', 'relativistic', 'cosmic radiation, flux', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802241'],"['Protons accelerated to high energies in the relativistic shocks that generate gamma ray bursts photoproduce pions, and then neutrinos in situ. I show that ultra high energy neutrinos (> 10^19 eV) are produced during the burst and the afterglow. A larger flux, also from bursts, is generated via photoproduction off CMBR photons in flight but is not correlated with currently observable bursts, appearing as a bright background. Temporal and directional coincidences with bursts detected by satellites can separate correlated neutrinos from the background, while background neutrinos will allow measurements of dipole and quadrupole moments of the distributions of their sources, thusly helping to establish the origin of ultra high energy cosmic rays. Both measurements may be doable with AIRWATCH--class experiments.']",['1998-02-19'] +1684,['eng'],"['Voskresensky, D N', 'Kolomeitsev, E E', 'Kämpfer, B']",['Contribution of the massive photon decay channel to neutrino cooling of neutron stars'],['Astrophysics and Astronomy'],"['astrophysics', 'n, matter', 'nuclear matter', 'photon, decay', 'neutrino, pair production', 'temperature', 'plasma', 'Feynman graph', 'superconducting', 'energy spectrum, (photon)', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802251'],['We consider massive photon decay reactions via intermediate states of electron-electron-holes and proton-proton-holes into neutrino-antineutrino pairs in the course of neutron star cooling. These reactions may become operative in hot neutron stars in the region of proton pairing where the photon due to the Higgs-Meissner effect acquires an effective mass $m_{\\gamma}$ that is small compared to the corresponding plasma frequency. The contribution of these reactions to neutrino emissivity is calculated; it varies with the temperature and the photon mass as $T^{3/2}m_{\\gamma}^{7/2} e^{-m_{\\gamma}/T}$ for $T < m_{\\gamma}$. Estimates show that these processes appear as extra efficient cooling channels of neutron stars at temperatures $T \\simeq (10^9-10^{10})$ K.'],['1998-02-20'] +1685,['eng'],"['Biller, S D', 'Buckley, J H', 'Burdett, A C', 'Gordo, J B', 'Carter-Lewis, D A', 'Fegan, D J', 'Findley, J', 'Gaidos, J A', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'McEnery, J E', 'Mohanty, G', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F', 'Sembroski, G H', 'Skelton, P', 'Weekes, T C']",['New Limits to the IR Background'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'background, flux', 'upper limit', 'neutrino, radiative decay', 'neutrino, massive', 'astrophysics, missing-mass', 'astrophysics, model', 'photon photon, interaction', 'neutrino, lifetime', 'neutrino, branching ratio', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802234'],"['From considering the effect of gamma-gamma interactions on recently observed TeV gamma-ray spectra, improved limits are set to the density of extragalactic infrared (IR) photons which are robust and essentially model-independent. The resulting limits are up to two orders of magnitude more restrictive than direct observations in the 0.025-0.3eV regime. These limits are used to improve constraints on radiative neutrino decay in the mass range above 0.05eV and on Very Massive Objects (VMOs) as providing the dark matter needed to explain galaxy rotation curves.']",['1998-02-19'] +1686,['eng'],"['Souradeep, T', 'Bond, J R', 'Knox, L', 'Efstathiou, G P', 'Turner, M S']",['Prospects for measuring Inflation parameters with the CMB'],['Astrophysics and Astronomy'],"['talk, Ambleside 1997/09/15', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802262'],"['We present the status of our study into the feasibility of estimating the parameters of inflation from planned satellite observations of the anisotropy of the cosmic microwave background (CMB).We describe a perturbative procedure for studying inflation models with soft departures from scale free spectra and find that in this case the parameters of inflation are likely to be well determined. We also demonstrate that radical departures from scale free initial perturbations with broad features in $k$-space can be be measured by Planck. However, allowing for very fine features in $k$-space can very strongly compromise the ability to measure cosmological parameters.']",['1998-02-20'] +1687,['eng'],"['Kosenko, D I', 'Postnov, K A']",['On the Gravitational Wave Noise from Unresolved Extragalactic Binaries'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'astrophysics, matter', 'astrophysics, galaxy', 'counters and detectors, interference', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801032'],"['We calculate the level of the stochastic gravitational wave background produced by extragalactic merging binary white dwarfs at the LISA frequencies 10^{-3}-10^{-2} Hz with account of a strong evolution of global star formation rate in the Universe recently established observationally. We show that, depending of the assumed cosmological model and the redshift of the initial star formation, the level of the extragalactic background can be comparable with the mean Galactic level of such a noise.']",['1998-01-08'] +1688,['eng'],"['Belolaptikov, I A', 'Bezrukov, L B', 'Budnev, N M', 'Bugaev, E V', 'Djilkibaev, Z A M', 'Domogatsky, G V', 'Doroshenko, A A', 'Klabukov, A M', 'Klimushin, S I', 'Kuzmichev, L A', 'Panfilov, A I', 'Parfenov, Y V', 'Sokalski, I A']","['The Experimental Limits on Q-ball Flux with the Baikal Deep Underwater Array ""Gyrlyanda""']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'supersymmetry', 'soliton, Q-ball', 'flux, Q-ball', 'flux, magnetic monopole', 'upper limit', 'nucleus, absorption', 'Cherenkov counter, water', 'deep underground detector, Baikal', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802223'],"['Supersymmetric models allow for stable non-topological solitons, Q-balls, which can be produced in the early Universe and contribute to dark matter. Experimental signature of electrically neutral Q-balls is, in fact, the same as is expected for superheavy magnetic monopoles catalyzing baryon decay. Here we use the upper limits on monopole flux obtained with deep underwater Cherenkov array ""Gyrlyanda"" which operated in the Baikal lake in 1984-90 with 267 days of live time to obtain the limit on Q-ball flux. The last has been found to be equal to 3.9 x 10^{-16} cm^{-2} sr^{-1} s^{-1} (90% CL). This result is discussed and compared with other restrictions.']",['1998-02-18'] +1689,['eng'],"['Catanese, M', 'Akerlof, Carl W', 'Badran, H M', 'Biller, S D', 'Bond, I H', 'Boyle, P J', 'Bradbury, S M', 'Buckley, J H', 'Burdett, A M', 'Gordo, J B', 'Carter-Lewis, D A', 'Cawley, M F', 'Connaughton, V', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hall, T', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Schubnell, M S', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'Wilson, C W', 'Zweerink, J A']",['Discovery of >350 GeV Gamma Rays from the BL Lacertae Object 1ES 2344+514'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'showers, air', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'experimental results', '> 350 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712325'],"['We present the discovery of >350 GeV gamma-ray emission from the BL Lacertae object 1ES 2344+514 with the Whipple Observatory 10m gamma-ray telescope. This is the third BL Lac object detected at gamma-ray energies above 300 Gev, the other two being Markarian 421 (Mrk 421) and Mrk501. These three active galactic nuclei are all X-ray selected and have the lowest known redshifts of any BL Lac objects currently identified. The evidence for emission derives primarily from an apparent flare on December 20, 1995 when a 6 sigma excess was detected with a flux approximately 63% of the very high energy gamma-ray emission from the Crab Nebula, the standard candle for TeV gamma-ray sources. Excluding the flare, observations between October 1995 and January 1996 yield a 4 sigma detection corresponding to 11% of the VHE Crab Nebula flux. Observations spanning September 1996 to January 1997 failed to yield a significant detection of a steady flux or any flaring. For this period, the 99.9% confidence level upper limit is <8% of the Crab Nebula. The low baseline emission level and variations in nightly and yearly flux of 1ES 22344+514 are the same as the VHE emission characteristics of Mrk 421 and Mrk 501']",['1997-12-25'] +1690,['eng'],"['Cillis, A N', 'Sciutto, S J']",['Geomagnetic Field and Air Shower Simulations'],['Astrophysics and Astronomy'],"['cosmic radiation', 'showers, air', 'geophysics, magnetic field', 'cosmic radiation, spatial distribution', 'muon, cosmic radiation', 'energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712345'],"['The influence of the geomagnetic field on the development of air showers is studied. The well known International Geomagnetic Reference Field was included in the AIRES air shower simulation program as an auxiliary tool to allow calculating very accurate estimations of the geomagnetic field given the geographic coordinates, altitude above sea level and date of a given event. Some test simulations made for representative cases indicate that some quantities like the lateral distribution of muons experiment significant modifications when the geomagnetic field is taken into account.']",['1997-12-31'] +1691,['eng'],"['Heiselberg, H', 'Hjorth-Jensen, M']",['Phase Transitions in Neutron Stars'],['Astrophysics and Astronomy'],"['talk, Hirschegg 1998/01/11', 'n, matter', 'rotational', 'critical phenomena', 'quark, matter', 'K, condensation', 'velocity, pulsar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802028'],"['Phase transitions in neutron stars due to formation of quark matter, kaon condensates, etc. are discussed with particular attention to the order of these transitions. Observational consequences of phase transitions in pulsar angular velocities are examined.']",['1998-02-04'] +1692,['eng'],"['Heiselberg, H']",['Kaons in Nuclear Matter'],['Astrophysics and Astronomy'],"['talk, Hirschegg 1998/01/11', 'nuclear matter', 'K, energy', 'correlation, (nucleon K)', 'correlation, (2nucleon)', 'potential, Hartree', 'potential, Lenz', 'K, condensation', 'n, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802062'],"['The kaon energy in a nuclear medium and its dependence on kaon-nucleon and nucleon-nucleon correlations is discussed. The transition from the Lenz potential at low densities to the Hartree potential at high densities can be calculated analytically by making a Wigner-Seitz cell approximation and employing a square well potential. As the Hartree potential is less attractive than the Lenz one, kaon condensation inside cores of neutron stars appears to be less likely than previously estimated.']",['1998-02-06'] +1693,['eng'],"['Albrecht, Andreas']",['What is the future of causal models of cosmic structure formation?'],['Astrophysics and Astronomy'],"['talk, Ambleside 1997/09/15', 'astrophysics, string', 'topology, defect', 'causality', 'density, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802135'],"[""Recent research has severely constrained the standard ``defect'' models of cosmic structure formation. Here I discuss the nature of the problems with defect models, and place this discussion in the context of the big picture of cosmic structure formation. In particular, I classify models of cosmic structure formation as either ``causal'' or ``acausal'', and ask whether the problems with the defect models extend to all other causal models. I argue that determining the causal nature of the primordial perturbations is within the reach of modern cosmology, and that such a determination would yield deep insights into the very early Universe.""]",['1998-02-13'] +1694,['eng'],"['Thielemann, F K', 'Rauscher, T', 'Freiburghaus, C', 'Nomoto, K', 'Hashimoto, M', 'Pfeiffer, B', 'Kratz, K L']",['Nucleosynthesis Basics and Applications to Supernovae'],['Astrophysics and Astronomy'],['review'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802077'],"['This review concentrates on nucleosynthesis processes in general and their applications to massive stars and supernovae. A brief initial introduction is given to the physics in astrophysical plasmas which governs composition changes. We present the basic equations for thermonuclear reaction rates and nuclear reaction networks. The required nuclear physics input for reaction rates is discussed, i.e. cross sections for nuclear reactions, photodisintegrations, electron and positron captures, neutrino captures, inelastic neutrino scattering, and beta-decay half-lives. We examine especially the present state of uncertainties in predicting thermonuclear reaction rates, while the status of experiments is discussed by others in this volume (see M. Wiescher). It follows a brief review of hydrostatic burning stages in stellar evolution before discussing the fate of massive stars, i.e. the nucleosynthesis in type II supernova explosions (SNe II). Except for SNe Ia, which are explained by exploding white dwarfs in binary stellar systems (which will not be discussed here), all other supernova types seem to be linked to the gravitational collapse of massive stars (M$>$8M$_\\odot$) at the end of their hydrostatic evolution. SN1987A, the first type II supernova for which the progenitor star was known, is used as an example for nucleosynthesis calculations. Finally, we discuss the production of heavy elements in the r-process up to Th and U and its possible connection to supernovae.']",['1998-02-09'] +1695,['eng'],"['Kim, J E']",['Cosmic Axion'],['Astrophysics and Astronomy'],"['talk, Tokyo 1997/11/17', 'strong interaction, CP', 'potential, axion', 'mass, axion', 'astrophysics', 'search for, axion', 'domain wall', 'string model', 'coupling, (axion 2photon)']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802061'],['I review the axionic solution of the strong CP problem and current status of the cosmic axion search.'],['1998-02-06'] +1696,['eng'],"['Grasso, D']",['Neutrino oscillations in magnetized media and implications for the pulsar velocity puzzle'],['Astrophysics and Astronomy'],"['talk, Valencia 1997/10/13', 'neutrino, oscillation', 'resonance, oscillation', 'neutrino, potential', 'matter, magnetic', 'velocity, pulsar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9802060'],['After a brief presentation of the general techniques used to determine neutrino potentials in a magnetized medium I will discuss MSW resonant oscillations of active and sterile neutrinos in such environment. Using my results I will reconsider the viability of a solution of the pulsar velocity puzzle based on such a kind of neutrino oscillations.'],['1998-02-06'] +1697,['eng'],"['Tanimori, T', 'Hayami, Y', 'Kamei, S', 'Dazeley, S A', 'Edwards, P G', 'Gunji, S', 'Hara, S', 'Hara, T', 'Holder, J', 'Kawachi, A', 'Kifune, T', 'Kita, R', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Matsuoka, T', 'Mizumoto, Y', 'Mori, M', 'Moriya, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Oda, S', 'Ogio, S', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sakurazawa, K', 'Sako, T', 'Sato, Y', 'Susukita, R', 'Suzuki, A', 'Suzuki, R', 'Tamura, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['Discovery of TeV Gamma Rays from SN1006'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'astrophysics, supernova', 'cosmic radiation, background', 'acceleration, shock waves', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801275'],"['This paper reports the first discovery of TeV gamma-ray emission from a supernova remnant made with the CANGAROO 3.8 m Telescope. TeV gamma rays were detected at the sky position and extension coincident with the north-east (NE) rim of shell-type Supernova remnant (SNR) SN1006 (Type Ia). SN1006 has been a most likely candidate for an extended TeV Gamma-ray source, since the clear synchrotron X-ray emission from the rims was recently observed by ASCA (Koyama et al. 1995), which is a strong evidence of the existence of very high energy electrons up to hundreds of TeV in the SNR. The observed TeV gamma-ray flux was $(2.4\\pm 0.5(statistical) \\pm 0.7(systematic)) \\times 10^{-12}$ cm$^{-2}$ s$^{-1}$ ($\\ge 3.0\\pm 0.9$ TeV) and $ (4.6\\pm 0.6 \\pm 1.4) \\times 10^{-12}$ cm$^{-2}$ s$^{-1}$ ($\\ge 1.7\\pm 0.5$ TeV) from the 1996 and 1997 observations, respectively. Also we set an upper limit on the TeV gamma-ray emission from the SW rim, estimated to be $ 1.1 \\times 10^{-12}$ cm$^{-2}$ s$^{-1}$ ($\\ge 1.7\\pm 0.5$ TeV, 95% CL) in the 1997 data. The TeV gamma rays can be attributed to the 2.7 K cosmic background photons up-scattered by electrons of energies up to about 10$^{14}$ eV by the inverse Compton (IC) process. The observed flux of the TeV gamma rays, together with that of the non-thermal X-rays, gives firm constraints on the acceleration process in the SNR shell; a magnetic field of $6.5\\pm2$ $\\mu$G is inferred from both the synchrotron X-rays and inverse Compton TeV gamma-rays, which gives entirely consistent mechanisms that electrons of energies up to 10$^{14}$ eV are produced via the shock acceleration in SN1006.']",['1998-01-29'] +1698,['eng'],"['Burrows, A', 'Sawyer, R F']",['The Effects of Correlations on Neutrino Opacities in Nuclear Matter'],['Astrophysics and Astronomy'],"['neutrino nucleon, elastic scattering', 'neutral current', 'nuclear matter, effect', 'nuclear force', 'nucleon nucleon, correlation', 'fermion, statistics', 'thermodynamics', 'differential cross section, energy', 'nucleon, structure function', 'nucleon nucleon, potential', 'nuclear physics, collective phenomena', 'astrophysics, supernova', 'n, matter', 'neutrino, luminosity', 'time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801082'],"['Including nucleon-nucleon correlations due to both Fermi statistics and nuclear forces, we have developed a general formalism for calculating the neutral-current neutrino-nucleon opacities in nuclear matter. We derive corrections to the dynamic structure factors due to both density and spin correlations and find that neutrino-nucleon cross sections are suppressed by large factors around and above nuclear density. In addition, we find that the spectrum of energy transfers in neutrino scattering is considerably broadened by the interactions in the medium. An identifiable component of this broadening comes from the absorption and emission of quanta of collective modes akin to the Gamow-Teller and Giant Dipole resonances in nuclei (zero-sound; spin waves), with \\v{C}erenkov kinematics. Under the assumption that both the charged-current and the neutral-current cross sections are decreased by many-body effects, we calculate a set of ad hoc protoneutron star cooling models to gauge the potential importance of the new opacities to the supernova itself. We find that after many hundreds of milliseconds to seconds the driving neutrino luminosities might be increased by from 10% to 100%. However, the actual consequences, if any, of these new neutrino opacities remain to be determined.']",['1998-01-13'] +1699,['eng'],"['Fiorentini, G', 'Ricci, B']",['Solar neutrinos'],['Astrophysics and Astronomy'],"['talk, Valencia 1997/10/13', 'neutrino, solar', 'model, solar', 'neutrino, flux', 'deep underground detector', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801185'],"['We summarize the results of solar neutrino experiments and update a solar model independent analysis of solar neutrino data. We discuss the implications of helioseismology on solar models and predicted solar neutrino fluxes. Finally , we discuss the potential of new experiments for detecting specific signatures of the proposed solutions to the solar neutrino puzzle.']",['1998-01-21'] +1700,['eng'],"['Zioutas, Konstantin', 'Aalseth, C E', 'Abriola, D', 'Avignone, F T', 'Brodzinski, R L', 'Collar, J I', 'Creswick, R J', 'Gregorio, D E D', 'Farach, H A', 'Gattone, A O', 'Guérard, C K', 'Hasenbalg, F', 'Hasinoff, M', 'Huck, H', 'Liolios, A', 'Miley, H S', 'Morales, A', 'Morales, J', 'Nikas, D', 'Nussinov, S', 'Ortiz, A', 'Savvidis, E', 'Scopel, S', 'Sievers, P', 'Villar, J A', 'Walckiers, L']",['A Decommissioned LHC Model Magnet as an Axion Telescope'],['Astrophysics and Astronomy'],"['search for, axion', 'axion, solar', 'photon, production', 'magnetic field', 'Primakoff effect', 'bending magnet, superconducting', 'semiconductor detector, germanium', 'proposed experiment', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801176'],"['The 8.4 Tesla, 10 m long transverse magnetic field of a twin aperture LHC bending magnet can be utilized as a macroscopic coherent solar axion-to-photon converter. Numerical calculations show that the integrated time of alignment with the Sun would be 33 days per year with the magnet on a tracking table capable of $\\pm 5^o$ in the vertical direction and $\\pm 40^o$ in the horizontal direction. The existing lower bound on the axion-to-photon coupling constant can be improved by a factor between 50 and 100 in 3 years, i.e., ${\\it g_{a\\gamma \\gamma}} \\lesssim 9\\cdot 10^{-11}$ GeV$^{-1}$ for axion masses The same set-up can simultaneously search for low- and high-energy celestial axions, or axion-like particles, scanning the sky as the Earth rotates and orbits the Sun.']",['1998-01-20'] +1701,['eng'],"['Hagmann, C', 'Kinion, D S', 'Stoeffl, W', 'Van Bibber, K', 'Daw, E J', 'Peng, H', 'Rosenberg, L J', 'La Veigne, J D', 'Sikivie, P', 'Sullivan, N', 'Tanner, D B', 'Nezrick, F', 'Turner, M S', 'Moltz, D M', 'Powell, J', 'Golubev, N A']",['Results from a High-Sensitivity Search for Cosmic Axions'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'search for, axion', 'axion, radiative decay', 'mass, axion', 'coupling, axion', 'magnetic detector, superconducting', 'RF system', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801286'],['We report the first results of a high-sensitivity (10^{-23} Watt) search for light halo axions through their conversion to microwave photons. At 90 percent confidence we exclude a KSVZ axion of mass 2.9 x 10^{-6} eV to 3.3 x 10^{-6} eV as the dark matter in the halo of our Galaxy.'],['1998-01-29'] +1702,['eng'],"['Bonazzola, S', 'Gourgoulhon, E']",['Strategy to detect the gravitational radiation counterpart of gamma-ray bursts'],['Astrophysics and Astronomy'],"['talk, Orsay 1997/11/13', 'gravitational radiation, counters and detectors', 'n, matter', 'astrophysics', 'photon, cosmic radiation', 'gravitational radiation, particle source', 'background', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801162'],"['Both observational and theoretical rates of binary neutron star coalescence give low prospects for detection of a single event by the initial LIGO/VIRGO interferometers. However, by utilizing at the best all the a priori information on the expected signal, a positive detection can be achieved. This relies on the hypothesis that $\\gamma$-ray bursts are the electromagnetic signature of neutron star coalescences. The information about the direction of the source can then be used to add in phase the signals from different detectors in order (i) to increase the signal-to-noise ratio and (ii) to make the noise more Gaussian. Besides, the information about the time of arrival can be used to drastically decrease the observation time and thereby the false alarm rate. Moreover the fluence of the $\\gamma$-ray emission gives some information about the amplitude of the gravitational signal. One can then add the signals from years) to yield a positive detection. Such a detection, based on the Maximum a Posteriori Probability Criterium, is a minimal one, in the sense that no information on the position and time of the events, nor on any parameter of the model, is collected. The advantage is that this detection requires an improvement of the detector sensitivity by a factor of only $\\sim 1.5$ with respect to the initial LIGO/VIRGO interferometers, and that, if positive, it will confirm the $\\gamma$-ray burst model.']",['1998-01-19'] +1703,['eng'],"['Widerin, P', 'Schmid, C']",['Primordial black hole formation caused by the QCD transition?'],['Astrophysics and Astronomy'],"['talk, Ambleside 1997/09/15', 'astrophysics, model', 'black hole, production', 'density, perturbation', 'quantum chromodynamics', 'critical phenomena', 'temperature', 'space-time, horizon', 'relativity theory, general']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801163'],"['We consider the evolution of cosmological perturbations at the QCD transition, in particular the sudden reheating from a supercooled universe to the transition temperature. Sudden reheating happens at a specific temperature, hence density, and singles out one specific hypersurface. Underdensities reach the reheating earlier than overdensities, there is a short period of huge pressure differences which leads to a jump in the fluid velocity. Density perturbations of scales far below the Hubble radius $\\lambda\\ll R_H $ get an amplification which grows quadratically in wavenumber. Primordial black hole formation will not be sufficiently amplified by the QCD transition unless the initial spectrum is fine tuned.']",['1998-01-19'] +1704,['eng'],"['Capelle, K S', 'Cronin, J W', 'Parente, G', 'Zas, E']",['On the detection of Ultra High Energy Neutrinos with the Auger Observatory'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, energy spectrum', 'showers, air', 'cosmic radiation, flux', 'neutrino nucleus, deep inelastic scattering', 'charged current', 'neutral current', 'showers, hadronic', 'counters and detectors, acceptance', 'counters and detectors, proposed', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801313'],['We show that the Auger Air Shower Array has the potential to detect neutrinos of energies in the $10^{19}~$eV range through horizontal air showers. Assuming some simple conservative trigger requirements we obtain the acceptance for horizontal air showers as induced by high energy neutrinos by two alternative methods and we then give the expected event rates for a variety of neutrino fluxes as predicted in different models which are used for reference.'],['1998-02-02'] +1705,['eng'],"['Luminet, J P']",['Black Holes'],['Astrophysics and Astronomy'],"['introductory', 'black hole, production', 'relativity theory, general', 'space-time', 'thermodynamics', 'photon, cosmic radiation', 'galaxy', 'cosmic radiation, particle source']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801252'],"[""Our understanding of space and time is probed to its depths by black holes. These objects, which appear as a natural consequence of general relativity, provide a powerful analytical tool able to examine macroscopic and microscopic properties of the universe. This introductory article presents in a pictorial way the basic concepts of black hole's theory, as well as a description of the astronomical sites where black holes are suspected to lie, namely binary X-ray sources and galactic nuclei.""]",['1998-01-27'] +1706,['eng'],"['Wandelt, B D']",['Primordial Non-Gaussianity'],['Astrophysics and Astronomy'],"['astrophysics, string', 'gas', 'model, fluid', 'astrophysics, missing-mass', 'model, hydrodynamical', 'dimension, 3', 'baryon, density', 'galaxy, cluster', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801267'],"[""I compute the 3-D non-linear evolution of gas and dark matter fluids in the neighbourhood of cosmic string wakes which are formed at high redshift ($z\\simeq 2240$) for a ``realistic'' scenario of wake formation. These wakes are the ones which stand out most prominently as cosmological sheets and are expected to play a dominant rôle in the cosmic string model of structure formation. Employing a high-resolution 3-D hydrodynamics code to evolve these wakes until the present day yields results for the baryon bias generated in the inner wake region. I find that today, wakes would be $1.5 h^{-1}$ Mpc thick and contain a 70% excess in the density of baryons over the dark matter density in their centre. However, high density peaks in the wake region do not inherit a baryon enhancement. I propose a mechanism for this erasure of the baryon excess in spherically collapsed objects based on the geometry change around the collapsing region. Further, I present heuristic arguments for the consequences of this work for large scale structure in the cosmic string model and conclude that the peculiarities of wake formation are unlikely to have significant import on the discrepancy between power spectrum predictions and observations in this model. If one invokes the nucleosynthesis bound on $\\Omega_b$ this could be seen as strengthening the case against $\\Omega_m=1$ or for low Hubble constants.""]",['1998-01-28'] +1707,['eng'],"['Bilic, N', 'Munyaneza, F', 'Viollier, R D']",['Stars and Halos of Degenerate Relativistic Heavy-Neutrino and Neutralino Matter'],['Astrophysics and Astronomy'],"['neutrino, heavy', 'neutrino, matter', 'neutralino, matter', 'relativistic', 'matter, mass', 'astrophysics, missing-mass', 'neutrino, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801262'],['Heavy-neutrino (or neutralino) stars are studied using the general relativistic equations of hydrostatic equilibrium and the relativistic equation of state for degenerate fermionic matter. The Tolman-Oppenheimer-Volkoff equations are then generalized to include a system of degenerate neutrino and neutralino matter that is gravitationally coupled. The properties and implications of such an interacting astrophysical system are discussed in detail.'],['1998-01-28'] +1708,['eng'],"['Dawson, B R', 'Meyhandan, R', 'Simpson, K M']",['A Comparison of Cosmic Ray Composition Measurements at the Highest Energies'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'p, cosmic radiation', 'iron, cosmic radiation', 'cosmic radiation, flux', 'flux, ratio', 'cosmic radiation, showers', 'cosmic radiation, secondary radiation', 'muon, flux', 'model, hadronic', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801260'],"[""In recent years the Fly's Eye and Akeno groups have presented analyses of the cosmic ray mass composition at energies above 10^17 eV. The experiments employ different mass composition parameters - for the Fly's Eye it is X_max, the depth of maximum shower development, and for Akeno it is the muon content of showers at fixed energy. While the analysis of the Fly's Eye group points to a likely change in mass composition from heavy to light at energies above 10^18 eV, the Akeno analysis favours an unchanging composition. However, the two groups base their conclusions on simulations using quite different hadronic models. Here we present a comparison of the experiments using the same hadronic model.""]",['1998-01-28'] +1709,['eng'],"['Bergé, L', 'Berkès, I', 'Chambon, B', 'Chapellier, M', 'Chardin, G', 'Charvin, P', 'De Jésus, M', 'Stefano, P D', 'Drain, D', 'Dumoulin, L', 'Goldbach, C', 'Juillard, A', ""L'Hôte, D"", 'Marnieros, S', 'Miramonti, L', 'Mosca, L', 'Navick, X F', 'Nollez, G', 'Pari, P', 'Pastor, C', 'Pécourt, S', 'Tourbot, R', 'Yvon, D']",['Status of the EDELWEISS Experiment'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'astrophysics, missing-mass', 'WIMP, annihilation', 'ionization, temperature', 'bolometer, germanium', 'calibration', 'deep underground detector, proposed', 'particle identification, (n photon)', 'effect, surface']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801199'],"['The status of the EDELWEISS experiment (underground dark matter search with heat-ionisation bolometers) is reviewed. Auspicious results achieved with a prototype 70 g Ge heat-ionisation detector under a 2 V reverse bias tension are discussed. Based on gamma and neutron calibrations, a best-case rejection factor, over the 15-45 keV range, of 99.7 % for gammas, with an acceptance of 94 % for neutrons, is presented first. Some operational results of physical interest obtained under poor low radioactivity conditions follow. They include a raw event rate of around 30 events/day/kg/keV over the same energy range, and, after rejection of part of the background, lead to a conservative upper limit on the signal of approximately 1.6 events/day/kg/keV at a 90 % confidence level. Performance degrading surface effects of the detector are speculated upon; and planned upgrades are summarized.']",['1998-01-22'] +1710,['eng'],"['Schertler, K', 'Greiner, C', 'Thoma, M H']",['Medium effects and the structure of neutron stars in the effective mass bag model'],['Astrophysics and Astronomy'],"['talk, Hirschegg 1998/01/11', 'n, matter', 'quark, strangeness', 'bag model, mass spectrum', 'matter, hybrid', 'matter, hadronic', 'critical phenomena, confinement', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801200'],['One of the most intriguing consequence of the extreme conditions inside neutron stars is the possibility of the natural existence of a deconfined strange quark matter phase in the high density interior of the star. The equation of state (EOS) of strange quark matter (SQM) was recently improved in the framework of the MIT bag model by including medium effects. It was found that medium effects increase the energy per baryon of SQM and therefore lower the stability of this phase. In this work we investigate the influence of medium effects on the structure of hybrid stars within this model. We found that the medium effects reduce the extent of a pure SQM phase in the interior of an hybrid star significantly in favor of a mixed phase of quark and hadronic matter.'],['1998-01-22'] +1711,['eng'],"['Yoshikoshi, T', 'Kifune, T', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Hayami, Y', 'Kakimoto, F', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Matsuoka, T', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Oda, S', 'Ogio, S', 'Ohsaki, T', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Suzuki, A', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T']",['Very High Energy $\\gamma$ Rays from the Vela Pulsar Direction'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, pulsar', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707203'],"['We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cherenkov telescope near Woomera, South Australia between January 1993 and March 1995. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 sigma level. The detected gamma-ray flux is (2.9 +/- 0.5 +/- 0.4) x 10^-12 photons cm^-2 sec^-1 above 2.5 +/- 1.0 TeV and the signal is consistent with steady emission over the two years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0.13 deg. No pulsed emission modulated with the pulsar period has been detected and the 95 % confidence flux upper limit to the pulsed emission from the pulsar is (3.7 +/- 0.7) x 10^-13 photons cm^-2 sec^-1 above 2.5 +/- 1.0 TeV.']",['1997-07-25'] +1712,['eng'],"['Tanimori, T', 'Sakurazawa, K', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Hayami, Y', 'Kamei, S', 'Kita, R', 'Kifune, T', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Susukita, R', 'Suzuki, A', 'Suzuki, R', 'Tamura, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['Detection of $\\gamma$-Rays of up to 50 TeV from the Crab Nebula'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, background', 'cosmic radiation, particle source', 'Compton scattering', 'cosmic radiation, correlation', 'Cherenkov counter, imaging', 'experimental results', '< 50000 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710272'],"['Gamma rays with energies greater than 7 TeV from the Crab pulsar/nebula have been observed at large zenith angles, using the Imaging Atmospheric Technique from Woomera, South Australia. CANGAROO data taken in 1992, 1993 and 1995 indicate that the energy spectrum extends up to at least 50 TeV, without a change of the index of the power law spectrum. The observed differential spectrum is \\noindent $(2.01\\pm 0.36)\\times 10^{-13}(E/{7 TeV})^{-2.53 \\pm 0.18} TeV^{-1}cm^{-2}s^{-1}$ between 7 TeV and 50 TeV. There is no apparent cut-off. The spectrum for photon energies above $\\sim$10 TeV allows the maximum particle acceleration energy to be inferred, and implies that this unpulsed emission does not originate near the light cylinder of the pulsar, but in the nebula where the magnetic field is not strong enough to allow pair creation from the TeV photons. The hard gamma-ray energy spectrum above 10 TeV also provides information about the varying role of seed photons for the inverse Compton process at these high energies, as well as a possible contribution of']",['1997-10-27'] +1713,['eng'],"['Argyres, Philip C', 'Barvinsky, A O', 'Frolov, V', 'Giddings, Steven B', 'Lowe, D A', 'Strominger, A', 'Thorlacius, L']",['Quantum aspects of gravity'],['Astrophysics and Astronomy'],"['talk', 'black hole', 'effect, back reaction', 'quantum gravity', 'effective action, nonlocal', 'form factor']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412046'],"['Contributions from the G1 Working Group at the APS Summer Study on Particle and Nuclear Astrophysics and Cosmology in the Next Millennium, Snowmass, Colorado, June 29 - July 14, 1994. V. Frolov and L. Thorlacius: Quantum Aspects of Gravity. S.B. Giddings and L. Thorlacius: Introduction to the Information Problem. A. Strominger: Two-Dimensional Black Holes and the Information Puzzle. V. Frolov: Entropy of Black Holes. L. Thorlacius: Black Hole Complementarity. D.A. Lowe: Causality in String Theory. A.O. Barvinski: Nonlocal Effective Action and Black Holes. P.C. Argyres: Universality and Scaling in Black Hole Formation.']",['1994-12-14'] +1714,['eng'],"['Totani, T']",['$\\gamma$-Ray Bursts from Neutron Star Mergers and Evolution of Galaxies'],['Astrophysics and Astronomy'],"['talk, Tokyo 1997/11/11', 'photon, cosmic radiation', 'astrophysics, galaxy', 'n, matter', 'cosmic radiation, luminosity', 'energy, emission', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801105'],"['Most of proposed models of cosmological gamma-ray bursts (GRBs) are associated to gravitational collapses of massive stars, and hence evolution of the GRB rate, which is crucially important in GRB intensity distribution analysis, is determined by the cosmic star formation history. Here we present complementary results of GRB logN-logP analysis, which were omitted in the previous paper (Totani 1997, ApJ, 486, L71). A unique feature of the binary neutron-star merger scenario, in contrast to other scenarios associated to single stellar collapses, is that a time delay during binary spiral-in phase emitting gravitational waves is not negligible and makes the rate evolution flatter than that of star formation rate. We show that binary merger scenario is more favored than single stellar collapses. The estimated peak luminosity and total emitted energy in rest-frame 50-300 keV range is 1--3 $\\times 10^{51} respectively, where $Ømega$ is opening angle of gamma-ray emission. Absolute rate comparison between GRBs and neutron-star mergers suggests that a beaming factor of $(Ømega/4\\pi)^{-1} \\sim$ a few hundreds is required. High-$z$ SFR data ($z>2$) based on UV luminosity need to be corrected upwards by a factor of 5--10 for a good fit, and this is likely explained by the dust extinction effect.']",['1998-01-14'] +1715,['eng'],"['Lindner, A']",['A New Method to Reconstruct the Energy and Determine the Composition of Cosmic Rays from the Measurement of Cherenkov Light and Particle Densities in Extensive Air Showers'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy', 'elements, cosmic radiation', 'cosmic radiation, electromagnetic component', 'showers, air', 'showers, spatial distribution', 'radiation, Cherenkov', 'radiation, density', 'shower detector', 'Cherenkov counter', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801147'],['A Monte-Carlo study to reconstruct energy and mass of cosmic rays with energies above 300 TeV using ground based measurements of the electromagnetic part of showers initiated in the atmosphere is presented. The shower properties determined with two detector arrays measuring the air Cherenkov light and the particle densities as realized at the HEGRA experiment are processed to determine the energy of the primary particle without the need of any hypothesis concerning its mass. The mass of the primary particle is reconstructed coarsely from the same observables in parallel to the energy determination.'],['1998-01-16'] +1716,['eng'],"['De Vega, H J', 'Sánchez, N', 'Combes, F']",['Fractal Dimensions and Scaling Laws in the Interstellar Medium and Galaxy Distributions'],['Astrophysics and Astronomy'],"['talk, Erice 1997/09/04', 'astrophysics, galaxy', 'gravitation, gas', 'nonrelativistic', 'field theoretical model', 'renormalization group', 'temperature', 'scaling, finite size', 'correlation, density', 'critical phenomena', 'fractals', 'field theory, scalar', 'dimension, 3', 'Ising model', 'mean field approximation', 'statistical analysis', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801115'],"['We develop a field theoretical approach to the cold interstellar medium (ISM) and large structure of the universe. We show that a non-relativistic self- gravitating gas in thermal equilibrium with variable number of atoms or fragments is exactly equivalent to a field theory of a scalar field phi(x) with exponential self-interaction. We analyze this field theory perturbatively and non-perturbatively through the renormalization group(RG).We show scaling behaviour (critical) for a continuous range of the physical parameters as the temperature. We derive in this framework the scaling relation M(R) \\sim R^{d_H} for the mass on a region of size R, and Delta v \\sim R^\\frac12(d_H -1) for the velocity dispersion. For the density-density correlations we find a power-law behaviour for large distances \\sim |r_1 - r_2|^{2D - 6}.The fractal dimension D turns to be related with the critical exponent \\nu by D = 1/ \\nu. Mean field theory yields \\nu = 1/2, D = 2. Both the Ising and the mean field values are compatible with the present ISM observational data:1.4\\leq D \\leq 2. We develop a field theoretical approach to the galaxy distribution considering a gas of self-gravitating masses on the FRW background, in quasi-thermal equi- librium. We show that it exhibits scaling behaviour by RG methods. The galaxy correlations are computed without assuming homogeneity. We find <\\rho({\\vec r_0})\\rho({\\vec r_0} + {\\vec r}) > \\sim r^{D-3} $. The theory allows to compute the three and higher density correlators without any assumption.We find that the connected N-points density scales as r_1^{N(D-3)}, when $ r_1 >> r_i,']",['1998-01-14'] +1717,['eng'],"['Liddle, A R']",['Inflation and the cosmic microwave background'],['Astrophysics and Astronomy'],"['talk, Porto 1997/11/24', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'density, perturbation', 'astrophysics, missing-mass', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801148'],"['I give a status report and outlook concerning the use of the cosmic microwave background anisotropies to constrain the inflationary cosmology, and stress its crucial role as an underlying paradigm for the estimation of cosmological parameters.']",['1998-01-16'] +1718,['eng'],"['Bulian, N', 'Daum, A', 'Hermann, G', 'Hess, M', 'Hofmann, W', 'Lampeitl, H', 'Pühlhofer, G', 'Köhler, C', 'Panter, M', 'Stein, M L', 'Boerst, G', 'Rauterberg, G', 'Samorski, M', 'Sauerland, C', 'Stamm, W']",['Characteristics of the Multi-Telescope Coincidence Trigger of the HEGRA IACT System'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'Cherenkov counter', 'trigger']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712063'],"['The HEGRA--collaboration is operating a system of imaging atmospheric Cherenkov telescopes to search for sources of TeV-gamma-rays. Air showers are observed in stereoscopic mode with several telescopes simultaneously. To trigger the telescope system a versatile two-level trigger scheme has been implemented, which allows a significant reduction of the energy threshold with respect to single telescopes. The technical implementation of this trigger scheme and the performance of the trigger system are described. Results include the dependence of single- and multi-telescope trigger rates on the trigger thresholds, on the orientation of the telescopes, and on the type of the primary particle.']",['1997-12-08'] +1719,['eng'],"['Totani, T']",['Electron Neutrino Mass Measurement by Supernova Neutrino Bursts and Implications on Hot Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, cosmic radiation', 'neutrino/e, mass', 'mass, measurement', 'mass, hierarchy', 'astrophysics, missing-mass', 'deep underground detector', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801104'],"['We present a new strategy for measuring the electron neutrino mass ($\\mnue$) by future detection of a Galactic supernova in large underground detectors such as the Super-Kamiokande (SK). This method is nearly model-independent and one can get a mass constraint in a straightforward way from experimental data without specifying any model parameters for profiles of supernova neutrinos. We have tested this method using virtual data generated from a numerical model of supernova neutrino emission by realistic Monte-Carlo simulations of the SK detection. It is shown that this method is sensitive to $\\mnue$ of $\\sim$ 3 eV for a Galactic supernova, and this range is as low as the prediction of the cold+hot dark matter scenario with a nearly degenerate mass hierarchy of neutrinos, which is consistent with the current observations of solar and atmospheric neutrino anomalies and density fluctuations in the universe.']",['1998-01-14'] +1720,['eng'],"['Cardall, C Y', 'Fuller, G M']",['Semianalytic Analysis of Primordial Black Hole Formation During a First-order QCD Phase Transition'],['Astrophysics and Astronomy'],"['black hole, production', 'quantum chromodynamics', 'critical phenomena', 'density, perturbation', 'black hole, mass spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801103'],"[""It has recently been suggested that cosmologically significant numbers of black holes could form during a first-order QCD phase transition. Further, it has been asserted that these black holes would have masses corresponding naturally to the inferred mass ($\\sim 1 M_{\\odot}$) of the MACHOs responsible for the observed gravitational microlensing events. In this model, the underlying spectrum of primordial density perturbations provides the fluctuations that give rise to black holes at the epoch of the QCD transition. We employ a simplified model to estimate the reduction in the critical overdensity of a horizon-sized primordial perturbation required for collapse to a black hole. We find that a first-order QCD transition does indeed produce a sharp peak in the black hole mass spectrum, but that this peak corresponds to the horizon mass at an epoch somewhat earlier than the cosmological transition itself. Assuming a COBE normalized primordial density perturbation spectrum with constant spectral index, for the black holes so produced to be cosmologically significant would require an extremely finely tuned ``blue'' primordial density perturbation spectrum. Specifically, in the context of our simplified model, a spectral index in the range $n=1.37-1.42$ corresponds to the range $\\Omega \\sim 10^{-5}-10^3$ of the black hole contribution to the present-day density parameter.""]",['1998-01-14'] +1721,['eng'],"['Shi, X', 'Fuller, G M']",['Neutrinos and Supermassive Stars'],['Astrophysics and Astronomy'],"['astrophysics, matter', 'electron positron, annihilation', 'neutrino, emission', 'neutrino, energy spectrum', 'luminosity', 'neutrino, flux', 'neutrino, background', 'counters and detectors', 'signal processing', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801106'],['We calculate the luminosity and energy spectrum of the neutrino emission from electron-positron pair annihilation during the collapse of a supermassive star (${M} \\ga 5\\times10^4 {M_\\odot}$). We then estimate the cumulative flux and energy spectrum of the resulting neutrino background as a function of the abundance and redshift of supermassive stars and the efficiency of these objects in converting gravitational energy into neutrino energy. We estimate the expected signal in some of the new generation of astrophysical neutrino detectors from both a cumulative background of supermassive stars and single collapse events associated with these objects.'],['1998-01-14'] +1722,['eng'],"['Fiorentini, G', 'Moretti, M', 'Villante, F L']",['The anisotropy of inverse $\\beta$ decay and antineutrino detection'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'antineutrino p, exclusive reaction', 'antineutrino/e', 'positron, neutrinoproduction', 'angular distribution, anisotropy', 'antineutrino, solar', 'neutrino antineutrino, transition', 'astrophysics, supernova', 'astrophysics, galaxy', 'neutrino electron, elastic scattering', 'numerical calculations', 'deep underground detector, KAMIOKANDE']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801111'],"['The anisotropy of the positrons emitted in the reaction $\\bar{\\nu}_{e}+p\\to n+e^{+}$ has to be taken into account for extracting an antineutrino signal in Superkamiokande. For the Sun, this effect allows a sensitivity to the statistics collected in the first hundred days. For a supernova in the Galaxy, the effect is crucial for extracting the correct ratio of $\\nu-e$ to']",['1998-01-14'] +1723,['eng'],"['Ellis, R S']",['The Formation and Evolution of Galaxies'],['Astrophysics and Astronomy'],['review'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801113'],"['I review recent observational progress concerning the evolution of the morphological distribution of galaxies in the rich cluster environment and in the faint field population. By coupling HST imagery with ground-based spectroscopic diagnostics, evidence accumulates that galaxy morphology can be a transient phenomenon reflecting various changes in the star formation rate. Possible physical processes responsible for these changes are discussed. Future progress in understanding them will depend on securing 2-D spectroscopic data for representative systems.']",['1998-01-14'] +1724,['eng'],"['Hardy, S J', 'Melrose, D B']",['Langmuir Wave Generation Through A Neutrino Beam Instability'],['Astrophysics and Astronomy'],"['neutrino, beam instability', 'neutrino, radiative decay', 'Feynman graph, higher-order', 'electroweak interaction', 'expansion, mass', 'W, mass', 'plasma, dispersion relations', 'astrophysics, supernova', 'model, shock waves', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801090'],"['A standard version of a kinetic instability for the generation of Langmuir waves by a beam of electrons is adapted to describe the analogous instability due to a beam of neutrinos. The interaction between a Langmuir wave and a neutrino is treated in the one-loop approximation to lowest order in an expansion in $1/M_W^2$ in the standard electroweak model. It is shown that this kinetic instability is far too weak to occur in a suggested application to the reheating of the plasma behind a stalled shock in a type II supernova (SN). This theory is also used to test the validity of a previous analysis of a reactive neutrino beam instability and various shortcomings of this theory are noted. In particular, it is noted that relativistic plasma effects have a significant effect on the calculated growth rates, and that any theoretical description of neutrino-plasma interactions must be based directly on the electroweak theory. The basic scalings discussed in this paper suggest that a more complete investigation of neutrino-plasma processes should be undertaken to look for an efficient process capable of driving the stalled shock of a type II SN.']",['1998-01-13'] +1725,['eng'],"['Berezinsky, Veniamin Sergeevich']",['Ultra High Energy Cosmic Rays from Decaying Superheavy Particles'],['Astrophysics and Astronomy'],"['talk, College Park 1997/11/13', 'cosmic radiation, energy spectrum', 'topology, defect', 'cosmic radiation, particle source', 'magnetic monopole', 'supersymmetry', 'sparticle, mass', 'LSP, neutral particle', 'LSP, gluino', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801046'],"['Decaying superheavy particles can be produced by Topological Defects or, in case they are quasi-stable, as relics from the early Universe. The decays of these particles can be the sources of observed Ultra High Energy Cosmic Rays ($E \\sim 10^{10} - 10^{12} GeV$). The Topological Defects as the UHE CR sources are critically reviewed and cosmic necklaces and monopole-antiminopole pairs are identified as most plausible sources. The relic superheavy particles are shown to be clustering in the halo and their decays produce UHE CR without GZK cutoff. The Lightest Supersymmetric Particles with Ultra High Energies are naturally produced in the cascades accompanying the decays of superheavy particles. These particles are discussed as UHE carriers in the Universe.']",['1998-01-08'] +1726,['eng'],"['Spiering, C', 'Balkanov, V A', 'Belolaptikov, I A', 'Bezrukov, L B', 'Budnev, N M', 'Chensky, A G', 'Danilchenko, I A', 'Djilkibaev, Z A M', 'Domogatsky, G V', 'Doroshenko, A A', 'Fialkovsky, S V', 'Gaponenko, O N', 'Garus, A A', 'Gress, T I', 'Klabukov, A M', 'Klimov, A I', 'Klimushin, S I', 'Koshechkin, A P', 'Kulepov, V F', 'Kuzmichev, L A', 'Lovtsov, S V', 'Lubsandorzhiev, B K', 'Milenin, M B', 'Mirgazov, R R', 'Moroz, A V', 'Moseiko, N I', 'Nikiforov, S A', 'Osipova, E A', 'Panfilov, A I', 'Parfenov, Yu V', 'Pavlov, A A', 'Petukhov, D P', 'Pokhil, P G', 'Pokolev, P A', 'Popova, E G', 'Rozanov, M I', 'Rubzov, V Yu', 'Sokalski, I A', 'Spiering, C', 'Streicher, O', 'Tarashansky, B A', 'Thon, T', 'Wischnewski, R', 'Yashin, I V']",['The Baikal Deep Underwater Neutrino Experiment'],['Astrophysics and Astronomy'],"['talk, Erice 1997/09/16', 'muon, cosmic radiation', 'neutrino, cosmic radiation', 'WIMP, annihilation', 'search for, magnetic monopole', 'flux, upper limit', 'deep underground detector, Baikal', 'Cherenkov counter, water', 'electronics', 'track data analysis', 'particle identification', 'performance', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801044'],"['We review the present status of the Baikal Underwater Neutrino Experiment and present results obtained with the various stages of the stepwise increasing detector: NT-36 (1993-95), NT-72 (1995-96) and NT-96 (1996-97). Results cover atmospheric muons, first clear neutrino events, search for neutrinos from WIMP annihilation in the center of the Earth, search for magnetic monopoles, and -- far from astroparticle physics -- limnology.']",['1999-06-16'] +1727,['eng'],"['Schertler, K', 'Greiner, C', 'Sahu, P K', 'Thoma, M H']",['The influence of medium effects on the gross structure of hybrid stars'],['Astrophysics and Astronomy'],"['astrophysics', 'matter, hybrid', 'quark, strangeness', 'matter, hadronic', 'n, matter', 'critical phenomena', 'bag model', 'mass spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712165'],"['We investigate the influence of medium effects on the structure of hybrid stars, i.e. neutron stars possessing a quark matter core. We found that medium effects reduce the extent of a pure quark matter phase in the interior of a hybrid star significantly in favor of a mixed phase of quark and hadronic matter. Over a wide range of the strong coupling constant - which parameterizes the influence of medium effects - quark matter is able to exist at least in a mixed phase in the interior of neutron stars.']",['1997-12-15'] +1728,['eng'],"['Medina-Tanco, G A']",['On the significance of the observed clustering of ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, cluster', 'cosmic radiation, energy spectrum', 'astrophysics, galaxy', 'magnetic field', 'astrophysics, model', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801060'],"['Three pairs of possibly correlated ultra-high energy cosmic ray events were reported by Hayashida et al (1996). Here we calculate the propagation of the corresponding particles through both the intergalactic and galactic magnetic fields. The large scale disc and halo magnetic components are approximated by the models of Stanev (1997). The intergalactic magnetic field intensity is modulated by the actual density of luminous matter along the corresponding lines of sight, calculated from the CfA redshift catalogue (Huchra et al, 1995). The results indicate that, if the events of each pair had a common source and were simultaneously produced, they either originated inside the galactic halo or otherwise very unlikely events were observed. On the other hand, an estimate of the arrival probability of ultra-high energy cosmic rays, under the assumption that the distribution of luminous matter in the nearby universe traces the distribution of the sources of the particles and intensity of the intergalactic magnetic field, suggests that the pairs are chance clusterings.']",['1998-01-09'] +1729,['eng'],"['Farrar, Glennys R S']",['Can Ultra High Energy Cosmic Rays be Evidence for New Particle Physics?'],['Astrophysics and Astronomy'],"['talk, College Park 1997/11/13', 'cosmic radiation, energy spectrum', 'cosmic radiation, acceleration', 'new particle, search for', 'showers, air', 'supersymmetry', 'gluino', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801020'],"[""Candidate astrophysical acceleration sites capable of producing the highest energy cosmic rays (E > 10^{19.5} eV) appear to be at far greater distances than is compatible with their being known particles. The properties of a new particle which can account for observations are discussed and found to be tightly constrained. In order to travel 100's or 1000's of Mpc through the cosmic microwave background radiation without severe energy loss and yet produce a shower in Earth's atmosphere which is consistent with observations, it must be a hadron with mass of order a few GeV and lifetime greater than about 1 week. A particle with the required properties was identified years ago in the context of supersymmetric theories with a very light gluino. Laboratory experiments do not exclude it, as is discussed briefly.""]",['1998-01-06'] +1730,['eng'],"['Giampieri, G']",['Gravitational Waves from a Population of Galactic Neutron Stars'],['Astrophysics and Astronomy'],"['talk, Orsay 1997/11/13', 'gravitational radiation, measurement', 'n, matter', 'galaxy', 'signal processing, stochastic', 'amplitude analysis', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801019'],"['The existence of a large number of asymmetric, rotating neutron stars, each individually emitting periodic or quasi-periodic gravitational waves in the frequency band around 100 Hz, raises the possibility of detecting their combined signals, by exploiting the amplitude modulation of the received waves as the antenna changes its orientation with respect to fixed stars. This modulation is directly related to the amount of anisotropy present in the source distribution, and, if detected, could give valuable information about the spatial distribution of neutron stars in our Galaxy.']",['1998-01-06'] +1731,['eng'],"['Paczynski, B']",['GRBs as Hypernovae'],['Astrophysics and Astronomy'],"['talk, Huntsville 1997/09/15', 'photon, cosmic radiation', 'n, matter', 'black hole', 'energy', 'galaxy', 'binary', 'astrophysics, model']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712123'],"['A standard fireball/afterglow model of a gamma-ray burst relates the event to a merging neutron star binary, or a neutron star - black hole binary, which places the events far away from star forming regions, and is thought to have an energy of ~ 10^51 erg. A hypernova, the death of a massive and rapidly spinning star, may release ~ 10^54 erg of kinetic energy by tapping the rotational energy of a Kerr black hole formed in the core collapse. Only a small fraction of all energy is in the debris ejected with the largest Lorentz factors, those giving rise to the GRB itself, but all energy is available to power the afterglow for a long time. In this scenario GRBs should be found in star forming regions, the optical afterglows may be obscured by dust, and the early thermal emission of the massive ejecta may give rise to X-ray precursors, as observed by Ginga. The optical and X-ray afterglows of GRBs 970228, 97508, 97828 provide some evidence that these bursts were located in galaxies, most likely in dwarf galaxies, in or near star forming regions.']",['1997-12-09'] +1732,['eng'],"['Bernlöhr, K', 'Hofmann, W', 'Leffers, G', 'Matheis, V', 'Panter, M', 'Zink, R']",['Changes of the cosmic-ray mass composition in the $10^{14} - 10^{16}$ eV energy range'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, flux', 'elements, cosmic radiation', 'showers, air', 'showers, angular distribution', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801042'],"[""Changes of the cosmic-ray mass composition at the `knee' of the cosmic-ray flux spectrum near 10^{15} eV energy are investigated using data from ten Cosmic Ray Tracking (CRT) detectors and the HEGRA air-shower array on La Palma, Canary Islands. The analysis is based on the angular distribution of muons in air showers. Results can be easily expressed in terms of of primary cosmic rays. We find a rise of below 10^{15} eV, consistent with direct measurements. Simple cosmic-ray composition models are presented which are fully consistent with our results as well as the JACEE flux and composition measurements and the flux measurements of the Tibet AS-gamma collaboration.""]",['1998-01-08'] +1733,['eng'],"['Böttcher, M', 'Dermer, C D']",['High Energy $\\gamma$ Rays from Ultrahigh Energy Cosmic Ray Protons in $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'showers', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'p, cosmic radiation', 'lepton, cosmic radiation', 'pi, photoproduction', 'photon photon, interaction', 'synchrotron radiation', 'flux, time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801027'],"['It has recently been proposed that ultrahigh energy ($\\gtrsim 10^{19}$ eV) cosmic rays (UHECR) are accelerated by the blast waves associated with GRBs. We calculate the observed synchrotron radiation spectrum from protons and energetic leptons formed in the cascades initiated by photopion production, taking into account $\\gamma\\gamma$ attenuation at the source. Normalizing to the emission characteristics of GRB~970508, we predict $\\sim 10$ MeV - 100 GeV fluxes at a level which may have been observed with EGRET from bright GRBs, and could be detected with the proposed GLAST experiment or with ground-based air Cherenkov telescopes having thresholds $\\lesssim $ several hundred GeV. Besides testing the UHECR origin hypothesis, the short wavelength emission and afterglows can be used to probe the level of the diffuse intergalactic infrared radiation fields or constrain redshifts of GRB sources.']",['1998-01-08'] +1734,['eng'],"['Baring, M G', 'Ellison, D C', 'Reynolds, S P', 'Grenier, I A', 'Goret, P']",['Shock Acceleration and Gamma-Ray Emitting Supernova Remnants'],['Astrophysics and Astronomy'],"['talk, Kruger National Park 1997/08/08', 'astrophysics, supernova', 'photon, cosmic radiation', 'model, shock waves', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711257'],"[""Diffusive shock acceleration in the environs of a remnant's expanding shell is a popular candidate for the origin of SNR gamma-rays. In this paper, results from our study of non-linear effects in shock acceleration theory and their impact on the gamma-ray spectra of SNRs are presented. These effects describe the dynamical influence of the accelerated cosmic rays on the shocked plasma at the same time as addressing how the non-uniformities in the fluid flow force the distribution of the cosmic rays to deviate from pure power-laws. Such deviations are crucial to gamma-ray spectral determination. Our self-consistent Monte Carlo approach to shock acceleration is used to predict ion and electron distributions that spawn neutral pion decay, bremsstrahlung and inverse Compton emission components for SNRs. We demonstrate how the spatial and temporal limitations imposed by the expanding SNR shell quench acceleration above critical energies in the 500 GeV - 10 TeV range, thereby spawning gamma-ray spectral cutoffs that are quite consistent with Whipple's TeV upper limits to the EGRET unidentified sources that have SNR associations. We also discuss the role of electron injection in shocks and its impact on the significance of electromagnetic components to GeV--TeV spectral formation.""]",['1997-11-24'] +1735,['eng'],"['Gott, J R', 'Li, L X']",['Can the Universe Create Itself?'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'bubble', 'causality', 'tunneling', 'boundary condition', 'space-time, Minkowski', 'vacuum polarization', 'space-time, de Sitter', 'Einstein equation, solution', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712344'],"[""The question of first-cause has troubled philosophers and cosmologists alike. Now that it is apparent that our universe began in a Big Bang explosion, the question of what happened before the Big Bang arises. Inflation seems like a very promising answer, but as Borde and Vilenkin have shown, the inflationary state preceding the Big Bang must have had a beginning also. Ultimately, the difficult question seems to be how to make something out of nothing. This paper explores the idea that this is the wrong question --- that that is not how the Universe got here. Instead, we explore the idea of whether there is anything in the laws of physics that would prevent the Universe from creating itself. Because spacetimes can be curved and multiply connected, general relativity allows for the possibility of closed timelike curves (CTCs). Thus, tracing backwards in time through the original inflationary state we may eventually encounter a region of CTCs giving no first-cause. This region of CTCs, may well be over by now (being bounded toward the future by a Cauchy horizon). We illustrate that such models --- with CTCs --- are not necessarily inconsistent by demonstrating self-consistent vacua for Misner space and a multiply connected de Sitter space in which the renormalized energy-momentum tensor does not diverge as one approaches the Cauchy horizon and solves Einstein's equations. We show such a Universe can be classically stable and self-consistent if and only if the potentials are retarded, giving a natural explanation of the arrow of time. Some specific scenarios (out of many possible ones) for this type of model are described. For example: an inflationary universe gives rise to baby universes, one of which turns out to be itself. Interestingly, the laws of physics may allow the Universe to be its own mother.""]",['1997-12-31'] +1736,['eng'],"['Akerib, D S', 'Barnes, P B', 'Bauer, D A', 'Brink, P L', 'Cabrera, B', 'Caldwell, D O', 'Clarke, R M', 'Silva, A D', 'Davies, A K', 'Dougherty, B L', 'Irwin, K D', 'Gaitskell, R J', 'Golwala, S R', 'Haller, E E', 'Jochum, J', 'Knowlton, W B', 'Kuzminov, V V', 'Nam, S W', 'Novikov, V', 'Penn, M J', 'Perera, T A', 'Ross, R R', 'Sadoulet, Bernard', 'Schnee, R W', 'Shutt, T', 'Smith, A', 'Sonnenschein, A H', 'Spadafora, A L', 'Stockwell, W K', 'Yellin, S', 'Young, B A']",['Preliminary Limits on the WIMP-Nucleon Cross Section from the Cryogenic Dark Matter Search (CDMS)'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'astrophysics, missing-mass', 'search for, WIMP', 'scattering, WIMP nucleon', 'cross section, mass', 'upper limit', 'semiconductor detector, silicon', 'semiconductor detector, germanium', 'cryogenics', 'charge, yield', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712343'],"['We are conducting an experiment to search for WIMPs, or weakly-interacting massive particles, in the galactic halo using terrestrial detectors. This generic class of hypothetical particles, whose properties are similar to those predicted by extensions of the standard model of particle physics, could comprise the cold component of non-baryonic dark matter. We describe our experiment, which is based on cooled germanium and silicon detectors in a shielded low-background cryostat. The detectors achieve a high degree of background rejection through the simultaneous measurement of the energy in phonons and ionization. Using exposures on the order of one kilogram-day from initial runs of our experiment, we have achieved (preliminary) upper limits on the WIMP-nucleon cross section that are comparable to much longer runs of other experiments.']",['1997-12-31'] +1737,['eng'],"['Barwick, S W', 'Beatty, J J', 'Bower, C', 'Chaput, C J', 'Coutu, S', 'De Nolfo, G A', 'Duvernois, M A', 'Ellithorpe, D', 'Ficenec, D', 'Knapp, J', 'Lowder, D M', 'McKee, S', 'Müller, D', 'Musser, J A', 'Nutter, S L', 'Schneider, E', 'Swordy, S P', 'Tarlé, G', 'Tomasch, A D', 'Torbet, E']",['The Energy Spectra and Relative Abundances of Electrons and Positrons in the Galactic Cosmic Radiation'],['Astrophysics and Astronomy'],"['electron, cosmic radiation', 'positron, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'counters and detectors, satellite', 'experimental results', '((1)) ((2)) ((3))']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712324'],"['Observations of cosmic-ray electrons and positrons have been made with a new balloon-borne detector, HEAT (the ""High-Energy Antimatter Telescope""), first flown in 1994 May from Fort Sumner, NM. We describe the instrumental approach and the data analysis procedures, and we present results from this flight. The measurement has provided a new determination of the individual energy spectra of electrons and positrons from 5 GeV to about 50 GeV, and of the combined ""all-electron"" intensity (e+ + e-) up to about 100 GeV. The single power-law spectral indices for electrons and positrons are alpha = 3.09 +/- 0.08 and 3.3 +/- 0.2, respectively. We find that a contribution from primary sources to the positron intensity in this energy region, if it exists, must be quite small.']",['1997-12-25'] +1738,['eng'],"['Plaga, R']",['On an extragalactic origin of the dominant part of the hadronic cosmic rays'],['Astrophysics and Astronomy'],"['talk, Kruger National Park 1997/08/08', 'hadron, cosmic radiation', 'astrophysics, galaxy', 'cosmic radiation, particle source', 'cosmic radiation, spectra', 'energy, density', 'flux, magnetic', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712321'],"[""The possibility that the major part of all extrasolar hadronic cosmic rays with energies above 10 MeV/n is of extragalactic origin is discussed. Recent observational results on the galactocentric cosmic-ray density gradient and very high gamma-ray emission do not support expectations from the simplest models with a Galactic origin of cosmic rays. The hypothesis that ``flux trapping'' of extragalactical cosmic rays occurs in the Galactic confinement volume is advanced. Taking this phenomenon into account, I explicitely discuss how previous objections against an extragalactic origin of hadronic cosmic rays loose their strength. The local energy density of hadronic cosmic rays and other observational facts can be understood in a very natural way assuming an extragalactical origin. A promising scenario seems to be a Galactic origin of electrons and an extragalactic origin of hadrons.""]",['1997-12-25'] +1739,['eng'],"['Gattone, A O', 'Abriola, D', 'Avignone, F T', 'Brodzinski, R L', 'Collar, J I', 'Creswick, R J', 'Di Gregorio, D E', 'Farach, H A', 'Guérard, C K', 'Hasenbalg, F', 'Huck, H', 'Miley, H S', 'Morales, A', 'Morales, J', 'Nussinov, S', 'Ortizde-Solorzano, A', 'Reeves, J H', 'Villar, J A', 'Zioutas, Konstantin']",['Experimental Search for Solar Axions'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'search for, axion', 'axion, solar', 'transition, axion photon', 'Primakoff effect', 'coupling, (axion 2photon)', 'upper limit', 'semiconductor detector, germanium', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712308'],"['A new technique has been used to search for solar axions using a single crystal germanium detector. It exploits the coherent conversion of axions into photons when their angle of incidence satisfies a Bragg condition with a crystalline plane. The analysis of approximately 1.94 kg.yr of data from the 1-kg DEMOS detector in Sierra Grande, Argentina, yields a new laboratory bound on axion-photon coupling of g_{a,\\gamma\\gamma}<2.7\\times 10^{-9} GeV^{-1} independent of axion mass up to \\sim 1 keV.']",['1997-12-24'] +1740,['eng'],"['Bergström, L', 'Ullio, P', 'Buckley, J H']",['Observability of $\\gamma$ Rays from Dark Matter Neutralino Annihilations in the Milky Way Halo'],['Astrophysics and Astronomy'],"['electroweak interaction', 'supersymmetry', 'photon, cosmic radiation', 'photon, flux', 'astrophysics, missing-mass', 'neutralino, annihilation', 'astrophysics, galaxy', 'photon, particle identification', 'Cherenkov counter', 'counters and detectors, satellite', 'counters and detectors, proposed', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712318'],"['Recent advances in N-body simulations of cold dark matter halos point to a substantial density enhancement near the center. This means that, e.g., the significantly enhanced compared to old estimates based on an isothermal sphere model with large core radius. Another important development concerns new detectors, both space- and ground-based, which will cover the window between 50 and 300 GeV where presently no cosmic $\\gamma$-ray data are available. Thirdly, new calculations of the $\\gamma$-ray line signal (a sharp spike of $10^{-3}$ relative width) from neutralino annihilations have revealed a hitherto neglected contribution which, for heavy higgsino-like neutralinos, gives an annihilation rate an order of magnitude larger than previously predicted. We make a detailed phenomenological study of the possible detection rates given these three pieces of new information. We show that the proposed upgrade of the Whipple telescope will make it sensitive to a region of parameter space, with substantial improvements possible with the planned new generation of Air Cherenkov Telescope Arrays. We also comment on the potential of the GLAST satellite detector. An evaluation of the continuum $\\gamma$-rays produced in neutralino annihilations into the main modes is also done. It is shown that a combination of high-rate models and very peaked halo models are already severely constrained by existing data.']",['1997-12-24'] +1741,['eng'],"['Usov, Yu V']",['Bare Quark Matter Surfaces of Strange Stars and $e^{+}e^{-}$ Emission'],['Astrophysics and Astronomy'],"['matter, strangeness', 'quark, matter', 'electron, pair production', 'potential, Coulomb', 'plasma, luminosity', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712304'],"['We show that the Coulomb barrier at the quark surface of a hot strange star may be a powerful source of $e^+e^-$ pairs which are created in an extremely strong electric field of the barrier and flow away from the star. The luminosity in the outflowing pair plasma depends on the surface temperature $T_{_S}$ and may be very high, up to $\\sim 3\\times 10^{51} ergs/s$ at $T_{_S}\\sim 10^{11}$ K. The effect of pair creation by the Coulomb barrier may be a good observational signature of strange stars which can give an answer to the question of whether a compact object is a neutron or strange star.']",['1997-12-24'] +1742,['eng'],"['Cohn, J D']",['Update on Open Universe Inflationary Models'],['Astrophysics and Astronomy'],"['talk, Ambleside 1997/09/15', 'inflationary universe, open', 'gravitational radiation', 'cosmic radiation, background']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712315'],"['An overview of some new results in open inflation over the past year, including the calculation of gravity wave contributions to the Cosmic Microwave Background. Proceedings for COSMO-97, held in Ambleside, U.K., hence very short due to space limitations (the version for the web is more than 3 pages because archive numbers have been added for the references).']",['1997-12-24'] +1743,['eng'],"['Duff, Michael J', 'Hoxha, P', 'Lü, H', 'Martínez-Acosta, R R', 'Pope, C N']",['A Lattice Universe from M-theory'],['Astrophysics and Astronomy'],"['astrophysics', 'lattice, galaxy', 'dimension, 3', 'M-theory', 'domain wall']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712301'],"[""A recent paper on the large-scale structure of the Universe presented evidence for a rectangular three-dimensional lattice of galaxy superclusters and voids, with lattice spacing ~ 120 Mpc, and called for some ``hitherto unknown process'' to explain it. Here we report that a rectangular three-dimensional lattice of intersecting domain walls, with arbitrary spacing, emerges naturally as a classical solution of M-theory.""]",['1997-12-23'] +1744,['eng'],"['Dolgov, A D', 'Pagel, B E J']",['Varying leptonic chemical potentials and spatial variation of primordial deuterium at high z'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'deuterium', 'spatial distribution', 'potential, chemical', 'potential, leptonic', 'lepton, production', 'helium', 'lithium', 'background, microwaves', 'thermodynamics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711202'],"['We try to explain the spatial variation of primordial deuterium suggested by some observations by varying leptonic chemical potentials. The variation of the latter may take place in some scenarios of leptogenesis. The model predicts a large mass fraction of $^4 He$ (35-60%) and $^7 Li$ (up to $10^{-9}$) in deuterium-rich regions. Because of lepton family symmetry, the angular variations of cosmic microwave background radiation can be sufficiently small although still observable in future measurements.']",['1997-11-19'] +1745,['eng'],"['Kamionkowski, M P']",['Cosmic Microwave Background Tests of Inflation'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'talk, Rome 1997/05/19', 'inflationary universe, validity test', 'cosmic radiation, background', 'density, perturbation', 'spectra, perturbation', 'gravitational radiation', 'cosmic radiation, polarization', 'temperature, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712215'],"['Inflation provides a unified paradigm for understanding the isotropy of the cosmic microwave background (CMB), the flatness problem, and the origin of large-scale structure. Although the physics responsible for inflation is not yet well understood, slow-roll inflation generically makes several predictions: a flat Universe, primordial adiabatic density perturbations, and a stochastic gravity-wave background. Inflation further predicts specific relations between the amplitudes and shapes of the spectrum of density perturbations and gravity waves. There are now excellent prospects for testing precisely these predictions with forthcoming CMB temperature and polarization maps. Here I discuss these new CMB tests of inflation.']",['1997-12-17'] +1746,['eng'],"['Gnedin, N Yu', 'Gnedin, O Yu']",['Cosmological Neutrino Background Revisited'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, density', 'neutrino, background', 'Boltzmann equation, solution', 'energy, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'neutrino, temperature', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712199'],"['In the standard cosmological theory the abundance of primordial neutrinos (cosmological neutrino background) has been computed using the freeze-out approximation. We verify the accuracy of this approximation by solving the Boltzmann equation for cosmological neutrinos around the epoch of the electron-positron annihilation. We find the radiation energy density to be about 1% higher than has been calculated previously. As a result, the spectrum of the Cosmic Microwave Background anisotropies changes by about 1-1.5%, depending on the angular scale. Also, the primordial helium abundance increases by about 0.001 as compared to the freeze-out approximation.']",['1997-12-17'] +1747,['eng'],"['Castellani, V', ""Degl'Innocenti, S"", 'Dziembowski, W A', 'Fiorentini, G', 'Ricci, B']","['Helioseismology, solar models and neutrino fluxes']",['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'model, solar', 'neutrino, solar', 'neutrino, flux', 'temperature, solar', 'thermodynamics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712174'],"['We present our results concerning a systematical analysis of helioseismic implications on solar structure and neutrino production. We find Y$_{ph}=0.238-0.259$, $R_b/R_\\odot=0.708-0.714$ and $\\rho_b=(0.185-0.199)$ gr/cm$^3$. In the interval $0.2 0.65 background experiments, which are themselves insensitive to m_\\nu, measure two other cosmological parameters. There is significant overlap between this region and that implied by the LSND experiment, and even m_\\nu ~ 0.1 eV, as implied by the atmospheric neutrino anomaly, can affect cosmological measurements.']",['1997-12-08'] +1764,['eng'],"['Anoushirvani, B', 'Enström, D', 'Fredriksson, S', 'Hansson, J', 'Nicolaidis, A', 'Ekelin, S']",['Gamma-Ray Bursts from Primordial Quark Objects in Space'],['Astrophysics and Astronomy'],"['talk, Ouranoupolis 1997/05/27', 'photon, cosmic radiation', 'quark, matter', 'nuclear matter', 'critical phenomena', 'astrophysics, galaxy', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711346'],"['We investigate the possibility that gamma-ray bursts originate in a concentric spherical shell with a given average redshift and find that this is indeed compatible with the data from the third BATSE (3B) catalog. It is also shown that there is enough freedom in the choice of unknown burst properties to allow even for extremely large distances to the majority of bursts. Therefore, we speculate about an early, and very energetic, origin of bursts, and suggest that they come from phase transitions in massive objects of pure quark matter, left over from the Big Bang.']",['2000-10-05'] +1765,['eng'],"['Pina-Avelino, P', 'Shellard, E P S', 'Wu, J H P', 'Allen, B']",['Cosmic string-seeded structure formation'],['Astrophysics and Astronomy'],"['astrophysics, string', 'astrophysics, missing-mass', 'density, perturbation', 'spectra, perturbation', 'cosmic radiation, background', 'anisotropy', 'astrophysics, model', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9712008'],"['We describe the results of high-resolution numerical simulations of string-induced structure formation using a cosmic string network with cold and hot dark matter backgrounds. The resulting linear power spectrum ${\\cal P}(k)$ of density perturbations is calculated and compared with the linear power spectrum inferred from various galaxy surveys. We investigate the performance of cosmic string models in open universes and those with a non-zero cosmological constant. In particular, we show that for $\\Gamma = \\Omega h = 0.1--0.2$ both the mass fluctuation amplitude $\\sigma_8$ at $8 h^{-1}$Mpc and the power spectrum shape of cosmic string-induced CDM fluctuations agree well with those inferred from observations. The HDM scenario with cosmic strings seems to require a strongly scale-dependent bias in order to be consistent with observations.']",['1997-12-02'] +1766,['eng'],"['Komatsu, E', 'Futamase, T']","['Constraints on the chaotic inflationary scenario with a nonminimally coupled ""inflaton"" field from the cosmic microwave background radiation anisotropy']",['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'inflaton, coupling', 'cosmic radiation, background', 'anisotropy', 'gravitational radiation', 'space-time, perturbation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711340'],"['We investigate a possibility to restrict the chaotic inflationary scenario with ""large"" nonminimally coupled inflaton(""phi"") field considered by Fakir and Unruh by means of the observed CMBR anisotropy. We calculate the contributions of the long wavelength gravitational waves generated in the inflationary period to CMBR anisotropy quadrupole moment. We obtain the constraint lambda/(xi^2) = 1.8 X 10^(-8)/psi_i, where ""lambda"" is the self coupling, ""xi"" is the nonminimal coupling constant and ""psi_i"" means the initial value of psi = 8piG(phi^2). Combining this with previously obtained constraint that 2.1 times squre root of lambda/(xi^2) = dT/T = 1.1 X 10^(-5), we conclude that the initial value has to be psi_i = 1.6 X 10^3. If the self-coupling has a reasonably values of order 10^(-2), then xi = 10^4 and phi_i = 10^(-1) times Planck mass.']",['1997-12-01'] +1767,['eng'],"['Battye, R A', 'Robinson, J', 'Albrecht, Andreas']",['Structure formation by cosmic strings with a cosmological constant'],['Astrophysics and Astronomy'],"['astrophysics, string', 'astrophysics, fundamental constant', 'density, perturbation', 'scaling', 'cosmic radiation, background', 'anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711336'],['We investigate cosmic string models for structure formation which include a non-zero cosmological constant. We find that the background evolution of density perturbations and modifications to the scaling behaviour of the strings both act to increase the amount of power present on $100h^{-1}$Mpc scales. We estimate the size of this effect using an analytic model for the evolution of the string network and find that a bias $b\\sim 2$ can give acceptable agreement with the current observations. An interesting by product of these modifications is a broad peak in the CMB angular power spectrum around $l=400-600$.'],['1997-12-01'] +1768,['eng'],"['Kim, J E']",['The Axino-Gravitino Cosmology'],['Astrophysics and Astronomy'],"['talk, Ambleside 1997/09/15', 'astrophysics, missing-mass', 'axino', 'gravitino', 'strong interaction, CP', 'supergravity', 'quantum chromodynamics, Theta parameter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711310'],['A cosmological scenario of a light axino and a lighter gravitino is presented. The most important consequence is that it can mimick the mixed dark matter (MDM) model of the large scale structure formation. The presence of axino and gravitino is inevitable in supergravity extension of the invisible axion solution of the strong CP problem. The possibility of a light gravitino is popular in the recent efforts of gauge mediated supersymmetry breaking.'],['1997-11-27'] +1769,['eng'],"['Wilson, J R', 'Salmonson, J D', 'Mathews, G J']",['A Binary Neutron Star GRB Model'],['Astrophysics and Astronomy'],"['talk, Huntsville 1997/09/15', 'photon, cosmic radiation', 'cosmic radiation, production', 'n, matter', 'binary', 'neutrino, pair production', 'neutrino antineutrino, annihilation', 'electron, pair production', 'photon, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711307'],['In this paper we present the preliminary results of a model for the production of gamma-ray bursts (GRBs) through the compressional heating of binary neutron stars near their last stable orbit prior to merger.'],['1997-11-27'] +1770,['eng'],"['Baring, M G', 'Harding, A K']",['The Escape of High-Energy Photons from Gamma-Ray Bursts'],['Astrophysics and Astronomy'],"['photon, showers', 'cosmic radiation, particle source', 'photon photon, interaction', 'electron, pair production', 'relativistic', 'dependence, geometrical', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711217'],"['Eleven bright gamma-ray bursts (GRBs) detected by BATSE have also been seen at much higher energies by EGRET, six at energies above 10 MeV. Such observations imply that these bursts are optically thin to photon-photon pair production at all observed energies. For bursts more than about 30pc away, internal transparency can be achieved only if the source is moving with a relativistic bulk Lorentz factor $\\Gamma\\gg 1$, or if the radiation is highly beamed. Early calculations of $\\gamma\\gamma\\to e^+e^-$ considerations for GRBs were limited to cases of a beam with opening half-angle $\\Thetab\\sim 1/\\Gamma$, or expansions of infinitely thin spherical shells. This paper presents our extension of pair production optical depth calculations in relativistically expanding sources to more general geometries, including shells of finite thickness and arbitrary opening angle. The problem is reduced analytically to a single integral in the broadly applicable case of observing photons along the axis of the expansion. We find that the minimum bulk Lorentz factor for the EGRET sources to be optically thin is only moderately dependent on the shell thickness and virtually independent of its opening solid angle if commonly-perceived number problem for non-repeating sources at cosmological distances, i.e. it is not necessary to invoke small $\\Thetab$ to effect photon escape.']",['1997-11-20'] +1771,['eng'],"['Pohl, M', 'Kanbach, G', 'Hunter, S D', 'Jones, B B']",['The pulsar contribution to the diffuse galactic gamma-ray emission'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, pulsar', 'cosmic radiation, energy', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711183'],"['There is active interest in the extent to which unresolved gamma-ray pulsars contribute to the galactic diffuse emission, and whether unresolved gamma-ray pulsars could be responsible for the excess of diffuse galactic emission above 1 GeV which has been observed by EGRET. The diffuse gamma-ray intensity due to unresolved pulsars is directly linked to the number of objects which should be observed in the EGRET data. We can therefore use our knowledge of the unidentified EGRET sources to constrain model parameters like the pulsar birth rate, their beaming angle, etc. This analysis is based only on the properties of the six pulsars which have been identified in the EGRET data, and is independent of choice of a pulsar emission model. We find that pulsars contribute very little to the diffuse emission at lower energies, whereas above 1 GeV they can account for 18% of the observed intensity in selected regions for a reasonable number of directly observable gamma-ray pulsars (14). The latitude distribution of the diffuse emission caused by unresolved pulsars is narrower than that of the observed diffuse emission. While the excess above 1 GeV gamma-ray energy is observed up to at least 6-8 degrees off the plane, the pulsar contribution would be small there. Thus pulsars do significantly contribute to the diffuse galactic gamma-ray emission above 1 GeV, but they can not be made responsible for all the discrepancy between observed intensity and model predictions in this energy range.']",['1997-11-18'] +1772,['eng'],"['Anderson, G W', 'Carroll, S M']",['Dark Matter with Time-Dependent Mass'],['Astrophysics and Astronomy'],"['talk, Ambleside 1997/09/15', 'astrophysics, missing-mass', 'mass, time dependence', 'field theory, scalar', 'particle, density', 'energy, density', 'effective potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711288'],"[""We propose a simple model in which the cosmological dark matter consists of particles whose mass increases with the scale factor of the universe. The particle mass is generated by the expectation value of a scalar field which does not have a stable vacuum state, but which is effectively stabilized by the rest energy of the ambient particles. As the universe expands, the density of particles decreases, leading to an increase in the vacuum expectation value of the scalar (and hence the mass of the particle). The energy density of the coupled system of variable-mass particles (``vamps'') redshifts more slowly than that of ordinary matter. Consequently, the age of the universe is larger than in conventional scenarios.""]",['1997-11-25'] +1773,['eng'],"['Burns, S D']",['Microwave Background Anisotropy and Large Scale Structure in Warm Dark Matter Models'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'astrophysics, galaxy', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitino', 'neutrino, right-handed', 'neutrino, sterile', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711304'],"['Large scale structure and microwave background anisotropies are studied for warm dark matter models. Two warm dark matter candidates are considered: gravitinos and sterile neutrinos. Linear large scale structure properties such as $\\sigma_{8}$ and the excess power are calculated, as well as microwave background anisotropies. A rather robust feature of warm dark matter models is that the large scale structure properties are similar to those of mixed dark matter, but that the microwave background anisotropy is very similar to that of standard cold dark matter.']",['1997-11-26'] +1774,['eng'],"['Baring, M G']",['Gamma-Ray Bursts Above 1 GeV'],['Astrophysics and Astronomy'],"['talk, Kruger National Park 1997/08/08', 'photon, cosmic radiation', 'showers', 'energy', 'flux', 'photon photon, interaction', 'electron, pair production', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711256'],"[""One of the principal results obtained by the Compton Gamma Ray Observatory relating to the study of gamma-ray bursts was the detection by the EGRET instrument of energetic ($>$100 MeV) photons from a handful of bright bursts. The most extreme of these was the single 18 GeV photon from the GRB940217 source. Given EGRET's sensitivity and limited field of view, the detection rate implies that such high energy emission may be ubiquitous in bursts. Hence expectations that bursts emit out to at least TeV energies are quite realistic, and the associated target-of-opportunity activity of the TeV gamma-ray community is well-founded. This review summarizes the observations and a handful of theoretical models for generating GeV--TeV emission in bursts sources, outlining possible ways that future positive detections could discriminate between different scenarios. The power of observations in the GeV--TeV range to distinguish between spectral structure intrinsic to bursts and that due to the intervening medium between source and observer is also discussed.""]",['1997-11-24'] +1775,['eng'],"['Brocato, E', 'Castellani, V', ""Degl'Innocenti, S"", 'Fiorentini, G', 'Raimondo, G']",['Stars as galactic neutrino sources'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'neutrino, flux', 'neutrino, yield', 'matter, solar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711269'],"[""Theoretical expectations concerning stars as neutrino sources are presented according to detailed evaluations of the stellar evolutionary histories for an extended grid of stellar masses. Neutrino fluxes and cumulative neutrino yields are given for both `thermo-nuclear' and `cooling' neutrinos all over the nuclear life of the stars and along the final cooling as White Dwarfs. Predictions concerning the galactic and the cosmic neutrino background are presented and discussed.""]",['1997-11-25'] +1776,['eng'],"['Straumann, N']",['The Membrane Model of Black Holes and Applications'],['Astrophysics and Astronomy'],"['lectures, Bad Honnef 1997/08/18', 'black hole', 'membrane model', 'Maxwell equation, solution', 'space-time, horizon', 'energy, magnetic', 'model, rotator', 'magnetic field, external field', 'current', 'conservation law', 'entropy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711276'],"['These lectures provide a detailed introduction to the electro- dynamics of black holes. A simplified derivation of the basic membrane equations for stationary, axisymmetric black holes is given. The general theory is applied to idealized current generators involving rotating black holes, and we also analyse the Blandford-Znajek process for magnetic energy extraction from rotating black holes.']",['1997-11-25'] +1777,['eng'],"['Völk, H J']",['Particle Acceleration and Gamma-Ray Production in Shell Remnants'],['Astrophysics and Astronomy'],"['talk, Kruger National Park 1997/08/08', 'cosmic radiation, acceleration', 'shock waves', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'flux', 'astrophysics, supernova', 'Compton scattering', 'pi0, radiative decay', 'magnetic field', 'model, fluid', 'model, hydrodynamical', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711204'],"[""A number of nearby Northern Hemisphere shell-type Supernova Remnants (SNRs) has been observed in TeV gamma rays, but none of them could be detected so far. This failure calls for a critical reevaluation of the theoretical arguments for gamma-ray emission of SNRs. The present paper discusses diffusive shock acceleration in shell-type SNRs in full kinetic theory. Emphasis is also given to the possible problems for VHE gamma-ray production due to the environmental conditions a SN progenitor finds itself in. Observational upper limits are compared with theoretical predictions for the gamma-ray flux. Empirical arguments from the observation of X-ray power law continua for electron-induced Inverse Compton gamma-ray emission at TeV energies are discussed in their relation to the nucleonic Pi-zero decay emission from the same objects. Finally, a point is made for the simplest case of SNe Ia, expected to explode in a uniform circumstellar medium. Here in particular the very recently detected Southern Hemisphere remnant of SN 1006 is compared with Tycho's SNR. On the basis of the assumed parameters for the two remnants SN 1006 is tentatively identified with a remnant whose TeV gamma-ray emission is dominated by Inverse Compton radiation. Tycho might be dominantly a Pi-zero decay gamma-ray source.""]",['1997-11-19'] +1778,['eng'],"['Kopf, A', 'Raffelt, G G']",['Photon Dispersion in a Supernova Core'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'photon, dispersion relations', 'n, magnetic moment', 'spin, susceptibility', 'bremsstrahlung', 'photon, absorption', 'photon, mass', 'mass, transverse', 'structure function', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711196'],"['While the photon forward-scattering amplitude on free magnetic dipoles (e.g. free neutrons) vanishes, the nucleon magnetic moments still contribute significantly to the photon dispersion relation in a supernova (SN) core where the nucleon spins are not free due to their interaction. We study the frequency dependence of the relevant spin susceptibility in a toy model with only neutrons which interact by one-pion exchange. Our approach amounts to calculating the photon absorption rate from the inverse bremsstrahlung process gamma n n --> n n, and then deriving the refractive index n_refr with the help of the Kramers-Kronig relation. In the static limit (omega --> 0) the dispersion relation is governed by the Pauli susceptibility chi_Pauli so that (n_refr)^2-1 approx chi_Pauli > 0. For omega somewhat above the neutron spin-relaxation rate Gamma_sigma we find (n_refr)^2-1< 0, and for omega >> Gamma_sigma the photon dispersion relation acquires the form omega^2-k^2=(m_gamma)^2. An exact expression for the ""transverse photon mass"" m_gamma is given in terms of the f-sum of the neutron spin autocorrelation function; an estimate is (m_gamma)^2 approx chi_Pauli T Gamma_sigma. The dominant contribution to n_refr$ in a SN core remains the electron plasma frequency so that the Cherenkov processes gamma nu <--> nu remain forbidden for all photon frequencies.']",['1997-11-19'] +1779,['eng'],"['Cui, W', 'Chen, W', 'Zhang, S N']",['Cygnus X-1'],['Astrophysics and Astronomy'],"['talk, Hong Kong 1997/08/13', 'astrophysics', 'black hole, spin', 'radiation, time dependence', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711168'],"['It has been a long-standing puzzle what triggers the spectral transition between the hard and soft states in Cyg X-1. Also, the origin of the frequently observed X-ray flares in the source still remains a mystery. In this paper, we will make an attempt to address these issues in light of our recent work on black hole spin and its observational consequences.']",['1997-11-17'] +1780,['eng'],"['Abdalla, Elcio', 'Mohayaee, R']",['Evolution of Scale-invariant Inhomogeneities in Standard Cosmology'],['Astrophysics and Astronomy'],"['Friedman model, open', 'density, fluctuation', 'scaling', 'inflationary universe', 'Einstein equation, solution', 'differential equations, solution', 'effect, pressure']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711162'],"['It is shown that density fluctuations obey a scaling law in an open Friedmann universe. In a flat universe, the fluctuations are not scale-invariant. We compute the growth rate of adiabatic scale-invariant density fluctuations in flat, open and inflationary universes. We find that, given a sufficiently long time, the density perturbations decay away in the Einstein-de-Sitter universe. On the contrary, the rapid growth of the density instabilities makes an open universe inhomogeneous in a time scale comparable to the age of our universe. We also find that the fluctuations grow exponentially in a flat inflationary universe.']",['1997-11-17'] +1781,['eng'],"['Capuzzo-Dolcetta, R', 'Miocchi, P']",['Gravitational Waves Generated by Globular Cluster Systems Collapse'],['Astrophysics and Astronomy'],"['talk, Kyoto 1997/08/18', 'gravitational radiation', 'cluster, galaxy', 'counters and detectors, laser', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711049'],"['According to the hypothesis that AGNs are massive black holes and the mass which feeds them is made of stars belonging to globular clusters frictionally decayed and tidally destroyed by the field of the central object, it is possible to give an estimate of the number and spectral characteristics of detectable gravitational wave impulses generated by the falling of such stars into the black hole. We find that the orbitating gravitational antenna LISA, should detect from 10 to 100 impulses per year.']",['1997-11-07'] +1782,['eng'],"['Hannestad, S', 'Raffelt, G G']",['Supernova Neutrino Opacity from Nucleon-Nucleon Bremsstrahlung and Related Processes'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, path length', 'neutrino/mu', 'neutrino/tau', 'n n, inelastic scattering', 'neutrino, bremsstrahlung', 'interaction, (2nucleon neutrino antineutrino)', 'thermodynamics', 'neutrino, energy loss', 'neutrino, flux', 'effective Hamiltonian, weak interaction', 'nuclear physics', 'exchange, one-pion', 'Born approximation', 'multiple scattering', 'Boltzmann equation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711132'],"['In numerical studies of the transport of mu and tau neutrinos in supernova (SN) cores, nu anti-nu <--> e+ e- has been used as the dominant number-changing and nu e- --> e- nu as the dominant energy-changing process. However, Suzuki (1993) has found that the bremsstrahlung process nu_mu anti-nu_mu N N <--> N N modifies the neutrino spectra and fluxes significantly. This is by far the most important number-changing process, and even dominates electrons for energy exchange. The related ""inelastic scattering process"" nu N N <--> N N nu is even more effective at energy exchange by a factor of about 10. To facilitate the numerical study of the nu_mu and nu_tau spectra formation we derive the scattering kernel which governs both bremsstrahlung and inelastic scattering and give an analytic approximation formula. We consider only neutron-neutron interactions, we use a one-pion exchange potential in Born approximation, nonrelativistic neutrons, and the long-wavelength limit, simplifications which appear justified for the surface layers of a SN core. We include the pion mass in the potential and we allow for an arbitrary degree of neutron degeneracy. Our treatment does not include the neutron-proton process and does not include nucleon-nucleon correlations. Our perturbative approach is certainly not valid at densities above about 10^14 g/cm^3 where it implies a large reduction of the overall nu N scattering cross section. The spin-density structure function at such high densities has not been calculated so that the magnitude of the effective nu N scattering cross section in the inner part of a SN core remains very poorly known.']",['1997-11-13'] +1783,['eng'],"['Baccigalupi, C']",['Sub-degree CMB anisotropies from inflationary bubbles'],['Astrophysics and Astronomy'],"['inflationary universe, bubble', 'cosmic radiation, background', 'anisotropy', 'spectra, perturbation', 'perturbation theory, linear', 'photon baryon, plasma', 'decoupling', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711095'],"['It is well known that processes of first order phase transitions may have occurred in the inflationary era. If one or more occurred well before the end of inflation, the nucleated bubbles are stretched to large scales and the primordial power spectrum contains a scale dependent non-Gaussian component provided by the remnants of the bubbles. We predict the anisotropies in the cosmic microwave background (CMB) induced by inflationary bubbles. We build a general analytic model for describing a bubbly perturbation; we evolve each Fourier mode using the linear theory of perturbations from reheating until decoupling; we get the CMB anisotropies by considering the bubbly perturbation intersecting the last scattering surface. The CMB image of an inflationary bubble is a series of concentric isothermal rings of different color (sign of the sky); the resulting anisotropy is therefore strongly non-Gaussian. The mean amplitude of $\\delta T/T$ for a bubble of size $L$ follows the known estimates for linear perturbations, $\\delta T/T\\simeq\\delta\\rho /\\rho\\cdot (L/H^{-1})^{2}$. In particular, bubbles with size corresponding to the seeds of the observed large scale voids (tens of comoving Mpc) induce an interesting pattern of CMB anisotropies on the sub-degree angular scale, to be further investigated and compared with the forthcoming high resolution CMB maps provided by the MAP and the Planck experiments.']",['1997-11-11'] +1784,['eng'],"['Durrer, R', 'Kunz, M']",['Cosmic Microwave Background Anisotropies from Scaling Seeds'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'anisotropy', 'spectra, fluctuation', 'scaling', 'correlation function', 'tensor, energy-momentum', 'perturbation, scalar', 'perturbation, vector', 'perturbation, tensor', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711133'],"['In this work we present a partially new method to analyze fluctuations which are induced by causal scaling seeds. We show that the power spectra due to this kind of seed perturbations are determined by five analytic functions, which we determine numerically for a special example. We put forward the view that, even if recent work disfavors the models with cosmic strings and global O(4) texture, causal scaling seed perturbations merit a more thorough and general analysis, which we initiate in this paper.']",['1997-11-13'] +1785,['eng'],"['Lesgourgues, Julien', 'Polarski, D', 'Starobinsky, A A']",['CDM models with a BSI steplike primordial spectrum and a cosmological constant'],['Astrophysics and Astronomy'],"['inflationary universe', 'astrophysics, missing-mass', 'astrophysics, fundamental constant', 'spectra, perturbation', 'adiabatic', 'cluster, galaxy', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711139'],"['A class of spatially-flat models with cold dark matter (CDM), a cosmological constant and a broken-scale-invariant (BSI) steplike primordial (initial) spectrum of adiabatic perturbations, generated in an exactly solvable inflationary model where the inflaton potential has a rapid change of its first derivative at some point, is confronted with existing observational data on angular fluctuations of the CMB temperature, galaxy clustering and peculiar velocities of galaxies. If we locate the step in the initial spectrum at k=0.05 h/Mpc, where some feature in the spectrum of Abell clusters of galaxies was found that could reflect a property of the initial spectrum, and if the large scales flat plateau of the spectrum is normalized according to the COBE data, the only remaining parameter of the spectrum is p - the ratio of amplitudes of the metric perturbations between the small scales and large scales flat plateaux. Allowed regions in the plane of parameters (Omega=1-Omega_Lambda, H_0) satisfying all data have been found for p lying in the region (0.8-1.7). Especially good agreement of the form of the present power spectrum in this model with the form of the cluster power spectrum is obtained for the inverted step (p<1, p=0.7-0.8), when the initial spectrum has slightly more power on small scales.']",['1997-11-13'] +1786,['eng'],"['Baltz, E A', 'Westphal, A J', 'Snowden-Ifft, D P']",['Probing the structure of the cold dark matter halo with ancient mica'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'WIMP', 'astrophysics, galaxy', 'tracks', 'numerical calculations', 'experimental methods, proposed']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711039'],"['Mica can store (for >1 Gy) etchable tracks caused by atoms recoiling from WIMPs. Ancient mica is a directional detector despite the complex motions it makes with respect to the WIMP ""wind"". We can exploit the properties of directionality and long integration time to probe for structure in the dark matter halo of our galaxy. We compute a sample of possible signals in mica for a plausible model of halo structure.']",['1997-11-06'] +1787,['eng'],"['Boothby, K', 'Chantell, M C', 'Green, K D', 'Kieda, D B', 'Knapp, J', 'Larsen, C G', 'Swordy, S P']",['A New Measurement of Cosmic Ray Composition at the Knee'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'elements, cosmic radiation', 'cosmic radiation, flux', 'showers, air', 'cosmic radiation, spatial distribution', 'astrophysics, supernova', 'Cherenkov counter, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710168'],"['The Dual Imaging Cerenkov Experiment (DICE) was designed and operated for making elemental composition measurements of cosmic rays near the knee of the spectrum at several PeV. Here we present the first results using this experiment from the measurement of the average location of the depth of shower maximum, , in the atmosphere as a function of particle energy. The value of near the instrument threshold of ~0.1 PeV is consistent with expectations from previous direct measurements. At higher energies there is little change in composition up to ~5 PeV. Above this energy is deeper than expected for a constant elemental composition implying the overall elemental composition is becoming lighter above the knee region. These results disagree with the idea that cosmic rays should become on average heavier above the knee. Instead they suggest a transition to a qualitatively different population of particles above 5 PeV.']",['1997-10-16'] +1788,['eng'],"['Baring, M G']",['Gamma-ray Production in Supernova Remnants'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1997/01/18', 'astrophysics, supernova', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'astrophysics, galaxy', 'cosmic radiation, acceleration', 'model, shock waves', 'nonlinear', 'cosmic radiation, primary', 'pi0, radiative decay', 'bremsstrahlung', 'Compton scattering', 'energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711186'],"[""Supernova remnants are widely believed to be a principal source of galactic cosmic rays, produced by diffusive shock acceleration in the environs of the remnant's expanding shock. This review discusses recent modelling of how such energetic particles can produce gamma-rays via interactions with the remnants' ambient interstellar medium, specifically via neutral pion decay, bremsstrahlung and inverse Compton emission. Predictions that relate to the handful of associations between EGRET unidentified sources and known radio/optical/X-ray emitting remnants are summarized. The cessation of acceleration above 1 TeV - 10 TeV energies in young shell-type remnants is critical to model consistency with Whipple's TeV upper limits; these observations provide important diagnostics for theoretical models.""]",['1997-11-18'] +1789,['eng'],"['Brandenberger, R H']",['Inflation and the Theory of Cosmological Perturbations'],['Astrophysics and Astronomy'],"['lectures, Trieste 1997/06/02', 'inflationary universe', 'density, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitation, back reaction', 'vacuum state, fluctuation', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711106'],"['The hypothesis that the Universe underwent a period of exponential expansion at very early times has become the most popular theory of the early Universe. Not only does it solve some of the problems of standard big bang cosmology, but it also provides a causal theory for the origin of primordial density fluctuations which may explain the observed density inhomogeneities and cosmic microwave fluctuations in the Universe. In these lectures, a review of the basic principles of inflationary cosmology is given, focusing on the theory of the origin and growth of cosmological perturbations. The lectures also focus on some recent progress in inflationary cosmology (in particular on an improved theory of reheating), and on several problems with the present inflationary Universe models. A couple of possible approaches to resolve these issues are suggested.']",['1997-11-12'] +1790,['eng'],"['Plaga, R']","['An extragalactic ""flux trapping"" origin of the dominant part of hadronic cosmic rays?']",['Astrophysics and Astronomy'],"['cosmic radiation, hadronic component', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'magnetic field', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711094'],"[""An extragalactic origin of the dominant part of all extrasolar hadronic cosmic rays above about 10 MeV/nucleon has long been considered unlikely due to energy considerations. In order to circumvent such arguments, the hypothesis that ``flux trapping'' of extragalactic cosmic rays occurs in the Galactic confinement volume is advanced in this paper. This hypothesis is based on a number of speculative assumptions about the properties of Galactic and intergalactic magnetic fields. The intergalactic cosmic-ray density expected under conservative assumptions about its extragalactic origins is then shown to be of the right order of magnitude to account for the locally observed cosmic radiation. It is demonstrated that an extragalactic scenario of cosmic-ray origin that is consistent with the observed cosmic-ray energy spectrum and preserves the successes of Galactic propagation theory can be constructed. The position of the ``ankle'' in the cosmic-ray energy spectrum follows as a natural consequence from this explanation. The $\\gamma$-ray flux from the Magellanic clouds is shown to provide no suitable testing ground for the decision for or against an extragalactical origin in this scenario. It is argued that recent observational evidence seems to be in favour of a dual origin of cosmic-rays. The hadronic component is mainly extragalactic while the electrons are accelerated in Galactic supernova remnants.""]",['1997-11-11'] +1791,['eng'],"['Sigl, G', 'Lemoine, M']",['Reconstruction of Source and Cosmic Magnetic Field Characteristics from Clusters of Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'nucleon, cluster', 'cosmic radiation, particle source', 'magnetic field', 'cosmic radiation, time delay', 'statistical analysis', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9711060'],"['We present a detailed Monte Carlo study coupled to a likelihood analysis of the potential of next generation ultra-high energy cosmic ray experiments to reconstruct properties of the sources and the extra-galactic magnetic field. Such characteristics are encoded in the distributions of arrival time, direction, and energy of clusters of charged cosmic rays above a few 10**(19) eV. The parameters we consider for reconstruction are the emission timescale, total fluence (or power), injection spectrum, and distance of the source, as well as the r.m.s. field strength, power spectrum, and coherence length of the magnetic field. We discuss five generic situations which can be identified relatively easily and allow a reasonable reconstruction of at least part of these parameters. Our numerical code is set up such that it can easily be applied to the data from future experiments.']",['1997-11-07'] +1792,['eng'],"['Pian, E', 'Vacanti, G', 'Tagliaferri, G', 'Ghisellini, G', 'Maraschi, L', 'Treves, A', 'Urry, C M', 'Fiore, F', 'Giommi, P', 'Palazzi, E', 'Chiappetti, L', 'Sambruna, R M']",['BeppoSAX Observations of Unprecedented Synchrotron Activity in the BL Lac Object Mkn 501'],['Astrophysics and Astronomy'],"['astrophysics', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'synchrotron radiation', 'Compton scattering', 'counters and detectors, satellite', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710331'],"['The BL Lac object Mkn 501, one of the only three extragalactic sources (with Mkn 421 and 1ES 2344+514) so far detected at TeV energies, was observed with the BeppoSAX satellite on 7, 11, and 16 April 1997 during a phase of high activity at TeV energies, as monitored with the Whipple, HEGRA and CAT Cherenkov telescopes. Over the whole 0.1-200 keV range the spectrum was exceptionally hard (alpha =< 1, with F_nu ~ nu^{-alpha}) indicating that the X-ray power output peaked at (or above) ~100 keV. This represents a shift of at least two orders of magnitude with respect to previous observations of Mkn 501, a behavior never seen before in this or any other blazar. The overall X-ray spectrum hardens with increasing intensity and, at each epoch, it is softer at larger energies. The correlated variability from soft X-rays to the TeV band points to models in which the same population of relativistic electrons produces the X-ray continuum via synchrotron radiation and the TeV emission by inverse Compton scattering of the synchrotron photons or other seed photons. For the first time in any blazar the synchrotron power is observed to peak at hard X-ray energies. The large shift of the synchrotron peak frequency with respect to previous observations of Mkn 501 implies that intrinsic changes in the relativistic electron spectrum caused the increase in emitted power. Due to the very high electron energies, the inverse Compton process is limited by the Klein-Nishina regime. This implies a quasi-linear (as opposed to quadratic) relation of the variability amplitude in the TeV and hard X-ray ranges (for the SSC model) and an increase of the inverse Compton peak frequency smaller than that of the synchrotron peak frequency.']",['1997-10-30'] +1793,['eng'],"['Stecker, F W']",['On the Origin of the Highest Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['nucleus, cosmic radiation', 'nucleus, photofission', 'astrophysics, galaxy', 'cosmic radiation, energy loss', 'photon, cosmic radiation', 'cosmic radiation, background', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710353'],"['We present the results of a new estimation of the photodisintegration and propagation of ultrahigh energy cosmic ray (UHCR) nuclei in intergalactic space. The critical interactions for photodisintegration and energy loss of UHCR nuclei occur with photons of the infrared background radiation (IBR). We have reexamined this problem making use of a new determination of the IBR based on empirical data, primarily from IRAS galaxies, and also collateral information from TeV gamma-ray observations of two nearby BL Lac objects. Our results indicate that a 200 EeV Fe nucleus can propagate apx. 100 Mpc through the IBR. We argue that it is possible that the highest energy cosmic rays observed may be heavy nuclei.']",['1997-10-31'] +1794,['eng'],"['Saeki, T', 'Anraku, K', 'Orito, S', 'Ormes, J', 'Imori, M', 'Kimbell, B L', 'Makida, Y', 'Matsumoto, H', 'Matsunaga, H', 'Mitchell, J', 'Motoki, M', 'Nishimura, J', 'Nozaki, M', 'Otoba, M', 'Sanuki, T', 'Streitmatter, R E', 'Suzuki, J', 'Tanaka, K', 'Ueda, I', 'Yajima, N', 'Yamagami, T', 'Yamamoto, A', 'Yoshida, T', 'Yoshimura, K']",['A New Limit on the Flux of Cosmic Antihelium'],['Astrophysics and Astronomy'],"['cosmic radiation, antinucleus', 'cosmic radiation, flux', 'upper limit', 'helium, antiparticle', 'magnetic spectrometer, satellite', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710228'],"['A very sensitive search for cosmic-ray antihelium was performed using data obtained from three scientific flights of BESS magnetic rigidity spectrometer. We have not observed any antihelium; this places a model-independent upper limit (95 % C.L.) on the antihelium flux of 6*10**(-4) m**(-2)sr**(-1)s**(-1) at the top of the atmosphere in the rigidity region 1 to 16 GV, after correcting for the estimated interaction loss of antihelium in the air and in the instrument. The corresponding upper limit on the Hebar/He flux ratio is 3.1*10**(-6), 30 times more stringent than the limits obtained in similar rigidity regions with magnetic spectrometers previous to BESS.']",['1997-10-22'] +1795,['eng'],"['Protheroe, R J', 'Bhat, C L', 'Fleury, P', 'Lorenz, E', 'Teshima, M', 'Weekes, T C']",['Very high energy gamma rays from Markarian 501'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710118'],"['During remarkable flaring activity in 1997 Markarian 501 was the brightest source in the sky at TeV energies, outshining the Crab Nebula by a factor of up to 10. Periods of flaring activity each lasting a few days were observed simultaneously by several gamma ray telescopes. Contemporaneous multiwavelength observations in April 1997 show that a substantial fraction of the total AGN power is at TeV energies indicating that high energy processes dominate the energetics of this object. Rapid variability, on time scales of less than a day, and a flat spectrum extending up to at least 10 TeV characterize this object. Results of 1997 observations by 6 telescopes are summarized and some of the implications of these results are discussed.']",['1997-10-14'] +1796,['eng'],"['Lee, W H', 'Kluzniak, W']",['Gravitational radiation from mergers of black hole neutron star binaries'],['Astrophysics and Astronomy'],"['talk, Geneva 1997/07/01', 'gravitational radiation', 'black hole', 'n, matter', 'angular momentum', 'counters and detectors', 'luminosity', 'approximation, multipole', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709301'],"['Angular momentum loss via the emission of gravitational waves must eventually drive compact binaries containing black holes and/or neutron stars to coalesce. The resulting events are primary candidate sources for detectors such as VIRGO and LIGO. We present calculations of gravitational radiation waveforms and luminosities for the coalescence of a black hole-neutron star binary, performed in the quadrupole approximation using a Newtonian smooth particle hydrodynamics code. We discuss the dependence of the waveforms and the total emitted luminosity as well as the final configuration of the system on the initial mass ratio and the degree of tidal locking.']",['1997-10-01'] +1797,['eng'],"['De van Bruck, C']",['The Peculiar-Velocity-Field in Structure Formation Theories with Cosmic Strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'velocity, galaxy', 'astrophysics, model', 'matter, density', 'scaling', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710332'],"['We investigate the peculiar velocity field due to long cosmic strings in several cosmological models and analyse the influence of a nonscaling behaviour of the string network, which is expected in open cosmological models or models with a cosmological constant. It is shown that the deviation of the propability distribution of the peculiar velocity field from the normal distribution is only weak in all models. It is further argued that one can not necessarily obtain the parameter $\\beta=\\Omega_{0}^{0.6}/b$ from density and velocity fields, where $\\Omega_0$ is the density parameter and $b$ the linear biasing parameter, if cosmic strings are responsible for structure formation in the universe. An explanation for this finding is given.']",['1997-10-30'] +1798,['eng'],"['Hofmann, W']",['Measuring Gamma-Ray Energy Spectra with the HEGRA IACT System'],['Astrophysics and Astronomy'],"['talk, Kruger National Park 1997/08/08', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'showers, air', 'showers, energy', 'showers, spatial distribution', 'data analysis method', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710297'],"[""The stereoscopic reconstruction of air showers viewed by multiple imaging atmospheric Cherenkov telescopes (IACTs) allows a more precise reconstruction of shower energies and hence an improved determination of energy spectra. Reconstruction techniques and in particular new systematic checks are discussed on the basis of the large sample of gamma-rays from Mkn 501 detected with the HEGRA IACT system. (Talk presented at the Workshop ``Towards a Major Atmospheric Cherenkov Detector V'', Kruger Park, South Africa, 1997)""]",['1997-10-28'] +1799,['eng'],"['Bernabei, R', 'Belli, P', 'Montecchia, F', 'Nicolantonio, W D', 'Incicchitti, A', 'Prosperi, D', 'Bacci, Cesare', 'Dai, C J', 'Ding, L K', 'Kuang, H H', 'Ma, J M']",['WIMPs search by scintillators'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'cosmic radiation, time variation', 'search for, WIMP', 'scattering, WIMP nucleus', 'data analysis method', 'scintillation counter, sodium-iodide', 'experimental results', 'deep underground detector, Gran Sasso']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710290'],['The DAMA experiments are running deep underground in the Gran Sasso National Laboratory. Several interesting results have been achieved so far. Here a maximum likelihood method to search for the WIMP annual modulation signature is discussed and applied to a set of preliminary test data collected with large mass highly radiopure NaI(Tl) detectors. Various related technical arguments are briefly addressed.'],['1997-10-28'] +1800,['eng'],"[""Degl'Innocenti, S"", 'Ricci, B']","['A Mixed Solar Core, Solar Neutrinos and Helioseismology']",['Astrophysics and Astronomy'],"['model, solar', 'neutrino, solar', 'neutrino, flux', 'temperature, solar', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710292'],"['We consider a wide class of solar models with mixed core. Most of these models can be excluded as the predicted sound speed profile is in sharp disagreement with helioseismic constraints. All the remaining models predict $^7$Be and/or $^7$B neutrino fluxes at least as large as those of SSMs. In conclusion, helioseismology shows that a mixed solar core cannot account for the neutrino deficit implied by the current solar neutrino experiments.']",['1997-10-28'] +1801,['eng'],"['Knapp, J']",['High-Energy Interactions and Extensive Air Showers'],['Astrophysics and Astronomy'],"['review, Durban 1997/07/28', 'cosmic radiation', 'showers, air', 'nucleus nucleus, nuclear reaction', 'scattering, heavy ion', 'electron p, deep inelastic scattering', 'anti-p p, annihilation', 'p p, interaction', 'p nucleus, nuclear reaction', 'programming, Monte Carlo', 'counters and detectors', 'nuclear emulsion', 'rapidity spectrum', 'p, structure function', 'pi, production', 'cross section, energy dependence', 'electron, flux', 'muon, flux', 'hadron, energy spectrum', 'numerical calculations, Monte Carlo', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710277'],['In this report a summary of recent developments in the fields of high-energy nuclear interactions (HE 1) and air shower phenomenology (HE 2) is presented. New results from accelerator and cosmic-ray experiments and the progress in the theoretical understanding and simulation are reviewed and their impact on air shower analysis is discussed.'],['1997-10-27'] +1802,['eng'],"['Leinson, L B', 'Pérez, A']",['Collective effects in $\\nu \\overline{\\nu}$ synchrotron radiation from neutron stars'],['Astrophysics and Astronomy'],"['astrophysics', 'n, matter', 'magnetic field', 'synchrotron radiation, neutrino antineutrino', 'electron, gas', 'plasma, collective phenomena', 'neutrino, pair production', 'weak interaction, model', 'effective Lagrangian', 'Feynman graph', 'energy spectrum, (neutrino antineutrino)', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710257'],"['We have considered collective effects in $\\nu \\bar{\\nu}$ synchrotron radiation from an ultrarelativistic degenerate electron gas in neutron stars with strong magnetic fields. For this problem we apply a calculation method which explicitly makes use of the fact that the radiating electron moves semi-classically, but takes into account the interaction among particles in a quantum way. First we apply this method to calculate $\\nu \\bar{\\nu}$ synchrotron radiation by an ultrarelativistic electron in vacuum and we compare this result with that obtained previously by other techniques. When a degenerate plasma is considered, we show that collective effects lead to an essential enhancement (about three times) of the vector weak-current contribution to neutrino pair emissivity.']",['1997-10-24'] +1803,['eng'],"['Liddle, A R', 'Green, A M']",['Primordial black holes and early cosmology'],['Astrophysics and Astronomy'],"['black hole', 'density, perturbation', 'inflationary universe', 'light nucleus, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710235'],['We describe the changes to the standard primordial black hole constraints on density perturbations if there are modifications to the standard cosmology between the time of formation and nucleosynthesis.'],['1997-10-23'] +1804,['eng'],"['Totani, T', 'Sato, K', 'Dalhed, H E', 'Wilson, J R']",['Future Detection of Supernova Neutrino Burst and Explosion Mechanism'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, cosmic radiation', 'neutrino, particle identification', 'statistical analysis', 'neutrino, energy spectrum', 'neutrino, flux', 'neutrino, luminosity', 'time dependence', 'deep underground detector, KAMIOKANDE', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710203'],"['Future detection of a supernova neutrino burst by large underground detectors would give important information for the explosion mechanism of collapse-driven supernovae. We studied the statistical analysis for the future detection of a nearby supernova by using a numerical supernova model and realistic Monte-Carlo simulations of detection by the Super-Kamiokande detector. We mainly discuss the detectability of the signatures of the delayed explosion mechanism in the time evolution of the $\\anue$ luminosity and spectrum. For a supernova at 10 kpc away from the Earth, we find that not only the signature is clearly discernible, but also the deviation of energy spectrum from the Fermi-Dirac (FD) distribution can be observed. The deviation from the FD distribution would, if observed, provide a test for the standard picture of neutrino emission from collapse-driven supernovae. For the $D$ = 50 kpc case, the signature of the delayed explosion is still observable, but statistical fluctuation is too large to detect the deviation from the FD distribution. We also propose a method for statistical reconstruction of the time evolution of evolution and smaller statistical errors than a simple, time-binning analysis. This method is useful especially when the available number of events is relatively small, e.g., a supernova in the LMC or SMC. Neutronization burst of is difficult to distinguish from $\\anue p$ events.']",['1997-10-21'] +1805,['eng'],"['Eisenstein, D J', 'Hu, W']",['Small Scale Perturbations in a General MDM Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutrino, massive', 'neutrino, density', 'baryon', 'density, perturbation', 'astrophysics, fundamental constant', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710216'],"['For a universe with massive neutrinos, cold dark matter, and baryons, we solve the linear perturbation equations analytically in the small-scale limit and find agreement with numerical codes at the 1-2% level. The inclusion of baryons, a cosmological constant, or spatial curvature reduces the small-scale power and tightens limits on the neutrino density from observations of high redshift objects. Using the asymptotic solution, we investigate neutrino infall into potential wells and show that it can be described on all scales by a growth function that depends on time, wavenumber, and cosmological parameters. The growth function may be used to scale the present-day transfer functions back in redshift. This allows us to construct the time-dependent transfer function for each species from a single master function that is independent of time, cosmological constant, and curvature.']",['1997-10-22'] +1806,['eng'],"['Mathews, G J', 'Wilson, J R', 'Salmonson, J D']",['Gamma-Ray Bursts from Neutron Star Binaries'],['Astrophysics and Astronomy'],"['talk, Jerusalem 1997/06/22', 'n, matter', 'photon, cosmic radiation', 'photon, luminosity', 'model, hydrodynamical', 'relativistic', 'neutrino, cosmic radiation', 'model, fluid', 'magnetic field', 'electron positron, plasma', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710229'],"['We report on general relativistic hydrodynamic studies which indicate several new physical processes which may contribute to powering gamma-ray bursts in neutron star binaries. Relativistically driven compression, heating, and collapse of the individual stars can occur many seconds before inspiral and merger. This compression may produce a neutrino burst of $\\sim 10^{53}$ ergs lasting several seconds. The associated thermal neutrino emission produces an $e^+-e^-$ pair plasma by $\\nu \\bar \\nu$ annihilation. We show first results of a simulated burst which produces $\\sim 10^{51}$ erg in $\\gamma$-rays. We also discuss a preliminary study of the evolution of the magnetic field lines attached to the fluid as the stars orbit. We show that the relativistically driven fluid motion might lead to the formation of extremely strong magnetic fields ($\\sim 10^{17}$ gauss) in and around the stars which could affect to the formation and evolution of a gamma-ray burst.']",['1997-10-22'] +1807,['eng'],"['Kaniadakis, G', 'Lavagno, A', 'Lissia, M', 'Quarati, P']",['Anomalous diffusion modifies solar neutrino fluxes'],['Astrophysics and Astronomy'],"['neutrino, solar', 'flux', 'model, solar', 'electron, diffusion', 'ion, diffusion', 'many-body problem', 'correlation, time', 'thermodynamics', 'statistics', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710173'],"['Density and temperature conditions in the solar core suggest that the microscopic diffusion of electrons and ions could be nonstandard: diffusion and friction coefficients are energy dependent, collisions are not two-body processes and retain memory beyond the single scattering event. A direct consequence of nonstandard diffusion is that the equilibrium energy distribution of particles departs from the Maxwellian one (tails goes to zero more slowly or faster than exponentially) modifying the reaction rates. This effect is qualitatively different from temperature and/or composition modification: small changes in the number of particles in the distribution tails can strongly modify the rates without affecting bulk properties, such as the sound speed or hydrostatic equilibrium, which depend on the mean values from the distribution. This mechanism can considerably increase the range of predictions for the neutrino fluxes allowed by the current experimental values (cross sections and solar properties) and can be used to reduce the discrepancy between these predictions and the solar neutrino experiments.']",['1997-10-17'] +1808,['eng'],"['Szabelski, J']",['Cosmic Rays'],['Astrophysics and Astronomy'],"['review', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'photon, diffusion', 'cosmic radiation, mass spectrum', 'cosmic radiation, energy spectrum', 'muon, showers', 'counters and detectors', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710191'],"['Investigations of the origin of cosmic rays are presented. Different methods are discussed: studies of cosmic gamma rays of energy from 30 MeV to about 10^15 eV (since photons point to their places of origin), studies of the mass composition of cosmic rays (because it reflects source morphology), and studies of cosmic rays with energy above 10^19 eV (for these are the highest energies observed in nature).']",['1997-10-20'] +1809,['eng'],"['Gerbier, G', 'Mallet, J', 'Mosca, L', 'Tao, Charling']","['Note on a ""hint"" for an annual modulation signature of a 60 GeV WIMP']",['Astrophysics and Astronomy'],"['cosmic radiation, time variation', 'scattering, WIMP nucleus', 'mass, WIMP', 'scintillation counter, sodium-iodide', 'numerical calculations', 'interpretation of experiments, Gran Sasso']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710181'],"['In a recent presentation at the TAUP97 conference about the analysis of data from a NaI(Tl) 100 kg underground detector run at the Gran Sasso Laboratory by the DAMA/NaI group, the speaker concluded there was a hint for a WIMP of mass 60 GeV with a cross section on proton of 10-5 pb (Spin Independent coupling) (see also ROM2F/97/33). Even if no claim of any definite signal is made, such a statement is strong enough to deserve a critical look. The present note puts forward a few arguments which point towards a largely overestimated statistical significance of the effect, an inconsistency in the energy distribution and several experimental effects which could easily mimic the observed excess. The conclusion is that, in no way, the presented result can be considered as a hint of a WIMP annual modulation.']",['1997-10-17'] +1810,['eng'],"['Moskalenko, I V', 'Strong, A W']",['Production and propagation of cosmic-ray positrons and electrons'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'positron, cosmic radiation', 'nucleon, cosmic radiation', 'electron, cosmic radiation', 'cosmic radiation, energy spectrum', 'helium, cosmic radiation', 'cosmic radiation, fragmentation', 'cosmic radiation, energy loss', 'cosmic radiation, diffusion', 'astrophysics, galaxy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710124'],"['We have made a new calculation of the cosmic-ray secondary positron spectrum using a diffusive halo model for Galactic cosmic-ray propagation. The code computes self-consistently the spectra of primary and secondary nucleons, primary electrons, and secondary positrons and electrons. The models are first adjusted to agree with the observed cosmic-ray Boron/Carbon ratio, and the interstellar proton and Helium spectra are then computed; these spectra are used to obtain the source function for the secondary positrons/electrons which are finally propagated with the same model parameters. The primary electron spectrum is evaluated, again using the same model. Fragmentation and energy losses are computed using realistic distributions for the interstellar gas and radiation fields, and diffusive reacceleration is also incorporated. Our study includes a critical re-evaluation of the secondary decay calculation for positrons. The predicted positron fraction is in good agreement with the measurements up to 10 GeV, beyond which the observed flux is higher than that calculated. Since the positron fraction is now accurately measured in the 1-10 GeV range our primary electron spectrum should be a good estimate of the true interstellar spectrum in this range, of interest for gamma ray and solar modulation studies. We further show that a harder interstellar nucleon spectrum, similar to that suggested to explain EGRET diffuse Galactic gamma ray observations above 1 GeV, can reproduce the positron observations above 10 GeV without requiring a primary positron component.']",['1997-10-14'] +1811,['eng'],"['Stecker, F W', 'De Jager, O C']",['Absorption of Intergalactic TeV Gamma-Rays'],['Astrophysics and Astronomy'],"['talk, Kruger National Park 1997/08/08', 'photon, cosmic radiation', 'particle source', 'energy spectrum', 'absorption', 'astrophysics, galaxy', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710145'],"['We discuss the problem of the absorption of very high-energy gamma-rays by pair production interactions with extragalactic photons which originate from stellar emission in the near IR-UV and reradiation of starlight in the mid- and far-IR. The absorption of gamma-rays above 1 TeV is dominated by interactions with infrared photons. We make a new determination of the optical depth of the universe to multi-TeV photons as a function of energy and redshift and use the results to compare with recent spectral data of Mrk 421 and Mrk 501, sources that have been observed in the flaring state up to apx. 10 TeV energy. For the optical depth calculations, we have made use of a new, empirically based calculation of the intergalactic radiation field by Malkan & Stecker which we consider to be more accurate than that based on previous theoretical modeling. We also discuss the absorption of sub-TeV gamma-rays by starlight photons at high redshifts.']",['1997-10-15'] +1812,['eng'],"['Berezinsky, Veniamin Sergeevich']",['Solar neutrinos as highlight of astroparticle physics'],['Astrophysics and Astronomy'],"['review, Durban 1997/07/28', 'model, solar', 'neutrino, solar', 'neutrino, flux', 'nucleus nucleus, nuclear reaction', 'neutrino, oscillation', 'neutrino, energy spectrum', 'deep underground detector', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710126'],['Solar neutrinos are discussed in the light of the new data and of recent progress in helioseismology. Most attention is given to the new status of Standard Solar Models due to seismically measured density and sound speed in the inner solar core. The elementary particle solutions to the Solar Neutrino Problem and their observational signatures are discussed.'],['1997-10-14'] +1813,['eng'],"['Monaco, P']",['The Cosmological Mass Function'],['Astrophysics and Astronomy'],['Thesis'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710085'],"[""This thesis aims to review the cosmological mass function problem, both from the theoretical and the observational point of view, and to present a new mass function theory, based on realistic approximations for the dynamics of gravitational collapse. Chapter 1 gives a general introduction on gravitational dynamics in cosmological models. Chapter 2 gives a complete review of the mass function theory. Chapters 3 and 4 present the ``dynamical'' mass function theory, based on truncated Lagrangian dynamics and on the excursion set approach. Chapter 5 reviews the observational state-of-the-art and the main applications of the mass function theories described before. Finally, Chapter 6 gives conclusions and future prospects.""]",['1997-10-09'] +1814,['eng'],"['Reddy, S', 'Prakash, M', 'Lattimer, J M']",['Neutrino Interactions in Hot and Dense Matter'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'n, matter', 'charged current', 'neutral current', 'matter, opacity', 'neutrino, path length', 'transport theory', 'scattering, neutrino baryon', 'relativistic', 'nonrelativistic', 'differential cross section', 'scattering, path length', 'absorption, path length', 'strong interaction, correction', 'potential, model', 'hyperon, effect', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710115'],"['We study the charged and neutral current weak interaction rates relevant for the determination of neutrino opacities in dense matter found in supernovae and neutron stars. We establish an efficient formalism for calculating differential cross sections and mean free paths for interacting, asymmetric nuclear matter at arbitrary degeneracy. The formalism is valid for both charged and neutral current reactions. Strong interaction corrections are incorporated through the in-medium single particle energies at the relevant density and temperature. The effects of strong interactions on the weak interaction rates are investigated using both potential and effective field-theoretical models of matter. We investigate the relative importance of charged and neutral currents for different astrophysical situations, and also examine the influence of strangeness-bearing hyperons. Our findings show that the mean free paths are significantly altered by the effects of strong interactions and the multi-component nature of dense matter. The opacities are then discussed in the context of the evolution of the core of a protoneutron star.']",['1997-10-13'] +1815,['eng'],"['Adams, F C', 'Freese, Katherine', 'Laughlin, G', 'Tarlé, G', 'Schwadron, N']",['Constraints on the Intergalactic Transport of Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'flux', 'astrophysics, galaxy', 'magnetic field', 'path length', 'astrophysics, model', 'antimatter', 'photon, cosmic radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710113'],"['Motivated by recent experimental proposals to search for extragalactic cosmic rays (including anti-matter from distant galaxies), we study particle propagation through the intergalactic medium (IGM). We first use estimates of the magnetic field strength between galaxies to constrain the mean free path for diffusion of particles through the IGM. We then develop a simple analytic model to describe the diffusion of cosmic rays. Given the current age of galaxies, our results indicate that, in reasonable models, a completely negligible number of particles can enter our Galaxy from distances greater than that particle destruction in galaxies along the diffusion path produces an exponential suppression of the possible flux of extragalactic cosmic rays. Finally, we use gamma ray constraints to argue that the distance to any hypothetical domains of anti-matter must be roughly comparable to the horizon scale.']",['1997-10-13'] +1816,['eng'],"['Caldwell, R R', 'Steinhardt, Paul Joseph']",['The Imprint of Gravitational Waves in Models Dominated by a Dynamical Cosmic Scalar Field'],['Astrophysics and Astronomy'],"['gravitational radiation', 'inflationary universe', 'field theory, scalar', 'energy, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'spectra, perturbation', 'perturbation, scalar', 'perturbation, tensor', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710062'],"['An alternative to the standard cold dark matter model has been recently proposed in which a significant fraction of the energy density of the universe is due to a dynamical scalar field ($Q$) whose effective equation-of-state differs from that of matter, radiation or cosmological constant ($\\Lambda$). In this paper, we determine how the Q-component modifies the primordial inflation gravitational wave (tensor metric) contribution to the cosmic microwave background anisotropy and, thereby, one of the key tests of inflation.']",['1997-10-07'] +1817,['eng'],"['Walther, G']",['Absence of Correlation between the Solar Neutrino Flux and the Sunspot Number'],['Astrophysics and Astronomy'],"['neutrino, solar', 'flux, time variation', 'neutrino, particle identification', 'neutrino, magnetic moment', 'model, solar', 'correlation', 'statistical analysis', 'numerical calculations', 'interpretation of experiments, Homestake']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710031'],"['There exists a considerable amount of research claiming a puzzling anti-correlation between the neutrino detection rate at the Homestake experiment and indicators of solar activity such as the sunspot number, giving rise to explanations involving the hypothesis of a neutrino magnetic moment. It is argued here that the claimed significant anti-correlation is due to a statistical fallacy. A proper test based on certain optimality criteria fails to detect a significant time variation of the neutrino flux in concert with the sunspot number, providing evidence that the observations are consistent with no correlation between the two series.']",['1997-10-03'] +1818,['eng'],"['Bassett, B A']",['Resonant Gravitational Wave Amplification'],['Astrophysics and Astronomy'],"['talk, Geneva 1997/07/01', 'gravitational radiation, measurement', 'background, stochastic', 'inflationary universe', 'axion', 'resonance, effect', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710036'],"['We demonstrate the parametric amplification of the stochastic gravitational wave background during inflationary reheating and during axion/moduli oscillations. This amplification enhances the detectability of the string/inflationary gravity wave signal, leaving a finger-print on the spectrum which might be found with future gravitational wave detectors.']",['1997-10-03'] +1819,['eng'],"['Mukhanov, V F', 'Steinhardt, Paul Joseph']",['Density Perturbations in Multifield Inflationary Models'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'spectra, perturbation', 'potential', 'field theory, scalar', 'decoupling']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710038'],"['We derive a closed-form, analytical expression for the spectrum of long-wavelength density perturbations in inflationary models with two (or more) inflaton degrees of freedom that is valid in the slow-roll approximation. We illustrate several classes of potentials for which this expression reduces to a simple, algebraic expression.']",['1997-10-07'] +1820,['eng'],"['Fargion, D', 'Melé, B', 'Salis, A']",['Ultrahigh energy neutrino scattering onto relic light neutrinos in galactic halo as a possible source of highest energy extragalactic cosmic rays'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, cluster', 'particle source, galaxy', 'photon p, interaction', 'pi, photoproduction', 'pi, decay', 'channel cross section, energy dependence', 'neutrino antineutrino, interaction', 'W, pair production', 'p, production', 'photon, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9710029'],"[""The diffuse relic neutrinos with light mass are transparent to Ultrahigh energy (UHE) neutrinos at thousands EeV, born by photoproduction of pions by UHE protons on relic 2.73 K BBR radiation and originated in AGNs at cosmic distances. However these UHE $\\nu$s may interact with those (mainly heaviest galactic halos. UHE photons or protons, secondaries of $\\nu\\nu_R$ scattering, might be the final observed signature of such high-energy chain reactions and may be responsible of the highest extragalactic cosmic-ray (CR) events. The chain-reactions conversion efficiency, ramifications and energetics are considered for the October 1991 CR event at 320 EeV observed by the Fly's Eye detector in Utah. These quantities seem compatible with the distance, direction and power (observed at MeV gamma energies) of the Seyfert galaxy MCG 8-11-11. The $\\nu\\nu_R$ interaction probability is favoured by at least three order of magnitude with respect to a direct $\\nu$ scattering onto the Earth atmosphere. Therefore, it may better explain the extragalactic origin of the puzzling 320 EeV event, while offering indirect evidence of a hot dark galactic halo of light (i.e., $m_\\nu\\sim$ tens eV) neutrinos, probably of tau flavour.""]",['1997-10-03'] +1821,['eng'],"['Biermann, P L', 'Kang, H', 'Ryu, D']",['The supergalactic structure and the origin of the highest energy cosmic rays'],['Astrophysics and Astronomy'],"['talk, Tanashi 1996/09/25', 'astrophysics, galaxy', 'magnetic field', 'cosmic radiation', 'flux', 'particle source', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709250'],"['The recent discoveries of several reliable events of high energy cosmic rays at an energy above 10^20 eV raise questions about their path through the nearby universe. The two analyses of the Haverah Park data set and the Akeno data set appear to have an inconsistent pattern. Both data sets showed some measure of a correlation with the supergalactic plane, the locus of cosmologically nearby galaxies, radio galaxies and clusters of galaxies. We need a reasonable model of the true intergalactic magnetic field. Using recent cosmological simulations of structure formation in the universe, we estimate the magnetic fields which correspond to the upper limits in the Rotation Measure to distant radio sources. We estimate that the magnetic field strength in supergalactic sheets and filaments may be in the range of 0.1 to 1 muG. If such strengths are realized inside our Local Supercluster, this opens up the possibility to focus charged particles in the direction perpendicular to the supergalatic plane, analoguously but in the opposite direction to solar wind modulation. If focusing exists, it means that for all particles captured into the sheets, the dilution with distance d is 1/d instead of 1/d^2. This means in effect, that we may see sources to much larger distances than expected sofar. This effect is relevant only for energies for which the possible distances are smaller than the void scale of the cosmological galaxy distribution, in the range possibly up to 100 Mpc.']",['1997-09-26'] +1822,['eng'],"['Sreekumar, P', 'Bertsch, D L']",['EGRET Observations of the Extragalactic Gamma Ray Emission'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'energy spectrum', 'counters and detectors, satellite', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709257'],"['The all-sky survey in high-energy gamma rays (E$>$30 MeV) carried out by the Energetic Gamma Ray Experiment Telescope (EGRET) aboard the Compton Gamma-Ray Observatory provides a unique opportunity to examine in detail the diffuse gamma-ray emission. The observed diffuse emission has a Galactic component arising from cosmic-ray interactions with the local interstellar gas and radiation as well an almost uniformly distributed component that is generally believed to originate outside the Galaxy. Through a careful study and removal of the Galactic diffuse emission, the flux, spectrum and uniformity of the extragalactic emission is deduced. The analysis indicates that the extragalactic emission is well described by a power law photon spectrum with an index of -(2.10+-0.03) in the 30 MeV to 100 GeV energy range. No large scale spatial anisotropy or changes in the energy spectrum are observed in the deduced extragalactic emission. The most likely explanation for the origin of this extragalactic high-energy gamma-ray emission is that it arises primarily from unresolved gamma-ray-emitting blazars.']",['1997-09-26'] +1823,['eng'],"['Strong, A W', 'Moskalenko, I V']",['Modelling cosmic rays and gamma rays in the Galaxy'],['Astrophysics and Astronomy'],"['talk, Williamsburg 1997/04/27', 'cosmic radiation, primary', 'secondary radiation', 'photon, cosmic radiation', 'particle source, galaxy', 'diffusion', 'energy loss', 'fragmentation', 'nucleon, cosmic radiation', 'electron, cosmic radiation', 'positron, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709211'],"['An extensive program for the calculation of galactic cosmic-ray propagation has been developed. This is a continuation of the work described in Strong & Youssefi (1995). The main motivation for developing this code is the prediction of diffuse Galactic gamma rays for comparison with data from the CGRO instruments EGRET, COMPTEL, and OSSE. The basic spatial propagation mechanisms are (momentum-dependent) diffusion, convection, while in momentum space energy loss and diffusive reacceleration are treated. Primary and secondary nucleons, primary and secondary electrons, and secondary positrons are included. Fragmentation and energy losses are computed using realistic distributions for the interstellar gas and radiation fields. This study indicates that it is possible to construct a model satisfying a wide range of observational constraints and provides a basis for future developments.']",['1997-09-23'] +1824,['eng'],"['Allen, C', 'Bean, A', 'Besson, D', 'Frichter, G', 'Kotov, S A', 'Kravchenko, I V', 'McKay, D', 'Miller, T', 'Piccirillo, L', 'Ralston, J P', 'Seckel, D', 'Seunarine, S', 'Spiczak, G']",['Status of Radio Ice Cherenkov Experiment (RICE)'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, astrophysics', 'neutrino nucleon, interaction', 'charged current', 'Cherenkov counter, water', 'solids, water', 'electronics', 'performance', 'deep underground detector, AMANDA']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709223'],"['RICE is designed to detect ultrahigh energy (>100 TeV) neutrinos from astrophysical sources. It will consist of an array of compact radio (100 to 1000 MHz) receivers buried in ice at the South Pole. During the 1995-96 and 1996-97 austral summers, several receivers transmitters were deployed in bore holes drilled for the AMANDA project, at depths of 141 to 260 m. This was the first in situ test of radio receivers in deep ice for neutrino astronomy.']",['1997-09-24'] +1825,['eng'],"['Pina-Avelino, P', 'De Carvalho, J P M']",['Cosmic strings with interacting hot dark matter'],['Astrophysics and Astronomy'],"['astrophysics, string', 'spectra, linear', 'density, fluctuation', 'neutrino neutrino, interaction', 'astrophysics, missing-mass', 'galaxy', 'density, perturbation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709221'],"[""We compute the linear power spectrum of cosmic string sedeed fluctuations in the context of neutrinos with a strong self-interaction and show that it is very similar to that obtained in the context of `normal' neutrinos. We compare our results with observational data and show that for any value of the cosmological parameters $h$ and $\\Omega_0$ the interacting hot dark matter power spectrum requires a large scale dependent biasing parameter.""]",['1997-09-24'] +1826,['eng'],"['Kachelriess, M']",['Are strongly magnetized degenerate stars cooling by axion emission?'],['Astrophysics and Astronomy'],"['talk, Tegernsee 1997/06/08', 'n, matter', 'axion, emission', 'magnetic field, external field', 'luminosity, axion', 'coupling constant, (electron axion)', 'lower limit', 'astrophysics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709204'],"['We considered recently as a new axion production mechanism the process $e^- magnetized neutron star the axion luminosity is smaller than the neutrino luminosity we obtained the bound $g_{ae} \\lsim 10^{-10}$ for the axion electron coupling constant. This limit is considerably weaker than the bound derived earlier by Borisov and Grishina using the same method. Applying a similar argument to magnetic white dwarf stars we obtained $g_{ae}\\lsim 9 \\cdot 10^{-13} (T/10^7)^{5/4} (B/10^{10})^{-2}$, where $T$ is the internal temperature of the white dwarf. Here we note that the observed lack of magnetized white dwarfs with low-temperature in the galactic disc could also be interpreted as a signature of axion emission. Moreover, we speculate that axion emission could explain why the putative galactic halo population of white dwarfs is so dim.']",['1997-09-23'] +1827,['eng'],"['Kuzmin, V A', 'Rubakov, V A']",['Ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['talk, Tegernsee 1997/06/08', 'talk, Dubna 1997/07/07', 'cosmic radiation, energy spectrum', 'particle, heavy', 'particle, decay', 'particle, lifetime', 'instanton', 'showers, air', 'inflationary universe']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709187'],"['We conjecture that the highest energy cosmic rays beyond the Greisen-Zatsepin-Kuzmin cut-off may provide a unique window into the very early epoch of the Universe, namely, that of reheating after inflation, provided these cosmic rays are due to decays of parent superheavy long-living X-particles. These particles may constitute a considerable fraction of cold dark matter in the Universe. We argue that the unconventionally long lifetime of the superheavy particles, which should be in the range of $10^{10} - 10^{22}$ years, might require novel particle physics mechanisms of their decays, such as instantons. We propose a toy model illustrating the instanton scenario. Generic expected features of ultra-high energy extensive air showers in our scenario are similar to those of other top-down scenarios. However, some properties of the upper part of the cosmic ray spectrum make the instanton scenario distinguishable, at least in principle, from other ones.']",['1997-09-19'] +1828,['eng'],"['Mezzacappa, A', 'Calder, A C', 'Bruenn, S W', 'Blondin, J M', 'Guidry, M W', 'Strayer, M R', 'Umar, A S']",['Investigation of Neutrino-Driven Convection and the Core Collapse Supernova Mechanism Using Multigroup Neutrino Transport'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'matter, mass', 'energy, internal', 'gravitation', 'neutrino, cosmic radiation', 'neutrino, diffusion', 'transport theory', 'model, hydrodynamical', 'neutrino, density', 'entropy', 'electron, density', 'velocity', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709188'],"['We investigate neutrino-driven convection in core collapse supernovae and its ramifications for the explosion mechanism, for a 15 solar mass model. Our two-dimensional simulation begins at 12 ms after bounce and proceeds for 500 ms. We couple two-dimensional PPM hydrodynamics to precalculated one-dimensional MGFLD neutrino transport. (The accuracy of this approximation is assessed.) For the moment we sacrifice dimensionality for realism in other aspects of our neutrino transport. MGFLD is an implementation of neutrino transport that simultaneously (a) is multigroup and (b) simulates with greater realism the transport of neutrinos in opaque, semitransparent, and transparent regions. Both are crucial to the accurate determination of postshock neutrino heating, which sensitively depends on the luminosities, spectra, and flux factors of the electron neutrinos and antineutrinos emerging from their respective neutrinospheres. By 212 ms after bounce, we see large-scale, neutrino-driven convection beneath the shock, characterized by higher-entropy, expanding upflows and denser, lower-entropy, finger-like downflows. The radial convection velocities at this time become supersonic just below the shock, reaching magnitudes in excess of 10^{9} cm/sec. Eventually, however, the shock recedes to smaller radii, and at 500 ms after bounce there is no evidence in our simulation of an explosion. While vigorous, neutrino-driven convection in our model does not have a significant impact on the overall shock dynamics. The differences between our results and those of other groups are considered. These most likely result from differences in (1) numerical hydrodynamics methods, (2) initial postbounce models, and most important, (3) neutrino transport approximations.']",['1997-09-19'] +1829,['eng'],"['Mezzacappa, A', 'Calder, A C', 'Bruenn, S W', 'Blondin, J M', 'Guidry, M W', 'Strayer, M R', 'Umar, A S']",['The Interplay Between Protoneutron Star Convection and Neutrino Transport in Core Collapse Supernovae'],['Astrophysics and Astronomy'],"['n, matter', 'p, matter', 'astrophysics, supernova', 'neutrino, cosmic radiation', 'neutrino, diffusion', 'transport theory', 'entropy', 'velocity', 'model, hydrodynamical', 'boundary condition, time dependence', 'neutrino, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709184'],"[""We couple two-dimensional hydrodynamics to realistic one-dimensional multigroup flux-limited diffusion neutrino transport to investigate protoneutron star convection in core collapse supernovae, and more specifically, the interplay between its development and neutrino transport, for both 15 and 25 solar mass models. In the presence of neutrino transport, protoneutron star convection velocities are too small relative to bulk inflow velocities to result in any significant convective transport of entropy and leptons. A simple analytical model supports our numerical results, indicating that the inclusion of neutrino transport reduces the entropy-driven (lepton-driven) convection growth rates and asymptotic velocities by a factor of 3 (50) at the neutrinosphere and a factor 250 (1000) at a density of 10^{12} g/cm^{3}, for both our 15 and 25 solar mass models. Moreover, when transport is included, the initial postbounce entropy gradient is smoothed out by neutrino diffusion, whereas the initial lepton gradient is maintained by electron capture and neutrino escape near the neutrinosphere. Despite the maintenance of the lepton gradient, protoneutron star convection does not develop over the 100 ms duration typical of all our simulations, except in the instance where ``low-test'' initial conditions are used, which are generated by core collapse and bounce simulations that neglect neutrino-electron scattering and ion-ion screening corrections to neutrino- nucleus elastic scattering.""]",['1997-09-19'] +1830,['eng'],"['Frieman, Joshua A', 'Waga, I']",['Constraints from High Redshift Supernovae upon Scalar Field Cosmologies'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'astrophysics, fundamental constant', 'field theory, scalar', 'astrophysics, model', 'Goldstone particle', 'potential, model', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709063'],"['Recent observations of high-redshift Type Ia supernovae have placed stringent constraints on the cosmological constant $\\Lambda$. We explore the implications of these SNe observations for cosmological models in which a classically evolving scalar field currently dominates the energy density of the Universe. Such models have been shown to share the advantages of $\\Lambda$ models: compatibility with the spatial flatness predicted inflation; a Universe older than the standard Einstein-de Sitter model; and, combined with cold dark matter, predictions for large-scale structure formation in good agreement with data from galaxy surveys. Compared to the cosmological constant, these scalar field models are consistent with the SNe observations for a lower matter density, $\\Omega_{m0} \\sim 0.2$, and a higher age, $H_0 t_0 \\gtrsim 1$. Combined with the fact that scalar field models imprint a distinctive signature on the cosmic microwave background anisotropy, they remain currently viable and should be testable in the near future.']",['1997-09-09'] +1831,['eng'],"['Wandel, A']",['Secondary Accceleration of Cosmic Rays by Supernova Shocks'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'astrophysics, supernova', 'cosmic radiation, acceleration', 'energy spectrum, cosmic radiation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709133'],"['In the common model supernova shock-acceleration of cosmic rays there are two open questions: 1. where does the high energy cosmic rays below the knee (10$^4-10^6$ Gev) come from, and 2. are cosmic ray accelerated only at their origin or contineuosly during their residence in the Galaxy. We show that $10^15$ eV light nuclei are probably accelerted by associations of supernovae. The ratio of the spectra of secondary to primary cosmic rays would be affected by repeated acceleration (also called reacceleration or secondary acceleration) in the ISM during their propagation in the galaxy. The observed secondary and primary CR spectra are used to constrain the amount of such reacceleration by supernova remnants (SNR). Two cases are considered: weak shocks ($13$) of relatively young remnants. It is shown that weak shocks produce more reacceleration than what is permitted in the framework of the standard leaky box (SLB) model, making it inconsistent with dispersed acceleration that should be produced by SNR. If the SLB is modified to allow a moderate amount of RA by week shocks, the RA produced by old SNRs agrees with the rate required to fit the secondary-to primaray cosmic-ray data, making a self consistent picture. Significant reacceleration by strong shocks of young SNRs should lead to flattening of the secondary-to primaray ratio at high energies, near 1TeV/nucleon.']",['1997-09-16'] +1832,['eng'],"['Fierro, J M', 'Michelson, P F', 'Nolan, P L', 'Thompson, D J']","['Phase-Resolved Studies of the High-Energy Gamma-Ray Emission from the Crab, Geminga, and Vela Pulsars']",['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'energy spectrum', 'flux', 'cosmic radiation, particle source', 'astrophysics, pulsar', 'time variation', 'statistical analysis', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709123'],"['Using the first three and a half years of observations from the Energetic Gamma Ray Telescope (EGRET) on board the Compton Gamma Ray Observatory (CGRO), phase-resolved analyses are performed on the emission from the three brightest high-energy gamma-ray pulsars, Crab, Geminga, and Vela. For each pulsar, it is found that there is detectable high-energy gamma-ray emission above the galactic diffuse background throughout much of the pulsar rotation cycle. A hardness ratio is introduced to characterize the evolution of the spectral index as a function of pulsar phase. While the hardest emission from the Crab and Vela pulsars comes from the bridge region between the two gamma-ray peaks, the hardest emission from Geminga corresponds to the second gamma-ray peak. For all three pulsars, phase-resolved spectra of the pulse profile components reveal that although there is a large variation in the spectral index over the pulsar phase interval, the high-energy spectral turnover, if any, occurs at roughly the same energy in each component. The high-energy gamma-ray emission from the Crab complex appears to include an unpulsed ultra-soft component of spectral index ~ -4.3 which dominates the total emission below 100 MeV. This component is consistent with the expected emission from the tail end of the Crab nebula synchrotron emission.']",['1997-09-15'] +1833,['eng'],"['Cohen, Andrew G', 'De Rújula, Alvaro']",['Scars on the CBR?'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'matter, antimatter', 'photon, cosmic radiation', 'photon, spectra', 'photon, Compton scattering', 'anti-p p, annihilation', 'electron, energy loss']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709132'],"['We ask whether the universe can be a patchwork consisting of distinct regions of matter and antimatter. In previous work we demonstrated that post-recombination matter-antimatter contact near regional boundaries leads to an observable (but unobserved) gamma-ray flux for domain sizes of less than a few thousand Mpc, thereby excluding such domains. In this paper we consider the pre-recombination signal from domains of larger size.']",['1997-09-16'] +1834,['eng'],"['Escobar, C O', 'Vázquez, R A']",['Are High Energy Cosmic Rays Magnetic Monopoles?'],['Astrophysics and Astronomy'],"['cosmic radiation, spectra', 'cosmic radiation, flux', 'magnetic monopole', 'astrophysics, galaxy', 'magnetic field', 'energy spectrum', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709148'],['We argue that magnetic monopoles can not be associated to the highest energy cosmic rays as recently suggested. Both the observed spectrum and the arrival direction disagree with observation.'],['1997-09-16'] +1835,['eng'],"['Frampton, Paul H', 'Keszthelyi, B', 'Ng, Y J']",['Longevity and Highest-Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['astrophysics, model', 'cosmic radiation, primary', 'p, cosmic radiation', 'cosmic radiation, energy', 'postulated particle, neutral particle', 'decay', 'lifetime', 'density', 'grand unified theory, SU(15)', 'model, composite', 'cosmic radiation, background', 'photon p, interaction', 'pi, photoproduction', 'p, path length', '> 10**10 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709080'],"['It is proposed that the highest energy $\\sim 10^{20}$eV cosmic ray primaries are protons, decay products of a long-lived progenitor which has propagated from typically $\\sim 100$Mpc. Such a scenario can occur in e.g. SU(15) grand unification and in some preon models, but is more generic; if true, these unusual cosmic rays provide a window into new physics.']",['1997-09-11'] +1836,['eng'],"['Balkanov, V A']",['The Baikal Deep Underwater Neutrino Experiment'],['Astrophysics and Astronomy'],"['talk, Dubna 1997/07/07', 'neutrino, particle identification', 'muon, flux', 'new particle, search for', 'neutralino, annihilation', 'magnetic monopole', 'Rubakov effect', 'p, semileptonic decay', 'neutrino, cosmic radiation', 'track data analysis', 'photoelectron, amplifier', 'background', 'Cherenkov counter, water', 'deep underground detector, Baikal', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709070'],"['We review the present status of the Baikal Deep Underwater Neutrino Experiment. The construction and performance of the large deep underwater Cherenkov detector for muons and neutrinos, NT-200 (Neutrino Telescope with 200 phototubes), which is currently under construction in Lake Baikal are described. Some results obtained with the intermediate detectors NT-36 (1993-95), NT-72 (1995-96) and NT-96 (1996-97) are presented, including the first clear neutrino candidates selected with 1994 and 1996 data.']",['1997-09-10'] +1837,['eng'],"['Kar, K', 'Sarkar, S', 'Goswami, S', 'Raychaudhuri, A K']",['Excited States of 71Ge above the Neutron Emission Threshold and Solar Neutrino Capture rates for Ga Detectors'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, energy', 'neutrino nucleus, capture', 'gallium, ground state', 'model, nuclear reaction', 'germanium, excited nucleus', 'n, emission', 'threshold', 'excited nucleus, radiative decay', 'width, ratio', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709078'],"['In Gallium detectors for solar neutrinos, the capture rate due to Gamow-Teller transitions to excited states of 71Ge beyond the neutron emission threshold is usually neglected. We make a model calculation to estimate its effect and find that this yields an additional contribution which may be as much as 0.4 SNU, even larger than that from the Isobaric Analog State in 71Ge reached by Fermi transitions, which is normally included in the standard predictions.']",['1997-09-10'] +1838,['eng'],"['Pierpaoli, E', 'Borgani, S', 'Masiero, A', 'Yamaguchi, M']",['The Formation of Cosmic Structures in a Light Gravitino Dominated Universe'],['Astrophysics and Astronomy'],"['supersymmetry, symmetry breaking', 'model, messenger', 'gravitino', 'LSP', 'astrophysics, missing-mass', 'astrophysics, fundamental constant', 'density, fluctuation', 'spectra, fluctuation', 'hydrogen, density', 'galaxy, cluster', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709047'],"['We analyse the formation of cosmic structures in models where the dark matter is dominated by light gravitinos with mass of $ 100$ eV -- 1 keV, as predicted by gauge-mediated supersymmetry (SUSY) breaking models. After evaluating the number of degrees of freedom at the gravitinos decoupling ($g_*$), we compute the transfer function for matter fluctuations and show that gravitinos behave like warm dark matter (WDM) with free-streaming scale comparable to the galaxy mass scale. We consider different low-density variants of the WDM model, both with and without cosmological constant, and compare the predictions on the abundances of neutral hydrogen within high-redshift damped Ly--$\\alpha$ systems and on the number density of local galaxy clusters with the corresponding observational constraints. We find that none of the models satisfies both constraints at the same time, unless a rather small $\\Omega_0$ value ($\\mincir 0.4$) and a rather large Hubble parameter ($\\magcir 0.9$) is assumed. Furthermore, in a model with warm + hot dark matter, with hot component provided by massive neutrinos, the strong suppression of fluctuation on scales of $\\sim 1\\hm$ precludes the formation of high-redshift objects, when the low--$z$ cluster abundance is required. We conclude that all different variants of a light gravitino DM dominated model show strong difficulties for what concerns cosmic structure formation. This gives a severe cosmological constraint on the gauge-mediated SUSY breaking scheme.']",['1997-09-08'] +1839,['eng'],"['Janka, H T', 'Keil, W']",['Perspectives of Core-Collapse Supernovae beyond SN 1987A'],['Astrophysics and Astronomy'],"['talk, Augst 1997/06/13', 'astrophysics, supernova', 'neutrino, emission', 'model, supernova', 'temperature', 'neutrino nucleon, interaction', 'charged current', 'energy, time dependence', 'model, hydrodynamical', 'entropy', 'velocity', 'neutrino, luminosity', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709012'],"['The observation of neutrinos from Supernova 1987A has confirmed the theoretical conjecture that these particles play a crucial role during the collapse of the core of a massive star. Only one per cent of the energy they carry away from the newly formed neutron star may account for all the kinetic and electromagnetic energy responsible for the spectacular display of the supernova explosion. However, the neutrinos emitted from the collapsed stellar core at the center of the explosion couple so weakly to the surrounding matter that convective processes behind the supernova shock and/or inside the nascent neutron star might be required to increase the efficiency of the energy transfer to the stellar mantle and envelope. The conditions for a successful explosion by the neutrino-heating mechanism and the possible importance of convection in and around the neutron star are shortly discussed. Neutrino-driven explosions turn out to be very sensitive to the parameters describing the neutrino emission of the proto-neutron star and to the details of the dynamical processes in the collapsed stellar core. Therefore uniform explosions with a well defined energy seem unlikely and type-II supernova explosions do not offer promising perspectives for being useful as standard candles.']",['1997-09-03'] +1840,['eng'],"['Hartmann, D H', 'Dixon, D D', 'Kolaczyk, E D', 'Samimi, J']",['Evidence for GeV emission from the Galactic Center Fountain'],['Astrophysics and Astronomy'],"['talk, Williamsburg 1997/04/27', 'astrophysics, galaxy', 'photon, cosmic radiation', 'photon, emission', 'supernova', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709029'],"['The region near the Galactic center may have experienced recurrent episodes of injection of energy in excess of $\\sim$ 10$^{55}$ ergs due to repeated starbursts involving more than $\\sim$ 10$^4$ supernovae. This hypothesis can be tested by measurements of $\\gamma$-ray lines produced by the decay of radioactive isotopes and positron annihilation, or by searches for pulsars produced during starbursts. Recent OSSE observations of 511 keV emission extending above the Galactic center led to the suggestion of a starburst driven fountain from the Galactic center. We present EGRET observations that might support this picture.']",['1997-09-04'] +1841,['eng'],"['Janka, H T']",['Explosion Mechanism of Core-Collapse Supernovae'],['Astrophysics and Astronomy'],"['talk, La Serena 1997/02/22', 'astrophysics, supernova', 'model, supernova', 'neutrino, emission', 'temperature', 'neutrino nucleon, interaction', 'model, hydrodynamical', 'energy, time dependence', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709013'],"['The observation of neutrinos from Supernova~1987A has confirmed the theoretical conjecture that these particles play a crucial role during the collapse of the core of a massive star. Only one per cent of the energy they carry away from the newly formed neutron star may account for all the kinetic and electromagnetic energy responsible for the spectacular display of the supernova explosion. However, the neutrinos emitted from the collapsed stellar core at the center of the explosion couple so weakly to the surrounding matter that convective processes behind the supernova shock and/or inside the nascent neutron star might be required to increase the efficiency of the energy transfer to the stellar mantle and envelope. The conditions for a successful explosion by the neutrino-heating mechanism and the possible importance of convection in and around the neutron star are shortly reviewed.']",['1997-09-03'] +1842,['eng'],"['Wang, L', 'Mukhanov, V F', 'Steinhardt, Paul Joseph']",['On the Problem of Predicting Inflationary Perturbations'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'time delay', 'space-time, horizon', 'cosmic radiation, anisotropy', 'potential, inflaton', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709032'],"['We examine the theoretical foundations of standard methods for computing density perturbations in inflationary models. We find that: (1) the time-delay formalism (introduced by Guth and Pi, 1982) is only valid when inflation is well-described by the de Sitter solution and the equation-of-state is nearly unchanging; and, (2) the horizon-crossing/Bessel approximation extends to non-exponential inflation, but only if the equation-of-state is changing slowly. Integration of the gauge-invariant perturbation equations mode-by-mode is the only method reliable for general models. For models with rapidly varying equation-of-state, the correction leads to significantly different predictions for the microwave background anisotropy. An important corollary is that methods proposed for ""reconstruction"" of the inflaton potential from anisotropy data are unreliable for general models.']",['1997-09-04'] +1843,['eng'],"['Stanev, T', 'Franceschini, A']",['Constraints on the Extragalactic Infrared Background from Gamma-Ray Observations of MKN 501'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'photon, cosmic radiation', 'cosmic radiation, background', 'energy, density', 'upper limit', 'photon, energy spectrum', 'photon, absorption', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708162'],"['We use the new results of the HEGRA detector on the TeV gamma-ray emission from Mrk 501 to set upper limits on the energy density of the infrared background (CIRB). The measured gamma-ray spectrum extends beyond 10 TeV and appears to be unattenuated in collisions with the low-energy CIRB photons. The upper limits on the CIBR intensity are thus quite strong and come close to the observational evaluations based on deep surveys of extragalactic sources in the near- and mid-IR. Any significant emissions from astrophysical sources other than galaxies may be virtually ruled out, unless the process of gamma-gamma interaction in the intergalactic space is more complex than expected and the average magnetic field extremely weak.']",['1997-08-19'] +1844,['eng'],"['Zlatev, I S', 'Huey, G', 'Steinhardt, Paul Joseph']",['Parametric Resonance in an Expanding Universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'model, resonance', 'particle, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9709006'],['Parametric resonance has been discussed as a mechanism for copious particle production following inflation. Here we present a simple and intuitive calculational method for estimating the efficiency of parametric amplification as a function of parameters. This is important for determining whether resonant amplification plays an important role in the reheating process. We find that significant amplification occurs only for a limited range of couplings and interactions.'],['1997-09-02'] +1845,['eng'],"['Durrer, R', 'Sakellariadou, M']",['Microwave Background Anisotropies from Scaling Seed Perturbations'],['Astrophysics and Astronomy'],"['astrophysics, model', 'cosmic radiation, background', 'microwaves', 'cosmic radiation, anisotropy', 'correlation function', 'astrophysics, missing-mass', 'perturbation', 'invariance, gauge', 'differential equations, solution', 'topology, defect', 'tensor, energy-momentum', 'parametrization', 'inflationary universe', 'photon, density', 'fluctuation, acoustic', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702028'],"[""We study microwave background anisotropies induced by scaling seed perturbations in a universe dominated by cold dark matter. Using a gauge invariant linear perturbation analysis, we solve the perturbation equations on super-horizon scales, for CMB anisotropies triggered by generic gravitational seeds. We find that perturbations induced by seeds -- under very mild restrictions -- are nearly isocurvature. Thus, compensation, which is mainly the consequence of physically sensible initial conditions, is very generic. We then restrict our study to the case of scaling sources, motivated by global scalar fields. We parameterize the energy momentum tensor of the source by ``seed functions'' and calculate the Sachs-Wolfe and acoustic contributions to the CMB anisotropies. We discuss the dependence of the anisotropy spectrum on the parameters of the model considered. Even within the restricted class of models investigated in this work, we find a surprising variety of results for the position and height of the first acoustic peak as well as for the overall amplitude. In particular, for certain choices of parameters, the spectrum resembles very much the well known adiabatic inflationary spectrum, whereas for others, the position of the first acoustic peak is significantly shifted towards smaller angular scales.""]",['1997-02-04'] +1846,['eng'],"['Viana, P T P', 'Liddle, A R']",['Perturbation evolution in cosmologies with a decaying cosmological constant'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'fundamental constant, decay', 'field theory, scalar', 'density, perturbation', 'Goldstone particle', 'potential', 'energy, adiabatic', 'inflationary universe', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708247'],"[""Structure formation models with a cosmological constant are successful in explaining large-scale structure data, but are threatened by the magnitude-redshift relation for Type Ia supernovae. This has led to discussion of models where the cosmological `constant' decays with time, which might anyway be better motivated in a particle physics context. The simplest such models are based on scalar fields, and general covariance demands that a time-evolving scalar field also supports spatial perturbations. We consider the effect of such perturbations on the growth of adiabatic energy density perturbations in a cold dark matter component. We study two types of model, one based on an exponential potential for the scalar field and the other on a pseudo-Nambu Goldstone boson. For each potential, we study two different scenarios, one where the scalar field presently behaves as a decaying cosmological constant and one where it behaves as dust. The initial scalar field perturbations are fixed by the adiabatic condition, as expected from the inflationary cosmology, though in fact we show that the choice of initial condition is of little importance. Calculations are carried out in both the zero-shear (conformal newtonian) and uniform-curvature gauges. We find that both potentials allow models which can provide a successful alternative to cosmological constant models.""]",['1997-08-28'] +1847,['eng'],"['Cabot, H', 'Meynadier, C', 'Sobczynska, D', 'Szabelska, B', 'Szabelski, J', 'Wibig, T']",['Measurable difference in Cherenkov light between $\\gamma$ and hadron induced EAS'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'hadron, cosmic radiation', 'showers, air', 'showers, electromagnetic', 'showers, hadronic', 'radiation, Cherenkov', 'time delay', 'spatial distribution', 'correlation', 'cosmic radiation, secondary radiation', 'muon, energy spectrum', 'numerical calculations, Monte Carlo', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708236'],"['We describe the possibly measurable difference in the Cherenkov light component of EAS induced by an electromagnetic particle (e+, e- or gamma) and induced by a hadron (i.e. proton or heavier nuclei) in TeV range. The method can be applied in experiments which use wavefront sampling method of EAS Cherenkov light detection (e.g. THEMISTOCLE, ASGAT).']",['1997-08-27'] +1848,['eng'],"['Li, L H', 'Cheng, Q L', 'Peng, Q H', 'Zhang, H Q']",['The Mikheyev-Smirnov-Wolfenstein Effect as a Probe of the Solar Interior'],['Astrophysics and Astronomy'],"['neutrino, oscillation', 'resonance, oscillation', 'energy, absorption', 'neutrino, solar', 'model, solar', 'plasma, absorption']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708192'],"['We relate the MSW effect to the efective absorption of the electronic collective motion energy by retaining the imaginary part of the index of refraction associated with the charged-current scattering and show that the small angle MSW solution to the solar neutrino anomaly can be used as a probe of the physical conditions of the solar interior if it is correct. We find that the constraint on the absorption imposed by the small angle MSW solution and the theoretical estimate of the absorption by the Boltzmann kinetic theory are consistent, which shows that a consistent theoretical picture can be developed when plasma absorption processes are taken into account.']",['1997-08-22'] +1849,['eng'],"['Ivanov, P']",['Non-linear metric perturbations and production of primordial black holes'],['Astrophysics and Astronomy'],"['inflationary universe', 'potential, inflaton', 'model, classical', 'space-time, perturbation', 'effect, nonlinear', 'black hole, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708224'],"['We consider the simple inflationary model with peculiarity in the form of ""plateau"" in the inflaton potential. We use the formalism of coarse-grained field to describe the production of metric perturbations $h$ of an arbitrary amplitude and obtain non-Gaussian probability function for such metric perturbations. We associate the spatial regions having large perturbations $h\\sim 1$ with the regions going to primordial black holes after inflation. We show that in our model the non-linear effects can lead to overproduction of the primordial black holes.']",['1997-08-26'] +1850,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Kachelriess, M', 'Vilenkin, A']",['Ultra-high energy cosmic rays without GZK cutoff'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'particle, heavy', 'particle, lifetime', 'particle, decay', 'fermion, neutral particle', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'photon, cosmic radiation', 'nucleon, cosmic radiation', 'astrophysics, galaxy', 'showers, air', 'numerical calculations, interpretation of experiments', 'cosmic radiation, energy', 'postulated particle, heavy', 'postulated particle, decay', 'postulated particle, lifetime', 'fermion, neutral particle', 'gauge field theory, SU(2) x U(1)', 'effective Lagrangian', 'symmetry, discrete', 'astrophysics, model', 'astrophysics, missing-mass', 'temperature', 'supersymmetry, symmetry breaking', 'inflaton', 'topology, defect', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'nucleon, cosmic radiation', 'cosmic radiation, flux', 'showers, air', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708217'],"['We study the decays of ultraheavy (m_X \\geq 10^{13}GeV) and quasistable (lifetime \\tau_X much larger than the age of the Universe t_0) particles as the source of Ultra High Energy Cosmic Rays (UHE CR). These particles are assumed to constitute a tiny fraction \\xi_X of CDM in the Universe, with \\xi_X being the same in the halo of our Galaxy and in the intergalactic space. The elementary-particle and cosmological scenarios for these particles are briefly outlined. The UHE CR fluxes produced at the decays of X- particles are calculated. The dominant contribution is given by fluxes of photons and nucleons from the halo of our Galaxy and thus they do not exibit the GZK cutoff. The extragalactic components of UHE CR are suppressed by the smaller extragalactic density of X-particles and hence the cascade limit is relaxed. We discuss the spectrum of produced Extensive Air Showers (EAS) and a signal from Virgo cluster as signatures of this model.']",['1997-08-26'] +1851,['eng'],"['Salamon, M H', 'Stecker, F W']",['Absorption of High Energy Gamma Rays by Interactions with Extragalactic Starlight Photons at High Redshifts'],['Astrophysics and Astronomy'],"['talk, Williamsburg 1997/04/27', 'photon, cosmic radiation', 'photon, absorption', 'photon photon, interaction', 'cosmic radiation, background', 'energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708182'],"['We extend earlier calculations of the attenuation suffered by gamma rays during their propagation from extragalactic sources, obtaining new extinction curves for gamma rays down to 10 GeV in energy, from sources up to a redshift of z=3.']",['1997-08-21'] +1852,['eng'],"['Dar, Arnon']","['Cometary Knots and Broad Emission Lines, Gamma Rays And Neutrinos From AGN']",['Astrophysics and Astronomy'],"['astrophysics, nebula', 'astrophysics, model', 'photon, cosmic radiation', 'astrophysics, quasar', 'black hole', 'cosmic radiation, acceleration', 'p p, interaction', 'neutrino, emission', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708160'],"['Recent observations with the Hubble Space Telescope have discovered in the nearest planetary nebula, the Helix Nebula, thousands of gigantic comet-like objects with planet like masses in a ring around the central brilliant star at a distance comparable to our own Oort cloud of comets. We propose that such circumstellar rings of planets exist around most stars and that the gas clouds which emit the broad optical lines from quasars are radiation ablated planets which have been stripped off by gravitational collisions from stars that orbit near the central massive black hole. We propose that collisions of jet accelerated particles with these targets crossing the line of sight produce TeV Hadronic production of TeV GRFs from blazars implies that they are accompanied by a simultaneous emission of high energy neutrinos, and of electrons and positrons with similar intensities, light curves and energy spectra. Cooling of these electrons and positrons by emission of synchrotron radiation and inverse Compton scattering produces $\\gamma$-ray, X-ray, optical and radio afterglows.']",['1997-08-19'] +1853,['eng'],"['Bezchastnov, V G', 'Haensel, P', 'Kaminker, A D', 'Yakovlev, D G']",['Neutrino synchrotron emission from dense magnetized electron gas of neutron stars'],['Astrophysics and Astronomy'],"['astrophysics', 'n, matter', 'electron, gas', 'relativistic', 'magnetic field', 'neutrino, synchrotron radiation', 'quantum mechanics', 'approximation, quasiclassical', 'energy loss', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708181'],"['We study the synchrotron emission of neutrino pairs by relativistic, degenerate electrons in strong magnetic fields. Particular attention is paid to the case in which the dominant contribution comes from one or several lowest cyclotron harmonics. Calculations are performed using the exact quantum formalism and the quasiclassical approach. Simple analytic fits to the neutrino synchrotron emissivity are obtained in the domain of magnetized, degenerate and relativistic electron gas provided the electrons populate either many Landau levels or the ground level alone. The significance of the neutrino synchrotron energy losses in the interiors of cooling neutron stars is discussed.']",['1997-08-21'] +1854,['eng'],"['Mollerach, S']",['Gravitational lensing on the Cosmic Microwave Background by gravity waves'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'gravitation, lens', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'space-time, Robertson-Walker', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708196'],"['We study the effect of a stochastic background of gravitational waves on the gravitational lensing of the Cosmic Microwave Background (CMB) radiation. It has been shown that matter density inhomogeneities produce a smoothing of the acoustic peaks in the angular power spectrum of the CMB anisotropies. A gravitational wave background gives rise to an additional smoothing of the spectrum. For the most simple case of a gravitational wave background arising during a period of inflation, the effect results to be three to four orders of magnitude smaller than its scalar counterpart, and is thus undetectable. It could play a more relevant role in models where a larger background of gravitational waves is produced.']",['1997-08-22'] +1855,['eng'],"['Gaisser, T K', 'Stanev, T']",['Pathlength distribution of atmospheric neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, path length', 'K, decay', 'pi, decay', 'muon, decay', 'neutrino, production', 'energy dependence', 'angular dependence', 'neutrino, oscillation', 'parametrization', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708146'],['We present the distribution of the production heights of atmsopheric neutrinos as a function of zenith angle and neutrino energy. The distributions can be used as the input for evaluation of neutrino propagation under various hypotheses for neutrino flavor oscillations.'],['1997-08-18'] +1856,['eng'],"['Balberg, S']",['Constraints on the Existence of Strange Quark Stars'],['Astrophysics and Astronomy'],"['quark', 'matter, strangeness', 'strong interaction, confinement', 'hyperon, production', 'n, matter', 'matter, density', 'baryon, energy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708134'],"['Creation of strange quark stars through strong interaction deconfinement is studied based on modern estimates of hyperon formation in neutron stars. The hyperon abundance is shown to be large enough so that if strange quark matter (SQM) is the true ground state of matter, the deconfinement density should be at most 2.5-3 times the nuclear saturation density. If so, deconfinement occurs in neutron stars at birth, and all neutron stars must be strange quark stars. Alternatively, sould observation indicate that some neutron stars have a baryonic interior, SQM is unlikely to be absolutely stable.']",['1997-08-15'] +1857,['eng'],"['Atrio-Barandela, F', 'Einasto, J', 'Gottlöber, S', 'Müller, V', 'Starobinsky, A A']",['A built-in scale in the initial spectrum of density perturbations'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'temperature, anisotropy', 'density, perturbation', 'spectra, perturbation', 'galaxy, cluster', 'inflationary universe', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708128'],"['We calculate temperature anisotropies of the cosmic microwave background (CMB) for several initial power spectra of density perturbations with a built-in scale suggested by recent optical data on the spatial distribution of rich clusters of galaxies. Using cosmological models with different values of spectral index, baryon fraction, Hubble constant and cosmological constant, we compare the calculated radiation power spectrum with the CMB temperature anisotropies measured by the Saskatoon experiment. We show that spectra with a sharp peak at 120 h^{-1} Mpc are in agreement with the Saskatoon data. The combined evidence from cluster and CMB data favours the presence of a peak and a subsequent break in the initial matter power spectrum. Such feature is similar to the prediction of an inflationary model where an inflaton field is evolving through a kink in the potential.']",['1997-08-14'] +1858,['eng'],"['Essex, C', 'Kennedy, Dallas C']",['Minimum Entropy Production of Neutrino Radiation in the Steady State'],['Astrophysics and Astronomy'],"['neutrino, radiation', 'photon, radiation', 'entropy, production', 'thermodynamics', 'statistics', 'potential, chemical', 'lepton number, conservation law']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708118'],"['A thermodynamical minimum principle valid for photon radiation is shown to hold for arbitrary geometries. It is successfully extended to neutrinos, in the zero mass and chemical potential case, following a parallel development of photon and neutrino statistics. This minimum principle stems more from that of Planck than that of classical Onsager-Prigogine irreversible thermodynamics. Its extension from bosons to fermions suggests that it may have a still wider validity.']",['1997-08-13'] +1859,['eng'],"['Anchordoqui, L A', 'Dova, M T', 'Epele, L N', 'Swain, J D']",['A depression before the bump in the highest energy cosmic ray spectrum'],['Astrophysics and Astronomy'],"['nucleus, cosmic radiation', 'cosmic radiation, energy spectrum', 'microwaves, background', 'energy loss', 'iron', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708082'],"[""We re-examine the interaction of ultra high energy nuclei with the microwave background radiation. We find that the giant dipole resonance leaves a new signature in the differential energy spectrum of iron sources located around 3 Mpc: A depression before the bump which is followed by the expected cutoff. This feature could be related to the apparent gap in the existing data and thus support ``bottom up'' models for the origin of the highest energy cosmic rays.""]",['1997-08-11'] +1860,['eng'],"['Schaab, C', 'Hermann, B', 'Weber, F', 'Weigel, M K']",['Are strange stars distinguishable from neutron stars by their cooling behaviour?'],['Astrophysics and Astronomy'],"['talk, Thera 1997/04/14', 'n, matter', 'matter, strangeness', 'quark, matter', 'neutrino, emission', 'temperature, surface', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708092'],"['The general statement that strange stars cool more rapidly than neutron stars is investigated in greater detail. It is found that the direct Urca process could be forbidden not only in neutron stars but also in strange stars. If so, strange stars would be slowly cooling and their surface temperatures would be more or less indistinguishable from those of slowly cooling neutron stars. The case of enhanced cooling is reinvestigated as well. It is found that strange stars cool significantly more rapidly than neutron stars within the first $\\sim 30$ years after birth. This feature could become particularly interesting if continued observation of SN 1987A would reveal the temperature of the possibly existing pulsar at its centre.']",['1997-08-12'] +1861,['eng'],"['Bharadwaj, S', 'Munshi, D', 'Souradeep, T']",['Skewness in the Cosmic Microwave Background Anisotropy from Inflationary Gravity Wave Background'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'inflationary universe', 'space-time, perturbation', 'photon, multiple scattering', 'temperature, fluctuation', 'gravitational radiation', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708015'],"[""In the context of inflationary scenarios, the observed large angle anisotropy of the Cosmic Microwave Background (CMB) temperature is believed to probe the primordial metric perturbations from inflation. Although the perturbations from inflation are expected to be gaussian random fields, there remains the possibility that nonlinear processes at later epochs induce ``secondary'' non-gaussian features in the corresponding CMB anisotropy maps. The non-gaussianity induced by nonlinear gravitational instability of scalar (density) perturbations has been investigated in existing literature. In this paper, we highlight another source of non-gaussianity arising out of higher order scattering of CMB photons off the metric perturbations. We provide a simple and elegant formalism for deriving the CMB temperature fluctuations arising due to the Sachs-Wolfe effect beyond the linear order. In particular, we derive the expression for the second order CMB temperature fluctuations. The multiple scattering effect pointed out in this paper leads to the possibility that tensor metric perturbation, i.e., gravity waves (GW) which do not exhibit gravitational instability can still contribute to the skewness in the CMB anisotropy maps. We find that in a flat $\\Omega =1$ universe, the skewness in CMB contributed by gravity waves via multiple scattering effect is comparable to that from the gravitational instability of scalar perturbations for equal contribution of the gravity waves and scalar perturbations to the total rms CMB anisotropy. The secondary skewness is found to be smaller than the cosmic variance leading to the conclusion that inflationary scenarios do predict that the observed CMB anisotropy should be statistically consistent with a gaussian random distribution.""]",['1997-08-05'] +1862,['eng'],"['Benesh, C J', 'Horowitz, C J']",['Neutrino Annihilation in Stellar Magnetic Fields'],['Astrophysics and Astronomy'],"['neutrino antineutrino, annihilation', 'electron, pair production', 'magnetic field, external field', 'cross section, annihilation', 'violation, CP', 'asymmetry', 'astrophysics, supernova', 'parity, violation', 'temperature, dependence', 'approximation, weak field', 'dependence, density', 'n, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708033'],"[""The potential enhancement of the cross section $\\nu\\bar\\nu\\to e^+e^-$ in the presence of a magnetic field is of critical interest for the study of supernovae and as a possible mechanism for gamma ray bursts. While parity violation(PV) in this reaction in free space is forbidden by CP, the presence of a CP non-invariant background gas of electrons creates an asymmetry in the cross section which may contribute to the asymmetry of a supernova and the natal velocities of neutron stars. We calculate the cross section in the presence of fields as high as $B = 10^{16}$G and find no significant enhancement of the cross section with magnetic field strength. By studying the systematics of our results as a function of environmental variables(field strength, density,temperature), we extrapolate the relative strength of the parity violating terms to the weak field limit, and find the parity violation is insufficient to provide the ``kick'' required to explain the observed velocities of neutron stars.""]",['1997-08-05'] +1863,['eng'],"['Pina-Avelino, P', 'Caldwell, R R', 'Martins, C J A P']",['Cosmic Strings in an Open Universe'],['Astrophysics and Astronomy'],"['astrophysics, string', 'space-time, open', 'space-time, Robertson-Walker', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'density, fluctuation', 'spectra, fluctuation', 'astrophysics, missing-mass', 'tensor, energy-momentum', 'astrophysics, fundamental constant', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708057'],"['The cosmic string scenario in an open universe is developed -- including the equations of motion, a model of network evolution, the large angular scale CMB temperature anisotropy, and the power spectrum of density fluctuations produced by cosmic strings with dark matter. First we derive the equations of motion for cosmic string in an open FRW space-time and construct a quantitative model of the evolution of the gross features of a cosmic string network. Second, we apply this model of network evolution to estimate the rms CMB temperature anisotropy induced by cosmic strings, obtaining the normalization for the mass per unit length $\\mu$ as a function of $\\Omega$. Third, we consider the effects of the network evolution and normalization in an open universe on the large scale structure formation scenarios with either cold or hot dark matter.']",['1997-08-07'] +1864,['eng'],"['Dar, Arnon']",['Cometary Knots and High Energy Photons And Neutrinos From Gamma Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'neutrino, cosmic radiation', 'cosmic radiation, flux', 'matter', 'p p, interaction', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708042'],"['The Hubble Space Telescope has recently discovered thousands of gigantic comet-like objects in a ring around the central star in the nearest planetary nebula. We suggest that such circumstellar rings exist around most stars. Collisions of the relativistic debris from gamma ray bursts in dense stellar regions with such gigantic comet-like objects, which have been stripped off from the circumstellar rings by gravitational perturbations, produce detectable fluxes of high energy $\\gamma$-rays and neutrinos.']",['1997-08-06'] +1865,['eng'],"['Dolgov, A D']",['The Problem of Vacuum Energy and Cosmology'],['Astrophysics and Astronomy'],"['talk, Paris 1997/06/04', 'vacuum state, energy', 'astrophysics, fundamental constant', 'field theory, vector', 'field theory, tensor', 'massless', 'field theory, scalar', 'back reaction']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708045'],"['Quantum field theory predicts that vacuum energy (or what is the same, cosmological constant) should be 50-100 orders of magnitude larger than the existing astronomical limit. A very brief review of possible solutions of this problem is presented. A mechanism of adjustment of vacuum energy down to (almost) zero by the back-reaction of massless vector or second rank tensor fields is discussed.']",['1997-08-06'] +1866,['eng'],"['Catanese, M', 'Bradbury, S M', 'Breslin, A C', 'Buckley, J H', 'Carter-Lewis, D A', 'Cawley, M F', 'Dermer, C D', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hillas, A M', 'Johnson, W N', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'Macomb, D J', 'McEnery, J E', 'Moriarty, P', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'Zweerink, J A']",['Multiwavelength Observations of a Flare from Markarian 501'],['Astrophysics and Astronomy'],"['review, experimental results', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707179'],"['We present multiwavelength observations of the BL Lacertae object Markarian 501 (Mrk 501) in 1997 between April 8 and April 19. Evidence of correlated variability is seen in very high energy (VHE, E > 350 GeV) gamma-ray observations taken with the Whipple Observatory gamma-ray telescope, data from the Oriented Scintillation Spectrometer Experiment of the Compton Gamma-Ray Observatory, and quicklook results from the All-Sky Monitor of the Rossi X-ray Timing Explorer while the Energetic Gamma-Ray Experiment Telescope did not detect Mrk 501. Short term optical correlations are not conclusive but the U-band flux observed with the 1.2m telescope of the Whipple Observatory was 10% higher than in March. The average energy output of Mrk 501 appears to peak in the 2 keV to 100 keV range suggesting an extension of the synchrotron emission to at least 100 keV, the highest observed in a blazar and ~100 times higher than that seen in the other TeV-emitting BL Lac object, Mrk 421. The VHE gamma-ray flux observed during this period is the highest ever detected from this object. The VHE gamma-ray energy output is somewhat lower than the 2-100 keV range but the variability amplitude is larger. The correlations seen here do not require relativistic beaming of the emission unless the VHE spectrum extends to >5 TeV.']",['1997-07-17'] +1867,['eng'],"['Hindmarsh, M B', 'Everett, A E']",['Magnetic Fields from Phase Transitions'],['Astrophysics and Astronomy'],"['astrophysics, model', 'critical phenomena', 'magnetic field, production', 'electroweak interaction', 'causality', 'energy, conservation law', 'radiation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708004'],"[""The generation of primordial magnetic fields from cosmological phase transitions is discussed, paying particular attention to the electroweak transition and to the various definitions of the `average' field that have been put forward. It is emphasised that only the volume average has dynamical significance as a seed for galactic dynamos. On rather general grounds of causality and energy conservation, it is shown that, in the absence of MHD effects that transfer power in the magnetic field from small to large scales, processes occurring at the electroweak transition cannot generate fields stronger than $10^{-20}$ Gauss on a scale of 0.5 Mpc. However, it is implausible that this upper bound could ever be reached, as it would require all the energy in the Universe to be turned into a magnetic field coherent at the horizon scale. Non-linear MHD effects seem therefore to be necessary if the electroweak transition is to create a primordial seed field.""]",['1997-09-08'] +1868,['eng'],"['Avignone, F T', 'Abriola, D', 'Brodzinski, R L', 'Collar, J I', 'Creswick, R J', 'Di Gregorio, D E', 'Farach, H A', 'Gattone, A O', 'Guérard, C K', 'Hasenbalg, F', 'Huck, H', 'Miley, H S', 'Morales, A', 'Morales, J', 'Nussinov, S', 'De Solorzano, A O', 'Reeves, J H', 'Villar, J A', 'Zioutas, Konstantin']",['Experimental Search for Solar Axions via Coherent Primakoff Conversion in a Germanium Spectrometer'],['Astrophysics and Astronomy'],"['search for, axion', 'axion, solar', 'scattering, axion nucleus', 'Primakoff effect', 'photon, production', 'semiconductor detector, germanium', 'coupling, (axion 2photon)', 'upper limit', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708008'],"['Results are reported of an experimental search for the unique, rapidly varying temporal pattern of solar axions coherently converting into photons via the Primakoff effect in a single crystal germanium detector. This conversion is predicted when axions are incident at a Bragg angle with a crystalline plane. The analysis of approximately 1.94 kg.yr of data from the 1 kg DEMOS detector in Sierra Grande, Argentina, yields a new laboratory bound on axion-photon coupling of $g_{a\\gamma \\gamma} < 2.7\\cdot 10^{-9}$ GeV$^{-1}$, independent of axion mass up to ~ 1 keV.']",['1997-08-05'] +1869,['eng'],"['Glendenning, N K']",['Strangeness in Compact Stars and Signal of Deconfinement'],['Astrophysics and Astronomy'],"['talk, Thera 1997/04/14', 'critical phenomena, confinement', 'hyperon, matter', 'n, matter', 'matter, hybrid', 'matter, strangeness', 'crystal', 'astrophysics, pulsar', 'spin', 'K, condensation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707351'],"['Phase transitions in compact stars are discussed including hyperonization, deconfinement and crystalline phases. Reasons why kaon condensation is unlikely is reviewed. Particular emphasis is placed on the evolution of internal structure with spin-down of pulsars. A signature of a first order phase transition in the timing structure of pulsars which is strong and easy to measure, is identified.']",['1997-08-01'] +1870,['eng'],"['Bahcall, J N', 'Kamionkowski, M P']","['The Proton-Proton Reaction, Solar Neutrinos, and a Relativistic Field Theoretic Model of the Deuteron']",['Astrophysics and Astronomy'],"['neutrino, solar', 'model, solar', 'p p, exclusive reaction', 'fusion', 'deuteron, model', 'field theory, relativistic', 'effective Lagrangian', 'four-fermion interaction', 'p p, scattering length', 'approximation, effective range', 'p p --> deuteron positron neutrino/e']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707320'],"['In a series of recent papers, Ivanov et al. and Oberhummer et al. have calculated the rate for the $p + p \\to d + e^+ + \\nu_e$ reaction with a zero-range four-fermion effective interaction and find a result 2.9 times higher than the standard value calculated from non-relativistic potential theory. Their procedure is shown to give a wrong answer because their assumed interaction disagrees with low-energy $pp$ scattering data.']",['1997-07-30'] +1871,['eng'],"['Garriga, J', 'Vilenkin, A']",['Recycling universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'vacuum state, bubble', 'bubble, production', 'geometry, bubble', 'model, stochastic', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707292'],"[""If the effective cosmological constant is non-zero, our observable universe may enter a stage of exponential expansion. In such case, regions of it may tunnel back to the false vacuum of an inflaton scalar field, and inflation with a high expansion rate may resume in those regions. An ``ideal'' eternal observer would then witness an infinite succession of cycles from false vacuum to true, and back. Within each cycle, the entire history of a hot universe would be replayed. If there were several minima of the inflaton potential, our ideal observer would visit each one of these minima with a frequency which depends on the shape of the potential. We generalize the formalism of stochastic inflation to analyze the global structure of the universe when this `recycling' process is taken into account.""]",['1997-07-29'] +1872,['eng'],"['Kranich, D', 'Deckers, T', 'Lorenz, E', 'Petry, D', 'Rauterberg, G']",['Recent Observations of gamma-rays above 1.5 TeV from Mkn 501 with the HEGRA $5 m^2$ Air Cherenkov Telescope'],['Astrophysics and Astronomy'],"['talk, Williamsburg 1997/04/27', 'photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'Cherenkov counter, air', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707293'],"[""Since February 1997 the BL Lac object Mkn 501 is in a ``high state'' of gamma-ray emission. The HEGRA collaboration has studied Mkn 501 with their air Cherenkov telescopes on La Palma. Here we report on observations with the 5 m^2 telescope (threshold approx. 1.5 TeV) operated in a stand alone mode. We observed a rapidly varying flux between 0.5 to 6 times of that from the Crab Nebula. On average an integral flux above 1.5 TeV of (2 + 1.3 - 0.5) x 10^-11 cm^-2 s^-1 has been determined. The spectrum extends at least up to 10 TeV with an integral power law coefficient of 1.8 +- 0.2 and seems to be steeper than in 1996.""]",['1997-07-29'] +1873,['eng'],"['Roukema, B F', 'Peterson, B A', 'Quinn, P J', 'Rocca-Volmerange, B']",['Merging History Trees of Dark Matter Haloes'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'astrophysics, missing-mass', 'many-body problem', 'spectra, perturbation', 'galaxy, production', 'luminosity', 'correlation function', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707294'],"[""A method of deriving and using merging history trees of dark matter galaxy haloes directly from pure gravity N-body simulations is presented. This combines the full non-linearity of N-body simulations with the flexibility of the semi-analytical approach. Merging history trees derived from power-law initial perturbation spectrum simulations (for indices $n=-2$ and $n=0$) by Warren et al. (1992) are shown. As an example of a galaxy formation model, these are combined with evolutionary stellar population synthesis, via simple scaling laws for star formation rates, showing that if most star formation occurs during merger-induced bursts, then a nearly flat faint-end slope of the galaxy luminosity function may be obtained in certain cases. Interesting properties of hierarchical halo formation are noted: (1) In a given model, merger rates may vary widely between individual haloes, and typically 20%-30% of a halo's mass may be due to infall of uncollapsed material. (2) Small mass haloes continue to form at recent times: as expected, the existence of young, low redshift, low metallicity galaxies (e.g., Izotov et al. 1997) is consistent with hierarchical galaxy formation models. (3) For $n=-2,$ the halo spatial correlation function can have a very high initial bias due to the high power on large scales.""]",['1997-07-29'] +1874,['eng'],"['Frass, A', 'Köhler, C', 'Hermann, G', 'Hess, M', 'Hofmann, W']",['Calibration of the Sensitivity of Imaging Atmospheric Cherenkov Telescopes using a Reference Light Source'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'showers, air', 'Cherenkov counter, air', 'imaging', 'photoelectron, amplifier', 'analog-to-digital converter']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707304'],"['The sensitivity of an Imaging Atmospheric Cherenkov telescope is calibrated by shining, from a distant pulsed monochromatic light source, a defined photon flux onto the mirror. The light pulse is captured and reconstructed by the telescope in an identical fashion as real Cherenkov light. The intensity of the calibration light pulse is monitored via a calibrated sensor at the telescope; in order to account for the lower sensitivity of this sensor compared to the Cherenkov telescope, an attenuator is inserted in the light source between the measurements with the calibrated sensor, and with the telescope. The resulting telescope sensitivities have errors of 10%, and compare well with other estimates of the sensitivity.']",['1997-07-29'] +1875,['eng'],"['Petry, D', 'Bradbury, S M', 'Konopelko, A K', 'Kranich, D', 'Raubenheimer, B C']",['AGN sudies above 1.5 TeV with the HEGRA $5 m^2$ Cherenkov Telescope (Sources observed'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'Cherenkov counter, air', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707291'],"[""The HEGRA 5 m^2 air Cherenkov telescope (CT1) was used to search for gamma-ray emission above 1.5 TeV from a series of low redshift AGN (Mkn 421, Mkn 501, MS 0116+319, PKS 2209+236, NGC 315 and W Comae). Here we present results from a total of 383 hours of ON-source observations at zenith angles up to 35$^\\circ$ made between February 1996 and April 1997 showing positive detections of Mkn 421 and Mkn 501 and upper limits on the other objects' emission. More recent results from observations of Mkn 421 und Mkn 501 will be added at the conference.""]",['1997-07-29'] +1876,['eng'],"['Matarrese, S', 'Mollerach, S', 'Bruni, M']",['Second-order perturbations of the Einstein-de Sitter Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'perturbation, relativistic', 'higher-order, 2', 'dependence, gauge', 'transformation, gauge', 'density, perturbation', 'gravitational radiation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707278'],"['We consider the evolution of relativistic perturbations in the Einstein-de Sitter cosmological model, including second-order effects. The perturbations are considered in two different settings: the widely used synchronous gauge and the Poisson (generalized longitudinal) one. Since, in general, perturbations are gauge dependent, we start by considering gauge transformations at second order. Next, we give the evolution of perturbations in the synchronous gauge, taking into account both scalar and tensor modes in the initial conditions. Using the second-order gauge transformation previously defined, we are then able to transform these perturbations to the Poisson gauge. The most important feature of second-order perturbation theory is mode-mixing, which here also means, for instance, that primordial density perturbations act as a source for gravitational waves, while primordial gravitational waves give rise to second-order density fluctuations. Possible applications of our formalism range from the study of the evolution of perturbations in the mildly non-linear regime to the analysis of secondary anisotropies of the Cosmic Microwave Background.']",['1997-07-28'] +1877,['eng'],"['Gaisser, T K']",['Neutrino astronomy'],['Astrophysics and Astronomy'],"['talk, Taormina 1997/02/22', 'neutrino, astrophysics', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'neutrino, flux', 'neutrino, air', 'quark, charm', 'energy spectrum, cosmic radiation', 'muon, neutrinoproduction', 'muon, flux', 'muon, energy loss', 'muon, angular distribution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707283'],"['This is a review of high energy neutrino astronomy that might be done with a kilometer-scale detector. The emphasis is on diffuse neutrinos of extragalactic origin and their relation to possible sources of the highest energy cosmic rays, such as active galaxies, cosmological gamma-ray burst sources and topological defects.']",['1997-07-28'] +1878,['eng'],"['Primack, Joel R']",['Dark Matter and Structure Formation in the Universe'],['Astrophysics and Astronomy'],"['lectures, Jerusalem 1996/12/30', 'astrophysics, missing-mass', 'space-time, Robertson-Walker', 'astrophysics, fundamental constant', 'matter, density', 'topology, defect', 'inflationary universe', 'fluctuation', 'astrophysics, model', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707285'],"['This chapter aims to present an introduction to current research on the nature of the cosmological dark matter and the origin of galaxies and large scale structure within the standard theoretical framework: gravitational collapse of fluctuations as the origin of structure in the expanding universe. General relativistic cosmology is summarized, and the data on the basic cosmological parameters ($t_o$ and $H_0 \\equiv 100 h \\kmsmpc$, $\\Omega_0$, candidates for hot, warm, and cold dark matter are briefly reviewed, together with current constraints and experiments that could detect or eliminate them. Also included is a very brief summary of the theory of cosmic defects, and a somewhat more extended exposition of the idea of cosmological inflation with a summary of some current models of inflation. The remainder is a discussion of observational constraints on cosmological model building, emphasizing models in which most of the dark matter is cold and the primordial fluctuations are the sort predicted by inflation. It is argued that the simplest models that have a hope of working are Cold Dark Matter with a cosmological constant ($\\Lambda$CDM) if the Hubble parameter is high ($h \\gsim 0.7$), and Cold + Hot Dark Matter (CHDM) if the Hubble parameter and age permit an $\\Omega=1$ cosmology, as seems plausible in light of the data from the Hipparcos astrometric satellite. The most attractive variants of these models and the critical tests for each are discussed.']",['1997-07-28'] +1879,['eng'],"['Ferreira, P G', 'Joyce, M']",['Structure formation with a self-tuning scalar field'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'field theory, scalar', 'potential', 'energy, density', 'light nucleus, production', 'inflationary universe', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707286'],"['A scalar field with an exponential potential has the particular property that it is attracted into a solution in which its energy scales as the dominant component (radiation or matter) of the Universe, contributing a fixed fraction of the total energy density. We study the growth of perturbations in a CDM dominated $\\Omega=1$ universe with this extra field, with an initial flat spectrum of adiabatic fluctuations. The observational constraints from structure formation are satisfied as well, or better, than in other models, with a contribution to the energy density from the scalar field $Ømega_\\phi prior to nucleosynthesis.']",['1997-07-28'] +1880,['eng'],"['Halzen, Francis']",['The AMANDA Neutrino Telescope'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, primary', 'neutrino, flux', 'photon, flux', 'neutrino, mass', 'astrophysics, missing-mass', 'supersymmetry', 'Cherenkov counter, water', 'solids, water', 'performance', 'optics, diffusion', 'deep underground detector, AMANDA']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707289'],"['We update the science prospects for the recently completed AMANDA South Pole neutrino detector. With an effective telescope area of order 10^4 m^2 and a threshold of ~50 GeV, it represents the first instrument of a new generation of high energy neutrino detectors, envisaged over 25 years ago. We describe the instrument and its performance, and map its expansion to a detector of kilometer dimension.']",['1997-07-28'] +1881,['eng'],"['Cen, R']",['A Critical Test of Topological Defect Models'],['Astrophysics and Astronomy'],"['astrophysics, model', 'topology, defect', 'correlation function, cluster', 'cluster, galaxy', 'correlation, length', 'astrophysics, texture', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707240'],"['Gaussian cosmological models, typified by the inflationary cold dark matter models, and non-Gaussian topological defect based cosmological models, such as the texture seeded model, differ in the origin of large-scale cosmic structures. In the former it is believed that peaks at appropriate scales in the initial high density field are the sites onto which matter accretes and collapses to form the present galaxies and clusters of galaxies, whereas in the latter these structures can form around the density perturbation seeds (which are textures in the texture model). Textures initially are randomly distributed on scales larger than their size, in sharp contrast to the initial high density peaks in the Gaussian models which are already strongly clustered before any gravitational evolution has occured. One thus expects that the resultant correlation of large cosmic objects such as clusters of galaxies in the texture model should be significantly weaker than its Gaussian counterpart. We show that an $\\Omega_0=1$ biased $b=2$ (as required by cluster abundance observations) texture model (or any random seed model) predicts a two-point correlation length of $\\le 6.0h^{-1}$Mpc for rich clusters, independent of richness. On the other hand, the observed correlation length for rich clusters is $\\ge 10.0h^{-1}$Mpc at an approximately $2\\sigma$ confidence level. It thus appears that the global texture cosmological model or any random seed cosmological models of this sort are ruled out at a very high confidence ($>3\\sigma$).']",['1997-07-23'] +1882,['eng'],"['Boyanovsky, D', 'Cormier, D', 'De Vega, H J', 'Holman, R', 'Kumar, S P']",['Self-Consistent Dynamics of Inflationary Phase Transitions'],['Astrophysics and Astronomy'],"['talk, Eger 1997/05/21', 'inflationary universe, fluctuation', 'critical phenomena', 'geometry', 'expansion 1/N, nonperturbative', 'gravitation, quasiclassical', 'back reaction', 'approximation, classical', 'field equations', 'renormalization', 'density, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707267'],"[""The physics of the inflationary universe requires the study of the out of equilibrium evolution of quantum fields in curved spacetime. We present the evolution for both the geometry and the matter (described by the quantum inflaton field) by means of the non-perturbative large N limit combined with semi-classical gravitational dynamics including the back-reaction of quantum fluctuations self-consistently for a new inflation scenario. We provide a criterion for the validity of the classical approximation and a full analysis of the case in which spinodal quantum fluctuations drive the evolution of the scale factor. Under carefully determined conditions, we show that the full field equations may be well approximated by those of a single composite field which obeys the classical equation of motion in all cases. The de Sitter stage is found to be followed by a matter dominated phase. We compute the spectrum of scalar density perturbations and argue that the spinodal instabilities are responsible for a `red' spectrum with more power at longer wavelengths. A criterion for the validity of these models is provided and contact with the reconstruction program is established.""]",['1997-07-25'] +1883,['eng'],"['Raffelt, G G']",['Astrophysical axion bounds'],['Astrophysics and Astronomy'],"['talk, Ringberg 1997/06/08', 'astrophysics, supernova', 'astrophysics, missing-mass', 'mass, axion', 'upper limit', 'phase space', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707268'],"['The observed properties of stars and especially the neutrino signal of the supernova 1987A provide an upper limit to the axion mass, while the age and expansion rate of the universe provide a lower limit. There remains a ""window of opportunity"" 10^{-5} eV < m_a < 10^{-2} eV, with large uncertainties on either side, where axions could still exist and where they would provide a significant fraction or all of the cosmic dark matter. The current status of this axion window is reviewed.']",['1997-07-25'] +1884,['eng'],"['Faraoni, V']",['Multiple imaging by gravitational waves'],['Astrophysics and Astronomy'],"['gravitational radiation', 'gravitation, lens', 'black hole', 'n, matter', 'astrophysics, pulsar', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707236'],"['Gravitational waves act like lenses for the light propagating through them. This phenomenon is described using the vector formalism employed for ordinary gravitational lenses, which was proved to be applicable also to a non-stationary spacetime, with the appropriate modifications. In order to have multiple imaging, an approximate condition analogous to that for ordinary gravitational lenses must be satisfied. Certain astrophysical sources of gravitational waves satisfy this condition, while the gravitational wave background, on average, does not. Multiple imaging by gravitational waves is, in principle, possible, but the probability of observing such a phenomenon is extremely low.']",['1997-07-22'] +1885,['eng'],"['Sumiyoshi, K', 'Yamada, S', 'Suzuki, H', 'Hillebrandt, W']",['The fate of a neutron star just below the minimum mass'],['Astrophysics and Astronomy'],"['n, matter', 'model, hydrodynamical', 'mass, stability', 'light nucleus, production', 'nucleus, semileptonic decay', 'nucleus, temperature', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707230'],"['First results of numerical simulations are presented which compute the dynamical evolution of a neutron star with a mass slightly below the minimum stable mass by means of a new implicit (general relativistic) hydrodynamic code. We show that such a star first undergoes a phase of quasi-static expansion, caused by slow nuclear $\\beta$-decays, lasting for about 20 seconds, but then explodes violently. The kinetic energy of the explosion is around $10^{49} erg$, the peak luminosity in electron anti-neutrinos is of order $10^{52} erg/s$, and the thermodynamic conditions of the expanding matter are favorable for r-process nucleosynthesis. These results are obtained for the Harrison-Wheeler equation of state and a simple and, possibly, unrealistic treatment of $\\beta$-decay rates and nuclear fission, which were adopted for comparison with previous works. However, we do not expect that the outcome will change qualitatively if more recent nuclear input physics used. Although our study does not rely on a specific scenario ofhow a neutron star starting from a bigger (and stable) masscan reach the dynamical phase, we assume that the final mass-loss event happens on a very short time scale, i.e., on a time scale shorter than a sound-crossing time, by removing a certain amount of mass as an initial perturbation. This assumption implies that the star has no time to adjust its nuclear composition to the new mass mass through a sequence of quasi-equilibria. In the latter case, however, there exists no stable configuration below the minimum mass, because the equation of state of fully catalyzed matter is too soft. Therefore, the dynamics of the explosion will not be too different from what have obtained if different initial perturbations are assumed.']",['1997-07-22'] +1886,['eng'],"['Sutaria, F K', 'Ray, A K']",['Neutrino Spectroscopy of the Early Phase of Nearby Supernovae'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino/e, emission', 'electron, capture', 'neutrino/e, spectra', 'deep underground detector', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707222'],"['Neutrinos emitted during stellar core collapse up to their trapping phase carry information about the stage from which the Supernova explosion process initiates. The dominant $\\nu_e$ emission mechanism is by electron capture on free protons and f-p shell nuclei and the spectrum of these neutrinos is a function of the ambient physical conditions within the core as well as the nuclear equation of state. The number of collapse phase $\\nu_e$ which can be detected by Super-Kamioka and Sudbury Neutrino Observatory from a Supernova within 1 kpc, and their generic energy spectra are given.']",['1997-07-22'] +1887,['eng'],"['Zimdahl, W']",['Cosmological perturbations in the inflationary Universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'perturbation, linear', 'energy, density', 'space-time, horizon', 'fluid, perturbation', 'space-time, Robertson-Walker', 'space-time, de Sitter']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707313'],"[""Previously defined covariant and gauge-invariant perturbation variables, representing, e.g., the fractional spatial energy density gradient on hypersurfaces of constant expansion, are used to simplify the linear perturbation analysis of a classical scalar field. With the help of conserved quantities on large scales we establish an exact first-order relation between comoving fluid energy density perturbations at `reentry' into the horizon and corresponding scalar field energy density perturbations at the first Hubble scale crossing during an early de Sitter phase of a standard inflationary scenario.""]",['1997-07-30'] +1888,['eng'],"['Calzetta, E A', 'Kandus, A', 'Mazzitelli, F D']",['Primordial Magnetic Fields Induced by Cosmological Particle Creation'],['Astrophysics and Astronomy'],"['astrophysics, model', 'charged particle, production', 'current, stochastic', 'magnetic field, induced', 'astrophysics, galaxy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707220'],['We study the primordial magnetic field generated by stochastic currents produced by charged particles created at the beginning of the radiation dominated epoch. We find that for a mass of the order m=10^2 GeV a field of sufficient intensity to seed the galactic dynamo is generated coherently over a galactic scale.'],['1997-07-25'] +1889,['eng'],"['Ray, A K', 'Sutaria, F K', 'Sheikh-Javid, A']",['Electron Capture in Early Gravitational Collapse'],['Astrophysics and Astronomy'],"['talk, La Serena 1997/02/22', 'astrophysics, supernova', 'gravitation', 'neutrino, emission', 'neutrino, yield', 'energy spectrum, neutrino', 'electron, capture', 'nuclear properties', 'temperature', 'mean field approximation, relativistic', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707218'],"['We present the spectra of pre trapping neutrinos emitted from a core collapse supernova (having main sequence masses 15 and 25 $M_{\\sun}$) within 1 kpc which can be detected by terrestrial detectors. The neutrino spectrum depends on the abundance of nuclei and free protons which undergo electron capture which in turn is determined by nuclear properties of the stellar core. The ambient temperature in the early pre-trapping phase is not so high as to wipe out shell and pairing effects. We present results from Relativistic Mean Field (RMF) calculations, which we use to predict properties of the neutron rich nuclei which dominate the stellar composition at this stage of stellar collapse and compare the RMF results with the Baron et al (BCK) equation of state.']",['1997-07-25'] +1890,['eng'],"['Tetradis, N']",['Fine Tuning of the Initial Conditions for Hybrid Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'model, hybrid', 'boundary condition', 'potential', 'field theory, scalar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707214'],['We study the evolution of regions of space with various initial field values for a simple theory that can support hybrid inflation. Only very narrow domains within the range of initial field values below the Planck scale lead to the onset of inflation. This implies a severe fine tuning for the initial configuration that will produce inflation.'],['1997-07-21'] +1891,['eng'],"['Bisnovatyi-Kogan, G S']",['High Velocity Neutron Stars as a Result of Asymmetric Neutrino Emission'],['Astrophysics and Astronomy'],"['talk, La Jolla 1995/03/15', 'n, matter', 'velocity, high', 'neutrino, emission', 'magnetic field, asymmetry', 'symmetry, mirror', 'neutrino, flux', 'flux, asymmetry', 'neutrino, energy loss', 'matter, acceleration']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707172'],['Formation of a neutron star is accompanied by neutrino emission carring about 10% of the rest energy of the star. Toroidal field produced by twisting of a dipole field in differentially rotating star is antisymmetric. Its summation with antisymmetric toroidal field results in braking of mirror symmetry of the magnetic field . For large magnetic field the neutron decay rate depends on its strength. Neutrino is emitted more in one direction leading to flux asymmetry and recoil of the neutron star. Estimations show that the neutron star can reach velocities $\\sim 1000$ km/s for 3% asymmetry of the neutrino flux.'],['1997-07-17'] +1892,['eng'],"['Lasenby, A N', 'Doran, C J L', 'Dabrowski, Y', 'Challinor, A D']",['Rotating Astrophysical Systems and a Gauge Theory Approach to Gravity'],['Astrophysics and Astronomy'],"['talk, Gran Sasso 1997/09/07', 'astrophysics, matter', 'matter, rotator', 'gravitation, gauge field theory', 'space-time, Minkowski', 'iron, spectra', 'black hole, singularity', 'black hole, Kerr', 'astrophysics, string', 'tensor, energy-momentum', 'model, fluid', 'algebra, geometrical', 'space-time, algebra', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707165'],"['We discuss three applications of a gauge theory of gravity to rotating astrophysical systems. The theory employs gauge fields in a flat Minkowski background spacetime to describe gravitational interactions. The iron fluorescence line observed in AGN is discussed, assuming that the line originates from matter in an accretion disk around a Kerr (rotating) black hole. Gauge-theory gravity, expressed in the language of Geometric Algebra, allows very efficient numerical calculation of photon paths. From these paths we are able to infer the line shape of the iron line. Comparison with observational data allows us to constrain the black hole parameters, and, for the first time, infer an emissivity profile for the accretion disk. The topological constraints imposed by gauge-theory gravity are exploited to investigate the nature of the Kerr singularity. This reveals a simple physical picture of a ring of matter moving at the speed of light which surrounds a sheet of pure isotropic tension. Implications for the end-points of collapse processes are discussed. Finally we consider rigidly-rotating cosmic strings. It is shown that a solution in the literature has an unphysical stress-energy tensor on the axis. Well defined solutions are presented for an ideal two-dimensional fluid. The exterior vacuum solution admits closed timelike curves and exerts a confining force.']",['1997-07-17'] +1893,['eng'],"['Bharadwaj, S', 'Sethi, S K']",['Decaying Neutrinos and Large Scale Structure Formation'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'density, perturbation', 'matter, spectra', 'cosmic radiation, background', 'neutrino, decay', 'neutrino, lifetime', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707143'],['We study the growth of density perturbations in a universe with unstable dark matter particles. The mass (m_\\nu) range 30 eV < m_\\nu < 10 keV with lifetimes ($t_d$) in the range 10^7 sec < t_d < 10^16 sec are considered. We calculate the COBE normalized matter power spectrum for these models. We find that it is possible to construct models consistent with observations for masses $m_\\nu > 50 eV by adjusting t_d so as to keep the quantity (m_\\nu(keV))^2 t_d(yr) constant at a value around 100. For m_\\nu < 1 keV the power spectrum has extra power at small scales which could result in an early epoch of galaxy formation. We do not find any value of t_d which gives a viable model in the mass range m_\\nu < 50 eV. We also consider the implications of radiatively decaying neutrinos---models in which a small fraction B << 1 of neutrinos decay into photons-which could possibly ionize the intergalactic medium (IGM) at high redshift. We show that the parameter space of decaying particles which satisfies the IGM observations does not give viable models of structure formation.'],['1997-07-15'] +1894,['eng'],"['Amram, P', 'Arpesella, C', 'Aslanides, Elie', 'Aubert, Jean-Jacques', 'Azoulay, R', 'Bailey, D', 'Basa, S', 'Berthier, R', 'Bertin, V', 'Billault, M', 'Biller, S D', 'Blanc, F', 'Blanc, P E', 'Blondeau, F', 'Boulesteix, J', 'Brooks, B', 'Calzas, A', 'Cârloganu, C', 'Carr, J', 'Carton, P H', 'Cases, R', 'Cribier, M', 'De Botton, N R', 'Desages, F E', 'Destelle, J J', 'Dispau, G', 'Drogou, J F', 'Feinstein, F', 'Festy, D', 'Fuda, J L', 'Galumian, P I', 'Goret, P', 'Gosset, L G', 'Gournay, J F', 'Hernández, J J', 'Herrouin, G', 'Hubaut, F', 'Jelley, N A', 'Kajfasz, E', 'Lachartre, D', 'Lamare, P', 'Languillat, J C', 'Laubier, L', 'Laugier, J P', 'Le Gac, R', 'Le Provost, H', 'Le Van Suu, A', 'Lemoine, L', 'Loiseau, D', 'Loucatos, S', 'Magnier, P', 'Marcelin, M', 'Martin, L', 'Mazéas, F', 'Mazure, A', 'McNutt, J R', 'Meessen, C', 'Millot, C', 'Mols, P', 'Montanet, F', 'Moorhead, M E', 'Moscoso, L', 'Navas, S', 'Olivetto, C', 'Payre, P', 'Perrin, P', 'Poinsignon, J', 'Potheau, R', 'Raymond, M', 'Sacquin, Yu', 'Schuller, J P', 'Soirat, J P', 'Tabary, A', 'Talby, M', 'Triay, R', 'Valdy, P', 'Velasco, J', 'Vigeolas, E', 'Vignaud, D', 'Vilanova, D', 'Wark, D', 'Zúñiga, J']",['ANTARES proposal'],['Astrophysics and Astronomy'],"['proposal', 'neutrino, cosmic radiation', 'deep underground detector, water', 'Cherenkov counter, water', 'photoelectron', 'data management', 'data acquisition', 'trigger', 'control system', 'numerical calculations', 'bibliography']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=ext&id=cppm-97-02', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707136']","['The ANTARES collaboration propose to observe high energy cosmic neutrinos using a deep sea Cherenkov detector. The sky survey with high energy neutrinos is complementary to the observations with photons and will shed a new light on the understanding of the origin of cosmics rays. We propose to explore the possibility of a km-scale detector to be installed in a deep site in the Mediterranean sea, for which a broad collaboration will be needed. With the help of collaborators and partners which have experience in sea science engineering (COM, CSTN, CTME, IFREMER, France Télécom Câbles, INSU-CNRS...) we will test the sea engineering part of a detector including test deployments close to the Toulon coast (France) where technical support is available and where several sites at depths down to 2500~m are easily accessible. We propose to build and install a demonstrator (a fully equipped 3-dimensional test array) the design of which can be extended to a km-scale detector. During the same time, autonomous systems allowing to measure undersea optical parameters in view of the selection of a site for the future km-scale detector will be realized.']",['1997-07-03'] +1895,['eng'],"['Bisnovatyi-Kogan, G S']",['Asymmetric neutrino emision and formation of rapidly moving pulsars'],['Astrophysics and Astronomy'],"['n, matter', 'symmetry, mirror', 'magnetic field, asymmetry', 'weak interaction, cross section', 'neutrino, flux', 'pulsar, production', 'recoil', 'black hole', 'neutrino, energy loss', 'matter, acceleration', 'astrophysics, supernova', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707120'],['The neutron star formation during the collapse with the strong magnetic field may lead to a mirror symmetry violation and formation of an asymmetric magnetic field. Dependence of the week interaction cross-section on the magnetic field strength lead to the asymmetric neutrino flux and formation of rapidly mooving pulsars due to the recoil action as well as rapidly moving black holes.'],['1997-07-14'] +1896,['eng'],"['MacGibbon, J H', 'Brandenberger, R H', 'Wichoski, U F']",['Limits on Black Hole Formation from Cosmic String Loops'],['Astrophysics and Astronomy'],"['astrophysics, string', 'black hole, production', 'radiation, Hawking', 'photon, cosmic radiation', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707146'],"['In theories with cosmic strings, a small fraction of string loops may collapse to form black holes. In this Letter, various constraints on such models involving black holes are considered. Hawking radiation from black holes, gamma and cosmic ray flux limits and constraints from the possible formation of stable black hole remnants are reanalyzed. The constraints which emerge from these considerations are remarkably close to those derived from the normalization of the cosmic string model to the cosmic microwave background anisotropies.']",['1997-07-15'] +1897,['eng'],"[""Degl'Innocenti, S"", 'Fiorentini, G', 'Ricci, B']",['Helioseismology and $p+p \\to d + e^{+} + \\nu_e$ in the sun'],['Astrophysics and Astronomy'],"['model, scalar', 'p p, interaction', 'neutrino/e, hadroproduction', 'neutrino/e, solar', 'numerical calculations, interpretation of experiments', 'p p --> deuterium positron neutrino/e']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707133'],"['By using a phenomenological field theory of nucleon-nucleon interactions, Oberhummer et al. found a cross section of p+p $\\to$ d + e$^+$ + $\\nu _e$ about 2.9 times that given by the potential approach and adopted in Standard Solar Model calculations. We show that a solar model with $S=2.9 S_{SSM}$ is inconsistent with helioseismic data, the difference between model predictions and helioseismic determinations being typically a factor ten larger than estimated uncertainties. We also show that, according to helioseismology,']",['1997-07-17'] +1898,['eng'],"['Celotti, A', 'Fabian, A C', 'Rees, M J']",['Limits from rapid TeV variability of Mrk 421'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'galaxy, AGN', 'plasma', 'cosmic radiation, background', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707131'],"['The extreme variability event in the TeV emission of Mrk 421, recently reported by the Whipple team, imposes the tightest limits on the typical size of the TeV emitting regions in Active Galactic Nuclei (AGN). We examine the consequences that this imposes on the bulk Lorentz factor of the emitting plasma and on the radiation fields present in the central region of this Active Nucleus. No strong evidence is found for extreme Lorentz factors. However, energetics arguments suggest that any accretion in Mrk 421 has to take place at small rates, compatible with an advection-dominated regime.']",['1997-07-17'] +1899,['eng'],"['Albrecht, Andreas', 'Battye, R A', 'Robinson, J']",['The case against scaling defect models of cosmic structure formation'],['Astrophysics and Astronomy'],"['astrophysics, texture', 'topology, defect', 'matter', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'scaling, defect', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707129'],"['We calculate predictions from defect models of structure formation for both the matter and Cosmic Microwave Background (CMB) over all observable scales. Our results point to a serious problem reconciling the observed large-scale galaxy distribution with the COBE normalization, a result which is robust for a wide range of defect parameters. We conclude that standard scaling defect models are in conflict with the data, and show how attempts to resolve the problem by considering non-scaling defects would require radical departures from the standard scaling picture.']",['1997-07-17'] +1900,['eng'],"['Harris, M', 'Wang, J', 'Teplitz, V L']",['Astrophysical Effects of $\\nu \\gamma \\to \\nu \\gamma \\gamma$ and Its Crossed Processes'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'scattering, neutrino photon', 'neutrino, cosmic radiation', 'photon, cosmic radiation', 'channel cross section', 'path length', 'numerical calculations', 'neutrino photon --> 2photon neutrino']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707113'],"['Recently, Dicus and Repko computed nu gamma --> nu gamma gamma for energies below the threshold for e^{+}e^{-} pair production. They found across section on the order of 10^{-52} omega ^{gamma} with gamma =10, where omega is the CMS energy of one of the initial particles in MeV. Cross sections for the crossed processes are the same to factors of order one. This note investigates the extent to which these processes could, if their result extrapolates past 1 MeV: affect supernova dynamics; cut off the energy distribution of very high energy cosmic photons and neutrinos; and possibly give rise to an observable gamma signal from scattering of neutrinos from one supernova by those of a second supernova close in space and time. We also estimate, from Supernova 1987A, that, in the region above a few MeV, gamma must fall below 8.4.']",['1997-07-10'] +1901,['eng'],"['Roberts, M D', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Hayami, Y', 'Kamei, S', 'Kifune, T', 'Kita, R', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Suzuki, A', 'Suzuki, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['TeV $\\gamma$-ray Observations of Southern AGN with the CANGAROO 3.8 m Telescope'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, pulsar', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707014'],"['Since 1992 the CANGAROO 3.8m imaging telescope has been used to search for sources of TeV gamma-rays. Results are presented here for observations of four Southern Hemisphere BL-Lacs - PKS0521-365, PKS2316-423, PKS2005-489 and EXO0423-084. In addition to testing for steady DC emission, a night by night burst excess search has been performed for each source.']",['1997-07-03'] +1902,['eng'],"['Yoshikoshi, T', 'Kifune, T', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Hayami, Y', 'Kamei, S', 'Kita, R', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Suzuki, A', 'Suzuki, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T']",['Very High Energy $\\gamma$ Rays from the Vela Pulsar/Nebula'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, pulsar', 'cosmic radiation, energy', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707013'],"['We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Cherenkov telescope near Woomera, South Australia every year since 1992. This is the first concerted search for pulsed and unpulsed emission from the Vela region, and the imaging technique also allows the location of the emission within the field of view to be examined. A significant excess of gamma-ray-like events is found offset from the Vela pulsar to the southeast by about 0.13deg. The excess shows the behavior expected of gamma-ray images when the asymmetry cut is applied to the data. There is no evidence for the emission being modulated with the pulsar period -- in contrast to earlier claims of signals from the Vela pulsar direction.']",['1997-07-03'] +1903,['eng'],"['Sako, T', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Hayami, Y', 'Kamei, S', 'Kifune, T', 'Kita, R', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Matsuoka, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sakurazawa, K', 'Susukita, R', 'Suzuki, A', 'Suzuki, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']","['Observations of Pulsars, PSR 1509-58 and PSR 1259-63, by CANGAROO 3.8 m Telescope']",['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'astrophysics, pulsar', 'cosmic radiation, energy', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707012'],"['The data for VHE (~TeV) gamma rays from young gamma-ray pulsar PSR1509-58 observed in 1996 with the CANGAROO 3.8m Cerenkov imaging telescope are presented, as well as the additional data from March to June of 1997. The high spin-down luminosity of the pulsar and the plerionic feature around the pulsar observed with radio and X-rays suggest that VHE gamma-ray emission is quite likely above the sensitivity of the CANGAROO telescope. The CANGAROO results on other pulsars, such as PSR1259-63, are also presented. PSR1259-63 is a highly eccentric X-ray binary system, which includes a high mass Be companion star, and a preliminary analysis on the data taken 4 months after the periastron in 1994 suggests emission of VHE gamma rays.']",['1997-07-03'] +1904,['eng'],"['Sakurazawa, K', 'Tanimori, T', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Kamei, S', 'Kifune, T', 'Kita, R', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Matsuoka, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Susukita, R', 'Suzuki, A', 'Suzuki, R', 'Tamura, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['Observation of Spectrum of TeV $\\gamma$ Rays up to 60 TeV from the Crab at the Large Zenith Angles'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, particle source', 'cosmic radiation, energy spectrum', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707002'],"['The CANGAROO experiment has observed gamma-ray above 7TeV from the Crab pulsar/nebula at large zenith angle in Woomera, South Australia. We report the CANGAROO data taken in 1992, 1993 and 1995, from which it appears that the energy spectrum extends at least up to 50 TeV. The observed integral spectrum is (8.4+-1.0) x 10^{-13}(E/7 TeV)^(-1.53+-0.15)cm^{-2}s^{-1} between 7 TeV and 50 TeV. In November 1996, the 3.8m mirror was recoated in Australia, and its reflectivity was improved to be about 90% as twice as before. Due to this recoating, the threshold energy of ~4 TeV for gamma rays has been attained in the observation of the Crab at large zenith angle. Here we also report the preliminary result taken in 1996.']",['1997-07-02'] +1905,['eng'],"['Fiorentini, G', 'Moretti, M', 'Villante, F L']",['Superkamiokande and solar antineutrinos'],['Astrophysics and Astronomy'],"['antineutrino p, exclusive reaction', 'charged current', 'positron, angular distribution', 'antineutrino/e, flux', 'upper limit', 'neutrino, solar', 'neutrino antineutrino, oscillation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707097'],"['We propose to exploit the angular distribution of the positrons emitted in the inverse beta decay to extract a possible antineutrino signal from the Superkamiokande background. From the statistics collected in just 101.9 days one obtains a model independent upper bound on the antineutrino flux (for energy greater than 8.3 MeV) Phi < 9*10^4 cm^-2 s^-1 at the 95% C.L. By assuming the same energy spectrum as for the 8B neutrinos, the 95% C.L. bound is Phi < 6*10^4 cm^-2 s^-1. Within three years of data taking, the sensitivity to neutrino-antineutrino transition probability will reach the 1% level, thus providing a stringent test of hybrid oscillation models.']",['1997-07-09'] +1906,['eng'],"['Fukasaku, K', 'Fujita, T']",['Reexamination of standard solar model to the solar neutrino problems'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'model, solar', 'p nucleus, nuclear reaction', 'beryllium', 'channel cross section', 'deep underground detector', 'numerical calculations, interpretation of experiments', 'p beryllium --> boron photon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707092'],"['We examine the calculation of the solar neutrino flux based on the standard solar model (SSM). It is found that the solar neutrino data (KAMIOKANDE experiment) can be well described by the SSM with careful employment of nuclear data of $^7Be (p,\\gamma) ^{8} B$. The main point is that the simple-minded product ansatz of Coulomb plus nuclear parts should have a few percent uncertainties which induce the large reduction of the neutrino flux from $^8 B$. Also, if the electron capture of $^7 Be$ inside the sun is suppressed, then the GALLEX experiment can be understood by the SSM calculation.']",['1997-07-09'] +1907,['eng'],"['Cohen, Andrew G', 'De Rújula, Alvaro', 'Glashow, Sheldon Lee']",['A Matter-Antimatter Universe?'],['Astrophysics and Astronomy'],"['astrophysics, model', 'matter, antimatter', 'particle antiparticle, annihilation', 'photon, cosmic radiation', 'photon, spectra', 'photon, flux', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707087'],"['We ask whether the universe can be a patchwork consisting of distinct regions of matter and antimatter. We demonstrate that, after recombination, it is impossible to avoid annihilation near regional boundaries. We study the dynamics of this process to estimate two of its signatures: a contribution to the cosmic diffuse gamma-ray background and a distortion of the cosmic microwave background. The former signal exceeds observational limits unless the matter domain we inhabit is virtually the entire visible universe. On general grounds, we conclude that a matter-antimatter symmetric universe is empirically excluded.']",['1997-07-08'] +1908,['eng'],"['Medina-Tanco, G A']",['Large scale distribution of matter in the nearby universe and ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'p, cosmic radiation', 'magnetic field, galaxy', 'matter, density', 'cosmic radiation, particle source', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707054'],"['The deflection of extragalactic ultra-high energy protons (E > 4E19 eV) travelling to our galaxy is studied assuming that visible matter traces both, the sources of the particles and the intergalactic magnetic field. The reversal scale and the magnitude of the magnetic field are determined by the local density of matter. The CfA Redshift Catalog is used to determine the distribution of galaxies inside 50 Mpc, where the sources are believed to reside. It is demonstrated that the arrival directions of ultra high energy cosmic rays are consistent with the distribution of galaxies inside 50 Mpc and that the proposed clusters of events point to regions of high density of sources instead of individual ones.']",['1997-07-07'] +1909,['eng'],"['Cassidy, M J', 'Fortson, Lucy F', 'Fowler, J W', 'Ong, R A', 'Jui, C', 'Kieda, D B', 'Loh, E C', 'Sommers, P']",['CASA-BLANCA'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'cosmic radiation', 'showers, air', 'Cherenkov counter', 'photoelectron, amplifier']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707038'],"['The lateral distribution of Cherenkov light at ground level records important information on the development of the cosmic ray air shower which produces it. We have constructed an array of 144 non-imaging Cherenkov detectors at the CASA-MIA experiment site in Dugway, Utah. The various arrays can sample simultaneously the lateral distributions of electrons, muons, and Cherenkov light at many locations. We describe the design and operation of the CASA-BLANCA experiment and its potential to address the composition of primary cosmic rays between 300 and 30,000 TeV.']",['1997-07-03'] +1910,['eng'],"['Chung, D J H', 'Farrar, Glennys R S', 'Kolb, E W']",['Are ultrahigh energy cosmic rays a signal for supersymmetry?'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'supersymmetry, search for', 'sparticle, bound state', 'postulated particle, gluino', 'baryon, sparticle', 'sparticle, production', 'cosmic radiation, acceleration', 'p, energy loss', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707036'],"['We investigate the suggestion that cosmic ray particles of energy larger than the Greisen-Zatsepin-Kuzmin cutoff are not nucleons, but stable, massive, supersymmetric hadrons, $S^0$s, which are $uds$-gluino bound states. Because the propagation range of $S^0$s through the cosmic background radiation is significantly longer than the range of nucleons, $S^0$s can originate from sources at cosmological distances.']",['1997-07-03'] +1911,['eng'],"['Bordes, J', 'Chan, H M', 'Faridani, J', 'Pfaudler, J', 'Tsou, S T']",['Possible Test for the Suggestion that Air Showers with $E > 10^{20}$ eV are due to Strongly Interacting Neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'showers, air', 'neutral current, flavor changing', 'neutrino, strong interaction', 'gluon, exchange', 'duality, color', 'cosmic radiation, spatial distribution', 'numerical calculations, interpretation of experiments', '> 10**11 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707031'],"[""The suggestion is made that air showers with energies beyond the Greisen-Zatsepin-Kuz'min spectral cut-off may have primary vertices some 6 km lower in height than those of proton initiated showers with energies below the GZK cut-off. This estimate is based on the assumption that post-GZK showers are due to neutrinos having acquired strong interactions from generation-changing dual gluon exchange as recently proposed.""]",['1997-07-03'] +1912,['eng'],"['Medina-Tanco, G A', 'De Gouveia dal Pino, E M']",['Galactic Diffuse $\\gamma$-ray Emission at TeV Energies and the Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Williamsburg 1997/04/27', 'cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'photon nucleus, interaction', 'cosmic radiation, background', 'p, cosmic radiation', 'photon, showers', 'showers, electromagnetic', 'showers, spatial distribution', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707023'],"['Using the cosmic ray (CR) data available in the energy interval $(10 - 2 nuclei of the ISM. Normalized to the EGRET measurements, this allows an estimate of the galactic diffuse $\\gamma$-ray background due to intermediate and high energy CR at TeV energies. On the other hand, over the last few years, several particles with energies above $10^{20}$ eV (beyond the Greisen-Zatsepin-Kuzmin cut-off) have been detected. These particles are very likely extragalactic protons originated at distances not greater than $30 - 50$ Mpc [e.g., 1]. The propagation of these ultra-high energy protons (UHEP) through the intergalactic medium leads to the development of $\\gamma$-ray cascades and an ultimate signature at TeV energies. To assess the statistical significance of this $\\gamma$-ray signature by the UHEP, we have also simulated the development of electromagnetic cascades triggered by the decay of a $10^{19}$ eV $\\pi^{o}$ in the intergalactic medium after an UHEP collision with a cosmic microwave background photon.']",['1997-07-03'] +1913,['eng'],"['Medina-Tanco, G A', 'De Gouveia dal Pino, E M', 'Horváth, J E']",['Deflection of ultra high energy cosmic rays by the galactic magnetic field'],['Astrophysics and Astronomy'],"['cosmic radiation, hadronic component', 'p, cosmic radiation', 'iron, cosmic radiation', 'cosmic radiation, particle source', 'magnetic field, galaxy', 'cosmic radiation, spatial distribution', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707041'],"[""We report the results of 3D simulations of the trajectories of ultra-high energy protons and Fe nuclei (with energies $E = 4 \\times 10^{19}$ and $2.5 sources to the detector. A uniform distribution of anti-particles is backtracked from the detector, at the Earth, to the halo of the Galaxy. We assume an axisymmetric, large scale spiral magnetic field permeating both the disc and the halo. A normal field component to the galactic plane ($B_z$) is also included in part of the simulations. We find that the presence of a large scale galactic magnetic field does not generally affect the arrival directions of the protons, although the inclusion of a $B_z$ component may cause significant deflection of the lower energy protons ($E = 4 \\times 10^{19} $ eV). Error boxes larger than or equal to $\\sim 5^{\\circ}$ are most expected in this case. On the other hand, in the case of heavy nuclei, the arrival direction of the particles is strongly dependent on the coordinates of the particle source. The deflection may be high enough ($> 20^{\\circ}$) as to make extremely difficult any identification of the sources unless the real magnetic field configuration is accurately determined. Moreover, not every incoming particle direction is allowed between a given source and the detector. This generates sky patches which are virtually unobservable from the Earth. In the particular case of the UHE events of Yakutsk, Fly's Eye, and Akeno, they come from locations for which the deflection caused by the assumed magnetic field is not significant.""]",['1997-07-04'] +1914,['eng'],"['Kifune, T', 'Dazeley, S A', 'Edwards, P G', 'Hara, T', 'Hayami, Y', 'Kamei, S', 'Kita, R', 'Konishi, T', 'Masaike, A', 'Matsubara, Y', 'Matsuoka, Y', 'Mizumoto, Y', 'Mori, M', 'Muraishi, H', 'Muraki, Y', 'Naito, T', 'Nishijima, K', 'Ogio, S', 'Patterson, J R', 'Roberts, M D', 'Rowell, G P', 'Sako, T', 'Sakurazawa, K', 'Susukita, R', 'Suzuki, A', 'Suzuki, R', 'Tamura, T', 'Tanimori, T', 'Thornton, G J', 'Yanagita, S', 'Yoshida, T', 'Yoshikoshi, T']",['TeV $\\gamma$ Ray Emission from Southern Sky Objects and CANGAROO Project'],['Astrophysics and Astronomy'],"['talk, Williamsburg 1997/04/27', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'photon electron, Compton scattering', 'electron, energy', 'astrophysics, magnetic field', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707001'],"['We report recent results of the CANGAROO Collaboration on very high energy gamma ray emission from pulsars, their nebulae, SNR and AGN in the southern sky. Observations are made in South Australia using the imaging technique of detecting atmospheric Cerenkov light from gamma rays higher than about 1 TeV. The detected gamma rays are most likely produced by the inverse Compton process by electrons which also radiate synchrotron X-rays. Together with information from longer wavelengths, our results can be used to infer the strength of magnetic field in the emission region of gamma rays as well as the energy of the progenitor electrons. A description of the CANGAROO project is also given, as well as details of the new telescope of 7 m diameter which is scheduled to be in operation within two years.']",['1997-07-02'] +1915,['eng'],"['Dar, Arnon']",['Solar Neutrinos and The Standard Solar Model'],['Astrophysics and Astronomy'],"['talk, Moscow 1997/02/18', 'model, solar', 'neutrino, solar', 'neutrino, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707015'],"['The standard solar model (SSM) yield a $^8$B solar neutrino flux which is consistent within the theoretical and experimental uncertainties with that observed at Super-Kamiokande. The combined results from the Super- Kamiokande and the Chlorine solar neutrino experiments do not provide a solid evidence for neutrino properties beyond the minimal standard electroweak model. The results from the Gallium experiments and independently the combined results from Super-Kamiokande and the Chlorine experiment imply that the $^7$Be solar neutrino flux is strongly suppressed compared with that predicted by the SSM. This conclusion, however, is valid only if the neutrino absorption cross sections near threshold in Gallium and Chlorine do not differ significantly from their theoretical estimates. Such a departure has not been ruled out by the Chromium source experiments in Gallium. Even if the $^7$Be solar neutrino flux is suppressed compared with that predicted by the SSM, still it can be due to astrophysical effects not included in the simplistic SSM. Such effects include spatial and/or temporal variations in the temperature in the solar core induced by the convective layer through g-modes or by rotational mixing in the solar core, and dense plasma effects which may strongly enhance p-capture by $^7$Be relative to e-capture. The new generation of solar observations, which already look non stop deep into the sun, like Super-Kamiokande through neutrinos, and SOHO and GONG through acoustic waves, may be able to point at the correct solution; astrophysical solutions if they detect unexpected temporal and/or spatial behaviour, or particle physics solutions if Super-Kamiokande detects characteristic spectral distortion or temporal variations (e.g., the day-night effect) of the $^8$B solar neutrino flux . If']",['1997-07-03'] +1916,['eng'],"['Masperi, L', 'Silva, G']",['Cosmic Rays from Decaying Vortons'],['Astrophysics and Astronomy'],"['cosmic radiation, flux', 'decay, vorton', 'lifetime, vorton', 'density, vorton', 'superconducting, string']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706299'],"['The flux of high energy cosmic rays coming from the decay of vortons is estimated. If the abundance of loops corresponding to a superconductivity scale coincident with that of the string formation is corrected to be compatible with the critical density of universe, it is found that the emission of one carrier per vorton may produce a flux of one cosmic ray event per $km^2$ of detector and per year.']",['1997-07-01'] +1917,['eng'],"['Martins, C J A P', 'Shellard, E P S']",['Galactic Magnetic Fields from Superconducting Strings'],['Astrophysics and Astronomy'],"['superconducting, string', 'current', 'magnetic field, galaxy', 'grand unified theory', 'electroweak interaction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706287'],"[""We use a simple analytic model for the evolution of currents in superconducting strings to estimate the strength of the `seed' magnetic fields generated by these strings. This model is an extension of the evolution model of Martins and Shellard depending on a parameter $f$ which characterizes the importance of equilibration process in the evolution of the currents. For GUT-scale strings, we find that a viable seed magnetic field for the galactic dynamo can be generated if equilibration is weak. On the other hand, electroweak-scale strings originate magnetic fields that are smaller than required.""]",['1997-06-30'] +1918,['eng'],"['Törnkvist, O', 'Riotto, A']",['CP Violating Solitons in the Early Universe'],['Astrophysics and Astronomy'],"['talk, Rome 1997/05/19', 'astrophysics, model', 'violation, CP', 'soliton', 'membrane model', 'baryon, asymmetry', 'Higgs particle, multiplet', 'doublet, 2', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706271'],"['Solitons in extensions of the Standard Model can serve as localized sources of CP violation. Depending on their stability properties, they may serve either to create or to deplete the baryon asymmetry. The conditions for existence of a particular soliton candidate, the membrane solution of the two-Higgs model, are presented. In the generic case, investigated by Bachas and Tomaras, membranes exist and are metastable for a wide range of parameters. For the more viable supersymmetric case, it is shown that the present-day existence of CP-violating membranes is experimentally excluded, but preliminary studies suggest that they may have existed in the early universe soon after the electroweak phase transition, with important consequences for the baryon asymmetry of the universe.']",['1997-06-30'] +1919,['eng'],"['Abel, T', 'Stebbins, A J', 'Anninos, P', 'Norman, M L']","['First Structure Formation; 2, Cosmic String + Hot Dark Matter Models']",['Astrophysics and Astronomy'],"['astrophysics, string', 'model, fluid', 'baryon, matter', 'astrophysics, missing-mass', 'neutrino, density', 'model, hydrodynamical', 'cosmic radiation, anisotropy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706262'],"['We examine the structure of baryonic wakes in the cosmological fluid which would form behind GUT-scale cosmic strings at early times (redshifts z > 100) in a neutrino-dominated universe. We show, using simple analytical arguments as well as 1- and 2-dimensional hydrodynamical simulations, that these wakes will NOT be able to form interesting cosmological objects before the neutrino component collapses. The width of the baryonic wakes (< 10 kpc comoving) is smaller than the scale of wiggles on the strings and are probably not enhanced by the wiggliness of the string network.']",['1997-06-30'] +1920,['eng'],"['Salopek, D S']",['Coordinate-free Solutions for Cosmological Superspace'],['Astrophysics and Astronomy'],"['astrophysics, superspace', 'relativity theory, general', 'gravitation', 'matter', 'Hamilton-Jacobi equation, solution', 'field theory, scalar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9801161'],"[""Hamilton-Jacobi theory for general relativity provides an elegant covariant formulation of the gravitational field. A general `coordinate-free' method of integrating the functional Hamilton-Jacobi equation for gravity and matter is described. This series approximation method represents a large generalization of the spatial gradient expansion that had been employed earlier. Additional solutions may be constructed using a nonlinear superposition principle. This formalism may be applied to problems in cosmology.""]",['1998-01-19'] +1921,['eng'],"['Balantekin, A B']",['Selected Topics in Neutrino Astrophysics'],['Astrophysics and Astronomy'],"['review, Sao Paulo 1997/01/16', 'neutrino, solar', 'neutrino, cosmic radiation', 'astrophysics, supernova', 'neutrino, oscillation', 'neutrino, flavor', 'neutrino, interference', 'matter, stochastic', 'neutrino, fluctuation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706256'],"['This review covers a subset of the astrophysical phenomena where neutrinos play a significant role and where the underlying microphysics is nuclear physics. The current status of the solar neutrino problem, atmospheric neutrino experiments, the role of neutrinos in determining the dynamics of type-II supernovae, and recent developments in exploring neutrino propagation in stochastic media are reviewed.']",['1997-06-26'] +1922,['eng'],"['Turok, Neil G', 'Pen, U L', 'Seljak, Yu']","['The Scalar, Vector and Tensor Contributions to CMB anisotropies from Cosmic Defects']",['Astrophysics and Astronomy'],"['astrophysics, defect', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, fluctuation', 'causality', 'scaling', 'analytic properties', 'perturbation, scalar', 'perturbation, vector', 'perturbation, tensor', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706250'],"['Recent work has emphasised the importance of vector and tensor contributions to the large scale microwave anisotropy fluctuations produced by cosmic defects. In this paper we provide a general discussion of these contributions, and how their magnitude is constrained by the fundamental assumptions of causality, scaling, and statistical isotropy. We discuss an analytic model which illustrates and explains how the ratios of isotropic and anisotropic scalar, vector and tensor microwave anisotropies are determined. This provides a check of the results from large scale numerical simulations, confirming the numerical finding that vector and tensor modes provide substantial contributions to the large angle anisotropies. This leads to a suppression of the scalar normalisation and consequently of the Doppler peaks.']",['1997-06-26'] +1923,['eng'],"['McEnery, J E', 'Bond, I H', 'Boyle, P J', 'Bradbury, S M', 'Breslin, A C', 'Buckley, J H', 'Burdett, A M', 'Bussons-Gordo, J', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hall, A', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'Masterson, C', 'Mohanty, G', 'Moriarty, P', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'Zweerink, J A']",['Tev Observations of the Variability and Spectrum of Markarian 421'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'astrophysics', 'photon, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'time dependence', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706125'],"['Markarian 421 was the first extragalactic source to be detected with high statistical certainty at TeV energies. The Whipple Observatory gamma-ray telescope has been used to observe the Active Galactic Nucleus, Markarian 421 in 1996 and 1997. The rapid variability observed in TeV gamma rays in previous years is confirmed. Doubling times as short as 15 minutes are reported with flux levels reaching 15 photons per minute. The TeV energy spectrum is derived using two independent methods. The implications for the intergalactic infra-red medium of an observed unbroken power law spectrum up to energies of 5 TeV is discussed.']",['1997-06-16'] +1924,['eng'],"['Glendenning, N K']",['Internal Constitution of Neutron and Strange Stars'],['Astrophysics and Astronomy'],"['lectures, Lipari 1996/10/01', 'n, matter', 'matter, strangeness', 'fermion, statistics', 'black hole, production', 'quark, matter', 'crystal', 'astrophysics, pulsar', 'critical phenomena', 'energy, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706236'],"['In the first of these two lectures I will discuss the rich constitution of neutron stars as a consequence of the Pauli principle which is engaged by the dominance of gravity over the nuclear force. Three especially interesting phenomena are discussed in this contect---(1) a mechanism for the formation of low-mass black holes distinct in their mass-range from the black holes formed in the prompt collapse of an entire star, (2) a multilayered crystalline structure consisting of confined hadronic matter embedded in a background of deconfined quark matter (or vice versa) which occupies a many kilometer thick inner region, and (3) a clean and pronounced signal of the formation of quark matter in the interior of neutron stars. In the second lecture I will discuss the strange matter hypothesis, its viability as well as its consequences for compact stars and a new family of white dwarfs with dense nuclear matter central regions some orders of magnuitude greater than in ordinary white dwarfs.']",['1997-06-24'] +1925,['eng'],"['Garriga, J', 'Montes, X', 'Sasaki, M', 'Tanaka, T']",['Canonical Quantization of Cosmological Perturbations in the One Bubble Open Universe'],['Astrophysics and Astronomy'],"['inflationary universe, bubble', 'perturbation, scalar', 'invariance, gauge', 'phase space', 'gravitational radiation, spectra']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706229'],"[""Faddeev and Jackiw's method for constrained systems is used to derive a gauge invariant formulation of cosmological perturbations in the one bubble inflationary universe. For scalar perturbations in a flat universe, reduction of the action to the one with a single physical degree of freedom has been derived in the literature. A straightforward generalization of it to the case of an open universe is possible but it is not adequate for quantizing perturbations in the one bubble universe, because of the lack of Cauchy surfaces inside the bubble. Therefore we perform the reduction of the action outside the lightcone emanating from the center of the bubble or nucleation event, where the natural time constant hypersurfaces are no longer homogeneous and isotropic and as a result the conventional classification of perturbations in terms of scalar and tensor modes is not possible. Nevertheless, after reduction of the action we find three decoupled actions for three independent degrees of freedom, one of which corresponds to the scalar mode and the other two to the tensor modes. Implications for the one bubble open inflationary models are briefly discussed. As an application of our formalism, the spectrum of long wavelength gravity waves is simply obtained in terms of the real part of the reflection amplitude for a one dimensional scattering problem, where the potential barrier is given in terms of the bubble profile.""]",['1997-06-24'] +1926,['eng'],"['McGraw, P N']",['Evolution of a Non-Abelian Cosmic String Network'],['Astrophysics and Astronomy'],"['astrophysics, string', 'gauge field theory, nonabelian', 'scattering, string', 'flux, magnetic', 'noncommutative', 'string tension', 'energy, density', 'time dependence', 'vortex', 'statistics', 'lattice field theory', 'scaling', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706182'],"[""We describe a numerical simulation of the evolution of an $S_3$ cosmic string network which takes fully into account the non-commutative nature of the cosmic string fluxes and the topological obstructions which hinder strings from moving past each other or intercommuting. The influence of initial conditions, string tensions, and other parameters on the network's evolution is explored. In a broad range of regimes, the total energy density as a function of time exhibits a familiar power-law behavior, and we do not find strong support for a string-dominated cosmological scenario. However, the speed of the network's collapse (coefficient of the power law) can vary quite a bit, as can the qualitative features of the network. There is a surprisingly strong dependence on the statistical properties of the initial conditions. The results give some insight as to which processes play the most important roles in the evolution of a non-Abelian network.""]",['1997-06-18'] +1927,['eng'],"['Buckley, J H', 'Boyle, P J', 'Bradbury, S M', 'Burdett, A M', 'Gordo, J B', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Rovero, A C', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'Zweerink, J A']",['A Search for TeV Emission from Unidentified Sources in the Galactic Plane'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'upper limit', 'data analysis method', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706178'],"['The ~70 unidentified sources of the EGRET sky survey may be one of its most important legacies. The identification of these sources at other wavelengths is critical to understanding their nature. Many have flat spectra out to 10 GeV which, if extrapolated to TeV energies, would be easily detectable relative to the steeply falling diffuse background. The Whipple Observatory gamma-ray telescope has been used to observe a number of these which were selected based on their position, intensity and spectrum and in some cases based on a possible association with a supernova remnant or pulsar. No significant emission has been detected from these sources, and upper limits are given.']",['1997-06-18'] +1928,['eng'],"['Quinn, J', 'Bond, I H', 'Boyle, P J', 'Buckley, J H', 'Bradbury, S M', 'Breslin, A C', 'Burdett, A M', 'Gordo, J B', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hall, A', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Moriarty, P', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Weeke, T C', 'Zweerink, J A']",['TeV Observations of the Variability and Spectrum of Markarian 501'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics', 'cosmic radiation, energy spectrum', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706142'],"['Markarian 501 is only the second extragalactic source to be detected with high statistical certainty at TeV energies; it is similar in many ways to Markarian 421. The Whipple Observatory gamma-ray telescope has been used to observe the AGN Markarian 501 in 1996 and 1997, the years subsequent to its initial detection. The apparent variability on the one-day time-scale observed in TeV gamma rays in 1995 is confirmed and compared with the variability in Markarian 421. Observations at X-ray and optical wavelengths from 1997 are also presented.']",['1997-06-18'] +1929,['eng'],"['Srinivasan, R', 'Boyle, P J', 'Buckley, J H', 'Burdett, A M', 'Gordo, J B', 'Carter-Lewis, D A', 'Cawley, M F', 'Catanese, M', 'Colombo, E', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hillas, A M', 'Lamb, R C', 'Krennrich, F', 'Lessard, R W', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Moriarty, P', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Weekes, T C', 'Zweerink, J A']",['Very High Energy Observations of PSR B1951+32'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'upper limit', 'astrophysics, pulsar', 'cosmic radiation, time variation', 'Cherenkov counter, experimental results', '> 30 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706144'],"['PSR B1951+32 is a gamma-ray pulsar detected by the Energetic Gamma Ray Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The EGRET data shows no evidence for a spectral turnover. Here we report on the first observations of PSR B1951+32 beyond 30 GeV. The observations were carried out with the 10m gamma-ray telescope at the Whipple Observatory on Mt. Hopkins, Arizona. In 8.1 hours of observation we find no evidence for steady or periodic emission from PSR B1951+32 above ~260 GeV. FLux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models.']",['1997-06-18'] +1930,['eng'],"['Carter-Lewis, D A', 'Biller, S D', 'Boyle, P J', 'Buckley, J H', 'Burdett, A C', 'Gordo, J B', 'Catanese, M', 'Cawley, M F', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'West, M', 'Zweerink, J A']",['Spectrum of TeV $\\gamma$-Rays from the Crab Nebula'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'data analysis method', 'Cherenkov counter, imaging', 'experimental results', '300-8000 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706145'],"['The Crab Nebula has become established as the standard candle for TeV gamma-ray astronomy using the atmospheric Cherenkov technique. No evidence for variability has been seen. The spectrum of gamma rays from the Crab Nebula has been measured in the energy range 500 GeV to 8 TeV at the Whipple Observatory by the atmospheric Cherenkov imaging technique. Two methods of analysis involving independent Monte Carlo simulations and two databases of observations (1988-89 and 1995-96) were used and gave close agreement. Using the complete spectrum of the Crab Nebula, the spectrum of relativistic electrons is deduced and the spectrum of the resulting inverse Compton gamma-ray emission is in good agreement with the measured spectrum if the ambient magnetic field is about 25-30 nT.']",['1997-06-18'] +1931,['eng'],"['Weekes, T C', 'Akerlof, Carl W', 'Biller, S D', 'Breslin, A C', 'Buckley, J H', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Dingus, B L', 'Fazio, G G', 'Fegan, D J', 'Finley, J', 'Fishman, G', 'Gaidos, J A', 'Gillanders, G H', 'Gorham, P W', 'Grindlay, J E', 'Hillas, A M', 'Huchra, J P', 'Kaaret, P E', 'Kertzman, M P', 'Kieda, D B', 'Krennrich, F', 'Lamb, R C', 'Lang, M J', 'Marscher, A P', 'Matz, S', 'McKay, T', 'Müller, D', 'Ong, R', 'Purcell, W', 'Rose, J', 'Sembroski, G H', 'Seward, F D', 'Slane, P', 'Swordy, S P', 'Tumer, T O', 'Ulmer, M P', 'Urban, M', 'Wilkes, B J']",['VERITAS'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'Cherenkov counter, air', 'imaging', 'energy resolution', 'angular resolution', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706143'],['A next generation atmospheric Cherenkov observatory is described based on the Whipple Observatory $\\gamma$-ray telescope. A total of nine such imaging telescopes will be deployed in an array that will permit the maximum versatility and give high sensitivity in the 50 GeV - 50 TeV band (with maximum sensitivity from 100 GeV to 10 TeV).'],['1997-06-18'] +1932,['eng'],"['Catanese, M', 'Boyle, P J', 'Buckley, J H', 'Burdett, A M', 'Gordo, J B', 'Carter-Lewis, D A', 'Cawley, M F', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'Zweerink, J A']",['First Results from a Search for TeV Emission from BL Lacs'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706136'],"['Two active galactic nuclei have been detected at TeV energies using the atmospheric Cherenkov imaging technique. The Whipple Observatory gamma-ray telescope has been used to observe all the BL Lacertae objects in the northern hemisphere out to a redshift of 0.1. We report the tentative detection of VHE emission from a third BL Lac object, 1ES 2344+514. Progress in extending this survey out to z=0.2 will also be reported.']",['1997-06-16'] +1933,['eng'],"['Boyle, P J', 'Buckley, J H', 'Burdett, A M', 'Gordo, J B', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Connaughton, V', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Harris, K', 'Hillas, A M', 'Lamb, R C', 'Krennrich, F', 'Lessard, R W', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Porter, N A', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'Zweerink, J A']",['Search for TeV Counterparts in $\\gamma$-Ray Bursts'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'photon, showers', 'cosmic radiation, energy', 'cosmic radiation, time delay', 'correlation', 'cosmic radiation, particle source', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706132'],"['Based on BACODINE network notification the Whipple Observatory gamma-ray telescope has been used to search for the delayed TeV counterpart to BATSE-detected gamma-ray bursts. In the fast slew mode, any point in the sky can be reached within two minutes of the burst notification. The search strategy, necessary because of the uncertainty in burst position and limited FOV of the camera, is described.']",['1997-06-16'] +1934,['eng'],"['Lessard, R W', 'Boyle, P J', 'Bradbury, S M', 'Buckley, J H', 'Burdett, A C', 'Gordo, J B', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Fegan, D J', 'Finley, J P', 'Gaidos, J A', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Masterson, C', 'McEnery, J E', 'Mohanty, G', 'Quinn, J', 'Rodgers, A J', 'Rose, H J', 'Samuelson, F W', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'Zweerink, J A']",['Constraints on Cosmic-Ray Origin Theories from TeV $\\gamma$-Ray Observations'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'cosmic radiation, flux', 'upper limit', 'astrophysics, supernova', 'cosmic radiation, acceleration', 'shock waves', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706131'],"['If supernova remnants (SNRs) are the sites of cosmic-ray acceleration, the associated nuclear interactions should result in observable fluxes of TeV gamma-rays from the nearest SNRs. Measurements of the gamma-ray flux from six nearby, radio-bright, SNRs have been made with the Whipple Observatory gamma-ray telescope. No significant emission has been detected and upper limits on the $>$300 GeV flux are reported. Three of these SNRs (IC443, gamma-Cygni and W44) are spatially coincident with low latitude unidentified sources detected with EGRET. These upper limits weaken the case for the simplest models of shock acceleration and energy dependent propagation.']",['1997-06-16'] +1935,['eng'],"['Akerlof, Carl W', 'Biller, S D', 'Boyle, P', 'Buckley, J H', 'Carter-Lewis, D A', 'Catanese, M', 'Cawley, M F', 'Connaughton, V', 'Fegan, D J', 'Finley, J', 'Gaidos, J A', 'Hillas, A M', 'Krennrich, F', 'Lamb, R C', 'Lessard, R W', 'McEnery, J E', 'Mohanty, G', 'Porter, N A', 'Quinn, J', 'Rodgers, A', 'Rose, H J', 'Samuelson, F', 'Schubnell, M S', 'Sembroski, G H', 'Srinivasan, R', 'Weekes, T C', 'Zweerink, J A']",['A search for correlations of TeV $\\gamma$-rays with ultra-high energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, energy', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'correlation', 'defect, topological', 'cosmic radiation, flux', 'upper limit', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706123'],"[""A search was conducted for TeV gamma-rays emitted from the direction of the ultra-high energy cosmic ray detected by the Fly's Eye Experiment with E ~ 3 x 10**20 eV. No enhancement was found at a level of 10**-10 gamma/cm**2-sec for E>350 GeV. This upper limit is consistent with theoretical estimates based on topological defects as sources of UHE cosmic rays. An upper limit was also set for the flux of TeV gamma rays from 3C147, the most prominent AGN in the error box.""]",['1997-06-27'] +1936,['eng'],"['Broderick, J J', 'Herrin, E T', 'Krisher, T P', 'Morgan, D L', 'Rosenbaum, D C', 'Sher, M', 'Teplitz, V L']",['Millimeter-wave Signature of Strange Matter Stars'],['Astrophysics and Astronomy'],"['astrophysics, matter', 'matter, strangeness', 'quark, matter', 'effect, rotational', 'radiation, flux', 'astrophysics, pulsar', 'n, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706094'],"['One of the most important questions in the study of compact objects is the nature of pulsars, including whether they consist of neutron matter or strange quark matter (SQM). However, few mechanisms for distinguishing between these two possibilities have been proposed. The purpose of this paper is to show that a strange star (one made of SQM) will have a vibratory mode with an oscillation frequency of approximately 250 GHz (millimeter wave). This mode corresponds to motion of the center of the expected crust of normal matter relative to the center of the strange quark core, without distortion of either. Radiation from currents generated in the crust at the mode frequency would be a SQM signature. We also consider effects of stellar rotation, estimate power emission and signal-to-noise ratio, and discuss briefly possible mechanisms for exciting the mode.']",['1997-06-11'] +1937,['eng'],"['Lee, W', 'Fang, L Z']",['Density Perturbations of Thermal Origin During Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'thermodynamics', 'spectra, perturbation', 'radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706101'],"['We study thermally induced density perturbations during inflation. This scenario is characterized by two thermodynamical conditions: (1) The primordial perturbations originate in the epoch when the inflationary universe contains a thermalized heat bath. (2) The perturbations of the inflationary scalar field are given by the fluctuation-dissipation relation. We show that the spectrum of the primordial perturbations is of power law, but tilted, and there is a relation between the amplitude and the index of the power spectrum. Aside from the mass scale of the inflation, the amplitude-index relation does not depend on other parameters like $g$-factor. These results are found to be well consistent with observations of the temperature fluctuations of cosmic microwave background if the mass scale of the inflation is about $10^{15}$ GeV. Instead of the purely adiabatic case, the consequent density perturbation is an admixture of adiabatic and isocurvature one. Therefore, the detection of super-Hubble suppression of the spectrum would be effective for further discrimination between the thermally originated models and others.']",['1997-06-11'] +1938,['eng'],"['Aiso, S', 'Chikawa, M', 'Hayashi, Y', 'Hayashida, N', 'Hibino, K', 'Hirasawa, H', 'Honda, K', 'Hotta, N', 'Inoue, N', 'Ishikawa, F', 'Ito, N', 'Kabe, S', 'Kajino, F', 'Kashiwagi, T', 'Kawakami, S', 'Kawasaki, Y', 'Kawasumi, N', 'Kitamura, H', 'Kuramochi, K', 'Kurata, K', 'Kusano, E', 'Lafoux, H', 'Loh, E C', 'Matsubara, Y', 'Matsuyama, T', 'Mizumoto, Y', 'Mizutani, K', 'Nagano, M', 'Nishikawa, D', 'Nishimura, J', 'Nishizawa, M', 'Ouchi, T', 'Ohoka, H', 'Ohnishi, M', 'Saitô, T', 'Sakaki, N', 'Sakata, M', 'Sakumoto, K', 'Sasaki, M', 'Sasano, M', 'Shimodaira, H', 'Shiomi, A', 'Sokolsky, P', 'Sugiyama, T', 'Takahashi, T', 'Taylor, S', 'Teshima, M', 'Tsushima, I', 'Uchihori, Y', 'Yamamoto, T', 'Yamamoto, Y', 'Yoshida, S', 'Yoshii, H', 'Yuda, T']",['The Detection of TeV $\\gamma$ Rays from Crab using the Telescope Array Prototype'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, counters and detectors', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706079'],"[""The Telescope Array prototype detectors were installed at Akeno Observatory and at the Utah Fly's Eye site. Using these detectors, we have observed the Crab Nebula and AGN's since the end of 1995. The successful detections of TeV gamma rays from Crab Nebula and Mkn501 are reported.""]",['1997-06-10'] +1939,['eng'],"['Schramm, David N', 'Turner, M S']",['Big-bang Nucleosynthesis Enters the Precision Era'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'baryon, density', 'cosmic radiation, background', 'helium, nuclide', 'astrophysics, galaxy', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706069'],"[""The last parameter of big-bang nucleosynthesis, the baryon density, is being pinned down by measurements of the deuterium abundance in high-redshift hydrogen clouds. When it is determined, it will fix the primeval light-element abundances. D, ^3He and ^7Li will become ``tracers'' for the study of Galactic and stellar chemical evolution, and big-bang nucleosynthesis will become an even sharper probe of particle physics, e.g., the bound to the number of light neutrino species will be tightened significantly. Two key tests of the consistency of the standard theory are on the horizon: an independent, high-precision determination of the baryon density from anisotropy of the cosmic background radiation and a precision determination of the primeval $^4$He abundance.""]",['1997-06-10'] +1940,['eng'],"['Bloom, Elliott D', 'Wells, J D']",['Multi-GeV photons from electron-dark matter scattering near Active Galactic Nuclei'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'electron, emission', 'electron, jet', 'photon, cosmic radiation', 'astrophysics, missing-mass', 'supersymmetry', 'LSP', 'scattering, electron LSP', 'sparticle, production', 'selectron', 'Feynman graph', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706085'],"['Active Galactic Nuclei (AGN) may emit highly collimated and intense jets of relativistic electrons which upscatter ambient photons. These electrons can also scatter off the cold dark matter halo of the galaxy to produce high energy photons which have a more isotropic signature than the upscattered photons from QED processes. We propose to look for these high energy photons coming from AGN as a method to detect dark matter. As a primary example we work out the expected signal from electrons scattering off the lightest supersymmetric partner into a photon plus selectron. Using the optimistic side of astrophysical uncertainties, we still find the signal from M87 or Centaurus A, two close-by AGN, smaller than the sensitivities expected of the currently proposed photon detectors. However, long running photon detectors and future detectors of higher sensitivity might be able to distinguish a signal from AGN sources. In order to have confidence that new physics sources are discernible, we also emphasize the importance of multi-wavelength studies of AGN with varying jet axis orientation to the earth.']",['1997-06-10'] +1941,['eng'],"['Aharonian, F A']","['Measurement of the flux, spectrum, and variability of TeV $\\gamma$-rays from Mkn 501 during a state of high activity']",['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, time variation', 'Cherenkov counter, experimental results', '1000-10000 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706019'],"['Between March 16, 1997 and April 14, 1997, a high flux level of TeV gamma-rays was observed from Mkn 501, using the HEGRA stereoscopic system of four imaging Cherenkov telescopes. The flux level varied during this period from about one up to eight times the flux observed from the Crab Nebula. Changes of the detection rate by a factor of up to 4 within 1 day have been observed. The measured differential energy spectrum of the radiation follows a power law from 1 TeV to 10 TeV. The differential spectral index of 2.49{+-}0.11{+-}0.25 is close to that of the Crab Nebula of 2.71{+-}0.17{+-}0.25.']",['1997-06-05'] +1942,['eng'],"['Morel, P', 'Provos, J', 'Berthomieu, G']",['Updated Solar Models'],['Astrophysics and Astronomy'],"['model, solar', 'helium, diffusion', 'lithium', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705251'],"['Solar models computed with mass loss, microscopic diffusion of helium and heavy elements and with updated physics have been evolved from the pre-main sequence to present days; they are compared to the observational constraints including lithium depletion and to the Solar Reference Model (SRM) of Basu et al. (1996), derived by inversion. Microscopic diffusion significantly improves the agreement with the observed solar frequencies and agree with the SRM within +- 0.2% for the sound velocity and +- 1% for the density, but slightly worsens the neutrino problem. Neither microscopic diffusion nor overshooting explain the observed lithium depletion consistently with helioseismological constraints, while a mass loss process does it. Models computed with OPAL equation of state and opacities are in better agreement with the seimic sound speed. To reach the level of precision of helioseismological observations the accuracy of solar models still needs to be improved by one magnitude; any such improvement will necessitate equation of state and opacity data taking into account of detailed changes in the mixture.']",['1997-06-02'] +1943,['eng'],"['Bolesta, J J', 'Bradner, H', 'Camerini, U', 'Clem, J', 'Dye, S T', 'George, J', 'Gorham, P W', 'Grieder, P K F', 'Hauptman, J M', 'Hayashino, T', 'Jaworski, M', 'Kitamura, T', 'Kondo, S', 'Learned, J G', 'March, R H', 'Matsumoto, T', 'Matsuno, S', 'Mauritz, K M', 'Minkowski, Peter', 'Narita, T', ""O'Connor, D J"", 'Ohashi, Y', 'Okada, A', 'Peterson, V', 'Stenger, Victor J', 'Uehara, S', 'Webster, M', 'Wilkes, R J', 'Young, K K', 'Yamaguchi, A']",['A Search for Very High Energy Neutrinos from Active Galactic Nuclei'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'astrophysics, galaxy', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy', 'neutrino nucleon, interaction', 'showers, search for', 'Cherenkov counter, water', 'deep underground detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705198'],"['We report the results of a search for neutrino-induced particle cascades using a deep ocean water Cherenkov detector. The effective mass of the detector, a string of seven 40 cm diameter photomultipliers at 5.2 m spacing, is found through simulation analysis to be surprisingly large: greater than 1 megaton of water at incident neutrino energies of 1 PeV. We find no evidence for neutrino-induced cascades in 18.6 hours of observation. Although the limit implied by this observation is the strongest yet for predictions of active galatic nuclei (AGN) neutrinos at energies above 100 TeV, perhaps the more intriguing result is that the power of these techniques can be exploited to test these AGN models in a relatively short time.']",['1997-05-27'] +1944,['eng'],"['Alvarez-Muñiz, J', 'Zas, E']",['Cherenkov radio pulses from EeV neutrino interactions'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'matter, electric field', 'showers, electromagnetic', 'radiation, Cherenkov', 'angular distribution', 'neutrino, counters and detectors', 'counters and detectors, proposed', 'showers, length', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706064'],['We study the implications of the LPM effect for the Cherenkov radiation of EeV electromagnetic showers in the coherent radiowave regime for ice. We show that for showers above 100~PeV the electric field scales with shower energy but has a markedly narrower angular distribution than for lower energy showers. We give an electric field frequency and angular spectrum parameterization valid for showers having energy up to the EeV regime and discuss the implications for neutrino detectors based on arrays of radio antennas. Implications of the LPM effect for under water neutrino detectors in project are also briefly addressed.'],['1997-06-09'] +1945,['eng'],"['Christiansen, M B', 'Glendenning, N K']",['Finite size effects and the mixed quark-hadron phase in neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'effect, finite size', 'transition, quark hadron', 'crystal', 'bag model', 'surface tension', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706056'],"['We demonstrate that the form and location (not the size or spacing) of the energetically preferred geometrical structure of the crystalline quark-hadron mixed phase in a neutron star is very sensitive to finite size terms beyond the surface term. We consider two independent approaches of including further finite size terms, namely the multiple reflection expansion of the bag model and an effective surface tension description. Thus care should be taken in any model requiring detailed knowledge of these crystalline structures.']",['1997-06-06'] +1946,['eng'],"['Postnov, K A']",['Astrophysical Sources of Stochastic Gravitational Radiation in the Universe'],['Astrophysics and Astronomy'],"['talk, Baksan 1997/04/15', 'gravitational radiation, stochastic', 'interference, laser', 'n, matter', 'gravitational radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706053'],"['Stochastic gravitational waves (GW) associated with unresolved astrophysical sources at frequency bands of the ongoing GW interferometers LIGO/VIRGO and LISA are studied. We show that GW noise from rotating galactic neutron stars with low magnetic fields may reach the advanced LIGO sensitivity level at frequency $f\\sim 100$ Hz. Within LISA frequency band (10^{-4}-10^{-1} Hz), the GW background from galactic binary stars is shown to mainly contribute up to a frequency of 3.10^{-2} Hz, depending on the galactic rate of binary white dwarf mergers. To be detectable by LISA, relic GW backgrounds should be as high as']",['1997-06-06'] +1947,['eng'],"['Olive, Keith A']",['Primordial Nucleosynthesis and Dark Matter'],['Astrophysics and Astronomy'],"['lectures, Lake Louise 1997/02/16', 'astrophysics, model', 'light nucleus, production', 'helium', 'lithium', 'astrophysics, galaxy', 'astrophysics, missing-mass', 'baryon, missing-mass', 'chemistry', 'thermodynamics', 'neutrino, massive', 'supersymmetry', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9707212'],"['Following a brief introduction to early Universe cosmology, the current of status of big bang nucleosynthesis is reviewed and the concordance between theory and observation is examined in detail. The abundances of He4 and Li7 determine the value of the baryon-to-photon ratio, $\\eta$ to be relatively low, D/H in quasar absorption systems. These results have far reaching consequences for galactic chemical evolution, the amount of baryonic dark matter in the Universe and on the allowed number of degrees of freedom in the early Universe. Finally, motivations for cosmological dark matter will be reviewed with special emphasis placed on supersymmetric candidates.']",['1997-07-25'] +1948,['eng'],"['Bhat, P N']",['Pachmarhi Array of Cerenkov Telescopes'],['Astrophysics and Astronomy'],"['talk, Bombay 1996/08/12', 'photon, cosmic radiation', 'Cherenkov counter, air', 'optics, reflection', 'photoelectron, amplifier', 'background', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706033'],"['This talk is based on the Very High Energy Gamma Ray Astronomy observations planned to be carried out at Pachmarhi in the central Indian state of Madhya Pradesh using the well known atmospheric \\v Cerenkov technique. The development of a ground based array of 25 \\v Cerenkov telescopes is currently underway at Pachmarhi situated at an altitutde of about a kilometer. Using this array it is proposed to sample the \\v Cerenkov light pool at various distances from the shower core in order to estimate the lateral distribution parameters of the shower. Simulation studies have shown that these parametrs would enable one to distinguish gamma ray initiated showers from those by cosmic ray charged particles, thus significantly improving the signal to noise ratio. After summarizing the genesis of VHE gamma ray astronomy in our institute we will discuss the scientific motivation of this concept of enriching the gamma ray signal as compared to the standard imaging technique. The current status of the detector development and the expected results will be presented.']",['1997-06-05'] +1949,['eng'],"['Dobado, A', 'Maroto, A L']",['Primordial torsion fields as an explanation of the anisotropy in electromagnetic propagation over cosmological distances'],['Astrophysics and Astronomy'],"['coupling, torsion', 'radiation, electromagnetic', 'radiation, anisotropy', 'galaxy', 'fermion, charged particle', 'Feynman graph']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706044'],"['In this note we provide a simple explanation of the recent finding of anisotropy in electromagnetic (EM) propagation claimed by Nodland and Ralston. We consider, as a possible origin of such an effect, the effective coupling between EM fields and some background torsion field that is obtained after integrating out charged fermions.']",['1997-06-05'] +1950,['eng'],"['Bhat, P N', 'Vishwanath, P R', 'Acharya, B S', 'Krishnaswamy, M R']",['Pachmarhi Array of Cerenkov Telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'Cherenkov counter, air', 'photoelectron, amplifier', 'signal processing', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706027'],['Very High Energy (VHE) gamma -ray Astronomy observations are planned to be carried out at Pachmarhi in the central Indian state of Madhya Pradesh using the well known atmospheric Cerenkov technique. An array of 25 Cerenkov telescopes is currently under construction. Using this array it is proposed to sample the Cerenkov light pool at various distances from the shower core in order to estimate the lateral distribution parameters of the shower. In this paper we discuss the scientific motivation of this concept of enriching the gamma -ray signal as compared to the standard imaging technique. The current status of the detector development and the expected results will be presented.'],['1997-06-05'] +1951,['eng'],"['Barrau, A', 'Bazer-Bachi, R', 'Cabot, H', 'Chounet, L M', 'Debiais, G', 'Degrange, B', 'Dezalay, J P', 'Djannati-Ataï, A', 'Dumora, D', 'Espigat, P', 'Fabre, B', 'Fleury, P', 'Fontaine, G', 'George, R', 'Ghesquière, C', 'Goret, P', 'Gouiffes, C', 'Grenier, I A', 'Iacoucci, L', 'Le Bohec, S', 'Mallet, J', 'Meynadier, C', 'Munz, F', 'Palfrey, T A', 'Paré, E', 'Pons, Y', 'Punch, M', 'Québert, J', 'Ragan, K', 'Renault, C', 'Rivoal, M', 'Rob, L', 'Schovanek, P', 'Smith, D', 'Tavernet, J P', 'Vrana, J']",['Detection of the $\\gamma$-Rays from MRK 501 with the Cat Imaging Telescope'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics', 'cosmic radiation, flux', 'cosmic radiation, time variation', 'Cherenkov counter, imaging', 'experimental results', '> 220 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705249'],['The CAT imaging telescope on the site on the former solar plant Themis has been observing gamma-rays from Mrk501 above 220 GeV in March and April 1997. This source is shown to be highly variable and the light curve is presented. The detected gamma-ray rate for the most intense flare is in excess of 10 per minute.'],['1997-06-02'] +1952,['eng'],"['Barrau, A', 'Bazer-Bachi, R', 'Cabot, H', 'Chounet, L M', 'Debiais, G', 'Degrange, B', 'Dezalay, J P', 'Djannati-Ataï, A', 'Dumora, D', 'Espigat, P', 'Fabre, B', 'Fleury, P', 'Fontaine, G', 'George, R', 'Ghesquière, C', 'Goret, P', 'Gouiffes, C', 'Grenier, I A', 'Iacoucci, L', 'Le Bohec, S', 'Mallet, J', 'Meynadier, C', 'Munz, F', 'Palfrey, T A', 'Paré, E', 'Pons, Y', 'Punch, M', 'Québert, J', 'Ragan, K', 'Renault, C', 'Rivoal, M', 'Rob, L', 'Schovanek, P', 'Smith, D', 'Tavernet, J P', 'Vrana, J']",['Observation of the Crab Nebula $\\gamma$-Ray Emission Above 220 Gev by the Cat Cherenkov Imaging Telescope'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics', 'showers, spatial distribution', 'Cherenkov counter, imaging', 'trigger', 'energy, threshold', 'performance', '> 220 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705248'],"['The CAT imaging telescope, recently built on the site of the former solar plant Themis (French Pyrenees), observed gamma-rays from the Crab nebula from October 1996 to March 1997. This steady source, often considered as the standard candle of very-high-energy gamma-ray astronomy, is used as a test-beam to probe the performances of the new telescope, particularly its energy threshold (220 GeV at 20 degrees zenith angle) and the stability of its response. Due to the fine-grain camera, an accurate analysis of the longitudinal profiles of shower images is performed, yielding the source position in two dimensions for each individual shower.']",['1997-06-02'] +1953,['eng'],"['Battye, R A', 'Shellard, E P S']",['Recent Perspectives on Axion Cosmology'],['Astrophysics and Astronomy'],"['review, Heidelberg 1996/06/27', 'astrophysics, string', 'astrophysics, missing-mass', 'radiation, axion', 'radiation, spectra', 'axion, density', 'inflationary universe', 'entropy, production', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706014'],"['We review current cosmological constraints on the axion. We describe the basic mechanisms by which axions are created in the early universe, focussing on the standard thermal scenario where the dominant process is through axion radiation by a string network. A dark matter axion in this case would have a mass $\\ma \\sim 100 \\microeV$, with specified large uncertainties. This cosmological lower bound leaves a viable window for the axion below the astrophysical upper limit, $\\ma \\lapp 1-10 \\meV$. We also discuss alternative axion cosmologies which allow a much wider, but indefinite, mass range.']",['1997-06-03'] +1954,['eng'],"['Battye, R A', 'Caldwell, R R', 'Shellard, E P S']",['Gravitational Waves From Cosmic Strings'],['Astrophysics and Astronomy'],"['gravitational radiation, spectra', 'astrophysics, string', 'background, stochastic', 'spectra, density', 'spectra, measurement', 'effect, back reaction', 'topology, defect', 'pulsar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706013'],"['Gravitational waves from cosmic strings are generated in the first fractions of a second after the Big Bang, potentially providing a unprecedented probe of the early universe. We discuss the key dynamical processes underlying calculations of the stochasti c background produced by a string network and we detail the parameter dependencies of the resulting spectral density arising from the millisecond pulsar timings and primor dial nucleosynthesis are discussed, justifying our present conservative bound $G\\mu/c^2 < 5.4(\\pm 1.1)\\times 10^{-6}$. We then discuss the strong prospect of detecting (or ruling out) cosmic string background with the next generation of gravitational wave experiments. Comparison is also made with alternative cosmological sources of gravitational waves such as inflation and hybrid topological defects.']",['1997-06-03'] +1955,['eng'],"['Barrau, A', 'Bazer-Bachi, R', 'Cabot, H', 'Chounet, L M', 'Debiais, G', 'Degrange, B', 'Dezalay, J P', 'Djannati-Ataï, A', 'Dumora, D', 'Espigat, P', 'Fabre, B', 'Fleury, P', 'Fontaine, G', 'George, R', 'Ghesquière, C', 'Goret, P', 'Gouiffes, C', 'Grenier, I A', 'Iacoucci, L', 'Le Bohec, S', 'Mallet, J', 'Meynadier, C', 'Munz, F', 'Palfrey, T A', 'Paré, E', 'Pons, Y', 'Punch, M', 'Québert, J', 'Ragan, K', 'Renault, C', 'Rivoal, M', 'Rob, L', 'Schovanek, P', 'Smith, D', 'Tavernet, J P', 'Vrana, J']",['The CAT Imaging Telescope'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'photon, cosmic radiation', 'astrophysics', 'Cherenkov counter, imaging']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705247'],"['The VHE gamma-ray imaging telescope CAT started taking data in October 1996. Located at the Themis solar site in southern France, it features a 17.7 m^2 Davies-Cotton mirror equipped with 600 PMT camera at the focal plane. The mechanics and optics, the PMTs and the electronics are presented. The performance, based on the first 7 months of operation, is discribed.']",['1997-06-02'] +1956,['eng'],"['Palle, D']",['On certain relationships between cosmological observables in the Einstein-Cartan gravity'],['Astrophysics and Astronomy'],"['gravitation, model', 'gravitation, coupling', 'transformation, conformal', 'astrophysics, model', 'astrophysics, missing-mass']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706012'],"[""We show that in the Einstein-Cartan gravity it is possible to obtain a relation between Hubble's expansion and the global rotation (vorticity) of the Universe. Gravitational coupling can be reduced to dimensionless quantity of order unity, fixing the scalar mass density and the resulting negative cosmological constant at spacelike infinity. Current estimates of the expansion and rotation (see also astro-ph/9703082) of the Universe favour the massive spinning particles as candidate particles for cold and hot dark matter. Nodland and Ralston vorticity (Phys. Rev. Lett. 78 (1997) 3043) overestimates the value favoured by the Einstein-Cartan gravity for three orders of magnitude.""]",['1997-06-03'] +1957,['eng'],"['Strong, A W', 'Moskalenko, I V', 'Schönfelder, V']",['Numerical models for cosmic ray propagation and gamma ray production'],['Astrophysics and Astronomy'],"['talk, Durban 1997/07/28', 'cosmic radiation, primary', 'cosmic radiation, secondary radiation', 'nucleon, cosmic radiation', 'electron, cosmic radiation', 'positron, cosmic radiation', 'astrophysics, galaxy', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'cosmic radiation, spatial distribution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9706010'],"['An extensive program for the calculation of galactic cosmic-ray propagation has been developed. Primary and secondary nucleons, primary and secondary electrons, and secondary positrons are included. The basic spatial propagation mechanisms are (momentum-dependent) diffusion, convection, while in momentum space energy loss and diffusive reacceleration are treated. Fragmentation and energy losses are computed using realistic distributions for the interstellar gas and radiation fields. Predictions of the diffuse Galactic gamma ray and synchrotron emission are made. Our new estimate of the cosmic-ray positron spectrum is compared with the latest experimental data.']",['1997-06-03'] +1958,['eng'],"['Fuller, G M', 'Shi, X']",['Neutrino Production of Deuterium in Supermassive Stars and Possible Implications for Deuterium Detections in Ly-Limit Systems'],['Astrophysics and Astronomy'],"['astrophysics, matter', 'antineutrino/e, production', 'deuterium, density', 'helium, nuclide', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705256'],"['We describe how thermally produced anti-electron neutrinos ($\\bar\\nu_e$) from the homologously collapsing core of a supermassive star ($M \\ga 5\\times10^4 M_\\odot$) can lead to significant deuterium enrichment in the ejected envelope of such a star. Deuterium-enriched material at high redshift might then serve as a clue to the existence of pregalactic supermassive stars. Conceivably, the ejected deuterium-enriched material could intercept the line of sight to a distant QSO and mimic a Lyman limit absorber. In such a case, the deuterium abundance inferred from absorption lines might not reflect the true primordial abundance of deuterium. We discuss relevant theoretical uncertainties in supermassive star physics as well as potential observational signatures in Lyman $\\alpha$ absorber clouds for processing by stars of this kind.']",['1997-06-02'] +1959,['eng'],"['Glendenning, N K', 'Pei, S', 'Weber, F']",['Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down'],['Astrophysics and Astronomy'],"['nuclear matter', 'quark, matter', 'critical phenomena, confinement', 'astrophysics, pulsar', 'spin', 'angular momentum', 'magnetic field', 'radiation, electromagnetic', 'time dependence']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705235'],"['The conversion of nuclear matter to quark matter in the core of a rotating neutron star alters its moment of inertia. Hence the epoch over which conversion takes place will be signaled in the spin-down ""signal_prl.tex"" 581 lines, 22203 characters characteristics of pulsars. We find that an observable called the braking index should be easily measurable during the transition epoch and can have a value far removed (by orders of magnitude) from the canonical value of three expected for magnetic dipole radiation, and may have either sign. The duration of the transition epoch is governed by the slow loss of angular momentum to radiation and is further prolonged by the reduction in the moment of inertia caused by the phase change which can even introduce an era of spin-up. We estimate that about one in a hundred pulsars may be passing through this phase. The phenomenon is analogous to ``bachbending\'\' observed in the moment of inertia of rotating nuclei observed in the 1970\'s, which also signaled a change in internal structure with changing spin.']",['1997-05-30'] +1960,['eng'],"['Antoniadis, Ignatios', 'Mazur, P O', 'Mottola, E']","['Comment on ""Nongaussian Isocurvature Perturbations from Inflation""']",['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'cosmic radiation, background', 'invariance, conformal', 'field theory, scalar', 'two-point function']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705200'],"[""In a recent paper of Linde and Mukhanov, a hybrid inflationary model with nongaussian density perturbations and a ``blue'' spectral index n > 1 was presented. In this comment we point out that this model can be considered as a particular realization of the general framework for the spectrum and statistics of the CMBR we proposed in astro-ph/9611208, based on the hypothesis of conformal invariance. The implication of this hypothesis is that density perturbations are nongaussian with a spectral index n > 1.""]",['1997-05-27'] +1961,['eng'],"['De Laix, A A']",['Observing Long Cosmic Strings Through Gravitational Lensing'],['Astrophysics and Astronomy'],"['astrophysics, string', 'grand unified theory, critical phenomena', 'gravitation, lens', 'photon, scattering', 'energy, density', 'galaxy', 'quasar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705223'],"['We consider the gravitational lensing produced by long cosmic strings formed in a GUT scale phase transition. We derive a formula for the deflection of photons which pass near the strings that reduces to an integral over the light cone projection of the string configuration plus constant terms which are not important for lensing. Our strings are produced by performing numerical simulations of cosmic string networks in flat, Minkowski space ignoring the effects of cosmological expansion. These strings have more small scale structure than those from an expanding universe simulation - fractal dimension 1.3 for Minkowski versus 1.1 for expanding - but share the same qualitative features. Lensing simulations show that for both point-like and extended objects, strings produce patterns unlike more traditional lenses, and, in particluar, the kinks in strings tend to generate demagnified images which reside close to the string. Thus lensing acts as a probe of the small scale structure of a string. Estimates of lensing probablity suggest that for string energy densities consistant with string seeded structure formation, on the order of tens of string lenses should be observed in the Sloan Digital Sky Survey quasar catalog. We propose a search strategy in which string lenses would be identified in the SDSS quasar survey, and the string nature of the lens can be confirmed by the observation of nearby high redshift galaxies which are also be lensed by the string.']",['1997-05-29'] +1962,['eng'],"['Iida, K', 'Sato, K']",['Quantum Nucleation of Two-Flavor Quark Matter in Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'quark, matter', 'droplet, production', 'flavor, 2', 'tunneling', 'energy, electric', 'effect, screening', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705211'],"['Rates for nucleation of two-flavor quark matter in a neutron star core, originally composed of nuclear matter in $\\beta$ equilibrium, are calculated at zero temperature by a quantum tunneling analysis incorporating the electrostatic energy. We find that a nucleated droplet would develop into bulk matter due to electron screening effects.']",['1997-05-28'] +1963,['eng'],"['Kamionkowski, M P', 'Kosowsky, A']",['Detectability of Inflationary Gravitational Waves with Microwave Background Polarization'],['Astrophysics and Astronomy'],"['inflationary universe', 'gravitational radiation, measurement', 'background, stochastic', 'cosmic radiation, background', 'cosmic radiation, polarization', 'statistics', 'spectra, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705219'],"['Inflation predicts specific relations between the amplitudes and spectral indices of the primordial spectrum of density (scalar metric) perturbations and gravitational waves (tensor metric perturbations). Detection of a stochastic gravitational-wave background is essential for identifying this unmistakable signature. Polarization of the cosmic microwave background can isolate these tensor modes in a model-independent way and thereby circumvent the cosmic-variance limit to detecting a small tensor signal with only a temperature map. Here we assess the detectability of a gravity-wave background with a temperature and polarization map. For detector sensitivities better than $10-20 \\mu$K $\\sqrt{sec}$, the sensitivity to a tensor signal is always dominated by the polarization map. With a detector sensitivity of order $1 \\mu$K $\\sqrt{sec}$, polarization could improve on a temperature-map sensitivity to tensor modes by two to three orders of magnitude. Even a small amount of reionization substantially enhances tensor-mode detectability. We also argue that the sensitivity of the Planck Surveyor to tensor modes is significantly improved with polarization, even taking into account the resulting degradation of the intensity determination in the high-frequency channels.']",['1997-05-28'] +1964,['eng'],"['De van Bruck, C']",['Cosmic String Network Evolution in arbitrary Friedmann-Lemaître models'],['Astrophysics and Astronomy'],"['astrophysics, string', 'Friedman model', 'velocity, dependence', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705208'],['We use the velocity-dependent one-scale model by Martins & Shellard to investigate the evolution of a GUT long cosmic string network in arbitrary Friedmann-Lemaitre models. Four representative models are used to show that in general there is no scaling solution. The implications for structure formation are briefly discussed.'],['1997-05-27'] +1965,['eng'],"['Weber, F', 'Glendenning, N K', 'Pei, S']",['Signal for the Quark-Hadron Phase Transition in Rotating Hybrid Stars'],['Astrophysics and Astronomy'],"['talk, Jaipur 1997/03/17', 'astrophysics, matter', 'n, matter', 'critical phenomena, quark hadron', 'quark, matter', 'baryon number', 'astrophysics, pulsar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705202'],"[""For the past 20 years it had been thought that the coexistence phase of the confined hadronic and quark matter phases, assumed to be a first order transition, was strictly excluded from neutron stars. This, however, was due to a seemingly innocuous idealization which has approximated away important physics. The reason is that neutron stars constitute multi-component bodies rather than single-component ones formerly (and incorrectly) used to describe the deconfinement phase transition in neutron stars. So, contrary to earlier claims, `neutron' stars may very well contain quark matter in their cores surrounded by a mixed-phase region of quark and hadronic matter. Such objects are called hybrid stars. The structure of such stars as well as an observable signature that could signal the existence of quark matter in their cores are discussed in this paper.""]",['1997-05-27'] +1966,['eng'],"['Dedenko, L G', 'Furduev, A V', 'Karlik, Y S', 'Learned, J G', 'Mironovich, A A', 'Svet, V D', 'Zheleznykh, I M']",['Hydroacoustic Detection of Ultra-High Energy Cosmic Neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'deep underground detector, water', 'deep underground detector, acoustic', 'showers']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705189'],"['An attractive technique to explore for super-high-energy cosmic neutrino fluxes, via deep underwater acoustic detection, is discussed. Acoustic signals emitted by the neutrino induced cascades at large distances (10-50 km) from cascades are considered. It is argued that an existing hydroacoustic array of 2400 hydrophones, which is available in the Great Ocean near Kamchatka Peninsula, could be used as a base for an exploratory acoustic neutrino telescope SADCO (Sea Acoustic Detector of Cosmic Objects). The detection volume for registration of cascades with energies in the range of $10^{20-21} eV$ is estimated to be hundreds of cubic kilometers. Some models of extremely high energy elementary particle production in the Universe (for example the topological defect model) may be examined by such a detector. Tests of this technique are hoped for within a year.']",['1997-05-26'] +1967,['eng'],"['Spergel, D N', 'Zaldarriaga, M']",['CMB polarization as a direct test of Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, polarization', 'correlation function', 'temperature, fluctuation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705182'],"['We study the auto-correlation function of CMB polarization anisotropies and their cross correlation with temperature fluctuations as probe of the causal structure of the universe. Because polarization is generated at the last scattering surface, models in which fluctuations are causally produced on sub-horizon scales cannot generate correlations on scales larger then $\\sim 2^o$. Inflationary models, on the other hand, predict a peak in the correlation functions at these scales: its detection would be definitive evidence in favor of a period of inflation. This signal could be detected with the next generation of satellites.']",['1997-05-23'] +1968,['eng'],"['Stebbins, A J', 'Dodelson, S']",['On the Computation of CMBR Anisotropies from Simulations of Topological Defects'],['Astrophysics and Astronomy'],"['talk, Rome 1996/10/10', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'topology, defect', 'numerical methods']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705177'],['Techniques for computing the CMBR anisotropy from simulations of topological defects are discussed with an eye to getting as much information from a simulation as possible. Here we consider the practical details of which sums and multiplications to do and how many terms there are.'],['1997-05-22'] +1969,['eng'],"['Green, A M', 'Liddle, A R', 'Riotto, A']",['Primordial black hole constraints in cosmologies with early matter domination'],['Astrophysics and Astronomy'],"['astrophysics, model', 'field theory, moduli', 'black hole', 'density, perturbation', 'numerical calculations']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705166', 'http://www-lib.fnal.gov/archive/1997/pub/Pub-97-139-A.html']","['Moduli fields, a natural prediction of any supergravity and superstring-inspired supersymmetry theory, may lead to a prolonged period of matter domination in the early Universe. This can be observationally viable provided the moduli decay early enough to avoid harming nucleosynthesis. If primordial black holes form, they would be expected to do so before or during this matter dominated era. We examine the extent to which the standard primordial black hole constraints are weakened in such a cosmology. Permitted mass fractions of black holes at formation are of order $10^{-8}$, rather than the usual $10^{-20}$ or so. If the black holes form from density perturbations with a power-law spectrum, its spectral index is limited to $n \\lesssim 1.3$, rather than the $n \\lesssim 1.25$ obtained in the standard cosmology.']",['1997-05-22'] +1970,['eng'],"['Ricci, B', 'Berezinsky, Veniamin Sergeevich', ""Degl'Innocenti, S"", 'Dziembowski, W A', 'Fiorentini, G']",['Helioseismic constraints to the central solar temperature and neutrino fluxes'],['Astrophysics and Astronomy'],"['model, solar', 'temperature, solar', 'neutrino, solar', 'neutrino, flux', 'lower limit', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705164'],"['The central solar temperature T and its uncertainties are calculated in helioseismologically-constrained solar models. From the best fit to the convective radius, density at the convective radius and seismically determined helium abundance the central temperature is found to be T=1.58x10^7 K, in excellent agreement with Standard Solar Models. Conservatively, we estimate that the accuracy of this determination is Delta T/T=1.4 %, better than that in SSM. Neutrino fluxes are calculated. The lower limit to the boron neutrino flux, obtained with maximum reduction factors from all sources of uncertainties, is 2 sigma higher than the flux measured recently by SuperKamiokande.']",['1997-05-22'] +1971,['eng'],"['Matarrese, S', 'Mollerach, S']",['The stochastic gravitational-wave background produced by non-linear cosmological perturbations'],['Astrophysics and Astronomy'],"['talk, Valencia 1996/09/09', 'gravitational radiation', 'background, stochastic', 'density, perturbation', 'nonlinear', 'dependence, gauge']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705168'],"['The cosmological stochastic gravitational-wave background produced by the mildly non-linear evolution of density fluctuations is analyzed, in the frame of an Einstein-de Sitter model, by means of a fully relativistic perturbation expansion up to second order. The form of these gravitational-instability-induced gravitational waves is gauge-dependent. In the synchronous gauge, where the second-order expansion is most easily carried out, the transverse and traceless tensor modes which are produced also contain a Newtonian and post-Newtonian piece, whose interpretation as gravitational waves is non-trivial. A more direct physical understanding of this background is obtained in the so-called Poisson gauge, where it is seen to consist of a constant term plus an oscillating piece whose amplitude decays inside the Hubble radius.']",['1997-05-22'] +1972,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Bergström, L', 'Rubinstein, H R']",['50TeV HEGRA Sources and Infrared Radiation'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy', 'energy, density', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'cosmic radiation, background', 'photon, absorption', 'p nucleus, nuclear reaction', 'photon p, interaction', 'neutrino, flux', 'neutrino nucleon, interaction', 'charged current', 'muon, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705156'],"['The recent observations of 50 TeV gamma radiation by HEGRA have the potential of determining the extragalactic flux of infrared radiation. The fact that radiation is observed in the range between 30 and 100 TeV sets an upper limit on the infrared flux, while a cutoff at $E_{\\gamma} \\approx 50$ TeV fixes this flux with a good accuracy. If the intrinsic radiation is produced due to interaction of high energy protons with gas or low-energy target photons, then an accompaning high-energy neutrino flux is unavoidable. We calculate this flux and underground muon flux produced by it. The muon flux is dominated by muons with energies about 1 TeV and can be marginally detected by a 1 km$^2$ detector like an expanded AMANDA.']",['1997-05-21'] +1973,['eng'],"['Kawasaki, M', 'Kohri, K', 'Sato, K']",['Massive Decaying $\\tau$ Neutrino and Big Bang Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'neutrino/tau, massive', 'neutrino/tau, decay', 'neutrino/tau, lifetime', 'neutrino/tau, density', 'neutrino, flavor', 'scalar particle, annihilation', 'Boltzmann equation, solution', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705148'],['It has been pointed out by Hata et al. that the standard big bang nucleosynthes gives a poor fit to the primordial abundances of light elements inferred from observational data and the BBN predictions are consistent with observations if the effective number of neutrino species N_{\\nu} is about 2.1. We study the effect on BBN of an unstable massive $\\tau$ neutrino with mass 1-40 MeV and lifetime 10^{-4}-10^{3} sec and find that if 0.01 \\lesssim theoretical predictions agree with the observational data.'],['1997-05-21'] +1974,['eng'],"['Oberhummer, H', 'Ivanov, A N', 'Troitskaya, N I', 'Faber, M']",['On the solar neutrino problem in the relativistic field theory model of the deuteron'],['Astrophysics and Astronomy'],"['deuteron, model', 'field theory, relativistic', 'p p, fusion', 'cross section, fusion', 'effective Lagrangian', 'neutrino, solar', 'neutrino, flux', 'numerical calculations, interpretation of experiments', 'p p --> deuteron positron neutrino/e']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705119'],['The relativistic field theory model of the deuteron suggested by us previously is applied to the calculation of the reaction rate of the low-energy two-proton fusion p + p -> D + e+ + nu. The theoretical prediction of the reaction rate obtained is 2.9 times larger than given by the potential approach. This leads to a strong suppression of the high energy solar neutrino fluxes.'],['1997-05-19'] +1975,['eng'],"['Horowitz, C J', 'Li, G']",['Cumulative Parity Violation in Supernovae'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'parity, violation', 'neutrino, emission', 'magnetic field, high', 'n, matter', 'neutrino n, elastic scattering', 'n, polarization', 'multiple scattering', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705126'],"['Supernovae provide a unique opportunity for large scale parity violation because they are dominated by neutrinos. We calculate the parity violating asymmetry A of neutrino emission in a strong magnetic field. We assume the neutrinos elastically scatter many times from slightly polarized neutrons. Because of multple interactions, A grows with the optical thickness of the proto-neutron star and may be much larger than previous estimates. As a result, the neutron star could recoil at a significant velocity.']",['1997-05-19'] +1976,['eng'],"['Chardonnet, P', 'Orloff, J', 'Salati, Pierre']",['The Production of Anti-Matter in our Galaxy'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'cosmic radiation, antinucleus', 'antimatter, helium', 'baryon, asymmetry', 'antimatter, deuterium', 'p p, interaction', 'antinucleus, hadroproduction', 'cosmic radiation, flux', 'anti-p', 'coalescence', 'cross section, factorization', 'cosmic radiation, diffusion', 'antinucleus, density', 'numerical calculations, interpretation of experiments']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705110', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=capp98&id=salati']","['The discovery of a single anti-helium nucleus in the cosmic ray flux would definitely point toward the existence of stars and even of entire galaxies made of anti-matter. The presence of anti-nuclei in cosmic rays has actually profound implications on the fundamental question of the baryon asymmetry of the universe. It is therefore crucial to determine the amount of anti-matter which our own galaxy already produces through the spallation of high-energy protons on the interstellar gas of the galactic disk. We have used here a coalescence model to assess the amount of anti-deuterium and anti-helium 3 present in cosmic rays together with anti-protons. The propagation of cosmic rays in the galaxy is described through a two-zone diffusion model which correctly describes the observed abundances. We find that the antideuterium/proton ratio exceeds $10^{-9}$ above a momentum per anti-nucleon of about 4 GeV/c. Would the universe be purely made of matter, the AMS collaboration should be able to detect a few anti-deuterons during the space station stage of the experiment. However, the antihelium3/proton abundance does not exceed $4 10^{-13}$. Heavier anti-nuclei are even further suppressed.']",['1997-05-16'] +1977,['eng'],"['Vietri, M']",['GeV Photons from Ultra High Energy Cosmic Rays accelerated in $\\gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'synchrotron radiation', 'fireball', 'cosmic radiation, flux', 'model, shock waves', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705061'],"['Gamma-ray bursts are produced by the dissipation of the kinetic energy of a highly relativistic fireball, via the formation of a collisionless shock. When this happens, Ultra High Energy Cosmic Rays up to 10^20 eV are produced. I show in this paper that these particles produce, via synchrotron emission as they cross the acceleration region, photons up to 300 GeV which carry away a small, ~0.01, but non-negligible fraction of the total burst energy. I show that, when the shock occurs with the interstellar medium, the optical depth to photon-photon scattering, which might cause energy degradation of the photons, is small. The burst thusly produced would be detected at Earth simultaneoulsy with the parent gamma-ray burst, although its duration may differ significantly from that of the lower energy photons. The expected fluences, ~10^{-5}-10^{-6} erg/cm^2 are well within the range of planned detectors. A new explanation for the exceptional burst GRB 940217 is discussed.']",['1997-05-12'] +1978,['eng'],"['Nakamura, T', 'Sasaki, M', 'Tanaka, T', 'Thorne, K S']",['Gravitational Waves from Coalescing Black Hole MACHO Binaries'],['Astrophysics and Astronomy'],"['gravitational radiation, measurement', 'black hole, mass', 'counters and detectors, interference', 'astrophysics, missing-mass', 'gravitation, lens', 'MACHO', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9708060'],"[""If MACHOs are black holes of mass about 0.5 solar mass, they must have been formed in the early universe when the temperature was about 1 GeV. We estimate that in this case in our galaxy's halo out to about 50kpc there exist about half billion black hole binaries whose coalescence times are comparable to the age of the universe, so that the coalescence rate will be about five hundredth events/year/galaxy. This suggests that we can expect a few events/year within 15Mpc. The gravitational waves from such coalescing black hole MACHOs can be detected by the first generation of interferometers in the LIGO/VIRGO/TAMA/GEO network. Therefore, the existence of black hole MACHOs can be tested within the next five years by gravitational waves.""]",['1997-08-08'] +1979,['eng'],"['Calzetta, E A', 'Graña, M']",['Mode - mode coupling and primordial fluctuations'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, inflaton', 'coupling, effect', 'density, fluctuation', 'turbulence', 'fluid', 'space-time, de Sitter', 'field theory, nonlinear', 'transport theory', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705069'],"['We consider the influence of mode - mode coupling in the inflaton field on the spectrum of primordial fluctuations. To this end, we formulate a phenomenological model where the inflaton fluctuations are treated as a fluid undergoing turbulent motion. Under suitable assumptions, it is possible to estimate the size and scale of turbulent fluctuations in velocity, which upon reheating induce corresponding fluctuations in the radiation energy density. For De Sitter inflation the resulting spectrum is scale invariant on all scales of interest, in agreement with the expectation that scale invariance is a reflection of the symmetries of De Sitter space time independently of the underlying dynamics. The amplitude of the resulting spectrum is compatible with known observational limits. This suggests that the hypothesis of a extremely weakly coupled inflation could be relaxed without affecting the predictions of the model.']",['1997-05-12'] +1980,['eng'],"['De Rújula, Alvaro']",['Avatars of a Matter-Antimatter Universe'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1997/01/18', 'astrophysics', 'antimatter', 'cosmic radiation, flux', 'baryon, production', 'fluid, annihilation', 'cosmic radiation, background', 'particle source, galaxy', 'spectrometer, satellite', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705045'],"['An elegantly symmetric Universe, consisting of large islands of matter and antimatter, is by no means obviously out of the question. I review the observations that lead to the usual prejudice that the Universe contains only matter. I discuss recent work inferring that this prejudice can be converted into an inescapable conclusion. I argue that our theoretical conviction should not discourage direct searches for antimatter in cosmic rays.']",['1997-05-08'] +1981,['eng'],"['Bahcall, J N']",['Prioritizing Science'],['Astrophysics and Astronomy'],"['astrophysics', 'sociology', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704255'],['This article summarizes the process by which astronomers and astrophysicists reached a consensus view as to what are the highest priority scientific projects for the decade of the 1990s. I also review the remarkable success of these recommendations.'],['1997-04-28'] +1982,['eng'],"['Moorhouse, R G', 'Henriques, A B', 'Mendes, L E']",['Post-inflationary reheating and perturbations of the cosmic microwave background'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'Friedman model', 'space-time, Robertson-Walker', 'cosmic radiation, background', 'cosmic radiation, fluctuation', 'density, perturbation', 'gravitational radiation, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705016'],"['We formulate a gradual dynamical transition from a power-law inflation era with a scalar field to a radiation era with no scalar field including inhomogeneous perturbations to the Friedmann- Robertson-Walker universe. We show that for the cosmic microwave background radiation fluctuations this is excellently approximated by a sudden transition, with application of the Lichnerowicz conditions, both for density and gravitational wave perturbations.']",['1997-05-06'] +1983,['eng'],"['Balkanov, V A', 'Belolaptikov, I A', 'Bezrukov, L B', 'Borisovets, B A', 'Budnev, N M', 'Chensky, A G', 'Danilchenko, I A', 'Djilkibaev, Z A M', 'Dobrynin, V I', 'Domogatsky, G V', 'Doroshenko, A A', 'Fialkovsky, S V', 'Gaponenko, O N', 'Garus, A A', 'Ignatiev, S B', 'Karle, A', 'Klabukov, A M', 'Klimov, A I', 'Klimushin, S I', 'Koshechkin, A P', 'Kulepov, V F', 'Kuzmichev, L A', 'Lubsandorzhiev, B K', 'Mikolajski, T', 'Milenin, M B', 'Mirgazov, R R', 'Moroz, A V', 'Moseiko, N I', 'Nikiforov, S A', 'Osipova, E A', 'Panfilov, A I', 'Parfenov, Y V', 'Pavlov, A A', 'Petukhov, D P', 'Pokhil, P G', 'Pokolev, P A', 'Rozanov, M I', 'Rubzov, V Yu', 'Sokalski, I A', 'Spiering, C', 'Streicher, O', 'Tarashansky, V A', 'Thon, T', 'Volkov, D B', 'Wiebusch, C', 'Wischnewski, R']",['The Baikal Experiment'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1997/01/18', 'neutrino, cosmic radiation', 'muon, cosmic radiation', 'muon, flux', 'nucleon, decay', 'Rubakov effect', 'flux, magnetic monopole', 'Cherenkov counter, water', 'photoelectron, amplifier', 'track data analysis', 'deep underground detector, Baikal']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9705017'],"['We review the present status of the Baikal Neutrino Project. The construction and performance of the large deep underwater Cherenkov detector for muons and neutrinos, NT-200, which is currently under construction in Lake Baikal are described. Some results obtained with the first stages of NT-200 - NT-36 (1993-95), NT-72 (1995-96) and NT-96 (1996-97) - are presented, including the first clear neutrino candidates selected with 1994 and 1996 data.']",['1997-05-06'] +1984,['eng'],"['Meyer, J P', ""O'Connor-Drury, L"", 'Ellison, D C']","['Galactic Cosmic Rays from Supernova Remnants; 1, a Cosmic Ray Composition controlled by Volatility and Mass-to-Charge Ratio']",['Astrophysics and Astronomy'],"['cosmic radiation', 'galaxy', 'supernova', 'cosmic radiation, particle source', 'mass, dependence', 'charge, mass', 'astrophysics, model', 'cosmic radiation, acceleration', 'ionization, potential', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704267'],"['This is the first of a series of papers analysing the Galactic Cosmic Ray composition and origin. We show that the Galactic Cosmic Ray source (GCRS) composition is best described in terms of (i) a general enhancement of the refractory elements relative to the volatile ones, and (ii) among the volatile elements, an enhancement of the heavier elements relative to the lighter ones; this mass dependence most likely reflects a mass-to-charge (A/Q) dependence of the acceleration efficiency; among the refractory elements, there is NO such enhancement of heavier species, or only a much weaker one. We regard as coincidental the similarity between the GCRS composition and that of the solar corona, which is biased according to first ionization potential. In a companion paper, this GCRS composition is interpreted in terms of an acceleration by supernova shock waves of interstellar and/or circumstellar (eg Ne22 rich Wolf-Rayet wind) gas-phase and especially dust material.']",['1997-04-29'] +1985,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Vilenkin, A']",['Cosmic Necklaces and Ultrahigh Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['astrophysics, string', 'monopole, annihilation', 'p, cosmic radiation', 'p, flux', 'topology, defect', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704257'],"['Cosmic necklaces are hybrid topological defects consisting of monopoles and strings, with two strings attached to each monopole. We argue that the cosmological evolution of necklaces may significantly differ from that of cosmic strings. The typical velocity of necklaces can be much smaller than the speed of light, and the characteristic scale of the network much smaller than the horizon. We estimate the flux of high-energy protons produced by monopole annihilation in the decaying closed loops. For some reasonable values of the parameters it is comparable to the observed flux of ultrahigh-energy cosmic rays.']",['1997-04-28'] +1986,['eng'],"['Serna, A', 'Alimi, J M']",['Upper limit to $\\Omega_B$ in scalar-tensor gravity theories'],['Astrophysics and Astronomy'],"['astrophysics, model', 'gravitation, scalar', 'gravitation, tensor', 'baryon, density', 'upper limit', 'light nucleus, production', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704254'],"['In a previous paper (Serna & Alimi 1996), we have pointed out the existence of some particular scalar-tensor gravity theories able to relax the nucleosynthesis constraint on the cosmic baryonic density. In this paper, we present an exhaustive study of primordial nucleosynthesis in the framework of such theories taking into account the currently adopted observational constraints. We show that a wide class of them allows for a baryonic density very close to that needed for the universe closure. This class of theories converges soon enough towards General Relativity and, hence, is compatible with all solar-system and binary pulsar gravitational tests. In other words, we show that primordial nucleosynthesis does not always impose a very stringent bound on the baryon contribution to the density parameter.']",['1997-04-28'] +1987,['eng'],"['Green, A M', 'Liddle, A R']",['Constraints on the density perturbation spectrum from primordial black holes'],['Astrophysics and Astronomy'],"['black hole, production', 'density, perturbation', 'spectra, perturbation', 'black hole, mass', 'inflationary universe', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704251'],"[""We re-examine the constraints on the density perturbation spectrum, including its spectral index $n$, from the production of primordial black holes. The standard cosmology, where the Universe is radiation dominated from the end of inflation up until the recent past, was studied by Carr, Gilbert and Lidsey; we correct two errors in their derivation and find a significantly stronger constraint than they did, $n \\lesssim 1.25$ rather than their 1.5. We then consider an alternative cosmology in which a second period of inflation, known as thermal inflation and designed to solve additional relic over-density problems, occurs at a lower energy scale than the main inflationary period. In that case, the constraint weakens to $n \\lesssim 1.3$, and thermal inflation also leads to a `missing mass' range, $10^{18} g \\lesssim M \\lesssim 10^{26} g$, in which primordial black holes cannot form. Finally, we discuss the effect of allowing for the expected non-gaussianity in the density perturbations predicted by Bullock and Primack, which can weaken the constraints further by up to 0.05.""]",['1997-04-28'] +1988,['eng'],"['Schwarz, Dominik J', 'Schmid, C', 'Widerin, P']","[""Distortions of the Harrison-Zel'dovich spectrum from the QCD transition""]",['Astrophysics and Astronomy'],"['talk, Jaipur 1997/03/17', 'astrophysics, model', 'critical phenomena', 'quantum chromodynamics, effect', 'density, perturbation', 'spectra, fluctuation', 'black hole', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704250'],"[""We investigate the effect of the cosmological QCD transition on the evolution of primordial density perturbations. If the phase transition is first order, the sound speed vanishes during the transition and density perturbations fall freely. The Harrison-Zel'dovich spectrum of density fluctuations develops large peaks on scales below the Hubble radius at the transition. These peaks above the primordial spectrum grow with wavenumber and produce cold dark matter clumps of masses less than $10^{-10} M_\\odot$. At the horizon scale the amplification of overdensities is of order unity, and thus no $1 M_\\odot$ black hole production is possible for a COBE normalized scale-invariant spectrum.""]",['1997-04-28'] +1989,['eng'],"['Alam, J', 'Raha, S', 'Sinha, B']",['Quark Nuggets as Baryonic Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'baryon, matter', 'quark, matter', 'astrophysics, model', 'critical phenomena', 'baryon number', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704226'],"['The cosmic first order phase transition from quarks to hadrons, occurring a few microseconds after the Big Bang, would lead to the formation of quark nuggets which would be stable on a cosmological time scale, if the associated baryon number is larger than a critical value. We examine the possibility that these surviving quark nuggets may not only be viable candidates for cold dark matter but even close the universe.']",['1997-04-24'] +1990,['eng'],"['Seljak, Yu', 'Pen, U L', 'Turok, Neil G']",['Polarization of the Microwave Background in Defect Models'],['Astrophysics and Astronomy'],"['astrophysics, defect', 'cosmic radiation, background', 'microwaves', 'polarization', 'coherence, decoherence', 'energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704231'],"['We compute the polarization power spectra for global strings, monopoles, textures and nontopological textures, and compare them to inflationary models. We find that topological defect models predict a significant (1 microK) contribution to magnetic type polarization on degree angular scales, which is produced by the large vector component of the defect source. We also investigate the effect of decoherence on polarization. It leads to a smoothing of acoustic oscillations both in temperature and polarization power spectra and strongly suppresses the cross-correlation between temperature and polarization relative to inflationary models. Presence or absence of magnetic polarization or cross-correlation would be a strong discriminator between the two theories of structure formation and will be testable with the next generation of CMB satellites.']",['1997-04-24'] +1991,['eng'],"['Baym, G A', 'Heiselberg, H']",['The Electrical Conductivity in the Early Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'conductivity, electric', 'electroweak interaction, critical phenomena', 'quantum electrodynamics', 'finite temperature', 'transport theory', 'effect, screening', 'lepton, current', 'W, exchange', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704214'],"['We calculate the electrical conductivity in the early universe at temperatures below as well as above the electroweak vacuum scale, $T_c\\simeq 100$GeV. Debye and dynamical screening of electric and magnetic interactions leads to a finite conductivity, $\\sigma_{el}\\sim T/\\alpha\\ln(1/\\alpha)$, at temperatures well below $T_c$. At temperatures above, $W^\\pm$ charge-exchange processes -- analogous to color exchange through gluons in QCD -- effectively stop left-handed charged leptons. However, right-handed leptons can carry current, resulting in $\\sigma_{el}/T$ being only a factor $\\sim \\cos^4\\theta_W$ smaller than at temperatures below $T_c$.']",['1997-04-23'] +1992,['eng'],"['Lemoine, M', 'Sigl, G', 'Olinto, A V', 'Schramm, David N']",['Ultra-high energy cosmic ray sources and large scale magnetic fields'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'p, cosmic radiation', 'magnetic field', 'cosmic radiation, time delay', 'astrophysics, galaxy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704203'],"['Protons of energies up to 10**20 eV can be subject to significant deflection and energy dependent time delay in lage scale extragalactic or halo magnetic fields of strengths comparable to current upper limits. By performing 3-dimensional Monte Carlo simulations of nucleon propagation, we show how observations of arrival direction and time distributions can be used to measure the structure and strength of large-scale magnetic fields, and constrain the nature of the source of ultra-high energy cosmic rays.']",['1997-04-22'] +1993,['eng'],"['Sigl, G', 'Lemoine, M', 'Olinto, A V']",['Maximum Likelihood Analysis of Clusters of Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'energy spectrum', 'nucleon, cluster', 'astrophysics, particle source', 'magnetic field', 'cosmic radiation, time delay', 'showers, air', 'statistical analysis', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704204'],"['We present a numerical code designed to conduct a likelihood analysis for clusters of nucleons above 10**19 eV originating from discrete astrophysical sources such as powerful radio galaxies, gamma-ray bursts or topological defects. The code simulates the propagation of nucleons in a large-scale magnetic field and constructs the likelihood of a given observed event cluster as a function of the average time delay due to deflection in the magnetic field, the source activity time scale, the total fluence of the source, and the power law index of the particle injection spectrum. Other parameters such as the coherence length and the power spectrum of the magnetic field are also considered. We apply it to the three pairs of events above 4X10**19 eV recently reported by the Akeno Giant Air Shower Array (AGASA) experiment, assuming that these pairs were caused by nucleon primaries which originated from a common source. Although current data are too sparse to fully constrain each of the parameters considered, and/or to discriminate models of the origin of ultra-high energy cosmic rays, several tendencies are indicated. If the clustering suggested by AGASA is real, next generation experiments with their increased exposure should detect more than 10 particles per source over a few years and our method will put strong constraints on both the large-scale magnetic field parameters and the nature of these sources.']",['1997-04-22'] +1994,['eng'],"['Fargion, D']",['The role of $\\nu_{\\tau}$ ultrahigh energy astrophysics in $km^3$ detectors'],['Astrophysics and Astronomy'],"['neutrino/tau, search for', 'neutrino/tau, particle source', 'astrophysics', 'neutrino nucleon, interaction', 'tau, neutrinoproduction', 'tau, path length', 'muon, path length', 'energy dependence', 'antineutrino electron, interaction', 'antineutrino/e', 'antineutrino/tau, neutrinoproduction', 'channel cross section', 'numerical calculations', 'neutrino/tau nucleon --> tau anything', 'antineutrino/e electron --> tau antineutrino/tau', 'antineutrino/tau electron --> tau antineutrino/e']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704205'],"['We show that the expected $ \\nu_{\\tau} $ signals, by their secondary tau tracks, in Km^3 detectors at highest cosmic ray energy window $ 1.7\\cdot 10^{21} eV \\gt E_{\\tau} \\gt 1.6 x 10^{17} eV$, must overcome the corresponding $ \\nu_{\\mu} $ (or muonic) ones. Indeed, the Lorentz-boosted tau range length grows (linearly) above muon range, for $ E_{\\tau} \\RAISE 1.6 x 10^8 GeV$ and reaches its maxima extension, $ R_{\\tau_{\\max}} \\simeq 191 km$, at energy $E_{\\tau} \\simeq 3.8 x 10^9 GeV$. At this peak the tau range is nearly 20 times the corresponding muon range (at the same energy) implying a similar ratio in $ \\nu_{\\tau} $ over $ \\nu_{\\mu} $ detectability. This dominance, however may lead (at present most abundant $ \\nu_{\\tau} $ model fluxes) to just a rare spectacular event a year (if flavor mixing occurs). Lower energetic $ \\tau $ and $ \\nu_{\\tau} $ signals $ (\\bar{\\nu}_e e\\to 10^7 GeV$) may be more easily observed in km^3 detectors at a rate of a few $']",['1997-04-22'] +1995,['eng'],"['Mezzacappa, A']",['Simulations of Core Collapse Supernovae In One and Two Dimemsions Using Multigroup Neutrino Transport'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'astrophysics, supernova', 'neutrino, diffusion', 'Boltzmann equation', 'dimension, 1', 'dimension, 2', 'model, hydrodynamical', 'transport theory']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704181'],"['In one dimension, we present results from comparisons of stationary state multigroup flux-limited diffusion and Boltzmann neutrino transport, focusing on quantities central to the postbounce shock reheating. In two dimensions, we present results from simulations that couple one-dimensional multigroup flux-limited diffusion to two-dimensional PPM hydrodynamics.']",['1997-04-18'] +1996,['eng'],"['Dar, Arnon']",['The Afterglow of GRBs'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'neutrino, cosmic radiation', 'n, matter', 'jet, relativistic', 'time delay', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704187'],"['Models where relativistic jets from merger or accretion induced collapse in compact binary systems produce cosmological gamma ray bursts (GRBs) also predict that GRBs are accompanied by delayed emission of high energy photons, TeV neutrinos, X-rays, optical photons and radio waves. Their emission mechanisms are similar to those responsible for their emissions by blazars during gamma ray flares. The recently observed afterglow of GRB 970228 in X-rays and optical photons is well accounted by such models. In particular, the predicted power-law spectrum, time delay which is inversely proportional to frequency and a power-law decay with time which is energy independent, are all in excellent agreement with the observations.']",['1997-04-21'] +1997,['eng'],"['Cheng, K S', 'Dai, Z G']",['A New Model for Soft $\\gamma$-Ray Repeaters'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'matter, strangeness', 'vortex', 'flux tube, magnetic', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704110'],"['We consider a model in which the soft gamma-ray repeaters (SGRs) result from young, magnetized strange stars with superconducting cores. As such a strange star spins down, the quantized vortex lines move outward and drag the magnetic field tubes because of the strong coupling between them. Since the terminations of the tubes interact with the stellar crust, the dragged tubes can produce sufficient tension to crack the crust. Part of the broken platelet will be dragged into the quark core, which is only $10^4$ cm from the surface, leading to the deconfinement of crustal matter into strange quark matter and thus the release of energy. We will show that the burst energy, duration, time interval and spectrum for our model are in agreement with the observational results. The persistent X-ray emission from the SGRs can be well explained by our model.']",['1997-04-14'] +1998,['eng'],"['Baring, M G', 'Ellison, D C', 'Grenier, I']",['$\\gamma$-Rays from Supernova Remnants and the Signatures of Diffusive Shock Acceleration'],['Astrophysics and Astronomy'],"['talk, St. Malo 1996/09/16', 'astrophysics, supernova', 'photon, cosmic radiation', 'photon, emission', 'acceleration, shock waves', 'photon, flux', 'p, cosmic radiation', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704137'],"['While the definitive detection of gamma-rays from known supernova remnants (SNRs) remains elusive, the collection of unidentified EGRET sources that may be associated with SNRs has motivated recent modelling of TeV emission from these sources. Current theoretical models use power-law shock-accelerated protons and electrons in their predictions of expected gamma-ray TeV fluxes from those unidentified EGRET sources with remnant associations. In this paper, we explore a more detailed non-linear shock acceleration model, which generates non-thermal proton distributions and includes a self-consistent determination of shock hydrodynamics. We obtain gamma-ray spectra for SNRs allowing for the cessation of acceleration to high energies that is due to the finite ages and sizes of remnants. Gamma-ray spectral cutoffs can be observed in the TeV range for reasonable remnant parameters, and deviations from power-law behaviour are found at all energies ranging from 1 MeV up to the cutoff. Correlated observations by INTEGRAL, Whipple and other instruments may provide stringent constraints to our understanding of supernova remnants.']",['1997-04-16'] +1999,['eng'],"['Allen, B', 'Caldwell, R R', 'Dodelson, S', 'Knox, L', 'Shellard, E P S', 'Stebbins, A J']","[""CMB Anisotropy Induced by Cosmic Strings on Angular Scales $\\geq{'}$""]",['Astrophysics and Astronomy'],"['astrophysics, string', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704160'],"[""We have computed an estimate of the angular power spectrum of the Cosmic Microwave Background (CMB) induced by cosmic strings on angular scales $>~ 15'$, using a numerical simulation of a cosmic string network; and decomposed this pattern into scalar, vector, and tensor parts. We find no evidence for strong acoustic oscillations in the scalar anisotropy but rather a broad peak. The anisotropies from vector modes dominate except on very small angular scales while the tensor anisotropies are sub-dominant on all angular scales. The anisotropies generated after recombination are even more important than in adiabatic models. We expect that these qualitative features are robust to the varying of cosmological parameters, a study which has not yet been done.""]",['1997-04-17'] +2000,['eng'],"['Cheng, K S', 'Dai, Z G']",['Gravitational Waves from Phase Transition of Accreting Neutron Stars'],['Astrophysics and Astronomy'],"['gravitational radiation', 'n, matter', 'critical phenomena', 'astrophysics, pulsar', 'K, condensation', 'matter, strangeness', 'model, oscillation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704161'],"['We propose that when neutron stars in low-mass X-ray binaries accrete sufficient mass and become millisecond pulsars, the interiors of these stars may undergo phase transitions, which excite stellar radial oscillations. We show that the radial oscillations will be mainly damped by gravitational-wave radiation instead of internal viscosity. The gravitational waves can be detected by the advanced Laser Interferometer Gravitational-Wave Observatory at a rate of about three events per year.']",['1997-04-17'] +2001,['eng'],"['Pen, U L', 'Seljak, Yu', 'Turok, Neil G']",['Power Spectra in Global Defect Theories of Cosmic Structure Formation'],['Astrophysics and Astronomy'],"['astrophysics, texture', 'topology, defect', 'spectra, perturbation', 'correlation function', 'cosmic radiation, anisotropy', 'magnetic monopole', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704165'],"['An efficient technique for computing perturbation power spectra in field ordering theories of cosmic structure formation is introduced, enabling computations to be carried out with unprecedented precision. Large scale simulations are used to measure unequal time correlators of the source stress energy, taking advantage of scaling during matter and radiation domination, and causality, to make optimal use of the available dynamic range. The correlators are then re-expressed in terms of a sum of eigenvector products, a representation which we argue is optimal, enabling the computation of the final power spectra to be performed at high accuracy. Microwave anisotropy and matter perturbation power spectra for global strings, monopoles, textures and non-topological textures are presented and compared with recent observations.']",['1997-04-17'] +2002,['eng'],"['Salamon, M H', 'Stecker, F W']",['Absorption of High Energy $\\gamma$ Rays by Interactions With Starlight Photons in Extragalactic Space at High Redshifts and the High Energy $\\gamma$-Ray Background'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, absorption', 'photon photon, interaction', 'cosmic radiation, background', 'energy spectrum', 'neutralino, annihilation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704166'],"['We calculate the absorption of 10-500 GeV gamma-rays at high redshifts. This calculation requires the determination of the high-redshift evolution of the intergalactic starlight photon field, including its IR-UV spectral energy distribution. To estimate this evolution, we have followed a recent analysis of Fall, Charlot and Pei which gives results consistent with recent data. We give our results for the gamma-ray opacity as a function of redshift out to a redshift of 3. We also give predicted gamma-ray spectra for selected blazars and give an extragalactic unresolved blazar background spectrum up to 500 GeV. Our results indicate that this background should steepen significantly above 20 GeV owing to intergalactic absorption. Future observations of this steepening would provide a test for the blazar background origin hypothesis. We have used our results to discuss upper limits on the redshifts of gamma-ray bursts. We note that the 17 Feb. 1994 burst observed by EGRET must have originated at a redshift less than 2. We also use our estimates of the background to determine the observability of multi-GeV gamma-ray lines from the annihilation of supersymmetric dark matter particles in the galactic halo.']",['1997-04-17'] +2003,['eng'],"['Birkel, M', 'Toldrà, R']",['On Pulsar Velocities from Neutrino Oscillations'],['Astrophysics and Astronomy'],"['neutrino, oscillation', 'effect, magnetic', 'n, matter', 'velocity, pulsar', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704138'],"['It has been recently suggested that magnetically affected neutrino oscillations inside a cooling protoneutron star, created in a supernova explosion, could explain the large proper motion of pulsars. We investigate whether this hypothesis is in agreement with the observed properties of pulsars and find that present data disfavor the suggested mechanism.']",['1997-04-16'] +2004,['eng'],"['Sornborger, A T', 'Brandenberger, R H', 'Fryxell, B', 'Olson, K']",['The Structure of Cosmic String Wakes (Proceedings)'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'astrophysics, string', 'gravitation, perturbation', 'model, hydrodynamical', 'baryon, matter', 'astrophysics, missing-mass']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704145'],"['We present results of a cosmological hydrodynamical study of gravitational accretion in cosmic string wakes and filaments. Cosmic string wakes are formed by fast moving (v ~ c) strings. A conical deficit angle in the string spacetime induces a velocity perturbation in the background matter and a two-dimensional wake accretes in the path of the string. Filaments are formed by slow moving strings with a large amount of small scale structure. The major gravitational perturbation from slow moving strings is due to the Newtonian field induced by the effective mass of the wiggles. In cosmic string wakes, cool streams of baryons collide and are trapped at the center of the wake causing an enhancement of baryons versus dark matter by a factor of 2.4. In filaments, a high pressure is induced at the filament core and baryonic matter is expelled leading to a baryon deficit in the center of the filament.']",['1997-04-16'] +2005,['eng'],"['De Pacheco, J A F', 'Horváth, J E']",['Gravitational Wave Emission from Galactic Radio Pulsars'],['Astrophysics and Astronomy'],"['gravitational radiation, emission', 'astrophysics, pulsar', 'statistics', 'counters and detectors', 'interference', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704155'],"['We consider in this work continuous gravitational wave (GW) emission from non-axisymmetric radio pulsars. We treat in some detail the observational issues related to the known radio pulsar sample with the aim of unveiling the actual number of sources contributing to GW, which are likely to be the main contributors of GWs. It is shown that the operation of spheroidal GW detectors and full-size interferometers could detect this component of the radiation or impose useful limits on the effective oblateness of young radio pulsars.']",['1997-04-16'] +2006,['eng'],"['Gurevich, A V', 'Zybin, K P']",['$\\gamma$ radiation by Neutralino Stars'],['Astrophysics and Astronomy'],"['neutralino, matter', 'neutralino, annihilation', 'annihilation, neutralino', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'flux, cosmic radiation', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704122'],"['A new model of gamma radiation (GR) generated by neutralino annihilation in neutralino stars (NeS) is proposed. Diffuse Galactic and extragalactic GR is calculated for this model and is shown to be in a reasonable agreement with observations. The point source component (P) is picked out among nonidentified discrete gamma sources from EGRET catalog. This component is shown to be distributed isotropically and homogeneously, as it should be for NeS. Gamma radiation from significant part of P-sources is supposed to be the direct radiation from individual NeS. This supposition is shown to be in agreement with observations. The comparison of the theory with observed GR gives a possibility to establish some important features of CDM particle.']",['1997-04-15'] +2007,['eng'],"['Sciama, D W']",['Decaying Neutrinos and the Flattening of the Galactic Halo'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'neutrino, decay', 'neutrino, lifetime', 'neutrino, density', 'ionization', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704081'],"['The recently constructed Dehnen-Binney set of mass models for the Galaxy is used to show that the decaying neutrino theory for the ionisation of the interstellar medium (Sciama 1990a, 1993) requires the neutrino halo of the Galaxy to be as flattened as is observationally permitted (axial ratio q=0.2 or shape E8). The argument involves an evaluation of the contribution of red-shifted decay photons from the cosmological distribution of neutrinos to the extragalactic diffuse background at 1500 Angstroms. This contribution must be as large as is observationally permitted. These two requirements depend on the decay lifetime in potentially conflicting ways. For consistency to be achieved the lifetime must lie within 30 per cent of 10^23 seconds.']",['1997-04-11'] +2008,['eng'],"['Kinney, W H', 'Kolb, E W', 'Turner, M S']",['Ribbons on the CBR Sky'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'baryon, symmetry', 'antimatter', 'matter, annihilation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704070'],"['If the Universe consists of domains of matter and antimatter, annihilations at domain interfaces leave a distinctive imprint on the Cosmic Background Radiation (CBR) sky. The signature is anisotropies in the form of long, thin ribbons of width $\\theta_W\\sim 0.15^\\circ $, separated by angle $\\theta_L\\simeq 1^\\circ(L/100h^{-1} Mpc)$ where $L$ is the characteristic domain size, and $y$-distortion parameter $y \\simeq 2.5 \\times 10^{-6}$. Such a pattern could be detected by the high-resolution CBR anisotropy experiments planned for the next decade, and such experiments should finally settle the question of whether or not our Hubble volume is baryon symmetric.']",['1997-04-10'] +2009,['eng'],"['Frichter, G M', 'Gaisser, T K', 'Stanev, T']",['Inelasticity in p-nucleus collisions and its application to high energy cosmic-ray cascades'],['Astrophysics and Astronomy'],"['p nucleus, nuclear reaction', 'p nucleus, inclusive reaction', 'p, emission', 'multiple scattering, model', 'p p, inclusive reaction', 'differential cross section, x-dependence', 'model, cascade', 'cosmic radiation', 'showers, air', 'numerical calculations, interpretation of experiments', '100-200 GeV/c']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704061'],['We employ a simple multiple scattering model to investigate the inclusive reaction p + A --> p + X for projectile momenta in the 100-200 GeV/c range. We find that data are consistent with a class of interaction models in which the stopping power of nuclei is rather low. We discuss extrapolation to ultra-high energy and the application to interpretation of cosmic-ray air showers at energies up to 10^20 eV.'],['1997-04-08'] +2010,['eng'],"['Turner, M S']",['Ten Things Everyone Should Know About Inflation'],['Astrophysics and Astronomy'],"['lectures', 'inflationary universe', 'astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation', 'vacuum state, fluctuation', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704062'],['These lecture notes are organized into ten lessons that summarize the status of inflationary cosmology.'],['1997-04-08'] +2011,['eng'],"['Prokhorov, M E', 'Lipunov, V M', 'Postnov, K A']",['Merging Rates of Compact Binaries in the Universe'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1997/01/18', 'gravitational radiation', 'counters and detectors', 'interference, laser', 'n, matter', 'black hole', 'photon, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704039'],['Merging rates of compact binaries (double neutron stars or black holes) are calculated based on the modern concept of binary stellar evolution. It is found that the initial laser interferometers with an rms-sensitivity of $10^{-21}$ at the frequency 100 Hz can detect 10-700 black holes and only \\sim 1 neutron star coalescences in a 1-year integration time. Implications of the evolutionary effects to the cosmological origin of GRB are also discussed.'],['1997-04-04'] +2012,['eng'],"['Turner, M S']",['Inflationary Cosmology'],['Astrophysics and Astronomy'],"['talk, Copenhagen 1996/01/10', 'inflationary universe', 'astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704040'],['Inflation is a bold and expansive extension of the Standard Cosmology. It holds the promise to extend our understanding of the Universe to within 10^{-32}sec of the big bang and answer most of the pressing questions in cosmology. Its boldest assertion is that all the structure observed in the Universe today arose from quantum-mechanical fluctuations on subatomic scales. A flood of cosmological observations and laboratory experiments are testing inflation and within five years we should know whether inflation is to become part of a new standard cosmology.'],['1997-04-04'] +2013,['eng'],"['Zas, E']",['The Highest Energy Neutrinos'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1997/01/18', 'neutrino, cosmic radiation', 'neutrino, particle source', 'neutrino, flux', 'astrophysics', 'black hole', 'annihilation, WIMP', 'shower detector', 'deep underground detector', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704016'],['Some neutrino predictions at the highest energies for a number of production mechanisms are comparatively reviewed in the light of future projects for neutrino detection.'],['1997-04-03'] +2014,['eng'],"['Halzen, Francis']",['The Search for the Source of the Highest Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Faro 1996/09/08', 'photon, cosmic radiation', 'particle source, galaxy', 'p, acceleration', 'pi, decay', 'neutrino, flux', 'photon, flux', 'neutrino/mu, measurement', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704020'],"['Active galaxies and gamma ray bursts are the sources of the highest energy photons detected by astronomical telescopes. We speculate that they may be the sources of the highest energy cosmic rays. This makes them true proton accelerators, where the highest energy photons are the decay products of neutral pions photoproduced when the proton beams interacts with ambient radiation. Neutrinos from the decay of charged pions represent an incontrovertible signature for proton acceleration. A main theme of this talk is that their fluxes can be estimated from the measured gamma ray luminosity by model-independent methods, based on dimensional analysis and textbook particle physics.']",['1997-04-03'] +2015,['eng'],"['Turner, M S']",['Cosmology 1996'],['Astrophysics and Astronomy'],"['talk, Tsukuba 1996/10/29', 'astrophysics, model', 'inflationary universe', 'astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments', 'talk, Notre Dame 1996/06/20']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9704024'],['The current state of cosmology is easy to summarize: a very successful standard model -- the hot big-bang cosmology -- that accounts for the evolution of the Universe from 10^{-2} sec until the present; bold ideas based upon early-Universe physics -- foremost among them inflation and cold dark matter -- that can extend the standard cosmology to times as early as 10^{-32} sec and address the most pressing questions; and a flood of observations -- from determinations of the Hubble constant to measurements of CBR anisotropy -- that are testing inflation and cold dark matter.'],['1997-04-03'] +2016,['eng'],"['Vilenkin, A']",['Topological defects and open inflation'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'topology, defect', 'field equations, monopole', 'string model', 'gravitation, lens', 'bubble, production']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703201'],['Topological defects can naturally be formed soon after bubble nucleation in the open inflation scenario. The defects are not completely diluted away by the subsequent period of inflation in the bubble interior and can produce observable large-scale microwave background anisotropies. Superheavy strings and monopoles attached to the strings can act as gravitational lenses with angular separation between the images of up to an arc minute.'],['1997-04-01'] +2017,['eng'],"['Turner, M S']",['Cosmology'],['Astrophysics and Astronomy'],"['talk, Beijing 1995/08/10', 'astrophysics, model', 'inflationary universe', 'astrophysics, missing-mass', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703197'],"['Cosmology is very exciting for three reasons. There is a very successful standard model -- the hot big bang -- which describes the evolution of the Universe from 10^{-2} sec onward. There are bold ideas, foremost among them are inflation and cold dark matter, which can extend the standard cosmology to within 10^{-32} sec of the bang and address some of the most fundamental questions in cosmology. There is a flood of data -- from determinations of the Hubble constant to measurements of CBR anisotropy -- that are testing inflation and cold dark matter.']",['1997-04-01'] +2018,['eng'],"['Barwick, S W', 'Schneider, E', 'Beatty, J J', 'De Nolfo, G A', 'Bhattacharya, A', 'Bower, C', 'Musser, J A', 'Chaput, C J', 'Coutu, S', 'McKee, S', 'Tarlé, G', 'Tomasch, A D', 'Knapp, J', 'Lowder, D M', 'Müller, D', 'Swordy, S P', 'Torbet, E', 'Nutter, S L']",['Measurements of the Cosmic-Ray Positron Fraction From 1 to 50 GeV'],['Astrophysics and Astronomy'],"['positron, cosmic radiation', 'yield, (positron electron)', 'energy dependence', 'counters and detectors, satellite', 'experimental results', '1-50 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703192'],"[""Two measurements of the cosmic-ray positron fraction as a function of energy have been made using the High Energy Antimatter Telescope (HEAT) balloon-borne instrument. The first flight took place from Ft. Sumner, New Mexico in 1994, and yielded results above the geomagnetic cutoff energy of 4.5 GeV. The second flight from Lynn Lake, Manitoba in 1995 permitted measurements over a larger energy interval, from 1 GeV to 50 GeV. In this letter we present results on the positron fraction based on data from the Lynn Lake flight, and compare these with the previously published results from the Ft. Sumner flight. The results confirm that the positron fraction does not increase with energy above ~10 GeV, although a small excess above purely secondary production cannot be ruled out. At low energies the positron fraction is slightly larger than that reported from measurements made in the 1960's. This effect could possibly be a consequence of charge dependence in the level of solar modulation.""]",['1997-03-31'] +2019,['eng'],"['Turner, M S']",['The Cosmology of Nothing'],['Astrophysics and Astronomy'],"['lectures', 'astrophysics, model', 'vacuum state, energy', 'inflationary universe', 'matter, density', 'cosmic radiation, background', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703195'],"[""For more seventy years physicists have appreciated that Nature's vacuum is far from empty. The discovery of the Lamb shift in Hydrogen provided dramatic verification of the reality of the quantum vacuum. The advent of gauge theories has led us to believe that the physics of the vacuum is even richer, with the possibility of instantons, vacuum phase transitions, vacuum defects (monopoles, domain walls, cosmic strings and nontopological solitons), vacuum energy, and degenerate vacua states (with different local realizations of the laws of physics). Cosmology offers a unique laboratory for exploring the ``physics of nothing.'' In this lecture I focus on the implications of vacuum energy for cosmology -- in particular, inflation -- and discuss the flood of observations that are testing the inflationary paradigm and in process probing the physics of nothing. I also discuss the possibility that today vacuum energy plays a dynamically important role (as a cosmological constant).""]",['1997-03-31'] +2020,['eng'],"['Turner, M S']",['Cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'inflationary universe', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703174'],"['The Hubble constant sets the size and age of the Universe, and, together with independent determinations of the age, provides a consistency check of the standard cosmology. The Hubble constant also provides an important test of our most attractive paradigm for extending the standard cosmology, inflation and cold dark matter.']",['1997-03-27'] +2021,['eng'],"['Kampert, K H']",['First Results from the KASCADE Experiment'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1997/01/18', 'elements, cosmic radiation', 'energy spectrum', 'showers, air', 'electromagnetic component', 'hadronic component', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703182'],"['A new extensive air shower (EAS) experiment has been installed at the laboratory site of the Forschungszentrum Karlsruhe. The major goal of the experiment is to determine the chemical composition in the energy range around and above the knee of the primary cosmic ray spectrum. An important advantage of the installation is the capability to simultaneously measure the electromagnetic, muonic and hadronic components of EAS event-by-event, thereby reducing systematic uncertainties to a large extend. Data taking with a large part of the experiment has started at the end of 1995 with further installations continuing during 1996. First preliminary results are presented.']",['1997-03-28'] +2022,['eng'],"['Turner, M S']",['The Case for $\\Lambda$CDM'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'astrophysics, fundamental constant', 'matter, density', 'astrophysics, model', 'Hubble constant', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703161'],"['The case is simple: there is no compelling theoretical argument against a cosmological constant and $\\Lambda$CDM is the only CDM model that is consistent with all present observations. $\\Lambda$CDM has two noteworthy features: it can be falsified in the near future (the prediction $q_0\\sim -1/2$ is an especially good test), and, if correct, it has important implications for fundamental physics.']",['1997-03-26'] +2023,['eng'],"['Drago, A', 'Tambini, U']",['Finite Temperature Quark Matter and Supernova Explosion'],['Astrophysics and Astronomy'],"['quark, matter', 'finite temperature', 'model, confinement', 'astrophysics, supernova', 'n, matter', 'critical phenomena', 'binding energy', 'color, dielectric', 'neutrino, emission', 'thermodynamics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703138'],"['We study the equation of state of quark matter at finite temperature, using a confinement model in which chiral symmetry remains broken in the deconfined phase. Implications for type II supernova explosion and for the structure and evolution of the proto-neutron star are discussed.']",['1997-03-24'] +2024,['eng'],"['Nesteruk, A', 'Maartens, R', 'Gunzig, E']",['A self-consistent inflationary cosmology'],['Astrophysics and Astronomy'],"['inflationary universe', 'vacuum state, decay', 'radiation, production', 'entropy', 'field equations, solution', 'thermodynamics']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703137'],"['We present a simple, exact and self-consistent cosmology with a phenomenological model of quantum creation of radiation due to vacuum decay. The decay drives a non-isentropic inflationary era, which exits smoothly to the radiation era, without reheating. The initial vacuum for radiation is a regular Minkowski vacuum. The created radiation obeys standard thermodynamic laws, and the total entropy produced is consistent with the accepted value.']",['1997-03-24'] +2025,['eng'],"['Chung, D J H', 'Farrar, Glennys R S', 'Kolb, E W']",['On the relic abundance of light photinos'],['Astrophysics and Astronomy'],"['scattering, photino pi', 'bound state, (gluon gluino)', 'bound state, mass', 'lifetime', 'Boltzmann equation, solution', 'pi', 'mass, photino', 'symmetry, crossing', 'effective Lagrangian', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703145'],"[""We solve the coupled Boltzmann equation for the system of light photinos interacting with pions and $R^0$'s (the gluon-gluino bound state) to determine the relic abundance of light photinos in the light gaugino scenario. Cosmology bounds the ratio r of the R^0 mass to the photino mass to be less than about 1.8. We also use a model Lagrangian embodying crossing symmetry between the $R^0 \\leftrightarrow \\photino \\pi \\pi$ and $R^0 \\pi \\leftrightarrow \\photino a function of $R^0$ and photino masses.""]",['1997-03-24'] +2026,['eng'],"['Kolb, E W', 'Riotto, A', 'Tkachev, Igor I']",['Evolution of the Order Parameter after Bubble Collisions'],['Astrophysics and Astronomy'],"['scattering, bubble', 'critical phenomena', 'time dependence', 'thermodynamics, fluctuation', 'electroweak interaction', 'baryon, production', 'field theory, scalar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703119'],"['If a first-order phase transition is terminated by collisions of new-phase bubbles, there will exist a period of nonequilibrium between the time bubbles collide and the time thermal equilibrium is established. We study the behavior of the order parameter during this phase. We find that large nonthermal fluctuations at this stage tend to restore symmetry, i.e., the order parameter is smaller than its eventual thermal equilibrium value. We comment on possible consequences for electroweak baryogenesis.']",['1997-03-19'] +2027,['eng'],"['López, R E', 'Turner, M S', 'Gyuk, G']",['Effect of Finite Mass on Primordial Nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'nucleon, mass', 'mass, correction', 'weak interaction', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703065'],"['We have calculated the small effect of finite nucleon mass on the weak-interaction rates that interconvert protons and neutrons in the early Universe. We have modified the standard code for primordial nucleosynthesis to include these corrections and find a small, systematic increase in the 4He yield, $\\delta Y / Y \\simeq (0.47 - 0.50)% $, depending slightly on the baryon-to-photon ratio. The fractional changes in the abundances of the other light elements are a few percent or less for interesting values of the baryon-to-photon ratio.']",['1997-03-12'] +2028,['eng'],"['Bandyopadhyay, D', 'Pal, S', 'Chakrabarti, S']",['The quantizing magnetic field and quark-hadron phase transition in a neutron star'],['Astrophysics and Astronomy'],"['n, matter', 'critical phenomena, quark hadron', 'magnetic field, high', 'gluon, exchange', 'Hartree-Fock approximation', 'baryon, density', 'phase space', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703066'],"['We investigate the influence of a strong magnetic field on various properties of neutron stars with quark-hadron phase transition. The one-gluon exchange contribution in a magnetic field is calculated in a relativistic Dirac-Hartree-Fock approach. In a magnetic field $B_m \\sim 10^{19}$G, the phase spaces of electrons, u and d quarks are strongly modified. This shifts the onset of phase transition to lower baryon density and also reduces the extent of mixed phase. As a result the overall equation of state is softer in comparison to the field-free case. The abundances of electrons and u quark are considerably enhanced in the mixed phase in presence of the magnetic field.']",['1997-03-12'] +2029,['eng'],"['Sciama, D W']",['An updated precision estimate of the Hubble constant and the age and density of the Universe in the decaying neutrino theory'],['Astrophysics and Astronomy'],"['astrophysics, model', 'matter, density', 'neutrino, decay', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703068'],"['We here update the derivation of precise values for the Hubble constant H_0, the age t_0 and the density parameter Omega*h^2 of the universe in the decaying neutrino theory for the ionisation of the interstellar medium (Sciama 1990 a, 1993). Using recent measurements of the temperature of the cosmic microwave background, of the abundances of D, He^4 and Li^7, and of the intergalactic hydrogen-ionising photon flux at zero red shift, we obtain for the density parameter of the universe Omega*h^2=0.300\\pm 0.003. Observed limits on H_0 and t_0 then imply that, for a zero cosmological constant, H_0=52.5\\pm 2.5 km. sec^{-1} Mpc^{-1}, t_0=12.7\\pm 0.7 Gyr and Omega=1.1\\pm 0.1. If Omega=1 exactly, then H_0=54.8\\pm 0.3 km. sec^{-1} Mpc^{-1}, and t_0=11.96\\pm 0.06 Gyr. These precise predictions of the decaying neutrino theory are compatible with current observational estimates of these quantities.']",['1997-03-12'] +2030,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Martin, X', 'Vilenkin, A']",['High energy particles from monopoles connected by strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'monopole, pair production', 'gauge boson, massive', 'gauge boson, massless', 'gauge boson, radiation', 'radiation, spectra', 'gluon, emission', 'hadron, production', 'hadron, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703077'],"['Monopole-antimonopole pairs connected by strings and monopole-string networks with $N>2$ strings attached to each monopole can be formed at phase transitions in the early universe. In such hybrid defects, monopoles accelerate under the string tension and can reach ultrarelativistic Lorentz factors, $\\gamma\\gg 1$. We study the radiation of gauge quanta by accelerating monopoles. For monopoles with a chromomagnetic charge, we also discuss the high-energy hadron production through emission of virtual gluons and their subsequent fragmentation into hadrons. The relevant parameter for gauge boson radiation is $M/a$, where $M$ is the boson mass and $a$ is the proper acceleration of the monopole. For $M\\ll a$, the gauge bosons can be considered as massless and the typical energy of the emitted quanta is $E\\sim\\gamma a$. In the opposite limit, $M\\gg a$, the radiation power is exponentially suppressed and gauge quanta are emitted with a typical energy $E\\sim\\gamma M$ in a narrow range $\\Delta E/E\\sim (a/M)^{1/2}$. Cosmological monopole-string networks can produce photons and hadrons of extremely high energies. For a wide range of parameters these energies can be much greater than the Planck scale.']",['1997-03-12'] +2031,['eng'],"['Sigl, G']",['Nucleon Spin Fluctuations and Neutrino-Nucleon Energy Transfer in Supernovae'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'nuclear matter, temperature', 'weak interaction', 'nucleon, spin', 'spin, fluctuation', 'neutrino nucleon, interaction', 'spin, density', 'structure function', 'nucleon nucleon, interaction', 'Born approximation', 'nucleon, bremsstrahlung', 'wave function, (2nucleon)', 'exchange, one-pion', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703056'],"['The formation of neutrino spectra in a supernova depends crucially on strength and inelasticity of weak interactions in hot nuclear matter. Neutrino interactions with nonrelativistic nucleons are mainly governed by the dynamical structure function for the nucleon spin density which describes its fluctuations. It has recently been shown that these fluctuations give rise to a new mode of energy transfer between neutrinos and nucleons which inside the neutrinosphere is of comparable or greater importance than ordinary recoil. We calculate numerically the spin density structure function in the limit of a dilute, non-degenerate medium from exact two-nucleon wave functions for some representative nuclear interaction potentials. We show that spectrum and magnitude of the energy transfer can deviate significantly from those based on the Born approximation. They are, however, rather insensitive to the particular nuclear potential as long as it reproduces experimental nucleon scattering phase shifts at energies up to a few tens of MeV. We also compare with calculations based on a one-pion exchange potential in Born approximation and briefly comment on their applicability near the center of a supernova core. Our study is relevant for numerical simulations of the neutrino spectra emerging from type-II supernovae.']",['1997-03-11'] +2032,['eng'],"['Borione, A', 'Catanese, M', 'Chantell, M C', 'Covault, C E', 'Cronin, J W', 'Fick, B E', 'Fortson, Lucy F', 'Fowler, J', 'Glasmacher, M A K', 'Green, K D', 'Kieda, D B', 'Matthews, J', 'Newport, B J', 'Nitz, D', 'Ong, R A', 'Oser, S M', 'Sinclair, D', 'Van der Velde, J C']",['Constraints on $\\gamma$-ray Emission from the Galactic Plane at 300 TeV'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'showers, air', 'muon, flux', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'counters and detectors, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703063'],"['We describe a new search for diffuse ultrahigh energy gamma-ray emission associated with molecular clouds in the galactic disk. The Chicago Air Shower Array (CASA), operating in coincidence with the Michigan muon array (MIA), has recorded over 2.2 x 10^{9} air showers from April 4, 1990 to October 7, 1995. We search for gamma rays based upon the muon content of air showers arriving from the direction of the galactic plane. We find no significant evidence for diffuse gamma-ray emission, and we set an upper limit on the ratio of gamma rays to normal hadronic cosmic rays at less than 2.4 x 10^{-5} at 310 TeV (90% confidence limit) from the galactic plane region: (50 degrees < l < 200 degrees); -5 degrees < b < 5 degrees). This limit places a strong constraint on models for emission from molecular clouds in the galaxy. We rule out significant spectral hardening in the outer galaxy, and conclude that emission from the plane at these energies is likely to be dominated by the decay of neutral pions resulting from cosmic rays interactions with passive target gas molecules.']",['1997-03-11'] +2033,['eng'],"['Kubis, S', 'Kutschera, M']",['Nuclear Matter in Relativistic Mean Field Theory with Isovector Scalar Meson'],['Astrophysics and Astronomy'],"['nuclear matter', 'meson, field theory', 'mean field approximation, relativistic', 'effective Lagrangian', 'coupling, Yukawa', 'scalar meson, exchange', 'scalar meson, isovector', 'a0(980)', 'astrophysics', 'n, matter', 'energy, density', 'nucleon, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703049'],"['Relativistic mean field (RMF) theory of nuclear matter with the isovector scalar mean field corresponding to the delta-meson [a_0(980)] is studied. While the delta-meson mean field vanishes in symmetric nuclear matter, it can influence properties of asymmetric nuclear matter in neutron stars. The RMF contribution due to delta-field to the nuclear symmetry energy is negative. To fit the empirical value, E_s=30 MeV, a stronger rho-meson coupling is required than in the absence of the delta-field. The energy per particle of neutron matter is then larger at high densities than the one with no delta-field included. Also, the proton fraction of beta-stable matter increases. Splitting of proton and neutron effective masses due to the delta-field can affect transport properties of neutron star matter.']",['1997-03-10'] +2034,['eng'],"['Protheroe, R J', 'Bednarek, W', 'Luo, Q']",['$\\gamma$-Rays and Neutrinos from Very Young Supernova Remnants'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'neutrino, cosmic radiation', 'supernova', 'astrophysics, pulsar', 'ion, acceleration', 'nucleus, photofission', 'n, energy spectrum', 'n nucleus, nuclear reaction', 'neutrino, energy spectrum', 'photon, energy spectrum']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703045'],"['We consider the result of acceleration of heavy ions in the slot gap potential of a very young pulsar with a hot polar cap. Photodisintegration of the heavy ions in the radiation field of the polar cap and pulsar surface gives rise to a flux of energetic neutrons. Some fraction of these neutrons interact with target nuclei in the supernova shell to produce a prompt neutrino and gamma-ray signal. Neutrons that do not interact promptly travel far from the pulsar where they decay into protons which await the arrival of target nuclei in the supernova shell, and then produce a delayed neutrino and gamma-ray signal. The TeV neutrino and 100 MeV and TeV gamma-ray signals should be observable from very young supernova remnants in our galaxy for a range of pulsar parameters.']",['1997-03-10'] +2035,['eng'],"['Narayan, M', 'Rajasekaran, G', 'Sinha, R']",['Solar neutrinos'],['Astrophysics and Astronomy'],"['astrophysics', 'neutrino, solar', 'neutrino, oscillation', 'neutrino, flux', 'flux, enhancement', 'neutrino, flavor', 'flavor, 3', 'neutrino, wave function', 'time dependence', 'neutrino, regeneration', 'neutrino, mixing angle', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703044'],"['It is pointed out that the enhancement of the solar neutrino rate in a real time detector like Super-Kamioka, SNO or Borexino due to neutrino oscillations in the moon during a partial or total solar eclipse may be observable. The enhancement is calculated as a function of the neutrino parameters in the case of three flavor mixing. This enhancement if seen, can further help to determine the neutrino parameters.']",['1997-03-10'] +2036,['eng'],"['Usov, Yu V']",['Low-mass normal-matter atmospheres of strange stars and their radiation'],['Astrophysics and Astronomy'],"['astrophysics', 'matter, strangeness', 'quark, surface', 'photon, emission', 'luminosity', 'thermodynamics', 'photon, energy spectrum', 'n, matter']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703037'],"['The quark surface of a strange star has a very low emissivity for X-ray photons. I find that a small amount of normal matter at the quark surface with temperature in the range $10^7\\la T_{_S}} \\ll mc^2/k\\simeq 6\\times 10^9$ K is enough to produce X-rays with high luminosity, $L_X\\simeq 10^{32}- 10^{34}(\\Delta M/10^{-22}M_\\odot)^2 erg s^{-1}$. For the total atmosphere mass the Eddington limit. The mean energy of X-ray photons which are radiated from such a low-mass atmosphere of a strange star is $\\sim 10^2(T_S/10^8 K)^{0.45} which are radiated from the surface of both a neutron star and a strange star with a massive normal-matter envelope, $\\Delta M\\sim 10^{-5}M_ødot$, for a fixed temperature at the stellar core. This raises the possibility that some black hole candidates with hard X-ray spectra are, in fact, such strange stars with a low-mass atmosphere. The X-ray emission from single strange stars is estimated.']",['1997-03-07'] +2037,['eng'],"['Berera, A', 'Fang, L Z', 'Hinshaw, G']",['An Attempt to Determine the Largest Scale of Primordial Density Perturbations in the Universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'cosmic radiation, background', 'causality', 'spectra, perturbation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703020'],"['Inflationary cosmology predicts that the particle horizon should be generically much bigger than the present-day Hubble radius, $1/H_0$. This implies a special regime of super-Hubble scale energy density fluctuations imprinted on the cosmic microwave background radiation (CMBR), which from present theory could only be explained by inflation Causality constraints are used to determine models for the power spectrum that accommodate a suppression scale. A three parameter likelihood analysis is performed of the COBE-DMR 4-year data with respect to the amplitude, spectral index, and suppression scale. It is found that all suppression length scales larger than $1/H_0$ are consistent with the data, but that scales of order $1/H_0$ are slightly preferred, at roughly the one-sigma level. Many non-inflation models would be consistent with a small suppression length scale, whereas for standard inflation models, the duration of the inflation epoch would have to be bounded by a fairly small upper limit. Suppression scales smaller than $1/H_0$ are strongly excluded by the anisotrophy data.']",['1997-03-05'] +2038,['eng'],"['Durrer, R']",['Signatures of Topological Defects in the Microwave Sky'],['Astrophysics and Astronomy'],"['talk, Rome 1996/10/10', 'inflationary universe', 'topology, defect', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703001'],['An introduction to topological defects in cosmology is given. We discuss their possible relevance for structure formation. Especial emphasis is given on the signature of topological defects in the spectrum of anisotropies in the cosmic microwave background. We present simple analytic estimates for the CMB spectrum on large and intermediate scales and compare them with the corresponding approximations for models where initial perturbations are generated during an inflationary epoch.'],['1997-03-03'] +2039,['eng'],"['Halzen, Francis']",['Very High Energy Phenomena in the Universe'],['Astrophysics and Astronomy'],"['conference, review', 'Les Arcs 1997/01/18', 'photon, cosmic radiation', 'cosmic radiation, flux', 'photon, absorption', 'p, absorption', 'gravitational radiation', 'p, cosmic radiation', 'energy spectrum', 'black hole', 'neutrino, astrophysics', 'astrophysics, galaxy', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703004'],"['This is the summary of a week of very informative presentations on new ways to probe the Universe using gravitational detectors, space and ground based gamma ray telescopes, EeV air shower detectors and neutrino telescopes. Gamma ray bursts and active galaxies were hot theoretical themes in the multi-wavelength discussions.']",['1997-03-03'] +2040,['eng'],"['Joyce, M', 'Shaposhnikov, M E']","['Primordial Magnetic Fields, Right Electrons, and the Abelian Anomaly']",['Astrophysics and Astronomy'],"['astrophysics, model', 'charge', 'anomaly, abelian', 'magnetic field', 'electron, asymmetry', 'electron, right-handed', 'potential, chemical', 'stability']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703005'],"['In the standard model there are charges with abelian anomaly only (e.g. right-handed electron number) which are effectively conserved in the early universe until some time shortly before the electroweak scale. A state at finite chemical potential of such a charge, possibly arising due to asymmetries produced at the GUT scale, is unstable to the generation of hypercharge magnetic field. We argue that quite large magnetic fields ($\\sim 10^{23}$ gauss at $T\\sim 3$ TeV with typical inhomogeneity scale up to $\\sim interest, potentially acting as seeds for amplification to larger scale magnetic fields through non-linear mechanisms.']",['1997-03-03'] +2041,['eng'],"['Henriques, A B', 'Mendes, L E', 'Moorhouse, R G']",['Density and Graviton Perturbations in the Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'gravitational radiation', 'density, perturbation', 'inflationary universe', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702238'],"['This paper evaluates and compares the gravitational wave and density perturbation contributions to the cosmic microwave background radiation, on the basis of the same power law inflationary model. The inflation to radiation transition is treated as instantaneous, but a model is constructed to allow for a smooth transition from the radiation to the matter dominated eras. The equations are numerically investigated and integrated, without any basic approximations being made. Use is made of the synchronous gauge, with appropriate gauge invariant variables, thus eliminating any confusion arising from unphysical gauge modes. We find a non- negligible gravitational wave contribution, which becomes dominant for a power law expansion with exponent $q < 13$. We also explore the dependence of our results with the main characteristic of the transition region, its length.']",['1997-02-28'] +2042,['eng'],"['Atrio-Barandela, F', 'Davidson, S']",['Interacting Hot Dark Matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'neutrino, diffusion', 'spectra, perturbation', 'density, perturbation', 'approximation, fluid', 'Boltzmann equation', 'phase space', 'galaxy', 'neutrino neutrino, interaction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702236'],"['We discuss the viability of a light particle ($\\sim 30$ eV neutrino) with strong self-interactions as a dark matter candidate. The interaction prevents the neutrinos from free-streaming during the radiation dominated regime so galaxy sized density perturbations can survive. Smaller scale perturbations are damped due to neutrino diffusion. We calculate the power spectrum in the imperfect fluid approximation, and show that it is damped at the length scale one would estimate due to neutrino diffusion. The strength of the neutrino--neutrino coupling is only weakly constrained by observations, and could be chosen by fitting the power spectrum to the observed amplitude of matter density perturbations. The main shortcoming of our model is that interacting neutrinos can not provide the dark matter in dwarf galaxies.']",['1997-02-28'] +2043,['eng'],"['Mollerach, S', 'Matarrese, S']",['Cosmic Microwave Background anisotropies from second order gravitational perturbations'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'temperature, anisotropy', 'relativity theory, general', 'gravitation, effect', 'perturbation, higher-order', 'higher-order, 2', 'transformation, gauge']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702234'],"['This paper presents a complete analysis of the effects of second order gravitational perturbations on Cosmic Microwave Background anisotropies, taking explicitly into account scalar, vector and tensor modes. We also consider the second order perturbations of the metric itself obtaining them, for a universe dominated by a collision-less fluid, in the Poisson gauge, by transforming the known results in the synchronous gauge. We discuss the resulting second order anisotropies in the Poisson gauge, pointing out the potentially most relevant effects.']",['1997-02-28'] +2044,['eng'],"['Durrer, R', 'Kahniashvili, T A']",['CMB anisotropies caused by gravitational waves'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation, spectra', 'astrophysics, missing-mass', 'astrophysics, fundamental constant', 'particle, massless', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702226'],"['Anisotropies in the cosmic microwave background radiation due to gravity waves are investigated. An initial spectrum of gravity waves may have been induced during an epoch of inflation. We study the propagation of such a spectrum in a Friedmann background of hot and cold dark matter, radiation and (possibly) a cosmological constant. We finally calculate its imprint as anisotropies on the cosmic microwave background. We also take into account that massless particles can source gravity waves by their anisotropic stresses. We consider general mixed dark matter models with and without cosmological constant. For a given, scale invariant input spectrum of gravity waves, we determine the dependence of the resulting spectrum of CMB anisotropies on the different model parameters.']",['1997-02-27'] +2045,['eng'],"['García-Bellido, J']",['Open inflation models and gravitational wave anisotropies in the CMB'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'gravitational radiation', 'spectra, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'tunneling', 'density, perturbation', 'temperature, anisotropy', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702211'],"['We study the large scale power spectrum of gravitational wave perturbations of the microwave background in the context of single-bubble open inflation models. We compute the ratio of tensor to scalar contributions to the CMB anisotropies as a function of $\\Omega_0$, the spectral index $n_S$ and the tunneling parameter $2\\pi GS_1/H$. We find that gravitational wave anisotropies can be very large at small values of this tunneling parameter. We also consider the contribution of supercurvature and bubble wall modes and find constraints on the parameters of open inflation models from the observed temperature anisotropies of the CMB. We show that the induced gravity and open hybrid scenarios are compatible with present observations for a reasonable range of parameters.']",['1997-02-25'] +2046,['eng'],"['Schaab, C', 'Hermann, B', 'Weber, F', 'Weigel, M K']",['Differences in the Cooling Behavior of Strange Quark Matter Stars and Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'matter, strangeness', 'neutrino, emission', 'temperature, surface', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702189'],"['The general statement that hypothetical strange (quark matter) stars cool more rapidly than neutron stars is investigated in greater detail. It is found that the direct Urca process could be forbidden not only in neutron stars but also in strange stars. In this case, strange stars are slowly cooling, and their surface temperatures are more or less indistinguishable from those of slowly cooling neutron stars. Furthermore the case of enhanced cooling is reinvestigated. It shows that strange stars cool significantly more rapidly than neutron stars within the first $\\sim 30$ years after birth. This feature could become particularly interesting if continued observation of SN 1987A would reveal the temperature of the possibly existing pulsar at its center.']",['1997-02-24'] +2047,['eng'],"['Halzen, Francis', 'Zas, E']",['Neutrino Fluxes from Active Galaxies'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino, flux', 'astrophysics, galaxy', 'p, blazar', 'p, jet', 'p, acceleration', 'pi, decay', 'neutrino/mu, diffusion', 'deep underground detector', 'photon, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702193'],"['There are tantalizing hints that jets, powered by supermassive black holes at the center of active galaxies, are true cosmic proton accelerators. They produce photons of TeV energy, possible higher, and may be the enigmatic source of the highest energy cosmic rays. Photoproduction of neutral pions by accelerated protons on UV light is the source of the highest energy photons, in which most of the bolometric luminosity of the galaxy may be emitted. The case that proton beams power active galaxies is, however, far from conclusive. Neutrinos from the decay of charged pions represent an uncontrovertible signature for the proton induced cascades. We show that their flux can be estimated by model-independent methods, based on dimensional analysis and textbook particle physics. Our calculations also demonstrate why different models for the proton blazar yield very similar results for the neutrino flux, consistent with the ones obtained here.']",['1997-02-24'] +2048,['eng'],"['Garriga, J', 'Mukhanov, V F']",['On classical anisotropies in models of Open Inflation'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'field theory, inflaton', 'bubble, production', 'tunneling', 'space-time, anisotropy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702201'],"['In the simplest model of open inflation there are two inflaton fields decoupled from each other. One of them, the tunneling field, produces a first stage of inflation which prepares the ground for the nucleation of a highly symmetric bubble. The other, a free field, drives a second period of slow roll inflation inside the bubble. However, the second field also evolves during the first stage of inflation, which to some extent breaks the needed symmetry. We show that this generates large supercurvature anisotropies which, together with the results of Tanaka and Sasaki, rule out this class of simple models (unless, of course, $\\Omega_0$ is sufficiently close to one.) The problem does not arise in modified models where the second field does not evolve in the first stage of inflation.']",['1997-02-24'] +2049,['eng'],"['Sasaki, M', 'Tanaka, T', 'Yakushige, Y']",['Wall fluctuation modes and tensor CMB anisotropy in open inflation models'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation, fluctuation', 'model, bubble', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702174'],"['We calculate the spectrum of large angle cosmic microwave background (CMB) anisotropies due to quantum fluctuations of the gravitational wave modes in one-bubble open inflation models. We find the bubble-wall fluctuation modes, which had been thought to exist discretely in previous analyses, are actually contained in the continuous spectrum of gravitational wave modes when the gravitational coupling is correctly taken into account. Then we find that the spectrum of the tensor CMB anisotropy can be decomposed into the part due to the wall fluctuation modes and that due to the usual gravitational wave modes in a way which is almost model-independent, even when the gravitational coupling is strong. We also discuss observational constraints on the model parameters. We find that an appreciable portion of the parameter space is excluded but the remaining allowable region is still wide enough to leave the one-bubble scenario viable.']",['1997-02-21'] +2050,['eng'],"['Dodelson, S', 'Kinney, W H', 'Kolb, E W']",['Cosmic microwave background measurements can discriminate among inflation models'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'fluctuation', 'spectra, perturbation', 'potential', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702166'],['Quantum fluctuations during inflation may be responsible for temperature anisotropies in the cosmic microwave background (CMB). Observations of CMB anisotropies can be used to falsify many currently popular models. In this paper we discuss the prospectus for observations of CMB anisotropies at the accuracy of planned satellite missions to reject currently popular inflation models and to provide some direction for model building.'],['1997-02-20'] +2051,['eng'],"['Hu, W', 'White, M']",['CMB Anisotropies'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'angular momentum', 'perturbation', 'Boltzmann equation', 'transport theory', 'temperature', 'polarization', 'photon baryon, fluid', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702170'],"['A total angular momentum representation simplifies the radiation transport problem for temperature and polarization anisotropy in the CMB. Scattering terms couple only the quadrupole moments of the distributions and each moment corresponds directly to the observable angular pattern on the sky. We develop and employ these techniques to study the general properties of anisotropy generation from scalar, vector and tensor perturbations to the metric and the matter, both in the cosmological fluids and from any seed perturbations (e.g.~defects) that may be present. The simpler, more transparent form and derivation of the Boltzmann equations brings out the geometric and model-independent aspects of temperature and polarization anisotropy formation. Large angle scalar polarization provides a robust means to distinguish between isocurvature and adiabatic models for structure formation in principle. Vector modes have the unique property that the CMB polarization is dominated by magnetic type parity at small angles and hence potentially distinguishable independent of the model for the seed. The tensor modes produce a different sign from the scalars and vectors for the temperature-polarization correlations at large angles. We explore conditions under which one perturbation type may dominate over the others including a detailed treatment of the photon-baryon fluid before recombination.']",['1997-02-20'] +2052,['eng'],"['Kaminker, A D', 'Yakovlev, D G', 'Haensel, P']",['Neutrino pair emission due to scattering of electrons off fluxoids in superfluid neutron star cores'],['Astrophysics and Astronomy'],"['n, matter', 'electron, scattering', 'flux tube, magnetic', 'neutrino, emission', 'synchrotron radiation', 'neutrino, pair production', 'p, superfluid', 'p, superconducting', 'energy loss', 'electron electron, interaction', 'electron p, interaction', 'neutrino, bremsstrahlung', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702155'],"['We study the emission of neutrinos, resulting from the scattering of electrons off magnetic flux tubes (fluxoids) in the neutron star cores with superfluid (superconducting) protons. In the absence of proton superfluidity (T> T_{cp}), this process transforms into the well known electron synchrotron emission of neutrino pairs in a locally uniform magnetic field B, with the neutrino energy loss rate Q proportional to B^2 T^5. For temperatures T not much below T_{cp}, the synchrotron regime (Q \\propto T^5) persists and the emissivity Q can be amplified by several orders of magnitude due to the appearance of the fluxoids and associated enhancement of the field within them. For lower T, the synchrotron regime transforms into the bremsstrahlung regime (Q \\propto T^6) similar to the ordinary neutrino-pair bremsstrahlung of electrons which scatter off atomic nuclei. We calculate Q numerically and represent our results through a suitable analytic fit. In addition, we estimate the emissivities of two other neutrino-production mechanisms which are usually neglected -- neutrino-pair bremsstrahlung processes due to electron-proton and electron-electron collisions. We show that the electron-fluxoid and electron-electron scattering can provide the main neutrino production mechanisms in the neutron star cores with highly superfluid protons and neutrons at T < 5 10^8 K. The electron-fluxoid scattering is significant if the initial, locally uniform magnetic field B > 10^{13} G.']",['1997-03-04'] +2053,['eng'],"['Magueijo, J', 'Lewin, A']",['Non-Gaussian spectra and the search for cosmic strings'],['Astrophysics and Astronomy'],"['talk, Rome 1996/10/10', 'astrophysics, string', 'spectra, fluctuation', 'cosmic radiation, background', 'angular distribution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702131'],['We present a new tool for relating theory and experiment suited for non-Gaussian theories: non-Gaussian spectra. It does for non-Gaussian theories what the angular power spectrum $C_\\ell$ does for Gaussian theories. We then show how previous studies of cosmic strings have over rated their non-Gaussian signature. More realistic maps are not visually stringy. However non-Gaussian spectra will accuse their stringiness. We finally summarise the steps of an undergoing experimental project aiming at searching for cosmic strings by means of this technique.'],['1997-02-17'] +2054,['eng'],"['Hannestad, S', 'Madsen, J']",['A Cosmological Three Level Neutrino Laser'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, flavor', 'neutrino, decay modes', 'neutrino, laser', 'Majoron', 'Boltzmann equation, solution', 'numerical calculations', 'neutrino --> boson neutrino']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702125'],"['We present a calculation of a neutrino decay scenario in the early Universe. The specific decay is \\nu_{2} \\to \\nu_{1} + \\phi, where \\phi is a boson. If there is a neutrino mass hierarchy, m_{\\nu_{e}} < m_{\\nu_{\\mu}} < m_{\\nu_{\\tau}}, we show that it is possible to generate stimulated decay and effects similar to atomic lasing without invoking new neutrinos, even starting from identical neutrino distributions. Under the right circumstances the decay can be to very low momentum boson states thereby producing something similar to a Bose condensate, with possible consequences for structure formation. Finally, we argue that this type of decay may also be important other places in early Universe physics.']",['1997-02-17'] +2055,['eng'],"['Christensen-Dalsgaard, J']",['Helioseismology and solar neutrinos'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'neutrino, solar', 'model, solar', 'neutrino, flux', 'velocity, acoustic', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702094'],"['Helioseismology has provided very precise information about the solar internal sound speed and density throughout most of the solar interior. The results are generally quite close to the properties of standard solar models. Since the solar oscillation frequencies do not provide direct information about temperature and composition, the helioseismic results to not completely rule out an astrophysical solution to the discrepancy between the predicted and measured neutrino fluxes from the Sun. However, such a solution does appear rather implausible.']",['1997-02-12'] +2056,['eng'],"['Keohane, J W', 'Petre, R', 'Gotthelf, E V', 'Ozaki, M', 'Koyama, K']",['A Possible Site of Cosmic Ray Acceleration in the Supernova Remnant IC 443'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'model, shock waves', 'bremsstrahlung', 'Compton scattering', 'synchrotron radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702056'],"['We present evidence for shock acceleration of cosmic rays to high energies (about 10 TeV) in the supernova remnant IC 443. X-ray imaging spectroscopy with ASCA reveals two regions of particularly hard emission: an unresolved source embedded in an extended emission region, and a ridge of emission coincident with the southeastern rim. Both features are located on part of the radio shell where the shock wave is interacting with molecular gas, and together they account for a majority of the emission at 7 keV. Though we would not have noticed it a priori, the unresolved feature is coincident with one resolved by the ROSAT HRI. Because this feature overlaps a unique region of flat radio spectral index (alpha < 0.24), has about equal light-crossing and synchrotron loss times, and a power law spectrum with a spectral index of 2, we conclude that the hard X-ray feature is synchrotron radiation from a site of enhanced particle acceleration. Evidence against a plerion includes a lack of observed periodicity (the pulsed fraction upper limit is 33%), the spectral similarity with the more extended hard region, the location of the source outside the 95% error circle of the nearby EGRET source, the fact that it is nestled in a bend in the molecular cloud ring with which IC 443 is interacting, and the requirement of an extremely high transverse velocity (>5,000 km/s). We conclude that the anomalous feature is most likely tracing enhanced particle acceleration by shocks that are formed as the supernova blast wave impacts the ring of molecular clouds.']",['1997-02-06'] +2057,['eng'],"['Aharonian, F A', 'Heinzelmann, G']",['The HEGRA Experiment'],['Astrophysics and Astronomy'],"['review, Perpignan 1996/08/26', 'photon, cosmic radiation', 'showers, air', 'cosmic radiation, anisotropy', 'cosmic radiation, energy spectrum', 'cosmic radiation, primary', 'cosmic radiation, particle source', 'scintillation counter', 'Cherenkov counter, imaging', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702059'],"['A report is given on the status and recent results from the HEGRA imaging atmospheric Cherenkov telescopes (IACT) concerning Mrk 501 and GRS 1915+105 and on recent results from the HEGRA arrays concerning galactic and extragalactic gamma-ray sources, counterparts of TeV Gamma-Ray-Bursts, cosmic ray anisotropies, energy spectrum and composition of primary cosmic rays. The report summarizes the presentations given at the 15th European Cosmic Ray Symposium 1996.']",['1997-02-07'] +2058,['eng'],"['Bergström, L', 'Edsjö, J', 'Kamionkowski, M P']",['Astrophysical-Neutrino Detection with Angular and Energy Resolution'],['Astrophysics and Astronomy'],"['neutrino, astrophysics', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'muon, neutrinoproduction', 'muon, flux', 'angular distribution, (muon)', 'energy spectrum, muon', 'counters and detectors, energy resolution', 'counters and detectors, angular resolution', 'astrophysics, missing-mass', 'WIMP', 'sparticle, mass', 'LSP', 'background', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702037'],"['We investigate the improvement in sensitivity to astrophysical point sources of energetic ($\\gtrsim1$ GeV) neutrinos which can be achieved with angular and/or energy resolution of the neutrino-induced muon. As a specific example we consider WIMP annihilation in the Sun and in the Earth as a neutrino source. The sensitivity is improved by using the angular and energy distribution to reduce the atmospheric-neutrino background. Although the specific improvements depend on the backgrounds and assumed sources, the sensitivity to a WIMP signal may be improved, with equal exposure, by up to roughly a factor of two with good angular resolution, and by up to roughly a factor of three with good energy resolution. In case of a positive detection, energy resolution would also improve the measurement of the neutrino energy spectrum and therefore provide information on the WIMP mass and composition.']",['1997-03-04'] +2059,['eng'],"['Sornborger, A T']",['High-Resolution Analysis of Cold and Hot Dark Matter in Cosmic String Wakes'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'astrophysics, string', 'particle, velocity', 'particle, tracks', 'phase space', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702038'],"[""We study the accretion of cold and hot dark matter onto a cosmic string wake using a high-resolution numerical simulation. We verify previous analytical calculations predicting the radius of bound matter around wakes and inflow velocities of the dark matter, as well as assumptions about the self-similarity of the solution. In cold wakes, we show that self-similarity is approached quickly after a `binding' transition. Hot wakes approach self-similarity rapidly once the free streaming `pressure' falls below a critical value and accretion begins. We also analytically calculate the size of the overdensity in wakes with cold dark matter and compare the results to simulations. We remark that the results derived may be used in testing gravitational numerical codes in the non-linear regime.""]",['1997-02-06'] +2060,['eng'],"['Cheung, C', 'Magueijo, J']",['Painless causality in defect calculations'],['Astrophysics and Astronomy'],"['astrophysics, perturbation', 'topology, defect', 'causality', 'astrophysics, missing-mass', 'back reaction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702041'],"[""Topological defects must respect causality, a statement leading to restrictive constraints on the power spectrum of the total cosmological perturbations they induce. Causality constraints have for long been known to require the presence of an under-density in the surrounding matter compensating the defect network on large scales. This so-called compensation can never be neglected and significantly complicates calculations in defect scenarios, eg. computing cosmic microwave background fluctuations. A quick and dirty way to implement the compensation are the so-called compensation fudge factors. Here we derive the complete photon-baryon-CDM backreaction effects in defect scenarios. The fudge factor comes out as an algebraic identity and so we drop the negative qualifier ``fudge''. The compensation scale is computed and physically interpreted. Secondary backreaction effects exist, and neglecting them constitutes the well-defined approximation scheme within which one should consider compensation factor calculations. We quantitatively assess the accuracy of this approximation, and conclude that the considerable pains associated with improving on it are often a waste of effort.""]",['1997-02-06'] +2061,['eng'],"['Rachen, J P']",['Propagation of UHE cosmic rays in a structured universe'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'cosmic radiation, acceleration', 'magnetic field, galaxy', 'cosmic radiation, confinement', 'shock waves', 'cosmic radiation, background', 'cosmic radiation, particle source', 'pi, production', 'energy loss', 'stochastic', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702046'],"['In a gravitationally unstable universe, the structure of dark matter and galaxies, intergalactic gas and magnetic field can have severe impact on the propagation of ultra high energy cosmic rays (UHECR) (Ryu & Kang, this proceedings). The possible effects include spatial confinement and directional focusing along the supergalactic matter sheets, as well as universal re-acceleration at large scale shock fronts, and spectral modification due to energy dependent leakage into cosmic voids. As a result, the GZK-cutoff may be less pronounced and occur at a higher energy, where the stochastic nature of both acceleration and energy loss processes has to be taken into account.']",['1997-02-06'] +2062,['eng'],"['Bergström, L']",['High-Energy $\\gamma$ and Neutrino Astronomy'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'neutrino, astrophysics', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'neutrino, solar', 'astrophysics, missing-mass', 'supersymmetry', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702052'],"['An overview is given of high-energy gamma-ray and neutrino astronomy, emphasizing the links between the two fields. With several new large detectors just becoming operational, the TeV gamma-ray and neutrino sky will soon be surveyed with unprecedented sensitivity.']",['1997-02-06'] +2063,['eng'],"['Bahcall, J N']",['Solar Neutrinos'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'neutrino, solar', 'model, solar', 'electroweak interaction', 'neutrino, flux', 'helium, interference', 'neutrino, oscillation', 'resonance, oscillation', 'velocity, acoustic', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702057'],"[""This talk compares standard model predictions for solar neutrino experiments with the results of actual observations. Here `standard model' means the combined standard model of minimal electroweak theory plus a standard solar model. I emphasize the importance of recent analyses in which the neutrino fluxes are treated as free parameters, independent of any constraints from solar models, and the stunning agreement between the predictions of standard solar models and helioseismological measurements.""]",['1997-02-06'] +2064,['eng'],"['Collar, J I']","['Reply to astro-ph/9612003 ""Comments on Biological Effects of Stellar Collapse Neutrinos"" and astro-ph/9612214 ""Volcanogenic Dark Matter and Mass Extinctions""']",['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'astrophysics, matter', 'biology, effect', 'astrophysics, missing-mass', 'WIMP']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702026'],['A Reply to the criticisms contained in astro-ph/9612003 is provided and a logical inconsistency in astro-ph/9612214 is pointed out.'],['1997-02-04'] +2065,['eng'],"['Heckler, A F']",['Calculation of the emergent spectrum and observation of primordial black holes'],['Astrophysics and Astronomy'],"['black hole, radiation', 'radiation, Hawking', 'radiation, spectra', 'quark, emission', 'gluon, emission', 'fragmentation', 'quantum chromodynamics', 'photon, energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702027'],"[""We calculate the emergent spectrum of microscopic black holes, which emit copious amounts of thermal ``Hawking'' radiation, taking into account the proposition that (contrary to previous models) emitted quarks and gluons do not directly fragment into hadrons, but rather interact and form a photosphere and decrease in energy before fragmenting. The resulting spectrum emits copious amount of photons at energies around 100MeV. We find that the limit on the average universal density of black holes is not significantly affected by the photosphere. However we also find that gamma ray satellites such as EGRET and GLAST are well suited to look for nearby black holes out to a distance on the order of 0.3 parsecs, and conclude that if black holes are clustered locally as much as luminous matter, they may be directly detectable.""]",['1997-02-04'] +2066,['eng'],"['De Laix, A A', 'Krauss, L M', 'Vachaspati, T']",['Gravitational Lensing Signatures of Long Cosmic Strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'gravitation, lens', 'astrophysics, quasar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702033'],"['The gravitational lensing by long, wiggly cosmic strings is shown to produce a large number of lensed images of a background source. In addition to pairs of images on either side of the string, a number of small images outline the string due to small-scale structure on the string. This image pattern could provide a highly distinctive signature of cosmic strings. Since the optical depth for multiple imaging of distant quasar sources by long strings may be comparable to that by galaxies, these image patterns should be clearly observable in the next generation of redshift surveys such as the Sloan Digital Sky Survey.']",['1997-02-04'] +2067,['eng'],"['Cardall, C Y', 'Fuller, G M']",['Neutrino Physics and the Primordial Elemental Abundances'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'light nucleus, production', 'deuterium', 'helium, nuclide', 'lithium', 'neutrino, sterile', 'neutrino, interference', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702001'],"['Limits can be placed on nonstandard neutrino physics when big bang nucleosynthesis (BBN) calculations employing standard neutrino physics agree with the observationally inferred primordial abundances of deuterium (D), $^3$He, $^4$He, and $^7$Li. These constraints depend most sensitively on the abundances of D and $^4$He. New observational determinations of the primordial D and/or $^4$He abundances could force revisions in BBN constraints on nonstandard neutrino physics.']",['1997-02-03'] +2068,['eng'],"['Hindmarsh, M B', 'Liddle, A R', 'Chen, X', 'Kamionkowski, M P']",['On the instability of the one-texture universe'],['Astrophysics and Astronomy'],"['astrophysics, texture', 'stability', 'space-time, closed', 'field theory, scalar', 'perturbation theory', 'cosmic radiation, background']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9702006'],"['The one-texture universe, introduced by Davis in 1987, is a homogeneous mapping of a scalar field with an $S^3$ vacuum into a closed universe. It has long been known to mathematicians that such solutions, although static, are unstable. We show by explicit construction that there is only one unstable mode, corresponding to collapse of the texture towards a single point, in the case where gravitational backreaction is neglected. We discuss the instability timescale in both static and expanding space-times; in the latter case it is of order of the present age of the universe, suggesting that, though unstable, the one-texture universe could survive to the present. The cosmic microwave background constrains the initial magnitude of this unstable perturbation to be less than of order 10^{-3}.']",['1997-02-03'] +2069,['eng'],"['Fiorentini, G', 'Acerbi, C']",['Supernova Neutrinos and the $\\tau$-Neutrino Mass'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'neutrino/tau, mass', 'upper limit', 'astrophysics, supernova', 'data analysis method', 'Cherenkov counter, water', 'neutrino electron, interaction', 'electron, angular distribution', 'deep underground detector, KAMIOKANDE', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701232'],"['We perform an extensive investigation of the sensitivity to non-vanishing tau-neutrino mass in a large water Cherenkov detector, developing an analysis method for neutrino events originated by a supernova explosion. This approach, based on directional considerations, provides informations almost undepending on the supernova model. We analyze several theoretical models from numerical simulations and phenomenological models based on SN1987A data, and determine optimal values of the analysis parameters so as to reach the highest sensitivity to a non-vanishing tau-neutrino mass. The minimal detectable mass is generally just above the cosmologically interesting range, m ~ 100 eV, in the case of a supernova explosion near the galactic center. For the case that no positive signal is obtained, observation of a neutrino burst with Super-Kamiokande will anyhow lower the present upper bound on tau-neutrino mass to few hundred eV.']",['1997-02-24'] +2070,['eng'],"['Ong, R A']",['Development of the Solar Tower Atmospheric Cherenkov Effect Experiment (STACEE)'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'astrophysics', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'Cherenkov counter, proposed', 'activity report', '25-500 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701236'],"['STACEE is a proposed atmospheric Cherenkov telescope for ground-based gamma-ray astrophysics between 25 and 500 GeV. The telescope will make use of the large solar mirrors (heliostats) available at a solar research facility to achieve an energy threshold lower than any existing ground-based instrument. This paper describes the development of STACEE, including an overview of the complete instrument design and a discussion of results from recent prototype tests at the large solar heliostat field of Sandia National Laboratories.']",['1997-02-24'] +2071,['eng'],"['Snowden-Ifft, D P', 'Westphal, A J']",['Unique Signature of Dark Matter in Ancient Mica'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'mass, WIMP', 'scattering, atom WIMP', 'particle identification, WIMP', 'mineral, track sensitive', 'crystal, mica', 'numerical calculations', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701215'],"[""Mica can store (for >1 Gy) etchable tracks caused by atoms recoiling from WIMPs. Because a background from fission neutrons will eventually limit this technique, a unique signature for WIMPs in ancient mica is needed. Our motion around the center of the Galaxy causes WIMPs, unlike neutrons, to enter the mica from a preferred direction on the sky. Mica is a directional detector and despite the complex rotations that natural mica crystals make with respect to this WIMP ``wind,'' there is a substantial dependence of etch pit density on present day mica orientation.""]",['1997-01-29'] +2072,['eng'],"['Hu, W', 'White, M']",['Tensor Anisotropies in an Open Universe'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation', 'space-time, open', 'perturbation, tensor', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701210'],"[""We calculate the anisotropies in the cosmic microwave background induced by long-wavelength primordial gravitational waves in a universe with negative spatial curvature, such as are produced in the ``open inflation'' scenario. The impact of these results on the COBE normalization of open models is discussed.""]",['1997-01-28'] +2073,['eng'],"['Moessner, R', 'Brandenberger, R H']",['Early Objects in the Cosmic String Theory with Hot Dark Matter'],['Astrophysics and Astronomy'],"['talk, Hangzhou 1996/10/13', 'astrophysics, string', 'astrophysics, missing-mass', 'mass, nonlinear', 'astrophysics, galaxy', 'astrophysics, quasar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701208'],"['We study the accretion of hot dark matter onto moving cosmic string loops, using an adaptation of the Zeldovich approximation to HDM. We show that a large number of nonlinear objects of mass greater than $10^{12}M_\\odot$, which could be the hosts of high redshift quasars, are formed by a redshift of $z=4$.']",['1997-01-28'] +2074,['eng'],"['Mathews, G J', 'Wilson, J R']","['Binary Induced Neutron-Star Compression, Heating, and Collapse']",['Astrophysics and Astronomy'],"['astrophysics, model', 'n, matter', 'relativity theory, general', 'model, hydrodynamical', 'neutrino, luminosity', 'temperature', 'gravitational radiation', 'photon, cosmic radiation', 'field equations', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701142'],"['We analyze several aspects of the recently noted neutron star collapse instability in close binary systems. We utilize (3+1) dimensional and spherical numerical general relativistic hydrodynamics to study the origin, evolution, and parametric sensitivity of this instability. We derive the modified conditions of hydrostatic equilibrium for the stars in the curved space of quasi-static orbits. We examine the sensitivity of the instability to the neutron star mass and equation of state. We also estimate limits to the possible interior heating and associated neutrino luminosity which could be generated as the stars gradually compress prior to collapse. We show that the radiative loss in neutrinos from this heating could exceed the power radiated in gravity waves for several hours prior to collapse. The possibility that the radiation neutrinos could produce gamma-ray (or other electromagnetic) burst phenomena is also discussed.']",['1997-01-21'] +2075,['eng'],"['García-Bellido, J', 'Linde, Andrei D']",['Open Hybrid Inflation'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'spectra, perturbation', 'symmetry breaking', 'density, perturbation', 'temperature, anisotropy', 'bubble, fluctuation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701173'],"[""We propose an open hybrid inflation scenario that produces an open universe with a `tilted' n>1 spectrum of metric perturbations. The model contains a symmetry breaking field that tunnels to its true vacuum, producing a single bubble inside which hybrid inflation drives the universe to almost flatness. In order to obtain density perturbations with n > 1 we use the recently proposed new version of hybrid inflation scenario called tilted hybrid inflation. In this scenario, unlike in the previously known versions of hybrid inflation, a considerable tilt of the spectrum can be obtained without fine-tuning. The stage of inflation in this model is rather short, which allows us to obtain an inflationary universe with Omega < 1 in a more natural way. We study the separate contribution of scalar perturbations coming from the continuum subcurvature modes, the discrete supercurvature mode and the bubble wall mode to the angular power spectrum of temperature fluctuations in open inflation. We derive bounds on the parameters of the model so that the predicted spectrum is compatible with the observed anisotropy of the microwave background.""]",['1997-01-23'] +2076,['eng'],"['Bucher, M', 'Cohn, J D']",['Primordial Gravitational Waves From Open Inflation'],['Astrophysics and Astronomy'],"['gravitational radiation, spectra', 'inflationary universe, open', 'graviton', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'vacuum state, bubble', 'energy, density', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701117'],"['We calculate the spectrum of gravitational waves generated during inflation in open $(\\Omega _0<1)$ inflationary models. In such models an initial epoch of old inflation solves the horizon and flatness problems, and during this first epoch of inflation the quantum state of the graviton field rapidly approaches the Bunch-Davies vacuum. Then old inflation ends by the nucleation of a single bubble, inside of which there is a shortened epoch of slow-roll inflation giving $\\Omega _0<1$ today. In this paper we re-express the Bunch-Davies vacuum for the graviton field in terms of the hyperbolic modes inside the bubble and propagate these modes forward in time into the present era. We derive the expression for the contribution from these gravity waves to the cosmic microwave background anisotropy including the effect of a finite energy difference across the bubble wall.']",['1997-01-20'] +2077,['eng'],"['Kaniadakis, G', 'Lavagno, A', 'Quarati, P']",['Non-Extensive Statistics and Solar Neutrinos'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, solar', 'statistical analysis', 'model, solar', 'neutrino, flux', 'temperature', 'entropy', 'astrophysics, galaxy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701118'],"['In this paper we will show that, because of the long-range microscopic memory of the random force, acting in the solar core, mainly on the electrons and the protons than on the light and heavy ions (or, equally, because of anomalous diffusion of solar core constituents of light mass and of normal diffusion of heavy ions), the equilibrium statistical distribution that these particles must obey, is that of generalized Boltzmann-Gibbs statistics (or the Tsallis non-extensive statistics), the distribution differing very slightly from the usual Maxwellian distribution. Due to the high-energy depleted tail of the distribution, the nuclear rates are reduced and, using earlier results on the standard solar model neutrino fluxes, calculated by Clayton and collaborators, we can evaluate fluxes in good agreement with the experimental data. While proton distribution is only very slightly different from Maxwellian there is a little more difference with electron distribution. We can define one central electron temperature as a few percent higher than the ion central temperature nearly equal to the standard solar model temperature. The difference is related to the different reductions with respect to the standard solar model values needed for $B$ and $CNO$ neutrinos and for $Be$ neutrinos.']",['1997-01-20'] +2078,['eng'],"['Lipunov, V M', 'Postnov, K A', 'Prokhorov, M E']",['Black holes and gravitational waves'],['Astrophysics and Astronomy'],"['black hole', 'n, matter', 'gravitational radiation, counters and detectors', 'interference, laser', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701134'],['Study of gravitational-radiation induced merging rates of relativistic binary stars (double neutron stars; neutron star + black hole; double black holes) shows that the first-generation gravitational wave interferometers with an rms-sensitivity of $10^{-21}$ at frequency 100 Hz can detect 10-700 black hole and only $\\sim 1$ neutron star coalescences in a 1-year integration time in a wide range of stellar evolution parameters. It is notable that modern concepts of stellar evolution predict that the first detection of gravitational wave will independently discover black holes.'],['1997-01-21'] +2079,['eng'],"['McLaughlin, G C', 'Fuller, G M']",['Weak Charge-Changing Flow in Expanding r-Process Environments'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'nucleus, production', 'n, capture', 'nucleus, semileptonic decay', 'neutrino, capture', 'nucleus, particle flow', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701082'],"['We assess the prospects for attaining steady nuclear flow equilibrium in expanding r-process environments where beta decay and/or neutrino capture determine the nuclear charge-changing rates. For very rapid expansions, we find that weak steady flow equilibrium normally cannot be attained. However, even when neutron capture processes freeze out in such nonequilibrium conditions, abundance ratios of nuclear species in the r-process peaks might still mimic those attained in weak steady flow. This result suggests that the r-process yield in a regime of rapid expansion can be calculated reliably only when all neutron capture, photodisintegration, and weak interaction processes are fully coupled in a dynamical calculation. We discuss the implications of these results for models of the r-process sited in rapidly expanding neutrino-heated ejecta.']",['1997-01-16'] +2080,['eng'],"['Sigurdsson, S']",['Estimating the detectable rate of capture of stellar mass black holes by massive central black holes in normal galaxies'],['Astrophysics and Astronomy'],"['black hole, mass', 'astrophysics, galaxy', 'gravitational radiation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701079'],"['The capture and subsequent inspiral of stellar mass black holes on eccentric orbits by central massive black holes, is one of the more interesting likely sources of gravitational radiation detectable by LISA. We estimate the rate of observable events and the associated uncertainties. A moderately favourable mass function could provide many detectable bursts each year, and a detection of at least one burst per year is very likely given our current understanding of the populations in cores of normal spiral galaxies.']",['1997-01-15'] +2081,['eng'],"['Tanaka, T', 'Sasaki, M']",['The Spectrum of Gravitational Wave Perturbations in the One-Bubble Open Inflationary Universe'],['Astrophysics and Astronomy'],"['gravitational radiation, perturbation', 'inflationary universe, bubble', 'quantization', 'space-time, O(3,1)', 'field theory, scalar', 'field theory, massless', 'massless, field theory', 'analytic properties']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701053'],"['We give the initial spectrum of quantized gravitational waves in the context of the one-bubble open inflationary universe scenario. In determining the quantum state after the bubble nucleation we adopt the prescription to require the analyticity of positive frequency functions in half of the Euclidean extension of the background O(3,1)-symmetric spacetime. We find the spectrum is well behaved at the infrared limit and there appears no supercurvature mode. In the thin wall approximation, the explicit form of the spectrum of gravitational wave perturbations is calculated.']",['1997-01-13'] +2082,['eng'],"['Martins, C J A P']",['String Evolution in Open Universes'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, string', 'dependence, velocity', 'grand unified theory', 'scaling', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701055'],"[""The velocity-dependent `one-scale' model of Martins and Shellard is used to study the evolution of a cosmic string network (and the corresponding loop population) in open universes. It is shown that in this case there is no linear scaling regime and that even though curvature still dominates the dynamics, at late times strings become the main component of the universe. We also comment on the possible consequences of these results.""]",['1997-01-13'] +2083,['eng'],"['Kachelriess, M', 'Wilke, C', 'Wunner, G']",['Axion cyclotron emissivity of magnetized white dwarfs and neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'axion, emission', 'electron, energy loss', 'electron, gas', 'magnetic field, external field', 'luminosity, axion', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701056'],['The energy loss rate of a magnetized electron gas emitting axions a due to the process $e^- \\to e^- +a$ is derived for arbitrary magnetic field strength B. Requiring that for a strongly magnetized neutron star the axion luminosity is smaller than the neutrino luminosity we obtain the bound $g_{ae}\\lsim 10^{-10}$ for the axion electron coupling constant. This limit is considerably weaker than the bound derived earlier by Borisov and Grishina using the same method. Applying a similar argument to magnetic white dwarf stars results in the more stringent bound $g_{ae}\\lsim 5x10^{-13} (T/10^7 K)^{5/4} (B/10^{10} G)^{-2}$ where T is the internal temperature of the white dwarf.'],['1997-01-13'] +2084,['eng'],"['Liddle, A R', 'Grivell, I J']",['Accurately determining inflationary perturbations'],['Astrophysics and Astronomy'],"['talk, Chicago 1996/12/15', 'inflationary universe', 'spectra, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701031'],"['Cosmic microwave anisotropy satellites promise extremely accurate measures of the amplitude of perturbations in the universe. We use a numerical code to test the accuracy of existing approximate expressions for the amplitude of perturbations produced by single-field inflation models. We find that the second-order Stewart-Lyth calculation gives extremely accurate results, typically better than one percent. We use our code to carry out an expansion about the general power-law inflation solution, providing a fitting function giving results of even higher accuracy.']",['1997-01-09'] +2085,['eng'],"['Halzen, Francis']",['Status of Neutrino Astronomy'],['Astrophysics and Astronomy'],"['neutrino, astrophysics', 'deep underground detector, AMANDA', 'counters and detectors, proposed', 'Cherenkov counter, water', 'solids, water']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701029'],"['This is a (very) personal attempt to summarize the status of neutrino astronomy: its scientific motivations, our understanding of natural water and ice as particle detectors and, finally, the detector technology.']",['1997-01-08'] +2086,['eng'],"['Kim, J B', 'Kim, J H', 'Lee, H K']",['Electron-Neutrino Degeneracy and Primordial Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Pusan 1996/08/19', 'astrophysics, model', 'light nucleus, production', 'neutrino/e, astrophysics', 'Fermi gas', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9701011'],"['We discuss the possible ranges of electron neutrino degeneracy which is consistent with the inferred primordial abundances of the light elements. It is found that the electron neutrino degeneracy, $|\\xi_e|$, up to order of $10^{-1}$ is consistent with the present data.']",['1997-01-06'] +2087,['eng'],"['Russ, H', 'Soffel, M H', 'Kasai, M', 'Börner, G']",['Age of the Universe'],['Astrophysics and Astronomy'],"['Friedman model', 'cosmic radiation, background', 'approximation, relativistic', 'effect, back reaction', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612218'],"[""For the first time we calculate quantitatively the influence of inhomogeneities on the global expansion factor by averaging the Friedmann equation. In the framework of the relativistic second-order Zel'dovich-approximation scheme for irrotational dust we use observational results in form of the normalisation constant fixed by the COBE results and we check different power spectra, namely for adiabatic CDM, isocurvature CDM, HDM, WDM, Strings and Textures. We find that the influence of the inhomogeneities on the global expansion factor is very small. So the error in determining the age of the universe using the Hubble constant in the usual way is negligible. This does not imply that the effect is negligible for local astronomical measurements of the Hubble constant. Locally the determination of the redshift-distance relation can be strongly influenced by the peculiar velocity fields due to inhomogeneities. Our calculation does not consider such effects, but is contrained to comparing globally homogeneous and averaged inhomogeneous matter distributions. In addition we relate our work to previous treatments.""]",['1997-01-02'] +2088,['eng'],"['Protheroe, R J']",['Astrophysical sources of high energy neutrinos'],['Astrophysics and Astronomy'],"['talk, Erice 1996/06/16', 'neutrino, cosmic radiation', 'neutrino, particle source', 'cosmic radiation, interaction', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612213'],"['I give a brief critical review of the predicted intensity of diffuse high energy neutrinos of astrophysical origin over the energy range from 10^12 eV to 10^24 eV. Neutrinos from interactions of galactic cosmic rays with interstellar matter are guaranteed, and the intensity can be reliably predicted to within a factor of about 2 up to 10^17 eV. Somewhat less certain are intensities in the same energy range from cosmic rays escaping from normal galaxies or active galactic nuclei (AGN) and interacting with intracluster gas. At higher energies, neutrinos will be produced by interactions of extragalactic cosmic rays with the microwave background. Other sources, such as AGN, in particular blazars, and topological defects, are more speculative. However, searches for neutrinos from all of these potential sources should be made because their observation would have important implications for high energy astrophysics and cosmology.']",['1997-01-02'] +2089,['eng'],"['Protheroe, R J']",['Origin and propagation of the highest energy cosmic rays'],['Astrophysics and Astronomy'],"['lectures, Erice 1996/06/16', 'astrophysics, model', 'cosmic radiation, acceleration', 'model, shock waves', 'cosmic radiation, interaction', 'cosmic radiation, background', 'showers, electromagnetic', 'astrophysics, galaxy', 'magnetic field', 'cosmic radiation, energy spectrum', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612212'],"['In this lecture I give an overview of shock acceleration, interactions of high energy cosmic rays with, and propagation through, the background radiation, and the resulting electron-photon cascade. I argue that while the origin of the highest energy cosmic rays is still uncertain, it is not necessary to invoke exotic models such as emission by topological defects to explain the existing data. It seems likely that shock acceleration at Fanaroff-Riley Class II radio galaxies can account for the existing data. However, new cosmic ray data, as well as better estimates of the extragalactic radiation fields and magnetic fields will be necessary before we will be certain of the origin of the highest energy particles occurring in nature.']",['1997-01-02'] +2090,['eng'],"['Turok, Neil G', 'Zhu, Y']",['Inflationary Textures'],['Astrophysics and Astronomy'],"['inflationary universe, texture', 'spectra, fluctuation', 'field theory, scalar', 'symmetry breaking, O(N)', 'expansion 1/N', 'effective potential', 'space-time, de Sitter', 'vacuum state', 'Friedman model', 'sigma model, nonlinear', 'renormalization', 'correlation, long-range', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612242'],"['We present a calculation of the power spectrum generated in a classically symmetry-breaking O(N) scalar field through inflationary quantum fluctuations, using the large-N limit. The effective potential of the theory in de Sitter space is obtained from a gap equation which is exact at large N. Quantum fluctuations restore the O(N) symmetry in de Sitter space, but for the finite values of N of interest, there is symmetry breaking and phase ordering after inflation, described by the classical nonlinear sigma model. The main difference with the usual cosmic texture scenario is that the initial conditions possess long range correlations, with calculable exponents.']",['1997-02-18'] +2091,['eng'],"['Kohri, K', 'Kawasaki, M', 'Sato, K']",['Big Bang Nucleosynthesis and Lepton Number Asymmetry in the Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'neutrino/e, density', 'potential, chemical', 'lepton number, asymmetry', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612237'],"['Recently it is reported that there is the discrepancy between big bang nucleosynthesis theory and observations (BBN crisis). We show that BBN predictions agree with the primordial abundances of light elements, ${}^4$He, D, ${}^3$He and ${}^7$Li inferred from the observational data if an electron neutrino has a net chemical potential $\\xi_{\\nu_e}$ due to lepton asymmetry. We estimate that $\\xi_{\\nu_e} = 0.043^{+0.040}_{-0.040}$ (95% C.L.) and']",['1997-01-02'] +2092,['eng'],"['Kunz, M', 'Durrer, R']",['Microwave Background Anisotropies Induced by Global Scalar Fields'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'field theory, scalar', 'symmetry, O(N)', 'expansion 1/N', 'time, correlation function', 'model, texture', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612202'],"[""We present an analysis of CMB anisotropies induced by global scalar fields in the large N limit. In this limit, the CMB anisotropy spectrum can be determined without cumbersome 3D simulations. We determine the source functions and their unequal time correlation functions and show that they are quite similar to the corresponding functions in the texture model. This leads us to the conclusion that the large N limit provides a 'cheap approximation' to the texture model of structure formation.""]",['1997-01-02'] +2093,['eng'],"['Venkatesan, A', 'Miller, M C', 'Olinto, A V']",['Constraints on the Production of Ultra-High-Energy Cosmic Rays by Isolated Neutron Stars'],['Astrophysics and Astronomy'],"['astrophysics, model', 'constraint', 'cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'n, matter', 'cosmic radiation, acceleration', 'numerical calculations', '> 10**6 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612210'],"['The energetics, spectrum, and composition of cosmic rays with energies below about $10^{15}$ eV are fairly well explained by models involving supernova shocks. In contrast, no widely accepted theory exists for the origin of ultra-high energy cosmic rays (UHECRS), which have energies above $10^{15}$ eV. Instead of proposing a specific model, here we place strong constraints on any model of UHECRS involving isolated neutron stars (no companions). We consider the total power requirements and show that the only viable power source associated with isolated neutron stars is rotation. Mechanisms based on accretion from the interstellar medium fall short of the necessary power despite the most optimistic assumptions. Power considerations also demonstrate that not enough rotational energy is tapped by a ""propeller""-like acceleration of interstellar matter. The most promising source of energy is rotational spindown via magnetic braking. We examine microphysical energy loss processes near magnetized neutron stars and conclude that the most likely site for yielding UHECRS from isolated neutron stars is near the light cylinder.']",['1997-01-02'] +2094,['eng'],"['Lemos, J P S']",['Black Holes'],['Astrophysics and Astronomy'],"['review', 'black hole, mass', 'radiation, Hawking', 'quantization, effect', 'information theory', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612220'],"['We present a broad review on black holes. We analyse some of the fundamental concepts in black hole theory, the observational and theoretical status of stellar and galactic black holes, and their appearance as quantum objects.']",['1997-01-02'] +2095,['eng'],"['Keil, W', 'Janka, H T', 'Schramm, David N', 'Sigl, G', 'Turner, M S', 'Ellis, Jonathan Richard']",['A Fresh Look at Axions and SN 1987A'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'mass, axion', 'axion, emission', 'neutrino, cosmic radiation', 'nucleon, spin', 'spin, fluctuation', 'coupling, (nucleon axion)', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612222'],"['We re-examine the very stringent limits on the axion mass based on the strength and duration of the neutrino signal from SN 1987A, in the light of new measurements of the axial-vector coupling strength of nucleons, possible suppression of axion emission due to many-body effects, and additional emission processes involving pions. The suppression of axion emission due to nucleon spin fluctuations induced by many-body effects degrades previous limits by a factor of about 2. Emission processes involving thermal pions can strengthen the limits by a factor of 3-4 within a perturbative treatment that neglects saturation of nucleon spin fluctuations. Inclusion of saturation effects, however, tends to make the limits less dependent on pion abundances. The resulting axion mass limit also depends on the precise couplings of the axion and ranges from 0.5x10**(-3) eV to 6x10**(-3) eV.']",['1997-01-02'] +2096,['eng'],"['Kutschera, M']",['Hadron Physics and the Structure of Neutron Stars'],['Astrophysics and Astronomy'],"['lectures, Cracow 1996/06', 'n, matter', 'hadron, matter', 'nucleon hyperon, interaction', 'meson, condensation', 'quark, matter', 'thermodynamics', 'astrophysics, supernova', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612143'],['The equation of state of hadronic matter in neutron stars is briefly reviewed. Uncertainties regarding the stiffness and composition of hadronic matter are discussed. Importance of poorly known short range interactions of nucleons and hyperons is emphasized. Condensation of meson fields and the role of subhadronic degrees of freedom is considered. Empirical constraints on the equation of state emerging from observations of neutron stars are discussed. Implications of possible black hole remnant of SN1987A for the equation of state are also discussed.'],['1996-12-16'] +2097,['eng'],"['García-Bellido, J', 'Linde, Andrei D']",['Tilted Hybrid Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time, perturbation', 'density, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612141'],"['We propose a new version of the hybrid inflation scenario that produces a significantly tilted n>1 spectrum of curvature perturbations. This may happen in supersymmetric models where the inflaton field acquires a mass proportional to the Hubble constant, and in the models where this field non-minimally couples to gravity. A large tilt of the spectrum in this scenario is often accompanied by a considerable contribution of tensor perturbations to the temperature anisotropies. We also show that under certain conditions the spectrum of density perturbations in this scenario may have a minimum on an intermediate length scale.']",['1996-12-16'] +2098,['eng'],"['Kolb, E W']",['Inflation in the Postmodern Era'],['Astrophysics and Astronomy'],"['lectures, Erice 1996/09/07', 'inflationary universe', 'density, perturbation', 'space-time, perturbation', 'perturbation, scalar', 'perturbation, tensor', 'tensor, energy-momentum', 'quantization']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612138'],['In this lecture I will review some recent progress in improving the accuracy of the calculation of density perturbations resulting from inflation.'],['1996-12-16'] +2099,['eng'],"['Vincent, G R', 'Hindmarsh, M B', 'Sakellariadou, M']",['Scaling and Small Scale Structure in Cosmic String Networks'],['Astrophysics and Astronomy'],"['astrophysics, string', 'string, interaction', 'scaling', 'correlation function', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612135'],"['We examine the scaling properties of an evolving network of strings in Minkowski spacetime and study the evolution of length scales in terms of a 3-scale model proposed by Austin, Copeland and Kibble (ACK). We find good qualitative and some quantitative agreement between the model and our simulations. We also investigate small-scale structure by altering the minimum allowed size for loop production E_c. Certain quantities depend significantly on this parameter: for example the scaling density can vary by a factor of two or more with increasing E_c. Small-scale structure as defined by ACK disappears if no restrictions are placed on loop production, and the fractal dimension of the string changes smoothly from 2 to 1 as the resolution scale is decreased. Loops are nearly all produced at the lattice cut-off. We suggest that the lattice cut-off should be interpreted as corresponding to the string width, and that in a real network loops are actually produced with this size. This leads to a radically different string scenario, with particle production rather than gravitational radiation being the dominant mode of energy dissipation. At the very least, a better understanding of the discretisation effects in all simulations of cosmic strings is called for.']",['1996-12-16'] +2100,['eng'],"['Bergström, L']",['The AMANDA Experiment'],['Astrophysics and Astronomy'],"['talk, Sheffield 1996/09/08', 'astrophysics, missing-mass', 'neutrino, cosmic radiation', 'muon, cosmic radiation', 'correlation, time', 'radiation, laser', 'scattering, length', 'optics, absorption', 'Cherenkov counter, water', 'solids, water', 'photoelectron, amplifier', 'time resolution', 'mechanical engineering', 'deep underground detector, AMANDA']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612122'],"['At the AMANDA South Pole site, four new holes were drilled to depths 2050 m to 2180 m and instrumented with 86 photomultipliers (PMTs) at depths 1520-2000 m. Of these PMTs 79 are working, with 4-ns timing resolution and noise rates 300 to 600 Hz. Various diagnostic devices were deployed and are working. An observed factor 60 increase in scattering length and a sharpening of the distribution of arrival times of laser pulses relative to measurements at 800-1000 m showed that air bubbles are absent below 1500 m. Absorption lengths are 100 to 150 m at wavelengths in the blue and UV to 337 nm. Muon coincidences are seen between the SPASE air shower array and the AMANDA PMTs at 800-1000 m and 1500-1900 m. The muon track rate is 30 Hz for 8-fold triggers and 10 Hz for 10-fold triggers. The present array is the nucleus for a future expanded array. The potential of AMANDA for SUSY dark matter search through the detection of high-energy neutrinos from the centre of the Sun or Earth is discussed.']",['1996-12-13'] +2101,['eng'],"['Mezzacappa, A', 'Calder, A C', 'Bruenn, S W', 'Blondin, J M', 'Guidry, M W', 'Strayer, M R', 'Umar, A S']",['An Investigation of Neutrino-Driven Convection and the Core Collapse Supernova Mechanism Using Multigroup Neutrino Transport'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'model, supernova', 'neutrino, astrophysics', 'transport theory', 'entropy', 'neutrino/e, luminosity', 'antineutrino/e, luminosity', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612107'],"[""We investigate neutrino-driven convection in core collapse supernovae and its ramifications for the explosion mechanism. We begin with an ``optimistic'' 15 solar mass precollapse model, which is representative of the class of stars with compact iron cores. This model is evolved through core collapse and bounce in one dimension using multigroup (neutrino-energy--dependent) flux-limited diffusion (MGFLD) neutrino transport and Lagrangian hydrodynamics, providing realistic initial conditions for the postbounce convection and evolution. Our two-dimensional simulation begins at 106 ms after bounce at a time when there is a well-developed gain region, and proceeds for 400 ms. We couple two-dimensional (PPM) hydrodynamics to one-dimensional MGFLD neutrino transport. At 225 ms after bounce we see large-scale convection behind the shock, characterized by high-entropy, mushroom-like, expanding upflows and dense, low-entropy, finger-like downflows. The upflows reach the shock and distort it from sphericity. The radial convection velocities become supersonic just below the shock, reaching magnitudes in excess of 10^9 cm/sec. Eventually, however, the shock recedes to smaller radii, and at about 500 ms after bounce there is no evidence in our simulation of an explosion or of a developing explosion. Failure in our ``optimistic'' 15 solar mass Newtonian model leads us to conclude that it is unlikely, at least in our approximation, that neutrino-driven convection will lead to explosions for more massive stars with fatter iron cores or in cases in which general relativity is included.""]",['1996-12-11'] +2102,['eng'],"['Liddle, A R']",['The early universe'],['Astrophysics and Astronomy'],"['talk, Casablanca 1996/12/01', 'astrophysics, model', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'density, perturbation', 'gravitational radiation', 'baryon, production', 'topology, defect', 'astrophysics, missing-mass', 'black hole']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612093'],"[""An introductory account is given of the modern understanding of the physics of the early Universe. Particular emphasis is placed on the paradigm of cosmological inflation, which postulates a period of accelerated expansion during the Universe's earliest stages. Inflation provides a possible origin for structure in the Universe, such as microwave background anisotropies, galaxies and galaxy clusters; these observed structures can therefore be used to test models of inflation. A brief account is given of other early Universe topics, namely baryogenesis, topological defects, dark matter candidates and primordial black holes.""]",['1996-12-11'] +2103,['eng'],"['Sakellariadou, M']",['The Nexus between Cosmology and Elementary Particle Physics'],['Astrophysics and Astronomy'],"['talk, Pasadena 1996/11/07', 'inflationary universe', 'topology, defect', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'density, fluctuation', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612075'],"['The origin of the large scale structure in the universe - galaxies, quasars, clusters, voids, sheets - is one of the most important questions in cosmology. One can show that some non-thermal energy density fluctuations must have been present in the early universe. These fluctuations grew by gravitational instability to form the observed structures. There are at present two families of models to explain the origin of these initial fluctuations: inflationary models and topological defect scenarios. Current observational developments provide a link with theoretical predictions, allowing us to test our theoretical models. In this contribution, I present a sketch of the current status of the origin of cosmological structure formation.']",['1996-12-09'] +2104,['eng'],"['Mannheim, K']",['Hadronic $\\gamma$-ray emission models'],['Astrophysics and Astronomy'],"['talk, Heidelberg 1996/10/16', 'astrophysics, galaxy', 'hadron hadron, interaction', 'photon, emission', 'photon, cosmic radiation', 'synchrotron radiation', 'Compton scattering', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612066'],"['The discovery of rapid and simultaneous TeV/optical (UV, X-ray) variability provides strong evidence against the interaction between a thermal radiation field produced by an accretion flow and relativistic electrons in a jet as the origin of the gamma-rays in BL Lacertae objects. Synchrotron-self-Compton scattering (SSC) or proton-initiated cascades (PIC) remain viable mechanisms. The mechanisms predict very different magnetic field strengths and upper cut-off energies in the gamma-ray sources, i.e. the field strengths in SSC models are more than two orders of magnitude lower than in PIC models and the PIC spectra do not cut-off at TeV.']",['1996-12-09'] +2105,['eng'],"['Haubold, H J']",['Fourier Spectrum Analysis of the New Solar Neutrino Capture Rate Data for the Homestake Experiment'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'flux, time variation', 'neutrino nucleus, nuclear reaction', 'chlorine', 'deep underground detector, Homestake', 'talk, Notre Dame 1996/06/20']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612076'],"['The paper provides results of the Fourier spectrum analysis of the new Ar-37 production rate data of the Homestake solar neutrino experiment and compares them with results for earlier data, revealing the harmonic content in the Ar-37 production in the Homestake experiment.']",['1996-12-09'] +2106,['eng'],"['Hulth, P O']",['The Amanda Experiment'],['Astrophysics and Astronomy'],"['talk, Helsinki 1996/06/13', 'neutrino, cosmic radiation', 'photon, cosmic radiation', 'astrophysics, supernova', 'muon, cosmic radiation', 'correlation, time', 'Cherenkov counter, water', 'solids, water', 'radiation, laser', 'optics, absorption', 'scattering, length', 'photoelectron, amplifier', 'time resolution', 'radiation, laser', 'mechanical engineering', 'deep underground detector, AMANDA']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612068'],"['At the AMANDA South Pole site, four new holes were drilled to depths 2050 m to 2180 m and instrumented with 86 photomultipliers (PMTs) at depths 1520-2000 m. Of these PMTs 79 are working, with 4-ns timing resolution and noise rates 300 to 600 Hz. Various diagnostic devices were deployed and are working. An observed factor 60 increase in scattering length and a sharpening of the distribution of arrival times of laser pulses relative to measurements at 800-1000 m showed that bubbles are absent below 1500 m. Absorption lengths are 100 to 150 m at wavelengths in the blue and UV to 337 nm. Muon coincidences are seen between the SPASE air shower array and the AMANDA PMTs at 800-1000 m and 1500-1900 m. The muon track rate is 30 Hz for 8-fold triggers and 10 Hz for 10-fold triggers. The present array is the nucleus for a future expanded array.']",['1996-12-09'] +2107,['eng'],"['Waxman, E']",['Predictions of the $\\gamma$-Ray Burst Model of Ultra High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Tanashi 1996/09/25', 'cosmic radiation, primary', 'photon, cosmic radiation', 'astrophysics, model', 'cosmic radiation, acceleration', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'magnetic field', 'correlation', 'numerical calculations', '> 10**10 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612061'],"['The cosmological gamma-ray burst (GRB) model for the production of ultra- high energy cosmic rays is described, and the current observational evidence which support it discussed. Several predictions of the model are presented, which would allow it to be tested by future high energy cosmic ray and gamma- ray experiments. If the predicted signatures of the GRB model are observed, they will not only corroborate the model, but will also provide information about the source population, and will allow to investigate the unknown structure of the inter-galactic magnetic field.']",['1996-12-09'] +2108,['eng'],"['Rehm, J B', 'Raffelt, G G', 'Weiss, A']",['Primordial Nucleosynthesis with Massive $\\tau$ Neutrinos'],['Astrophysics and Astronomy'],"['light nucleus, production', 'neutrino/tau, mass', 'baryon, density', 'helium', 'deuterium', 'lithium', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612085'],"['A massive long-lived tau neutrino in the MeV regime modifies the primordial light-element abundances predicted by big-bang nucleosynthesis (BBN) calculations. This effect has been used to derive limits on the tau neutrino mass. Because recently the observational situation has become somewhat confusing and, in part, intrinsically inconsistent, we reconsider the BBN limits on the tau neutrino mass. To this end we use our newly developed BBN code to calculate the primordial abundances as a function of the tau neutrino mass and of the cosmic baryon density eta. We derive concordance regions in the eta - tau-neutrino-mass - plane for several sets of alleged primordial abundances. In some cases a concordance region exists only for a nonvanishing tau neutrino mass. At the present time BBN does not provide clear evidence for or against a tau neutrino mass.']",['1996-12-10'] +2109,['eng'],"['Haxton, W C', 'Langanke, K', 'Qian, Y Z', 'Vogel, P']",['Neutrino-induced nucleosynthesis and the site of the r-process'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'nucleus, production', 'n, capture', 'neutrino, astrophysics', 'neutrino, flux', 'n, matter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612047'],"['If the r-process occurs deep within a Type II supernova, probably the most popular of the proposed sites, abundances of r-process elements may be altered by the intense neutrino flux. We point out that the effects would be especially pronounced for 8 isotopes that can be efficiently synthesized by the neutrino reactions following r-process freeze-out. We show that the observed abundances of these isotopes are entirely consistent with neutrino-induced nucleosynthesis, strongly arguing for a supernova r-process site. The deduced fluences place stringent constraints on the freeze-out radius and dynamic timescale of the r-process.']",['1996-12-05'] +2110,['eng'],"['Bradbury, S M', 'Deckers, T', 'Petry, D', 'Konopelko, A K']",['Detection of $\\gamma$-Rays above 1.5 TeV from Mkn 501'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'Cherenkov counter, imaging', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612058'],"['A detection of TeV gamma-rays from Mkn 501 is reported, based on observations made between March and August 1996 with the first HEGRA Cherenkov telescope (CT1). From the image analysis, 351 excess candidate gamma-ray events are obtained from the 147 h dataset. The statistical significance of the excess is 5.2 sigma. The average excess rate is 2.4 \\pm 0.5 h^{-1} above the $\\approx$ 1.5 TeV threshold of CT1. Under the assumption that the spectrum of Mkn 501 follows a power law we find a differential spectral index of 2.6 \\pm 0.5 and obtain a time-averaged integral flux above 1.5 TeV of $2.3 (\\pm 0.4)_{Stat} (+1.5-0.6)_{Syst} \\times 10^{-12}$ cm^{-2}s^{-1}. Comparison with our near contemporary observations of the Crab Nebula, used as a standard candle to test CT1 after upgrading to a 127 pixel camera, indicates that Mkn 501 has a spectrum similar to that of the Crab Nebula above 1.5 TeV. The integral flux above 1.5 TeV from Mkn 501 is found to have been between 2.2 and 3.6 times smaller than that from the Crab Nebula. HEGRA is the second experiment to have detected Mkn 501 in the TeV range.']",['1996-12-06'] +2111,['eng'],"['Albrecht, Andreas']",['How to falsify scenarios with primordial fluctuations from inflation'],['Astrophysics and Astronomy'],"['talk, Princeton 1996/06/24', 'inflationary universe', 'matter, density', 'spectra, perturbation', 'spectra, fluctuation', 'cosmic radiation, background', 'coherence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612017'],"[""I argue that the proposition that primordial perturbations were produced by inflation is most definitely falsifyable. Far from ``predicting anything you want'', the Gaussianity and passivity of inflationary perturbations strongly constrain the possible outcomes. For example, the next generation of CMB satellites could easily prove that the perturbations do not have an inflationary origin.""]",['1996-12-04'] +2112,['eng'],"['Nagasawa, M', 'Yokoyama, J']",['On the Jeans Instability During the QCD Phase Transition'],['Astrophysics and Astronomy'],"['astrophysics, model', 'quantum chromodynamics', 'critical phenomena', 'transition, quark hadron', 'density, fluctuation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612014'],"['The Jeans scale is estimated during the coexistence epoch of quark-gluon and hadron phases in the first-order QCD phase transition. It is shown that, contrary to the previous claims, reduction of the sound speed is so little that the phase transition does not affect evolution of cosmological density fluctuations appreciably.']",['1996-12-04'] +2113,['eng'],"['Gibilisco, M']",['Reionization of the Universe induced by Primordial Black Holes'],['Astrophysics and Astronomy'],"['black hole, mass', 'mass, black hole', 'ionization', 'photon, emission', 'emission, photon', 'plasma, temperature', 'differential equations, solution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611227'],"['In this paper I will discuss the possibility of a reionization of the Universe due to the photons emitted by evaporating primordial black holes (PBHs); this process should happen during the last stages of the PBHs life, when the particle emission is very intense. I will study the time evolution of the ionization degree x, of the plasma temperature $T_{e}$ and of the photon number density $n_{\\gamma}$ characterizing the Universe after the recombination epoch: a system of coupled differential equations for these variables is solved in an analytical way by assuming, as a photon source, PBHs having an initial mass $M\\sim 10^{14}$ g. The results I obtain prove that such a kind of reionization is possible, being able to increase the ionization degree of the Universe from a value x=0.002 (just after the recombination) to values near 1 (when the black holes evaporation ends).']",['1996-11-28'] +2114,['eng'],"['Sakellariadou, M']",['Can Doppler Peaks discriminate among Inflationary models and Topological Defect scenarios ?'],['Astrophysics and Astronomy'],"['talk, Ascona 1996/05/26', 'inflationary universe', 'topology, defect', 'cosmic radiation, background', 'density, perturbation', 'field theory, scalar', 'field theory, fluctuation', 'astrophysics, texture', 'coherence', 'Doppler effect', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612004'],"['Doppler peaks in the cosmic microwave background may allow us to distinguish among the two classes of theories-inflationary models and topological defect scenarios-which attempt to explain the origin of structure formation in the universe. We consider density perturbations seeded by global textures in a universe dominated by cold dark matter. We calculate the height and the position of the primary peak and conclude a different signature than the one obtained if the initial perturbations were due to the amplification of quantum fluctuations of a scalar field during a generic inflationary era. We believe that our analysis holds for all kinds of global defects and general global scalar fields. We then question the validity of the temporal coherence of the sources, assumed in the texture models. We finally discuss the temporal coherence of cosmic string sources, through correlations of the energy and momentum in an evolving cosmic string network in Minkowski space.']",['1996-12-02'] +2115,['eng'],"['Blanco-Pillado, J J', 'Vázquez, R A', 'Zas, E']",['Limits on Topological Defect Neutrino fluxes from Horizontal Air Shower measurements'],['Astrophysics and Astronomy'],"['neutrino, flux', 'topology, defect', 'showers, air', 'muon, showers', 'astrophysics, string', 'superconducting', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612010'],"['We obtain the horizontal air shower rate from the (EeV) high energy neutrino flux predicted in some topological defect scenarios as the source for the highest energy cosmic rays. Emphasis is made on the different character of the events depending on the neutrino flavor an type of interaction. We show that the bound for muon poor showers in the $10^5-10^7$ GeV energy range is violated by maximal predictions for superconducting cosmic string neutrino fluxes, we compare it to other neutrino flux limits and we discuss the future of such measurements to further constrain these models.']",['1996-12-02'] +2116,['eng'],"['Malaney, R A']",['Evolution of the Cosmic Gas and the Relic Supernova Neutrino Background'],['Astrophysics and Astronomy'],"['astrophysics, gas', 'supernova', 'neutrino, cosmic radiation', 'neutrino, flux', 'galaxy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9612012'],"['Using the redshift evolution of the cosmic gas, as inferred from QSO absorption line studies, we calculate the past supernova rate and the relic supernova neutrino background. Using this new technique we find the predicted relic neutrino flux at low energies to be at least an order of magnitude below previous estimates. We argue that the evolution of the cosmic gas is consistent with a large decrease in the number of early-type galaxies at redshifts $\\sim 3$, and that this evolution is the source of the reduction in the predicted neutrino flux. Additional observational constraints from recent redshift surveys lead us to propose a modified model for the evolution of the cosmic gas in which significant infall at low redshift occurs. We discuss the possible relevance of our calculations to the X-ray emitting metal-enriched gas observed in the intergalactic medium.']",['1996-12-02'] +2117,['eng'],"['Mori, M']",['The Galactic Diffuse $\\gamma$-ray Spectrum from Cosmic-ray Proton Interactions'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'cosmic radiation, flux', 'p, cosmic radiation', 'p p, interaction', 'nucleus nucleus, nuclear reaction', 'pi0, hadroproduction', 'pi0, radiative decay', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611233'],"['A new calculation of the Galactic diffuse gamma-ray spectrum from the decay of secondary particles produced by interactions of cosmic-ray protons with interstellar matter is presented. The calculation utilizes the modern Monte Carlo event generators, Hadrin, Fritiof and Pythia, which simulate high-energy proton-proton collisions and are widely used in studies of nuclear and particle physics, in addition to scaling calculation. This study is motivated by the result on the Galactic diffuse gamma-ray flux observed by the EGRET detector on the Compton Gamma-ray Observatory, which indicates an excess above about 1 GeV of the observed intensity compared with a model prediction. The prediction is based on cosmic-ray interactions with interstellar matter, in which secondary pion productions are treated by a simple model. With the improved interaction model used here, however, the diffuse gamma-ray flux agrees rather well with previous calculations within uncertainties, which mainly come from the unobservable demodulated cosmic-ray spectrum in interstellar space. As a possible solution to the excess flux, flatter spectra of cosmic-ray protons have been tested and we found that the power-law spectrum with an index of about $-(2.4\\sim2.5)$ gives a better fit to the EGRET data, though the spectrum is not explained completely.']",['1996-11-28'] +2118,['eng'],"['Sarkar, S']",['Primordial Nucleosynthesis and Dark Matter'],['Astrophysics and Astronomy'],"['talk, Heidelberg 1996/09/16', 'astrophysics, missing-mass', 'light nucleus, production', 'helium, density', 'deuterium, density', 'nucleon, density', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611232'],"['The cosmological abundance of nucleons determined from considerations of Big Bang nucleosynthesis allegedly provides compelling evidence for non-nucleonic dark matter. Recent developments in measurements of primordial light element abundances, in particular deuterium and helium, require reexamination of this important issue. The present situation is uncertain but exciting.']",['1996-11-28'] +2119,['eng'],"['Maartens, R', 'Méndez, V']",['Nonlinear bulk viscosity and inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'thermodynamics, viscosity', 'entropy', 'model, fluid', 'transport theory']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611205'],"['We develop a nonlinear generalisation of the causal linear thermodynamics of bulk viscosity, incorporating positivity of the entropy production rate and the effective specific entropy. The theory is applied to viscous fluid inflation (which is necessarily far from equilibrium), and we find thermodynamically consistent inflationary solutions, both exponential and power-law.']",['1996-11-26'] +2120,['eng'],"['Antoniadis, Ignatios', 'Mazur, P O', 'Mottola, E']",['Conformal Invariance and Cosmic Background Radiation'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, spectra', 'statistics', 'density, fluctuation', 'invariance, conformal', 'correlation function', 'anomaly', 'numerical calculations']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611208', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=capp98&id=antoniadis']","[""The spectrum and statistics of the cosmic microwave background radiation (CMBR) are investigated under the hypothesis that scale invariance of the primordial density fluctuations should be promoted to full conformal invariance. As in the theory of critical phenomena, this hypothesis leads in general to deviations from naive scaling. The spectral index of the two-point function of density fluctuations is given in terms of the quantum trace anomaly and is greater than one, leading to less power at large distance scales than a strict Harrison-Zel'dovich spectrum. Conformal invariance also implies non-gaussian statistics for the higher point correlations and in particular, it completely determines the large angular dependence of the three-point correlations of the CMBR.""]",['1996-11-26'] +2121,['eng'],"['Schmid, C', 'Schwarz, Dominik J', 'Widerin, P']","[""Deviations from the Harrison-Zel'dovich spectrum due to the Quark-Gluon to Hadron Transition""]",['Astrophysics and Astronomy'],"['talk, Ascona 1996/05/26', 'astrophysics, model', 'critical phenomena', 'transition, quark hadron', 'transition, gluon hadron', 'density, perturbation', 'model, fluid', 'astrophysics, missing-mass', 'quantum chromodynamics', 'quark gluon, plasma', 'supersymmetry', 'postulated particle, LSP', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611186'],"[""We investigate the effect of the quark-gluon to hadron transition on the evolution of cosmological perturbations. If the phase transition is first order, the sound speed vanishes during the transition, and density perturbations fall freely. The primordial Harrison-Zel'dovich density fluctuations for scales below the Hubble radius at the transition develop peaks, which grow linearly with the wavenumber, both for the hadron-photon-lepton fluid and for cold dark matter. The large peaks in the spectrum produce cold dark matter clumps of $10^{-8}$ to $10^{-11} M_\\odot$.""]",['1996-11-25'] +2122,['eng'],"['Sigl, G']",['Topological Defect Models of Ultra-High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['talk, Erice 1996/06/16', 'cosmic radiation, production', 'particle, massive', 'particle, decay', 'topology, defect', 'cosmic radiation, flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611190'],"['We give an overview over models in which cosmic rays above 1 EeV = 10**(18) eV are produced by the decay of supermassive ""X"" particles released from topological defects possibly created in cosmological phase transitions. We note that, for an interesting particle physics parameter range, these models are still consistent with current data, and discuss signatures for the topological defect mechanism which can be tested by the next generation experiments.']",['1996-11-25'] +2123,['eng'],"['Spergel, D N', 'Pen, U L']",['Cosmology in a String-Dominated Universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'string model, nonabelian', 'matter, density', 'crystal', 'cosmic radiation, fluctuation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611198'],"['The string-dominated universe locally resembles an open universe, and fits dynamical measures of power spectra, cluster abundances, redshift distortions, lensing constraints, luminosity and angular diameter distance relations and microwave background observations. We show examples of networks which might give rise to recent string-domination without requiring any fine-tuned parameters. We discuss how future observations can distinguish this model from other cosmologies.']",['1996-11-25'] +2124,['eng'],"['Giazotto, A', 'Bonazzola, S', 'Gourgoulhon, E']",['On gravitational waves emitted by an ensemble of rotating neutron stars'],['Astrophysics and Astronomy'],"['gravitational radiation, measurement', 'counters and detectors, interference', 'n, matter', 'background', 'astrophysics, galaxy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611188'],"[""We study the possibility to detect the gravitational wave background generated by all the neutron stars in the Galaxy with only one gravitational wave interferometric detector. The proposed strategy consists in squaring the detector's output and searching for a sidereal modulation. The shape of the squared signal is computed for a disk and a halo distribution of neutron stars. The required noise stability of the interferometric detector is discussed. We argue that a possible population of old neutron stars, originating from a high stellar formation rate at the birth of the Galaxy and not emitting as radio pulsars, could be detected by the proposed technique in the low frequency range of interferometric experiments.""]",['1996-11-25'] +2125,['eng'],"['Horváth, J E', 'Pacheco, J A F']",['Equilibrium configurations for quark-diquark stars and the problem of Her X-1 mass'],['Astrophysics and Astronomy'],"['astrophysics, model', 'plasma, diquark', 'quark, plasma', 'vacuum state', 'baryon, density', 'n, matter', 'mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611167'],"['We report new calculations of the physical properties of a quark-diquark plasma. A vacuum contribution is taken into account and is responsible for the appearance of a stable state at zero pressure and at a baryon density of about 2.2 times the nuclear matter density in this model. The resulting equation of state was used to integrate numerically the Tolman-Oppenheimer-Volkoff equations. The mass-radius relationship has been derived from a series of equilibrium configurations constituted by a mixture of quarks and diquarks. These stellar models, which are representative of a whole class, may be helpful to understand the possible compactness of the X-ray source Her X-1 and related objects.']",['1996-11-21'] +2126,['eng'],"['Lindner, A']",['A New Method to Reconstruct the Energy and Determine the Composition of Cosmic Rays from the Measurement of Cherenkov Light and Particle Densities in Extended Air Showers'],['Astrophysics and Astronomy'],"['talk, Lodz 1996/07/15', 'elements, cosmic radiation', 'cosmic radiation, primary', 'cosmic radiation, energy', 'showers, air', 'showers, spatial distribution', 'cosmic radiation, electromagnetic component', 'particle, density', 'Cherenkov counter', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611175'],['A Monte-Carlo study is presented using ground based measurements of the electromagnetic part of showers initiated in the atmosphere by high energetic cosmic rays to reconstruct energy and mass of primary particles with energies above 300 TeV. With two detector arrays measuring Cherenkov light and particle densities as realized in the HEGRA experiment shower properties are reconstructed and interpreted to determine energy and energy per nucleon of the primary particle.'],['1996-11-22'] +2127,['eng'],"['Zimdahl, W', 'Pavón, D', 'Maartens, R']",['Reheating and causal thermodynamics'],['Astrophysics and Astronomy'],"['inflationary universe', 'model, fluid', 'thermodynamics', 'causality', 'temperature', 'decay, width', 'expansion, perturbation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611147'],"['The reheating process in inflationary universe models is considered as an out-of-equilibrium mixture of two interacting and reacting fluids, and studied within the framework of causal, irreversible thermodynamics. The evolution of the temperature and the decay rate as determined by causal thermodynamics are estimated at different stages of the process. A simple model is also used to find the perturbations of the expansion rate, including the possibility of damped oscillations.']",['1996-11-20'] +2128,['eng'],"['Mignola, G']",['Cosmic Antiprotons from Neutralino Annihilation in the Galactic halo'],['Astrophysics and Astronomy'],"['talk, Sheffield 1996/09/08', 'astrophysics, galaxy', 'supersymmetry', 'neutralino, annihilation', 'p, cosmic radiation', 'anti-p, cosmic radiation', 'ratio, (anti-p p)', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611138'],"['We investigate the possibility that the antiproton-to-proton flux ratio which is measured in cosmic rays may be generated by neutralino-neutralino annihilation in the galactic halo. We study the most general compositions for the relic neutralinos. We compare our results with the present experimental sensitivity and find that the theoretical predictions are at the level of the current experimental limits for some regions in the parameter space of the model.We expect that the future measurements of the pbar/p will provide very useful information, complementary to the ones obtainable with other experimental means.']",['1996-11-19'] +2129,['eng'],"['Fuller, G M', 'Qian, Y Z']",['Neutrino Gravitational Redshift and the Electron Fraction Above Nascent Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'neutrino, energy spectrum', 'antineutrino, energy spectrum', 'electron, density', 'astrophysics, supernova', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611126'],"['Neutrinos emitted from near the surface of the hot proto-neutron star produced by a supernova explosion may be subject to significant gravitational redshift at late times. Electron antineutrinos decouple deeper in the gravitational potential well of the neutron star than do the electron neutrinos, so that the electron antineutrinos experience a larger redshift effect than do the electron neutrinos. We show how this differential redshift can increase the electron fraction Ye in the neutrino-heated ejecta from the neutron star. Any r-process nucleosynthesis originating in the neutrino-heated ejecta would require a low Ye, implying that the differential redshift effect cannot be too large. In turn, this effect may allow nucleosynthesis to probe the nuclear equation of state parameters which set the neutron star radius and surface density scale height at times of order tpb = 10 to 25 s after core bounce.']",['1996-11-18'] +2130,['eng'],"['Bullock, J S', 'Primack, Joel R']",['Non-Gaussian Fluctuations and Primordial Black Holes from Inflation'],['Astrophysics and Astronomy'],"['black hole, production', 'density, fluctuation', 'inflationary universe, stochastic', 'statistics', 'spectra', 'potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611106'],"[""We explore the role of non-Gaussian fluctuations in primordial black hole (PBH) formation and show that the standard Gaussian assumption, used in all PBH formation papers to date, is not justified. Since large spikes in power are usually associated with flat regions of the inflaton potential, quantum fluctuations become more important in the field dynamics, leading to mode-mode coupling and non-Gaussian statistics. Moreover, PBH production requires several sigma (rare) fluctuations in order to prevent premature matter dominance of the universe, so we are necessarily concerned with distribution tails, where any intrinsic skewness will be especially important. We quantify this argument by using the stochastic slow-roll equation and a relatively simple analytic method to obtain the final distribution of fluctuations. We work out several examples with toy models that produce PBH's, and show that the naive Gaussian assumption can result in errors of many orders of magnitude. For models with spikes in power, our calculations give sharp cut-offs in the probability of large positive fluctuations, meaning that Gaussian distributions would vastly over-produce PBH's. The standard results that link inflation-produced power spectra and PBH number densities must then be reconsidered, since they rely quite heavily on the Gaussian assumption. We point out that since the probability distributions depend on the nature of the potential, it is impossible to obtain results for general models. However, calculating the distribution of fluctuations for any specific model seems to be relatively straightforward, at least in the single inflaton case.""]",['1996-11-14'] +2131,['eng'],"['Qian, Y Z']",['Neutrino-nucleus interaction and supernova r-process nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Notre Dame 1996/06/20', 'astrophysics, supernova', 'light nucleus, production', 'neutrino nucleus, interaction', 'electron, density', 'helium, effect', 'neutrino/e, capture']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611098'],"['We discuss various neutrino-nucleus interactions in connection with the supernova r-process nucleosynthesis, which possibly occurs in the neutrino-driven wind of a young neutron star. These interactions include absorptions of electron neutrinos and antineutrinos on free nucleons, electron-neutrino captures on neutron-rich nuclei, and neutral-current interactions of heavy-flavor neutrinos with alpha particles and neutron-rich nuclei. We describe how these interactions can affect the r-process nucleosynthesis and discuss the implications of their effects for the physical conditions leading to a successful supernova r-process. We conclude that a low electron fraction and/or a short dynamic time scale may be required to give the sufficient neutron-to-seed ratio for an r-process in the neutrino-driven wind. In the case of a short dynamic time scale, the wind has to be contained during the r-process. Possible mechanisms which can give a low electron fraction or contain the wind are discussed.']",['1996-11-14'] +2132,['eng'],"['Hoffman, R D', 'Woosley, S E', 'Qian, Y Z']","['Nucleosynthesis in neutrino-driven winds; 2, Implications for heavy element synthesis']",['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, luminosity', 'n, matter', 'nucleus, production', 'thermodynamics', 'nuclear reaction', 'neural network', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611097'],"['During the first 20 seconds of its life, the enormous neutrino luminosity of a neutron star drives appreciable mass loss from its surface. This neutrino-driven wind has been previously identified as a likely site for the r-process. Qian & Woosley (1996) have derived, both analytically and numerically, the physical conditions relevant for heavy element synthesis in the wind. These conditions include the entropy (S), the electron fraction (Ye), the dynamic time scale, and the mass loss rate. Here we explore the implications of these conditions for nucleosynthesis. We find that the standard wind models derived in that paper are inadequate to make the r-process, though they do produce some rare species above the iron group. We further determine the general restrictions on the entropy, the electron fraction, and the dynamic time scale that are required to make the r-process. In particular, we derive from nuclear reaction network calculations the conditions required to give a sufficient neutron-to-seed ratio for production of the platinum peak. These conditions range from Ye = 0.2 and S < 100 per baryon for reasonable dynamic time scales of 0.001-0.1 s, to Ye = 0.4-0.495 and S > 400 per baryon for a dynamic time scale of 0.1 s. These conditions are also derived analytically to illustrate the physics determining the neutron-to-seed ratio.']",['1996-11-14'] +2133,['eng'],"['Vitale, S', 'Cerdonio, M', 'Coccia, E', 'Ortolan, A']",['Gravitational-Wave Stochastic Background Detection with Resonant-Mass Detectors'],['Astrophysics and Astronomy'],"['gravitational radiation, background', 'gravitational radiation, stochastic', 'optics, interference', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611088'],"['In this paper we discuss how the standard optimal Wiener filter theory can be applied, within a linear approximation, to the detection of an isotropic stochastic gravitational-wave background with two or more detectors. We apply then the method to the AURIGA-NAUTILUS pair of ultra low temperature bar detectors, near to operate in coincidence in Italy, obtaining an estimate for the sensitivity to the background spectral density of $\\simeq 10^{-49}\\ Hz^{-1}$, that converts to an energy density per unit logarithmic frequency of kg/m^3$ the closure density of the Universe. We also show that by adding the VIRGO interferometric detector under construction in Italy to the array, and by properly re- orienting the detectors, one can reach a sensitivity of $\\simeq 6 one large mass spherical detector properly located in one of the nearby available sites in Italy can reah a sensitivity of $\\simeq 2\\times10^{-5}\\times and NAUTILUS can achieve sensitivities of $\\simeq 2 \\times10^{-6}\\rho_c$.']",['1996-11-14'] +2134,['eng'],"['Qian, Y Z', 'Woosley, S E']","['Nucleosynthesis in neutrino-driven winds; 1, The physical conditions']",['Astrophysics and Astronomy'],"['light nucleus, production', 'neutrino, luminosity', 'baryon, entropy', 'n, matter', 'electron, density', 'astrophysics, supernova', 'model, hydrodynamical', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611094'],"['During the first 20 seconds of its life, the enormous neutrino luminosity of a neutron star drives appreciable mass loss from its surface. Previous investigations have shown that this neutrino-driven wind could be the site where the r-process occurs. The nucleosynthesis is sensitive to four physical parameters characterizing the wind: its mass loss rate, the entropy per baryon, the electron fraction, and the dynamic time scale. Different authors, using numerical models for supernovae, have arrived at qualitatively different values for these key parameters. Here we derive their values analytically and test our analytic results by numerical calculations using an implicit hydrodynamic code. Employing our analytic and numerical methods, we also investigate how various factors can affect our results. The derived entropy typically falls short, by a factor of two to three, of the value required to produce a strong r-process. Various factors that might give a higher entropy or a more rapid expansion in the wind are discussed.']",['1996-11-14'] +2135,['eng'],"['Bahcall, N A']",['Dark Matter'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, missing-mass', 'baryon, matter', 'astrophysics, galaxy', 'astrophysics, cluster', 'gravitation, lens', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611080'],"['Observations in the optical, in X-rays, and gravitational lensing of galaxies, clusters of galaxies, and large-scale structure are beginning to provide clues to the dark matter problem. I review the impact of these observations on some of the main questions relating to dark matter: How much dark matter is there? Where is it located? What is the nature of the dark matter? and what is the amount of baryonic dark matter.']",['1996-11-12'] +2136,['eng'],"['Chakrabarti, S K']",['New Twists In The Study Of Gravity Wave Emission In Systems With Massive Black Holes'],['Astrophysics and Astronomy'],"['talk, Brisbane 1994/07/04', 'gravitational radiation', 'black hole', 'angular momentum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611075'],"['Traditionlly, gravitational wave emission from a coalescing binary system is computed using point mass approximations without considering any accretion disk. However, it is believed that in many of the galactic nuclei, there are supermassive central black holes surrounded by accretion disks. These accretion disks must be necessarily supersonic on and outside the horizon simply because the radial velocity (in the corotating frame) has to be the velocity of light on the horizon while the sound speed must be smaller. However, supersonic flows are typically sub-Keplerian. Thus, smaller black holes and neutron stars (which are on instantaneously Keplerian orbit and lose energy and angular momentum through gravitational radiation) on their way to coalesce with the central black hole must accrete negative angular momentum from the disk. We study here the way these disks affect the gravitational wave emission.']",['1996-11-11'] +2137,['eng'],"['Ruffert, M', 'Rampp, M', 'Janka, H T']",['Coalescing neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'coalescence', 'gravitational radiation', 'effect, back reaction', 'model, hydrodynamical', 'energy spectrum', 'luminosity', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611056'],"[""The dynamics, time evolution of the mass distribution, and gravitational wave signature of coalescing neutron stars described by polytropes are compared with three simulations published previously: (a) ``Run 2'' of Zhuge et al. (1994), (b) ``Model III'' of Shibata et al. (1992), and (c) ``Model A64'' of Ruffert et al. (1996). We aim at studying the differences due to the use of different numerical methods, different implementations of the gravitational wave backreaction, and different equations of state. Comparison (a) confronts the results of our grid-based PPM scheme with those from an SPH code. We found that due to the lower numerical viscosity of the PPM code, the post-merging oscillations and pulsations could be followed for a longer time and lead to larger secondary and tertiary maxima of the gravitational wave luminosity. In case (b) two grid based codes with the same backreaction formalism but differing hydrodynamic integrators and different numerical resolution are compared. Satisfactory agreement of the amplitude of the gravitational wave luminosity is established, although due to the different initial conditions a small time delay develops in the onset of the dynamical instability. In (c) we find that using a polytropic equation of state instead of the high-density equation of state of Lattimer & Swesty (1991) does not change the overall dynamical evolution of the merger and yields agreement of the gravitational wave signature to within 20% accuracy. However, differences of the structure and evolution of the outer layers of the neutron stars are present, which has important implications for questions like mass loss and disk formation during the merging of binary neutron stars.""]",['1996-11-08'] +2138,['eng'],"['Krawczynski, H', 'Funk, B', 'Barthelmy, S D', 'Butterworth, P S', 'Cline, T', 'Gehrels, N', 'Kouveliotou, C', 'Fishman, J', 'Meegan, C A']",['Search for TeV Counterparts of $\\gamma$-Ray Bursts with the HEGRA Experiment'],['Astrophysics and Astronomy'],"['talk, Erice 1996/06/16', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'correlation, time', 'photon, showers', 'shower detector, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611044'],"['The HEGRA experiment is an air shower detector system for the study of neutral and charged cosmic rays in the energy range between 500 GeV to 10 PeV. Here we give an overview of how the HEGRA detector is used to search for TeV gamma-radiation associated with Gamma-Ray Bursts (GRBs) registered with the Burst And Transient Source Experiment (BATSE) on board the Compton Gamma-Ray Observatory. Furthermore, results of an archival search for GRB radiation above 15 TeV carried out with the HEGRA air shower arrays are shown. We conclude with a summary of the search activities planned for the future.']",['1996-11-07'] +2139,['eng'],"['Bottino, A', 'Fornengo, N', 'Mignola, G', 'Olechowski, M', 'Scopel, S']",['Perspectives for Detection of a Higgsino-like Relic Neutralino'],['Astrophysics and Astronomy'],"['anti-p p, inclusive reaction', 'electron, pair production', 'positron, pair production', 'supersymmetry', 'sparticle, pair production', 'selectron', 'sparticle, decay modes', 'neutrino', 'postulated particle, LSP', 'postulated particle, Higgsino', 'sparticle, search for', 'astrophysics, missing-mass', 'sparticle, annihilation', 'muon, flux', 'neutrino, solar', 'p, cosmic radiation', 'anti-p, cosmic radiation', 'cosmic radiation, flux', 'scattering, nucleon sparticle', 'numerical calculations', 'anti-p p --> positron electron 2photon anything']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611030'],"[""It has been conjectured by Ambrosanio, Kane, Kribs, Martin and Mrenna (AKM) that the CDF event $p \\bar p \\to e^+ e^- \\gamma \\gamma + missing E_T$ is due to a decay chain involving two neutralino states (the lightest and the next-to-lightest ones). The lightest neutralino ($\\chi_{AKM}$) has been further considered by Kane and Wells as a candidate for cold dark matter. In this paper we examine the properties of relic $\\chi_{AKM}$'s in their full parameter space, and examine the perspectives for detection by comparing theoretical predictions to sensitivities of various experimental searches. We find that for most regions of the parameter space the detectability of a relic $\\chi_{AKM}$ would require quite substantial improvements in current experimental sensitivities. The measurements of neutrino fluxes from the center of the Earth and of an excess of $\\bar{p}/p$ in cosmic rays are shown to offer some favorable perspectives for investigating a region of the the model.""]",['1996-11-06'] +2140,['eng'],"['Dar, Arnon']",['Standard Physics Solution To The Solar Neutrino Problem?'],['Astrophysics and Astronomy'],"['talk, Helsinki 1996/06/13', 'talk, Zuoz 1996/08/04', 'talk, Faro 1996/09/08', 'model, solar', 'neutrino, solar', 'neutrino, flux', 'boron', 'electroweak interaction', 'beryllium', 'neutrino, oscillation', 'resonance, oscillation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611014'],"['The $^8$B solar neutrino flux predicted by the standard solar model (SSM) is consistent within the theoretical and experimental uncertainties with that observed at Kamiokande. The Gallium and Chlorine solar neutrino experiments, however, seem to imply that the $^7$Be solar neutrino flux is strongly suppressed compared with that predicted by the SSM. If the $^7$Be solar neutrino flux is suppressed, still it can be due to astrophysical effects not included in the simplistic SSM. Such effects include short term fluctuations or periodic variation of the temperature in the solar core, rotational mixing of $^3$He in the solar core, and dense plasma effects which may strongly enhance p-capture by $^7$Be relative to e-capture. The new generation of solar observations which already look non stop deep into the sun, like Superkamiokande through neutrinos, and SOHO and GONG through acoustic waves, may point at the correct solution. Only Superkamiokande and/or future solar neutrino experiments, such as SNO, BOREXINO and HELLAZ, will be able to find out whether the solar neutrino problem is caused by neutrino properties beyond the minimal standard electroweak model or whether it is just a problem of the too simplistic standard solar model.']",['1996-11-05'] +2141,['eng'],"['Keil, W', 'Janka, H T', 'Müller, E']",['Ledoux-Convection in Protoneutron Stars'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'n, matter', 'light nucleus, production', 'model, hydrodynamical', 'model, turbulence', 'neutrino/e, luminosity', 'antineutrino/e', 'energy spectrum, (neutrino)', 'lepton, flux', 'temperature', 'time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610203'],"['Two-dimensional hydrodynamical simulations of the deleptonization of a newly formed neutron star were performed. Driven by negative lepton fraction and entropy gradients, convection starts near the neutrinosphere about 20-30 ms after core bounce, but moves deeper into the protoneutron star, and after about one second the whole protoneutron star is convective. The deleptonization of the star proceeds much faster than in the corresponding spherically symmetrical model because the lepton flux and the neutrino luminosities increase by up to a factor of two. The convection below the neutrinosphere raises the neutrinospheric temperatures and mean energies of the emitted neutrinos by 10-20%. This can have important implications for the supernova explosion mechanism and changes the detectable neutrino signal from the Kelvin-Helmholtz cooling of the protoneutron star. In particular, the enhanced electron neutrino flux relative to the electron antineutrino flux during the early post-bounce evolution might solve the overproduction problem of certain elements in the neutrino-heated ejecta in models of type-II supernova explosions.']",['1996-10-28'] +2142,['eng'],"['Kumar, P', 'Quataert, E J']",['Angular momentum transport by gravity waves and its effect on the rotation of the solar interior'],['Astrophysics and Astronomy'],"['gravitational radiation', 'matter, solar', 'angular momentum, effect', 'matter, rotator', 'energy, luminosity', 'excited state, turbulence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611006'],"[""We calculate the excitation of low frequency gravity waves by turbulent convection in the sun and the effect of the angular momentum carried by these waves on the rotation profile of the sun's radiative interior. We find that the gravity waves generated by convection in the sun provide a very efficient means of coupling the rotation in the radiative interior to that of the convection zone. In a differentially rotating star, waves of different azimuthal number have their frequencies in the local rest frame of the star Doppler shifted by different amounts. This leads to a difference in their local dissipation rate and hence a redistribution of angular momentum in the star. We find that the time scale for establishing uniform rotation throughout much of the radiative interior of the sun is $\\sim 10^7$ years, which provides a possible explanation for the helioseismic observations that the solar interior is rotating as a solid body.""]",['1996-11-04'] +2143,['eng'],"['Berezinsky, Veniamin Sergeevich']",['Dark matter particles'],['Astrophysics and Astronomy'],"['talk, Helsinki 1996/06/13', 'astrophysics, missing-mass', 'astrophysics, model', 'astrophysics, MACHO', 'baryon', 'neutralino', 'axino', 'mass, axion', 'upper limit', 'supersymmetry', 'grand unified theory', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610263'],"['The baryonic and cold dark matter are reviewed in the context of cosmological models. The theoretical search for the particle candidates is limited by supersymmetric extension of the Standard Model. Generically in such models there are just two candidates associated with each other: generalized neutralino, which components are usual neutralino and axino, and axion which is a partner of axino in supermultiplet. The status of these particles as DM candidates is described.']",['1996-11-01'] +2144,['eng'],"['Bahcall, J N', 'Pinsonneault, M H', 'Basu, S', 'Christensen-Dalsgaard, J']",['Are Standard Solar Models Reliable?'],['Astrophysics and Astronomy'],"['model, solar', 'neutrino, solar', 'neutrino, flux', 'diffusion', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610250'],"['The sound speeds of solar models that include element diffusion agree with helioseismological measurements to a rms discrepancy of better than 0.2% throughout almost the entire sun. Models that do not include diffusion, or in which the interior of the sun is assumed to be significantly mixed, are effectively ruled out by helioseismology. Standard solar models predict the measured properties of the sun more accurately than is required for applications involving solar neutrinos.']",['1996-10-31'] +2145,['eng'],"['Dar, Arnon', 'Laor, A']",['Hadronic Production of TeV $\\gamma$ Ray Flares From Blazars'],['Astrophysics and Astronomy'],"['astrophysics, blazar', 'photon, cosmic radiation', 'p p, interaction', 'photon, hadroproduction', 'p, jet', 'neutrino, emission', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610252'],"['We propose that TeV $\\gamma$-ray emission from blazars is produced by collisions close to the line of sight of high energy jet protons with clouds from the broad emission-line region (BLR). Quasi quiescent emission is produced when the jet interacts with relatively many distant clouds in the BLR. Strong TeV $\\gamma$-ray flares (GRFs) are produced when BLR clouds cross the line of sight at much closer distances. The observed properties of both the quasi quiescent emission and the GRFs are well reproduced, including those of the recently reported very short and strong TeV GRFs from the blazar Markarian 421. An hadronic origin of the TeV $\\gamma$-ray emission from blazars implies that it is accompanied by a simultaneous emission of high energy neutrinos, electrons and positrons with similar intensities, light curves and energy spectra. The cooling of the hadronicly produced electrons and positrons by emission of synchrotron radiation and inverse Compton scattering produces delayed emission of optical photons, X-rays and $\\gamma$-rays.']",['1996-10-31'] +2146,['eng'],"['Collar, J I', 'Girard, T A', 'Limagne, D', 'Waysand, G']",['Superheated Droplet Detectors as CDM Detectors'],['Astrophysics and Astronomy'],"['talk, Sheffield 1996/09/08', 'astrophysics, missing-mass', 'sparticle, neutral particle', 'postulated particle, WIMP', 'superconducting, droplet', 'fluorine', 'background', 'n, flux', 'proposed experiment', 'deep underground detector', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610266'],"[""Superheated Droplet Detectors (SDDs) are becoming commonplace in neutron personnel dosimetry. Their total insensitivity to minimum ionizing radiation (while responsive to nuclear recoils of energies ~ few keV), together with their low cost, ease of production, and operation at room temperature and 1 atm makes them ideal for Cold Dark Matter (CDM) searches. SDD's are optimal for the exploration of the spin-dependent neutralino coupling due to their high fluorine content. The status of SIMPLE (Superheated Instrument for Massive ParticLe Experiments) is presented. Under realistic background considerations, we expect an improvement in the present Cold Dark Matter sensitivity of 2-3 orders of magnitude after ~1 kg-y of data acquisition.""]",['1996-11-01'] +2147,['eng'],"['Durrer, R']",['Anisotropies in the Cosmic Microwave Background'],['Astrophysics and Astronomy'],"['talk, Ascona 1996/05/26', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'microwaves', 'astrophysics, model', 'perturbation, density', 'field equations, Liouville', 'particle, massless', 'Friedman model', 'Compton scattering, nonrelativistic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610234'],"['The analysis of anisotropies in the cosmic microwave background (CMB) has become an extremely valuable tool for cosmology. We even have hopes that planned CMB anisotropy experiments may revolutionize cosmology. Together with determinations of the CMB spectrum, they represent the first cosmological precision measurements. This is illustrated in the talk by Anthony Lasenby. The value of CMB anisotropies lies to a big part in the simplicity of the theoretical analysis. Fluctuations in the CMB can be determined almost fully within linear cosmological perturbations theory and are not severely influenced by complicated nonlinear physics. In this contribution the different physical processes causing or influencing anisotropies in the CMB are discussed. The geometry perturbations at and after last scattering, the acoustic oscillations in the baryon-photon-plasma prior to recombination, and the diffusion damping during the process of recombination. The perturbations due to the fluctuating gravitational field, the so called Sachs-Wolfe contribution, is described in a very general form using the Weyl tensor of the perturbed geometry.']",['1996-10-30'] +2148,['eng'],"['Page, D']",['Fast Cooling of Neutron Stars'],['Astrophysics and Astronomy'],"['n, matter', 'K, condensation', 'neutrino, emission', 'temperature, surface', 'light nucleus', 'superfluid', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610191'],"['It is generally considered that the neutron star cooling scenarios involving fast neutrino emission, from a kaon or pion condensate, quark matter, or the direct Urca process, require the presence of baryon pairing in the central core of the star to control the strong neutrino emission and produce surface temperatures compatible with observations. I show here that within the kaon condensate scenario pairing is not necessary if: 1) the equation of state is stiff enough for the star to have a thick crust in which sufficient friction can occur to heat the star and 2) a thin layer, of mass larger than 10^{-12} Msol, of light elements (H and He) is present at the stellar surface. The effect of the light elements is to increase the heat flow and thus produce a higher surface temperature. Both the occurrence of heating and the presence of H and/or He at the surface (deposited during the late post-supernova accretion) can possibly be confirmed or infirmed by future observations.']",['1996-10-24'] +2149,['eng'],"['Linde, Andrei D', 'Mukhanov, V']",['Nongaussian Isocurvature Perturbations from Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'supersymmetry', 'perturbation, adiabatic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610219'],"['We present a class of very simple inflationary models of two scalar fields which leads to nongaussian isothermal perturbations with ``blue"" spectrum, n > 1. One of the models is inspired by supersymmetric theories where light scalar fields naturally acquire masses of the order of the Hubble constant H during inflation. Another model presumes that one of the fields has a nonminimal interaction with gravity. By a slight modification of parameters of these models one can obtain either gaussian isothermal perturbations, or nongaussian adiabatic perturbations with n > 1.']",['1996-10-28'] +2150,['eng'],"['Liddle, A R', 'Viana, P T P']","['Inflation, structure formation and dark matter']",['Astrophysics and Astronomy'],"['talk, Heidelberg 1996/09/16', 'inflationary universe', 'astrophysics, missing-mass', 'galaxy, cluster', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610215'],"['The formation of structure in the Universe offers some of the most powerful evidence in favour of the existence of dark matter in the Universe. We summarize recent work by ourselves and our collaborators, using linear and quasi-linear theory to probe the allowed parameter space of structure formation models with perturbations based on the inflationary cosmology. Observations used include large and intermediate angle microwave background anisotropies, galaxy clustering, the abundance of galaxy clusters and object abundances at high redshift. The cosmologies studied include critical density models with cold dark matter and with mixed dark matter, cold dark matter models with a cosmological constant and open cold dark matter models. Where possible, we have updated results from our journal papers.']",['1996-10-28'] +2151,['eng'],"['Nunokawa, H', 'Qian, Y Z', 'Fuller, G M']",['Resonant Neutrino Spin-Flavor Precession and Supernova Nucleosynthesis and Dynamics'],['Astrophysics and Astronomy'],"['neutrino, Majorana', 'neutrino, transition', 'resonance, transition', 'spin, flavor', 'supernova', 'nucleus, production', 'neutrino, magnetic moment', 'neutrino, mass', 'n, matter', 'magnetic field', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610209'],"['We discuss the effects of resonant spin-flavor precession (RSFP) of Majorana neutrinos on heavy element nucleosynthesis in neutrino-heated supernova ejecta and the dynamics of supernovae. In assessing the effects of RSFP, we explicitly include matter-enhanced (MSW) resonant neutrino flavor conversion effects where appropriate. We point out that for plausible ranges of neutrino magnetic moments and proto-neutron star magnetic fields, spin-flavor conversion of into a light $\\bar \\nu_e$ could lead to an enhanced neutron excess in neutrino-heated supernova ejecta. This could be beneficial for models of $r$-process nucleosynthesis associated with late-time neutrino-heated ejecta from supernovae. Similar spin-flavor conversion of neutrinos at earlier epochs could lead to an increased shock reheating rate and, concomitantly, a larger supernova explosion energy. We show, however, that such increased neutrino heating likely will be accompanied by an enhanced neutron excess which could exacerbate the problem of the overproduction of the neutron number $N = 50$ nuclei in the supernova ejecta from this stage. In all of these scenarios, the average $\\bar\\nu_e$ energy will be increased over those predicted by supernova models with no neutrino mixings. This may allow the SN1987a data to constrain RSFP-based schemes.']",['1996-10-28'] +2152,['eng'],"['Grifols, J A', 'Massó, E']",['Leptonic Photons and Nucleosynthesis'],['Astrophysics and Astronomy'],"['electron number', 'muon number', 'tau, lepton number', 'symmetry, U(1)', 'intermediate boson, postulated particle', 'intermediate boson, massless', 'fundamental constant, fine structure', 'upper limit', 'forces, long-range', 'astrophysics, model', 'postulated particle, interaction', 'light nucleus, production']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610205'],"['Should $U(1)$ long-range forces be associated to electron, muon and/or tau quantum number then their \'\'fine structure constants"" are seen to be bound by nucleosynthesis data to be less than about $1.7 \\times 10^{-11}$. For $\\tau$ and $\\mu$ this is the best upper limit up to date']",['1996-10-28'] +2153,['eng'],"['Sigl, G', 'Lee, S', 'Schramm, David N', 'Coppi, P S']",['Cosmological Neutrino Signatures for Grand Unification Scale Physics'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, flux', 'grand unified theory', 'photon, cosmic radiation', 'nucleon, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610221'],"['Physics beyond the standard model might imply the cosmological production of particles with grand unification scale energies. Nucleons and gamma-rays from such processes are candidates for the cosmic rays observed beyond 100 EeV [10**(20) eV]. Using a new particle propagation code, we calculate the neutrino fluxes predicted by such scenarios if consistency with the observed cosmic ray flux and the universal gamma-ray background at 1-10 GeV is required. Flux levels detectable by proposed km**3 scale neutrino observatories are allowed by these constraints. Bounds on or detection of a neutrino flux above about 1 EeV would allow neutrino astronomy to probe grand unification scale physics.']",['1996-10-29'] +2154,['eng'],"['Bucher, M', 'Zhu, Y']",['Non-Gaussian Isocurvature Perturbations From Goldstone Modes Generated During Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'Goldstone theorem', 'density, perturbation', 'symmetry, U(1)', 'symmetry breaking', 'critical phenomena', 'tensor, energy-momentum', 'renormalization', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610223'],"['We investigate non-Gaussian isocurvature perturbations generated by the evolution of Goldstone modes during inflation. If a global symmetry is broken inflation in a precise and predictable way. After inflation these Goldstone modes order themselves in a self-similar way, much as Goldstone modes in field ordering scenarios based on the Kibble mechanism. For $(H_{inf}^2/M_{pl}^2)\\sim 10^{-6},$ through their gravitational interaction these Goldstone modes generate density perturbations of approximately the right magnitude to explain the cosmic microwave background (CMB) anisotropy and seed the structure seen in the universe today. We point out that for the pattern of symmetry breaking in which a global $U(1)$ is completely broken, the inflationary evolution of the Goldstone field may be treated as that of a massless scalar field. Unlike the more commonly discussed case in which a global $U(1)$ is completely broken in a cosmological phase transition, in the inflationary case the production of defects can be made exponentially small, so that Goldstone field evolution is completely linear. In such a model non-Gaussian perturbations result because to lowest order density perturbations are sourced by products of Gaussian fields. Consequently, in this non-Gaussian model N-point correlations may be calculated by evaluating Feynman diagrams. We explore the issue of phase dispersion and conclude that this non-Gaussian model predicts Doppler peaks in the CMB anisotropy.']",['1996-10-29'] +2155,['eng'],"['Ostrowski, M']",['Acceleration of UHE Cosmic Ray Particles at Relativistic Jets in Extragalactic Radio Sources'],['Astrophysics and Astronomy'],"['talk, Tanashi 1996/09/25', 'cosmic radiation, acceleration', 'cosmic radiation, energy spectrum', 'jet', 'relativistic', 'cosmic radiation, particle source', 'model, shock waves', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610190'],"[""A mechanism of ultra-high energy (UHE) cosmic ray acceleration in extragalactic radio sources at the interface between the relativistic jet and the ambient medium is discussed as a supplement to the shock acceleration in `hot spots'. Particles accelerated at the jet side boundary are expected to dominate at highest energies. The spectrum formation near the cut-off energy is modeled using the Monte Carlo particle simulations.""]",['1996-10-24'] +2156,['eng'],"['García-Bellido, J', 'Liddle, A R']",['Complete power spectrum for an induced gravity open inflation model'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'gravitation, induced', 'density, perturbation', 'spectra, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'temperature, fluctuation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610183'],"['We study the phenomenological constraints on a recently proposed model of open inflation in the context of induced gravity. The main interest of this model is the relatively small number of parameters, which may be constrained by many different types of observation. We evaluate the complete spectrum of density perturbations, which contains continuum sub-curvature modes, a discrete super curvature mode, and a mode associated with fluctuations in the bubble wall. From these, we compute the angular power spectrum of temperature fluctuations in the microwave background, and derive bounds on the parameters of the model so that the predicted spectrum is compatible with the observed anisotropy of the microwave background and with large-scale structure observations. We analyze the matter era and the approach of the model to general relativity. The model passes all existing constraints.']",['1996-10-24'] +2157,['eng'],"['Sigl, G', 'Olinto, A V', 'Jedamzik, K']",['Primordial Magnetic Fields from Cosmological First Order Phase Transitions'],['Astrophysics and Astronomy'],"['astrophysics, model', 'critical phenomena', 'magnetic field', 'charge, density', 'stability, bubble', 'electroweak interaction', 'quantum chromodynamics', 'model, fluid', 'model, hydrodynamical']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610201'],"['We give an improved estimate of primordial magnetic fields generated during cosmological first order phase transitions. We examine the charge distribution at the nucleated bubble wall and its dynamics. We consider instabilities on the bubble walls developing during the phase transition. It is found that damping of these instabilities due to viscosity and heat conductivity caused by particle diffusion can be important in the QCD phase transition, but is probably negligible in the electroweak transition. We show how such instabilities together with the surface charge densities on bubble walls excite magnetic fields within a certain range of wavelengths. We discuss how these magnetic seed fields may be amplified by MHD effects in the turbulent fluid. The strength and spectrum of the primordial magnetic field at the present time for the cases where this mechanism was operative during the electroweak or the QCD phase transition are estimated. On a 10 Mpc comoving scale, field strengths of the order 10**(-29) G for electroweak and 10**(-20) G for QCD, could be attained for reasonable phase transition parameters.']",['1996-10-25'] +2158,['eng'],"['Battye, R A', 'Shellard, E P S']",['Relic gravitational waves'],['Astrophysics and Astronomy'],"['talk, London 1995/10/16', 'gravitational radiation', 'inflationary universe', 'fluctuation', 'critical phenomena', 'scattering, bubble', 'astrophysics, string', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610196'],"['The next generation of gravitational wave detectors holds out the prospect of detecting a stochastic gravitational background generated in the very early universe. In this article, we review the various cosmological processes which can lead to such a background, including quantum fluctuations during inflation, bubble collisions in a first-order phase transition and the decay of a network of cosmic strings. We conclude that signals from strongly first-order phase transitions, possibily at the end of inflation, and networks fo local cosmic strings are within the sensitivity of proposed detectors. However, backgrouds from slow-roll inflation and the electroweak phase transition are too weak.']",['1996-10-25'] +2159,['eng'],"['Raffelt, G G', 'Strobel, T']",['Reduction of Weak Interaction Rates in Neutron Stars by Nucleon Spin Fluctuations'],['Astrophysics and Astronomy'],"['n, matter', 'nucleon, spin', 'spin, fluctuation', 'weak interaction', 'structure function, spin', 'sum rule', 'neutrino n, interaction', 'total cross section', 'exchange, one-pion']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610193'],"[""Nucleon spin fluctuations in a dense medium reduce the ``naive'' values of weak interaction rates (neutrino opacities, neutrino emissivities). We extend previous studies of this effect to the degenerate case which is appropriate for neutron stars a few ten seconds after formation. If neutron-neutron interactions by a one-pion exchange potential are the dominant cause of neutron spin fluctuations, a perturbative calculation of weak interaction rates is justified for $T\\alt 3m/(4\\pi\\alpha_\\pi^2)\\approx 1 MeV$, where $m$ is the neutron mass and $\\alpha_\\pi\\approx15$ the pion fine-structure constant. At higher temperatures, the application of Landau's theory of Fermi liquids is no longer justified, i.e. the neutrons cannot be viewed as simple quasiparticles in any obvious sense.""]",['1996-10-25'] +2160,['eng'],"['Medina-Tanco, G A', 'De Gouveia dal Pino, E M', 'Horváth, J E']",['Non-Diffusive Propagation of Ultra High Energy Cosmic Rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'p, cosmic radiation', 'cosmic radiation, particle source', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610172'],"['We report the results of 3-D simulations of non-diffusive propagation of Ultra-High Energy Cosmic Rays (UHECR) (E > 10^{20} eV) through the intergalactic and extended halo media. We quantify the expected angular and temporal correlations between the events and the sources, and the temporal delay between protons and gamma-ray counterparts with a common origin for both halo and extragalactic origins. It is shown that the proposed UHECR-supergalactic plane source associations require either extremely high values of the halo magnetic field over as much as 100 kpc length scale or a very large correlation length for the IGM, even for the largest possible values of the intergalactic magnetic field. It can be stated that the UHECR seem to point to the sources even more strongly than previously believed. The simulations also show that the calculated time delays between UHE protons and gamma-ray counterparts do not match the claimed GRB-UHECR associations for either cosmological or extended halo distance scales.']",['1996-10-23'] +2161,['eng'],"['Faraoni, V']",['The creation of multiple images by a gravitational wave'],['Astrophysics and Astronomy'],"['talk, Seoul 1996/02/01', 'gravitational radiation', 'gravitation, lens']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610164'],"['We describe gravitational lensing by a gravitational wave, in the regime in which multiple images of a light source are created. We adapt the vector formalism employed for ordinary gravitational lenses to the case of a non-stationary spacetime, and we derive an approximate condition for multiple imaging. It is shown that certain astrophysical sources of gravitational waves satisfy this condition.']",['1996-10-22'] +2162,['eng'],"['Linde, Andrei D']",['Prospects of Inflationary Cosmology'],['Astrophysics and Astronomy'],"['talk, Princeton 1996/06/24', 'inflationary universe', 'matter, density', 'field theory, scalar', 'density, perturbation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610077'],"['In this review I briefly describe the evolution of the inflationary theory from the scenario based on the idea of supercooling and expansion in the false vacuum toward the theory of eternally expanding self-reproducing inflationary universe. I describe recent development of inflationary cosmology with Omega < 1, and then discuss some issues related to the possibility to verify inflation by comparing its predictions with observational data. I argue that it is possible to verify and disprove many particular models of inflationary cosmology, but it is very difficult to kill the basic idea of inflation. It seems that the best (and may be even the only) way to do so is to suggest a better cosmological theory.']",['1996-10-11'] +2163,['eng'],"['Reddy, S', 'Prakash, M']",['Neutrino Scattering in a Newly Born Neutron Star'],['Astrophysics and Astronomy'],"['n, matter', 'astrophysics, model', 'neutrino, astrophysics', 'neutrino nucleon, interaction', 'scattering, neutrino hyperon', 'cross section, energy dependence', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610115'],"['We calculate neutrino cross sections from neutral current reactions in the dense matter encountered in the evolution of a newly born neutron star. Effects of composition and of strong interactions in the deleptonization and cooling phases of the evolution are studied. The influence of the possible pWe calculate neutrino cross sections from neutral current reactions in the dense matter encountered in the evolution of a newly born neutron star. Effects of composition and of strong interactions in the deleptonization and cooling phases of the evolution are studied. The influence of the possible presence of strangeness-rich hyperons on the neutrino scattering cross sections is explored. Due to the large vector couplings of the Sigma^- and Cascade^-, |C_V| ~ 2, these particles, if present in protoneutron star matter, give significant contributions to neutrino scattering. In the deleptonization phase, the presence of strangeness leads to large neutrino energies, which results in large enhancements in the cross sections compared to those in matter with nucleons only. In the cooling phase, in which matter is nearly neutrino free, the response of the Sigma^- hyperons to thermal neutrinos is the most significant. Neutrinos couple relatively weakly to the Lambda hyperons and, hence, their contributions are significant only at high density. resence of strangeness-rich hyperons on the neutrino scattering cross sections is explored. Due to the large vector couplings of the Sigma^- and Cascade^-, |C_V| ~ 2, these particles, if present in protoneutron star matter, give significant contributions to neutrino scattering. In the deleptonization phase, the presence of strangeness leads to large neutrino energies, which results in large enhancements in the cross sections compared to those in matter with']",['1996-10-16'] +2164,['eng'],"['Vilenkin, A']",['Cosmic Defects'],['Astrophysics and Astronomy'],"['talk, Princeton 1996/06/24', 'astrophysics, string', 'topology, defect', 'inflationary universe', 'critical phenomena']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610125'],"['A (very) brief review of topological defects and their possible cosmic roles. I emphasize in particular that superheavy defects needed for structure formation can peacefully coexist with inflation, despite the claims to the contrary which are often made in the literature.']",['1996-10-17'] +2165,['eng'],"['González-Mestres, L']","['Physics, Cosmology and Experimental Signatures of a Possible New Class of Superluminal Particles']",['Astrophysics and Astronomy'],"['talk, Sheffield 1996/09/08', 'space-time', 'astrophysics, model', 'astrophysics, missing-mass', 'field theory, scalar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610089'],"['The apparent Lorentz invariance of the laws of physics does not imply that space-time is indeed minkowskian. We consider a scenario where Lorentz invariance is only an approximate property of equations describing a sector of matter at a given scale and superluminal sectors of matter exist related to new degrees of freedom not yet discovered experimentally. The new particles would not be tachyons: they may feel different minkowskian space-times with critical speeds much higher than c (speed of light) and behave kinematically like ordinary particles apart from the difference in critical speed. Superluminal particles may provide most of the dark matter at cosmic scale, and be mainly dark. We present a discussion of possible theoretical, cosmological and experimental consequences of such a scenario, with particular emphasis on problems related to the identification of dark matter.']",['1996-10-14'] +2166,['eng'],"['Gwinn, C R', 'Eubanks, T M', 'Pyne, T', 'Birkinshaw, M', 'Matsakis, D N']",['Quasar Proper Motions and Low-Frequency Gravitational Waves'],['Astrophysics and Astronomy'],"['astrophysics, quasar', 'gravitational radiation', 'mass, upper limit', 'energy, upper limit', 'interference', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610086'],"['We report observational upper limits on the mass-energy of the cosmological gravitational-wave background, from limits on proper motions of quasars. Gravitational waves with periods longer than the time span of observations produce a simple pattern of apparent proper motions over the sky, composed primarily of second-order transverse vector spherical harmonics. A fit of such harmonics to measured motions yields a 95%-confidence limit on the mass-energy of gravitational waves with frequencies <2e-9 Hz, of <0.11/h*h times the closure density of the universe.']",['1996-10-14'] +2167,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Bottino, A', 'Mignola, G']",['On neutralino stars as microlensing objects'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'astrophysics, MACHO', 'supersymmetry', 'sparticle, neutral particle', 'sparticle, matter', 'gravitation', 'sparticle, gas', 'sparticle, annihilation', 'photon, cosmic radiation', 'flux', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610060'],"['The microlensing objects, Machos, recently observed in the halo of our Galaxy, can be interpreted as dense neutralino objects, neutralino stars, produced by the gravitational instability of neutralino gas. Taking the mass and radius of these objects from microlensing observations we calculated the diffuse gamma-ray flux produced in neutralino--neutralino annihilation inside the objects. The resulting flux is many orders of magnitude higher than the observed one.']",['1996-10-10'] +2168,['eng'],"['Grupen, Claus']",['Neutrino astronomy'],['Astrophysics and Astronomy'],"['talk, Lodz 1996/07/15', 'neutrino, astrophysics', 'astrophysics, supernova', 'neutrino, cosmic radiation', 'neutrino, solar', 'model, solar', 'neutrino/e, energy spectrum', 'neutrino, oscillation', 'neutrino, magnetic moment', 'astrophysics, pulsar', 'astrophysics, string', 'defect, topological', 'neutrino, flux', 'photon, flux', 'nucleon, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610057'],['Neutrino astronomy offers the prospect to be able to look into the interior of compact astrophysical objects which may be the sources of cosmic radiation. This paper describes the results on neutrino observations from the sun and the supernova SN1987A along with an outlook on neutrino astronomy beyond the TeV scale.'],['1996-10-10'] +2169,['eng'],"['Weinberg, S']",['Theories of the Cosmological Constant'],['Astrophysics and Astronomy'],"['talk, Princeton 1996/06/24', 'astrophysics, fundamental constant', 'vacuum state', 'energy, density', 'symmetry', 'gravitation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610044'],"[""This is a talk given at the conference ``Critical Dialogues in Cosmology'' at Princeton University, June 24-- 27, 1996. It gives a brief summary of our present theoretical understanding regarding the value of the cosmological constant, and describes how to calculate the probability distribution of the observed cosmological constant in cosmological theories with a large number of subuniverses (i. e., different expanding regions, or different terms in the wave function of the universe) in which this constant takes different values.""]",['1996-10-08'] +2170,['eng'],"['Hwang, J']",['Roles of a coherent scalar field on the evolution of cosmic structures'],['Astrophysics and Astronomy'],"['field theory, scalar', 'field theory, oscillation', 'coherence', 'perturbation, scalar', 'dependence, gauge', 'astrophysics, model', 'astrophysics, missing-mass', 'background']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610042'],"['A coherently oscillating scalar field, an axion as an example, is known to behave as a cold dark matter. The arguments were usually made in the Newtonian context. Ratra proved the case in relativistic context using the synchronous gauge. In this paper we present another proof based on a more suitable gauge choice, the uniform-curvature gauge, which fits the problem. By a proper time averaging the perturbed oscillating scalar field behaves as a cold dark matter on the relevant scales including the superhorizon scale.']",['1996-10-08'] +2171,['eng'],"['De Paolis, F', 'Ingrosso, G', 'Jetzer, Philippe', 'Roncadelli, Marco']",['Baryonic dark matter'],['Astrophysics and Astronomy'],"['talk, Sesto Pusteria 1996/07/02', 'astrophysics, missing-mass', 'baryon, matter', 'astrophysics, galaxy', 'astrophysics, MACHO']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610031'],['Reasons supporting the idea that most of the dark matter in galaxies and clusters of galaxies is baryonic is discussed. Moreover it is argued that most of the dark matter in galactic halo should be in the form of MACHOs and cold molecular clouds.'],['1996-10-08'] +2172,['eng'],"['Amendola, L', 'Baccigalupi, C', 'Konoplich, R V', 'Occhionero, F', 'Rubin, S G']",['Reconstruction of the bubble nucleating potential'],['Astrophysics and Astronomy'],"['inflationary universe', 'bubble, production', 'potential', 'critical phenomena', 'gravitation, correction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610038'],"['We calculate analytically the bubble nucleation rate in a model of first order inflation which is able to produce large scale structure. The computation includes the first-order departure from the thin-wall limit, the explicit derivation of the pre-exponential factor, and the gravitational correction. The resulting bubble spectrum is then compared with constraints from the large scale structure and the microwave background. We show that there are models which pass all the constraints and produce bubble-like perturbations of interesting size. Furthermore, we show that it is in principle possible to reconstruct completely the inflationary two-field potential from observations.']",['1996-10-08'] +2173,['eng'],"['Dimopoulos, K', 'Davis, A C']",['On the Evolution of Primordial Magnetic Fields'],['Astrophysics and Astronomy'],"['astrophysics', 'magnetic field', 'plasma', 'critical phenomena', 'electroweak interaction', 'correlation, length', 'grand unified theory', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9610013'],"['A new mechanism for the evolution of primordial magnetic fields is described and analysed. The field evolution is followed from the time of its creation until the epoch of structure and galaxy formation. The mechanism takes into account the turbulent behaviour of the early universe plasma, whose properties determine strongly the evolution of the field configuration. A number of other related issues such as the case of an electroweak plasma are also considered. Finally, as an example, the mechanism is applied to specific models.']",['1996-10-03'] +2174,['eng'],"['Maartens, R']",['Linearisation instability of gravity waves?'],['Astrophysics and Astronomy'],"['gravitational radiation, stability', 'space-time, Bianchi', 'constraint']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609198'],"['Gravity waves in irrotational dust spacetimes are characterised by nonzero magnetic Weyl tensor $H_{ab}$. In the linearised theory, the divergence of $H_{ab}$ is set to zero. Recently Lesame et al. [Phys. Rev. D {\\bf 53}, 738 (1996)] presented an argument to show that, in the exact nonlinear theory, $div H=0$ forces $H_{ab}=0$, thus implying a linearisation instability for gravity waves interacting with matter. However a sign error in the equations invalidates their conclusion. Bianchi type V spacetimes are shown to include examples with $div H=0\\neq H_{ab}$. An improved covariant formalism is used to show that in a generic irrotational dust spacetime, the covariant constraint equations are preserved under evolution. It is shown elsewhere that $\\mbox{div} H=0$ does not generate further conditions.']",['1996-10-01'] +2175,['eng'],"['Seljak, Yu', 'Zaldarriaga, M']",['Signature of Gravity Waves in Polarization of the Microwave Background'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, polarization', 'gravitational radiation', 'temperature, fluctuation', 'polarization, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609169'],"['Using spin-weighted decomposition of polarization in the Cosmic Microwave Background (CMB) we show that a particular combination of Stokes $Q$ and $U$ parameters vanishes for primordial fluctuations generated by scalar modes, but does not for those generated by primordial gravity waves. Because of this gravity wave detection is not limited by cosmic variance as in the case of temperature fluctuations. Numerical evaluation in inflation-based models shows that the expected signal for tensor to scalar ratio of unity is of the order of 0.5 $\\mu K$, which could be directly tested in future CMB experiments.']",['1996-09-26'] +2176,['eng'],"['Masperi, L', 'Savaglio, S']",['Comparison of stars and decaying neutrinos as additional sources of Intergalactic UV background'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'ionization', 'astrophysics, quasar', 'neutrino, decay', 'hydrogen', 'helium', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609173'],"['A numerical calculation of properties of finite absorbers and of intergalactic medium based on photoionization equilibrium is performed to confront alternative UV sources in addition to quasars. It is seen that a spectrum including a large peak around the HI ionization energy due to decaying neutrinos is too soft in the region up to the HeI edge to explain the relatively small observed ratio of neutral He and H densities in Lyman-limit systems if their size is of the kpc order. The recently proposed decrease of the contribution from unstable neutrinos solves this problem but tends to spoil the consistence between IGM and Lyman-$\\alpha$ clouds, which requires a large ratio of fluxes for the HI and HeII ionization frequencies, unless there is a very fast decline of quasars above $z = 3$. On the other hand, the addition of stars to quasars may produce a spectrum sufficiently hard between HI and HeI and thereafter soft up to HeII to allow a reasonable agreement of the properties of denser absorbers with those of IGM. This model seems to favour cold dark matter with additional cosmological constant.']",['1996-09-26'] +2177,['eng'],"['Kamionkowski, M P', 'Kosowsky, A', 'Stebbins, A J']",['A Probe of Primordial Gravity Waves and Vorticity'],['Astrophysics and Astronomy'],"['cosmic radiation, anisotropy', 'cosmic radiation, background', 'cosmic radiation, polarization', 'gravitational radiation', 'perturbation, tensor', 'perturbation, vector']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609132'],['A formalism for describing an all-sky map of the polarization of the cosmic microwave background is presented. The polarization pattern on the sky can be decomposed into two geometrically distinct components. One of these components is not coupled to density inhomogeneities. A non-zero amplitude for this component of polarization can only be caused by tensor or vector metric perturbations. This allows unambiguous identification of long-wavelength gravity waves or large-scale vortical flows at the time of last scattering.'],['1996-09-20'] +2178,['eng'],"['Vauclair, S', 'Richard, O']","['Local Mixing near the Solar Core, Neutrino Fluxes and Helioseismology']",['Astrophysics and Astronomy'],"['talk, Blois 1996/06/08', 'neutrino, solar', 'neutrino, flux', 'model, solar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609133'],"['We have computed solar models similar to those published in Richard et al 1996, in which we have added local mixing near the solar core in order to decrease the neutrino production. The results show that the neutrino fluxes are reduced as expected (although not enough to account for the observed values), but the obtained models are incompatible with the inversion of the helioseismic modes.']",['1996-09-20'] +2179,['eng'],"['Sturrock, P A', 'Walther, G']","['An Apparent Periodicity in the Gallex, Homestake and Kamiokande Neutrino Data']",['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'flux, time variation', 'model, solar', 'deep underground detector', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609151'],"['In order to explore a recent proposal that the solar core may contain a component that varies periodically with a period in the range 21.0 - 22.4 days, due either to rotation or to some form of oscillation, we have examined the time series formed from measurements of the solar neutrino flux by means of the GALLEX, Homestake and Kamiokande experiments. Direct Fourier transform analysis of the Homestake data shows that the most prominent peak in the entire spectrum (examined down to 5 days period) is found at a frequency of approximately 17.2 y-1 corresponding to a period of approximately 21.3 days. According to the ""shuffle test,"" the probability of finding this large a peak in the prescribed search band is about 0.03%, if it is assumed that there is no correlation between count rate and time. The GALLEX and Kamiokande data are examined in a way that searches for similarity in the shapes of the two spectra in sliding windows in frequency. We find that the ""spectral correlation measure"" peaks at 17.2 y-1, and the shuffle test indicates that the probability of finding this large a peak at a specified frequency is 2%, if it is again assumed that for each time series there is no correlation between count rate and time. The combined significance estimate is of order 1 part in 105 that the results are due to chance, on the assumption that there is no real structure to the count-rate time series.']",['1996-09-23'] +2180,['eng'],"['Gaisser, T K', 'Protheroe, R J', 'Stanev, T']",['$\\gamma$-ray production in supernova remnants'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'astrophysics, supernova', 'photon, particle source', 'cosmic radiation, acceleration', 'pi, production', 'bremsstrahlung', 'Compton scattering', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609044'],"['The bulk of the cosmic rays up to about 100 TeV are thought to be accelerated by the 1st order Fermi mechanism at supernova shocks, producing a power-law spectrum. Both electrons and protons should be accelerated, but their ratio on acceleration is not well known. Recently, the EGRET instrument on the Compton Gamma Ray Observatory has observed supernova remnants IC 443 and gamma Cygni at GeV energies. On the assumption that the observed gamma-rays are produced by accelerated particles in the remnants (rather than, for example, from a central compact object) we model the contributions due to pion production, bremsstrahlung, and inverse Compton scattering on the cosmic microwave, diffuse galactic radiation, and locally produced radiation fields. We find that a spectral index of accelerated particles close to 2.4, and a ratio of electrons to protons in the range 0.2 to 0.3, gives a good fit to the observed spectra. We discuss the implications of this result for observations at air shower energies, and for the propagation of cosmic rays.']",['1996-09-09'] +2181,['eng'],"['Karle, A', 'Mikolajski, T', 'Cichos, S', 'Hundertmark, S', 'Pandel, D', 'Spiering, C', 'Streicher, O', 'Thon, T', 'Wiebusch, C', 'Wischnewski, R']",['Analog Optical Transmission of Fast Photomultiplier Pulses Over Distances of 2 km'],['Astrophysics and Astronomy'],"['talk, Beaune 1996/06/24', 'photoelectron, amplifier', 'photoelectron, readout', 'semiconductor, optical', 'optics, fibre', 'optics, analog', 'Cherenkov counter, water', 'deep underground detector, AMANDA']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9611102'],"['New LED-transmitters have been used to develop a new method of fast analog transmission of PMT pulses over large distances. The transmitters, consisting basically of InGaAsP LEDs with the maximum emission of light at 1300 nm, allow the transmission of fast photomultiplier pulses over distances of more than 2 km. The shape of the photomultiplier pulses is maintained, with an attenuation less than 1 dB/km. Typical applications of analog optical signal transmission are surface air shower detectors and underwater/ice neutrino experiments, which measure fast Cherenkov or scintillator pulses at large detector distances to the central DAQ system.']",['1996-11-14'] +2182,['eng'],"['Stecker, F W', 'De Jager, O C', 'Salamon, M H']",['Predicted Extragalactic TeV $\\gamma$-Ray Sources'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'synchrotron radiation', 'Compton scattering', 'cosmic radiation, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609102'],"['We suggest that low-redshift XBLs (X-ray selected BL Lacertae objects) may be the only extragalactic gamma-ray sources observable at TeV energies. We use simple physical considerations involving synchrotron and Compton component spectra for blazars to suggest why the observed TeV sources are XBLs, whereas mostly RBLs and FSRQs are seen at GeV energies. These considerations indicate that the differences between XBLs and RBLs cannot be explained purely as relativistic jet orientation effects. We note that the only extragalactic TeV sources which have been observed are XBLs and that a nearby RBL with a very hard spectrum in the GeV range has not been seen at TeV energies. We also note that of the 14 BL Lacs observed by EGRET, 12 are RBLs, whereas only 2 are XBLs. We give a list of nearby XBLs which we consider to be good candidate TeV sources and predict estimated TeV fluxes for these objects.']",['1996-09-17'] +2183,['eng'],"['Diwan, M V']",['Decays of Long Lived Lightest Supersymmetric Particles in the Galactic Halo'],['Astrophysics and Astronomy'],"['talk, Snowmass 1996/06/25', 'astrophysics, missing-mass', 'astrophysics, galaxy', 'supersymmetry', 'R parity, violation', 'postulated particle, LSP', 'sparticle, decay', 'photon, production', 'neutrino, production', 'postulated particle, gravitino', 'postulated particle, Majoron', 'final state, two-particle', 'sparticle, mass', 'sparticle, lifetime', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609081'],"['If dark matter neutral LSPs in the galactic halo decay into two body final states containing photons or neutrinos they could be detected even if the decay rates are very small, 10**{-32} per sec. I calculate mass and lifetime bounds from current astrophysical data on monochromatic photons and neutrinos and suggest that the poorly explored region between 10 GeV and 1 TeV be explored for signs of supersymmetry from space.']",['1996-09-12'] +2184,['eng'],"['De Vega, H J', 'Sánchez, N', 'Combes, F']",['Fractal Dimensions and Scaling Laws in the Interstellar Medium'],['Astrophysics and Astronomy'],"['astrophysics', 'fractals, dimension', 'scaling', 'gas, nonrelativistic', 'field theory, scalar', 'renormalization group, fixed point', 'critical phenomena', 'Ising model', 'mean field approximation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609129'],"['We develop a field theoretical approach to the cold interstellar medium (ISM). We show that a non-relativistic self-gravitating gas in thermal equilibrium with variable number of atoms or fragments is exactly equivalent to a field theory of a single scalar field \\phi({\\vec x}) with exponential self interaction. We analyze this field theory perturbatively and non-perturbatively through the renormalization group approach.We show scaling behaviour(critical) for a continuous range of the temperature and of the other physical parameters. We derive in this framework the scaling relation Delta M(R) \\sim R^{d_H} for the mass on a region of size R and \\Delta v \\sim R^q for the velocity dispersion where q = \\frac12(d_H -1). For the density-density correlations we find a power-law behaviour for large distances \\sim |{\\vec r_1} -{\\vec r_2}|^{2 d_H -6}. The fractal dimension d_H turns to be related with the critical exponent \\nu of the correlation length by d_H = 1/ \\nu. The renormalization group approach for a single component scalar field in three dimensions states that the long-distance critical behaviour is governed by the (non-perturbative) Ising fixed point. The corresponding values of the scaling exponents are \\nu = 0.631..., d_H = 1.585... and q = 0.293.... Mean field theory yields for the scaling exponents \\nu =1/2, d_H = 2 and q = 1/2. Both the Ising and the mean field values are compatible with the present ISM observational data: 1.4 \\leq d_H \\leq 2, 0.3 \\leq q \\leq 0.6.As typical in critical phenomena, the scaling behaviour and critical exponents of the ISM can be obtained without dwelling into the dynamical (time-dependent) behaviour. The relevant rôle of selfgravity is stressed by the authors in a Letter to Nature, September 5, 1996.']",['1996-09-20'] +2185,['eng'],"['Olive, Keith A']",['Primordial Nucleosynthesis'],['Astrophysics and Astronomy'],"['talk, Blois 1996/06/08', 'talk, Helsinki 1996/06/13', 'astrophysics, model', 'light nucleus, production', 'helium, nuclide', 'lithium, nuclide', 'astrophysics, galaxy', 'astrophysics, missing-mass', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609071'],"['The current of status of big bang nucleosynthesis is reviewed and the concordance between theory and observation is examined in detail. It is argued that when using the observational data on \\he4 and \\li7, the two isotopes whose abundances are least affected by chemical and stellar evolution, it is found that both are completely consistent with BBN theory and determine the value of the baryon-to-photon ratio, $\\eta$ to be relatively low, $\\eta \\approx 1.8 is quasar absorption systems. These results have far reaching consequences for galactic chemical evolution, the amount of baryonic dark matter in the Universe and on the allowed number of degrees of freedom in the early Universe.']",['1996-09-10'] +2186,['eng'],"['Jetzer, Philippe']",['Neutrinos and dark matter in galactic halos'],['Astrophysics and Astronomy'],"['talk, Zuoz 1996/08/04', 'astrophysics, missing-mass', 'astrophysics, galaxy', 'neutrino, cosmic radiation', 'baryon, matter', 'astrophysics, MACHO', 'numerical calculations, interpretation of experiments', 'proposed experiment', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609068'],"['One of the most important problems in astrophysics concerns the nature of the dark matter in galactic halos, whose presence is implied mainly by the observed flat rotation curves in spiral galaxies. Due to the Pauli exclusion principle it can be shown that neutrinos cannot be a major constituent of the halo dark matter. As far as cold dark matter is concerned there might be a discrepancy between the results of the N-body simulations and the measured rotation curves for dwarf galaxies. A fact this, if confirmed which would exclude cold dark matter as a viable candidate for the halo dark matter. In the framework of a baryonic scenario the most plausible candidates are brown or white dwarfs and cold molecular clouds (mainly of $H_2$). The former can be detected with the ongoing microlensing experiments. In fact, the French collaboration EROS and the American-Australian collaboration MACHO have reported the observation of altogether $\\sim$ 10 microlensing events by monitoring during several years the brightness of millions of stars in the Large Magellanic Cloud. In particular, the MACHO team announced the discovery of 8 microlensing candidates by analysing their first 2 years of observations. This would imply that the halo dark matter fraction in form of MACHOs (Massive Astrophysical Compact Halo Objects) is of the order of 45-50% assuming a standard spherical halo model. The most accurate way to get information on the mass of the MACHOs is to use the method of mass moments, which leads to an average mass of 0.27$M_{\\odot}$.']",['1996-09-10'] +2187,['eng'],"['Weber, F', 'Schaab, C', 'Weigel, M K', 'Glendenning, N K']",['From Quark Matter to Strange Machos'],['Astrophysics and Astronomy'],"['talk, Vulcano 1996/05/27', 'astrophysics, galaxy', 'quark, matter', 'matter, strangeness', 'n, matter', 'astrophysics, model', 'quark, density', 'lepton, density', 'potential, electrostatic', 'temperature', 'pi, condensation', 'K, condensation', 'nuclear matter', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609067'],"['This paper gives an overview of the properties of all possible equilibrium sequences of compact strange-matter stars with nuclear crusts, which range from strange stars to strange dwarfs. In contrast to their non-strange counterparts, --neutron stars and white dwarfs--, their properties are determined by two (rather than one) parameters, the central star density and the density at the base of the nuclear crust. This leads to stellar strange-matter configurations whose properties are much more complex than those of the conventional sequence. As an example, two generically different categories of stable strange dwarfs are found, which could be the observed white dwarfs. Furthermore we find very-low-mass strange stellar objects, with masses as small as those of Jupiter or even lighter planets. Such objects, if abundant enough in our Galaxy, should be seen by the presently performed gravitational microlensing searches.']",['1996-09-10'] +2188,['eng'],"['Pethick, C J', 'Thorsson, V']",['Effects of Electron Band Structure on Neutrino Pair Bremsstrahlung in Neutron Star Crusts'],['Astrophysics and Astronomy'],"['astrophysics', 'n, matter', 'crystal, lattice', 'scattering, electron ion', 'neutrino, pair production', 'neutrino, bremsstrahlung', 'temperature, dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607065'],"['We calculate the rate of energy emission by bremsstrahlung of neutrino pairs by electrons moving in the crystalline lattice of ions in dense matter in the crust of a neutron star. Since the periodic potential in the solid gives rise to electronic band gaps which can be as large as about 1 MeV, it is necessary in estimating the bremsstrahlung rate at low temperatures to take into account band structure in detail. We find that, in the densest parts of the inner crust of a neutron star, neutrino emission at temperatures of about $2\\times 10^9$K or less is much suppressed compared with earlier estimates that treated the electron-lattice interaction perturbatively, and conclude that neutrino pair bremsstrahlung by electrons in the crusts of neutron stars is much less important for neutron star thermal evolution than was previously thought.']",['1996-07-17'] +2189,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Blasi, P', 'Ptuskin, V S']",['Clusters of galaxies as a storage room for cosmic rays'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'galaxy, cluster', 'astrophysics, model', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'cosmic radiation, flux', 'gas, interaction', 'baryon, density', 'cosmic radiation, particle source', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609048'],"['It is demonstrated that clusters of galaxies are able to keep cosmic rays for a time exceeding the age of the Universe. This phenomenon reveals itself by the production of the diffuse flux of high energy gamma and neutrino radiation due to the interaction of the cosmic rays with the intracluster gas. The produced flux is determined by the cosmological density of baryons, $\\Omega_b$, if a large part of this density is provided by the intracluster gas. The signal from relic cosmic rays has to be compared with the flux produced by the late sources, which can be considered as a background in the search for cosmic ray production in the past. We calculate this flux considering the normal galaxies and AGN in the clusters as the sources of cosmic rays. Another potential cosmic ray source is the shock in the gas accreting to a cluster. We found that this background is relatively high: the diffuse fluxes produced by relic cosmic rays are of the same order of magnitude which can be expected from AGN in the clusters. In all cases the predicted diffuse gamma-ray flux is smaller than the observed one and the diffuse neutrino flux can be seen as the small bump at $E\\sim 10^6 GeV$ over the atmospheric neutrino flux. A bright phase in the galaxy evolution can be a source of the relic cosmic rays in clusters, revealing itself by diffuse gamma and neutrino radiations. We found that the observation of a signal from the bright phase is better for an individual cluster.']",['1996-09-09'] +2190,['eng'],"['Mészáros, P', 'Rees, M J']",['Poynting Jets from Black Holes and Cosmological $\\gamma$-Ray Bursts'],['Astrophysics and Astronomy'],"['astrophysics, jet', 'black hole, mass', 'n, matter', 'magnetic field', 'baryon, particle flow', 'photon, emission']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609065'],"['We discuss the properties of magnetically dominated jet-like outflows from stellar mass black holes surrounded by debris tori resulting from neutron star disruption. These jets may have narrow cores (along the rotation axis) which are almost free of baryons and attain very high bulk Lorentz factors $\\sim 10^6$. The jets give rise to a characteristic GeV emission as well as to relativistic shocks producing the usual MeV bursts. Because the outflow is highly directional the properties of the observed gamma-rays would depend on the viewing angle relative to the rotation axis. Even for the most intense bursts, which under the assumption of isotropic emission and substantial redshifts would be inferred to emit $10^{52}-10^{53}$ erg, the efficiencies required are only $10^{-2}-10^{-4}$.']",['1996-09-09'] +2191,['eng'],"['Brandenberger, R H']",['Some Key Issues Confronting Inflationary Cosmology'],['Astrophysics and Astronomy'],"['talk, Princeton 1996/06/24', 'inflationary universe', 'cosmic radiation, anisotropy', 'density, perturbation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609045'],"['Does inflation provide a compelling explanation for why the universe is so large, so flat, and so old, and a predictive theory of density perturbations? In this brief contribution (based on the role of the author as moderator of the discussion session on inflation), a list of some of the key issues confronting inflationary cosmology will be given, with the hope of focusing the debate on inflation and drawing more attention to some of the potential problems of the inflationary theory.']",['1996-09-09'] +2192,['eng'],"['Kaiser, N', 'Jaffe, A']",['Bending of Light by Gravity Waves'],['Astrophysics and Astronomy'],"['gravitational radiation', 'photon, tracks', 'space-time, perturbation', 'perturbation, scalar', 'random walk', 'gravitation, lens', 'astrophysics, galaxy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609043'],"[""We describe the statistical properties of light rays propagating though a random sea of gravity waves and compare with the case for scalar metric perturbations from density inhomogeneities. For scalar fluctuations the deflection angle grows as the square-root of the path length $D$ in the manner of a random walk, and the rms displacement of a ray from the unperturbed trajectory grows as $D^{3/2}$. For gravity waves the situation is very different. The mean square deflection angle remains finite and is dominated by the effect of the metric fluctuations at the ends of the ray, and the mean square displacement grows only as the logarithm of the path length. In terms of power spectra, the displacement for scalar perturbations has $P(k) \\propto 1/ k^4$ while for gravity waves the trajectories of photons have $P(k) \\propto 1/k$ which is a scale-invariant or `flicker-noise' process, and departures from rectilinear motion are suppressed, relative to the scalar case, by a factor metric fluctuations and $D$ is the path length. This result casts doubt on the viability of some recent proposals for detecting or constraining the gravity wave background by astronomical measurements.""]",['1996-09-06'] +2193,['eng'],"['Allen, B', 'Caldwell, R R', 'Shellard, E P S', 'Stebbins, A J', 'Veeraraghavan, S']",['Large Angular Scale CMB Anisotropy Induced by Cosmic Strings'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, string', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609038'],"['We simulate the anisotropy in the cosmic microwave background (CMB) induced by cosmic strings. By numerically evolving a network of cosmic strings we generate full-sky CMB temperature anisotropy maps. Based on $192$ maps, we compute the anisotropy power spectrum for multipole moments $\\ell \\le 20$. By comparing with the observed temperature anisotropy, we set the normalization for the cosmic string mass-per-unit-length $\\mu$, obtaining $G\\mu/c^2=1.05 {}^{+0.35}_{-0.20} \\times10^{-6}$, which is consistent with all other observational constraints on cosmic strings. We demonstrate that the anisotropy pattern is consistent with a Gaussian random field on large angular scales.']",['1996-09-06'] +2194,['eng'],"['Totani, T', 'Sato, K']",['Resonant Spin-Flavor Conversion of Supernova Neutrinos and Deformation of the Electron Antineutrino Spectrum'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, astrophysics', 'neutrino, oscillation', 'spin, flavor', 'antineutrino/e', 'neutrino/mu', 'neutrino, mass', 'neutrino, magnetic moment', 'magnetic field', 'astrophysics, model', 'energy spectrum, (antineutrino/e)', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609035'],"['The neutrino spin-flavor conversion of \\bar\\nu_e and \\nu_\\mu which is induced by the interaction of the Majorana neutrino magnetic moment and magnetic fields in the collapse-driven supernova is investigated in detail. We calculate the conversion probability by using the latest precollapse models of Woosley and Weaver (1995), and also those of Nomono and Hashimoto (1988), changing the stellar mass and metallicity in order to estimate the effect of the astrophysical uncertainties. Contour maps of the conversion probability are given for all the models as a function of neutrino mass squared difference and the neutrino magnetic moment times magnetic fields. It is shown that in the solar metallicity models some observational effects are expected with \\Delta m^2 = 10^{-5}--10^{-1} [eV^2] and \\mu_\\nu >~ 10^{-12} (10^9 G / B_0) [\\mu_B], where B_0 is the strength of the magnetic fields at the surface of the iron core. We also find that although the dependence on the stellar models or stellar mass is not so large, the metallicity of precollapse stars has considerable effects on this conversion. Such effects may be seen in a supernova in the Large or Small Magellanic Clouds, and should be taken into account when one considers an upper bound on \\mu_\\nu from the SN1987A data.']",['1996-09-06'] +2195,['eng'],"['Sikivie, P', 'Tkachev, Igor I', 'Wang, Y']",['The secondary infall model of galactic halo formation and the spectrum of cold dark matter particles on Earth'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'astrophysics, galaxy', 'astrophysics, model', 'postulated particle, axion', 'postulated particle, WIMP', 'gravitation, scattering', 'angular momentum, postulated particle', 'velocity', 'postulated particle, density', 'phase space', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609022'],"['The spectrum of cold dark matter particles on Earth is expected to have peaks in velocity space associated with particles which are falling onto the Galaxy for the first time and with particles which have fallen in and out of the Galaxy only a small number of times in the past. We obtain estimates for the velocity magnitudes and the local densities of the particles in these peaks. To this end we use the secondary infall model of galactic halo formation which we have generalized to take account of the angular momentum of the dark matter particles. The new model is still spherically symmetric and it admits self-similar solutions. In the absence of angular momentum, the model produces flat rotation curves for a large range of values of a parameter $\\epsilon$ which is related to the spectrum of primordial density perturbations. We find that the presence of angular momentum produces an effective core radius, i.e. it makes the contribution of the halo to the rotation curve go to zero at zero radius. The model provides a detailed description of the large scale properties of galactic halos including their density profiles, their extent and total mass. We obtain predictions for the kinetic energies of the particles in the velocity peaks and estimates for their local densities as functions of the amount of angular momentum, the age of the universe and $\\epsilon$.']",['1996-09-04'] +2196,['eng'],"['Boyanovsky, D', 'De Vega, H J', 'Holman, R', 'Salgado, J F J']",['Preheating and Reheating in Inflationary Cosmology'],['Astrophysics and Astronomy'],"['talk, Paris 1996/06/06', 'inflationary universe', 'field equations, nonlinear', 'bootstrap', 'effect, back reaction', 'expansion 1/N', 'symmetry breaking', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609007'],"[""Recent progress in the preheating phenomena for inflationary cosmology is reviewed. We first discuss estimates of the preheating time scale and particle production at the early stages of parametric amplification within the Mathieu and Lam'e approximations and we analyze their precision and limitations. The necessity of self-consistent calculations including the non-linearity of the field theory equations in an energy conserving scheme is stressed. The large N calculations including the field back-reaction are reviewed. For spontaneously broken theories the issue of symmetry restoration is analyzed. A discussion of the possibility and criterion for symmetry restoration is presented.""]",['1996-09-02'] +2197,['eng'],"['Moffat, J W']",['Lagrangian Formulation of a Solution to the Cosmological Constant Problem'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'Lagrangian formalism', 'vacuum state', 'energy, fluctuation', 'model, stochastic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608202'],"['A covariant Lagrangian formulation of a solution to the cosmological constant problem, based on vizualising the fluctuations of the vacuum energy as a non-equilibrium process with stochastic behaviour, is presented. The variational principle yields equations of motion for the cosmological ``constant"" $\\Lambda$, treated as a dynamical field, together with an equation for a Lagrange multiplier field $\\phi$, and the standard Einstein field equations with a variable cosmological constant term. A stochastic model of constant in the present epoch and its large value in an era of inflation in the early universe.']",['1996-08-30'] +2198,['eng'],"['Halzen, Francis', 'Stanev, T', 'Yodh, G B']",['Gamma Ray Astronomy with Muons'],['Astrophysics and Astronomy'],"['astrophysics', 'muon, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, energy', 'showers', 'cosmic radiation, particle source', 'muon, flux', 'counters and detectors, efficiency', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608201'],"[""Although gamma ray showers are muon-poor, they still produce a number of muons sufficient to make the sources observed by GeV and TeV telescopes observable also in muons. For sources with hard gamma ray spectra there is a relative `enhancement' of muons from gamma ray primaries as compared to that from nucleon primaries. All shower gamma rays above the photoproduction threshold contribute to the number of muons $N_\\mu$, which is thus proportional to the primary gamma ray energy. With gamma ray energy 50 times higher than the muon energy and a probability of muon production by the gammas of about 1\\%, muon detectors can match the detection efficiency of a GeV satellite detector if their effective area is larger by $10^4$. The muons must have enough energy for sufficiently accurate reconstruction of their direction for doing astronomy. These conditions are satisfied by relatively shallow neutrino detectors such as AMANDA and Lake Baikal and by gamma ray detectors like MILAGRO. TeV muons from gamma ray primaries, on the other hand, are rare because they are only produced by higher energy gamma rays whose flux is suppressed by the decreasing flux at the source and by absorption on interstellar light. We show that there is a window of opportunity for muon astronomy with the AMANDA, Lake Baikal and MILAGRO detectors.""]",['1996-08-30'] +2199,['eng'],"['Yoshida, S', 'Dai, H', 'Jui, C', 'Sommers, P']",['Extremely High Energy Neutrinos and their Detection'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, background', 'neutrino, cosmic radiation', 'cosmic radiation, particle source', 'pi, photoproduction', 'pi, leptonic decay', 'neutrino, production', 'energy spectrum, (neutrino)', 'defect, topological', 'astrophysics, string', 'astrophysics, monopole', 'neutrino, flux', 'neutrino, massless', 'neutrino, massive', 'showers, air', 'counters and detectors, fluorescence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608186'],"['We discuss in some detail the production of extremely high energy (EHE) neutrinos with energies above 10^18 eV. The most certain process for producing such neutrinos results from photopion production by EHE cosmic rays in the cosmic background photon field. However, using assumptions for the EHE cosmic ray source evolution which are consistent with results from the deep QSO survey in the radio and X-ray range, the resultant flux of neutrinos from this process is not strong enough for plausible detection. A measurable flux of EHE neutrinos may be present, however, if the highest energy cosmic rays which have recently been detected well beyond 10^20 eV are the result of the annihilation of topological defects which formed in the early universe. Neutrinos resulting from such decays reach energies of the grand unification (GUT) scale, and collisions of superhigh energy neutrinos with the cosmic background neutrinos initiate neutrino cascading which enhances the EHE neutrino flux at Earth. We have calculated the neutrino flux including this cascading effect for either massless or massive neutrinos and we find that these fluxes are conceivably detectable by air fluorescence detectors now in development. The neutrino-induced showers would be recognized by their starting deep in the atmosphere. We evaluate the feasibility of detecting EHE neutrinos this way using air fluorescence air shower detectors and derive the expected event rate. Other processes for producing deeply penetrating air showers constitute a negligible background.']",['1996-08-29'] +2200,['eng'],"['Halzen, Francis']",['Active Galaxies as Particle Accelerators'],['Astrophysics and Astronomy'],"['talk, Blois 1996/06/08', 'talk, Helsinki 1996/06/13', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'p, acceleration', 'photon, cosmic radiation', 'p, cosmic radiation', 'electron, cosmic radiation', 'cosmic radiation, flux', 'jet', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608185'],"['We present the theoretical arguments and describe the accumulating experimental evidence that jets, powered by supermassive black holes, are true cosmic accelerators. They produce photons of TeV energy, possible higher, and may be the enigmatic source of the highest energy cosmic rays. The features of the multi-wavelength emission spectrum are dictated by the interactions of electrons and protons, accelerated in the vicinity of the black hole, with the ambient light in the galaxy. Photoproduction of neutral pions by protons on UV light is the source of the highest energy photons, in which most of the bolometric luminosity of the galaxy may be emitted. They initiate an electromagnetic cascade which via pair production on the magnetic field and photon-photon interactions determines the emerging gamma-ray spectrum at lower energies. The lower energy photons, observed by conventional astronomical techniques, are, as a result of the cascade process, several generations removed from the primary high energy beams. The case that proton beams power active galaxies is far from conclusive. A three-prong technological assault on the problem will, in the near future, hopefully provide new insights into the structure of active galactic nuclei with the construction of second-generation atmospheric Cherenkov telescopes, large-scale EeV cosmic ray detectors and high energy neutrino telescopes.']",['1996-08-29'] +2201,['eng'],"['Porter, T', 'Protheroe, R J']",['Cosmic ray electrons and the diffuse gamma ray spectrum'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'cosmic radiation', 'electron, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'transport theory', 'Compton scattering', 'bremsstrahlung', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608182'],"['The bulk of the diffuse galactic gamma ray emission above a few tens of GeV has been conventionally ascribed to the decay of neutral pions produced in cosmic ray interactions with interstellar matter. This is based in part on the observed electron spectrum being relatively steep, implying a source spectrum with index 2.4. However, this steep spectrum may arise due to severe energy losses if the nearest acceleration region is about 50 pc or more away. Thus, flatter injection spectra are possible, and we investigate the consequences of this for the diffuse galactic gamma ray spectrum. We perform a propagation calculation for cosmic ray electrons, and use the resulting interstellar electron spectrum to obtain the gamma ray spectrum due to inverse Compton and bremsstrahlung interactions consistently from MeV to PeV energies. We find that inverse Compton scattering can contribute significantly to the high energy diffuse galactic gamma ray spectrum, and may dominate over neutral pion decay above about 10 GeV. We compare our results with available observations from satellite-borne telescopes, optical Cherenkov telescopes and air shower arrays. With future observations at TeV-PeV energies it should be possible to determine the average interstellar spectrum of cosmic ray electrons, and hence estimate their spectrum on acceleration.']",['1996-08-29'] +2202,['eng'],"['White, M', 'Silk, J']",['Observational Constraints on Open Inflation Models'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608177'],['We discuss observational constraints on models of open inflation. Current data from large-scale structure and the cosmic microwave background prefer models with blue spectra and/or Omega_0>=0.3--0.5. Models with minimal anisotropy at large angles are strongly preferred.'],['1996-08-28'] +2203,['eng'],"['Dolgov, A D']",['Higher spin fields and the problem of cosmological constant'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'field theory, vector', 'field theory, tensor', 'coupling, minimal', 'gravitation', 'space-time, de Sitter', 'effect, back reaction']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608175'],['The cosmological evolution of free massless vector or tensor (but not gauge) fields minimally coupled to gravity is analyzed. It is shown that there are some unstable solutions for these fields in De Sitter background. The back reaction of the energy-momentum tensor of such solutions to the original cosmological constant exactly cancels the latter and the expansion regime changes from the exponential to the power law one. In contrast to the adjustment mechanism realized by a scalar field the gravitational coupling constant in this model is time-independent and the resulting cosmology may resemble the realistic one.'],['1996-08-28'] +2204,['eng'],"['Lipunov, V M', 'Panchenko, I E']",['Pulsars revived by gravitational waves'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'n, matter', 'gravitational radiation', 'magnetic field', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608155'],"['Binary neutron stars mergers that are expected to be the most powerful source of energy in the Universe definitely exist in nature, as is proven by the observed behavior of the Hulse-Taylor binary radio pulsar. Though most of energy in such events is radiated in gravitational waves, there probably exist several mechanisms giving also electromagnetic radiation. We propose a new one, involving a revival of the radio pulsar several orbital cycles before the merger.']",['1996-08-26'] +2205,['eng'],"['Coble, K', 'Dodelson, S', 'Frieman, Joshua A']",['Dynamical Lambda Models of Structure Formation'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'astrophysics, fundamental constant', 'spectra', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'field theory, scalar', 'Goldstone particle', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608122'],"['Models of structure formation with a cosmological constant $\\Lambda$ provide a good fit to the observed power spectrum of galaxy clustering. However, they suffer from several problems. Theoretically, it is difficult to understand why the cosmological constant is so small in Planck units. Observationally, while the power spectra of cold dark matter plus $\\Lambda$ models have approximately the right shape, the COBE-normalized amplitude for a scale invariant spectrum is too high, requiring galaxies to be anti-biased relative to the mass distribution. Attempts to address the first problem have led to models in which a dynamical field supplies the vacuum energy, which is thereby determined by fundamental physics scales. We explore the implications of such dynamical are dynamical models for which the amplitude of the COBE-normalized spectrum matches the observations. We also calculate the cosmic microwave background anisotropies in these models and show that the angular power spectra are distinguishable from those of standard cosmological constant models.']",['1996-08-21'] +2206,['eng'],"['Mitsui, T', 'Mäki, K', 'Orito, S']",['Expected Enhancement of the Primary Antiproton Flux at the Solar Minimum'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'anti-p, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, particle source', 'astrophysics, model', 'model, solar', 'cosmic radiation, energy spectrum', 'astrophysics, missing-mass', 'supersymmetry', 'sparticle, annihilation', 'sparticle, neutral particle', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608123'],"[""We calculate the solar-modulated energy spectra of cosmic-ray antiprotons ($\\bar{p}$'s) from two candidate primary sources, i.e., evaporating primordial black holes and the annihilation of neutralino dark matter, as well as for the secondary $\\bar{p}$'s produced by cosmic-ray interactions with interstellar gas. A large enhancement toward the solar minimum phase emerges in the low-energy flux of $\\bar{p}$'s from the primary sources, whereas the flux of the secondary $\\bar{p}$'s, falling steeply below 2 GeV, does not significantly vary. This enables us to conduct a very sensitive search for primary $\\bar{p}$ components by precisely measuring the $\\bar{p}$ spectrum, especially at low energies, throughout the forthcoming solar minimum phase.""]",['1996-08-21'] +2207,['eng'],"['Samurovic, S', 'Celebonovic, V']",['A note on the neutrino decay line and the possibilities of its detection'],['Astrophysics and Astronomy'],"['neutrino, massive', 'massive, neutrino', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, model', 'neutrino, radiative decay', 'radiative decay, neutrino', 'neutrino, flavor', 'neutrino, lifetime', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9512029'],"['Using simple physical reasoning we have estimated the wavelengths and line-widths of spectral lines arising from the decays of massive neutrinos. We have, also, to some extent, discussed the possible consequences of these decays in observable astrophysical settings. We have compared our conclusions with the predictions of the decaying dark matter (DDM) model and cold + hot dark matter ({\\rm C\\nu ^2DM}) model.']",['1995-12-07'] +2208,['eng'],"['Ruffert, M', 'Schäfer, G']",['Coalescing neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'model, hydrodynamical', 'gravitational radiation', 'electron, density', 'energy loss', 'temperature', 'velocity', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509006'],"[""We investigate the dynamics and evolution of coalescing neutron stars. Although the code (Piecewise Parabolic Method) is purely Newtonian, we do include the emission of gravitational waves and their backreaction on the hydrodynamic flow. The properties of neutron star matter are described by the physical equation of state of Lattimer \\& Swesty (1991). Energy loss by all types of neutrinos and changes of the electron fraction due to the emission of electron neutrinos and antineutrinos are taken into account by an elaborate ``neutrino leakage scheme''. We simulate the coalescence of two identical, cool neutron stars with a baryonic mass of \\approx\\!1.6\\,M_\\odot and a radius of \\approx\\!15~km and with an initial center-to-center distance of 42~km. The initial distributions of density and electron concentration are given from a model of a cold neutron star in hydrostatic equilibrium (central temperature about 8\\,{\\rm MeV}). We investigate three cases which differ by the initial velocity distribution in the neutron stars, representing different cases of the neutron star spins relative to the direction of the orbital angular momentum vector. Within about 1~ms the neutron stars merge into a rapidly spinning (P_{\\rm spin}\\approx 1~ms), high-density body (\\rho\\approx 10^{14}~g/cm^3) with a surrounding thick disk of material with densities \\rho\\approx 10^{10}-10^{12}~g/cm^3 and orbital velocities of~0.3--0.5~c. In this work we evaluate the models in detail with respect to the gravitational wave emission using the quadrupole approximation. In a forthcoming paper we will concentrate on the neutrino emission and implications for gamma-ray bursters. A maximum luminosity in excess of 10^{55}~erg/s is reached for about 1~ms.""]",['1995-09-04'] +2209,['eng'],"['Fukuyama, T', 'Hatakeyama, M', 'Miyoshi, M', 'Morikawa, M', 'Nakamichi, A']",['Late-Time Mild Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'Hubble constant', 'field theory, scalar', 'energy', 'gravitation, fundamental constant', 'luminosity', 'light nucleus, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608097'],"['We explore the cosmological model in which a late-time mild inflation is realized after the star formation epoch. Non-vanishing curvature coupling of a classical boson field yields this mild inflation without a cosmological constant. Accordingly the lifetime of the present Universe is remarkably increased in our model. Thus we show that the present observed high value of the Hubble parameter $H_0 \\approx 70-80{\\rm km/sec/Mpc}$ is compatible with the age of the oldest stars $14{\\rm Gyr}$ without introducing the cosmological constant or the open Universe model. Moreover in our model, the local Hubble parameter becomes larger than the global one. Thus we show that the present observed local Hubble parameter measured by using the Cepheid variables is compatible with the global Hubble parameter measured by using the Sunyaev-Zeldovich effect. We also examine the energy conditions, evolution of the effective gravitational constant and the nucleosynthesis process.']",['1996-08-16'] +2210,['eng'],"['García-Bellido, J', 'Liddle, A R', 'Lyth, D H', 'Wands, D']",['Normalization of modes in an open universe'],['Astrophysics and Astronomy'],"['Friedman model', 'space-time, Robertson-Walker', 'random field, scalar', 'random field, tensor', 'unitarity', 'space-time']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608106'],"['We discuss the appropriate normalization of modes required to generate a homogeneous random field in an open Friedmann-Robertson-Walker universe. We consider scalar random fields and certain tensor random fields that can be obtained by covariantly differentiating a scalar. Modes of interest fall into three categories: the familiar sub-curvature modes, the more recently discussed super-curvature modes, and a set of discrete modes with positive eigenvalues which can be used to generate homogeneous tensor random fields even though the underlying scalar field is not homogeneous. A particular example of the last case which has been discussed in the literature is the bubble wall fluctuation in open inflationary universes.']",['1996-08-20'] +2211,['eng'],"['Raffelt, G G']",['Supernova Neutrino Opacities'],['Astrophysics and Astronomy'],"['talk, Helsinki 1996/06/13', 'astrophysics, supernova', 'neutrino nucleon, interaction', 'current, axial-vector', 'baryon, density', 'temperature', 'spin, density', 'nucleon, spin', 'correlation, spin', 'cross section', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608074'],"['In a supernova (SN) core during infall and after collapse, neutrinos are trapped by their interactions with nucleons. For the axial-vector current interactions it is not enough to include static particle-particle correlations. Even the single-nucleon spin autocorrelation reduces the scattering cross section dramatically. Therefore, the dynamical structure of the spin-density structure function has an important impact on neutrino transport in supernovae. At the present time, SN neutrino opacities cannot be calculated to a controlled degree of precision.']",['1996-08-14'] +2212,['eng'],"['Zimdahl, W', 'Pavón, D', 'Triginer, J']",['Cosmology with bulk pressure'],['Astrophysics and Astronomy'],"['talk, Ascona 1996/05/26', 'astrophysics', 'particle, production', 'pressure', 'gas', 'Boltzmann equation', 'back reaction', 'inflationary universe', 'thermodynamics, causality']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608060'],"['Different cooling rates of interacting fluid components of the expanding cosmic medium give rise to entropy producing bulk stresses. With the help of effective bulk pressures, on the other hand, one may phenomenologically take into account cosmological particle production processes. We report on recent progress in bulk viscous cosmology both on the phenomenological level and on the level of relativistic kinetic theory.']",['1996-08-14'] +2213,['eng'],"['Bednarek, I', 'Biesiada, M', 'Manka, R']",['QCD deconfinement'],['Astrophysics and Astronomy'],"['quark, matter', 'field equations, soliton', 'quark, confinement', 'quantum chromodynamics', 'critical phenomena, confinement', 'finite temperature', 'effective potential', 'temperature, dependence', 'photon, cosmic radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608053'],['In this paper we discuss the QCD phase-transitions in the nontopological soliton model of quark confinement and explore possible astrophysical consequences. Our key idea is to look at quark stars (which are believed to exist since the quark matter is energetically preferred over the ordinary matter) from the point of view of soliton model. We propose that the phase transition taking place during the core collapse of massive evolved star may provide a new physical effect not taken into account in modeling the supernova explosions. We also point out the possibility that merging quark stars may produce gamma-ray bursts energetic enough to be at cosmological distances. Our idea based on the finite-temperature nontopologiocal soliton model overcomes major difficulties present in neutron star merger scenario --- the baryon loading problem and nonthermal spectra of the bursts.'],['1996-08-12'] +2214,['eng'],"['Górski, K M', 'Ratra, B', 'Stompor, R', 'Sugiyama, N', 'Banday, A J']",['COBE-DMR-Normalized Open CDM Cosmogonies'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'matter, density', 'galaxy, production', 'inflationary universe, open', 'numerical calculations, interpretation of experiments', 'bibliography', 'tables']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608054'],"['Cut-sky orthogonal mode analyses of the COBE-DMR 53 and 90 GHz sky maps are used to determine the normalization of a variety of open cosmogonical models based on the cold dark matter scenario. To constrain the allowed cosmological-parameter range for these open cosmogonies, the predictions of the DMR-normalized models are compared to various observational measures of cosmography and large-scale structure, viz.: the age of the universe; small-scale dynamical estimates of the clustered-mass density parameter (Omega_0); constraints on the Hubble parameter (h), the X-ray cluster baryonic-mass fraction (Omega_B/Omega_0), and the matter power spectrum shape parameter; estimates of the mass perturbation amplitude; and constraints on the large-scale peculiar velocity field. The open-bubble inflation model is consistent with current determinations of the 95% confidence level range of these observational constraints.']",['1996-08-12'] +2215,['eng'],"['Bednarek, I', 'Manka, R']",['The soliton stars evolution'],['Astrophysics and Astronomy'],"['matter, soliton', 'relativity theory, general', 'surface tension', 'fermion number, density', 'space-time, de Sitter', 'domain wall', 'Friedman model', 'space-time, Schwarzschild', 'effective potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608055'],"['The evolution of a soliton star filled with fermions is studied in the framework of general relativity. Such a system can be described by the surface tension $\\sigma$, the bag constant $B$, and the fermion number density affects the spacetime inside the soliton. Whether it is described by Friedman or de Sitter metric depends on the prevailing parameter. The whole spacetime is devided by the surface of the soliton into the false vacuum region inside the soliton and the true vacuum region outside, the latter being described by the Schwarzschild line element. The aim of this paper is to study the equations of motion of the domain wall in two cases. In the first case the de Sitter metric describes the interior in the first case, and in the second case it is replaced by the Friedman metric. In both of them the Schwarzschild metric is outside the soliton. From the analysis of obtained equations one can draw conclusions concerning further evolution of a soliton star.']",['1996-08-12'] +2216,['eng'],"['Wands, D', 'García-Bellido, J']",['Density Perturbations from Two-field Inflation'],['Astrophysics and Astronomy'],"['talk, Ascona 1996/05/26', 'inflationary universe', 'density, perturbation', 'spectra, perturbation', 'perturbation, scalar', 'perturbation, tensor']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608042'],"['We discuss metric perturbations produced during a period of inflation in the early universe where two scalar fields evolve. The final scalar perturbation spectrum can be calculated in terms of the perturbed expansion along neighbouring trajectories in field-space. In the usual single field case this is fixed by the values of the fields at horizon-crossing, but in the presence of more than one field there is no longer a unique slow-roll trajectory. The presence of entropy as well as adiabatic fluctuations means that the super-horizon-sized metric perturbation $\\zeta$ may no longer be conserved and the evolution must be integrated along the whole of the subsequent trajectory. In general there is an inequality between the ratio of tensor to scalar perturbations and the tilt of the gravitational wave spectrum, which becomes an equality when only adiabatic perturbations are possible and $\\zeta$ is conserved.']",['1996-08-12'] +2217,['eng'],"['Sornborger, A T', 'Brandenberger, R H', 'Fryxell, B', 'Olson, K']",['The Structure of Cosmic String Wakes'],['Astrophysics and Astronomy'],"['astrophysics, string', 'baryon, matter', 'astrophysics, missing-mass', 'model, hydrodynamical', 'baryon, velocity', 'gravitation, potential', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608020'],"['The clustering of baryons and cold dark matter induced by a single moving string is analyzed numerically making use of a new three-dimensional Eulerian cosmological hydro code$^{1)}$ which is based on the PPM method to track the baryons and the PIC method to evolve the dark matter particles. A long straight string moving with a speed comparable to $c$ induces a planar overdensity (a``wake""). Since the initial perturbation is a velocity kick towards the plane behind the string and there is no initial Newtonian gravitational line source, the baryons are trapped in the center of the wake, leading to an enhanced baryon to dark matter ratio. The cold coherent flow leads to very low post--shock temperatures of the baryonic fluid. In contrast, long strings with a lot of small-scale structure (which can be described by adding a Newtonian gravitational line source) move slowly and form filamentary objects. The large central pressure due to the gravitational potential causes the baryons to be expelled from the central regions and leads to a relative deficit in the baryon to dark matter ratio. In this case, the velocity of the baryons is larger, leading to high post-shock temperatures.']",['1996-08-06'] +2218,['eng'],"['Kaiser, D I']",['Supercurvature Modes from Preheating in an Open Universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'postulated particle, inflaton', 'decay, inflaton']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608025'],"['Preheating following the inflationary phase in models of open inflation is considered. The most significant difference from a preheating scenario in flat space is that supercurvature modes can be populated and amplified in the open universe. In certain models, such modes can dominate the usual resonant particle production, thus altering the ensuing thermal history within an open universe. The accuracy to which the masses and couplings need to be tuned to produce such supercurvature modes, however, makes any large deviation from the flat space cases unlikely.']",['1996-08-06'] +2219,['eng'],"['Ramaty, R', 'Reeves, H', 'Lingenfelter, R E', 'Kozlovskii, B']",['LiBeB'],['Astrophysics and Astronomy'],"['talk, Notre Dame 1996/06/20', 'cosmic radiation, primary', 'cosmic radiation, acceleration', 'astrophysics, supernova', 'light nucleus, production', 'lithium', 'beryllium', 'boron, neutrinoproduction', 'yield, ratio', 'iron', 'neutrino, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608002'],"['We present new calculations of LiBeB production by accelerated particles with various compositions and energy spectra ranging from low energies to relativistic energies, and various ambient medium metallicities ($Z/Z_\\odot$). The observed, essentially constant, Be/Fe ratio as a function of $Z/Z_\\odot$ can be best understood if the metallicity of the accelerated particles (high energy or low energy) does not vary much with $Z/Z_\\odot$. This could be achieved if the particles are accelerated directly from the ejecta of Type II supernovae (SNII) and not from the interstellar medium. Using the observed Be/Fe and the fact that most of the Fe at low $Z/Z_\\odot$ is from SNII, we derive the energy content in accelerated particles per SNII (a few times 10$^{50}$ erg). We show that additional $^{11}$B production by neutrinos is consistent with the available data, allowing a neutrino yield from SNII less than or equal to the nominal published yields. We further show that the observed $^6$Li at low $Z/Z_\\odot$ suggests that the accelerated particles responsible for the LiBeB at such $Z/Z_\\odot$ are confined to low energies and have a relatively high He/O abundance.']",['1996-08-05'] +2220,['eng'],"['Green, A M', 'Liddle, A R']",['Open Inflationary Universes in the Induced Gravity Theory'],['Astrophysics and Astronomy'],"['inflationary universe', 'gravitation, induced', 'field theory, dilaton', 'potential', 'vacuum state', 'tunneling', 'density, perturbation', 'space-time, de Sitter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607166'],"[""The induced gravity theory is a variant of Jordan--Brans--Dicke theory where the `dilaton' field possesses a potential. It has the unusual feature that in the presence of a false vacuum there is a {\\em stable} static solution with the dilaton field displaced from the minimum of its potential, giving perfect de Sitter expansion. We demonstrate how this solution can be used to implement the open inflationary universe scenario. The necessary second phase of inflation after false vacuum decay by bubble nucleation is driven by the dilaton rolling from the static point to the minimum of its potential. Because the static solution is stable whilst the false vacuum persists, the required evolution occurs for a wide range of initial conditions. As the exterior of the bubble is perfect de Sitter space, there is no problem with fields rolling outside the bubble, as in one of the related models considered by Linde and Mezhlumian, and the expansion rates before and after tunnelling may be similar which prevents problematic high-amplitude super-curvature modes from being generated. Once normalized to the microwave background anisotropies seen by the COBE satellite, the viable models form a one-parameter family for each possible $\\Omega_0$.""]",['1996-08-01'] +2221,['eng'],"['Bahcall, J N', 'Krastev, P I']",['What can be learned by measuring the fluxes of the $^{7}$Be and the pep solar neutrino lines?'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'flux, neutrino', 'electron nucleus, interaction', 'interaction, electron nucleus', 'beryllium', 'electron, capture', 'capture, electron', 'p p, fusion', 'neutrino electron, elastic scattering', 'elastic scattering, neutrino electron', 'electron, energy spectrum', 'energy spectrum, electron', 'neutrino nucleus, interaction', 'interaction, neutrino nucleus', 'lithium', 'neutral current', 'electron number, conservation law', 'neutrino, sterile', 'neutrino, oscillation', 'neutrino/e', 'neutrino, mass', 'mass, neutrino', 'neutrino, mixing angle', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607013'],"['Measurements of the interaction rates of the solar neutrino lines of ^7Be and pep can be used, independent of solar models, to test whether electron flavor is conserved, to determine survival probabilities of electron-type neutrinos at specific energies, and to test for the existence of sterile neutrinos. We present analytic descriptions of these tests. We also illustrate by numerical simulations, assuming matter-enhanced and vacuum neutrino oscillations, what measurements of solar neutrino lines can teach us about neutrino masses and mixing angles.']",['1996-07-03'] +2222,['eng'],"['Stanev, T', 'Vankov, H P']",['The nature of the highest energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'photon, cosmic radiation', 'showers, air', 'magnetic field, geophysics', 'cosmic radiation, particle source', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607011'],['Ultra high energy gamma rays produce electron--positron pairs in interactions on the geomagnetic field. The pair electrons suffer magnetic bremsstrahlung and the energy of the primary gamma ray is shared by a bunch of lower energy secondaries. These processes reflect the structure of the geomagnetic field and cause experimentally observable effects. The study of these effects with future giant air shower arrays can identify the nature of the highest energy cosmic rays as either gamma-rays or nuclei.'],['1996-07-03'] +2223,['eng'],"['Protheroe, R J']",['High Energy Neutrinos from Blazars'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, flux', 'energy spectrum', 'neutrino/mu', 'antineutrino/mu', 'photon, cosmic radiation', 'astrophysics, model', 'cosmic radiation, acceleration', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607165'],"['I describe a model of energetic gamma ray and neutrino emission in blazars which is consistent with most of the gamma-ray observations, and use this model to estimate the diffuse intensity of high energy neutrinos from blazars.']",['1996-08-01'] +2224,['eng'],"['Gangui, A']",['Non-Gaussian Fluctuations From Textures'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1996/03/16', 'cosmic radiation, background', 'topology, defect', 'astrophysics, texture', 'cosmic radiation, fluctuation', 'correlation function', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607122'],"['One of the most powerful tools to probe the existence of cosmic defects in the early universe is through the Cosmic Microwave Background (CMB) radiation. It is well known that computations with causal sources are more involved than the adiabatic counterparts based on inflation, and this fact has in part hampered the development of fine detailed predictions. Analytical modeling, while necessarily limited in power, may tell us the overall characteristics of CMB from defects and hint at new features. We apply an analytical model for textures to the study of non-Gaussian features of the CMB sky and compare our predictions with the four-year COBE-DMR data.']",['1996-07-25'] +2225,['eng'],"['Hill, G C']",['Detecting Neutrinos from AGN'],['Astrophysics and Astronomy'],"['neutrino, astrophysics', 'neutrino, flux', 'astrophysics, galaxy', 'neutrino nucleon, inclusive reaction', 'antineutrino nucleon, inclusive reaction', 'neutrino/mu', 'charged current', 'neutral current', 'model, parton', 'cross section, energy dependence', 'electron p, deep inelastic scattering', 'p, structure function', 'momentum spectrum, parton', 'muon, neutrinoproduction', 'matter', 'counters and detectors', 'yield, (muon)', 'angular distribution, (muon)', 'neutrino, solar', 'astrophysics, model', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607140'],"['New information on the structure of the nucleon from the HERA ep collider leads to higher neutrino cross sections for the processes nu_mu + N --> mu + X needed to calculate the expected rates of astrophysical neutrino induced muons in large detectors either under construction, or in the design stage. These higher cross sections lead to higher muon rates for arrival angles where neutrino attenuation in the earth is less important. On the other hand, new estimates of AGN neutrino fluxes suggest that the expected muon rates in these detectors may be much lower than previously calculated. I use the new cross sections to calculate the expected muon rates and angular distributions in large detectors for a variety of AGN models and compare these rates with the atmospheric neutrino backrounds (from both conventional decay channels and the ""prompt"" charmed meson decay channels). If the lowest flux estimates are correct, there may be diffculties in determining the origin of a small excess of muons, due to the large uncertainty in the rate of the charmed meson neutrino production channel. However, the more optimistic AGN neutrino fluxes should be detectable in proposed detectors, such as DUMAND-II, AMANDA, NESTOR and Lake Baikal.']",['1996-07-30'] +2226,['eng'],"['Bonazzola, S', 'Frieben, J', 'Gourgoulhon, E']",['Triaxial neutron stars'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1996/01/20', 'n, matter', 'gravitational radiation', 'Einstein equation', 'dimension, 3', 'matter, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607123'],"[""Triaxial neutron stars may be important sources of gravitational radiation for the forthcoming generation of interferometric gravitational wave detectors such as LIGO, VIRGO, and GEO600. We investigate the viscosity triggered bar mode secular instability of rapidly rotating neutron stars by means of a perturbation analysis of numerically constructed ``exact'' general relativistic axisymmetric star models. In the theoretical approach, only the dominant parts of the nonaxisymmetric terms of the 3D-Einstein equations are taken into account. A comparison of our results with previous studies of Newtonian polytropic stars confirms James' classical result gamma_crit=2.238 for the critical polytropic index. Beyond the Newtonian regime, gamma_crit reveals a slight increase toward highly relativistic configurations. Six out of twelve employed realistic dense matter equations of state admit the spontaneous symmetry breaking for masses above 1.6 M_sol.""]",['1996-07-25'] +2227,['eng'],"['Widrow, L M']",['Modeling Collisionless Matter in General Relativity'],['Astrophysics and Astronomy'],"['relativity theory, general', 'matter', 'Klein-Gordon equation', 'Einstein equation', 'phase space', 'Vlasov equation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607124'],"['We propose a new numerical technique for following the evolution of a self-gravitating collisionless system in general relativity. Matter is modeled as a scalar field obeying the coupled Klein-Gordon and Einstein equations. A phase space distribution function, constructed using covariant coherent states, obeys the relativistic Vlasov equation provided the de Broglie wavelength for the field is very much smaller than the scales of interest. We illustrate the method by solving for the evolution of a system of particles in a static, plane-symmetric, background spacetime.']",['1996-07-25'] +2228,['eng'],"['Caldwell, R R', 'Battye, R A', 'Shellard, E P S']",['Relic Gravitational Waves from Cosmic Strings'],['Astrophysics and Astronomy'],"['gravitational radiation, spectra', 'astrophysics, string', 'effect, back reaction', 'mass, string', 'background, stochastic', 'counters and detectors', 'interference, laser', 'model, fluid', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607130'],"['We examine the spectrum of gravitational radiation emitted by a network of cosmic strings, with emphasis on the observational constraints and the opportunities for detection. The analysis improves over past work, as we use a phenomenological model for the radiation spectrum emitted by a cosmic string loop. This model attempts to include the effect of the gravitational back-reaction on the radiation emission by an individual loop with a high frequency cut-off in the spectrum. Comparison of the total spectrum due to a network of strings with the recently improved bound on the amplitude of a stochastic gravitational wave background, due to measurements of noise in pulsar signal arrival times, allows us to exclude a range of values of $\\mu$, the cosmic string linear mass density, for certain values of cosmic string and cosmological parameters. We find the conservative bound $G\\mu/c^2 < 5.4 (\\pm 1.1) \\times 10^{-6}$ which is consistent with all other limits. We consider variations of the standard cosmological scenario, finding that an under dense, of the spectrum probed by gravitational wave detectors is strongly sensitive to the thermal history of the cosmological fluid. We discuss the opportunity for the observation of this stochastic background by resonant mass and laser interferometer gravitational wave detectors.']",['1996-07-30'] +2229,['eng'],"['Capozziello, S', 'Ritis, R', ""Man'ko, V I"", 'Marino, A A', 'Marmo, G']",['Gravitational Waveguides in Cosmology'],['Astrophysics and Astronomy'],"['gravitational radiation', 'astrophysics', 'gravitation, lens', 'potential', 'electromagnetic field']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607125'],"['We discuss the possibility that, besides the usual gravitational lensing, there may exist a sort of gravitational waveguiding in cosmology which could explain some anomalous phenomena which cannot be understood by the current gravitational lensing models as the existence of ""brothers"" objects having different brilliancy but similar spectra and redshifts posed on the sky with large angular distance. Furthermore, such a phenomena could explain the huge luminosities coming from quasars using the cosmological structures as selfoc-type or planar waveguide. We describe the gravitational waveguide theory and then we discuss possible realizations in cosmology.']",['1996-07-25'] +2230,['eng'],"['Hindmarsh, M B', 'Sakellariadou, M', 'Vincent, G R']",['Cosmic Strings and Coherence'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1996/03/16', 'astrophysics, string', 'topology, defect', 'correlation function, time', 'scaling', 'matter, spectra', 'cosmic radiation, perturbation', 'Friedman model', 'coherent state', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607115'],"['Cosmic strings provide a radically different paradigm for the formation of structure to the prevailing inflationary one. They afford some extra technical complications: for example, the calculation of the power spectrum of matter and radiation perturbations requires the knowledge of the history of the evolution of the defects in the form of two-time correlation functions. We describe some numerical simulations of string networks, designed to measure the two-time correlations during their evolution.']",['1996-07-24'] +2231,['eng'],"['Turok, Neil G']",['A Causal Source which Mimics Inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'causality', 'perturbation', 'scaling', 'Einstein equation, linear', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607109'],"[""How unique are the inflationary predictions for the cosmic microwave anisotropy pattern? In this paper, it is asked whether an arbitrary causal source for perturbations in the standard hot big bang could effectively mimic the predictions of the simplest inflationary models. A surprisingly simple example of a `scaling' causal source is found to closely reproduce the inflationary predictions. This letter extends the work of a previous paper (ref. 6) to a full computation of the anisotropy pattern, including the Sachs Wolfe integral. I speculate on the possible physics behind such a source.""]",['1996-07-23'] +2232,['eng'],"['Grivell, I J', 'Liddle, A R']",['Accurate determination of inflationary perturbations'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'gravitational radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607096'],"['We use a numerical code for accurate computation of the amplitude of linear density perturbations and gravitational waves generated by single-field inflation models to study the accuracy of existing analytic results based on the slow-roll approximation. We use our code to calculate the coefficient of an expansion about the exact analytic result for power-law inflation; this generates a fitting function which can be applied to all inflationary models to obtain extremely accurate results. In the appropriate limit our results confirm the Stewart--Lyth analytic second-order calculation, and we find that their results are very accurate for inflationary models favoured by current observational constraints.']",['1996-07-21'] +2233,['eng'],"['Stanev, T']",['Ultra high energy cosmic rays and the large scale structure of the galactic magnetic field'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'p, cosmic radiation', 'cosmic radiation, energy spectrum', 'astrophysics, galaxy', 'magnetic field, galaxy', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607086'],['We study the deflection of ultra high energy cosmic ray protons in different models of the regular galactic magnetic field. Such particles have gyroradii well in excess of 1 kpc and their propagation in the galaxy reflects only the large scale structure of the galactic magnetic field. A future large experimental statistics of cosmic rays of energy above 10$^{19}$ eV could be used for a study of the large scale structure of the galactic magnetic field if such cosmic rays are indeed charged nuclei accelerated at powerful astrophysical objects and if the distribution of their sources is not fully isotropic.'],['1996-07-19'] +2234,['eng'],"['Viollier, R D']",['Gravitational Phase Transition of Heavy Neutrino Matter'],['Astrophysics and Astronomy'],"['neutrino, heavy', 'gravitation, critical phenomena', 'radiation, density', 'neutrino, gas', 'neutrino, matter', 'astrophysics, galaxy', 'astrophysics, quasar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607077'],"['We study the phase transition of a system of self-gravitating neutrinos in the presence of a large radiation density background in the framework of the Thomas-Fermi model. We show that, by cooling a non-degenerate gas of massive neutrinos below some critical temperature, a condensed phase emerges, consisting of quasi-degenerate supermassive neutrino stars. These compact dark objects could play an important role in structure formation in this universe, as they might in fact provide the seeds for galactic nuclei and quasi-stellar objects.']",['1996-07-18'] +2235,['eng'],"['Bezchastnov, V G', 'Haensel, P']",['Neutrino-electron scattering in dense magnetized plasma'],['Astrophysics and Astronomy'],"['neutrino electron, interaction', 'plasma', 'magnetic field, high', 'approximation, quasiclassical', 'differential cross section, angular dependence', 'differential cross section, energy dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9608090'],"['We derive exact expressions for the cross section of neutrino scattering on electrons in dense, hot stellar matter, in the presence of strong magnetic fields. Numerical calculations of the scattering cross sections at various densities, temperatures and magnetic fields, are performed. Strong, quantizing magnetic fields modify significantly the angular and energy dependence of the scattering cross section.']",['1996-08-15'] +2236,['eng'],"['Primack, Joel R', 'Klypin, A A']",['Dark matter and cosmology'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1996/02/14', 'astrophysics, missing-mass', 'galaxy', 'astrophysics, fundamental constant', 'astrophysics, model', 'energy spectrum', 'baryon, cluster', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607061'],"[""Here we discuss what are perhaps the two most popular variants of CDM that might agree with the data: \\lcdm\\ and CHDM. While the predictions of COBE-normalized \\lcdm\\ and CHDM both agree well with the available data on scales of \\sim 10 to 100 \\hMpc, each has potential virtues and defects. \\lcdm\\ with \\Omega_0 \\sim 0.3 has the possible virtue of allowing a higher expansion rate H_0 for a given cosmic age t_0, but the defect of predicting too much fluctuation power on small scales. CHDM has less power on small scales, so its predictions appear to be in good agreement with data on the galaxy distribution, but it remains to be seen whether it predicts early enough galaxy formation to be compatible with the latest high-redshift data. Also, two very recent observational results favor high cosmic density, and thus favor \\Omega=1 models such as CHDM over \\lcdm\\ --- (1) the positive deceleration parameter q_0>0 measured using high-redshift Type Ia supernovae, and (2) the low primordial deuterium/hydrogen ratio measured in two different quasar absorption spectra. We try to identify ``best'' variants of both \\lcdm\\ and CHDM, and discuss critical observational tests for both models.""]",['1996-07-15'] +2237,['eng'],"['Zanchin, V T', 'Lima, J A S', 'Brandenberger, R H']",['Accretion of Cold and Hot Dark Matter onto Cosmic String Filaments'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'astrophysics, string', 'mass, nonlinear', 'Friedman model', 'matter, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607062'],"['The Zeldovich approximation is applied to study the accretion of hot and cold dark matter onto moving long strings. It is assumed that such defects carry a substantial amount of small-scale structure, thereby acting gravitationally as a Newtonian line source whose effects dominate the velocity perturbations. Analytical expressions for the turn-around surfaces are derived and the mass inside of these surfaces is calculated. Estimates are given for the redshift dependence of $\\Omega_{nl}$, the fraction of mass in nonlinear objects. Depending on parameters, it is possible to obtain $\\Omega_{nl} = 1$ at the present time. Even with hot dark matter, the first nonlinear filamentary structures form at a redshift close to 100, and there is sufficient nonlinear mass to explain the observed abundance of high redshift quasars and damped Lyman alpha systems. These results imply that moving strings with small-scale structure are the most efficient seeds to produce massive nonlinear objects in the cosmic string model.']",['1996-07-17'] +2238,['eng'],"['Turner, M S']",['Detectability of inflation-produced gravitational waves'],['Astrophysics and Astronomy'],"['gravitational radiation, measurement', 'inflationary universe', 'quantum mechanics, fluctuation', 'cosmic radiation, anisotropy', 'cosmic radiation, background', 'polarization', 'interference, laser', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607066'],"['Detection of the gravitational waves excited during inflation as quantum mechanical fluctuations is a key test of inflation and crucial to learning about the specifics of the inflationary model. We discuss the potential of Cosmic Background Radiation (CBR) anisotropy and polarization and of laser interferometers such as LIGO, VIRGO/GEO and LISA to detect these gravity waves.']",['1996-07-17'] +2239,['eng'],"['Stern, B E', 'Svensson, R']",['Evidence for Chain Reaction in the Time Profiles of $\\Gamma$ Ray Bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, flux', 'flux, time variation', 'model, stochastic', 'model, avalanche', 'model, hydrodynamical', 'magnetic field', 'turbulence', 'n, matter', 'astrophysics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607070'],"['Although the time profiles of gamma ray bursts (GRBs) show extremely diverse behavior, their average statistical properties such as the average peak-aligned profile and the auto-correlation function show simple stretched-exponential behavior. This could indicate that the diversity of all bursts is just due to different random realizations of the same simple stochastic process where the process is scale invariant in time. We illustrate how both the diversity of GRB time profiles and some important average statistical properties can be reproduced in this way using a simple toy model for a stochastic pulse avalanche, which behaves as a chain reaction in a near-critical regime. We suggest that one possibility for the underlying physical process for generating GRBs could be a chain detonation in which reconnecting magnetic turbulent features trigger each other.']",['1996-07-17'] +2240,['eng'],"['Hagmann, C', 'Kinion, D S', 'Stoeffl, W', 'Van Bibber, K', 'Daw, E J', 'McBride, J', 'Peng, H', 'Rosenberg, L J', 'Xin, H', 'La Veigne, J D', 'Sikivie, P', 'Sullivan, N', 'Tanner, D B', 'Moltz, D M', 'Nezrick, F', 'Turner, M', 'Golubev, N A', 'Kravchuk, L V']",['First results from a second generation galactic axion experiment'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1996/02/14', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'search for, axion', 'mass, axion', 'axion, mass', 'Primakoff effect', 'experimental methods', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607022'],"['We report first results from a large scale search for dark matter axions. The experiment probes axion masses of 1.3-13 micro-eV at a sensitivity which is about 50 times higher than previous pilot experiments. We have already scanned part of this mass range at a sensitivity better than required to see at least one generic axion model, the KSVZ axion. Data taking at full sensitivity commenced in February 1996 and scanning the proposed mass range will require three years.']",['1996-07-04'] +2241,['eng'],"['Stecker, F W']",['$\\gamma$-rays and neutrinos from dark matter'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1996/02/14', 'astrophysics, missing-mass', 'neutralino, annihilation', 'LSP, decay', 'photon, production', 'neutrino, production', 'flux, energy spectrum', 'background', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607037'],"['High energy gamma-rays and neutrinos can be produced both by the annihilation and by the possible slow decay of dark matter particles. We discuss the fluxes and spectra of such secondaries produced by dark matter particles in the universe and their observability in competition with other astrophysical gamma-ray signals and with atmospheric neutrinos. To do this, we work within the assumption that the dark matter particles are neutralinos which are the lightest supersymmetric particles (LSPs) predicted by supersymmetry theory.']",['1996-07-08'] +2242,['eng'],"['Bunn, E F', 'Liddle, A R', 'White, M']",['Four-year COBE normalization of inflationary cosmologies'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'density, perturbation', 'gravitational radiation', 'potential', 'astrophysics, fundamental constant', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607038'],"['We supply fitting formulae enabling the normalization of slow-roll inflation models to the four-year COBE data. We fully include the effect of the gravitational wave modes, including the predicted relation of the amplitude of these modes to that of the density perturbations. We provide the normalization of the matter power spectrum, which can be directly used for large-scale structure studies. The normalization for tilted spectra is a special case. We also provide fitting functions for the inflationary energy scale of COBE-normalized models and discuss the validity of approximating the spectra by power-laws. In an Appendix, we extend our analysis to include models with a cosmological constant, both with and without gravitational waves.']",['1996-07-08'] +2243,['eng'],"['Castellani, V', ""Degl'Innocenti, S"", 'Fiorentini, G', 'Lissia, M', 'Ricci, B']",['Solar neutrinos'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'flux, neutrino', 'model, solar', 'temperature, solar', 'nucleus nucleus, nuclear reaction', 'helium, nuclide', 'p p, fusion', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606180'],"['After a short survey of the physics of solar neutrinos, giving an overview of hydrogen burning reactions, predictions of standard solar models and results of solar neutrino experiments, we discuss the solar-model-independent indications in favour of non-standard neutrino properties. The experimental results look to be in contradiction with each other, even disregarding some experiment: unless electron neutrinos disappear in their trip from the sun to the earth, the fluxes of intermediate energy neutrinos (those from 7Be electron capture and from the CNO cycle) result to be unphysically negative, or anyway extremely reduced with respect to standard solar model predictions. Next we review extensively non-standard solar models built as attempts to solve the solar neutrino puzzle. The dependence of the central solar temperature on chemical composition, opacity, age and on the values of the astrophysical S-factors for hydrogen-burning reactions is carefully investigated. Also, possible modifications of the branching among the various pp-chains in view of nuclear physics uncertainties are examined. Assuming standard neutrinos, all solar models examined fail in reconciling theory with experiments, even when the physical and chemical inputs are radically changed with respect to present knowledge and even if some of the experimental results are discarded.']",['1996-07-01'] +2244,['eng'],"['Blasi, P']",['High energy $\\gamma$ rays from old accreting neutron stars'],['Astrophysics and Astronomy'],"['astrophysics, model', 'n, matter', 'magnetic field', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, acceleration', 'model, shock waves', 'p p, inclusive reaction', 'pi0, hadroproduction', 'hadroproduction, pi0', 'photon, hadroproduction', 'hadroproduction, photon', 'numerical calculations', 'proposed experiment', 'p p --> pi0 anything']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606173'],"[""We consider a magnetized neutron star with accretion from a companion star or a gas cloud around it, as a possible source of gamma rays with energy between 100 MeV and 10^{14}-10^{16}~eV. The flow of the accreting plasma is terminated by a shock at the Alfv\\'en surface. Such a shock is the site for the acceleration of particles up to energies of \\sim 10^{15}-10^{17}~eV; gamma photons are produced in the inelastic pp collisions between shock-accelerated particles and accreting matter. The model is applied to old neutron stars both isolated or in binary systems. The gamma ray flux above 100~MeV is not easily detectable, but we propose that gamma rays with very high energy could be used by Cherenkov experiments as a possible signature of isolated old neutron stars in dense clouds in our galaxy.""]",['1996-07-01'] +2245,['eng'],"['Chardonnet, P', 'Mignola, G', 'Salati, Pierre', 'Taillet, R']",['Galactic diffusion and the antiproton signal of supersymmetric dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'supersymmetry', 'cosmic radiation, galaxy', 'sparticle, annihilation', 'annihilation, sparticle', 'neutralino', 'anti-p, production', 'production, anti-p', 'diffusion, anti-p', 'yield, (anti-p p)', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606174'],"['The leaky box model is now ruled out by measurements of a cosmic ray gradient throughout the galactic disk. It needs to be replaced by a more refined treatment which takes into account the diffusion of cosmic rays in the magnetic fields of the Galaxy. We have estimated the flux of antiprotons on the Earth in the framework of a two-zone diffusion model. Those species are created by the spallation reactions of high-energy nuclei with the interstellar gas. Another potential source of antiprotons is the annihilation of supersymmetric particles in the dark halo that surrounds our Galaxy. In this letter, we investigate both processes. Special emphasis is given to the antiproton signature of supersymmetric dark matter. The corresponding signal exceeds the conventional spallation flux below 300 MeV, a domain that will be thoroughly explored by the Antimatter Spectrometer experiment. The propagation of the antiprotons produced in the remote regions of the halo back to the Earth plays a crucial role. Depending on the energy, the leaky box estimates are wrong by a factor varying from 0.5 up to 3.']",['1996-07-01'] +2246,['eng'],"['Bahcall, J N']",['How well do standard solar models describe the results of solar neutrino experiments?'],['Astrophysics and Astronomy'],"['talk, Naples 1996/03/18', 'astrophysics', 'model, solar', 'neutrino, solar', 'neutrino, flux', 'flux, neutrino', 'neutrino, oscillation', 'neutrino, mass', 'mass, neutrino', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606161'],['The neutrino fluxes calculated from the 14 standard solar models published recently in refereed journals are inconsistent with the results of the 4 pioneering solar neutrino experiments if nothing happens to the neutrinos after they are created in the solar interior. The calculated fluxes and the experimental results are in good agreement if neutrino oscillations occur.'],['1996-06-27'] +2247,['eng'],"['Petry, D', 'Bradbury, S M', 'Konopelko, A K', 'Fernández, J']",['Detection of VHE $\\gamma$-rays from Mkn 421 with the HEGRA Cherenkov telescopes'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'Cherenkov counter, imaging', 'experimental results', '> 1000 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606159'],"['A detection of Gamma-rays from Mkn 421 at energies above 1 TeV is reported, based on observations made in December 1994 - May 1995 with the first two HEGRA Cherenkov telescopes. From the image analysis, 111 excess gamma candidates are obtained from the 26 h Telescope #1 (CT1) dataset (significance 4.0 sigma) and 218 from the 41 h Telescope #2 (CT2) dataset (significance 4.2 sigma) at zenith angles theta < 25 degrees. The combined significance is approx. 5.8 sigma. This is the second detection of Mkn 421 at TeV energies. The average excess rate is 4.3 +- 1.0 h^-1 for CT1 and 5.4 +- 1.3 h^-1 for CT2. Comparison with our contemporary observations of the Crab Nebula indicates that Mkn 421 has a steeper spectrum than the Crab Nebula above 1 TeV. Under the assumption that the spectrum of Mkn 421 follows a power law, we obtain a differential spectral index of 3.6 +- 1.0 and an integral flux above 1 TeV of 8 (+-2)_(Stat) (+6-3)_(Syst) x 10^-12 cm^-2 s^-1 from a comparison with Monte Carlo data. This flux is smaller than the Crab Nebula flux by a factor of 2.0 +- 0.8.']",['1996-06-27'] +2248,['eng'],"['Cheng, B', 'Olinto, A V', 'Schramm, David N', 'Truran, J W']",['Constraints on the strength of primordial magnetic fields from big bang nucleosynthesis revisited'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'magnetic field, constraint', 'electron, magnetic moment', 'magnetic moment, electron', 'weak interaction', 'positron n, exclusive reaction', 'neutrino n, exclusive reaction', 'n, semileptonic decay', 'semileptonic decay, n', 'electron, density', 'neutrino, density', 'numerical calculations', 'positron n --> p antineutrino/e', 'neutrino n --> p electron']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606163'],"['In this paper, we revisit in detail the effects of primordial magnetic fields on big bang nucleosynthesis (BBN) including a discussion of the magnetic field geometry and the anomalous magnetic moment. The presence of magnetic fields affects BBN by (1) increasing the weak reaction rates; (2) increasing the electron density due to changes to the electron phase space; and (3) by increasing the expansion rate of the universe, due both to the magnetic field energy density and to the modified electron energy density. Of the effects considered, the increase in the expansion rate due to the magnetic field energy is the most significant for the interests of BBN. The allowed magnetic field intensity at the end of nucleosynthesis (0.01 MeV) is about 2 \\times 10^{9}G and corresponds to an upper limit on the magnetic field energy density of about 28\\% of the neutrino energy density (\\rho_B \\le 0.28 \\rho_\\nu).']",['1996-06-27'] +2249,['eng'],"['Sikivie, P']",['What is the spectrum of cold dark matter particles on earth?'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1996/02/14', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'velocity, spectra', 'spectra, velocity', 'astrophysics, galaxy', 'angular momentum', 'phase space', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606151'],['It is argued that the spectrum of cold dark matter particles on Earth has peaks in velocity space associated with particles falling onto the Galaxy for the first time and with particles which have fallen in and out of the Galaxy only a small number of times in the past. Estimates are given for the sizes and velocity magnitudes of the first few peaks. The estimates are based upon the secondary infall model of halo formation which has been generalized to include the effect of angular momentum.'],['1996-06-25'] +2250,['eng'],"['Cillis, A N', 'Harari, D D']",['Photon-graviton conversion in a primordial magnetic field and the cosmic microwave background'],['Astrophysics and Astronomy'],"['postulated particle, graviton', 'transition, photon graviton', 'magnetic field, external field', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'plasma, effect']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9609200'],['We reconsider the effects of photon-graviton conversion in a primordial magnetic field upon the cosmic microwave background radiation. We argue that plasma effects make the photon-graviton conversion process negligible.'],['1996-10-01'] +2251,['eng'],"['Vincent, G R', 'Hindmarsh, M B', 'Sakellariadou, M']",['Correlations in cosmic string networks'],['Astrophysics and Astronomy'],"['astrophysics, string', 'space-time, Minkowski', 'correlation, energy-momentum', 'scaling', 'spectra, perturbation', 'perturbation, spectra', 'Friedman model', 'correlation function', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606137'],"['We investigate scaling and correlations of the energy and momentum in an evolving network of cosmic strings in Minkowski space. These quantities are of great interest, as they must be understood before accurate predictions for the power spectra of the perturbations in the matter and radiation in the early Universe can be made. We argue that Minkowski space provides a reasonable approximation to a Friedmann background for string dynamics and we use our results to construct a simple model of the network, in which it is considered to consist of randomly placed segments moving with random velocities. This model works well in accounting for features of the two-time correlation functions, and even better for the power spectra.']",['1996-06-24'] +2252,['eng'],"['Schmid, C', 'Schwarz, Dominik J', 'Widerin, P']","[""Peaks above the Harrison-Zel'dovich spectrum due to the quark-gluon to hadron transition""]",['Astrophysics and Astronomy'],"['talk, Batavia 1996/03/28', 'talk, Ascona 1996/05/26', 'astrophysics, model', 'transition, quark hadron', 'transition, gluon hadron', 'spectra, perturbation', 'perturbation, spectra', 'critical phenomena', 'density, perturbation', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606125'],"[""We investigate the effect of the quark-gluon to hadron transition at T_\\star\\sim 150 MeV on the evolution of primordial cosmological perturbations, in particular distortions of the Harrison-Zel'dovich spectrum. If the phase transition is first order, the sound velocity vanishes during the transition. Thus, density perturbations fall freely for about a Hubble time. The primordial Harrison-Zel'dovich rms density fluctuations for scales below the Hubble radius at the transition develop peaks and dips, which grow linearly with the wavenumber, both for the hadron-photon-lepton fluid and for cold dark matter. The large peaks in the spectrum may affect primordial black hole formation, big bang nucleosynthesis, and they produce cold dark matter clumps of 10^{-8} to 10^{-11} M_\\odot.""]",['1996-06-21'] +2253,['eng'],"['Bonazzola, S', 'Gourgoulhon, E']",['Gravitational waves from accreting neutron stars'],['Astrophysics and Astronomy'],"['talk, Pisa 1996/03/19', 'gravitational radiation', 'astrophysics', 'n, matter', 'symmetry breaking', 'nuclear matter', 'proposed experiment', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606123'],['We show that accreting neutron stars in binary systems or in Landau-Thorne-Zytkow objects are good candidates for continuous gravitational wave emission. Their gravitational radiation is strong enough to be detected by the next generation of detectors having a typical noise of 10^{-23} Hz^{-1/2}.'],['1996-06-21'] +2254,['eng'],"['Magueijo, J']",['The Doppler peaks from a generic defect'],['Astrophysics and Astronomy'],"['astrophysics, string', 'astrophysics, texture', 'topology, defect', 'inflationary universe', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606073'],"[""We investigate which of the exotic Doppler peak features found for textures and cosmic strings are generic novelties pertaining to defects. We find that the ``out of phase'' texture signature is an accident. Generic defects, when they generate a secondary peak structure similar to inflation, apply to it an additive shift. It is not necessary for this shift to be ``out of phase''. We also show which factors are responsible for the absence of secondary oscillations found for cosmic strings. Within this general analysis we finally consider the conditions under which topological defects and inflation can be confused. It is argued that only \\Omega=1 inflation and a defect with a horizon size coherence length have a chance to be confused. Any other inflationary or defect model always differ distinctly. (To appear in the proceedings of the XXXIth Moriond meeting, ``Microwave Background Anisotropies'')""]",['1996-06-14'] +2255,['eng'],"['Parente, G', 'Zas, E']",['Neutrino induced events in the Pierre Auger detector'],['Astrophysics and Astronomy'],"['talk, Venice 1996/02/27', 'neutrino, cosmic radiation', 'neutrino nucleon, interaction', 'interaction, neutrino nucleon', 'showers, air', 'trigger', 'neutrino, flux', 'flux, neutrino', 'astrophysics, particle source', 'defect, topological', 'cosmic radiation, background', 'microwaves', 'shower detector, proposed', 'acceptance', 'efficiency', 'Cherenkov counter, water', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606091'],"['We study the potential of the Pierre Auger detector for horizontal air showers initiated by ultra high energy neutrino. Assuming some simple trigger requirements we obtain measurable event rates for neutrino fluxes from AGN, from topological defects and from the interactions of cosmic rays with the microwave background.']",['1996-06-17'] +2256,['eng'],"['Turok, Neil G']",['Sub-degree scale microwave anisotropies from cosmic defects'],['Astrophysics and Astronomy'],"['astrophysics, texture', 'topology, defect', 'field equations, monopole', 'cosmic radiation, anisotropy', 'spectra, fluctuation', 'fluctuation, spectra', 'astrophysics, string', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606087'],"['If current ideas about unified field theories are correct, macroscopic cosmic defects may well exist. The observation of such an entity would have enormous significance for our understanding of fundamental physics. This paper points out a novel observable signature of cosmic texture and global monopoles, namely strong hot spots in the cosmic microwave anisotropy pattern on subdegree scales. This signal should be readily detectable by the next generation of anisotropy mapping experiments. The signature arises from overdensities in the photon-baryon fluid generated by the gravitational attraction of the defects. The angular power spectrum of the anisotropy fluctuations on subdegree scales is also calculated, for cosmic string, global monopoles, and texture.']",['1996-06-17'] +2257,['eng'],"['Moffat, J W']",['A Solution to the Cosmological Constant Problem'],['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'model, stochastic', 'vacuum state', 'energy, fluctuation', 'inflationary universe']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606071'],"['The fluctuations of the vacuum energy are treated as a non-equilibrium process and a stochastic model for the cosmological constant is presented, which yields a natural explanation for the smallness or zero value of the constant in the present epoch and its large value in an era of inflation in the early universe.']",['1996-06-18'] +2258,['eng'],"['Lohiya, D', 'Mahajan, S M', 'Mukherjee, A', 'Batra, A']",['Nucleosynthesis in a simmering universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'weak interaction', 'p, semileptonic decay', 'semileptonic decay, p', 'temperature', 'Friedman model', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606082'],"['Primordial nucleosynthesis is considered a success story of the standard big bang (SBB) cosmology. The cosmological and elementary particle physics parameters are believed to be severely constrained by the requirement of correct abundances of light elements. We demonstrate nucleosynthesis in a class of models very different from SBB. In these models the cosmological scale factor increases linearly with time from the period during which nucleosynthesis occurs. It turns out that weak interactions remain in thermal equilibrium upto temperatures which are two orders of magnitude lower than the corresponding temperatures in SBB. Inverse beta decay of the proton can ensure adequate production of several light elements while producing primordial metallicity much higher than that produced in SBB. Other attractive features of these models are the absence of the horizon, flatness and initial singularity problems, consistency with the age of globular clusters and consistent relationships between redshift and luminosity distance, angular diameter distance and the galaxy number count.']",['1996-06-14'] +2259,['eng'],"['Krauss, L M']",['Problems and Challenges for Cosmology involving Massive Neutrinos'],['Astrophysics and Astronomy'],"['lectures, Venice 1996/02/27', 'astrophysics, model', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'baryon, density', 'neutrino, massive', 'massive, neutrino', 'energy, density', 'astrophysics, fundamental constant', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606072'],"['I review the challenges and problems facing the standard cosmological model, involving an $\\Omega=1$ Universe dominated by non-baryonic dark matter, which arise due to: age estimates of the universe, estimates of the baryon fraction of the universe, and structure formation. Certain of these problems are exacerbated, and certain of these are eased, by the inclusion of some component to the energy density of matter from massive neutrinos. I conclude with a comparison of the two favored current cosmological models, involving either a mixture of cold dark matter and hot dark matter, or the inclusion of a cosmological constant.']",['1996-06-18'] +2260,['eng'],"['Copi, C J', 'Schramm, David N', 'Turner, M S']",['The Big-Bang Nucleosynthesis Limit to the Number of Neutrino Species'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'neutrino, massless', 'massless, neutrino', 'neutrino, flavor', 'helium', 'lithium', 'baryon, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606059'],"['Concern about systematic uncertainty in the $^4$He abundance as well as the chemical evolution of $^3$He leads us to re-examine this important limit. It is shown that with conservative assumptions no more than the equivalent of 4 massless neutrino species are allowed. Even with the most extreme estimates of the astrophysical uncertainties a meaningful limit still exists, less than 5 massless neutrino species, and illustrates the robustness of this argument. A definitive measurement of the deuterium abundance in high-redshift hydrogen clouds should soon sharpen the limit.']",['1996-06-18'] +2261,['eng'],"['Bar-Kana, R']",['Limits on a Stochastic Background of Gravitational Waves from Gravitational Lensing'],['Astrophysics and Astronomy'],"['gravitational radiation', 'background, stochastic', 'gravitation, lens', 'spectra', 'space-time, perturbation', 'cosmic radiation, anisotropy', 'energy, density', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606065'],"['We compute the effects of a stochastic background of gravitational waves on multiply imaged systems or on weak lensing. There are two possible observable effects, a static relative deflection of images or shear, and an induced time-dependent shift or proper motion. We evaluate the rms magnitude of these effects for a COBE normalized, scale-invariant spectrum, which is an upper limit on spectra produced by inflation. Previous work has shown that large-scale structure may cause a relative deflection large enough to affect observations, but we find that the corresponding effect of gravity waves is smaller by $\\sim 10^4$ and so cannot be observed. This results from the oscillation in time as well as the redshifting of the amplitude of gravity waves. We estimate the magnitude of the proper motion induced by deflection of light due to large-scale structure, and find it to be $\\sim 10^{-8}$ arcsec per year. This corresponds to $\\sim 50$ km/s at cosmological distances, which is quite small compared to typical peculiar velocities. The COBE normalized gravity wave spectrum produces motions smaller still by $\\sim 10^2$. We conclude that light deflection due to these cosmological perturbations cannot produce observable proper motions of lensed images. On the other hand, there are only a few known observational limits on a stochastic background of gravity waves at astrophysical wavelengths. High-resolution imaging of lens systems with VLBI can set limits on the relative motions of images. We show that a limit on gravity waves of $\\Omega_{\\lambda} \\labout 10^{-5}$, valid for wavelengths $\\lambda$ greater than a few pc (up to $\\sim 100$ Mpc), is feasible with a ten-year observation of a four-image system.']",['1996-06-18'] +2262,['eng'],"['Kull, A', 'Treumann, R A', 'Böhringer, H']",['Violent Relaxation of Indistinguishable Objects and Neutrino Hot Dark Matter in Clusters of Galaxies'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, massive', 'massive, neutrino', 'cluster, galaxy', 'statistical mechanics', 'matter, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606057'],"['The statistical mechanical investigation of violent relaxation (Lynden-Bell 1967) is extended to indistinguishable objects. It is found that, coincidentally, the equilibrium distribution is the same as that obtained for classical objects. For massive neutrinos the Tremaine \\& Gunn (1979) phase space bound is revisited and reinterpretated as the limit indicating the onset of degeneracy related to the coarse-grained phase space distribution. In the context of one of the currently most popular cosmological models, the Cold and Hot Dark Matter (CHDM) model (Primack et al. 1995), the onset of degeneracy may be of importance in the core region of clusters of galaxies. Degeneracy allows the neutrino HDM density to exceed the limit imposed by the Tremaine \\& Gunn (1979) bound while accounting for the phase space bound.']",['1996-06-18'] +2263,['eng'],"['Turner, M S']",['Cosmology'],['Astrophysics and Astronomy'],"['lectures, Stanford 1994/08/08', 'astrophysics, model', 'astrophysics, missing-mass', 'inflationary universe', 'density, perturbation', 'gravitational radiation, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703196'],"['In these lectures I review the standard hot big-bang cosmology, emphasizing its successes, its shortcomings, and its major challenges---developing a detailed understanding of the formation of structure in the Universe and identifying the constituents of the ubiquitous dark matter. I then discuss the motivations for--and the fundamentals of--inflationary cosmology, particularly emphasizing the quantum origin of metric (density and gravity-wave) perturbations. Inflation addresses the shortcomings of the standard cosmology, specifies the nature of the dark matter, and provides the ""initial data"" for structure formation. I conclude by addressing the implications of inflation for structure formation and discussing the different versions of cold dark matter. The flood of data--from the Heavens and from Earth--should in the next decade test inflation and discriminate between the different cold dark matter models.']",['1997-04-01'] +2264,['eng'],"['González-Mestres, L']",['Superluminal matter and high-energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation', 'postulated particle, superluminal', 'particle, annihilation', 'annihilation, particle']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606054'],"['High-energy cosmic ray events present important challenges to particle astrophysics. Their nature and origin are often not well understood and, as they occur in an energy domain not accessible to particle accelerators, there is no clear guide to their interpretation. We recently proposed a new, non-tachyonic, possible class of superluminal particles which may play an important cosmological role. In this note, we would like to point out that such particles, if they exist, are able to produce very high energy cosmic rays compatible with discoveries reported in the literature.']",['1996-06-11'] +2265,['eng'],"['Cohn, J D']",['Open universes from bubbles'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1996/03/16', 'inflationary universe, open', 'vacuum state, bubble', 'spectra, perturbation', 'perturbation, spectra', 'vacuum state, fluctuation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606052'],"['An introduction to models of open universes originating from bubbles, including a summary of recent theoretical results for the power spectrum. To appear in the proceedings of the XXXIth Moriond meeting, ""Microwave Background Anisotropies.""']",['1996-06-11'] +2266,['eng'],"['García-Bellido, J', 'Wands, D']",['The spectrum of curvature perturbations from hybrid inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606047'],"['We study the amplitude and spectral tilt of density perturbations in the simplest hybrid inflation models. We give an exact expression for the amplitude of quantum fluctuations on all scales in the limit where we can neglect the backreaction on the metric. This is a very good approximation for values of the inflaton field well below the Planck scale and our results remain valid far from the usual massless limit. We confirm that the primordial density spectrum in this model has a constant spectral index n>1 over all observable scales. For the small values of the tilt (n<1.4) required by observations, the results remain close to those obtained using the quasi-massless approximation.']",['1996-06-11'] +2267,['eng'],"['Grifols, J A', 'Massó, E', 'Toldrà, R']",['$\\gamma$ rays from SN1987A due to pseudoscalar conversion'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'flux, cosmic radiation', 'cosmic radiation, flux', 'pseudoscalar particle, production', 'production, pseudoscalar particle', 'Primakoff effect', 'pseudoscalar particle, radiative decay', 'radiative decay, pseudoscalar particle', 'astrophysics, supernova', 'magnetic field, galaxy', 'effective Lagrangian', 'coupling, (pseudoscalar particle 2photon)', '(pseudoscalar particle 2photon), coupling', 'upper limit', 'interpretation of experiments', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606028'],"['A light pseudoscalar coupled to two photons would be copiously emitted by the core of a supernova. Part of this flux would be converted to \\gamma-rays by the galactic magnetic field. Measurements on the SN1987A \\gamma-ray flux by the Gamma-Ray Spectrometer on the Solar Maximum Mission satellite already imply a bound on the coupling g < 3 \\times 10^{-12} GeV^{-1}. The improved generation of satellite-borne detectors, like EGRET or the project GLAST, could be able to detect a pseudoscalar-to-photon signal from a nearby supernova, for allowed values of g.']",['1996-06-06'] +2268,['eng'],"['Burrows, A']",['Towards a synthesis of core-collapse supernova theory'],['Astrophysics and Astronomy'],"['review', 'astrophysics, supernova', 'model, hydrodynamical', 'transport theory', 'neutrino, interaction', 'matter', 'light nucleus, production', 'astrophysics, pulsar', 'gravitational radiation', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606035'],"['New insights into the mechanism and character of core--collapse supernova explosions are transforming the approach of theorists to their subject. The universal realization that the direct hydrodynamic mechanism does not work and that a variety of hydrodynamic instabilities can influence the viability of theoretical explosions has ushered in a new era in supernova modeling. In this paper, I discuss the important physical and technical issues that remain. I review the neutrino--driven mechanism, the possible roles of Rayleigh--Taylor instabilities, questions in neutrino transport, and the various observational constraints within which theorists must operate. However, a consensus has yet to be achieved among active workers concerning many important details and some essential phenomenology. This synopsis is meant to accomplish two things: 1) to focus attention on the interesting problems whose resolution will bring needed progress, and 2) to assess the current status of the theoretical art.']",['1996-06-06'] +2269,['eng'],"['Cardall, C Y', 'Fuller, G M']",['Three-generation neutrino mixing and LSND dark matter neutrinos'],['Astrophysics and Astronomy'],"['talk, Santa Fe 1996/02/14', 'neutrino, interference', 'neutrino, mass', 'mass, neutrino', 'mass, hierarchy', 'hierarchy, mass', 'mass, oscillation', 'oscillation, mass', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, mixing angle', 'neutrino, sterile', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606024'],"[""The reported signal at the LSND experiment, when interpreted as neutrino mixing with \\delta m^2 = 6 \\;\\rm{eV}^2, provides evidence for neutrinos with a cosmologically significant mass. However, attempts to reconcile this interpretation of the experiment with other hints about neutrino properties require a (sterile) fourth neutrino and/or an ``inverted'' neutrino mass hierarchy. An interpretation of the LSND experiment employing \\delta m^2 = 0.3\\; \\rm{eV}^2, with three-generation mixing and a ``normal'' neutrino mass hierarchy, can just barely be reconciled with the negative results of other laboratory neutrino oscillation experiments and the positive hints of neutrino oscillation from the solar and atmospheric neutrino problems. Though subject to test by by future experiments, such a solution allows (but does not demand) neutrino masses relevant for dark matter.""]",['1996-06-05'] +2270,['eng'],"['Susperregi, M']",['Spectrum of density fluctuations in Brans-Dicke chaotic inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'Brans-Dicke model', 'density, fluctuation', 'potential', 'regularization', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606018'],"['In the context of Brans--Dicke theories, eternal inflation is described in such a way that the evolution of the inflaton field is determined by the value of the Planck mass in different regions of the universe. The Planck mass is given by the values of the Brans--Dicke field, which is coupled to the scalar curvature in the Lagrangian. We first calculate the joint probability distributions of the inflaton and Brans--Dicke fields, in order to compute the 3--volume ratios of homogeneous regions with arbitrary values of the fields still undergoing inflation with respect to thermalized regions. From these volume ratios one is able to extract information on the values of the fields measured by a typical observer for a given potential and, in particular, the typical value of the Planck mass at the end of inflation. In this paper, we investigate volume ratios using a regularization procedure suggested by Vilenkin, and the results are applied to powerlaw and double--well potentials. The spectrum of density fluctuations is calculated for generic potentials, and we discuss the likelihood of various scenarios that could tell us whether our region of the universe is typical or untypical depending on very general bounds on the evolution of the Brans--Dicke field.']",['1996-06-05'] +2271,['eng'],"['Schaab, C', 'Voskresensky, D N', 'Sedrakian, A D', 'Weber, F', 'Weigel, M K']",['Impact of medium effects on the cooling of non-superfluid and superfluid neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'superfluid', 'matter, density', 'neutrino, emission', 'emission, neutrino', 'matter, mass', 'mass, matter', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605188'],"['Neutrino emission from the dense hadronic component in neutron stars is subject to strong modifications due to collective effects in the nuclear medium. We implement two new neutrino--emission processes operating in the nuclear medium in numerical cooling simulations of neutron stars. The first process is the medium--modified Urca (MMU) process, which takes into account the softening of the pion exchange mode and other polarization effects as well as the neutrino emission arising from the intermediate reaction states in the modified Urca process. The second process concerns neutrino emission through superfluid pair formation and breaking processes. It is found that non--superfluid neutron star models cool mainly via the MMU process, which gives a smooth crossover from the standard to the nonstandard cooling scenario for increasing star masses. For superfluid stars, the superfluid pair formation and breaking processes accelerate mildly both the standard and the nonstandard cooling scenario. This leads to a good agreement between the theoretical cooling tracks and the rather low temperatures observed for objects like PSRs 0833-45 (Vela), 0656+14, and 0630+18 (Geminga). The robustness of our findings against variations in the underlying equation of state of baryonic matter is demonstrated. Hence we conclude that the two new neutrino-emission processes studied here enable one to reproduce theoretically most of the observed pulsar temperatures by varying the masses of neutron star models.']",['1996-06-03'] +2272,['eng'],"['Martin, X', 'Vilenkin, A']",['Gravitational wave background from hybrid topological defects'],['Astrophysics and Astronomy'],"['gravitational radiation, stochastic', 'gravitational radiation, spectra', 'spectra, gravitational radiation', 'topology, defect', 'domain wall', 'string model', 'field equations, monopole', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606022'],"['We investigate the spectrum of stochastic gravitational wave background generated by hybrid topological defects: domain walls bounded by strings and monopoles connected by strings. Such defects typically decay early in the history of the universe, and their mass scale is not subject to the constraints imposed by microwave background and millisecond pulsar observations. Nonetheless, the intensity of the gravitational wave background from hybrid defects can be quite high in the frequency range of LIGO, VIRGO and LISA detectors. For some values of the parameters, this background will be detectable by the first version of LIGO.']",['1996-06-05'] +2273,['eng'],"['Frichter, G M', 'Ralston, J P', 'McKay, D W']",['Toward radio detection of PeV neutrinos on the cubic kilometer scale'],['Astrophysics and Astronomy'],"['talk, Venice 1996/02/27', 'neutrino, cosmic radiation', 'showers, electromagnetic', 'Cherenkov counter, water', 'solids, water', 'photon, counters and detectors', 'efficiency', 'astrophysics, particle source', 'deep underground detector, AMANDA']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606008'],"['Interactions of ultrahigh energy neutrinos of cosmological origin in large volumes of radio-transparent South Polar ice can be detected via coherent Cherenkov emission from accompanying electromagnetic showers. A pilot experiment employing buried radio receivers has been successfully deployed at the South Pole and data are now being collected. The physics of coherent radio emission together with the properties of radio-pulse propagation in Antarctic ice clearly distinguishes the radio method from phototube detection. In the context of the proposed km^3-scale neutrino telescope, these two detection modes provide complementary information on UHE neutrino interactions.']",['1996-06-04'] +2274,['eng'],"['Ralston, J P', 'McKay, D W', 'Frichter, G M']",['The ultra high energy neutrino-nucleon cross section'],['Astrophysics and Astronomy'],"['talk, Venice 1996/02/27', 'neutrino nucleon, interaction', 'interaction, neutrino nucleon', 'total cross section, high energy behavior', 'high energy behavior, total cross section', 'quantum chromodynamics, effect', 'differential cross section', 'nucleon, structure function', 'electron p, deep inelastic scattering', 'deep inelastic scattering, electron p', 'momentum spectrum, parton', 'new interaction, search for', 'search for, new interaction']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9606007'],"[""The ultra-high energy neutrino nucleon cross section grows at a surprising rate with energy due to QCD effects in the target. Recent electroproduction data allows an update of earlier predictions. We compare the results of our own calculations with those of other groups, and critically review the foundation and reliability of the calculations. The question of the `new physics' potential of neutrino telescopes sensitive to the total cross section in multi-PeV energy domain is considered. We point out a loophole in the arguments which might be an important consideration in extrapolating the cross section to extremely high energies.""]",['1996-06-04'] +2275,['eng'],"['Vilenkin, A', 'Winitzki, S']",['Probability distribution for $\\Omega$ in open-universe inflation'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'matter, density', 'geometry, bubble', 'statistics', 'regularization', 'space-time, Robertson-Walker', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605191'],"[""The problem of making predictions in eternally inflating universe that thermalizes by bubble nucleation is considered. A recently introduced regularization procedure is applied to find the probability distribution for the ensemble of thermalized bubbles. The resulting probabilities are shown to be independent of the choice of the time parametrization. This formalism is applied to models of open ``hybrid'' inflation with \\Omega <1. Depending on the parameters of the model, the probability distribution for \\Omega is found to have a peak either very close to \\Omega =1, or at an intermediate value of \\Omega in the range 0.03\\lesssim \\Omega <1.""]",['1996-06-03'] +2276,['eng'],['Ma Chung Pei'],['Linear power spectra in cold+hot dark matter models'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'spectra, linear', 'linear, spectra', 'neutrino, massive', 'massive, neutrino', 'mass, fluctuation', 'fluctuation, mass', 'cluster', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605198'],"['This paper presents simple analytic approximations to the linear power spectra, linear growth rates, and rms mass fluctuations for both components in a family of cold+hot dark matter (CDM+HDM) models that are of current cosmological interest. The formulas are valid for a wide range of wavenumber, neutrino fraction, redshift, and Hubble constant: k\\lo 10\\,h Mpc^{-1}, 0.05\\lo \\onu\\lo 0.3, 0\\le z\\lo 15, and 0.5\\lo h \\lo 0.8. A new, redshift-dependent shape parameter \\Gamma_\\nu=a^{1/2}\\onu h^2 is introduced to simplify the multi-dimensional parameter space and to characterize the effect of massive neutrinos on the power spectrum. The physical origin of \\Gamma_\\nu lies in the neutrino free-streaming process, and the analytic approximations can be simplified to depend only on this variable and \\onu. Linear calculations with these power spectra as input are performed to compare the predictions of \\onu\\lo 0.3 models with observational constraints from the reconstructed linear power spectrum and cluster abundance. The usual assumption of an exact scale-invariant primordial power spectrum is relaxed to allow a spectral index of 0.8\\lo n\\le 1. It is found that a slight tilt of n=0.9 (no tensor mode) or n=0.95 (with tensor mode) in \\onu\\sim 0.1-0.2 CDM+HDM models gives a power spectrum similar to that of an open CDM model with a shape parameter \\Gamma=0.25, providing good agreement with the power spectrum reconstructed by Peacock and Dodds (1994) and the observed cluster abundance.']",['1996-06-03'] +2277,['eng'],"['Bonazzola, S', 'Gourgoulhon, E']",['Gravitational waves from neutron stars'],['Astrophysics and Astronomy'],"['lectures, Les Houches 1995/09/26', 'gravitational radiation', 'n, matter', 'symmetry, spontaneously broken', 'potential', 'astrophysics, pulsar', 'magnetic field', 'relativity theory, general', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605187'],['Contents: 1. Introduction 2. Spontaneous symmetry breaking 2.1 Review of classical results about Maclaurin/Jacobi ellipsoids 2.2 Spontaneous breaking of symmetry: a general phenomenom 2.3 Previous results for compressible Newtonian stars 2.4 Generation of gravitational waves 2.5 Finding the equilibrium configurations of a rotating star in the Newtonian regime 2.6 Extension to general relativity 2.7 First integral of fluid motion in general relativity 2.8 Gravitational field equations 2.9 Numerical results 3. CW emission from pulsars 4. Discussion and conclusion Appendix: Relativistic hydrodynamics in an accelerated frame'],['1996-06-03'] +2278,['eng'],"['Hu, W', 'Spergel, D N', 'White, M']",['Distinguishing causal seeds from inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'conservation law, energy-momentum', 'tensor, perturbation', 'scaling', 'gravitation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605193'],"['Causal seed models, such as cosmological defects, generically predict a distinctly different structure to the CMB power spectrum than inflation, due to the behavior of the perturbations outside the horizon. We provide a general analysis of their causal generation from isocurvature initial conditions by analyzing the role of stress perturbations and conservation laws in the causal evolution. As a special case, we consider the class of scaling models recently proposed by Turok. Energy-momentum conservation implies pathologies in the gravitational sector for this class unless the anisotropic stresses are tuned to avoid them. We propose and motivate a simpler cure for the pathologies that illustrates why such models tend to follow the canonical isocurvature pattern. Thus they can easily be distinguished from inflation by CMB experiments currently underway.']",['1996-06-03'] +2279,['eng'],"['Brockway, J W', 'Carlson, E D', 'Raffelt, G G']",['SN 1987A $\\gamma$-ray limits on the conversion of pseudoscalars'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'pseudoscalar particle, production', 'production, pseudoscalar particle', 'photon, cosmic radiation', 'magnetic field, galaxy', 'photon, flux', 'flux, photon', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605197'],"['Pseudoscalar particles \\phi usually couple electromagnetically by an interaction of the form \\frc14 g \\phi F {\\widetilde F}, allowing them to convert to photons in the presence of magnetic fields. Notably, new low-mass pseudoscalars emitted from supernova (SN) 1987A would have been converted to \\gamma-rays in the intervening magnetic field of the galaxy. Therefore, measurements by the Solar Maximum Mission (SMM) Gamma-Ray Spectrometer (GRS) can limit the inverse coupling constant to g^{-1}>1{\\times}10^{11}\\,\\rm GeV, assuming the pseudoscalar is massless. This is an improvement over other astrophysical limits of a factor of about 2.5.']",['1996-06-03'] +2280,['eng'],"['Samurovic, S', 'Celebonovic, V']",['Massive neutrinos and the problem of the dark matter in spiral galaxies'],['Astrophysics and Astronomy'],"['talk, Belgrade 1996/10/09', 'astrophysics, galaxy', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, mass', 'mass, neutrino', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605174'],['Using data on rotation curves of 134 spiral galaxies we have calculated the possible value of the tau neutrino mass. We have shown that this mass could explain the nature of the dark matter in spiral galaxies.'],['1996-05-29'] +2281,['eng'],"['Capozziello, S', 'De Ritis, R', 'Marino, A A']",['A time-dependent cosmological constant phenomenology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, fundamental constant', 'time dependence', 'energy, density', 'matter', 'radiation', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605176'],"[""We construct a cosmological toy model in which a step-function ``cosmological constant'' is taken into consideration beside ordinary matter. We assume that \\Lambda takes two values depending on the epoch, and matter goes from a radiation dominated era to a dust dominated era. The model is exactly solvable and it can be compared with recent observations.""]",['1996-05-30'] +2282,['eng'],"['Bernlöhr, K']",['Measuring the UHE cosmic-ray composition with tracking detectors in air shower arrays'],['Astrophysics and Astronomy'],"['showers, air', 'muon, cosmic radiation', 'electron, cosmic radiation', 'angular distribution', 'particle identification, (muon electron)', 'counters and detectors, proposed', 'numerical calculations, Monte Carlo', '10**6 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605177'],"['Measuring the angles of muons and electrons in air showers is proposed as a method for studying the primary cosmic-ray mass composition near the knee of the cosmic-ray energy spectrum at a few 10^{15} eV. Conventional tracking detectors at existing air shower arrays could serve this purpose, like the CRT detectors at the HEGRA array. When the average radial muon angles are examined as a function of shower core distance, the experimental resolution can be very well calibrated from the tangential angle distribution. The method is particularly promising for measuring changes in the average mass number of the primary cosmic rays with energy. The method is described and experimental and theoretical constraints are discussed.']",['1996-05-30'] +2283,['eng'],"['De Laix, A A', 'Vachaspati, T']",['Gravitational lensing by cosmic string loops'],['Astrophysics and Astronomy'],"['astrophysics, string', 'photon, cosmic radiation', 'approximation, weak field', 'gravitation, lens', 'perturbation theory, higher-order', 'grand unified theory', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605171'],"[""We calculate the deflection of a light ray caused by the gravitational field of a cosmic string loop in the weak field limit and reduce the problem to a single quadrature over a time slice of the loop's world sheet. We then apply this formalism to the problem of gravitational lensing by cosmic string loops. In particular, we find an analytic solution for the special case of a circular loop perpendicular to the optical axis. As examples of more complicated loops, we consider two loops with higher frequency Fourier modes. The numerical analysis illustrates the general features of loop lenses. Our estimates, using typical parameters for GUT scale loops, show that the stringy nature of loop lenses can be observed for lensing systems involving high redshift galaxies (z \\sim 2), and we suggest that gravitational lensing can confirm the existence of GUT scale strings if they are the seeds for large scale structure formation.""]",['1996-05-29'] +2284,['eng'],"['Fargion, D', 'Salis, A']",['Inverse Compton scattering onto BBR in high energy physics and $\\gamma$ (MeV-TeV) astrophysics'],['Astrophysics and Astronomy'],"['Compton scattering, inverse', 'inverse, Compton scattering', 'astrophysics', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'photon, flux', 'flux, photon', 'energy spectrum, cosmic radiation', 'cosmic radiation, energy spectrum', 'RF system', 'energy spectrum, (photon)', '(photon), energy spectrum', 'temperature', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605168'],"['We considered the Inverse Compton Scattering (ICS) of charged particles onto photons whose distribution is a Black Body Radiation (BBR) deriving the exact energy and angular differential distribution in the general case and in its most useful expansions. These results can be successfully applied in high energy accelerators experiments to evaluate the ICS contribution from the thermal photons in the cavity as well as in astrophysics where the ICS of cosmic rays plays a relevant role in a variety of phenomena. In particular we show how our formulae reproduce the ICS energy spectrum recently measured at LEP, how it could be considered a key tool in explaining the Gamma Ray Bursts (GRB) , SGRs energy spectrum. Finally we predicted the presence of a low gamma flux, nearly detectable at hundred of TeV from SNRs SN1006 as well as, at lower energy (tens TeV, due to gamma ray cascading in cosmic BBR), from relic extragalactic highest cosmic rays sources born by jets in AGN,as blazars 3C279,Mrk421,Mrk 501.']",['1996-05-29'] +2285,['eng'],"['Protheroe, R J', 'Biermann, P L']",['A new estimate of the extragalactic radio background and implications for ultra-high-energy gamma-ray propagation'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'microwaves, background', 'astrophysics, model', 'photon, cosmic radiation', 'photon photon, interaction', 'interaction, photon photon', 'pair production', 'synchrotron radiation', 'magnetic field', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605119'],"['We make a new estimate of the extragalactic radio background down to kHz frequencies based on the observed luminosity functions and radio spectra of normal galaxies and radio galaxies. We have constructed models for the spectra of these two classes of objects down to low frequencies based on observations of our Galaxy, other normal galaxies and radio galaxies. We check that the models and evolution of the luminosity functions give source counts consistent with data and calculate the radio background expected from kHz to GHz frequencies. The motivation for this calculation is that the propagation of ultra-high energy gamma-rays in the universe is limited by photon-photon pair production on the radio background. Electromagnetic cascades involving photon-photon pair production and subsequent synchrotron radiation in the intergalactic magnetic field may develop. Such gamma-rays may be produced in acceleration sites of ultra-high energy cosmic rays, as a result of interactions with the microwave background, or emitted as a result of decay or annihilation of topological defects. We find that photon-photon pair production on the radio background remains the dominant attenuation process for gamma-rays from 3 \\times 10^{10} GeV up to GUT scale energies.']",['1996-05-21'] +2286,['eng'],"['Boratav, M']",['Extremely high energy cosmic rays and the Auger observatory'],['Astrophysics and Astronomy'],"['talk', 'cosmic radiation', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605087'],"['Over the last 30 years or so, a handful of events observed in ground-based cosmic ray detectors seem to have opened a new window in the field of high-energy astrophysics. These events have energies exceeding 5x10**19 eV (the region of the so-called Greisen-Zatsepin-Kuzmin spectral cutoff); they seem to come from no known astrophysical source; their chemical composition is mostly unknown; no conventional accelerating mechanism is considered as being able to explain their production and propagation to earth. Only a dedicated detector can bring in the high-quality and statistically significant data needed to solve this long-lasting puzzle: this is the aim of the Auger Observatory project around which a world-wide collaboration is being mobilized.']",['1996-05-16'] +2287,['eng'],"['Kofman, L A']",['The origin of matter in the universe'],['Astrophysics and Astronomy'],"['talk, Copenhagen 1996/01/10', 'inflationary universe', 'critical phenomena', 'baryon, production', 'production, baryon', 'field theory, scalar', 'field theory, oscillation', 'background, time dependence', 'effect, back reaction', 'resonance']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605155'],"['In the inflationary scenario all the matter constituting the universe was created from the process of reheating after inflation. Recent development of the theory of reheating is briefly reviewed. The list of topics includes elementary (perturbative) theory of reheating; quantum field theory in a time-varying background; parametric resonance and explosive particle creation; non-thermal phase transitions from reheating; baryogenesis from reheating; residual oscillations of the scalar field, and other cosmological applications.']",['1996-05-27'] +2288,['eng'],"['Weiler, Thomas J', 'Kephart, T W']",['Are we seeing magnetic monopole cosmic rays at E $>$ 10$^{20}$ eV?'],['Astrophysics and Astronomy'],"['talk, Santa Monica 1996/02/14', 'cosmic radiation, primary', 'relativistic', 'magnetic monopole, mass', 'cosmic radiation, flux', 'cosmic radiation, acceleration', 'magnetic field, galaxy', 'showers, air', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605156'],"['We suggest that the highest energy \\gsim 10^{20} eV cosmic ray primaries may be relativistic magnetic monopoles. Motivations for this hypothesis are twofold: (i) conventional primaries are problematic, while monopoles are naturally accelerated to E \\sim 10^{20} eV by galactic magnetic fields; (ii) the observed highest energy cosmic ray flux is just below the Parker limit for monopoles. By matching the cosmic monopole production mechanism to the observed highest energy cosmic ray flux we estimate the monopole mass to be \\lsim 10^{10} GeV.']",['1996-05-27'] +2289,['eng'],"['Sigl, G', 'Schramm, David N', 'Lee, S', 'Coppi, P S', 'Hill, Christopher T']",['Implications of a possible clustering of highest energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, cluster', 'astrophysics, model', 'magnetic field', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605158'],"['Very recently, a possible clustering of a subset of observed ultrahigh energy cosmic rays above about 40EeV (4x10^19eV) in pairs near the supergalactic plane was reported. We show that a confirmation of this effect would provide information on origin and nature of these events and, in case of charged primaries, imply interesting constraints on the extragalactic magnetic field. The observed time correlation would most likely rule out an association of these events with cosmological gamma ray bursts. If no prominent astrophysical source candidates such as powerful radiogalaxies can be found, the existence of a mechanism involving new fundamental physics would be favored.']",['1996-05-27'] +2290,['eng'],"['Ricci, B']","['Solar opacity, neutrino signals and helioseismology']",['Astrophysics and Astronomy'],"['neutrino, solar', 'model, solar', 'helium, diffusion', 'neutrino, flux', 'flux, neutrino', 'effect, opacity', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605153'],"['In connection with the recent suggestion by Tsytovich et al. that opacity in the solar core could be overestimated, we consider the following questions: i) What would a 10\\% opacity reduction imply for the solar neutrino puzzle? ii) Is there any hope of solving the solar neutrino puzzle by changing opacity? iii) Is a 10\\% opacity reduction testable with helioseismological data?']",['1996-05-27'] +2291,['eng'],"['Jedamzik, K']",['Primordial black hole formation during the QCD epoch'],['Astrophysics and Astronomy'],"['black hole, production', 'production, black hole', 'critical phenomena', 'density, fluctuation', 'quantum chromodynamics', 'black hole, mass', 'mass, black hole']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605152', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=capp98&id=jedamzik']","[""We consider the formation of horizon-size primordial black holes (PBH's) from pre-existing density fluctuations during cosmic phase transitions. It is pointed out that the formation of PBH's should be particularly efficient during the QCD epoch due to a significant decrease of the effective speed of sound during the color-confinement transition. Our considerations imply that for generic initial density perturbation spectra PBH mass functions are expected to exhibit a peak on the QCD-horizon mass scale \\sim 1 M_{\\odot}. This mass scale is roughly coincident with the estimated masses for compact objects recently observed in our galactic halo by the MACHO collaboration. Black holes formed during the QCD epoch may offer an attractive explanation for the origin of halo dark matter evading possibly problematic nucleosynthesis and luminosity bounds on baryonic halo dark matter.""]",['1996-05-27'] +2292,['eng'],"['Ciacio, F', ""Degl'Innocenti, S"", 'Ricci, B']",['Updating standard solar models'],['Astrophysics and Astronomy'],"['model, solar', 'helium, diffusion', 'neutrino, production', 'production, neutrino', 'neutrino, flux', 'flux, neutrino', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605157'],"['We present an updated version of our standard solar model (SSM) where helium and heavy elements diffusion is included and the improved OPAL equation of state (Rogers 1994, Rogers Swenson \\& Iglesias 1996) is used. In such a way the EOS is consistent with the adopted opacity tables, from the same Livermore group, an occurrence which should further enhance the reliability of the model. The results for the physical characteristics and the neutrino production of our SSM are discussed and compared with previous works on the matter.']",['1996-05-27'] +2293,['eng'],"['Haensel, P']",['Solid interiors of neutron stars and gravitational radiation'],['Astrophysics and Astronomy'],"['lectures, Les Houches 1995/09/26', 'n, matter', 'matter, production', 'production, matter', 'nuclear matter, density', 'topology', 'solids', 'liquid', 'matter, deformation', 'matter, energy', 'gravitational radiation', 'astrophysics, pulsar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605164'],"['Contents: 1.Introduction 2. Formation and composition of the solid crust 3. The bottom layers of the crust: exotic nuclear shapes and topologies 4. Crust contribution to stellar mass and moment of inertia 5. Solid cores 6. Deformation, elastic strain and mountains 7. Shape and energy of rotating, partially solid neutron star 8. Oblateness and precession 9. Gravitational radiation from precessing pulsars 10. Gravitational radiation from precessing pulsars and pulsar timing 11. Detectability']",['1996-05-28'] +2294,['eng'],"['Gourgoulhon, E', 'Bonazzola, S']",['Gravitational waves from isolated neutron stars'],['Astrophysics and Astronomy'],"['talk, Pisa 1996/03/19', 'gravitational radiation', 'n, matter', 'amplitude analysis', 'magnetic field, effect', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605150'],['Continuous wave gravitational radiation from isolated rotating neutron stars is discussed. The general waveform and orders of magnitude for the amplitude are presented for various known pulsars. The specific case of gravitational radiation resulting from the distortion induced by the stellar magnetic field is presented. Finally some preliminary results about the signal from the whole population of neutron stars in the Galaxy are discussed.'],['1996-05-27'] +2295,['eng'],"['Wang, Y', 'Stebbins, A J', 'Turner, E L']",['Gravitational lensing of gravitational waves from merging neutron star binaries'],['Astrophysics and Astronomy'],"['gravitational radiation', 'gravitation, lens', 'n, matter', 'counters and detectors', 'interference, laser', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605140'],"['We discuss the gravitational lensing of gravitational waves from merging neutron star binaries, in the context of advanced LIGO type gravitational wave detectors. We consider properties of the expected observational data with cut on the signal-to-noise ratio \\rho, i.e., \\rho>\\rho_0. An advanced LIGO should see unlensed inspiral events with a redshift distribution with cut-off at a redshift z_{\\rm max} < 1 for h \\leq 0.8. Any inspiral events detected at z>z_{\\rm max} should be lensed. We compute the expected total number of events which are present due to gravitational lensing and their redshift distribution for an advanced LIGO in a flat Universe. If the matter fraction in compact lenses is close to 10\\%, an advanced LIGO should see a few strongly lensed events per year with \\rho >5.']",['1996-05-23'] +2296,['eng'],"['Cohn, J D']",['Open universes from finite radius bubbles'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'vacuum state, bubble', 'space-time, de Sitter', 'vacuum state, fluctuation', 'tunneling', 'field theory, scalar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605132'],"['The interior of a vacuum bubble in de Sitter space may give an open universe with sufficient homogeneity to agree with observations. Here, previous work by Bucher, Goldhaber and Turok is extended to describe a thin bubble wall with nonzero radius and energy difference across the wall. The vacuum modes present before formation of the bubble propagate into the interior of the open universe and the power spectrum of the resulting gauge invariant gravitational potential is calculated. It appears to become scale invariant on small scales, with onset at about the same scale as that found in the zero radius case. There is sensitivity to the radius and energy difference at large scales, but it is expected that they cannot be strongly constrained because of cosmic variance. As the prediction of a scale invariant spectrum seems to be robust with respect to variation of these parameters at small scales, it apparently is a generic feature of the contribution of these modes for these thin wall models.']",['1996-05-22'] +2297,['eng'],"['Mannheim, K', 'Hartmann, D', 'Funk, B']",['The $\\gamma$ ray burst rate at high photon energies'],['Astrophysics and Astronomy'],"['astrophysics, model', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'horizon', 'photon, absorption', 'absorption, photon', 'photon photon, exclusive reaction', 'electron, pair production', 'pair production, electron', 'radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605108'],"['Some gamma-ray burst (GRB) spectra exhibit high energy tails with the highest photon energy detected at 18 GeV. The spectral slope of the high-energy tails is sufficiently flat in nu F_nu to consider the possibility of their detection at still higher energies. We calculate how many bursts can reasonably be expected above a given energy threshold for a cosmological distribution of bursts satisfying the observed apparent brightness distribution. The crucial point is that the gamma-ray absorption by pair production in the intergalactic diffuse radiation field eliminates bursts from beyond the gamma-ray horizon tau ~ 1, thus drastically reducing the number of bursts at high energies. Our results are consistent with the non-detection of bursts by current experiments in the 100 GeV to 100 TeV energy range. For the earth-bound detector array MILAGRO, we predict a maximal GRB rate of ~ 10 events per year. The Whipple Observatory can detect, under favorable conditions, ~1 event per year. The event rate for the HEGRA array is ~ 0.01 per year. Detection of significantly higher rates of bursts would severely challenge cosmological burst scenarios.']",['1996-05-20'] +2298,['eng'],"['Davidson, S']",['Ingredients and equations for making a magnetic field in the early universe'],['Astrophysics and Astronomy'],"['astrophysics', 'magnetic field, coherence', 'baryon, asymmetry', 'critical phenomena', 'Maxwell equation', 'symmetry breaking', 'Higgs model']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605086'],"[""The ingredients required to create a magnetic field in the early Universe are identified, and compared with Sakharov's conditions for baryogenesis. It is also shown that a long range coherent magnetic field is not generated by the classical rolling Higgs vacuum expectation value during the electroweak phase transition.""]",['1996-05-16'] +2299,['eng'],"['Mannheim, K', 'Westerhoff, S', 'Meyer, H', 'Fink, H H']",['Beacons at the $\\gamma$ ray horizon'],['Astrophysics and Astronomy'],"['astrophysics', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'horizon', 'model, cascade', 'synchrotron radiation', 'counters and detectors', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605107'],"['Blazars with redshifts z<0.1 are likely candidates for detection at energies in the range 300 GeV - 50 TeV with Cerenkov telescopes and scintillator arrays. We present gamma-ray flux predictions for a sample of 15 nearby flat-spectrum radio sources fitting the proton blazar model of Mannheim (1993a) to their observed broad-band spectral energy distributions. At high energies, we use fluxes or flux limits measured by ROSAT, CGRO and the Whipple Observatory to constrain their spectra. We take into account absorption of the gamma-rays by pair production with low energy photons of the diffuse infrared-to-optical photon background produced by galaxies (cosmic absorption) and with low energy synchrotron photons of the blazar radiation field (internal absorption). Typically, the theoretical spectra decrease much faster above TeV (photon index s~3) than between GeV and TeV (s~2) owing to internal absorption. The predicted fluxes are confronted with flux limits in the 20-50 TeV energy range obtained by the High Energy Gamma Ray Astronomy (HEGRA) experiment. Without cosmic absorption, the fluxes are about equal to the current sensitivity of HEGRA. Improved gamma/hadron separation techniques could render a detection by HEGRA possible, if cosmic absorption by the far-infrared background at wavelengths ~100 mu is not exceedingly strong.']",['1996-05-20'] +2300,['eng'],"['García-Bellido, J', 'Linde, Andrei D', 'Wands, D']",['Density perturbations and black hole formation in hybrid inflation'],['Astrophysics and Astronomy'],"['inflationary universe, hybrid', 'critical phenomena', 'field theory, fluctuation', 'density, perturbation', 'black hole, production', 'production, black hole', 'topology, defect', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605094'],"['We investigate the recently proposed hybrid inflation models with two stages of inflation. In order to study density perturbations in these models we develop a new method to calculate density perturbations in a system of two scalar fields. We show that density perturbations in hybrid inflation models of the new type can be very large on the scale corresponding to the phase transition between the two inflationary stages. Moreover, quantum fluctuations at that time can trigger the formation of a large number of inflating topological defects. The resulting density inhomogeneities lead to a copious production of black holes. This could be an argument against hybrid inflation models with two stages of inflation. However, we find a class of models where this problem can be easily avoided. The number of black holes produced in these models typically is very small, but in general it could be made sufficiently large to have interesting cosmological and astrophysical implications. It may be even more interesting to have hybrid models with two stages of inflation where the black hole production is not suppressed, but the typical masses of the black holes are very small. Such models lead to a completely different thermal history of the universe, where post-inflationary reheating occurs via black hole evaporation.']",['1996-05-16'] +2301,['eng'],"['Yamammoto, K', 'Sasaki, M', 'Tanaka, T']",['Quantum fluctuations and CMB anisotropies in one-bubble open inflation models'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'bubble, production', 'production, bubble', 'model, fluctuation', 'field theory, scalar', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, perturbation', 'perturbation, spectra', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605103'],"[""We first develop a method to calculate a complete set of mode functions which describe the quantum fluctuations generated in one-bubble open inflation models. We consider two classes of models. One is a single scalar field model proposed by Bucher, Goldhaber and Turok and by us as an example of the open inflation scinario, and the other is a two-field model such as the ``supernatural'' inflation proposed by Linde and Mezhlumian. In both cases we assume the difference in the vacuum energy density between inside and outside the bubble is negligible. There are two kinds of mode functions. One kind has usual continuous spectrum and the other has discrete spectrum with characteristic wavelengths exceeding the spatial curvature scale. The latter can be further devided into two classes in terms of its origin. One is called the de Sitter super-curvature mode, which arises due to the global spacetime structure of de Sitter space, and the other is due to fluctuations of the bubble wall. We calculate the spectrum of quantum fluctuations in these models and evaluate the resulting large angular scale CMB anisotropies. We find there are ranges of model parameters that are consistent with observed CMB anisotropies.""]",['1996-05-20'] +2302,['eng'],"['Sasaki, M', 'Tanaka, T']",['Can the simplest two-field model of open inflation survive?'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'field theory, inflaton', 'model, fluctuation', 'vacuum state']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605104'],"['We investigate the quantum fluctuations of an inflaton field in a two-field model of one-bubble open inflation. One of the inflatons is assumed to be responsible for the first false vacuum stage of inflation and the other is assumed to be responsible for the second slow-roll stage of inflation. The mass of the second inflaton is assumed to be negligible throughout the whole era of inflation. We find the super-curvature fluctuations are enhanced by the factor given by the ratio of the Hubble constants at false vacuum and true vacuum. This gives a strong constraint on a class of open inflation models. In particular, this implies the simplest two-field model proposed by Linde and Mezhlumian is in trouble.']",['1996-05-20'] +2303,['eng'],"['Capozziello, S', 'De Ritis, R']","['A time-dependent cosmological ""constant""']",['Astrophysics and Astronomy'],"['gravitation', 'field theory, scalar', 'coupling, matter', 'matter, coupling', 'quantum number', 'astrophysics, fundamental constant', 'Einstein equation, solution', 'asymptotic behavior']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605070'],"['We extend the Wald cosmic no-hair theorem to a general class of scalar-tensor nonminimally coupled theories of gravity where ordinary matter is also present in the form of a perfect fluid. We give a set of conditions for obtaining a de Sitter expansion independently of any initial conditions, generalizing the treatment of such a problem as given by Wald. Finally we apply the results to some specific models.']",['1996-05-15'] +2304,['eng'],"['Marleau, F R', 'Starkman, G D']",['The universe as a diffusive medium'],['Astrophysics and Astronomy'],"['gravitational radiation, background', 'gravitational radiation, measurement', 'energy, density', 'scattering, photon graviton', 'photon graviton, scattering', 'random walk', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605066'],"[""We calculate the ``seeing'' effect on distant sources due to a gravitational wave background. We derive the limit in strain and energy density of the gravitational wave based on the limit of detectability of this effect with the present day telescope resolution. We also compare our detection limit to those obtained from existing methods.""]",['1996-05-14'] +2305,['eng'],"['Olive, Keith A']",['Why do we need non-baryonic dark matter?'],['Astrophysics and Astronomy'],"['talk, Les Arcs 1996/01/20', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, model', 'light nucleus, density', 'postulated particle, LSP', 'density, LSP', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605068'],['Observational evidence along with theoretical arguments which call for non-baryonic dark matter are reviewed. A brief summary of the dark matter session is included.'],['1996-05-14'] +2306,['eng'],"['Birkel, M', 'Sarkar, S']","['Nucleosynthesis bounds on a time-varying cosmological ""constant""']",['Astrophysics and Astronomy'],"['astrophysics, fundamental constant', 'fundamental constant, time variation', 'light nucleus, production', 'vacuum state, decay', 'vacuum state, energy', 'neutrino, temperature', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605055'],['We constrain proposed phenomenological models for a vacuum energy which decays with the expansion of the universe from considerations of standard big bang nucleosynthesis. Several models which are simple enough to be physically appealing are ruled out.'],['1996-05-13'] +2307,['eng'],"['Magueijo, J', 'Albrecht, Andreas', 'Ferreira, P', 'Coulson, D']",['The structure of Doppler peaks induced by active perturbations'],['Astrophysics and Astronomy'],"['cosmic radiation, anisotropy', 'inflationary universe', 'topology, defect', 'astrophysics, string', 'causality', 'scaling', 'perturbation', 'coherence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9605047'],"[""We investigate how the qualitative structure of Doppler peaks in the angular power spectrum of the cosmic microwave anisotropy is affected by basic assumptions going into theories of structure formation. We define the concepts of ``coherent'' and ``incoherent'' fluctuations, and also of ``active'' and ``passive'' fluctuations. In these terms inflationary fluctuations are passive and coherent while topological defects are active incoherent fluctuations. Causality and scale invariance are shown to have different implementations in theories differing in the above senses. We then extend the formalism of Hu and Sugiyama to treat models with cosmic defects. Using this formalism we show that the existence or absence of secondary Doppler peaks and the rough placing of the primary peak are very sensitive to the fundamental properties defined. We claim therefore that even a rough measurement of the angular power spectrum C_l shape at 100$10$^{19}$eV cosmic ray sources and large scale structure'],['Astrophysics and Astronomy'],"['astrophysics, model', 'cosmic radiation, particle source', 'cosmic radiation, angular distribution', 'cosmic radiation, anisotropy', 'galaxy', 'cosmic radiation, flux', 'cosmic radiation, energy spectrum', 'proposed experiment', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9604005'],"['We analyze the anisotropy signature expected if the high energy (above 10^{19}eV) cosmic ray (CR) sources are extra-Galactic and trace the distribution of luminous matter on large scales. We investigate the dependence of the anisotropy on both the relative bias between the CR sources and the galaxy distribution and on the (unknown) intrinsic CR source density. We find that the expected anisotropy associated with the large scale structure (LSS) should be detected once the number of CR events observed above 10^{19}{\\rm eV} is increased by a factor of \\sim10. This would require \\sim30 observation-years with existing experiments, but less then 1 year with the proposed \\sim5000\\ {\\rm km}^2 Auger detectors. We find that the recently reported concentration of the Haverah Park CR events towards the super-galactic plane is not consistent with the known LSS. If real, the Haverah Park result suggests that the CR sources are much more concentrated towards the super-galactic plane than the known LSS. Our results are not sensitive to the number density of CR sources. We show that once the number of detected events is increased by a factor of \\sim10, the number density would be strongly constrained by considering the probability for having repeating sources.']",['1996-04-02'] +2330,['eng'],"['Green, A M', 'Liddle, A R']",['Conditions for successful extended inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'critical phenomena', 'gravitation, coupling', 'coupling, gravitation', 'spectra, perturbation', 'perturbation, spectra']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9604001'],"[""We investigate, in a model-independent way, the conditions required to obtain a satisfactory model of extended inflation in which inflation is brought to an end by a first-order phase transition. The constraints are that the correct present strength of the gravitational coupling is obtained, that the present theory of gravity is satisfactorily close to general relativity, that the perturbation spectra from inflation are compatible with large scale structure observations and that the bubble spectrum produced at the phase transition doesn't conflict with the observed level of microwave background anisotropies. We demonstrate that these constraints can be summarized in terms of the behaviour in the conformally related Einstein frame, and can be compactly illustrated graphically. We confirm the failure of existing models including the original extended inflation model, and construct models, albeit rather contrived ones, which satisfy all existing constraints.""]",['1996-04-02'] +2331,['eng'],"['Starkman, G D', 'Vachaspati, T']",['Galactic cosmic strings as sources of primary antiprotons'],['Astrophysics and Astronomy'],"['astrophysics, string', 'superconducting, string', 'string, superconducting', 'plasma, galaxy', 'anti-p, cosmic radiation', 'anti-p, flux', 'flux, anti-p', 'anti-p, energy spectrum', 'energy spectrum, anti-p', 'baryon number, violation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9604007'],['A possible signature of a class of superconducting cosmic strings trapped in the Milky Way plasma is the emission of low energy antiprotons due to baryon number violating processes on the string. We find the terrestrial flux and the energy spectrum of such antiprotons. Current observational bounds on the flux of low energy antiprotons place a {\\it lower} bound on the string tension which is comparable to that given by the electroweak scale.'],['1996-04-02'] +2332,['eng'],"['Lee, S']",['On the propagation of extragalactic high energy cosmic and $\\gamma$-rays'],['Astrophysics and Astronomy'],"['astrophysics', 'cosmic radiation, primary', 'showers, air', 'nucleon, cosmic radiation', 'photon, cosmic radiation', 'electron, cosmic radiation', 'background, radiation', 'magnetic field', 'transport theory', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'flux, cosmic radiation', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9604098'],"['The origin and nature of ultrahigh energy cosmic rays with energies above 10^{20}\\,eV is a puzzle for the physics and astrophysics of cosmic rays which is still unresolved. In this paper, I report on an extensive study on the propagation of extragalactic nucleons, \\gamma-rays, and electrons in the energy range between 10^8\\,eV and 10^{23}\\,eV. I have devised an efficient numerical method to solve the transport equations for cosmic ray spectral evolution. The universal radiation background spectrum in the energy range between \\simeq 10^{9}\\,eV and \\simeq 1\\,eV is considered in the numerical code, including the diffuse radio background, the cosmic microwave background, and the infrared/optical background, as well as a possible extragalactic magnetic field. I apply the code to compute the particle spectra predicted by various models of ultrahigh energy cosmic ray origin. A comparison with the observed fluxes, especially the diffuse \\gamma-ray background in several energy ranges, allows one to constrain certain classes of models. I conclude that scenarios which attribute the highest energy cosmic rays to Grand Unification Scale physics or to cosmological Gamma Ray Bursts are viable at the present time.']",['1996-04-18'] +2333,['eng'],"['Waxman, E', 'Coppi, P S']",['Delayed GeV-TeV photons from gamma-ray bursts producing high-energy cosmic rays'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'effect, magnetic field', 'cosmic radiation, time delay', 'cosmic radiation, secondary radiation', 'cosmic radiation, background', 'numerical calculations', '> 10**11 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603144'],"[""A scenario in which cosmic rays (CRs) above 10^{20}{\\rm eV} are produced by cosmological gamma-ray bursts (GRBs) is consistent with observations provided that deflections by the inter-galactic magnetic field (IGMF) delay and spread the arrival time of the CRs over \\geq50{\\rm yr}. The energy lost by the CRs as they propagate and interact with the microwave background is transformed by cascading into secondary GeV-TeV photons. We show that a significant fraction of these photons can arrive with delays much smaller than the CR delay if much of inter-galactic space is occupied by large-scale magnetic ``voids'', regions of size \\gtrsim5{\\rm Mpc} and field weaker than 10^{-15}{\\rm G}. Such voids might be expected, for example, in models where a weak primordial field is amplified in shocked, turbulent regions of the intergalactic medium during the formation of large-scale structure. For a field strength \\sim4\\times10^{-11}{\\rm G} in the high field regions, the value required to account for observed galactic fields if the IGMF were frozen in the protogalactic plasma the delay of CRs produced by a burst at a distance of 100{\\rm Mpc} is \\sim100{\\rm yr}, and the fluence of secondary photons above 10{\\rm GeV} on hour--day time scales is I(>E)\\sim10^{-6}E_{\\rm TeV}^{-1}{\\rm cm}^{-2}. This fluence is close to the detection threshold of current high-energy \\gamma-ray experiments. Detection of the delayed flux would support the GRB-CR association and would also provide information on the IGMF structure.""]",['1996-03-28'] +2334,['eng'],"['Ma, F', 'Xie, B H']",['Super-giant glitches and quark stars'],['Astrophysics and Astronomy'],"['astrophysics, model', 'n, matter', 'critical phenomena', 'quark, matter', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'gravitational radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603134'],"['When a spinning-down neutron star undergoes a phase transition that produces quark matter in its core, a Super-Giant Glitch of the order {\\Delta} \\Omega/\\Omega\\sim 0.3 occurs on time scales from 0.05 seconds to a few minutes. The energy released is about 10^{52} ergs and can account for Gamma Ray Bursts at cosmological distances. The estimated burst frequency, 10^{-6} per year per galaxy, is in very good agreement with observations. We also discuss the possibility of distinguishing these even ts from neutron star mergers by observing the different temporal behavior of gravit ational waves.']",['1996-03-26'] +2335,['eng'],"['Moffat, J W']",['Linearization instability of gravitational waves interacting with matter in general relativity'],['Astrophysics and Astronomy'],"['relativity theory, general', 'gravitational radiation, stability', 'coupling, matter', 'matter, coupling', 'perturbation theory', 'Einstein equation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603128'],"['The gravitational wave solutions obtained from a perturbation about conformally flat backgrounds in Einstein gravity are investigated. A perturbation theory analysis of the Lesame, Ellis and Dunsby results, based on a covariant approach, shows that for gravitational waves interacting with irrotational dust, the equations are linearization unstable. The gravitational wave equations based on the Weyl curvature tensor must be solved by non-perturbative methods. The significance of this result for gravitational wave calculations and experiments is discussed.']",['1996-03-25'] +2336,['eng'],"['Calzetta, E A', 'Kandus, A']",['Non linear structures from inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'astrophysics, model', 'perturbation, nonlinear', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603125'],"[""We present an analytical method to extract observational predictions about non linear evolution of perturbations in a Tolman Universe. We assume no a priori profile for them, instead we find it through a matching procedure of the Tolman Universe to a flat Friedmann Robertson Walker Universe plus perturbations originated during Inflation. We solve perturbatively a Hamilton Jacobi equation for a timelike geodesic and obtain the null one as a limiting case in two situations: for an observer located in the center of symmetry and for a non centered one. In the first case we find expressions to evaluate the density contrast and the number count and luminosity distance vs redshift relationships up to second order in the perturbations. In the second one we calculate the CMBR anisotropies at large angular scales produced by the density contrast and by the asymmetry of the observer's location, up to first order in the perturbations. We develope our argument in such a way that the formulae are valid for any shape of the primordial spectrum, and choose a scale invariant one to compare with actual observations. Our method is a general tool to contrast the predictions of several scenarios of fluctuation generation regarding large scale structures in the Universe.""]",['1996-03-25'] +2337,['eng'],"['Cardall, C Y', 'Fuller, G M']",['Limits on active-sterile neutrino mixing and the primordial deuterium abundance'],['Astrophysics and Astronomy'],"['neutrino, sterile', 'neutrino, interference', 'astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'deuterium, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603105'],"['Studies of limits on active-sterile neutrino mixing derived from big bang nucleosynthesis considerations are extended to consider the dependance of these constraints on the primordial deuterium abundance. This study is motivated by recent measurements of D/H in quasar absorption systems, which at present yield discordant results. Limits on active-sterile mixing are somewhat relaxed for high D/H. For low D/H (\\approx 2 \\times 10^{-5}), no active-sterile neutrino mixing is allowed by currently popular upper limits on the primordial ^4He abundance Y. For such low primordial D/H values, the observational inference of active-sterile neutrino mixing by upcoming solar neutrino experiments would imply that Y has been systematically underestimated, unless there is new physics not included in standard BBN.']",['1996-03-20'] +2338,['eng'],"['Kaniadakis, G', 'Lavagno, A', 'Quarati, P']",['Generalized statistics and solar neutrinos'],['Astrophysics and Astronomy'],"['neutrino, solar', 'statistics', 'plasma, solar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603109'],"['The generalized Tsallis statistics produces a distribution function appropriate to describe the interior solar plasma, thought as a stellar polytrope, showing a tail depleted respect to the Maxwell-Boltzmann distribution and reduces to zero at energies greater than about 20 \\, k_{_B} T. The Tsallis statistics can theoretically support the distribution suggested in the past by Clayton and collaborators, which shows also a depleted tail, to explain the solar neutrino counting rate.']",['1996-03-21'] +2339,['eng'],"['Dodelson, S', 'Gates, E', 'Turner, M S']",['Cold dark matter models'],['Astrophysics and Astronomy'],"['introductory', 'missing-mass, astrophysics', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603081'],"['Motivated by inflation, the theory of big-bang nucleosynthesis and the quest for a deeper understanding of the fundamental forces and particles, a very successful paradigm for the development of structure in the Universe has evolved. It holds that most of the matter exists in the form of slowly moving elementary particles left over from the earliest moments (cold dark matter or CDM) and that the small density inhomogeneities that seed structure formation arose from quantum fluctuations around 10^{-34}\\sec after the bang. A flood of observations is now testing the cold dark matter paradigm -- from determinations of the Hubble constant to measurements of the anisotropy of the Cosmic Background Radiation (CBR) -- and could reveal the details of the theory as well.']",['1996-03-18'] +2340,['eng'],"['McLaughlin, G C', 'Fuller, G M']",['Evidence for an intense neutrino flux during r-process nucleosynthesis?'],['Astrophysics and Astronomy'],"['neutrino nucleus, nuclear reaction', 'neutrino, capture', 'capture, neutrino', 'nucleus, semileptonic decay', 'semileptonic decay, nucleus', 'nucleus, width', 'light nucleus, production', 'production, light nucleus', 'neutrino, flux', 'flux, neutrino', 'astrophysics, supernova', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603082'],"['We investigate the possibility that neutrino capture on heavy nuclei competes with beta decay in the environment where the r-Process elements are synthesized. We find that such neutrino capture is not excluded by existing abundance determinations. We show that inclusion of significant neutrino capture on the (neutron number) N=82 waiting point nuclei can allow the inferred abundances of these species to provide a good fit to steady weak (beta decay plus neutrino capture) flow equilibrium. In fact, for particular choices of neutrino flux conditions, this fit is improved over the case where nuclei change their charge by beta decay alone. However, this improved fit can be realized only if neutrino capture plays a negligible role in nuclear decay back toward stability. We discuss the implications of these considerations for current proposed sites and models for r-Process nucleosynthesis.']",['1996-03-18'] +2341,['eng'],"['Starobinsky, A A']",['Spectrum of initial perturbations in open and closed inflationary models'],['Astrophysics and Astronomy'],"['talk, Moscow 1994/12/04', 'inflationary universe', 'perturbation, scalar', 'perturbation, tensor', 'cosmic radiation, background', 'temperature, anisotropy', 'Friedman model, open', 'Friedman model, closed']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603075'],"['Spectrum of initial scalar and tensor perturbations created during an inflationary stage producing a closed or open FRW universe now is discussed. In the closed case, the CMB temperature anisotropy {\\Delta T/T} generated by scalar perturbations is enhanced for low multipoles. It is argued that in the open case there is no suppression of low multipoles. A possibility of the existence of a preferred space direction in the open case is noted.']",['1996-03-18'] +2342,['eng'],"['Starobinsky, A A']",['Modern cosmological models with dark matter and their confrontation with observational data'],['Astrophysics and Astronomy'],"['talk, Moscow 1994/12/04', 'astrophysics, model', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'inflationary universe', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603074'],['New systematic classification of cosmological models of the present Universe is introduced. After making the comparison of these models with all existing observational data three viable models remain: the cold dark matter model with the cosmological constant (which becomes the most reasonable one if the Hubble constant H_0>60 km/s/Mpc); the mixed cold-hot dark matter model (models with two and especially three types of neutrinos with equal masses are in a slightly better agreement with observational data than the model with one massive neutrino); the pure cold dark matter model with a step-like initial spectrum of perturbations. The two latter models require H_0\\leq 60 km/s/Mpc.'],['1996-03-18'] +2343,['eng'],"['Raffelt, G G', 'Seckel, D', 'Sigl, G']",['Supernova neutrino scattering rates reduced by nucleon spin fluctuations'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, astrophysics', 'neutrino nucleon, elastic scattering', 'elastic scattering, neutrino nucleon', 'neutral current, axial-vector', 'nucleon, spin', 'spin, nucleon', 'nuclear matter', 'potential, spin', 'spin, potential', 'perturbation theory', 'sum rule', 'structure function', 'correlation, spin', 'spin, correlation', 'cross section', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603044'],"[""In a nuclear medium, spin-dependent forces cause the nucleon spins to fluctuate with a rate \\Gamma_\\sigma. We have previously shown that as a consequence the effective axial-current neutrino-nucleon scattering cross section is reduced. Here, we calculate this reduction explicitly in the perturbative limit \\Gamma_\\sigma\\ll T. By virtue of an exact sum rule of the spin-density structure function, we express the modified cross section in terms of the matrix element for neutrino-nucleon scattering in the presence of a spin-dependent nuclear potential. This representation allows for a direct comparison with and confirmation of Sawyer's related perturbative result. In a supernova core with a typical temperature T=10\\,\\rm MeV, the perturbative limit is relevant for densities \\rho\\alt10^{13}\\,\\rm g\\,cm^{-3} and thus applies around the neutrino sphere. There, the cross-section reduction is of order a few percent and thus not large; however, a new mode of energy transfer between neutrinos and nucleons is enabled which may be important for neutrino spectra formation. We derive an analytic perturbative expression for the rate of energy transfer.""]",['1996-03-13'] +2344,['eng'],"['Kernan, P J', 'Sarkar, S']",['No crisis for big bang nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'neutrino, flavor', 'numerical calculations, Monte Carlo']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603045'],"['Contrary to a recent claim, the inferred primordial abundances of the light elements are quite consistent with the expectations from standard big bang nucleosynthesis when attention is restricted to direct observations rather than results from chemical evolution models. The number of light neutrino (or equivalent particle) species (N_\\nu) can be as high as 4.53 if the nucleon-to-photon ratio (\\eta) is at its lower limit of 1.65 \\times 10^{-10}, as constrained by measurements of a high {\\rm D} abundance in Lyman-\\alpha clouds at high redshift. Alternatively, with N_\\nu = 3 as in the standard model, \\eta can be as high as 8.90 \\times 10^{-10} if the primordial {\\rm D} abundance is close to its value in the interstellar medium.']",['1996-03-13'] +2345,['eng'],"['Mohapatra, R N', 'Teplitz, V L']",['Structures in the mirror universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'symmetry, mirror', 'fermion, mirror particle', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603049'],"['The idea of the universe with a mirror sector having all particles and forces identical to those in the familiar sector has been proposed in the context of neutrino physics as well as superstring theories. Assuming that all the quark and charged lepton masses in the mirror universe are scaled by a common factor, \\zeta, as is required in one interpretation of the neutrino data, we investigate domains of the parameter \\zeta where physical conditions are favorable for cooling in the age of the universe that can lead to the formation of compact structures given the initial condition \\Omega_B =\\Omega_{\\tilde{B}} (\\tilde{B} denoting the mirror baryon). In particular we ask whether there is a region in \\zeta-space for which primordial Jeans mass mirror clouds cannot cool in the present age of the universe. We find that for most of the area of interest in the parameter space, atomic hyperfine structure cooling is effective in a time period short compared to the age of the universe but long compared to the free fall time for globular-sized objects expected on the basis of simple Jeans length analysis.']",['1996-03-13'] +2346,['eng'],"['Grasso, D', 'Kolb, E W']",['Cosmological bounds to the magnetic moment of heavy $\\tau$ neutrinos'],['Astrophysics and Astronomy'],"['neutrino, magnetic moment', 'magnetic moment, neutrino', 'neutrino/tau, mass', 'mass, neutrino/tau', 'neutrino, density', 'astrophysics', 'light nucleus, production', 'production, light nucleus', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603051'],"['The magnetic moment of tau neutrinos in the MeV mass range may be large enough to modify the cosmological freeze-out calculation and determine the tau-neutrino relic density. In this paper we revisit such a possibility. We calculate the evolution and freeze-out of the tau neutrino number density as a function of its mass and magnetic moment. We then determine its relic density, then calculate its effect upon primordial nucleosynthesis including previously neglected effects.']",['1996-03-13'] +2347,['eng'],"['Collar, J I']",['Superheated Microdrops as Cold Dark Matter Detectors'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'WIMP', 'thermodynamics, critical phenomena', 'matter, droplet', 'tracks', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9607150'],"['It is shown that under realistic background considerations, an improvement in Cold Dark Matter sensitivity of several orders of magnitude is expected from a detector based on superheated liquid droplets. Such devices are totally insensitive to minimum ionizing radiation while responsive to nuclear recoils of energies ~ few keV. They operate on the same principle as the bubble chamber, but offer unattended, continuous, and safe operation at room temperature and atmospheric pressure.']",['1996-07-30'] +2348,['eng'],"['Pohl, M']",['Diffuse gamma-rays from galactic halos'],['Astrophysics and Astronomy'],"['talk, Bad Honnef 1996/02/12', 'astrophysics, galaxy', 'photon, cosmic radiation', 'diffusion, emission', 'emission, diffusion', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603046'],"['Here we review our current knowledge on diffuse gamma-rays from galactic halos. Estimates of the relative contribution of the various emission processes at low and high latitudes are compared to the data over 6 decades in energy. The observed spectral shape differs from what was expected, especially at ver low and very high energies. In the latter case, above 1 GeV, the sky emission related to gas exceeds the expected pi^0 decay spectrum. At energies below 1 MeV the relatively high gamma-ray intensity indicates at high density of nearly relativistic electrons which would have a strong influence on the energy and ionisation balance of the interstellar medium. Given the EGRET results for the Magellanic Clouds the gamma-ray emissivity in the outer halo is probably small, so that a substantial amount of baryonic dark matter may be hidden at 20-50 kpc radius without inducing observable gamma-ray emission.']",['1996-03-13'] +2349,['eng'],"['Semig, L V', 'Müller, V']",['Non-flat power spectra in the CDM model'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'spectra, perturbation', 'perturbation, spectra', 'field equations, solution', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, galaxy', 'potential', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508120'],"[""Standard inflation with one scalar field produces primordial perturbations with a nearly flat ('Harrison-Zeldovich') power spectrum. Here we consider first, a double inflation spectrum, and second, a massive scalar field with an interaction potential which mimics an early quartic interaction, but fading away at a characteristic scale. We solve numerically the linear perturbation equations with initial conditions due to scalar field quantum fluctuations at the initial horizon crossing. The resulting power spectra are shown to be non-flat, exhibiting either a break or a valley. Using the transfer function of cold dark matter model we study the influence of the shape of primordial power spectra on observations of large scale structure in the universe. We compare the power spectra in redshift space with reconstructed power spectra from the IRAS catalogue. Further we discuss the variances of galaxy counts in cells, and the mass function of galaxy clusters. Comparison with standard CDM demonstrates the advantages and benefits of the more complicated initial spectra.""]",['1995-08-28'] +2350,['eng'],"['Wang, Y', 'Turner, E L']",['The cosmological constant and advanced gravitational wave detectors'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'n, matter', 'astrophysics, fundamental constant', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603034'],"['Interferometric gravitational wave detectors could measure the frequency sweep of a binary inspiral [characterized by its chirp mass] to high accuracy. The observed chirp mass is the intrinsic chirp mass of the binary source multiplied by (1+z), where z is the redshift of the source. Assuming a non-zero cosmological constant, we compute the expected redshift distribution of observed events for an advanced LIGO detector. We find that the redshift distribution has a robust and sizable dependence on the cosmological constant; the data from advanced LIGO detectors could provide an independent measurement of the cosmological constant.']",['1996-03-11'] +2351,['eng'],"['Spergel, D N']",['Particle dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'baryon, matter', 'neutrino, massive', 'massive, neutrino', 'postulated particle, WIMP', 'postulated particle, axion', 'counters and detectors', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603026'],"[""Several lines of evidence suggest that some of the dark matter may be non-baryonic: the non-detection of various plausible baryonic candidates for dark matter inferred, e.g., from galaxy rotation curves and from cluster of galaxy velocity dispersions, the need for non-baryonic dark matter for theoretical models of galaxy formation, and the large discrepancy between dynamical measurements implying \\Omega_0 > 0.2 and the baryon abundance inferred from big bang nucleosynthesis, \\Omega_b h^2 = 0.015. There are a number of well-motivated dark matter candidates: massive neutrinos, supersymmetric dark matter and ``invisible'' axions. Many of these dark matter candidates are potentially detectable by the current generation of dark matter experiments.""]",['1996-03-21'] +2352,['eng'],"['Chakrabarti, S K']",['Gravitational wave emission from a binary black hole system in presence of an accretion disk'],['Astrophysics and Astronomy'],"['gravitational radiation, emission', 'emission, gravitational radiation', 'black hole', 'angular momentum, exchange', 'exchange, angular momentum']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9603117'],"['We study time evolution and gravitational wave emission properties of a black hole orbiting {\\it inside} an accretion disk surrounding a massive black hole. We simultaneously solve the structure equations of the accretion disk in presence of heating, cooling and viscosity as well as the equations governing the companion orbit. The deviation from Keplerian distribution of angular momentum of the disk due to pressure and advection effects causes a significant exchange of angular momentum between the disk and the companion. This significantly affects the gravitational wave emission properties from the binary system. We show that when the companion is light, the effect is extremely important and must be taken into account while interpreting gravitational wave signals from such systems.']",['1996-03-22'] +2353,['eng'],"['Durrer, R', 'Zhou, Z H']",['Large scale structure formation with global topological defects'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'space-time', 'topology, defect', 'matter, density', 'perturbation theory', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508016'],"['We investigate cosmological structure formation seeded by topological defects which may form during a phase transition in the early universe. First we derive a partially new, local and gauge invariant system of perturbation equations to treat microwave background and dark matter fluctuations induced by topological defects or any other type of seeds. We then show that this system is well suited for numerical analysis of structure formation by applying it to seeds induced by fluctuations of a global scalar field. Our numerical results are complementary to previous investigations since we use substantially different methods. The resulting microwave background fluctuations are compatible with older simulations. We also obtain a scale invariant spectrum of fluctuations with about the same amplitude. However, our dark matter results yield a smaller bias parameter compatible with b\\sim 2 on a scale of 20 Mpc in contrast to previous work which yielded to large bias factors. Our conclusions are thus more positive. According to the aspects analyzed in this work, global topological defect induced fluctuations yield viable scenarios of structure formation and do better than standard CDM on large scales.']",['1995-08-07'] +2354,['eng'],"['Faraoni, V']",['Light amplification by gravitational waves in scalar-tensor theories of gravity'],['Astrophysics and Astronomy'],"['gravitation, model', 'gravitational radiation', 'gravitation, scalar', 'gravitation, tensor']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602154'],"['It is shown that the amplification of a light beam by gravitational waves in scalar-tensor theories of gravity is a first order effect in the wave amplitudes. In general relativity, instead, the effect is only of second order.']",['1996-03-01'] +2355,['eng'],"['Shi, X']",['Chaotic amplification of neutrino chemical potentials by neutrino oscillations in Big Bang nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'neutrino, sterile', 'neutrino, oscillation', 'neutrino, flavor', 'potential, chemical', 'chaos', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602135'],"['We investigate in detail the parameter space of active-sterile neutrino oscillations that amplifies neutrino chemical potentials at the epoch of Big Bang Nucleosynthesis. We calculate the magnitude of the amplification and show evidences of chaos in the amplification process. We also discuss the implications of the neutrino chemical potential amplification in the Big Bang Nucleosynthesis. It is shown that with a \\sim 1 eV \\nue, the amplification of its chemical potential by active-sterile neutrino oscillations can lower the effective number of neutrino species at Big Bang Nucleosynthesis to significantly below 3.']",['1996-02-27'] +2356,['eng'],"['Robinson, J', 'Yates, A J']",['String formation and the power spectrum of field configurations'],['Astrophysics and Astronomy'],"['astrophysics, string', 'topology, defect', 'symmetry breaking, U(1)', 'Higgs model', 'spectra', 'string, density', 'lattice field theory', 'critical phenomena', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602131'],"['We examine the statistical properties of defects formed by the breaking of a U(1) symmetry when the Higgs field has a power spectrum P(k) \\propto k^n. We find a marked dependence of the amount of infinite string on the spectral index n, and confirm that this result is robust to changes in the definition of infinite string. It is possible that this result could account for the apparent absence of infinite string in recent lattice-free simulations.']",['1996-02-26'] +2357,['eng'],"['Kang, H', 'Ryu, D', 'Jones, T W']",['Cluster accretion shocks as possible acceleration sites for ultra high energy protons below the Greisen cutoff'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'p, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'energy spectrum, (p)', '(p), energy spectrum', 'astrophysics, model', 'model, hydrodynamical', 'cosmic radiation, acceleration', 'magnetic field', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507113'],"['Three-dimensional hydrodynamic simulations of large scale structure in the Universe have shown that accretion shocks form during the gravitational collapse of one-dimensional caustics, and that clusters of galaxies formed at intersections of the caustics are surrounded by these accretion shocks. Estimated speed and curvature radius of the shocks are 1000-3000 \\kms and about 5 Mpc, respectively, in the \\Omega=1 CDM universe. Assuming that energetic protons are accelerated by these accretion shocks via the first-order Fermi process and modeling particle transport around the shocks through Bohm diffusion, we suggest that protons can be accelerated up to the {\\it Greisen cutoff energy} near 6\\times 10^{19} eV, provided the mean magnetic field strength in the region around the shocks is at least of order a microgauss. We have also estimated the proton flux at earth from the Virgo cluster. Assuming a few (1-10) \\% of the ram pressure of the infalling matter would be transferred to the cosmic-rays, the estimated flux for E \\sim 10^{19}eV is consistent with observations, so that such clusters could be plausible sources of the UHE CRs.']",['1995-07-31'] +2358,['eng'],"['Pohl, M']",['Leptonic origin of TeV gamma-rays from supernova remnants'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, supernova', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'synchrotron radiation', 'photon electron, elastic scattering', 'elastic scattering, photon electron', 'cosmic radiation, background', 'microwaves', 'Cherenkov counter, efficiency', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602115'],"['The lineless power-law emission observed by ASCA from the northeastern rim of the supernova remnant SN1006 has recently been interpreted as synchrotron radiation of electrons with energies around 100 TeV. In this letter we calculate the flux of inverse Compton emission at TeV photon energies that is a natural consequence of the existence of such high energy electrons and the cosmic microwave background. We find that the predicted flux is near the present sensitivity limit of the southern \\v Cerenkov telescope CANGAROO, and should be detectable with the next performance improvements. The spectrum of SN1006 at a few TeV will be very soft. The existence of such highest energy electrons in SN1006 may not be a unique to this remnant. We can therefore conclude that the detection of TeV \\gamma-ray emission in any supernova remnant does not necessarily provide evidence for a large number of cosmic ray nucleons in these objects, and thus is no simple test of cosmic ray origin as far as nucleons are concerned.']",['1996-02-23'] +2359,['eng'],"['Pina-Avelino, P', 'Caldwell, R R']",['Entropy perturbations due to cosmic strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'model, fluid', 'entropy, perturbation', 'spectra, fluctuation', 'fluctuation, spectra', 'invariance, gauge', 'cosmic radiation, background', 'cosmic radiation, anisotropy']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602116'],"['We examine variations in the equation of state of the cosmic string portion of the cosmological fluid which lead to perturbations of the background matter density. These fluctuations in the equation of state are due to variations in the local density of cosmic string loops and gravitational radiation. Constructing a crude model of the distribution of entropy perturbations, we obtain the resulting fluctuation spectrum using a gauge-invariant formalism. We compute the resulting cosmic microwave background anisotropy, and estimate the effect of these perturbations on the cosmic string structure formation scenario.']",['1996-02-23'] +2360,['eng'],"['Faraoni, V']",['Non-minimal coupling of the scalar field and inflation'],['Astrophysics and Astronomy'],"['field theory, scalar', 'coupling constant', 'relativity theory, general', 'space-time', 'inflationary universe', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602111'],['We study the prescriptions for the coupling constant of a scalar field to the Ricci curvature of spacetime in specific gravity and scalar field theories. The results are applied to the most popular inflationary scenarios of the universe; their theoretical consistency and certain observational constraints are discussed.'],['1996-02-22'] +2361,['eng'],"['Costa, S', 'Halzen, Francis', 'Bellandi, J', 'Salles, C']","['Composition of primary cosmic rays beyond the ""knee"" from emulsion chamber observations']",['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'showers, hadronic', 'showers, electromagnetic', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'showers, air', 'hadron nucleus, nuclear reaction', 'air', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602108'],"['We show that the simplest assumptions for the dynamics of particle production allow us to understand the fluxes of hadrons and photons at mountain altitudes as well as the structure of individual events. The analysis requires a heavy nuclear component of primary cosmic rays above the ``knee"" in the spectrum with average mass number = 7.3 \\pm 0.9.']",['1996-02-22'] +2362,['eng'],"['Bonazzola, S', 'Gourgoulhon, E']",['Gravitational waves from pulsars'],['Astrophysics and Astronomy'],"['gravitational radiation', 'astrophysics, pulsar', 'magnetic field', 'n, matter', 'matter, fluid', 'counters and detectors, interference', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602107'],"['The gravitational wave emission by a distorted rotating fluid star is computed. The distortion is supposed to be symmetric around some axis inclined with respect to the rotation axis. In the general case, the gravitational radiation is emitted at two frequencies: \\Omega and 2\\Omega, where \\Omega is the rotation frequency. The obtained formul\\ae\\ are applied to the specific case of a neutron star distorted by its own magnetic field. Assuming that the period derivative \\dot P of pulsars is a measure of their magnetic dipole moment, the gravitational wave amplitude can be related to the observable parameters P and \\dot P and to a factor \\beta which measures the efficiency of a given magnetic dipole moment in distorting the star. \\beta depends on the nuclear matter equation of state and on the magnetic field distribution. The amplitude at the frequency 2\\Omega, expressed in terms of P, \\dot P and \\beta, is independent of the angle \\alpha between the magnetic axis and the rotation axis, whereas at the frequency \\Omega, the amplitude increases as \\alpha decreases. The value of \\beta for specific models of magnetic field distributions has been computed by means of a numerical code giving self-consistent models of magnetized neutron stars within general relativity. It is found that the distortion at fixed magnetic dipole moment is very dependent of the magnetic field distribution; a stochastic magnetic field or a superconductor stellar interior greatly increases \\beta with respect to the uniformly magnetized perfect conductor case and might lead to gravitational waves detectable by the VIRGO or LIGO interferometers. The amplitude modulation of the signal induced by the daily rotation of the Earth has been computed and specified to the case of the Crab pulsar and VIRGO']",['1996-02-22'] +2363,['eng'],"['Cardall, C Y', 'Fuller, G M']","['Can a ""natural"" three-generation neutrino mixing scheme satisfy everything?']",['Astrophysics and Astronomy'],"['bibliography', 'astrophysics', 'neutrino, cosmic radiation', 'neutrino, solar', 'neutrino, interference', 'neutrino, flavor', 'neutrino, oscillation', 'matter', 'astrophysics, supernova', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, sterile', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602104'],"[""We examine the potential for a ``natural'' three-neutrino mixing scheme to satisfy available data and astrophysical arguments. By ``natural'' we mean no sterile neutrinos, and a neutrino mass hierarchy similar to that of the charged leptons. We seek to satisfy (or solve): 1. Accelerator and reactor neutrino oscillation constraints, including LSND; 2. The atmospheric muon neutrino deficit problem; 3. The solar neutrino problem; 4. Supernova r-process nucleosynthesis in neutrino-heated supernova ejecta; 5. Cold+hot dark matter models. We argue that putative supernova r-process nucleosynthesis bounds on two-neutrino flavor mixing can be applied directly to three-neutrino mixing in the case where one vacuum neutrino mass eigenvalue difference dominates the others. We show that in this ``one mass scale dominance'' limit, a natural three-neutrino oscillation solution meeting all the above constraints exists only if the atmospheric neutrino data {\\em and} the LSND data can be explained with one neutrino mass difference. In this model, an explanation for the solar neutrino data can be effected by employing the {\\em other} independent neutrino mass difference. Such a solution is only marginally allowed by the current data, and proposed long-baseline neutrino oscillation experiments can definitively rule it out. If it were ruled out, the simultaneous solution of the above constraints by neutrino oscillations would then require sterile neutrinos and/or a neutrino mass hierarchy of a different nature than that of the charged leptons.""]",['1996-02-21'] +2364,['eng'],"['Kolb, E W', 'Riotto, A']",['Preheating and symmetry restoration in collisions of vacuum bubbles'],['Astrophysics and Astronomy'],"['inflationary universe', 'critical phenomena', 'vacuum state, bubble', 'scattering, bubble', 'bubble, scattering', 'symmetry, spontaneously broken', 'field theory, scalar', 'scalar particle, production', 'production, scalar particle']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602095'],"[""In first-order inflation a phase transition is completed by the collisions of expanding true-vacuum bubbles. If bubble collisions produce large numbers of soft scalar particles carrying quantum numbers associated with a spontaneously broken symmetry, then symmetry restoration may occur in a ``pre-heating'' phase in a manner similar to symmetry restoration in the pre-heating phase of slow-roll inflation. Since bubble collisions lead to inhomogeneities, there is the possibility of inhomogeneous symmetry restoration where restoration occurs only in the regions of wall collisions.""]",['1996-02-20'] +2365,['eng'],"['Ellis, Jonathan Richard']",['Astroparticle physics'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'LSP', 'neutrino, mass', 'mass, neutrino', 'neutrino, oscillation', 'search for, missing-mass', 'missing-mass, search for', 'axion', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602077'],"['At the request of the organizers, this talk surveys some of the hot topics discussed at this meeting, giving my {\\it subjective views} on them. Subjects covered include the present age and Hubble expansion rate of the Universe - {\\it inflation theorists need not yet abandon \\Omega = 1}, theories of structure formation in the light of COBE and other data - {\\it my favourite is a flat spectrum of initial perturbations subsequently amplified by mixed hot and cold dark matter}, neutrino masses and oscillations - {\\it the only experimental indication I take seriously at the moment is the persistent solar neutrino deficit}, the lightest supersymmetric particle - {\\it which may behave differently if conventional assumptions are relaxed}, and the axion - {\\it much of the window between limits from SN 1987a and cosmology will be explored in an ongoing experiment}. Finally, I present a chronology of some possible interesting future experiments.']",['1996-02-16'] +2366,['eng'],"['Christiansen, M B', 'Madsen, J']",['Large nucleation distances from impurities in the cosmological quark-hadron transition'],['Astrophysics and Astronomy'],"['astrophysics, model', 'transition, quark hadron', 'critical phenomena', 'light nucleus, production', 'production, light nucleus', 'thermodynamics', 'bag model', 'quark gluon, plasma', 'quark, mass', 'mass, quark', 'quark, strangeness', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602071'],"['We calculate the mean nucleation distance, d_{nuc}, in a first order cosmological quark-hadron phase transition. For homogeneous nucleation we find that self-consistent inclusion of curvature energy reduces d_{nuc} to \\lesssim 2cm. However, impurities can lead to heterogeneous nucleation with d_{nuc} of several meters, a value high enough to change the outcome of Big Bang nucleosynthesis.']",['1996-02-16'] +2367,['eng'],"['Bahcall, J N', 'Fukugita, M', 'Krastev, P I']",['How does the sun shine?'],['Astrophysics and Astronomy'],"['astrophysics', 'model, solar', 'luminosity, solar', 'neutrino, oscillation', 'fusion', 'numerical calculations', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602065'],"['Assuming that MSW neutrino oscillations occur and ignoring all solar physics except for the constraint that nuclear fusion produces the solar luminosity, we show that new solar neutrino experiments are required to rule out empirically the hypothesis that the sun shines via the CNO cycle.']",['1996-02-14'] +2368,['eng'],"['Zimdahl, W']",['Bulk viscous cosmology'],['Astrophysics and Astronomy'],"['astrophysics, model', 'inflationary universe', 'particle, production', 'production, particle', 'thermodynamics', 'temperature', 'model, fluid']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601189'],"['The full causal M\\""uller-Israel-Stewart (MIS) theory of dissipative processes in relativistic fluids is applied to a flat, homogeneous and isotropic universe with bulk viscosity. It is clarified in which sense the so called truncated version is a reasonable limiting case of the full theory. The possibility of bulk viscosity driven inflationary solutions of the full theory is discussed. As long as the particle number is conserved almost all these solutions exhibit an exponential increase of the temperature. Assuming that the bulk viscous pressure of the MIS theory may also be interpreted as an effective description for particle production processes, the thermodynamical behaviour of the Universe changes considerably. In the latter case the temperature increases at a lower rate or may remain constant during a hypothetical de Sitter stage, accompanied by a substantial growth of the comoving entropy.']",['1996-02-01'] +2369,['eng'],"['Calabresu, E', 'Fiorentini, G', 'Lissia, M']",['Physics potentials of pp and pep solar neutrino fluxes'],['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, flux', 'neutrino, oscillation', 'neutrino, sterile', 'angular dependence', 'counters and detectors, proposed', 'neutrino, particle identification', 'temperature, solar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602045'],"['Experimental determinations of the pp and pep fluxes have great potentialities. We briefly review the reasons that make such measurements privileged tests of neutrino properties. We discuss the predictions for these fluxes given by four good solutions to the solar neutrino problem: small- and large-angle MSW and Just-So oscillations into active neutrinos, and small-angle MSW oscillations into sterile neutrinos. In addition, we examine the impact of the planned Hellaz detector, which should measure separately the nu_e and nu_mu fluxes in the pp energy window and the signal from the pep neutrinos, for distinguishing among the different solutions and for determining the solar central temperature.']",['1996-02-13'] +2370,['eng'],"['Page, D']",['Strange stars'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, matter', 'matter, strangeness', 'n, matter', 'quantum chromodynamics, ground state', 'baryon number, finite', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602043'],"[""Witten's conjecture about strange quark matter (`Strange Matter') being the ground state of QCD at finite baryon number is presented and stars made of strange matter (`Strange Stars') are compared to neutron stars. The only observable way in which a strange star differs from a neutron star is in its early thermal history and a detailed study of strange star cooling is reported and compared to neutron star cooling. One concludes that future detection of thermal radiation from the compact object produced in the core collapse of SN 1987A could present the first evidence for strange matter.""]",['1996-02-13'] +2371,['eng'],"['Steigman, G']",['Big Bang nucleosynthesis'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'deuterium', 'helium, nuclide', 'lithium', 'electroweak interaction, model', 'model, electroweak interaction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602029'],"['In the first thousand seconds of its evolution the Universe was a primordial nuclear reactor synthesizing the nuclides D, ^3He, ^4He and ^7Li. These messengers from the Big Bang provide a unique window on the early, hot, dense Universe, offering the opportunity for tests of the standard models of particle physics and of cosmology. A new, statistically coherent comparison of the primordial abundances of these nuclides inferred from increasingly accurate observational data with those predicted by the standard model hints at a possible crisis. The case for this emerging crisis is presented and several paths towards ameliorating it are explored.']",['1996-02-07'] +2372,['eng'],"['Magueijo, J', 'Hobson, M P']",['Cosmic microwave background experiments targeting the cosmic strings Doppler peak signal'],['Astrophysics and Astronomy'],"['astrophysics, microwaves', 'astrophysics, string', 'numerical calculations', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602023'],"['We investigate which experiments are better suited to test the robust prediction that cosmic strings do not produce secondary Doppler peaks. We propose a statistic for detecting oscillations in the C^l spectrum, and study its statistical relevance given the truth of an inflationary competitor to cosmic strings. The analysis is performed for single-dish experiments and interferometers, subject to a variety of noise levels and scanning features. A high resolution of 0.2 degrees is found to be required for single-dish experiments with realistic levels of noise. Interferometers appear to be more suitable for detecting this signal.']",['1996-02-13'] +2373,['eng'],"['Hu, W', 'White, M']",['A new test of inflation'],['Astrophysics and Astronomy'],"['inflationary universe, validity test', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'matter, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602020'],"['We discuss a new test of inflation from the harmonic pattern of peaks in the cosmic microwave background radiation angular power spectrum. By characterizing the features of alternate models and revealing signatures unique to inflation, we show that the paradigm could be validated by the next generation of experiments.']",['1996-02-07'] +2374,['eng'],"['Gangui, A', 'Durrer, R', 'Sakellariadou, M']",['Global textures and the Doppler peaks'],['Astrophysics and Astronomy'],"['talk, Valencia 1995/09/18', 'astrophysics, texture', 'cosmic radiation, background', 'spectra, fluctuation', 'fluctuation, spectra', 'topology, defect', 'plasma, oscillation', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'inflationary universe', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602018'],"[""We review recent work aimed at showing how global topological defects influence the shape of the angular power spectrum of the CMB radiation on small scales. While Sachs-Wolfe fluctuations give the dominant contribution on angular scales larger than about a few degrees, on intermediate scales the main r\\^ole is played by coherent oscillations in the baryon radiation plasma before recombination. In standard cosmological models these oscillations lead to the `Doppler peaks' in the angular power spectrum. Inflation-based cold dark matter models predict the location of the first peak to be at \\ell\\sim 220/\\sqrt{\\Omega_0}, with a height which is a few times the level of anisotropies at large scales. Here we focus on perturbations induced by global textures. We find that the height of the first peak is reduced and is shifted to \\ell\\sim 350.""]",['1996-02-07'] +2375,['eng'],"['Bykov, A', 'Mészáros, P']",['Electron acceleration and efficiency in nonthermal gamma-ray sources'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, particle source', 'astrophysics, galaxy', 'electron, acceleration', 'electron, energy spectrum', 'energy spectrum, electron', 'astrophysics, jet', 'model, shock waves', 'model, hydrodynamical']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602016'],"['In energetic nonthermal sources such as gamma-ray bursts, AGN or galactic jet sources, etc., one expects both relativistic and transrelativistic shocks acompanied by violent motions of moderately relativistic plasma. We present general considerations indicating that these sites are electron and positron accelerators leading to a modified power law spectrum. The electron (or e^\\pm) energy index is very hard, \\propto \\gamma^{-1} or flatter up to a comoving frame break energy \\gamma_\\ast, and becomes steeper above that. In the example of gamma-ray bursts the Lorentz factor reaches \\gamma_\\ast\\sim 10^3 for e^{\\pm} accelerated by the internal shock ensemble on subhydrodynamical time scales. For pairs accelerated on hydrodynamical timescales in the external shocks similarly hard spectra are obtained, and the break Lorentz factor can be as high as \\gamma_\\star \\siml 10^5. Radiation from the nonthermal electrons produces photon spectra with shape and characteristic energies in qualitative agreement with observed generic gamma-ray burst and blazar spectra. The scenario described here provides a plausible way to solve one of the crucial problems of nonthermal high energy sources, namely the efficient transfer of energy from the proton flow to an apropriate nonthermal lepton component.']",['1996-02-07'] +2376,['eng'],"['Bahcall, J N', 'Ulmer, A']",['The temperature dependence of solar neutrino fluxes'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, solar', 'neutrino, flux', 'flux, neutrino', 'correlation', 'temperature, dependence', 'model, solar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9602012'],"['By comparing neutrino fluxes and central temperatures calculated from 1000 detailed numerical solar models, we derive improved scaling laws which show how each of the neutrino fluxes depends upon the central temperature (flux \\propto T^m); we also estimate uncertainties for the temperature exponents. With the aid of a one-zone model of the sun, we derive expressions for the temperature exponents of the neutrino fluxes. For the most important neutrino fluxes, the exponents calculated with the one-zone model agree to within 20\\% or better with the exponents extracted from the detailed numerical models. The one-zone model provides a physical understanding of the temperature dependence of the neutrino fluxes. For the pp neutrino flux, the one-zone model explains the (initially-surprising) dependence of the flux upon a negative power of the temperature and suggests a new functional dependence. This new function makes explicit the strong anti-correlation between the ^7Be and pp neutrino fluxes. The one-zone model also predicts successfully the average linear relations between neutrino fluxes, but cannot predict the appreciable scatter in a \\Delta \\phi_i/\\phi_i versus \\Delta \\phi_j/\\phi_j diagram.']",['1996-02-07'] +2377,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Bottino, A', 'Mignola, G']",['Non-baryonic dark matter'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutralino', 'LSP', 'axion, mass', 'mass, axion', 'upper limit', 'axino', 'Majoron', 'astrophysics, model', 'energy, density', 'supersymmetry, potential', 'electroweak interaction', 'symmetry breaking', 'grand unified theory, SU(5)', 'strong interaction, CP', 'CP, strong interaction']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601188'],"['The best particle candidates for non--baryonic cold dark matter are reviewed, namely, neutralino, axion, axino and Majoron. These particles are considered in the context of cosmological models with the restrictions given by the observed mass spectrum of large scale structures, data on clusters of galaxies, age of the Universe etc.']",['1996-02-01'] +2378,['eng'],"['Matarrese, S']",['Relativistic cosmology'],['Astrophysics and Astronomy'],"['talk, Varenna 1995/07/25', 'astrophysics, relativistic', 'model, fluid', 'relativity theory, general', 'space-time, horizon', 'Lagrangian formalism', 'gravitational radiation, stochastic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601172'],"['The general relativistic non--linear dynamics of a self--gravitating collisionless fluid with vanishing vorticity is studied in synchronous and comoving -- i.e. {\\em Lagrangian} -- coordinates. Writing the equations in terms of the metric tensor of the spatial sections orthogonal to the fluid flow allows an unambiguous expansion in inverse powers of the speed of light. The Newtonian and post--Newtonian approximations are derived in Lagrangian form; the non--linear evolution of the system on super--horizon scales, leading to the so--called ``silent universe"", is also briefly discussed. A general formula for the gravitational waves generated by the non--linear evolution of cosmological perturbations is given: a stochastic gravitational--wave background is shown to be produced by non--linear cosmic structures, with present--day closure density \\Omega_{gw} \\sim 10^{-5} -- 10^{-6} on the scale of 1 -- 10 Mpc.']",['1996-01-31'] +2379,['eng'],"['Turner, M S', 'Gates, E I', 'Gyuk, G']",['MACHOs'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'baryon, matter', 'astrophysics, galaxy', 'matter, density', 'astrophysics, MACHO', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601168'],"['We discuss the implications of the recent upward revision of the LMC microlensing rate by the MACHO Collaboration. We conclude: (i) A good case for the existence of baryonic dark matter in the halo has been made; (ii) The case for the existence of cold dark matter is unaffected and still compelling; and (iii) The Galactic halo is still an excellent place to search for cold dark matter particles (e.g., axions or neutralinos).']",['1996-01-30'] +2380,['eng'],"['Matarrese, S', 'Terranova, D', 'Matarrese, Sabino', 'Terranova, David']",['Lagrangian dynamics of collisionless matter'],['Astrophysics and Astronomy'],"['talk, Valencia 1995/09/18', 'astrophysics, model', 'gravitational radiation', 'model, fluid', 'astrophysics, perturbation', 'approximation, nonlinear', 'relativity theory, general', 'Lagrangian formalism']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601163'],"['The non--linear dynamics of self--gravitating irrotational dust is analyzed in a general relativistic framework, using synchronous and comoving coordinates. Writing the equations in terms of the metric tensor of the spatial sections orthogonal to the fluid flow allows an unambiguous expansion in inverse powers of the speed of light. The Newtonian and post--Newtonian approximations are derived in Lagrangian form. A general formula for the gravitational waves generated by the non--linear evolution of cosmological perturbations is given. It is argued that a stochastic gravitational--wave background is produced by non--linear cosmic structures, with present--day closure density \\Omega_{gw} \\sim 10^{-5} -- 10^{-6} on Mpc scale.']",['1996-01-30'] +2381,['eng'],"['Bezrukov, L B']",['Preliminary results on a search for neutrinos from the center of the earth with the Baikal underwater telescope'],['Astrophysics and Astronomy'],"['talk, Rome 1995/11/13', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'sparticle, neutral particle', 'sparticle, annihilation', 'annihilation, sparticle', 'neutrino, cosmic radiation', 'neutrino nucleon, interaction', 'interaction, neutrino nucleon', 'muon, flux', 'flux, muon', 'upper limit', 'counters and detectors, optical', 'deep underground detector, Baikal']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601161'],['The deep underwater Cherenkov neutrino telescope NT-200 is currently under construction at lake Baikal. Its first stage NT-36 consisting of 36 optical modules has operated over 2 years since April 1993 till March 1995. Here we present a method to search for nearly vertical upward going muons from neutralino annihilation in the center of the Earth. We present preliminary results obtained from experimental data taken with the NT-36 array in 1994.'],['1996-02-02'] +2382,['eng'],"['Belolaptikov, I A', 'Bezrukov, L B', 'Borisovets, B A', 'Budnev, N M', 'Chensky, A G', 'Danilchenko, I A', 'Djilkibaev, J A M', 'Dobrynin, V I', 'Domogatsky, G V', 'Doroshenko, A A', 'Fialkovsky, S V', 'Gaponenko, O N', 'Garus, A A', 'Gress, O A', 'Gress, T A', 'Heukenkamp, H', 'Karle, A', 'Klabukov, A M', 'Klimov, A I', 'Klimushin, S I', 'Koshechkin, A P', 'Kulepov, V F', 'Kuzmichov, L A', 'Lubsandorzhiev, B K', 'Mikolajski, T', 'Milenin, M B', 'Mirgazov, R R', 'Moroz, A V', 'Moseiko, N I', 'Nikiforov, S A', 'Osipova, E A', 'Panfilov, A I', 'Parfenov, Yu V', 'Pavlov, A A', 'Petukhov, D P']",['Search for magnetic monopoles with deep underwater Cherenkov detectors at Lake Baikal'],['Astrophysics and Astronomy'],"['talk, Rome 1995/11/13', 'postulated particle, magnetic monopole', 'scattering, p magnetic monopole', 'p magnetic monopole, scattering', 'Rubakov effect', 'p, semileptonic decay', 'semileptonic decay, p', 'muon, trigger', 'radiation, Cherenkov', 'velocity, magnetic monopole', 'flux, magnetic monopole', 'magnetic monopole, flux', 'upper limit', 'deep underground detector, Baikal', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601160'],"['The deep underwater Cherenkov neutrino telescope NT-200 is currently under construction at Lake Baikal. The ""subdetectors"" NT-36 (1993-95) and NT-72 (1995-96) have been operating successfully over 3 years. Various techniques have been developed to search for magnetic monopoles with these arrays. Here we describe a method used to detect superheavy slowly moving (beta = v/c = 0.00001 - 0.001) monopoles catalyzing baryon decay. We present results obtained from the preliminary analysis of the data taken with NT-36 detector in 1993. Furthermore, possibilities to observe faster (beta = 0.2 - 1) monopoles via other effects are discussed.']",['1996-01-30'] +2383,['eng'],"['Kamionkowski, M P', 'Toumbas, N']",['A low-density closed universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'matter, density', 'energy, density', 'cosmic radiation, background', 'astrophysics, galaxy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601147'],"['Matter with an equation of state p=-\\rho/3 may arise in certain scalar field theories, and the energy density of this matter decreases as a^{-2} with the scale factor a of the Universe. In this case, the Universe could be closed but still have a nonrelativistic-matter density \\Omega_0<1. Furthermore, the cosmic microwave background could come from a causally-connected region at the other side of the Universe. This model is currently viable and might be tested by a host of forthcoming observations.']",['1996-01-26'] +2384,['eng'],"['Stanev, T', 'Schäfer, R', 'Watson. A']",['Study of the correlations between the highest energy cosmic ray showers and gamma ray bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'search for, angular correlation', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601140'],['We examine the correlation between the arrival direction of ultra high energy cosmic ray showers and gamma ray bursts in the third BATSE catalog. We find no correlation between the two data sets. We also find no correlations between a pre-BATSE burst catalog and the Haverah Park Ultra High Energy shower set that cover approximately the same period of time.'],['1996-01-25'] +2385,['eng'],"['Peacock, J A']",['Inflationary cosmology and structure formation'],['Astrophysics and Astronomy'],"['talk, Leiden 1995/07/15', 'inflationary universe', 'field theory, scalar', 'density, fluctuation', 'Friedman model', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'gravitation, perturbation theory', 'astrophysics, galaxy', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601135'],"['These lectures cover the basics of inflationary models for the early universe, concentrating particularly on the generation of density fluctuations from scalar-field dynamics. The subsequent gravitational dynamics of these fluctuations in dark matter in a Friedmann model are described, leading to a review of the current situation in confronting inflationary models with the latest data on the clustering of galaxies and other measures of large-scale structure.']",['1996-01-25'] +2386,['eng'],"['Larsen, G B', 'Madsen, J']",['Mixed dark matter with low-mass bosons'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'boson, massive', 'massive, boson', 'neutrino, decay modes', 'decay modes, neutrino', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601134'],"['We calculate the linear power spectrum for a range of mixed dark matter (MDM) models assuming a massive (few eV) boson, \\phi, instead of a neutrino as the hot component. We consider both the case where the hot dark matter (HDM) particle is a boson and the cold component is some other unknown particle, and the case where there is only one dark matter particle, a boson, with the cold dark matter (CDM) component in a Bose condensate. Models resembling the latter type could arise from neutrino decays - we discuss some variants of this idea. The power spectra for MDM models with massive bosons are almost identical to neutrino MDM models for a given mass fraction of HDM if the bosons are distinct from their antiparticles (\\phi\\neq\\bar\\phi) and have a temperature like that of neutrinos, whereas models with \\phi=\\bar\\phi tend to overproduce small-scale structure.']",['1996-01-25'] +2387,['eng'],"['Mastichiadis, A']",['On the high energy non-thermal emission from shell-type supernova remnants'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'cosmic radiation, acceleration', 'model, shock waves', 'Compton scattering', 'energy spectrum, (electron)', '(electron), energy spectrum', 'synchrotron radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601132'],['Shock waves associated with shell type supernova remnants are considered to be possible sites of cosmic ray acceleration. Since shocks are capable of accelerating electrons in addition to protons one anticipates both species to contribute to the high energy radiation expected from these objects. Adopting a simple model for particle acceleration we calculate in a self-consistent manner the time-dependent synchrotron and inverse Compton radiation of high energy electrons assumed either to be accelerated directly by the shock wave or to be injected at high energies as secondaries from the hadronic collisions of relativistic protons with the circumstellar material. We deduce that for standard supernova parameters the TeV flux produced from neutral pion decay is about the same order as the flux expected from directly accelerated electrons.'],['1996-01-25'] +2388,['eng'],"['Bednarek, W', 'Kirk, J G', 'Mastichiadis, A']",['On the production of very high energy beamed gamma-rays in blazars'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, acceleration', 'astrophysics, galaxy', 'Compton scattering', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601131'],"['The variable flux of TeV gamma-rays detected from Mkn 421 and Mkn 501 requires the presence of high energy electrons, which could in principle produce large numbers of electron/positron pairs, leading to an electromagnetic cascade. We point out that this scenario can be avoided if electrons are accelerated to high energy rectilinearly, rather than being injected isotropically into a blob, as in most of the models of the GeV gamma-ray emission. By balancing linear acceleration by an electric field against inverse Compton losses in the radiation field of the accretion disk we calculate the emitted spectra and find the conditions which must be fulfilled in order to exclude the development of electromagnetic cascades during acceleration. Assuming these to be fulfilled, we show that the maximum possible photon energy is approximately 10M_8^{2/5}\\,TeV, where M_8 is the mass of the central black hole in units of 10^8\\,\\msolar. In addition we compute the optical depth to absorption of TeV photons on a possible isotropic scattered component and on the observed nonthermal radiation (in the case of Mkn 421) and find that TeV photons can escape provided the nonthermal X-rays originate in a jet moving with a Lorentz factor of around 8.']",['1996-01-25'] +2389,['eng'],"['Collar, J I']",['Biological effects of stellar collapse neutrinos'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'astrophysics, supernova', 'neutrino nucleus, elastic scattering', 'elastic scattering, neutrino nucleus', 'nucleus, recoil', 'biology', 'dosimetry', 'energy spectrum, recoil', 'recoil, energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505028'],"['Massive stars in their final stages of collapse radiate most of their binding energy in the form of MeV neutrinos. The recoil atoms that they produce in elastic scattering off nuclei in organic tissue create a radiation damage which is highly effective in the production of irreparable DNA harm, leading to cellular mutation, neoplasia and oncogenesis. Using a conventional model of the galaxy and of the collapse mechanism, the periodicity of nearby stellar collapses and the radiation dose are calculated. The possible contribution of this process to the paleontological record of mass extinctions is examined.']",['1995-05-08'] +2390,['eng'],"['Pina-Avelino, P']",['Genus statistics for structure formation with topological defects'],['Astrophysics and Astronomy'],"['astrophysics, string', 'topology, defect', 'statistics', 'density, perturbation', 'astrophysics, missing-mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601114'],"['We study the efficiency of genus statistics in differentiating between different models of structure formation. Simple models which reproduce the salient features of the structure seeded by topological defects are examined. We consider accretion onto static point masses, modeling slow-moving cosmic string loops or other primordial point-like sources. Filamentary structures and wakes are considered as models of the structures seeded by slow and fast moving string, respectively. Comparison is made with predictions of genus statistics for Gaussian fluctuations and with genus curves obtained by the CfA survey. A generic class of density models with wakes and filaments is found to provide results comparable or better than Gaussian models for this suite of tests.']",['1996-01-23'] +2391,['eng'],"['Jegerlehner, B', 'Neubig, F', 'Raffelt, G G']",['Neutrino oscillations and the supernova 1987A signal'],['Astrophysics and Astronomy'],"['neutrino, oscillation', 'neutrino, energy spectrum', 'energy spectrum, neutrino', 'astrophysics, supernova', 'antineutrino p, interaction', 'interaction, antineutrino p', 'antineutrino/e', 'neutrino, mass difference', 'mass difference, neutrino', 'neutrino, mixing angle', 'resonance, oscillation', 'oscillation, resonance', 'matter, effect', 'neutrino, regeneration', 'neutrino, solar', 'approximation, adiabatic', 'n, matter', 'binding energy', 'statistical analysis', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601111'],"['We study the impact of neutrino oscillations on the interpretation of the supernova (SN) 1987A neutrino signal by means of a maximum-likelihood analysis. We focus on oscillations between \\overline\\nu_e with \\overline\\nu_\\mu or \\overline\\nu_\\tau with those mixing parameters that would solve the solar neutrino problem. For the small-angle MSW solution (\\Delta m^2\\approx10^{-5}\\,\\rm eV^2, \\sin^22\\Theta_0\\approx0.006), there are no significant oscillation effects on the Kelvin-Helmholtz cooling signal; we confirm previous best-fit values for the neutron-star binding energy and average spectral \\overline\\nu_e temperature. There is only marginal overlap between the upper end of the 95.4\\% CL inferred range of \\langle E_{\\overline\\nu_e}\\rangle and the lower end of the range of theoretical predictions. Any admixture of the stiffer \\overline\\nu_\\mu spectrum by oscillations aggravates the conflict between experimentally inferred and theoretically predicted spectral properties. For mixing parameters in the neighborhood of the large-angle MSW solution (\\Delta m^2\\approx10^{-5}\\,\\rm eV^2, \\sin^22\\Theta_0\\approx0.7) the oscillations in the SN are adiabatic, but one needs to include the regeneration effect in the Earth which causes the Kamiokande and and IMB detectors to observe different \\overline\\nu_e spectra. For the solar vacuum solution (\\Delta m^2\\approx10^{-10}\\,\\rm eV^2, \\sin^22\\Theta_0\\approx1) the oscillations in the SN are nonadiabatic; vacuum oscillations take place between the SN and the detector. If either of the large-angle solutions were borne out by the upcoming round of solar neutrino experiments, one would have to conclude that the SN~1987A \\overline\\nu_\\mu and/or \\overline\\nu_e spectra had been much softer than predicted by current']",['1996-01-23'] +2392,['eng'],"['Kolb, E W', 'Riotto, A']",['Eternal annihilations of light photinos'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'postulated particle, photino', 'photino, annihilation', 'annihilation, photino', 'cascade, electromagnetic', 'helium, photofission']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601096'],['In a class of low-energy supersymmetry models the photino is a natural dark matter candidate. We investigate the effects of post-freeze-out photino annihilations which can generate electromognetic cascades and lead to photo-destruction of ^4He and subsequent overproduction of D and ^3He. We also generalize our analysis to a generic dark matter component whose relic abundance is {\\it not} determined by the cross section of the self-annihilations giving rise to electromagnetic showers.'],['1996-01-19'] +2393,['eng'],"['González-Mestres, L']",['Cosmological implications of a possible class of particles able to travel faster than light'],['Astrophysics and Astronomy'],"['talk', 'relativity theory', 'photon, velocity', 'invariance, Lorentz', 'astrophysics', 'tachyon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601090'],"['We discuss the possible cosmological implications of a class of superluminal particles, in a scenario where: a) Lorentz invariance is only an approximate property of the equations of a sector of matter; b) several critical speeds of matter in vacuum exist. The Big Bang scenario and the evolution of the very early universe, as well as large scale structure, can be strongly influenced by the new particles.']",['1996-01-18'] +2394,['eng'],"['Mannheim, P D']",['Conformal cosmology and the age of the universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'gravitation, conformal', 'astrophysics, fundamental constant', 'matter, density', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601071'],"['We show that within the cosmology associated with conformal gravity the age of the universe is given as 1/H_0, to thus overcome the current cosmological age crisis. We show that while the parameter \\Omega_{mat} = \\rho_{mat} / \\rho_C takes on all values between zero and infinity in conformal gravity, nonetheless it is of order one (but not identically equal to one) for half a Hubble time to thus naturally explain its current closeness to one without fine tuning. We show that the cosmological constant is naturally of order the energy density \\rho_{mat} of ordinary matter again without fine tuning. We compare and contrast conformal cosmology with that of the standard Friedmann cosmology.']",['1996-01-15'] +2395,['eng'],"['Sakai, N']",['Fluctuations of the gravitational constant induced by primordial bubbles'],['Astrophysics and Astronomy'],"['gravitation, fundamental constant', 'fundamental constant, fluctuation', 'inflationary universe', 'expansion, bubble', 'Brans-Dicke model', 'symmetry, O(4)']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601056'],"['We consider the classical fluctuations of the gravitational constant generated by bubbles in the inflationary universe. For extended inflation, we demonstrate numerically how and how large fluctuations are produced during bubbleexpansion. The amplitude of the fluctuations depends on the Brans-Dicke parameter \\omega: if \\omega is of the order of unity, the amplitude becomes of the order of unity within one Hubble expansion time; if \\omega is large (say, \\omega=1000), the growth rate of the fluctuations is small, but it keeps growing without freezing during inflation. We also discuss some astrophysical implications of our results.']",['1996-01-12'] +2396,['eng'],"['Jaffe, A', 'Turner, M S']",['Gamma rays and the decay of neutrinos from SN1987a'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, massive', 'massive, neutrino', 'neutrino, radiative decay', 'radiative decay, neutrino', 'neutrino, branching ratio', 'neutrino, mass', 'mass, neutrino', 'upper limit', 'neutrino, lifetime', 'lower limit', 'photon, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'counters and detectors, satellite', 'numerical calculations, interpretation of experiments', 'neutrino --> neutrino photon', 'neutrino --> neutrino positron electron photon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9601104'],"[""We calculate limits to the properties of massive, unstable neutrinos using data from gamma-ray detectors on the Pioneer Venus Orbiter Satellite; a massive neutrino emitted from SN1987A that decayed in flight and produced gamma rays would be detectable by this instruments. The lack of such a signal allows us to constrain the branching ratio to photons (\\Bg), mass (\\mnu), and radiative lifetime (\\tau_\\gamma = \\tau/\\Bg). For low mass (m-1), but their contribution to the solar abundances of \\be9, \\b10 and \\b11 is not dominant (35\\%, 30\\% and 20\\% respectively). Thus, with this LEN spectrum, GCR are {\\it not}\\ the main source of \\be9 and B in the Galaxy. The most favorable case for neutrinos, (adopting the same kind of spectrum) has E_c=20 MeV/n. Even in this case, the neutrino yields of Woosley and Weaver (1995) must to be reduced by a factor of 5 to avoid \\b11 overproduction. Furthermore, this solution leads to a high B/Be']",['1995-12-07'] +2409,['eng'],"['Salopek, D S']",['Cosmological inflation and the nature of time'],['Astrophysics and Astronomy'],"['talk', 'inflationary universe', 'time', 'relativity theory, general', 'astrophysics, superspace', 'cosmic radiation, background', 'cosmic radiation, fluctuation', 'cosmic radiation, anisotropy', 'correlation, galaxy', 'Hamilton-Jacobi equation, solution', 'spectra, perturbation', 'perturbation, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9512031'],"['Recent advances in observational cosmology are changing the way we view the nature of time. In general relativity, the freedom in choosing a time hypersurface has hampered the implementation of the theory. Fortunately, Hamilton-Jacobi theory enables one to describe all time hypersurfaces on an equal footing. Using an expansion in powers of the spatial curvature, one may solve for the wavefunctional in a semiclassical approximation. In this way, one may readily compare predictions of various inflation models with observations of microwave background anisotropies and galaxy clustering.']",['1995-12-07'] +2410,['eng'],"['Easther, R']",['An inflationary model with an exact perturbation spectrum'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'density, perturbation', 'spectra, perturbation', 'perturbation, spectra', 'potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511143'],"['We present a new, exact scalar field cosmology for which the spectrum of scalar (density) perturbations can be calculated exactly. We use this exact result to the probe the accuracy of approximate calculations of the perturbation spectrum.']",['1995-11-30'] +2411,['eng'],"['Strickland, R W', 'Schramm, David N']",['Concordance of x-ray cluster data with BBN in mixed dark matter models'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, model', 'astrophysics, cluster', 'light nucleus, production', 'production, light nucleus', 'neutrino, mass', 'mass, neutrino', 'neutrino, flux', 'flux, neutrino', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511111'],"['If the hot, X-ray emitting gas in rich clusters forms a fair sample of the universe (as in Cold Dark Matter (CDM) models), and the universe is at the critical density, \\Omega_T = 1, then the data appears to imply a baryon fraction, \\Omega_{b,x} (\\Omega_{b,x}\\equiv \\Omega_b derived from X-ray cluster data), larger than that predicted by Big Bang Nucleosynthesis (BBN). While various other systematic effects such as clumping can lower \\Omega_{b,x}, in this paper we use an elementary analysis to show that a simple admixture of Hot Dark Matter (HDM, low mass neutrinos) with CDM to yield mixed dark matter shifts \\Omega_{b,x} down so that significant overlap with \\Omega_b from BBN can occur for H_0 \\lsim 75\\;{\\rm km/sec/Mpc}, even without invoking the possible aforementioned effects. The overlap interval is slightly larger for lower mass neutrinos since fewer cluster on the scale of the hot X-ray gas. We illustrate this result quantitatively in terms of a simple isothermal model. More realistic velocity dispersion profiles, with less centrally-peaked density profiles, imply that fewer neutrinos are trapped and, thus, further increase the interval of overlap. However, we also note that if future observations of light element abundances find that \\Omega_b h^2 \\lsim 0.018, the range of concordance in this simple mixed dark matter model vanishes.']",['1996-02-22'] +2412,['eng'],"['Bludman, Sidney A']","['Solar core homology, solar neutrinos and helioseismology']",['Astrophysics and Astronomy'],"['astrophysics', 'model, solar', 'neutrino, solar', 'neutrino, flux', 'flux, neutrino', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511107'],"['Precise numerical standard solar models (SSMs) now agree with one another and with helioseismological observations in the convective and outer radiative zones. Nevertheless these models obscure how luminosity, neutrino production and g-mode core helioseismology depend on such inputs as opacity and nuclear cross sections. Although the Sun is not homologous, its inner core by itself is chemically evolved and almost homologous, because of its compactness, radiative energy transport, and ppI-dominated luminosity production. We apply luminosity-fixed homology transformations to the core to estimate theoretical uncertainties in the SSM and to obtain a broad class of non-SSMs, parametrized by central temperature and density and purely radiative energy transport in the core.']",['1995-11-23'] +2413,['eng'],"['Burrows, A', 'Hayes, J']",['Pulsar recoil and gravitational radiation due to asymmetrical stellar collapse and explosion'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'gravitational radiation', 'n, matter', 'recoil, velocity', 'neutrino, radiation', 'astrophysics, supernova', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511106'],"[""New data imply that the average velocity of radio pulsars is large \\cite{hla93}. Under the assumption that these data imply that a pulsar is born with an ``intrinsic'' kick, we investigate whether such kicks can be a consequence of asymmetrical stellar collapse and explosion. We calculate the gravitational wave (GW) signature of such asymmetries due to anisotropic neutrino radiation and mass motions. We predict that any recoils imparted to the neutron star at birth will result in a gravitational wave strain, h^{TT}_{zz}, that does not go to zero with time. Hence, there may be ``memory'' \\cite{bt87} in the gravitational waveform from a protoneutron star that is correlated with its recoil and neutrino emissions.""]",['1995-11-23'] +2414,['eng'],"['García-Bellido, J']",['Open inflation'],['Astrophysics and Astronomy'],"['talk', 'inflationary universe, open', 'cosmic radiation, background', 'temperature, anisotropy', 'tunneling', 'matter, density', 'density, perturbation', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511078'],"['Open Inflation has recently been suggested as a possible way out of the age crisis caused by observations of a large rate of expansion of the universe, in conflict with the existence of very old globular clusters. It proposes that our local patch of the universe originated in a quantum tunneling event, with the formation of a single bubble within which our universe inflated to almost flatness. I review the different models proposed together with their predictions for the amplitude of temperature anisotropies in the cosmic microwave background.']",['1995-11-17'] +2415,['eng'],"['Bergström, L']",['On self-similar global textures in an expanding universe'],['Astrophysics and Astronomy'],"['Friedman model', 'space-time, Robertson-Walker', 'astrophysics, texture', 'symmetry, O(4)', 'space-time, Minkowski', 'sigma model, nonlinear', 'field equations, solution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511064'],"['We discuss self-similar solutions to O(4) textures in Minkowski space and in flat Friedmann-Robertson-Walker backgrounds. We show that in the Minkowski case there exist no solutions with winding number greater than unity. However, we find besides the known solution with unit winding number also previously unknown solutions corresponding to winding number less than one. The validity of the non-linear sigma model approximation is discussed. We point out that no spherically symmetric exactly self-similar solutions exist for radiation or matter dominated FRW cosmologies, but we find a way to relax the assumptions of self-similarity that give us approximative solutions valid on intermediate scales.']",['1995-11-17'] +2416,['eng'],"['Liddle, A R', 'Lyth, D H', 'Schaefer, R K', 'Shafi, Qaisar', 'Viana, P T P']",['Pursuing parameters for critical density dark matter models'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'matter, density', 'spectra, perturbation', 'perturbation, spectra', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'correlation function, galaxy', 'gravitational radiation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511057'],"['We present an extensive comparison of models of structure formation with observations, based on linear and quasi-linear theory. We assume a critical matter density, and study both cold dark matter models and cold plus hot dark matter models. We explore a wide range of parameters, by varying the fraction of hot dark matter \\Omega_{\\nu}, the Hubble parameter h, the spectral index of density perturbations n, and allowing for the possibility of gravitational waves from inflation influencing large angle microwave background anisotropies. New calculations are made of the transfer functions describing the linear power spectrum, with special emphasis on improving the accuracy on short scales where there are strong constraints. For assessing early object formation, the transfer functions are explicitly evaluated at the appropriate redshift. The observations considered are microwave background anisotropies, peculiar velocity flows, the galaxy correlation function, and the abundances of galaxy clusters, quasars and damped Lyman alpha systems. Each observation is interpreted in terms of the power spectrum filtered by a top-hat window function. We find that there remains a viable region of parameter space for critical density models when all the dark matter is cold, though h must be less than 0.5 before any fit is found and n significantly below unity is preferred. Once a hot dark matter component is invoked, a wide parameter space is acceptable, including n\\simeq 1. The allowed region is characterized by \\Omega_\\nu \\la 0.30 and 0.6 \\la n \\la 1.2, at 95 per cent confidence on at least one piece of data. There is no useful lower bound on h, and for curious combinations of the other parameters it is possible to fit the data with h as high as 0.70.']",['1995-11-14'] +2417,['eng'],"['Collar, J I']","['Comments on ""Limits on dark matter using ancient mica""']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'postulated particle, WIMP', 'search for, WIMP', 'tracks, recoil', 'background', 'atomic physics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511055'],[],['1995-11-14'] +2418,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Blasi, P', 'Hnatyk, B I']",['SNI'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'model, particle source', 'astrophysics, supernova', 'magnetic field, low', 'model, shock waves', 'acceleration, hydrodynamical']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511047'],"['We propose a new mechanism for high energy gamma ray burst in Supernova type I (SNI) explosion. Presupernova is assumed to be a binary system comprised of a red giant and a white dwarf with a wind accretion. The accretion flow terminates by the accretion shock in the vicinity of the white dwarf at the distance of the order of the accretion radius. The gas inside the accretion radius constitutes the main body of a target for gamma ray production by pp collisions.\\par The supernova explosion and the shock propagation in the white dwarf result in the hydrodynamical acceleration of the outer layers of the star. The spectrum of accelerated particles is steep and the maximum energy does not exceed 1000 GeV.\\par The gamma ray burst is produced due to interaction of the accelerated particles with the gas in the binary system. Most of the photons have energies about 100 MeV, the total number of the emitted photons is between 10^{46} and 10^{47}. The gamma ray burst might have one or two precursors. The first one is produced during the shock breakout when the shock approaches the star surface and crosses it.\\par The calculations are valid in the case of a weak magnetic field. The case of strong magnetic field will be considered in part II (in preparation).']",['1996-02-22'] +2419,['eng'],"['Magueijo, J', 'Albrecht, Andreas', 'Coulson, D', 'Ferreira, P']",['Doppler peaks from active perturbations'],['Astrophysics and Astronomy'],"['astrophysics, perturbation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'topology, defect', 'causality', 'scaling', 'inflationary universe', 'coherence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511042'],"[""We examine how the qualitative structure of the Doppler peaks in the angular power spectrum of the cosmic microwave anisotropy depends on the fundamental nature of the perturbations which produced them. The formalism of Hu and Sugiyama is extended to treat models with cosmic defects. We discuss how perturbations can be ``active'' or ``passive'' and ``incoherent'' or ``coherent'', and show how causality and scale invariance play rather different roles in these various cases. We find that the existence of secondary Doppler peaks and the rough placing of the primary peak unambiguously reflect these basic properties.""]",['1996-02-22'] +2420,['eng'],"['Raffelt, G G']",['The nature of dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'search for, missing-mass', 'missing-mass, search for', 'astrophysics, galaxy', 'black hole', 'baryon, matter', 'astrophysics, fundamental constant']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511041'],"['The dynamics of the universe may be dominated by novel weakly interacting elementary particles, by baryons in an invisible form, by black holes, and globally by vacuum energy. The main arguments for and against such hypotheses are reviewed.']",['1996-02-22'] +2421,['eng'],"['García-Bellido, J', 'Wands, D']",['Metric perturbations in two-field inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time, perturbation', 'field theory, scalar', 'spectra, perturbation', 'perturbation, spectra', 'density, perturbation', 'gravitational radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9511029'],"['We study the metric perturbations produced during inflation in models with two scalar fields evolving simultaneously. In particular, we emphasize how the large-scale curvature perturbation \\zeta on fixed energy density hypersurfaces may not be conserved in general for multiple field inflation due to the presence of entropy as well as adiabatic fluctuations. We show that the usual method of solving the linearized perturbation equations is equivalent to the recently proposed analysis of Sasaki and Stewart in terms of the perturbed expansion along neighboring trajectories in field-space. In the case of a separable potential it is possible to compute in the slow-roll approximation the spectrum of density perturbations and gravitational waves at the end of inflation. In general there is an inequality between the ratio of tensor to scalar perturbations and the tilt of the gravitational wave spectrum, which becomes an equality when only adiabatic perturbations are possible and \\zeta is conserved.']",['1995-11-09'] +2422,['eng'],"['Serna, A', 'Alimi, J M']",['Constraints on the scalar-tensor theories of gravitation from primordial nucleosynthesis'],['Astrophysics and Astronomy'],"['gravitation', 'field theory, scalar', 'field theory, tensor', 'light nucleus, production', 'production, light nucleus', 'astrophysics, model', 'boundary condition', 'relativity theory, general', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510140'],"['We present a detailed calculation of the light element production in the framework of Scalar-Tensor (ST) theories of gravitation. The coupling function \\omega has been described by an appropriate form which reproduces all the possible asymptotic behaviors at early times of viable ST cosmological models with a monotonic \\omega(\\Phi). This form gives an exact representation for most of the particular theories proposed in the literature, but also a first-order approximation to many other theories. In most of ST theories, the nucleosynthesis bounds lead to cosmological models which do not significantly differ from the standard FRW ones. We have found however a particular class of ST theories where the expansion rate of the universe during nucleosynthesis can be very different from that found in GR, while the present value of \\omega is high enough to ensure compatibility with solar-system experiments. In the framework of this class of theories, right primordial abundances can be obtained for a baryon density range much wider (2.8 \\lesssim \\eta_{10} \\lesssim 58.7) than in GR. Consequently, the usual constraint on the baryon contribution to the density parameter of the universe can be drastically relaxed (0.01 \\lesssim \\Omega_{b0} \\lesssim 1.38) by considering these gravity theories. This is the first time that a ST theory is found to be compatible both with primordial nucleosynthesis and solar-system experiments while implying cosmological models significantly different from the FRW ones.']",['1996-03-12'] +2423,['eng'],"['Serna, A', 'Alimi, J M']",['Scalar-tensor cosmological models'],['Astrophysics and Astronomy'],"['astrophysics, model', 'gravitation', 'field theory, scalar', 'field theory, tensor', 'relativity theory, general', 'asymptotic behavior', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510139'],"['We analyze the qualitative behaviors of scalar-tensor cosmologies with an arbitrary monotonic \\omega(\\Phi) function. In particular, we are interested on scalar-tensor theories distinguishable at early epochs from General Relativity (GR) but leading to predictions compatible with solar-system experiments. After extending the method developed by Lorentz-Petzold and Barrow, we establish the conditions required for convergence towards GR at t\\rightarrow\\infty. Then, we obtain all the asymptotic analytical solutions at early times which are possible in the framework of these theories. The subsequent qualitative evolution, from these asymptotic solutions until their later convergence towards GR, has been then analyzed by means of numerical computations. From this analysis, we have been able to establish a classification of the different qualitative behaviors of scalar-tensor cosmological models with an arbitrary monotonic \\omega(\\Phi) function.']",['1996-03-12'] +2424,['eng'],"['Price, P B']","['Comparison of optical, radio, and acoustical detectors for ultrahigh-energy neutrinos']",['Astrophysics and Astronomy'],"['neutrino, solar', 'neutrino, cosmic radiation', 'particle identification, (neutrino)', 'Cherenkov counter, water', 'solids, water', 'counters and detectors, optical', 'counters and detectors, microwaves', 'counters and detectors, acoustic', 'photoelectron, amplifier', 'showers, electromagnetic', 'efficiency, energy dependence']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510119'],"['For electromagnetic cascades induced by electron-neutrinos in South Pole ice, the effective volume per detector element (phototube, radio antenna, or acoustic transducer) as a function of cascade energy is estimated, taking absorption and scattering into account. A comparison of the three techniques shows that the optical technique is most effective for energies below ~0.5 PeV, that the radio technique shows promise of being the most effective for higher energies, and that the acoustic method is not competitive. Due to the great transparency of ice, the event rate of AGN ne-induced cascades is an order of magnitude greater than in water. For hard source spectra, the rate of Glashow resonance events may be much greater than the rate for non-resonant energies. The radio technique will be particularly useful in the study of Glashow events and in studies of sources with very hard energy spectra.']",['1996-03-15'] +2425,['eng'],"['Hu, W', 'Sugiyama, N']",['Small scale cosmological perturbations'],['Astrophysics and Astronomy'],"['astrophysics, perturbation', 'cosmic radiation, background', 'photon, decoupling', 'decoupling, photon', 'oscillation, acoustic', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'matter, fluctuation', 'potential', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510117'],"['Through analytic techniques verified by numerical calculations, we establish general relations between the matter and cosmic microwave background (CMB) power spectra and their dependence on cosmological parameters on small scales. Fluctuations in the cosmic microwave background (CMB), baryons, cold dark matter, and neutrinos receive a boost at horizon crossing. Baryon drag on the photons causes alternating acoustic peak heights in the CMB and is uncovered in its bare form under the photon diffusion scale. Decoupling of the photons at last scattering and of the baryons at the end of the Compton drag epoch, freezes the diffusion-damped acoustic oscillations into the CMB and matter power spectra at different scales. We determine the dependence of the respective acoustic amplitudes and damping lengths on fundamental cosmological parameters. The baryonic oscillations, enhanced by the velocity overshoot effect, compete with CDM fluctuations in the present matter power spectrum. We present new {\\it exact} analytic solutions for the cold dark matter fluctuations in the presence of a growth-inhibiting radiation {\\it and} baryon background. Combined with the acoustic contributions and baryonic infall into CDM potential wells, this provides a highly accurate analytic form of the small-scale transfer function in the general case.']",['1996-03-15'] +2426,['eng'],"['Griest, K']",['The nature of the dark matter'],['Astrophysics and Astronomy'],"['lectures, Varenna 1995/07/25', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'search for, missing-mass', 'missing-mass, search for', 'astrophysics, galaxy', 'postulated particle, axion', 'sparticle, neutral particle', 'postulated particle, WIMP', 'astrophysics, MACHO', 'experimental results', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510089'],"['We review some recent determinations of the amount of dark matter on galactic and larger scales, with special attention to the dark matter in the Milky Way. We then briefly review the motivation for and basic physics of several dark matter candidates, and then go into more depth for two candidates, the neutralino from supersymmetry, and the baryonic Macho candidate. We give some motivation for supersymmetry and review neutralino detection strategies. For Machos we give a description of the discovery of Machos via gravitational microlensing and the interpretation of the results with respect to the dark matter problem.']",['1995-10-18'] +2427,['eng'],"['Cheng, K S', 'Dai, Z G']",['Conversion of neutron stars to strange stars as an origin of gamma-ray bursts'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'n, matter', 'matter, strangeness', 'energy', 'astrophysics, pulsar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510073'],['This paper argues that conversion of neutron stars to strange stars as an origin of cosmological stars in the binaries with low-mass companions. Our model may provide an explanation why the binary millisecond pulsars seem to have same low magnetic fields.'],['1995-10-16'] +2428,['eng'],"['Salopek, D S']",['The role of time in physical cosmology'],['Astrophysics and Astronomy'],"['astrophysics', 'time', 'relativity theory, general', 'Hamilton-Jacobi equation', 'cosmic radiation, background', 'correlation, galaxy', 'spectra, perturbation', 'perturbation, spectra', 'inflationary universe', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510059'],"['Recent advances in observational cosmology are changing the way we view the nature of time. In general relativity, the freedom in choosing a time hypersurface has hampered the implementation of the theory. Fortunately, Hamilton-Jacobi theory enables one to describe all time hypersurfaces on an equal footing. Using an expansion in powers of the spatial curvature, one may solve for the wavefunctional in a semiclassical approximation. In this way, one may readily compare predictions of various inflation models with observations of microwave background anisotropies and galaxy clustering.']",['1995-10-11'] +2429,['eng'],"['Kolb, E W', 'Tkachev, Igor I']",['Femtolensing and picolensing by axion miniclusters'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'postulated particle, axion', 'gravitation', 'axion, cluster', 'energy, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510043'],"[""Non-linear effects in the evolution of the axion field in the early Universe may lead to the formation of gravitationally bound clumps of axions, known as ``miniclusters.'' Minicluster masses and radii should be in the range M_{\\rm mc}\\sim10^{-12} M_\\odot and R_{\\rm mc} \\sim 10^{10}cm, and in plausible early-Universe scenarios a significant fraction of the mass density of the Universe may be in the form of axion miniclusters. If such axion miniclusters exist, they would have the physical properties required to be detected by ``femtolensing.''""]",['1995-10-09'] +2430,['eng'],"['Rezzolla, L', 'Miller, J C']",['Evaporation of cosmological quark drops and relativistic radiative transfer'],['Astrophysics and Astronomy'],"['quark, droplet', 'transition, quark hadron', 'astrophysics', 'model, hydrodynamical', 'radiation, fluid', 'relativistic', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510039'],"['We discuss the results of a full relativistic treatment of the hydrodynamics of disconnected quark regions during the final stages of the cosmological quark-hadron transition. In this study, which represents a further development of a previous analysis of the evaporation of cosmological quark drops, the effects of long range energy and momentum transfer via electromagnetically interacting particles are consistently taken into account. For this purpose, a set of relativistic Lagrangian equations describing the evolution of the strongly interacting fluids is coupled to a system of equivalent equations accounting for the hydrodynamics of the fluid of electromagnetically interacting particles. The complete set of equations has then been solved numerically and results are presented from this. The inclusion of relativistic radiative transfer produces significantly different results, with the formation of high density regions at the end of the drop evaporation being particularly relevant. A comparison is made with results obtained for the previous radiation-free model and the cosmological implications concerning baryon number concentrations are briefly discussed.']",['1995-10-09'] +2431,['eng'],"['García-Bellido, J']",['Density perturbations from quantum tunneling in open inflation'],['Astrophysics and Astronomy'],"['inflationary universe, open', 'bubble, production', 'production, bubble', 'spectra, fluctuation', 'fluctuation, spectra', 'cosmic radiation, anisotropy', 'cosmic radiation, background', 'tunneling', 'space-time, perturbation', 'amplitude analysis', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510029'],['We study the effect that quantum fluctuations produced during the nucleation of a single-bubble open inflationary universe have on the amplitude of temperature anisotropies in the cosmic microwave background. We compute the instanton action for the quantum tunneling between the false and true vacua in open inflation models and relate the amplitude of quantum fluctuations in the bubble wall to primordial curvature perturbations. We show that quantum fluctuations of the bubble wall are sensitive to the gravitational effects of the true vacuum and find the parameters of open inflation models for which their contribution to the temperature anisotropy in the microwave background can be neglected. We also study the contribution from long wavelength super-curvature modes and constrain the parameters of the models so that they do not distort the observed anisotropy.'],['1995-10-06'] +2432,['eng'],"['Moffat, J W']",['Stellar equilibrium and gravitational collapse in the nonsymmetric gravitational theory'],['Astrophysics and Astronomy'],"['gravitation, model', 'astrophysics, matter', 'field equations, solution', 'black hole']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510024'],"['We establish the formalism in the nonsymmetric gravitational theory (NGT) for stellar equilibrium and gravitational collapse. We study the collapse of a pressureless, spherically symmetric dust cloud. By assuming that the interior solution is smoothly matched at the surface of the star to the quasi-static, spherically symmetric vacuum solution, we find that the star does not collapse to a black hole. It is anticipated that the final collapsed object will reach a state of equilibrium, and will emit thermal, gravitational and other forms of radiation, although the radiation may be emitted only in small amounts if the red shift from the surface of the compact object is large. No Hawking radiation is emitted and the information loss problem can be resolved at the classical level.']",['1995-10-05'] +2433,['eng'],"['Cornish, N J', 'Levin, J J']",['Chaotic attractors for inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'field theory, scalar', 'astrophysics, model', 'fractals', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9510010'],"['In order to draw out the essential behavior of the universe, investigations of early universe cosmology often reduce the complex system to a simple integrable system. Inflationary models are of this kind as they focus on simple scalar field scenarios with correspondingly simple dynamics. However, we can be assured that the universe is crowded with many interacting fields of which the inflaton is but one. As we describe, the nonlinear nature of these interactions can result in a complex, chaotic evolution of the universe. Here we illustrate how chaotic effects can arise even in basic models such as homogeneous, isotropic universes with two scalar fields. We find inflating universes which act as chaotic attractors in the space of initial conditions. The chaotic character is reflected by the fractal border to the basin of attraction. The broader implications are likely to be felt in the process of reheating as well as in the nature of the cosmic background radiation.']",['1995-10-04'] +2434,['eng'],"['Brandenberger, R H']",['Physics of the very early universe'],['Astrophysics and Astronomy'],"['review, Florence 1995/08/06', 'astrophysics, model', 'string model', 'supersymmetry', 'astrophysics, texture', 'postulated particle, graviton', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509154'],"[""In this report of the workshop on `Physics of the Very Early Universe' held at GR14, the recent status and open problems in a selected number of major areas of interest are reviewed, focusing on attempts to develop a superstring cosmology and on progress in understanding current theories of structure formation.""]",['1995-10-02'] +2435,['eng'],"['Dodelson, S', 'Gates, E', 'Stebbins, A J']",['Cold + hot dark matter and the cosmic microwave background'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'cosmic radiation, background', 'model, adiabatic', 'neutrino, massive', 'massive, neutrino', 'potential, gravitation', 'energy, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509147'],"['We examine the cosmic microwave background power spectrum for adiabatic models with a massive neutrino component. We present the results of a detailed numerical evolution of cold + hot dark matter (CHDM) models and compare with the standard cold dark matter (CDM) spectrum. The difference is of order 5-10\\% for 400 < l < 1000 for currently popular CHDM models. With semi-analytic approximations, we also discuss the relevant physics involved. Finally we remark on the ability of future experiments to differentiate between these models. An all-sky experiment with a beam size smaller than 30 arcminutes can distinguish between CHDM and CDM if other cosmological parameters are known. Even allowing other parameters to vary, it may be possible to distinguish CDM from CHDM.']",['1995-09-29'] +2436,['eng'],"['Kofman, L A', 'Klypin, A A', 'Pogosian, D Y', 'Patrick, J']",['Mixed dark matter model in halos of clusters'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, astrophysics', 'neutrino, density', 'thermodynamics', 'astrophysics, cluster', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509145'],"['We discuss the structure of clusters in a class of flat cosmological models with the fraction of mass \\Omega_{CDM} ~0.8 in cold dark matter, and the rest in hot dark matter in the form of massive neutrinos. We consider such Cold+Hot Dark Matter (CHDM) models with one, two or three massive neutrinos, with total mass ~4.6eV. Neutrinos of such low mass cannot constitute halos of galaxies and groups, but only of clusters of galaxies. The limit on the density of neutrinos in the central parts of galaxy clusters is estimated from the phase space den- sity constraints. The ratio of the neutrino density to that of CDM through the cluster is found analytically. It appears that the density of neutrinos is suppressed within the Abell radius. However, neutrinos contribute ~20% of the mass density to the cluster halo. Our numerical simulations match analytical results. The simulations indicate that the cluster halo dark matter density profile has the power-law slope ~-2.5 which is close to that in the model with cosmological constant. We also found that in the CHDM models the velocity dispersion is almost constant across the cluster. This is quite different from the model with cosmological constant or the open model where the velocity dispersion falls in the cluster outskirts. We discuss X-ray emission and weak gravitational lensing by clusters in the model. We input the found spherically symmetrical fit to the CHDM mass density profile and the X-ray surface brightness for the cluster A2256 into simple equation of hydrostatic equilibrium of the hot gas. X-ray temperature derived this way departures from both the data and actual prediction of the model, which give almost constant temperature. We found also that the problem of high baryonic fraction in clusters is not resolved in the CHDM models.']",['1995-09-28'] +2437,['eng'],"['Moffat, J W', 'Sokolov, I Yu']",['Galaxy dynamics predictions in the nonsymmetric gravitational theory'],['Astrophysics and Astronomy'],"['gravitation, model', 'approximation, weak field', 'potential, Yukawa', 'fermion fermion, interaction', 'interaction, fermion fermion', 'exchange, one-boson', 'one-boson, exchange', 'astrophysics, galaxy', 'neutrino, mass', 'mass, neutrino', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'approximation, linear']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509143'],"['In the weak field approximation, the nonsymmetric gravitational theory (NGT) has, in addition to the Newtonian gravitational potential, a Yukawa-like potential produced by the exchange of a spin 1^+ boson between fermions. If the range r_0=\\mu^{-1} is 25 kpc, then this additional potential due to the interaction with matter in the halos of galaxies can explain the flat rotation curves of galaxies and the Tully-Fisher law (L\\sim v^4) without the dark matter hypothesis. Possible fits to clusters of galaxies and gravitational lensing observations are discussed. The results are based on a linear approximation to a new perturbatively consistent version of the NGT field equations, which does not violate the weak equivalence principle.']",['1995-09-28'] +2438,['eng'],"['Totani, T', 'Sato, K', 'Yoshii, Y']",['Spectrum of the supernova relic neutrino background and evolution of galaxies'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, background', 'neutrino, emission', 'emission, neutrino', 'neutrino, energy spectrum', 'energy spectrum, neutrino', 'astrophysics, fundamental constant', 'astrophysics, galaxy', 'astrophysics, model', 'neutrino, flux', 'flux, neutrino', 'deep underground detector, KAMIOKANDE', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509130'],"['The spectrum of the supernova relic neutrino background (SRN) from collapse-driven supernovae ever occurred in the universe is calculated by using a realistic, time-dependent supernova rate derived from a standard model of galaxy evolution based on the population synthesis method. The SRN spectrum we show here is the most realistic at present, because the largest uncertainty in previous theoretical predictions has come from unrealistic assumptions of the supernova rate so far made. The SRN is one of the targets of the Superkamiokande (SK) detector which will be constructed in a year and the SRN, if at all detected, would provide a new tool to probe the history of supernova explosions in the universe. The expected event rate at the SK is therefore calculated in this paper. Our major results include: (1) the supernova rate is much higher in the early phase of evolution of galaxies and there appears a hump in the SRN spectrum in the low-energy region of \\ltilde 5 MeV, (2) the SRN flux depends on the Hubble constant (H_0) in a way approximately proportional to H_0^2 and only weakly on the density parameter of the universe (\\Omega_0) and a cosmological constant (\\lambda_0), and (3) the plausible event rate at the SK is 1.2 yr^{-1} in the observable energy range. Such a low event rate is due mainly to a quite low supernova rate at present which is averaged over the morphological types of galaxies. The most optimistic rate in our model is found to be 4.7 yr^{-1}, and if more events are detected, we will have to reconsider our current understanding of collapse-driven supernovae and evolution of galaxies.']",['1995-09-27'] +2439,['eng'],"['Kernan, P J', 'Starkman, G D', 'Vachaspati, T']",['Big Bang Nucleosynthesis constraints on primordial magnetic fields'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'magnetic field, effect', 'electron, phase space', 'thermodynamics', 'n, density', 'weak interaction', 'temperature, time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509126'],"['We reanalyze the effect of magnetic fields in BBN, incorporating several features which were omitted in previous analyses. We find that the effects of coherent magnetic fields on the weak interaction rates and the electron thermodynamic functions (\\rhoe, \\Pe, and \\drhoedt ) are unimportant in comparison to the contribution of the magnetic field energy density in BBN. In consequence the effect of including magnetic fields in BBN is well approximated numerically by treating the additional energy density as effective neutrino number. A conservative upper bound on the primordial magnetic field, parameterized as \\zeta=2eB_{rms}/(T_\\nu^2), is \\zeta \\le 2 (\\rho_B < 0.27 \\rho_\\nu). This bound can be stronger than the conventional bound coming from the Faraday rotation measures of distant quasars if the cosmological magnetic field is generated by a causal mechanism.']",['1995-09-26'] +2440,['eng'],"['Berezinsky, Veniamin Sergeevich', 'Fiorentini, G', 'Lissia, M']",['Last hope for an astrophysical solution to the solar neutrino problem'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, solar', 'model, solar', 'neutrino, flux', 'flux, neutrino', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509116'],"['We discuss what appears the last hope for an astrophysical solution to the solar neutrino problem: a correlated variation of the astrophysical factors for the helium burning cross sections (S_{33} and S_{34}) and either S_{17} or the central temperature T_c. In this context, we recognize the important role played by the CNO neutrinos. In fact, we can obtain a fair fit to the experimental data only if three conditions are met simultaneously: the astrophysical factor S_{33} is about 200 times what is presently estimated, the astrophysical factor S_{17} is about 3 times larger and the ^{13}N and ^{15}O neutrino fluxes are negligible compared to the ones predicted by standard solar models. These conditions are not supported by the present data and their correlated combination is improbable.']",['1995-09-25'] +2441,['eng'],"['Asakimori, K']",['Energy spectra and elemental composition of nuclei above 100 TeV from a series of JACEE balloon flights'],['Astrophysics and Astronomy'],"['talk, Rome 1995/08/28', 'elements, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'nuclear emulsion, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509091'],[],['1995-09-21'] +2442,['eng'],"['Dolgov, A D']",['Problems of dark matter'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'vacuum state, energy', 'energy, density', 'astrophysics, texture', 'neutrino/tau, mass', 'mass, neutrino/tau', 'Majoron', 'light nucleus, production', 'production, light nucleus', 'matter, density', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509064'],['The data indicating existence of different forms of dark matter in the universe as well as the role of this matter in structure formation are briefly reviewed. It is argued that vacuum energy gives a dominant contribution into the total energy density of the universe. The model of structure formation with unstable tau-neutrino with MeV-mass and KeV-majoron is described.'],['1995-09-13'] +2443,['eng'],"['Dolgov, A D']",['Invisible matter'],['Astrophysics and Astronomy'],"['lectures, Zvenigorod 1995/02/21', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'baryon, density', 'gravitation, action', 'inflationary universe', 'astrophysics, texture', 'matter, density', 'astrophysics, galaxy', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509057'],"['These lectures have been given to particle physicists, mostly experimentalists and very briefly and at a pedestrian level review the problems of dark matter. The content of the lectures is the following: 1. Introduction. 2. Cosmological background. 3. Luminous matter. 4. Primordial nucleosynthesis and the total amount of baryons. 5. Gravitating invisible matter. 6. Baryonic crisis. 7. Inflationary omega. 8. Intermediate summary. 9. Possible forms of dark matter. 10. Structure formation: basic assumptions. 11. Structure formations: basics of the theory. 12. Evolution of perturbations with different forms of dark matter. 13. Conclusion. The presentation and conclusion reflects personal view of the author that a considerable amount of invisible energy in the universe is in the form of vacuum energy (cosmological constant) and possibly in the form of a classical field which adjusts vacuum energy to the value permitted and requested by astronomical data.']",['1995-09-11'] +2444,['eng'],"['Vera, R A']",['The new universe fixed by a standing wave particle model'],['Astrophysics and Astronomy'],"['particle, model', 'astrophysics, model', 'black hole', 'relativity theory, nonlocal', 'gravitation', 'quantum mechanics']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509053'],"['The theoretical properties of the black holes (BHs) and of the universe were derived from a unified relativistic theory based on a generalization of local relativity for nonlocal cases in gravitational fields and a quantized standing wave particle model that accounts for relativity, quantum mechanics and the gravitational tests (See gr-qc/9509014). They fix an isentropic and conservative steady state that is independent on an eventual universe expansion because matter also expands itself in the same proportion. The new black holes BHs resulting from linear properties of the model, after capturing enough radiation, would explode. Statistically, matter would evolve, indefinitely, in rather closed cycles between gas and BH states, and vice-versa. The expected astronomical objects and cosmic radiation backgrounds that are consistent with the observed facts. This leads to non conventional models for some celestial objects.']",['1995-09-11'] +2445,['eng'],"['Sahu, P K']",['Strange matter and its stability in presence of magnetic field'],['Astrophysics and Astronomy'],"['quark, matter', 'magnetic field, effect', 'matter, strangeness', 'low temperature expansion', 'n, matter', 'stability', 'quark, density', 'potential, chemical', 'pressure', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509041'],['We study the effect of a magnetic field on the interacting quark matter and apply to strange star. We considered the low temperature approximation to strange matter. We found that the interacting strange quark matter is less stable compare to free quark gas in presence of strong external magnetic field with zero and finite temperature. We then calculated strange star structure parameters such as mass and radius and found that the strange star is more compact for interacting quark matter than free quark matter in presence of strong magnetic field.'],['1995-09-08'] +2446,['eng'],"['Scoccimarro, R', 'Frieman, Joshua A']",['Loop corrections in non-linear cosmological perturbation theory'],['Astrophysics and Astronomy'],"['astrophysics', 'gravitation', 'density, perturbation', 'model, fluid', 'differential equations', 'perturbation theory, nonlinear', 'perturbation theory, higher-order', 'formula', 'tables', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509047'],"[""Using a diagrammatic approach to Eulerian perturbation theory, we analytically calculate the variance and skewness of the density and velocity divergence induced by gravitational evolution from Gaussian initial conditions, including corrections *beyond* leading order. Except for the power spectrum, previous calculations in cosmological perturbation theory have been confined to leading order (tree level)-we extend these to include loop corrections. For scale-free initial power spectra, the one-loop variance \\sigma^2 = \\sigma^2_l + 1.82 \\sigma^4_l and the skewness S_3 = 34/7 + 9.8 \\sigma^2_l, where \\sigma_l is the rms fluctuation of the linear density field. We also compute loop corrections to the variance, skewness, and kurtosis for several non-linear approximation schemes, where the calculation can be easily generalized to 1-point cumulants of higher order and arbitrary number of loops. We find that the Zel'dovich approximation gives the best approximation to the loop corrections of exact perturbation theory, followed by the Linear Potential approximation (LPA) and the Frozen Flow approximation (FFA), in qualitative agreement with the relative behavior of tree-level results. In LPA and FFA, loop corrections are infrared divergent for spectral indices n < 0; this is related to the breaking of Galilean invariance in these schemes.""]",['1995-09-08'] +2447,['eng'],"['Berera, A']",['Warm inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'critical phenomena', 'thermodynamics', 'scaling', 'coupling constant', 'effective potential', 'finite temperature', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509049'],"['Assuming a first order phase transition during inflation, a model scenario is described which does not require a tiny coupling constant. Thermal equilibrium is closely maintained as inflation commences. No large scale reheating is necessary. Solutions for N> 70 are found for any \\delta \\rho / \\rho in the range 10^{-5} - 10^{-3}.']",['1995-09-08'] +2448,['eng'],"['Prasanna, A R', 'Mohanty, S']",['Astrophysical signals of P and T violation by gravity'],['Astrophysics and Astronomy'],"['scattering, photon graviton', 'photon graviton, scattering', 'invariance, gauge', 'parity, violation', 'violation, parity', 'time reversal, violation', 'astrophysics, pulsar', 'relativity theory, general', 'time delay', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509025'],"[""We study the observational consequences of the leading order P and T violating gauge invariant graviton-photon interactions. Such interactions give rise to gravitational birefringence - the velocity of light signals depends upon their polarisation, which is absent in Einstein's gravity. Using experimentally established limits on the differential time delay in the radio signals from pulsars we put constraints on the magnitude of P and T violating graviton-photon couplings.""]",['1995-09-11'] +2449,['eng'],"['Shiromizu, T', 'Morikawa, M']",['Dynamics of subcritical bubbles in first order phase transition'],['Astrophysics and Astronomy'],"['electroweak interaction', 'critical phenomena, bubble', 'thermodynamics, fluctuation', 'symmetry, O(3)', 'Langevin equation', 'Higgs model', 'effective Lagrangian', 'Fokker-Planck equation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9509018'],['We derivate the Langevin and the Fokker-Planck equations for the radius of O(3)-symmetric subcritical bubbles as a phenomenological model to treat thermal fluctuation. The effect of thermal noise on subcritical bubbles is examined. We find that the fluctuation-dissipation relation holds and that in the high temperature phase the system settles down rapidly to the thermal equilibrium state even if it was in a nonequilibrium state initially. We then estimate the typical size of subcritical bubbles as well as the amplitude of fluctuations on that scale. We also discuss their implication to the electroweak phase transition.'],['1995-09-11'] +2450,['eng'],"['Brandenberger, R H']",['Formation of structure in the universe'],['Astrophysics and Astronomy'],"['lectures, Rio de Janeiro 1995/07/10', 'astrophysics, model', 'astrophysics, perturbation', 'astrophysics, galaxy', 'inflationary universe', 'topology, defect', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'temperature, fluctuation', 'astrophysics, string', 'astrophysics, texture', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'space-time, singularity', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508159'],"['An introduction to modern theories for the origin of structure in the Universe is given. After a brief review of the growth of cosmological perturbations in an expanding Universe and a summary of some important observational results, the lectures focus on the inflationary Universe scenario and on topological defect models of structure formation. A summary of the theory and current observational status of cosmic microwave background temperature fluctuations is given. The final chapter is devoted to some speculative ideas concerning the connection between cosmology and fundamental physics, in particular to ways in which the singularity problem of classical cosmology may be resolved.']",['1995-09-01'] +2451,['eng'],"['Hu, W']",['Wandering in the background'],['Astrophysics and Astronomy'],['Thesis'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508126'],"['We develop and examine the principles governing the formation of distortions in the cosmic microwave background. Distortions in the frequency or spectral distribution of the background probe the thermal history of the universe whereas those in the angular temperature distribution probe its dynamics and geometry. Stressing model independent results, we show how the microwave background can be used to extract information on the mass density, vacuum density, baryon content, radiation content, expansion rate and some aspects of structure formation in the universe. To address these issues, we systematically develop relativistic kinetic and perturbation theory addressing issues such as fluctuation representation, or gauge, normal mode analysis in an open geometry, and second order effects. Through analytic and numerical results, we construct anisotropies in a critical, open, or cosmological constant universe with adiabatic and/or isocurvature initial conditions allowing for possible early reionization. We find that anisotropy formation is a simple process governed by the Compton scattering of photons and electrons and their gravitational coupling to the other particle species in the universe.']",['1995-08-28'] +2452,['eng'],"['Piran, T']",['Towards understanding gamma-ray bursts'],['Astrophysics and Astronomy'],"['lectures', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, model', 'effect, relativistic', 'particle, acceleration', 'n, matter', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507114'],"['\\gamma-ray bursts (GRBs) have puzzled astronomers since their accidental discovery in the sixties. The BATSE detector on COMPTON-GRO satellite has been detecting GRBs for the last four years at a rate of one burst per day. Its findings has revolutionized our ideas about the nature of these objects. In this lecture I show that the simplest, most conventional and practically inevitable, interpretation of the observations is that GRBs form during the conversion of the kinetic energy of ultra-relativistic particles to radiation. The inner ``engine"" that accelerates these particles is well hidden from direct observations and its origin might remain mysterious for a long time.']",['1995-07-31'] +2453,['eng'],"['Hwang, J']",['A rigorous proof of the inflationary spectrum'],['Astrophysics and Astronomy'],"['talk, Seoul 1995/02/25', 'inflationary universe', 'density, perturbation', 'density, fluctuation', 'space-time, Robertson-Walker', 'field theory, scalar', 'gravitation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508108'],"['Fundamental formulae representing the density perturbation spectrums generated in inflationary scenarios are rigorously proved. Quantum fluctuations as initial conditions for structure generation in some inflationary era can be calculated in general scale. Thus, we could avoid the matching of the large and the small scale results at the horizon crossing epoch. This is possible because the perturbed scalar field equation in a special gauge has some remarkable nice properties. In the uniform-curvature gauge the contributions from the metric fluctuations effectively disappear in certain expansion stages, and also we can derive a simple general solution in the large scale limit.']",['1995-08-25'] +2454,['eng'],"['Bernlöhr, K']",['Low threshold particle arrays'],['Astrophysics and Astronomy'],"['talk, Heidelberg 1994/10/03', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'scintillation counter', 'energy, threshold']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508113'],"['While atmospheric Cherenkov telescopes have a small field of view and a small duty fraction, arrays of particle detectors on ground have a 1\\,sr field of view and a 100% duty fraction. On the other hand, particle detector arrays have a much higher energy threshold and an inferior hadron rejection as compared to Cherenkov telescopes. Low threshold particle detector arrays would have potential advantages over Cherenkov telescopes in the search for episodic or unexpected sources of gamma rays in the multi-TeV energy range. Ways to improve the threshold and hadron rejection of arrays are shown, based on existing technology for the timing method (with scintillator or water Cherenkov counters) and the tracking method (with tracking detectors). The performance that could be achieved is shown by examples for both methods. At mountain altitude (about 4000 m or above) an energy threshold close to 1\\,TeV could be achieved. For any significant reduction of the hadronic background by selecting muon-poor showers a muon detection area of at least 1000 m^2 is required, even for a compact array.']",['1995-08-25'] +2455,['eng'],"['Loreti, F N', 'Qian, Y Z', 'Fuller, G M', 'Balantekin, A B']",['Effects of random density fluctuations on matter-enhanced neutrino flavor transitions in supernovae and implications for supernova dynamics and nucleosynthesis'],['Astrophysics and Astronomy'],"['neutrino, oscillation', 'matter, effect', 'flavor, 2', 'density, fluctuation', 'astrophysics, supernova', 'light nucleus, production', 'production, light nucleus', 'effect, depolarization', 'depolarization, effect', 'correlation, length', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508106'],"['We calculate the effects of random density fluctuations on two-neutrino flavor transformations ({\\nu}_{\\tau(\\mu)} \\rightleftharpoons {\\nu}_e) in the post-core-bounce supernova environment. In particular, we follow numerically the flavor evolution of neutrino states propagating through a stochastic field of density fluctuations. We examine the approach to neutrino flavor depolarization, and study the effects of this phenomenon in both the early shock reheating epoch and the later r-process nucleosynthesis epoch. Our results suggest that significant fluctuation-induced neutrino flavor depolarization effects occur in these environments only when the zero-order (without density fluctautions) evolution of the neutrino states includes adiabatic propagation through resonances (mass level crossings). In the shock reheating epoch, depolarization effects from fluctuations with amplitudes larger than 0.05% of the local matter density can cause an increase in the heating rate of the material behind the shock compared to the case with no neutrino flavor transformation - but this corresponds to a significant decrease in this quantity relative to the case with adiabatic neutrino transformation. If r-process nucleosynthesis is to occur during the late stages of supernova evolution, then the requirement of neutron-rich conditions excludes a region of neutrino mass-squared difference and vacuum mixing angle (\\delta m^2,\\ \\sin^22\\theta) parameter space for neutrino flavor transformation. We find that in the presence of stochastic fluctuations, this excluded region is not significantly altered even for random fluctuations with an amplitude of 1% of the local matter density.']",['1995-08-24'] +2456,['eng'],"['Salopek, D S']",['The nature of cosmic time'],['Astrophysics and Astronomy'],"['talk, Fredericton 1995/05/25', 'astrophysics, superspace', 'time', 'wave function', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, galaxy', 'correlation function, galaxy', 'potential', 'relativity theory, general', 'density, perturbation', 'Hamilton-Jacobi equation, solution', 'inflationary universe', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508101'],"['Hamilton-Jacobi theory provides a natural starting point for a covariant description of the gravitational field. Using a spatial gradient expansion, one may solve for the phase of the wavefunction by using a line-integral in superspace. Each contour of integration corresponds to a particular choice of time-hypersurface, and each yields the same answer. In this way, one can describe all time choices simultaneously. In an interesting application to cosmology, I compute large-angle microwave background anisotropies and the galaxy-galaxy correlation function associated with the scalar and tensor fluctuations of power-law inflation.']",['1995-08-23'] +2457,['eng'],"['Plunkett, S P', 'Delaney, M', 'McBreen, B', 'Hurley, K J', ""O'Sullivan, C T""]",['A search for ultra-high energy counterparts to gamma-ray bursts'],['Astrophysics and Astronomy'],"['talk', 'cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, model', 'showers, air', 'yield, time dependence', 'cosmic radiation, flux', 'flux, cosmic radiation', 'upper limit', 'scintillation counter, plastics', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508083'],['A small air shower array operating over many years has been used to search for ultra-high energy (UHE) gamma radiation (\\geq 50 TeV) associated with gamma-ray bursts (GRBs) detected by the BATSE instrument on the Compton Gamma-Ray Observatory (CGRO). Upper limits for a one minute interval after each burst are presented for seven GRBs located with zenith angles \\theta < 20^{\\circ}. A 4.3\\sigma excess over background was observed between 10 and 20 minutes following the onset of a GRB on 11 May 1991. The confidence level that this is due to a real effect and not a background fluctuation is 99.8\\%. If this effect is real then cosmological models are excluded for this burst because of absorption of UHE gamma rays by the intergalactic radiation fields.'],['1995-08-21'] +2458,['eng'],"['Yamamoto, K', 'Bunn, E F']",['Observational tests of one-bubble open inflationary cosmological models'],['Astrophysics and Astronomy'],"['inflationary universe', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'spectra, perturbation', 'perturbation, spectra', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'density, perturbation', 'boundary condition', 'vacuum state', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508090'],"['Motivated by recent studies of the one-bubble inflationary scenario, simple open cold dark matter models are tested for consistency with cosmological observations. The initial perturbation spectrum is derived by solving for the evolution of fluctuations in an open inflationary stage. A likelihood analysis is performed for the Cosmic Microwave Background anisotropies using the two-year COBE DMR data and considering models based on both the Bunch-Davies and conformal vacua. Having normalized the perturbation spectrum to fit the COBE data, we reconsider the validity of the open model from the view point of cosmic structure formation. Open models may be severely constrained by the COBE likelihood analysis. In particular, small values of \\Omega_0 are ruled out in the Bunch-Davies case: we find that \\Omega_0\\ge 0.34 at 95\\% confidence for this model.']",['1995-08-21'] +2459,['eng'],"['Lidsey, J E', 'Liddle, A R', 'Kolb, E W', 'Copeland, E J', 'Barreiro, T', 'Abney, M']",['Reconstructing the inflaton potential'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'postulated particle, inflaton', 'potential, inflaton', 'density, perturbation', 'spectra, perturbation', 'perturbation, spectra', 'gravitational radiation', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508078'],"['We review the relation between the inflationary potential and the spectra of density (scalar) perturbations and gravitational waves (tensor perturbations) produced, with particular emphasis on the possibility of reconstructing the inflaton potential from observations. The spectra provide a potentially powerful test of the inflationary hypothesis; they are not independent but instead are linked by consistency relations reflecting their origin from a single inflationary potential. To lowest-order in a perturbation expansion there is a single, now familiar, relation between the tensor spectral index and the relative amplitude of the spectra. We demonstrate that there is an infinite hierarchy of such consistency equations, though observational difficulties suggest only the first is ever likely to be useful. We also note that since observations are expected to yield much better information on the scalars than on the tensors, it is likely to be the next-order version of this consistency equation which will be appropriate, not the lowest-order one. If inflation passes the consistency test, one can then confidently use the remaining observational information to constrain the inflationary potential, and we survey the general perturbative scheme for carrying out this procedure. Explicit expressions valid to next-lowest order in the expansion are presented. We then briefly assess the prospects for future observations reaching the quality required, and consider a simulated data set that is motivated by this outlook.']",['1995-08-18'] +2460,['eng'],"['Piran, T']",['Hydrodynamic time scales and temporal structure of GRBs'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'photon, particle source', 'flux, time variation', 'time variation, flux', 'matter, relativistic', 'model, hydrodynamical', 'model, shock waves', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508081'],"[""We calculate the hydrodynamic time scales for a spherical ultra-relativistic shell that is decelerated by the ISM and discuss the possible relation between these time scales and the observed temporal structure in \\gamma-ray bursts. We suggest that the bursts' duration is related to the deceleration time, the variability is related to the ISM inhomogeneities and precursors are related to internal shocks within the shell. Good agreement can be achieved for these quantities with reasonable, not fined tuned, astrophysical parameters. The difference between Newtonian and relativistic reverse shocks may lead to the observed bimodal distribution of bursts' durations.""]",['1995-08-18'] +2461,['eng'],"['Lima, J A S', 'Trodden, M']",['Decaying vacuum energy and deflationary cosmology in open and closed universes'],['Astrophysics and Astronomy'],"['astrophysics, model', 'energy, density', 'vacuum state, decay', 'decay, vacuum state', 'space-time, Robertson-Walker', 'matter, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508049'],"['We consider a nonsingular deflationary cosmological model with decaying vacuum energy density in universes of arbitrary spatial curvature. Irrespective of the value of k, the models are characterized by an arbitrary time scale H_I^{-1} which determines the initial temperature of the universe and the largest value of the vacuum energy density, the slow decay of which generates all the presently observed matter-energy of the universe. If H_I^{-1} is of the order of the Planck time, the models begin with the Planck temperature and the present day value of the cosmological constant satisfies \\Lambda_I/\\Lambda_0 \\simeq 10^{118} as theoretically suggested. It is also shown that all models allow a density parameter \\Omega_0 <2/3 and that the age of the universe is large enough to agree with observations even with the high value of H_0 suggested by recent measurements.']",['1995-08-10'] +2462,['eng'],"['Moessner, R']",['Statistics of peculiar velocities from cosmic strings'],['Astrophysics and Astronomy'],"['astrophysics, string', 'velocity, statistics', 'topology, defect', 'cosmic radiation, background', 'moment', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508051'],"['We calculate the probability distribution of a single component of peculiar velocities due to cosmic strings, smoothed over regions with a radius of several h^{-1} Mpc. The probability distribution is shown to be Gaussian to good accuracy, in agreement with the distribution of peculiar velocities deduced from the 1.9 Jy IRAS redshift survey. Using the normalization of parameters of the cosmic string model from CMB measurements, we show that the rms values for peculiar velocities inferred from IRAS are consistent with the cosmic string model provided that long strings have some small-scale structure.']",['1995-08-10'] +2463,['eng'],"['Schupp, B', 'Van der Bij, Jochum J']",['An axially-symmetric newtonian boson star'],['Astrophysics and Astronomy'],"['boson, matter', 'coupling, gravitation', 'gravitation, coupling', 'field equations, scalar', 'field equations, solution', 'symmetry, axial', 'mass', 'approximation, Newton', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508017'],"['A new solution to the coupled gravitational and scalar field equations for a condensed boson field is found in Newtonian approximation. The solution is axially symmetric, but not spherically symmetric. For N particles the mass of the object is given by M = Nm - 0.02298 N^3 G_N^2 m^5, to be compared with M = Nm - 0.05426 N^3 G_N^2 m^5 for the spherically symmetric case.']",['1995-08-07'] +2464,['eng'],"['Silveira, V', 'De Sousa, C M G']",['Boson star rotation'],['Astrophysics and Astronomy'],"['boson, matter', 'rotator', 'field theory, scalar', 'angular momentum', 'approximation, nonrelativistic', 'excited state', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508034'],"['Using the Newtonian approximation, we study rotating compact bosonic objects. The equations which describe stationary states with non-zero angular momentum are constructed and some numerical results are presented as examples. Limits on the applicability of the Newtonian approximation are discussed.']",['1995-08-09'] +2465,['eng'],"['Waxman, E']",['Cosmological origin for cosmic rays above 10$^{19}$ eV'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, hadronic component', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'numerical calculations, interpretation of experiments', '> 10**10 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508037'],"[""The cosmic ray spectrum at 10^{19}{\\rm eV}-10^{20}{\\rm eV}, reported by the Fly's Eye and the AGASA experiments, is shown to be consistent with a cosmological distribution of sources of protons, with a power law generation spectrum {\\rm d}\\ln N/{\\rm d}\\ln E=-2.3\\pm0.5 and energy production rate of 4.5\\pm1.5\\times10^{44}{\\rm erg}\\ {\\rm Mpc}^{-3}\\ {\\rm yr}^{-1}. The two events measured above 10^{20}{\\rm eV} are not inconsistent with this model. Verifying the existence of a ``black-body cutoff'', currently observed with low significance, would require \\sim30 observation-years with existing experiments, but only \\sim1 year with the proposed \\sim5000\\ {\\rm km}^2 detectors. For a cosmological source distribution, no anisotropy is expected in the angular distribution of events with energies up to \\sim5\\times10^{19}{\\rm eV}.""]",['1995-08-09'] +2466,['eng'],"['Dermer, C D', 'Weiler, Thomas J']",['Cosmological models of gamma-ray bursts'],['Astrophysics and Astronomy'],"['review', 'photon, cosmic radiation', 'photon, transparency', 'n, matter', 'black hole', 'astrophysics, model', 'model, fireball', 'statistics', 'neutrino, cosmic radiation', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508047'],"['We review models of cosmological gamma-ray bursts (GRBs). The statistical and \\gamma-ray transparency issues are summarized. Neutron-star and black-hole merger scenarios are described and estimates of merger rates are summarized. We review the simple fireball models for GRBs and the recent work on non-simple fireballs. Alternative cosmological models, including models where GRBs are analogs of active galactic nuclei and where they are produced by high-field, short period pulsars, are also mentioned. The value of neutrino astronomy to solve the GRB puzzle is briefly reviewed.']",['1995-08-10'] +2467,['eng'],"['Sigl, G']",['Weak interactions in supernova cores and saturation of nucleon spin fluctuations'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'weak interaction', 'nucleon, spin', 'spin, nucleon', 'spin, fluctuation', 'fluctuation, spin', 'structure function, spin', 'spin, structure function', 'sum rule', 'neutrino, interaction', 'interaction, neutrino', 'bremsstrahlung', 'axion, emission', 'emission, axion', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508046'],"['Extrapolation of perturbative nucleon spin fluctuation rates seems to suggest a strong suppression of weak interactions in supernova cores. We derive a new sum rule for the dynamical spin-density structure function which relates the spin fluctuation rate to the average nuclear interaction energy. For a bremsstrahlung like structure function profile we show that instead of strongly decreasing, the neutrino scattering cross section is roughly density independent and axion emission rates increase somewhat slower than the lowest order emissivities towards the center of a hot supernova core.']",['1995-08-10'] +2468,['eng'],"['Ng, K W', 'Speliotopoulos, A D']",['A calculation of cosmic variance in cosmic microwave background anisotropy'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation', 'inflationary universe', 'correlation function', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501088'],"['We present a theoretical calculation of the variance \\Delta C_l of the CMB anisotropy power spectrum \\langle C_l\\rangle caused by gravitational waves based on quantum field theory in an inflationary cosmology. We find that since the temporal phases of the waves are fixed and the degree of freedom of the components in C_l is limited by the gravition spin, \\Delta C_l = \\langle C_l\\rangle and {\\it does not decrease with l}. In addition, anisotropies at different scales are {\\it correlated} with a finite width. This new statistics is then applied to construct the temperature correlation function.']",['1995-01-25'] +2469,['eng'],"['Copi, C J', 'Schramm, David N', 'Turner, M S']",['Assessing big-bang nucleosynthesis'],['Astrophysics and Astronomy'],"['light nucleus, production', 'production, light nucleus', 'baryon, asymmetry', 'neutrino, flavor', 'astrophysics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508029'],"['Systematic uncertainties in the light-element abundances and their evolution make a rigorous statistical assessment difficult. However, using Bayesian methods we show that the following statement is robust: the predicted and measured abundances are consistent with 95\\% credibility only if the baryon-to-photon ratio is between 2\\times 10^{-10} and 6.5\\times 10^{-10} and the number of light neutrino species is less than 3.9. Our analysis suggests that the ^4He abundance may have been systematically underestimated.']",['1995-08-08'] +2470,['eng'],"['Hagmann, C', 'Stoeffl, W', 'Van Bibber, K', 'Daw, E J', 'Kinion, D S', 'Rosenberg, L J', 'Sikivie, P', 'Sullivan, N', 'Tanner, D B', 'Moltz, D M', 'Nezrick, F', 'Turner, M', 'Golubev, N A', 'Kravchuk, L V']",['A 2nd generation cosmic axion experiment'],['Astrophysics and Astronomy'],"['talk', 'postulated particle, axion', 'search for, axion', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'magnet, superconducting', 'superconducting, magnet', 'magnetic field, external field', 'transition, axion photon', 'Primakoff effect', 'RF system, microwaves']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9508013'],['An experiment is described to detect dark matter axions trapped in the halo of our galaxy. Galactic axions are converted into microwave photons via the Primakoff effect in a static background field provided by a superconducting magnet. The photons are collected in a high Q microwave cavity and detected by a low noise receiver. The axion mass range accessible by this experiment is 1.3-13 micro-eV. The expected sensitivity will be roughly 50 times greater than achieved by previous experiments in this mass range. The assembly of the detector is well under way at LLNL and data taking will start in mid-1995.'],['1995-08-04'] +2471,['eng'],"['Fakir, R']",['Direct detection of gravity waves through high-precision astrometry'],['Astrophysics and Astronomy'],"['talk', 'gravitational radiation, measurement', 'astrophysics, pulsar', 'n, matter', 'counters and detectors']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507112'],"[""It is generally accepted that a first ever direct detection of gravity waves would herald a new era in astronomy and in fundamental physics. Ever since the early sixties, increasingly larger human and material resources are being invested in the detection effort. Unfortunately, the gravity wave effects one has had to exploit so far are extraordinarily small and are usually very many orders of magnitude smaller than the noise involved. The detectors that are presently at the most advanced stage of development hope to register extremely rare, instantaneous longitudinal shifts that are expected to be orders of magnitude smaller than one Fermi. However, it was recently shown that gravity waves can manifest themselves through much larger effects than previously envisaged. One of these new effects is the periodic, apparent shift in a star's angular position due to a foreground gravity wave source. The comparative largeness of this effect stems from its being proportional not to the inverse of the gravity wave source's distance to the Earth, but to the inverse of its distance to the star's line of sight. In certain optimal but not unrealistic cases, the amplitude of this effect can reach the critical bar of one micro-arcsecond, thus raising the prospect that the long awaited first direct detection of gravity waves could be achieved by a high precision astrometry space mission such as GAIA.""]",['1995-07-31'] +2472,['eng'],"['Mangano, G', 'Miele, G', 'Stornaiolo, C']",['Inflaton potential reconstruction and generalized equations of state'],['Astrophysics and Astronomy'],"['inflationary universe', 'model, fluid', 'density, perturbation', 'spectra, perturbation', 'perturbation, spectra', 'postulated particle, inflaton', 'potential, inflaton', 'expansion 1/N']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507117'],"['We extend a previous analysis concerning cosmological fluids with generalized equations of state in order to study inflationary scenarios. In the framework of the slow-roll approximation we find the expressions for the perturbation parameters \\epsilon, \\eta and the density perturbation spectra in terms of the adiabatic index \\ga as a function of the universe scale factor. This connection allows to find straightforwardly \\ga corresponding, for example, to the simplest {\\it chaotic} model and to the Harrison-Zeldovich potential and shows its capability to be applied to more complicate situations. Finally, we use this description to develop a new approach to the early universe dynamics, based on a 1/N expansion, where N is the e-fold number. To this aim, we introduce a set of suitable dimensionless variables and show that at the zero-th order in 1/N, an improved slow-roll approximation is obtained.']",['1995-08-01'] +2473,['eng'],"['Sethi, S K']",['A new astrophysical constraint on radiatively decaying neutrinos'],['Astrophysics and Astronomy'],"['neutrino, radiative decay', 'radiative decay, neutrino', 'neutrino, width', 'helium, ionization', 'astrophysics, galaxy', 'neutrino, branching ratio', 'neutrino, magnetic moment', 'magnetic moment, neutrino', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507116'],"['We calculate constraints on radiatively decaying neutrinos from the recent detection of singly ionized helium in the diffuse intergalactic medium (IGM) at z \\simeq 3.3. We consider a model in which neutrinos predominantly decay into invisible relativistic particles with a rate \\tau^{-1}, and with a small branching ratio into the radiative mode. To satisfy the observation of singly ionized helium, which puts a lower bound on the number density of singly ionized helium in the IGM, we show that: for \\tau \\ga 10^{18} \\,{\\rm sec}(1 \\,{\\rm eV}/m_\\nu^2), transition moment of neutrinos \\mu_{12} is constrained to be \\le 4 \\hbox{--}8 \\times 10^{-17} \\,\\mu_{\\sc B} for 110 \\,{\\rm eV} \\la m_\\nu \\la 10 \\,{\\rm keV}. We compare this bound with other astrophysical and cosmological bounds on radiatively decaying neutrinos.']",['1995-07-31'] +2474,['eng'],"['Kaiser, D']",['Post-inflation reheating in an expanding universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'chaos', 'postulated particle, inflaton', 'decay, inflaton', 'inflaton, decay', 'resonance', 'expansion, background', 'field theory, scalar', 'particle, production', 'production, particle', 'temperature, fluctuation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507108'],"[""An analytic means of studying the resonant decay of the inflaton field is developed for the case of background expansion, H \\neq 0. It is shown that the parametric resonance in the inflaton's decay need not disappear when the expansion of the universe is taken into account, although the total number of particles produced is fewer than in the H \\simeq 0 case.""]",['1995-07-27'] +2475,['eng'],"['Frichter, G M', 'Ralston, J P', 'McKay, D W']",['On radio detection of ultra-high energy neutrinos in Antarctic ice'],['Astrophysics and Astronomy'],"['neutrino, counters and detectors', 'neutrino, cosmic radiation', 'neutrino, flux', 'flux, neutrino', 'showers, electromagnetic', 'radiation, Cherenkov', 'solids, water', 'RF system', 'deep underground detector, proposed', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507078'],"['Interactions of ultrahigh energy neutrinos of cosmological origin in large volumes of dense, radio-transparent media can be detected via coherent Cherenkov emission from accompanying electromagnetic showers. Antarctic ice meets the requirements for an efficient detection medium for a radio frequency neutrino telescope. We carefully estimate the sensitivity of realistic antennas embedded deep in the ice to 100 MHz - 1 GHz signals generated by predicted neutrino fluxes from active galactic nuclei. Our main conclusion is that a {\\it single radio receiver} can probe a \\sim 1 {\\rm km}^3 volume for events with primary energy near 2 PeV and that the total number of events registered would be roughly 200 to 400 {\\rm year}^{-1} in our most conservative estimate. An array of such receivers would increase sensitivity dramatically. A radio neutrino telescope could directly observe and test our understanding of the most powerful particle accelerators in the universe, simultaneously testing the standard theory of particle physics at unprecedented energies.']",['1995-07-21'] +2476,['eng'],"['Horváth, J E']",['Detectability of gravitational wave bursts from a class of neutron star starquake GRB models'],['Astrophysics and Astronomy'],"['n, matter', 'photon, cosmic radiation', 'gravitational radiation, measurement', 'counters and detectors', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507073'],"['A large class of gamma-ray burst (GRB) models (overwhelming until recently) involve the release of energy in a neutron star quake. Even though the extreme isotropy of the GRB sky established by the BATSE experiment has now shifted the interest to cosmological models, the former starquake scenarios are still attractive and may naturally produce a gravitational wave burst that carries most of the released energy. We discuss the prospects for detection of these high-frequency bursts by the forthcoming interferometers and spheroidal antennas, emphasizing the most recent results on the distribution and nature of GRB sources. We find that, even if the overall picture is correct, the positive detection of GRB-associated gravitational wave bursts is unlikely and therefore these events will not be a prime target for the detectors.']",['1995-07-20'] +2477,['eng'],"['Kitada, H']",['Theory of Local Times'],['Astrophysics and Astronomy'],"['astrophysics, model', 'space-time', 'axiomatic field theory', 'relativity theory', 'time', 'linear spaces, Hilbert space', 'quantum mechanics', 'fibre bundle']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9309051'],"['A model of a stationary universe is proposed. In this framework, time is defined as a local and quantum-mechanical notion in the sense that it is defined for each local and quantum-mechanical system consisting of finite number of particles. The total universe consisting of infinite number of particles has no time associated. It is a stationary bound state of the total Hamiltonian of infinite degrees of freedom. The quantum mechanics and the theory of general relativity are consistently united in this context if one uses this notion of local and quantum-mechanical time. As one of the consequences, the Einstein-Podolsky-Rosen paradox is resolved. The Hubble red-shift is explained as a consequence of general relativity which is consistent with quantum mechanics. This does not require us to argue on the beginning nor the end of the universe. The universe just exists without time. (published in Il Nuovo Cimento, Vol. 109 B, N. 3, 1994, pp. 281-302)']",['2002-03-18'] +2478,['eng'],"['Cowie, L L', 'Songaila, A']",['Astrophysical limits on the evolution of dimensionless physical constants over cosmological time'],['Astrophysics and Astronomy'],"['mass ratio, (p electron)', '(p electron), mass ratio', 'fundamental constant, fine structure', 'astrophysics, constraint', 'fundamental constant, time variation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507062'],"['We report new upper limits on any possible long-term time variation of the ratio of the electron to proton masses, (m_e/m_p), the fine-structure constant, (\\alpha), and the quantity \\alpha^2 g_p(m_e/m_p), where g_p is the proton gyromagnetic ratio. These limits are based on extremely high precision observations of H_2, Si^{3+}, C^0 and H^0 in high-redshift quasar absorption lines. They amount to 95\\% confidence ranges of (-7.6\\to 9.7) \\times 10^{-14} yr^{-1} for (m_e/m_p), (-4.6\\to 4.2)\\times 10^{-14} yr^{-1} for \\alpha\\ and (-2.2\\to 4.2) \\times 10^{-15} yr^{-1} for \\alpha^2 g_p(m_e/m_p), where the elapsed time has been computed for a cosmology with \\hnought = 75 km s^{-1} Mpc^{-1} and \\qnought = 0.5.']",['1995-07-17'] +2479,['eng'],"['Martin, A P', 'Davis, A C']",['The stability of primordial magnetic fields produced by phase transitions'],['Astrophysics and Astronomy'],"['astrophysics, model', 'critical phenomena', 'magnetic field, stability', 'thermodynamics, fluctuation', 'electric field', 'Salam-Weinberg model', 'statistical analysis']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507057'],"['Primordial magnetic fields seem to be a generic relic of phase transitions in the early universe. We consider a primordial electromagnetic field formed as a result of a second-order phase transition, and show that it is stable to thermal fluctuations in the period immediately following. We also show how such a field arises in first order phase transitions. In both cases there is a transitive electric field produced during the transition.']",['1995-07-17'] +2480,['eng'],"['Stelmach, J']",['Perturbation growth and cosmic microwave background anisotropies in the string-like matter dominated universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'temperature, correlation function', 'effect, perturbation', 'matter, string']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507049'],"[""It is well known that the \\Lambda-term is a very good candidate for the smooth component of the universe since it resolves the so-called ``\\Omega-problem'' giving, at the same time, sufficiently large age of the universe. However, the constant \\Lambda-term is not the only possibility. Some people consider the \\Lambda-term varying in time according to the law \\Lambda\\approx R^{-2}. Moreover the global texture in a closed universe and the network of cosmic strings obeying the same law of variation (\\rho\\approx R^{-2}) seem to be good candidates as well. We call the ``exotic'' form of matter scaling according to this law -- string-like matter. In the paper we discuss perturbation growth and anisotropies of the CMB in the string-like dominated universe. One can show that the perturbations cannot grow in the curvature dominated universe. Since the energy density of the string-like matter scales with the expansion in the same way as the curvature term one asserts that the perturbations cannot grow in the string-like matter dominated universe either. We find this generally accepted statement not quite correct and one of the purposes of the paper is to clear up this point. The second purpose of the paper is to check whether the eventual existence of the string-like matter may have an impact on the large-angular-scale anisotropies of the CMB. We show that such exotic matter has no effect on the value of the anisotropy amplitude \\delta T/T(theta).""]",['1995-07-14'] +2481,['eng'],"['Kaiser, D']",['Frame-independent calculation of spectral indices from inflation'],['Astrophysics and Astronomy'],"['relativity theory, general', 'field theory, scalar', 'Friedman model', 'space-time, Robertson-Walker', 'inflationary universe', 'energy, density', 'perturbation theory']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507048'],"['Spectral indices from models of inflation which incorporate a Generalized Einstein Theory (GET) gravity sector are calculated to first order in a slow-roll expansion. By quantizing a suitably- generalized measure of the intrinsic curvature perturbation, the spectral indices as calculated in the Jordan frame now match those as calculated following a conformal transformation, in the Einstein frame.']",['1995-07-13'] +2482,['eng'],"['Phillips, N G', 'Kogut, A J']",['Field ordering and energy density in texture cosmology'],['Astrophysics and Astronomy'],"['astrophysics, texture', 'energy, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'sigma model, nonlinear', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507045'],"['We use numerical simulations of the time evolution of global textures to investigate the relationship between ordering dynamics and energy density in an expanding universe. Events in which individual textures become fully wound are rare. The energy density is dominated by the more numerous partially wound configurations, with median topological charge alpha ~ 0.44. This verifies the recent supposition (Borrill et al. 1994) that such partially wound configurations should dominate the cosmic microwave background.']",['1995-07-13'] +2483,['eng'],"['Durrer, R', 'Gangui, A', 'Sakellariadou, M']",['Doppler peaks'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'plasma, oscillation', 'angular correlation', 'topology, defect', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507035'],"[""The fluctuations in the cosmic microwave background (CMB) on large angular scales (> few degrees) are caused by perturbations in the gravitational field via the Sachs--Wolfe effect. On intermediate scales, 0.1^\\circ\\lsim\\theta\\lsim 2^\\circ, the dominant contribution is due to coherent oscillations in the baryon radiation plasma before recombination. Unless the universe is reionized at some redshift z>50, these oscillations lead to the `Doppler peaks' in the angular power spectrum. In structure formation scenarios based on inflation the position of the first peak is typically at \\ell\\sim 200, with a height which is 4 -- 6 times that of the Sachs--Wolfe `plateau'. Here we present a corresponding study for perturbations induced by global textures. We find that the first Doppler peak is reduced to an amplitude comparable to that of the Sachs--Wolfe contribution, and that it is shifted to \\ell\\sim 350. We believe that our analysis can be easily extended to other types of global topological defects and general global scalar fields.""]",['1995-07-12'] +2484,['eng'],"['Pyne, T', 'Gwinn, C R', 'Birkinshaw, M', 'Eubanks, T M', 'Matsakis, D N']",['Gravitational radiation and very long baseline interferometry'],['Astrophysics and Astronomy'],"['gravitational radiation', 'time delay', 'space-time, de Sitter', 'space-time, Robertson-Walker', 'counters and detectors, interference']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507030'],"['Gravitational waves affect the observed direction of light from distant sources. At telescopes, this change in direction appears as periodic variations in the apparent positions of these sources on the sky; that is, as proper motion. A wave of a given phase, traveling in a given direction, produces a characteristic pattern of proper motions over the sky. Comparison of observed proper motions with this pattern serves to test for the presence of gravitational waves. A stochastic background of waves induces apparent proper motions with specific statistical properties, and so, may also be sought. In this paper we consider the effects of a cosmological background of gravitational radiation on astrometric observations. We derive an equation for the time delay measured by two antennae observing the same source in an Einstein-de Sitter spacetime containing gravitational radiation. We also show how to obtain similar expressions for curved Friedmann-Robertson-Walker spacetimes.']",['1995-07-11'] +2485,['eng'],"['Vidaurre, A', 'Pérez, A', 'Sivak, H D', 'Bernabeu, J', 'Ibáñez, J M']",['Neutrino pair synchrotron radiation from relativistic electrons in strong magnetic fields'],['Astrophysics and Astronomy'],"['magnetic field, external field', 'magnetic field, strong field', 'neutrino, pair production', 'pair production, neutrino', 'astrophysics, model', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507027'],"['The emissivity for the neutrino pair synchrotron radiation in strong magnetic fields has been calculated both analytically and numerically for high densities and moderate temperatures, as can be found in neutron stars. Under these conditions, the electrons are relativistic and degenerate. We give here our results in terms of an universal function of a single variable. For two different regimes of the electron gas we present a simplified calculation and compare our results to those of Kaminker et al. Agreement is found for the classical region, where many Landau levels contribute to the emissivity , but some differences arise in the quantum regime. One finds that the emissivity for neutrino pair synchrotron radiation is competitive, and can be dominant, with other neutrino processes for magnetic fields of the order B \\sim 10^{14} - 10^{15} G .This indicates the relevance of this process for some astrophysical scenarios, such as neutron stars and supernovae.']",['1995-07-10'] +2486,['eng'],"['Janka, H T', 'Keil, W', 'Raffelt, G G', 'Seckel, D']",['Nucleon spin fluctuations and the supernova emission of neutrinos and axions'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, emission', 'emission, neutrino', 'emission, axion', 'axion, emission', 'nucleon, spin', 'spin, nucleon', 'nucleon, structure function', 'neutrino nucleon, interaction', 'interaction, neutrino nucleon', 'current, axial-vector', 'multiple scattering']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507023'],"['In the hot and dense medium of a supernova (SN) core, the nucleon spins fluctuate so fast that the axial-vector neutrino opacity and the axion emissivity are expected to be significantly modified. Axions with m_a\\alt10^{-2}\\,{\\rm eV} are not excluded by SN~1987A. A substantial transfer of energy in neutrino-nucleon (\\nu N) collisions is enabled which may alter the spectra of SN neutrinos relative to calculations where energy-conserving \\nu N collisions had been assumed near the neutrinosphere.']",['1995-07-10'] +2487,['eng'],"['Sasaki, M', 'Stewart, E D']",['A general analytic formula for the spectral index of the density perturbations produced during inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'spectra, perturbation', 'perturbation, spectra', 'gravitational radiation', 'field theory, scalar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507001'],"['The standard calculation of the spectrum of density perturbations produced during inflation assumes that there is only one real dynamical degree of freedom during inflation. However, there is no reason to believe that this is actually the case. In this paper we derive general analytic formulae for the spectrum and spectral index of the density perturbations produced during inflation.']",['1995-07-04'] +2488,['eng'],"['Schaefer, R K', 'De Laix, A A']",['Gauge invariant density and temperature perturbations in the quasi-newtonian formulation'],['Astrophysics and Astronomy'],"['density, fluctuation', 'temperature, fluctuation', 'temperature, anisotropy', 'neutrino, massive', 'massive, neutrino', 'neutrino neutrino, interaction', 'interaction, neutrino neutrino', 'invariance, gauge', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'cosmic radiation, background', 'coupling, (baryon photon)', '(baryon photon), coupling', 'model, fluid', 'ionization', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507003'],"['We give an improved formalism for calculating the evolution of density fluctuations and temperature perturbations in flat universes. Our equations are general enough to treat the perturbations in collisionless relics like massive neutrinos. We find this formulation to be simpler to use than gauge dependent and other gauge--invariant formalisms. We show how to calculate temperature fluctuations (including multipole moments) and transfer functions, including the case of collisionless relics like massive neutrinos. We call this formalism ``quasi-Newtonian"" because the equations for the potential and cold matter fluctuation evolution have the same form as the Newtonian gravitational equations in an expanding space. The density fluctuation variable also has the same form inside and outside of the horizon which allows the initial conditions to be specified in a simple intuitive way. Our sample calculations demonstrate how to use these equations in cosmological models which have hot, cold, and mixed dark matter and adiabatic (isentropic) or isocurvature modes. We also give an approximation which may be used to get transfer functions quickly.']",['1995-07-04'] +2489,['eng'],"['Babu, K S', 'Schaefer, R K', 'Shafi, Qaisar']",['Cold plus hot dark matter cosmology in the light of solar and atmospheric neutrino oscillations'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, solar', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'neutrino, flavor', 'density, fluctuation', 'neutrino, mass', 'mass, neutrino', 'neutrino, interference', 'astrophysics, model', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9507006'],"[""We explore the implications of possible neutrino oscillations, as indicated by the solar and atmospheric neutrino experiments, for the cold plus hot dark matter scenario of large scale structure formation. We find that there are essentially three distinct schemes that can accommodate the oscillation data and which also allow for dark matter neutrinos. These include (i) three nearly degenerate (in mass) neutrinos, (ii) non-degenerate masses with \\nu_\\tau in the eV range, and (iii) nearly degenerate \\nu_\\mu-\\nu_\\tau pair (in the eV range), with the additional possibility that the electron neutrino is cosmologically significant. The last two schemes invoke a `sterile' neutrino which is light (< or ~ eV). We discuss the implications of these schemes for \\bar{\\nu}_\\mu - \\bar{\\nu}_e and \\nu_\\mu - \\nu_\\tau oscillation, and find that scheme (ii) in particular, predicts them to be in the observable range. As far as structure formation is concerned, we compare the one neutrino flavor case with a variety of other possibilities, including two and three degenerate neutrino flavors. We show, both analytically and numerically, the effects of these neutrino mass scenarios on the amplitude of cosmological density fluctuations. With a Hubble constant of 50 km s^{-1} Mpc^{-1}, a spectral index of unity, and \\Omega_{baryon} = 0.05, the two and three flavor scenarios fit the observational data marginally better than the single flavor scheme. However, taking account of the uncertainties in these parameters, we show that it is premature to pick a clear winner.""]",['1995-07-05'] +2490,['eng'],"['Salopek, D S']",['Characteristics of cosmic time'],['Astrophysics and Astronomy'],"['astrophysics', 'time', 'relativity theory, general', 'Hamilton-Jacobi equation', 'cosmic radiation, background', 'correlation, galaxy', 'spectra, perturbation', 'perturbation, spectra', 'inflationary universe', 'boundary condition', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506146'],"['The nature of cosmic time is illuminated using Hamilton-Jacobi theory for general relativity. For problems of interest to cosmology, one may solve for the phase of the wavefunctional by using a line integral in superspace. Each contour of integration corresponds to a particular choice of time hypersurface, and each yields the same answer. In this way, one can construct a covariant formalism where all time hypersurfaces are treated on an equal footing. Using the method of characteristics, explicit solutions for an inflationary epoch with several scalar fields are given. The theoretical predictions of double inflation are compared with recent galaxy data and large angle microwave background anisotropies.']",['1995-07-03'] +2491,['eng'],"['Davis, A C', 'Dimopoulos, K']",['Primordial magnetic fields in hybrid inflation'],['Astrophysics and Astronomy'],"['inflationary universe, hybrid', 'magnetic field, production', 'production, magnetic field', 'astrophysics, galaxy', 'correlation, length', 'critical phenomena']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506132'],"['We show that, during hybrid inflation, a primordial magnetic field can be created, sufficiently strong to seed the galactic dynamo and generate the observed galactic magnetic fields. Considering the inflaton dominated regime, our field is produced by the Higgs--field gradients, resulting from a grand unified phase transition. The evolution of the field is followed from its creation through to the epoch of structure formation, subject to the relevant constraints. We find that it is always possible to create a magnetic field of sufficient magnitude, provided the phase transition occurs during the final 15 e-foldings of the inflationary period. the achieved field can be coherent over large distances and, for some parameter space, it is strong enough to dispense with the galactic dynamo.']",['1995-06-29'] +2492,['eng'],"['Olive, Keith A', 'Scully, S T']",['Big bang nucleosynthesis'],['Astrophysics and Astronomy'],"['review', 'astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'neutrino, flavor', 'elements', 'matter, density', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506131'],"['The current status of big bang nucleosynthesis is reviewed with an emphasis on the comparison between the observational determination of the light element abundances of \\D, \\he3, \\he4 and \\li7 and the predictions from theory. In particular, we present new analyses for \\he4 and \\li7. Implications for physics beyond the standard model are also discussed. Limits on the effective number of neutrino flavors are also updated.']",['1995-06-28'] +2493,['eng'],"['Goldman, T', 'Hochberg, D', 'Laflamme, R']",['Ising model formulation of large scale dynamics'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'partition function', 'Ising model', 'gravitation', 'field theory, scalar', 'critical phenomena', 'correlation function', 'universality', 'renormalization', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506127'],"['The partition function of a system of galaxies in gravitational interaction can be cast in an Ising Model form, and this reformulated via a Hubbard--Stratonovich transformation into a three dimensional stochastic and classical scalar field theory, whose critical exponents are calculable and known. This allows one to {\\it compute\\/} the galaxy to galaxy correlation function, whose non--integer exponent is predicted to be between 1.530 and 1.862, to be compared with the phenomenological value of 1.6 to 1.8.']",['1995-06-28'] +2494,['eng'],"['Protheroe, R J', 'Johnson, P A']",['Propagation of ultra high energy protons over cosmological distances and implications for topological defect models'],['Astrophysics and Astronomy'],"['cosmic radiation, cascade', 'photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'cosmic radiation, secondary radiation', 'showers, cascade', 'photon, emission', 'emission, photon', 'neutrino, emission', 'emission, neutrino', 'topology, defect', 'transfer matrix', 'energy loss', 'magnetic field, galaxy', 'numerical calculations, Monte Carlo', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506119'],"['We describe the results of a hybrid matrix--Monte Carlo calculation of cascading of UHE cosmic rays and \\gamma-rays through the cosmic background radiation fields over cosmological distances. We calculate the \\gamma-ray and neutrino emission that results from the cascade, as well as the effect of cascading on the primary spectrum. We discuss the results for various cosmic ray injection spectra and primary species. Certain models for the production of the highest energy cosmic rays are ruled out.']",['1995-06-26'] +2495,['eng'],"['Milgrom, M', 'Usov, Yu V']",['Gamma-ray bursters as sources of cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'astrophysics, model']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506099'],"['The little we do know of the physical conditions in gamma-ray bursters makes them conducive to the acceleration of high-energy cosmic rays, especially if they are at cosmological distances. We find that, with the observed statistics and fluxes of gamma-ray bursts, cosmological bursters may be an important source of cosmic rays in two regions of the observed spectrum: 1. At the very-high-energy end (E>10^{19} eV), where cosmic rays must be of extragalactic origin. 2. Around and above the spectral feature that has been described as a bump and/or a knee, which occurs around 10^{15} eV, and starts at about 10^{14} eV. The occasional bursters that occur inside the Galaxy--about once in a few hundred thousand years if burst emission is isotropic; more often, if it is beamed--could maintain the density of galactic cosmic rays at the observed level in this range. These two energy ranges might correspond to two typical energy scales expected from bursters: one pertinent to acceleration due to interaction of a magnetized-fireball front with an ambient medium; the other to acceleration in the fireball itself (e.g. shock acceleration).']",['1995-06-20'] +2496,['eng'],"['Sigl, G', 'Lee, S', 'Schramm, David N', 'Bhattacharjee, P']",['A break in the highest energy cosmic ray spectrum'],['Astrophysics and Astronomy'],"['introductory', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'astrophysics, model', 'cosmic radiation, particle source', 'model, shock waves', 'numerical calculations, interpretation of experiments', '10**11 GeV']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506118'],"[""Recent experimental data from the Fly's Eye and the Akeno array seem to indicate significant structure in the ultrahigh energy cosmic ray spectrum above 10^{18}\\eV. A statistically significant dip has been established at about 5\\times10^{18}\\eV. In addition, each experiment observed a different superhigh energy event above 10^{20}\\eV separated from the rest of the data by about half a decade in energy. In this article we discuss what this implies for the existence or non-existence of the ``Greisen-Zatsepin-Kuz'min cutoff'', a long lasting and still open question in cosmic ray physics. This cutoff, caused by energy losses in the cosmic microwave background, is predicted to occur at a few times 10^{19}\\eV if cosmic rays are produced by shock acceleration of lower energy particles at extragalactic distances. We show that from the spectral point of view, sources nearer than a few \\Mpc are still consistent with the data at the 1\\sigma level, provided these sources accelerate particles beyond 3\\times10^{20}\\eV. However, persistence of the apparent gap in the existing data at the level of a 4 times higher total exposure would rule out a wide range of acceleration models at 98\\% C.L., whether they rely on nearby or extragalactic sources. This might hint to the existence of a ``top down'' mechanism which produces an additional hard component of ultrahigh energy particles directly, say, by decay from some higher energy scale in contrast to bottom up acceleration of charged particles. In this scenario a cutoff followed by a pronounced spectral flattening and possibly even a gap could naturally be formed.""]",['1995-06-23'] +2497,['eng'],"['Stompor, R', 'Górski, K M', 'Banday, A J']",['COBE-DMR-normalisation for inflationary flat dark matter models'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, model', 'inflationary universe', 'microwaves, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506088'],"['The two-year COBE-DMR 53 and 90 GHz sky maps, in both galactic and ecliptic coordinates, are used to determine the normalisation of inflationary universe models with a flat global geometry and adiabatic density perturbations. The appropriately normalised cold and mixed dark matter models and cosmological constant dominated, cold dark matter models, computed for a range of values of Omega_b and h, are then compared to various measures of structure in the universe. Critical density CDM models appear to be irreconcilable with observations on both large and small scales simultaneously, whereas MDM models provide a somewhat better fit to the data. Although the COBE-DMR data alone prefer a nearly critical value for the total density, low-density cosmological constant models with Omega_0 greater than or equal to 0.15 can not be rejected at a confidence level exceeding 95%. Such models may also provide a significantly better fit to the matter distribution data than critical density CDM.']",['1995-06-16'] +2498,['eng'],"['Vietri, M']",['On the acceleration of ultra high energy cosmic rays in gamma ray bursts'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, spatial distribution', 'cosmic radiation, particle source', 'model, hydrodynamical', 'cosmic radiation, acceleration', 'fireball', 'model, shock waves']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506081'],"[""UHECRs are roughly isotropic and attain very large energies, E \\gtrsim 3\\times 10^{20} \\; eV. Conventional models fail to explain both facts. I show here that acceleration of UHECRs in GRBs satisfies both observational constraints. Using M\\'esz\\'aros and Rees' (1994) model of GRBs as due to hyperrelativistic shocks, I show that the highest energies that can be attained thusly are E\\simeq 10^{20}\\;\\theta^{-5/3} n_1^{-5/6}\\; eV, explaining the energy of the Bird \\etal\\/ (1995) event even without beaming. The traditional photopion catastrophe affecting UHECR acceleration in AGNs is circumvented. An order of magnitude estimate shows that the total energy flux of UHECRs at the Earth is also correctly reproduced. A test of the model based upon the UHECRs' distribution upon the plane of the sky is briefly discussed.""]",['1995-06-14'] +2499,['eng'],"['Ma Chung Pei', 'Bertschinger, E']",['Cosmological perturbation theory in the synchronous and conformal newtonian gauges'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitation', 'perturbation theory', 'transformation, gauge', 'conservation law, energy-momentum', 'Boltzmann equation', 'Einstein equation', 'model, fluid', 'photon', 'neutrino', 'phase space', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506072'],"['This paper presents a systematic treatment of the linear theory of scalar gravitational perturbations in the synchronous gauge and the conformal Newtonian (or longitudinal) gauge. It differs from others in the literature in that we give, in both gauges, a complete discussion of all particle species that are relevant to any flat cold dark matter (CDM), hot dark matter (HDM), or CDM+HDM models (including a possible cosmological constant). The particles considered include CDM, baryons, photons, massless neutrinos, and massive neutrinos (an HDM candidate), where the CDM and baryons are treated as fluids while a detailed phase-space description is given to the photons and neutrinos. Particular care is applied to the massive neutrino component, which has been either ignored or approximated crudely in previous works. Isentropic initial conditions on super-horizon scales are derived. The coupled, linearized Boltzmann, Einstein and fluid equations that govern the evolution of the metric and density perturbations are then solved numerically in both gauges for the standard CDM model and two CDM+HDM models with neutrino mass densities \\onu=0.2 and 0.3, assuming a scale-invariant, adiabatic spectrum of primordial fluctuations. We also give the full details of the cosmic microwave background anisotropy, and present the first accurate calculations of the angular power spectra in the two CDM+HDM models including photon polarization, higher neutrino multipole moments, and helium recombination. The numerical programs for both gauges are available at http://arcturus.mit.edu/cosmics/ .']",['1995-06-12'] +2500,['eng'],"['Cucurull, L', 'Grifols, J A']","['Spin-statistics theorem, neutrinos, and big bang nucleosynthesis']",['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'helium', 'fermion, statistics', 'neutrino, thermodynamics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506040'],['We show how the ^4He-abundance in the early Universe can be used to demonstrate that macroscopic samples of neutrinos in thermal equilibrium are indeed distributed according to Fermi-Dirac statistics.'],['1995-06-07'] +2501,['eng'],"[""O'Connor-Drury, L"", 'Völk, H J', 'Berezhko, E G']",['Existence and interpretation of smooth cosmic-ray dominated shock structures in supernova remnants'],['Astrophysics and Astronomy'],"['cosmic radiation', 'astrophysics, supernova', 'model, shock waves', 'particle, acceleration']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506012'],"['Studies of energetic particle acceleration at collisionless shocks by the diffusive shock acceleration process indicate that completely smooth cosmic ray dominated shock structures are possible. The existence of these is discussed and conditions for their existence derived. It is shown that such solutions cannot dominate the evolution of supernova remnants if the particle diffusion coefficient has the expected strong momentum dependence To appear in Astronomy and Astrophysics, July 1995, vol 299 pp 222-224']",['1995-06-05'] +2502,['eng'],"['Sumiyoshi, K', 'Suzuki, H', 'Toki, H']",['Influence of the symmetry energy on the birth of neutron stars and supernova neutrinos'],['Astrophysics and Astronomy'],"['n, matter', 'astrophysics, supernova', 'neutrino, cosmic radiation', 'symmetry, energy', 'mean field approximation, relativistic', 'neutrino, flux', 'flux, neutrino', 'baryon, mass', 'mass, baryon', 'mass, density', 'density, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506024'],"[""We study the influence of the symmetry energy of the equation of state on the thermal evolution of protoneutron stars and the properties of supernova neutrinos by the numerical simulations after the protoneutron stars are formed. As for the equation of state (EOS) of nuclear matter, we take two EOS's with different symmetry energies obtained by the relativistic mean field theory. We find the symmetry energy plays the essential role on the evolution of lepton profiles and the neutrino fluxes.""]",['1995-06-06'] +2503,['eng'],"['Geddes, J', 'Quinn, T C', 'Wald, R M']",['On the injection energy distibution of ultra-high-energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'energy spectrum', 'flux, cosmic radiation', 'cosmic radiation, flux', 'p, cosmic radiation', 'astrophysics, model', 'cosmic radiation, background', 'energy loss', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506009'],"[""We investigate the injection spectrum of ultra-high-energy (>10^{15} eV) cosmic rays under the hypotheses that (1) these cosmic rays are protons and (2) the sources of these cosmic rays are extra-galactic and are homogeneously distributed in space. The most puzzling aspect of the observed ultra-high-energy cosmic ray spectrum is the apparent nonexistence of a ``Greisen cut-off'' at about 10^{19.8} eV. We show that this fact could be naturally explained if most (or all) of the cosmic rays presently observed above about 10^{19.6} eV were initially injected with energy above the Greisen cut-off. However, we find that the injection of cosmic rays above the Greisen cut-off cannot account for the observed flux below about 10^{19.6} eV unless the injection rate of these particles was enormously higher in the past, as would be the case if the injection resulted from the decay of an ultra-massive particle with lifetime of order 10^{9} yr. Even with such a rapid source evolution, the observed cosmic ray spectrum below about 10^{18.5} eV cannot be explained in this manner. However, we show that a 1/E^3 injection spectrum can account for the observed spectrum below 10^{18.5} eV}, with the steepening observed by the Fly's Eye group between 10^{17.6} eV and 10^{18.5} eV being very naturally explained by e+ - e- production effects. This latter fact lends support to the hypothesis that the cosmic rays in this energy regime are protons. However, due to e+ - e- production effects, a 1/E^3 injection spectrum cannot account for the observed flux above about 10^{18.5} eV.""]",['1995-06-02'] +2504,['eng'],"['Linde, Andrei D', 'Mezhlumian, A']",['Inflation with $\\Omega$ $\\neq$ 1'],['Astrophysics and Astronomy'],"['inflationary universe', 'matter, density', 'field theory, scalar', 'effective potential', 'tunneling', 'bubble, production', 'production, bubble', 'critical phenomena', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506017'],"['We discuss various models of inflationary universe with \\Omega \\not = 1. A homogeneous universe with \\Omega > 1 may appear due to creation of the universe ""from nothing"" in the theories where the effective potential becomes very steep at large \\phi, or in the theories where the inflaton field \\phi nonminimally couples to gravity. Inflation with \\Omega < 1 generally requires intermediate first order phase transition with the bubble formation, and with a second stage of inflation inside the bubble. It is possible to realize this scenario in the context of a theory of one scalar field, but typically it requires artificially bent effective potentials and/or nonminimal kinetic terms. It is much easier to obtain an open universe in the models involving two scalar fields. However, these models have their own specific problems. We propose three different models of this type which can describe an open homogeneous inflationary universe.']",['1995-06-05'] +2505,['eng'],"['Hannestad, S', 'Madsen, J']",['Neutrino decoupling in the early universe'],['Astrophysics and Astronomy'],"['neutrino, decoupling', 'decoupling, neutrino', 'astrophysics', 'Boltzmann equation, solution', 'neutrino, temperature']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506015'],"['A calculation of neutrino decoupling in the early Universe, including full Fermi-Dirac statistics and electron mass dependence in the weak reaction rates, is presented. We find that after decoupling, the electron neutrinos contribute 0.83\\% more to the relativistic energy density than in the standard scenario, where neutrinos are assumed not to share the heating from e^\\pm annihilation. The corresponding number for muon and tau neutrinos is 0.41\\% . This has the consequence of modifying the primordial ^4He abundance by \\Delta Y=+1.0\\times 10^{-4}, and the cosmological mass limit on light neutrinos by 0.2--0.5 eV.']",['1995-06-05'] +2506,['eng'],"['Doroshkevich, A G', 'Schneider, R J']",['Small scale CMB fluctuations as a probe of the mass of dark matter particles'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'cosmic radiation, background', 'microwaves', 'particle, mass', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505143'],"['The CMB anisotropy on arc second range is examined to test the power spectrum of perturbations in the small scale region and, in particular, to estimate the mass of dominant dark matter particles. It is shown that for the simplest evolutionary history with standard recombination, three and four beam observations could discriminate the mass of dark matter particles in the interval 0.5 KeV\\leq M_{DM}\\leq 4 KeV with an antenna beam (0.5 - 0.25) arc minute with amplitude \\approx 10^{-7}.']",['1995-06-01'] +2507,['eng'],"['Dolgov, A D', 'Pastor, S', 'Valle, José W F']",['Structure formation with a decaying MeV $\\tau$ neutrino and a keV majoron'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'postulated particle, Majoron', 'Majoron, production', 'production, Majoron', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'Majoron, radiative decay', 'radiative decay, Majoron', 'Majoron --> 2photon', 'neutrino/tau, mass', 'mass, neutrino/tau', 'neutrino/tau, decay', 'decay, neutrino/tau', 'neutrino/tau, lifetime']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9506011'],"['We consider the scenario of large scale structure formation with tau neutrino with mass in the MeV range and lifetime of order of years which decays into a massive majoron with KeV mass. The latter are the present-day cold dark matter particles. In contrast to the usual collisionless dark matter, the majorons have a relatively strong self-interaction and the picture of structure formation is rather different from the standard. The decay J \\ra \\gamma \\gamma leads to the existence of an X-ray line at E_\\gamma = m_J/2 which could be detectable. Electron and muon neutrinos are expected to be very light, as required in order to account for the solar neutrino deficit through \\ne to \\nm oscillations. Supersymmetry with spontaneously broken R parity provides a natural particle physics model for our scenario.']",['1995-06-05'] +2508,['eng'],"['Mazzitelli, F D', 'Spedalieri, F M']",['Scalar electrodynamics and primordial magnetic fields'],['Astrophysics and Astronomy'],"['inflationary universe', 'magnetic field', 'amplitude analysis', 'quantum electrodynamics, scalar', 'effective Lagrangian', 'Schwinger-DeWitt expansion', 'leading logarithm approximation', 'field theory, conformal']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505140'],"['A primordial magnetic field may be generated during an inflationary period if conformal invariance is broken. We reexamine and generalize previous results about the magnetic field produced by couplings of the form R^n F_{\\mu\\nu}F^{\\mu\\nu}. We show that the amplitude of the magnetic field depends strongly on n. For adequate values of n the field produced can serve as seed for galactic magnetic fields. We also compute the effective interaction between the electromagnetic field and the geometry in the context of scalar QED (with and without classical conformal invariance). In both cases, the amplitude of the magnetic field is too small to be of astrophysical interest.']",['1995-05-31'] +2509,['eng'],"['Kirk, J G', 'Duffy, P', 'Ball, L']",['Radio supernovae as TeV gamma-ray sources'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'photon, cosmic radiation', 'particle source', 'astrophysics, acceleration', 'model, shock waves']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411084'],"['When applied to the blast wave formed by the explosion of a massive star as a supernova (SN), the theory of diffusive particle acceleration at shock fronts predicts a very high energy density in cosmic rays. Almost immediately after particles begin to be injected into the process, the cosmic ray pressure rises until comparable to the ram-pressure encountered by the shock front. Those supernovae which are observed in the radio band i.e., radio supernovae (RSNe), provide direct evidence of particle acceleration in the form of synchrotron emitting electrons. Furthermore, these objects are particularly interesting, since they are usually surrounded by a relatively dense confining medium. The acceleration of cosmic rays can then lead to the production of very high energy (VHE) gamma-rays which arise from collisions between energetic particles and target nuclei. We estimate the cosmic ray energy density assuming a fraction \\phi\\lesim1 of the energy available at the shock front is converted into cosmic rays. Combining this with the parameters describing the environment of the SN progenitor, as deduced from observations, and from more detailed modelling, we compute the flux at Earth \\tevflux of photons of energy above 1\\,TeV. For the relatively weak but nearby supernova SN1987A we predict \\tevflux=2\\times10^{-13}\\,\\fluxunits before the shock front encounters the ring of dense matter seen by the Hubble Space Telescope. Subsequently, the flux is expected to rise further. The medium around SN1993J in M81 is thought to have a density']",['1994-11-22'] +2510,['eng'],"['Beatty, J J', 'Bower, C', 'Chaput, C', 'Coutu, S', 'De Nolfo, G A', 'Ficenec, D', 'Knapp, J', 'Lowder, D M', 'McKee, S', 'Müller, D', 'Musser, J A', 'Nutter, S L', 'Schneider, E', 'Swordy, S P', 'Tang, K K', 'Tarlé, G', 'Tomasch, A D']",['Cosmic ray positrons at high energies'],['Astrophysics and Astronomy'],"['positron, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'ratio, (positron electron)', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'magnetic spectrometer, experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505141'],"['We present a new measurement of the cosmic-ray positron fraction e+/(e+ + e-) obtained from the first balloon flight of the High Energy Antimatter Telescope (HEAT). Using a magnet spectrometer combined with a transition radiation detector, an electromagnetic calorimeter, and time-of-flight counters we have achieved a high degree of background rejection. Our results do not indicate a major contribution to the positron flux from primary sources. In particular, we see no evidence for the significant rise in the positron fraction at energies above ~10 GeV previously reported.']",['1995-05-31'] +2511,['eng'],"['Robinson, J', 'Albrecht, Andreas']",['A statistic for identifying cosmic string wakes and other sheet-like structure'],['Astrophysics and Astronomy'],"['astrophysics, string', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, model', 'statistics', 'spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505123'],"['We describe a flatness statistic which quantifies the sheet-like nature of a distribution of matter, and which does a better job at this than other statistics discussed in the literature. We test our statistic on a toy model describing cosmic string wakes. We conclude that the most favoured cosmic string model is unlikely to produce a significant increase in the sheet-like nature of the matter distribution beyond that which occurs in Gaussian models (with the same power spectrum) due to the formation of Zeldovich pancakes. Although the statistic was developed in the context of cosmic string wake formation, we expect it to be useful for comparing the observed galaxy distribution with a wide range of theoretical models with different power spectra.']",['1995-05-29'] +2512,['eng'],"['Kephart, T W', 'Weiler, Thomas J']",['Magnetic monopoles as the highest energy cosmic ray primaries'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'relativistic', 'mass, magnetic monopole', 'magnetic monopole, mass', 'cosmic radiation, flux', 'flux, cosmic radiation', 'magnetic field, galaxy', 'showers, air', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505134'],"['We suggest that the highest energy \\gsim 10^{20} eV cosmic ray primaries may be relativistic magnetic monopoles. Motivations for this hypothesis are that conventional primaries are problematic, while monopoles are naturally accelerated to E \\sim 10^{20} eV by galactic magnetic fields. By matching the cosmic monopole production mechanism to the observed highest energy cosmic ray flux we estimate the monopole mass to be \\sim 10^{10\\pm1} GeV.']",['1995-05-30'] +2513,['eng'],"['Polarski, D', 'Starobinsky, A A']",['Structure of primordial gravitational waves spectrum in a double inflationary model'],['Astrophysics and Astronomy'],"['inflationary universe', 'gravitational radiation', 'field theory, scalar', 'cosmic radiation, background', 'temperature, fluctuation', 'perturbation, adiabatic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505125'],"['The gravitational waves (GW) background generated in a double inflationary model, with two scalar fields mutually interacting through gravity only, and its relative contribution T/S to large-angle temperature fluctuations of the relic microwave background are investigated in detail. The relation between T/S and the slope of the GW spectrum n_T is shown to be a discriminative test between a slow-roll inflation driven by one scalar field and more complicated models. It is found that the GW amplitude is not exactly zero in minima of spectral oscillations, this property being an observational, in principle, manifestation of GW being in a squeezed vacuum state during inflation.']",['1995-05-29'] +2514,['eng'],"['Crittenden, R G', 'Turok, Neil G']",['The Doppler peaks from cosmic texture'],['Astrophysics and Astronomy'],"['astrophysics, texture', 'cosmic radiation, background', 'temperature, anisotropy', 'fluctuation, adiabatic', 'baryon, fluid', 'inflationary universe', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505120'],"[""We compute the angular power spectrum of temperature anisotropies on the microwave sky in the cosmic texture theory, with standard recombination assumed. The spectrum shows `Doppler' peaks analogous to those in scenarios based on primordial adiabatic fluctuations such as `standard CDM', but at quite different angular scales. There appear to be excellent prospects for using this as a discriminant between inflationary and cosmic defect theories.""]",['1995-05-26'] +2515,['eng'],"['González-Mestres, L']",['Properties of a possible class of particles able to travel faster than light'],['Astrophysics and Astronomy'],"['talk', 'invariance, Lorentz', 'photon, velocity', 'space-time', 'relativity theory', 'vacuum state', 'particle, density', 'particle, velocity', 'postulated particle, tachyon']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505117'],"['The apparent Lorentz invariance of the laws of physics does not imply that space-time is indeed minkowskian. Matter made of solutions of Lorentz-invariant equations would feel a relativistic space-time even if the actual space-time had a quite different geometry (i.e. a galilean space-time). A typical example is provided by sine-Gordon solitons in a galilean world. A ""sub-world"" restricted to such solitons would be ""relativistic"", with the critical speed of solitons playing the role of the speed of light. Only the study of the deep structure of matter will unravel the actual geometry of space and time which we expect to be scale-dependent and determined by the properties of matter itself. If Lorentz invariance is a property of equations describing a sector of matter at a given scale, an absolute frame (the ""vacuum rest frame"") may exist without contradicting the minkowskian sctructure of the space-time felt by ordinary particles. But c, the speed of light, will not necessarily be the only critical speed in vacuum: for instance, a superluminal sector of matter may exist related to new degrees of freedom not yet discovered experimentally. Such particles would not be tachyons: they may feel a different minkowskian space-time with a critical speed larger than c and behave kinematically like ordinary particles apart from the difference in critical speed. At speed larger than c , they are expected to release ""Cherenkov"" radiation (ordinary particles) in vacuum. We present a discussion of possible physical (theoretical experimental) and cosmological implications of such a scenario, assuming that the superluminal sector couples weakly to ordinary matter.']",['1995-05-26'] +2516,['eng'],"['Turner, M S']",['Inflation'],['Astrophysics and Astronomy'],"['talk, Munich 1994/12/12', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9703194'],"['Alan Guth introduced cosmologists to inflation at the 1980 Texas Symposium. Since, inflation has had almost as much impact on cosmology as the big-bang model itself. However, unlike the big-bang model, it has little observational support. Hopefully, that situation is about to change as a variety and abundance of data begin to test inflation in a significant way. The observations that are putting inflation to test involve the formation of structure in the Universe, especially measurements of the anisotropy of the cosmic background radiation. The cold dark matter models of structure formation motivated by inflation are holding up well as the observational tests become sharper. In the next decade inflation will be tested even more significantly, with more precise measurements of CBR anisotropy, the mean density of the Universe, the Hubble constant, and the distribution of matter, as well as sensitive searches for the nonbaryonic dark matter predicted to exist by inflation. As an optimist I believe that we may be well on our way to a standard cosmology that includes inflation and extends back to around 10^{-32} sec, providing an important window on the earliest moments and fundamental physics.']",['1997-03-31'] +2517,['eng'],"['Dyer, C C', 'Marleau, F R']","['Complete model of a self-gravitating cosmic string; 1, a new class of exact solutions and gravitational lensing']",['Astrophysics and Astronomy'],"['astrophysics, string', 'symmetry breaking, U(1)', 'Einstein equation, solution', 'gauge field theory, U(1)', 'field theory, scalar', 'Higgs model', 'gravitation, lens', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411087'],"[""We find solutions of Einstein's field equation for topologically stable strings associated with the breaking of a U(1) symmetry. Strings form in many GUTs and are expected whenever the homotopy group \\Pi_1(M_0) is non-trivial. The behavior of the fields making up the string is described by the Euler-Lagrange equations. These fields appear in the energy-momentum tensor so we must solve simultaneously for the coupled Einstein-scalar-gauge field equations. Numerical results are obtained using a Taylor-series method. We obtain a 5-parameter family of solutions and discuss their physical characteristics. Significant gravitational lensing can occur due to strings based on this model and are shown for different solutions. Finally, we prove that the assumption of regularity at the string axis is not necessary by looking at the physical properties of the string solutions.""]",['1994-11-22'] +2518,['eng'],"['Waxman, E']",['Cosmological gamma ray bursts and the highest energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, primary', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'flux, cosmic radiation', 'cosmic radiation, flux', 'energy spectrum', 'p, acceleration', 'astrophysics, model']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505082'],"[""We discuss a scenario in which the highest energy cosmic rays (CR's) and cosmological \\gamma-ray bursts (GRB's) have a common origin. This scenario is consistent with the observed CR flux above 10^{20}\\text{eV}, provided that each burst produces similar energies in \\gamma-rays and in CR's above 10^{20}\\text{eV}. Protons may be accelerated by Fermi's mechanism to energies \\sim10^{20}\\text{eV} in a dissipative, ultra-relativistic wind, with luminosity and Lorentz factor high enough to produce a GRB. For a homogeneous GRB distribution, this scenario predicts an isotropic, time-independent CR flux.""]",['1995-05-18'] +2519,['eng'],"['Ghizzardi, S', 'Bonometto, S A']",['Phase-space distribution of volatile dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'fermion, statistics', 'kinematics, phase space', 'numerical calculations', 'neutrino/tau, decay modes', 'decay modes, neutrino/tau', 'neutrino/tau, lifetime', 'neutrino/mu, emission', 'emission, neutrino/mu', 'momentum spectrum, (neutrino/mu)', 'neutrino/mu, mass', 'mass, neutrino/mu', 'neutrino/tau --> scalar particle neutrino/mu']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505076'],"['We discuss the phase--space distribution of \\mu neutrinos if \\tau neutrinos are unstable and decay into \\nu_\\mu + scalar. If this scalar is a familon or a Majoron, in the generic case the \\nu_\\mu background is NOT the straightforward overlap of neutrinos of thermal and decay origins. A delay in \\nu_\\tau decay, due to the Pauli exclusion principle, can modify it in a significant way. We provide the equations to calculate the \\nu_\\mu distribution and show that, in some cases, there exists a good approximate solution to them. However, even when such solution is not admitted, the equations can be numerically solved following a precise pattern. We give such a solution for a number of typical cases. If \\nu_\\mu has a mass \\sim 2 eV and the see--saw argument holds, \\nu_\\tau must be unstable and the decay into \\nu_\\mu + scalar is a reasonable possibility. The picture leads to a delayed equivalence redshift, which could allow to reconcile COBE data with a bias parameter b\\ge 1.']",['1995-05-18'] +2520,['eng'],"['Cervantes-Cota, J L', 'Dehnen, H']",['Induced gravity inflation in the standard model of particle physics'],['Astrophysics and Astronomy'],"['electroweak interaction', 'gravitation, induced', 'Friedman model', 'Higgs particle, mass', 'mass, Higgs particle', 'Higgs particle, oscillation', 'inflationary universe', 'chaos', 'density, perturbation', 'boundary condition', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505069'],"['We are considering the cosmological consequences of an induced gravity theory coupled to the minimal standard model of particle physics. The non-minimal coupling parameter between gravity and the Higgs field must then be very large, yielding some new cosmological consequences for the early Universe and new constraints on the Higgs mass. As an outcome, new inflation is only possible for very special initial conditions producing first a short contraction era after which an inflationary expansion automatically follows; a chaotic inflationary scenario is successfully achieved. The contrast of density perturbations required to explain the seed of astronomic structures are obtained for very large values of the Higgs mass (M_{H} >> G_{F}^{-1/2}), otherwise the perturbations have a small amplitude; in any case, the spectral index of scalar perturbations agrees with the observed one.']",['1995-05-17'] +2521,['eng'],"['Ostriker, J P', 'Steinhardt, Paul Joseph']",['Cosmic concordance'],['Astrophysics and Astronomy'],"['astrophysics, model', 'matter, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'moment, multipole', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505066'],"['Observational constraints guide one forcefully to examine models in which the matter density is substantially less than critical density. Particularly noteworthy are those which are consistent with inflation. For these models, microwave background anisotropy, large-scale structure measurements, direct measurements of the Hubble constant, H_0, and the closure parameter, \\Omega_{\\rm Matter}, ages of stars and a host of more minor facts are all consistent with a spatially flat model having significant cosmological constant \\Omega_{\\Lambda} = 0.65 \\pm 0.1, \\Omega_{\\rm Matter} = 1 - \\Omega_{\\Lambda} (in the form of ``cold dark matter"") and a small tilt: 0.8< n < 1.2. (Read comments at top of file to find out how to obtain figures.)']",['1995-05-16'] +2522,['eng'],"['Frieman, Joshua A', 'Hill, Christopher T', 'Stebbins, A J', 'Waga, I']",['Cosmology with ultra-light pseudo-Nambu-Goldstone bosons'],['Astrophysics and Astronomy'],"['astrophysics, model', 'symmetry, spontaneously broken', 'Goldstone particle, mass', 'mass, Goldstone particle', 'matter, density', 'astrophysics, fundamental constant', 'vacuum state', 'energy, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505060'],"['We explore the cosmological implications of an ultra-light pseudo-Nambu-Goldstone boson. With global spontaneous symmetry breaking scale f \\simeq 10^{18} GeV and explicit breaking scale comparable to MSW neutrino masses, M \\sim 10^{-3} eV, such a field, which acquires a mass m_\\phi \\sim M^2/f \\sim H_0, would have become dynamical at recent epochs and currently dominate the energy density of the universe. The field acts as an effective cosmological constant for several expansion times and then relaxes into a condensate of coherent non-relativistic bosons. Such a model can reconcile dynamical estimates of the density parameter, \\Omega_m \\sim 0.2, with a spatially flat universe, and can yield an expansion age H_0 t_0 \\simeq 1 while remaining consistent with limits from gravitational lens statistics.']",['1995-05-15'] +2523,['eng'],"['Collar, J I', 'Avignone, F T']",['Surface sputtering from cold dark matter interactions'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'elastic scattering, nucleus WIMP', 'recoil', 'energy spectrum, time variation', 'neutrino, Dirac', 'atom, yield', 'dependence, mass number', 'numerical calculations, Monte Carlo', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505058'],['Nuclear recoil cascades induced by Cold Dark Matter (CDM) elastic scattering can produce the ejection of target atoms from solid surfaces. We calculate the yield and energy distribution of these sputtered atoms in a variety of materials. These parameters would suffer a large diurnal modulation induced by the rotation of the Earth and its motion through the galactic halo. Schemes for the detection of this unique CDM signature are proposed.'],['1995-05-15'] +2524,['eng'],"['Collar, J I', 'Avignone, F T']",['Nuclear tracks from cold dark matter interactions in mineral crystals'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'nucleus, elastic scattering', 'elastic scattering, nucleus', 'crystal', 'tracks', 'postulated particle, WIMP', 'particle identification, WIMP', 'energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505055'],"['Recoiling nuclei from Cold Dark Matter (CDM) elastic scattering interactions with the constituent elements of some minerals may produce etchable damage tracks in the crystal structure. Present calculations show that in muscovite mica, CDM tracks from recoiling potassium atoms could be readily distinguished from others due to alpha-decays in the uranium and thorium chains. Under favorable conditions, this technique could greatly improve the existing limits on Weakly Interacting Massive Particles as the constituents of the galactic halo.']",['1995-05-12'] +2525,['eng'],"['Hu, W', 'Scott, D', 'Sugiyama, N', 'White, M']",['The effect of physical assumptions on the calculation of microwave background anisotropies'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'Boltzmann equation, solution', 'photon, temperature', 'neutrino, flavor', 'effect, recombination', 'neutrino, fluctuation', 'polarization', 'gravitational radiation', 'ionization', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505043'],"['As the data on CMB anisotropies improve and potential cosmological applications are realized, it will be increasingly important for theoretical calculations to be as accurate as possible. All modern calculations for inflationary-inspired fluctuations involve the numerical solution of coupled Boltzmann equations. There are many assumptions and choices to be made when carrying out such calculations. We go through each in turn, pointing out the best selections to make, and the level of inaccuracy expected through incorrect choice: (1) neglecting the effects of neutrinos or polarization has a 10% effect; (2) varying radiation temperature and He fraction can have smaller, but noticeable effects; (3) numerical issues, such as k-range and smoothing are discussed; (4) short-cut methods, e.g. free-streaming and tilt approximations, are generally inadequate at the few % level; (5) at the 1% level somewhat baroque effects are important, such as He recombination and even minimal reionization; (6) at smaller angular scales there are secondary effects which will ultimately have to be considered. Extracting information from the subsidiary acoustic peaks and the damping region will be an extremely challenging problem. However, given the prospect of measuring just such information on the sky, it will be important to meet this challenge. In principle we can obtain details about reionization history, neutrino contribution, helium abundance, non-power-law initial conditions etc.']",['1995-05-10'] +2526,['eng'],"['Gasperini, M', 'Giovannini, M', 'Veneziano, Gabriele']",['Electromagnetic origin of the CMB anisotropy in string cosmology'],['Astrophysics and Astronomy'],"['inflationary universe', 'string model', 'electromagnetic field', 'vacuum state, fluctuation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'spectra, perturbation', 'perturbation, spectra', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505041'],"['In the inflationary scenarios suggested by string theory, the vacuum fluctuations of the electromagnetic field can be amplified by the time-evolution of the dilaton background, and can grow large enough to explain both the origin of the cosmic magnetic fields and of the observed CMB anisotropy. The normalization of the perturbation spectrum is fixed, and implies a relation between the perturbation amplitude at the COBE scale and the spectral index n. Working within a generic two-parameter family of backgrounds, a large scale anisotropy \\Delta T/T\\simeq 10^{-5} is found to correspond to a spectral index in the range n\\simeq 1.11 - 1.17.']",['1995-05-10'] +2527,['eng'],"['Janka, H T']",['Neutrinos from SN 1987A'],['Astrophysics and Astronomy'],"['talk, Tegernsee 1995/03/06', 'astrophysics, supernova', 'neutrino, astrophysics', 'critical phenomena', 'n, matter', 'potential, chemical', 'baryon, density', 'numerical calculations, interpretation of experiments', 'deep underground detector, KAMIOKANDE']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505034'],"['The neutrino signal from SN~1987A provides an excellent opportunity to constrain physical theories for matter at extreme conditions and properties of particles that are produced in supernova (SN) cores. Phase transitions in the supranuclear equation of state (EOS) may change the cooling history of the collapsed stellar core and may even lead to a collapse of the protoneutron star to a black hole on a time scale of several seconds. The implications of such a scenario for the characteristics of the neutrino emission are tested. Moreover, the consequences of a reduction of the neutrino opacities by a possible suppression of the axial-vector interaction in a dense medium (Raffelt and Seckel 1994) are investigated. Since the strongest constraints from SN~1987A for the considered theories rely on the signal duration marked by the last three events in Kamiokande, we also discuss attempts to explain these events different from the standard protoneutron star cooling scenario. In particular, attention is focussed on the scenario of a rapid cooling of the protoneutron star within the time interval of the first 8 Kamiokande events or the IMB signal which is only about 2--5\\,{\\rm s}. Such a short neutrino emission could be the consequence of low neutrino opacities or convectively enhanced neutrino transport. Since the driving force of neutrino heating around the protoneutron star diminishes, the pressure support of the overlying material decreases and some matter might fall back to the neutron star. However, analytical estimates and numerical simulations indicate that the neutrino emission associated with the accretion of this material is hardly energetic enough to account for the last bunch of neutrinos at Kamiokande.']",['1995-05-08'] +2528,['eng'],"['Nazin, S N', 'Postnov, K A']",['Gravitational radiation during Thorne-Zytkow object formation'],['Astrophysics and Astronomy'],"['gravitational radiation, multipole', 'n, matter', 'relativity theory, general', 'model, hydrodynamical', 'spectra, density', 'density, spectra', 'counters and detectors', 'interference, laser', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505025'],"['Calculation of gravitational radiation during binary inspiral leading to possible formation of a Thorne-Zytkow (TZ) object (a neutron star inside a supergiant core) is performed. The calculations were done for polytropic density distributions with different indeces n, as well as for realistic models of supergiants. A maximum frequency of the emitted gravitational waves during this process was found to range from a few to 300 initial keplerian orbital frequensies, that is from 10^{-5} to \\sim 0.1 Hz, depending on the model. A dimensionless strain metric amplitude can reach h\\sim 10^{-23.5} for a source lying 10 kpc away from the Sun. We conclude that TZ objects forming at a rate of 1 per 500 yrs in the Galaxy could be potential astrophysical targets for space laser intereferometers. Analysis of gravitational waveforms emitted during TZ-object formation could bring a unique information about stellar structure.']",['1995-05-08'] +2529,['eng'],"['Albrecht, Andreas', 'Coulson, D', 'Ferreira, P', 'Magueijo, J']",['Causality and the microwave background'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'topology, defect', 'cosmic radiation, fluctuation', 'astrophysics, string', 'spectra, perturbation', 'perturbation, spectra', 'causality', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505030'],"[""Modern experiments are producing a growing body of data on the cosmic microwave background (CMB). These photons last scattered when the universe was a fraction of its present age, allowing us to explore deep into the history of the universe. Theories abound with which to confront this data, and the challenge is to maximize the impact of the data on our understanding. The origin of fluctuations observed in the CMB may be due to ``defects'' such as cosmic strings, or an early period of cosmic ``inflation''. Our understanding of both pictures is sufficiently incomplete to allow a wide range of predictions from each scenario. Here we show how the fundamentally different role played by ``causality'' in the two scenarios will allow the next generation of observations to transcend these uncertainties and identify whether the fluctuations originate with inflation or defects.""]",['1995-05-08'] +2530,['eng'],"['Colombi, S', 'Dodelson, S', 'Widrow, L M']",['Large scale structure tests of warm dark matter'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'temperature', 'neutrino, density', 'neutrino, right-handed', 'astrophysics, galaxy', 'numerical calculations']","['http://www-lib.fnal.gov/archive/1995/pub/Pub-95-093-A.html', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505029']","['Warm dark matter (WDM) is an intriguing model of structure formation from the point of view of both cosmology and particle physics. We consider a one-parameter family of WDM models. The linear power spectra for these models is calculated and compared with the corresponding spectra for cold dark matter (CDM), hot dark matter (HDM) and mixed dark matter (MDM) as well as the power spectrum derived from observations. Our linear analyses suggest that a model universe dominated by a particle whose mass to temperature ratio m_x/T_x is increased by a factor of two as compared with the standard HDM neutrino gives a reasonable fit to the data on large (>8h^{-1} {\\rm ~Mpc}) scales. N-body simulations for this particular WDM model show features of both HDM and CDM. As in HDM, the first objects to collapse are large pancake-like structures. The final matter distribution is rather smooth and structures as small as galaxy halos are excluded. However, there appear to be virialized rich clusters evident in the CDM but not the HDM simulations. Unfortunately, a simple comparison of the matter distribution and its statistical properties with observations indicates that WDM, like CDM, has too much power at small scales. This is particularly evident in the small-scale pairwize velocity dispersion. The cluster multiplicity function has the wrong shape with too many rich clusters being produced, though this conclusion is based on the simple assumption that light traces mass in groups of galaxies.']",['1995-05-08'] +2531,['eng'],"['Milgrom, M', 'Usov, Yu V']",['Possible association of ultra-high-energy cosmic-ray events with strong gamma-ray bursts'],['Astrophysics and Astronomy'],"['charged particle, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'correlation, time']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505009'],"[""We point out that each of the error boxes of the two highest-energy cosmic-ray shower events known, overlaps with that of a strong gamma-ray burst (GRB). The GRBs precede the cosmic rays by 5.5, and 11 months respectively. In one case the strongest known cosmic ray is paired with the strongest gamma-ray burst in the BATSE catalogue. The probability of this to have occurred by chance seems rather small. Without building on post-factum statistics, we think the above is remarkable enough to suggest that the cosmic ray and gamma-ray burst were produced by the same outburst. A time delay (and a small positional disparity) is expected, since the trajectory of a charged cosmic-ray particle is wriggled by intervening magnetic fields. We estimate that the Galaxy's field alone may produce a delay of the order observed. We discuss some of the implications that follow if such an association is confirmed. For example, the upper limit on the distance to the cosmic-ray source, combined with a much-better-determined position of the gamma-ray burst source, narrows greatly the volume in which to look for an optical counterpart. There is also useful information in the time delay regarding, e.g., intergalactic magnetic fields.""]",['1995-05-04'] +2532,['eng'],"['Scott, D', 'Silk, J', 'White, M']",['From microwave anisotropies to cosmology'],['Astrophysics and Astronomy'],['introductory'],['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9505015'],"['Fluctuations in the temperature of the cosmic microwave background have now been detected over a wide range of angular scales, and a consistent picture seems to be emerging. This article describes some of the implications for cosmology. Analysis of all the published detections suggests the existence of a peak on degree scales of height 2.4 to 10 (90%CL) relative to the amplitude of the power spectrum at large angular scales. This result confirms an early prediction, implies that the universe did in fact recombine, and limits theories of structure formation. Illustrative examples are provided of how the comparison of microwave background and large-scale structure data will be a potentially powerful means of answering fundamental questions about the universe.']",['1995-05-04'] +2533,['eng'],"['Amendola, L', 'Baccigalupi, C', 'Occhionero, F']",['Reconciling inflation with openness'],['Astrophysics and Astronomy'],"['inflationary universe', 'space-time, horizon', 'astrophysics, bubble', 'critical phenomena', 'tunneling', 'matter, density']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9504097'],"['It is already understood that the increasing observational evidence for an open Universe may be reconciled with inflation if our horizon is contained inside one single huge bubble nucleated during the inflationary phase transition. In the scenario we present here, the Universe consists of infinitely many superhorizon bubbles, like our own, the distribution of which can be made to peak at \\Omega_0\\approx 0.2. Therefore, unlike the existing literature, we do not have to rely upon the anthropic principle nor upon special initial conditions.']",['1995-04-28'] +2534,['eng'],"['Dar, Arnon', 'Shaviv, N J']",['The extragalactic neutrino background radiations from blazars and cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, galaxy', 'neutrino, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, particle source', 'gas', 'cosmic radiation, flux', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9504083'],['Blazar emission of gamma rays and cosmic ray production of gamma rays in gas-rich clusters have been proposed recently as alternative sources of the high energy extragalactic diffuse gamma ray background radiation. We show that these sources also produce a very different high energy extragalactic diffuse neutrino background radiation. This neutrino background may be detected by the new generation of large neutrino telescopes under construction and may be used to trace the origin of the extragalactic gamma radiation.'],['1995-04-25'] +2535,['eng'],"['Farrar, Glennys R S', 'Kolb, E W']",['Light photinos as dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'supersymmetry', 'postulated particle, photino', 'sparticle, mass', 'mass, sparticle', 'sparticle, annihilation', 'annihilation, sparticle', 'sparticle, density', 'critical phenomena', 'cross section', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9504081'],"['There are good reasons to consider models of low-energy supersymmetry with very light photinos and gluinos. In a wide class of models the lightest R-odd, color-singlet state containing a gluino, the \\r0, has a mass in the 1-2 GeV range and the slightly lighter photino, \\pho, would survive as the relic R-odd species. For the light photino masses considered here, previous calculations resulted in an unacceptable photino relic abundance. But we point out that processes other than photino self-annihilation determine the relic abundance when the photino and R^0 are close in mass. Including \\r0\\longleftrightarrow\\pho processes, we find that the photino relic abundance is most sensitive to the \\r0-to-\\pho mass ratio, and within model uncertainties, a critical density in photinos may be obtained for an \\r0-to-\\pho mass ratio in the range 1.2 to 2.2. We propose photinos in the mass range of 500 MeV to 1.6 GeV as a dark matter candidate, and discuss a strategy to test the hypothesis.']",['1995-04-25'] +2536,['eng'],"['Shaviv, N J']",['On the source and location of temporal variability in fireballs'],['Astrophysics and Astronomy'],"['astrophysics', 'fireball', 'photon, cosmic radiation', 'cosmic radiation, particle source']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9504077'],"[""Most cosmological models for gamma-ray bursts invoke the production of a ``fireball'' in a compact region, as indicated by the short time variability of the observed GRBs. The high density of e^+e^- pairs in such fireballs inevitably makes them opaque to gamma-rays and requires the gamma-ray emission to take place only after the fireball has expanded and became optically thin to gamma's. Many of the ``traditional'' scenarios explain the temporal variability of GRBs as being formed by growing instabilities in the expanding fireball. Here we explore this possiblity and examine its validity.""]",['1995-04-24'] +2537,['eng'],"['Knox, L']",['Determination of inflationary observables by cosmic microwave background anisotropy experiments'],['Astrophysics and Astronomy'],"['inflationary universe', 'spectra, perturbation', 'perturbation, spectra', 'perturbation, scalar', 'perturbation, tensor', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, fundamental constant', 'baryon, density', 'numerical calculations, interpretation of experiments']","['http://www-lib.fnal.gov/archive/1995/pub/Pub-95-008-A.html', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9504054']","[""Inflation produces nearly Harrison-Zel'dovich scalar and tensor perturbation spectra which lead to anisotropy in the cosmic microwave background (CMB). The amplitudes and shapes of these spectra can be parametrized by Q_S^2, r\\equiv Q_T^2/Q_S^2, n_S and n_T where Q_S^2 and Q_T^2 are the scalar and tensor contributions to the square of the CMB quadrupole and n_S and n_T are the power-lawspectral indices. Even if we restrict ourselves to information from angles greater than one third of a degree, three of these observables can be measured with some precision. The combination 130^{1-n_S}Q_S^2 can be known to better than \\pm 0.3\\%. The scalar index n_S can be determined to better than \\pm 0.02. The ratio r can be known to about \\pm 0.1 for n_S \\simeq 1 and slightly better for smaller n_S. The precision with which n_T can be measured depends weakly on n_S and strongly on r. For n_S \\simeq 1 n_T can be determined with a precision of about \\pm 0.056(1.5+r)/r. A full-sky experiment with a 20'beam using technology available today, similar to those being planned by several groups, can achieve the above precision. Good angular resolution is more important than high signal-to-noise ratio; for a given detector sensitivity and observing time a smaller beam provides significantly more information than a larger beam. The uncertainties in n_S and r are roughly proportional to the beam size. We briefly discuss the effects of uncertainty in the Hubble constant, baryon density, cosmological constant and ionization history.""]",['1995-04-18'] +2538,['eng'],"['Totani, T', 'Sato, K']",['Spectrum of the relic neutrino background from past supernovae and cosmological models'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, cosmic radiation', 'neutrino, background', 'neutrino, emission', 'emission, neutrino', 'energy spectrum', 'astrophysics, fundamental constant', 'astrophysics, galaxy', 'astrophysics, model', 'cosmic radiation, flux', 'flux, cosmic radiation', 'deep underground detector, KAMIOKANDE', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9504015'],"['It is greatly expected that the relic neutrino background from past supernovae is detected by Superkamiokande (SK) which is now under construction. We calculate the spectrum and the event rate at SK systematically by using the results of simulations of a supernova explosion and reasonable supernova rates. We also investigate the effect of a cosmological constant, \\Lambda, on the spectrum, since some recent cosmological observations strongly suggest the existence of \\Lambda. We find following results. 1) The spectrum has a peak at about 3 MeV, which is much lower than that of previous estimate (6 \\sim 10 MeV). 2) The event rate at SK in the range from 10 MeV to 50 MeV, where the relic neutrinos from past supernovae is dominant, is about 25 \\, {h_{50}}^2 \\, \\left( \\frac{R_{SN}}{0.1 {\\rm yr^{-1}}} \\right) \\left(\\frac{n_G \\, h_{50}^{-3}}{0.02{\\rm Mpc}^{-3}}\\right) events per year, where R_{SN} is the supernova rate in a galaxy, n_G is the number density of galaxies, and h_{50} = H_0 / (50km/s/Mpc), where H_0 is the Hubble constant. 3) The event rate is almost insensitive to \\Lambda. The flux increases in the low energy side (< 10 MeV) with increasing \\Lambda, but decreases in the high energy side (10 MeV <) in models in which the integrated number of supernovae in one galaxy is fixed.']",['1995-04-07'] +2539,['eng'],"['Malaney, R A', 'Starkman, G D', 'Widrow, L M']",['Warm-plus-hot neutrino dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, mass', 'mass, neutrino', 'astrophysics, model', 'neutrino, oscillation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9504014'],"[""We investigate a new hybrid-model universe containing two types of dark matter, one ``warm'' and the other ``hot''. The hot component is an ordinary light neutrino with mass \\sim 25h^2~eV while the warm component is a sterile neutrino with mass \\sim 700h^2~eV. The two types of dark matter arise entirely within the neutrino sector and do not require separate physical origins. We calculate the linear transfer functions for a representative sample of warm-plus-hot models. The transfer functions, and results from several observational tests of structure formation, are compared with those for the cold-plus-hot models that have been studied extensively in the literature. On the basis of these tests, we conclude that warm-plus-hot dark matter is essentially indistinguishable from cold-plus-hot dark matter, and therefore provides a viable scenario for large scale structure. We demonstrate that a neutrino mass matrix can be constructed which provides the requisite dark matter constituents, while remaining consistent with all cosmological bounds.""]",['1995-04-10'] +2540,['eng'],"['Krauss, L M', 'Turner, M S']",['The cosmological constant is back'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, fundamental constant', 'vacuum state, energy', 'energy, density', 'astrophysics, galaxy', 'matter, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9504003'],"['A diverse set of observations now compellingly suggest that Universe possesses a nonzero cosmological constant. In the context of quantum-field theory a cosmological constant corresponds to the energy density of the vacuum, and the wanted value for the cosmological constant corresponds to a very tiny vacuum energy density. We discuss future observational tests for a cosmological constant as well as the fundamental theoretical challenges---and opportunities---that this poses for particle physics and for extending our understanding of the evolution of the Universe back to the earliest moments.']",['1995-04-04'] +2541,['eng'],"['Shaviv, N J', 'Dar, Arnon']",['Fireballs in dense stellar regions as an explanation of gamma ray bursts'],['Astrophysics and Astronomy'],"['astrophysics, model', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'fireball', 'electron, pair production', 'pair production, electron', 'electron, density', 'baryon, density', 'temperature', 'Compton scattering', 'cosmic radiation, flux', 'flux, cosmic radiation', 'time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503105'],['We study a cosmological scenario for gamma ray bursts (GRBs) where relativistic flows interact with dense radiation fields. It is shown that this scenario is plausible in very dense stellar regions which are known to exist in collapsed cores of globular clusters or dense nuclei of galaxies. It yields a correct quantitative description of the temporal behavior of GRBs. Several other properties of GRBs are easily explained.'],['1995-03-29'] +2542,['eng'],"['Sigl, G', 'Jedamzik, K', 'Schramm, David N', 'Berezinsky, Veniamin Sergeevich']",['Helium photodisintegration and nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'helium, photofission', 'light nucleus, production', 'production, light nucleus', 'cosmic radiation, production', 'production, cosmic radiation', 'topology, defect', 'photon, cosmic radiation', 'black hole, massive', 'massive, black hole', 'superconducting, string', 'string, superconducting', 'postulated particle, magnetic monopole', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503094'],"['We consider the production of ^3He and ^2H by ^4He photodisintegration initiated by non-thermal energy releases during early cosmic epochs. We find that this process cannot be the predominant source of primordial ^2H since it would result in anomalously high ^3He/D ratios in conflict with standard chemical evolution assumptions. We apply this fact to constrain topological defect models of highest energy cosmic ray (HECR) production. Such models have been proposed as possible sources of ultrahigh energy particles and gamma-rays with energies above 10^{20}eV. The constraints on these models derived from ^4He-photodisintegration are compared to corresponding limits from spectral distortions of the cosmic microwave background radiation (CMBR) and from the observed diffuse gamma-ray background. It is shown that for reasonable primary particle injection spectra superconducting cosmic strings, unlike ordinary strings or annihilating monopoles, cannot produce the HECR flux at the present epoch without violating at least the ^4He-photodisintegration bound. The constraint from the diffuse gamma-ray background rules out the dominant production of HECR by the decay of Grand Unification particles in models with cosmological evolution assuming standard fragmentation functions. Constraints on massive black hole induced photodisintegration are also discussed.']",['1995-03-27'] +2543,['eng'],"['New, K C B', 'Chanmugam, G', 'Johnson, W W', 'Tohline, J E']",['Millisecond pulsars'],['Astrophysics and Astronomy'],"['astrophysics, pulsar', 'gravitational radiation, measurement', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503092'],"['Laboratory searches for the detection of gravitational waves have focused on the detection of burst signals emitted during a supernova explosion, but have not resulted in any confirmed detections. An alternative approach has been to search for continuous wave (CW) gravitational radiation from the Crab pulsar. In this paper, we examine the possibility of detecting CW gravitational radiation from pulsars and show that nearby millisecond pulsars are generally much better candidates. We show that the minimum strain h_c ~ 10E-26 that can be detected by tuning an antenna to the frequency of the milli- second pulsar PSR 1957+20, with presently available detector technology, is orders of magnitude better than what has been accomplished so far by observing the Crab pulsar, and within an order of magnitude of the maximum strain that may be produced by it. In addition, we point out that there is likely to be a population of rapidly rotating neutron stars (not necessarily radio pulsars) in the solar neighborhood whose spindown evolution is driven by gravitational radiation. We argue that the projected sensitivity of modern resonant detectors is sufficient to detect the subset of this population that lies within 0.1 kpc of the sun.']",['1995-03-27'] +2544,['eng'],"['Enomoto, R']",['A possible correlation between EGRET sources and an air-borne experiment'],['Astrophysics and Astronomy'],"['talk, Tokyo 1994/05/25', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503091'],"['In 1989, an air-borne experiments (VEGA experiment) aiming at the detection of a few 10 GeV \\gamma-ray were carried out. In these experiments, nine point-source candidates along the Galactic plane were reported. In these candidates, the five of five highest significance candidates positionally coincide with the EGRET galactic plane sources.']",['1995-03-27'] +2545,['eng'],"['Graziani, C', 'Harding, A K', 'Sina, R']",['Elimination of resonant divergences from QED in super-strong magnetic fields'],['Astrophysics and Astronomy'],"['quantum electrodynamics', 'scattering amplitude', 'magnetic field, external field', 'magnetic field, high', 'radiative correction', 'renormalization', 'propagator', 'S-matrix', 'differential cross section', 'Feynman graph']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503086'],"['We study the resonant divergences that occur in quantum scattering cross-sections in the presence of a strong external magnetic field. We demonstrate that all such divergences may be eliminated by introducing radiative corrections to the leading-order scattering amplitudes. These corrections impose a choice of basis states that must be used in scattering calculations: electron states must diagonalize the mass operator, while photon states must diagonalize the polarization operator. The radiative corrections introduce natural line-widths into the energy denominators of all propagators, as well as into the time-development exponentials of all scattering states corresponding to external lines. Since initial and final scattering states may now decay, it is logically necessary to compute scattering amplitudes for a finite time-lapse between the preparation of the initial state and the measurement of the final state. Strict energy conservation, which appeared in previous formulations of the theory, must thus be abandoned. We exhibit the generic formulae for the scattering cross-sections in two useful limits, corresponding to the cases where either the initial states or the final states are stable, and discuss the application of the general formula when neither of these limits applies.']",['1995-03-24'] +2546,['eng'],"['Janka, H T']",['When do supernova neutrinos of different flavors have similar luminosities but different spectra?'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, flavor', 'n, matter', 'neutrino, energy', 'potential, chemical', 'neutrino, flux', 'flux, neutrino', 'luminosity']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503068'],"['Muon and tau neutrinos (\\nu_x) interact with protoneutron star matter only via neutral currents and exchange energy with the stellar gas predominantly by neutrino-electron scattering and neutrino-pair processes. In contrast, electron neutrinos and antineutrinos (\\nu_e and \\bar\\nu_e) are frequently absorbed and produced in charged-current mediated reactions with nucleons. Therefore the emergent \\nu_e and \\bar\\nu_e originate from layers with lower temperatures further out in the star and are emitted with much lower characteristic spectral temperatures. In addition, a major contribution to the \\nu_e and \\bar\\nu_e opacities is due to absorptions, while the opacity of \\nu_x is strongly dominated by scattering reactions with nucleons and nuclei in which the \\nu_x energy is (essentially) conserved. Therefore the \\nu_x distribution is nearly isotropic when \\nu_x decouple energetically and their outward diffusion is slowed down. In a generalized form to include this effect, the Stefan-Boltzmann Radiation Law can account for both the facts that \\nu_e (\\bar\\nu_e) and \\nu_x emerge from the star with similar luminosities but with very different characteristic spectral temperatures. Simple analytical expressions to estimate the effect are given. If, as recently argued, even at densities significantly below nuclear matter density neutral-current scatterings were associated with considerable energy transfer between neutrino and target particle, one might expect spectral temperatures of \\nu_x much closer to those of \\nu_e and \\bar\\nu_e. This is of relevance for the detection of neutrino signals from supernovae.']",['1995-03-17'] +2547,['eng'],"['Bahcall, J N', 'Lande, K', 'Lanou, R E', 'Learned, J G', 'Hamish Robertson, R G', 'Wolfenstein, L']",['Progress and prospects in neutrino astrophysics'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'astrophysics', 'neutrino, solar', 'neutrino, energy spectrum', 'energy spectrum, neutrino', 'proposed experiment', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503047'],"['The neutrino deficits observed in four solar neutrino experiments, relative to the theoretical predictions, have led to fresh insights into neutrino and solar physics. Neutrino emission from distant, energetic astronomical systems may form the basis for a new field of astronomy. Additional experiments are needed to test explanations of the solar neutrino deficits and to allow the detection of more distant sources.']",['1995-03-13'] +2548,['eng'],"['Turner, M S']",['The hot Big Bang and beyond'],['Astrophysics and Astronomy'],"['talk, Cancun 1994/09/26', 'talk, The Hague 1994/08', 'astrophysics, model', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'inflationary universe', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503017'],"['The hot big-bang cosmology provides a reliable accounting of the Universe from about 10^{-2}\\sec after the bang until the present, as well as a robust framework for speculating back to times as early as 10^{-43}\\sec. Cosmology faces a number of important challenges; foremost among them are determining the quantity and composition of matter in the Universe and developing a detailed and coherent picture of how structure (galaxies, clusters of galaxies, superclusters, voids, great walls, and so on) developed. At present there is a working hypothesis---cold dark matter---which is based upon inflation and which, if correct, would extend the big bang model back to 10^{-32}\\sec and cast important light on the unification of the forces. Many experiments and observations, from CBR anisotropy experiments to Hubble Space Telescope observations to experiments at Fermilab and CERN,']",['1995-03-06'] +2549,['eng'],"['Müller, V']",['Cluster abundance from perturbation spectra with broken scale invariance'],['Astrophysics and Astronomy'],"['talk, Potsdam 1994/09/18', 'inflationary universe', 'spectra, perturbation', 'perturbation, spectra', 'astrophysics, galaxy', 'astrophysics, cluster', 'correlation function', 'mass spectrum, galaxy', 'galaxy, mass spectrum', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'velocity', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503018'],"[""A double inflationary model with enhanced power at large scales --- Broken Scale Invariant perturbations (BSI) --- leads to a promising scenario for the formation of large-scale structure. We use high-resolution PM simulations with a model for the thermodynamic evolution of baryons. Galactic halos are identified as peaks in the distribution of mass points which had time to cool providing a physical biasing mechanism. The clustering properties of galactic halos are in agreement with both small-scale and large-scale characteristics of the galaxy distribution, as variances of counts in cells, 'galaxy' correlation functions, 'cluster' abundances and 'cluster-cluster' correlation functions, and velocity dispersions at small scales.""]",['1995-03-06'] +2550,['eng'],"['Primack, Joel R']",['Status of cosmological parameters'],['Astrophysics and Astronomy'],"['talk, Snowmass 1994/06/29', 'astrophysics, missing-mass', 'matter, density', 'astrophysics, fundamental constant', 'light nucleus, production', 'galaxy, cluster', 'density, fluctuation', 'neutrino, mass', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503020'],"['I discuss the Hubble parameter H_0, the age of the universe t_0, the density \\Omega_0, and the cosmological constant \\Lambda. To focus the discussion, I will concentrate on the issue of the value of the density \\Omega_0 in currently popular cosmological models in which most of the dark matter is cold, especially Cold + Hot Dark Matter (CHDM) and flat low- \\Omega CDM with a Cosmological Constant (\\LambdaCDM). The evidence would favor a small \\Omega_0 \\approx 0.3 if (1) the Hubble parameter actually has the high value h \\approx 0.8 favored by many observers, and the age of the universe t_0 \\geq 13 Gy; or (2) the baryonic/total mass ratio in clusters is actually \\sim 20\\%, about 3-4 times larger than expected for standard Big Bang Nucleosynthesis in an \\Omega=1 universe, and standard BBN is actually right in predicting that the density of ordinary matter \\Omega_b lies in the range 0.009 \\leq \\Omega_b h^2 \\leq 0.02. The evidence would favor \\Omega=1 if (1) the POTENT analysis of galaxy peculiar velocity data is right, in particular regarding outflows from voids or the inability to obtain the present-epoch non-Gaussian density distribution from Gaussian initial fluctuations in a low-\\Omega universe; or (2) the preliminary report from LSND indicating a neutrino mass \\geq 2.4 eV is right, since that would be too much hot dark matter to allow significant structure formation in a low-\\Omega \\LambdaCDM model. Statistics on gravitational lensing of quasars provide a strong upper limit on \\Lambda. Reliable data on all of these issues is becoming available so rapidly today that a clear decision between these alternatives may be possible within the next few years.']",['1995-03-06'] +2551,['eng'],"['Sigl, G']",['Topological defects and highest energy cosmic and gamma rays'],['Astrophysics and Astronomy'],"['cosmic radiation, flux', 'flux, cosmic radiation', 'topology, defect', 'annihilation, defect', 'defect, annihilation', 'decay, defect', 'defect, decay', 'photon, cosmic radiation', 'astrophysics, string', 'postulated particle, magnetic monopole', 'energy spectrum', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503014'],['In this paper we review the hypothesis that a considerable part of the cosmic ray flux observed above about 10^{19}\\eV may be produced by decaying or annihilating topological defects left over from phase transitions in the early universe at grand unification energy scales (\\approx10^{16}\\GeV). Possible signatures of cosmic ray producing defect models are discussed which could be tested experimentally in the near future. We thereby focus on model independent universal spectral properties of the predicted particle fluxes.'],['1995-03-03'] +2552,['eng'],"['Gottlöber, S']",['The primordial perturbation spectrum and large scale structure'],['Astrophysics and Astronomy'],"['talk, Munich 1994/12/12', 'astrophysics, model', 'inflationary universe', 'astrophysics, missing-mass', 'astrophysics, fundamental constant', 'space-time, de Sitter', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9503004'],['Observational constraints on standard CDM spectra and perturbation spectra with broken scale invariance are discussed.'],['1995-03-02'] +2553,['eng'],"['Balland, C', 'Blanchard, A']",['Temperature distribution function of X-ray clusters of galaxies in a neutrino dominated universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'neutrino, astrophysics', 'astrophysics, galaxy', 'temperature, spectra', 'spectra, temperature', 'cosmic radiation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502103'],"[""The temperature distribution function (TDF) of X-ray clusters is derived for different normalizations of the HDM power spectrum in an Omega_0=1 universe using the statistics of peaks of a random Gaussian field. Concerning cluster formation only, the neutrino picture appears to be marginally consistent with observations for H_0=70 km/s/Mpc provided the normalization is alpha=sigma_0/delta_s=0.42 with sigma_0 the rms variance of the fluctuations linearly evolved to the present epoch and delta_s the collapse threshold required in structure formation models. However, using the constraint that the formation epoch of QSO's puts on the HDM model, it appears that this normalization is too small to be consistent with quasars formation. Allowing higher values for the Hubble constant alleviates this problem but leads to an unacceptable short age of the universe. Moreover, the constraint put by the recent measurement of the level of fluctuations in the cosmic background radiation by COBE tends to reject models with high values of H_0. We conclude that the neutrino model fails in any case to account for the whole set of available observations in a consistent way.""]",['1995-02-28'] +2554,['eng'],"['Górski, K M', 'Bennett, C L', 'Banday, A J']",['Collected contributions from the COBE-DMR group to the Maryland astrophysics meeting on dark matter'],['Astrophysics and Astronomy'],"['talk', 'astrophysics', 'microwaves, background', 'microwaves, anisotropy', 'correlation function', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502032'],['The three papers summarize the methods employed by the COBE-DMR group to analyze the power spectrum of the two-year DMR anisotropy maps. Results for the slope and normalization of the power spectrum are presented and compared. The implications of these results for various dark matter-based structure formation models are also discussed.'],['1995-02-07'] +2555,['eng'],"['Qian, Y Z', 'Fuller, G M']",['Matter-enhanced antineutrino flavor transformation and supernova nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'nucleus, production', 'production, nucleus', 'neutrino, oscillation', 'antineutrino, flavor', 'antineutrino, mixing angle', 'matter, enhancement', 'neutrino nucleon, interaction', 'interaction, neutrino nucleon', 'antineutrino p, interaction', 'interaction, antineutrino p', 'differential cross section, energy dependence', 'energy dependence, differential cross section', 'numerical calculations', 'antineutrino/e, capture', 'capture, antineutrino/e']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502080'],"['Matter-enhanced antineutrino flavor transformation between \\bar\\nu_e and \\bar\\nu_{\\mu(\\tau)} can occur in supernovae if the vacuum masses for these species satisfy m_{\\bar\\nu_e}>m_{\\bar\\nu_{\\mu(\\tau)}}. For \\delta m^2> 1 eV^2, such flavor transformation can affect the electron fraction Y_e in the neutrino-heated supernova ejecta. We point out that such flavor transformation will not drive Y_e>0.5 at the r-process nucleosynthesis epoch in the best available supernova model for such nucleosynthesis. Consequently, there is no obvious conflict between matter-enhanced antineutrino flavor transformation \\bar\\nu_e\\rightleftharpoons\\bar\\nu_{\\mu(\\tau)} and r-process nucleosynthesis in the neutrino-heated supernova ejecta.']",['1995-02-17'] +2556,['eng'],"['Fuller, G M', 'Primack, Joel R', 'Qian, Y Z']",['Do experiments and astrophysical considerations suggest an inverted neutrino mass hierarchy?'],['Astrophysics and Astronomy'],"['neutrino, mass', 'mass, neutrino', 'neutrino, mixing angle', 'neutrino, oscillation', 'mass, hierarchy', 'hierarchy, mass', 'neutrino, mass spectrum', 'mass spectrum, neutrino', 'astrophysics', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502081'],"['The recent results from the Los Alamos neutrino oscillation experiment together with assumptions of neutrino oscillation solutions for the solar and atmospheric neutrino deficit problems, may place powerful constraints on any putative scheme for neutrino masses and mixings. Assuming the validity of these experiments and assumptions, we argue that a nearly unique spectrum of neutrino masses emerges as a fit, if two additional astrophysical arguments are adopted: (1) the sum of the light neutrino masses is \\sim 5\\ {\\rm eV}, as large scale structure simulations with mixed cold plus hot dark matter seem to suggest; and (2) r-process nucleosynthesis originates in neutrino-heated ejecta from Type II supernovae. In this fit, the masses of the neutrinos must satisfy m_{{\\nu}_e} \\approx m_{{\\nu}_s} \\approx 2.7\\ {\\rm eV} (where {\\nu}_e is split from a sterile species, {\\nu}_s, by \\sim {10}^{-6} \\ {\\rm eV}) and m_{{\\nu}_{\\tau}} \\approx m_{{\\nu}_{\\mu}} \\approx 1.1\\ {\\rm eV} (where these species are split by \\sim {10}^{-2} \\ {\\rm eV}). We discuss alternative neutrino mass spectra that are allowed if we decline to adopt certain experiments or astrophysical models.']",['1995-02-17'] +2557,['eng'],"['Rezzolla, L', 'Miller, J C', 'Pantano, O']",['Evaporation of quark drops during the cosmological Q-H transition'],['Astrophysics and Astronomy'],"['quark, matter', 'matter, droplet', 'transition, quark hadron', 'astrophysics', 'model, hydrodynamical', 'production, bubble', 'bubble, production', 'baryon number', 'energy, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502064'],['We have carried out a study of the hydrodynamics of disconnected quark regions during the final stages of the cosmological quark-hadron transition. A set of relativistic Lagrangian equations is presented for following the evaporation of a single quark drop and results from the numerical solution of this are discussed. A self-similar solution is shown to exist and the formation of baryon number density inhomogeneities at the end of the drop contraction is discussed.'],['1995-02-14'] +2558,['eng'],"['Larsen, G B', 'Madsen, J']",['Reconciling mixed dark matter with a large Hubble parameter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, massive', 'massive, neutrino', 'neutrino, oscillation', 'neutrino, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502052'],['Standard mixed dark matter models with eV-mass neutrinos constituting the hot component are only viable for a low value of the Hubble parameter. In this {\\it Letter\\/} we show how to reconcile the mixed dark matter models with recent measurements of a large Hubble parameter by introducing neutrino degeneracy.'],['1995-02-10'] +2559,['eng'],"['Stompor, R', 'Górski, K M', 'Banday, A J']",['COBE-DMR-normalisation for cosmological constant dominated cold dark matter models'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, fundamental constant', 'inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'matter, density', 'astrophysics, galaxy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502035'],"['The two-year COBE-DMR 53 and 90 GHz sky maps are used to determine the normalization of inflationary, cosmological constant dominated, cold dark matter models. Although the COBE-DMR data prefer a nearly critical value for the total density, low-density models with Omega_0 > 0.15 can not be rejected at a confidence level > 95%. We compare theoretical predictions for various large scale statistics, computed for a range of values of Omega_0 and h=0.5, or 0.8, to various measures of structure in the universe.']",['1995-02-07'] +2560,['eng'],"['Górski, K M', 'Stompor, R', 'Banday, A J']",['COBE-DMR-normalisation for cold and mixed dark matter models inflationary cosmogony'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'cosmic radiation, background', 'cosmic radiation, microwaves', 'cosmic radiation, anisotropy', 'astrophysics, model', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502033'],"['The two-year COBE-DMR 53 and 90 GHz sky maps in both ecliptic and galactic coordinates, are used to determine the normalisation of inflationary, flat, dark matter dominated universe models. The appropriately normalized cold and mixed dark matter models, computed for a range of values of Omega_baryon and h, and several values of the hot to cold dark matter abundance ratio, are then compared to various measures of structure in the universe.']",['1995-02-07'] +2561,['eng'],"['Steinhardt, Paul Joseph']",['Cosmology at the crossroads'],['Astrophysics and Astronomy'],"['talk', 'inflationary universe, validity test', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'moment, multipole', 'polarization', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502024'],"['Observational tests during the next decade may determine if the evolution of the Universe can be understood from fundamental physical principles, or if special initial conditions, coincidences, and new, untestable physical laws must be invoked. The inflationary model of the Universe is an important example of a predictive cosmological theory based on physical principles. In this talk, we discuss the distinctive fingerprint that inflation leaves on the cosmic microwave background anisotropy. We then suggest a series of five milestone experimental tests of the microwave background which could determine the validity of the inflationary hypothesis within the next decade. The paper is a Review based on a Plenary talk given at the Snowmass Workshop on Particle Astrophysics and Cosmology, 1995 It will appear in the Proceedings edited by E. Kolb and R.Peccei. Software package for computing filter functions and band power estimates available thru world-wide-web at http://dept.physics.upenn.edu/~www/as tro-cosmo/ .']",['1995-02-06'] +2562,['eng'],"['Pogosian, D Y', 'Starobinsky, A A']",['Mixed cold-hot dark matter model with several massive neutrino types'],['Astrophysics and Astronomy'],"['talk, Potsdam 1994/09', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, model', 'neutrino, massive', 'massive, neutrino', 'spectra, perturbation', 'perturbation, spectra', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502019'],"['Mixed cold-hot dark matter cosmological models (CHDM) with \\Omega_{tot}=1, approximately flat initial spectrum of adiabatic perturbations and 1, 2 or 3 types of massive neutrinos are compared and tested using recent observational data. The models with 2 or 3 neutrino types of equal mass permit as the best fit larger values of both the Hubble constant (H_0\\le 60 for 2 types, H_0\\le 65 for 3 types) and the total \\Omega_{\\nu} (up to 0.3 for 3 types) than the model with 1 massive type. Also, they have less problems with abundances of early compact objects including Ly-\\alpha clouds.']",['1995-02-06'] +2563,['eng'],"['Yamamoto, K', 'Sasaki, M', 'Tanaka, T']",['Large angle CMB anisotropy in an open universe in the one-bubble inflationary scenario'],['Astrophysics and Astronomy'],"['inflationary universe', 'production, bubble', 'bubble, production', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'density, perturbation', 'spectra, perturbation', 'perturbation, spectra', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501109'],"['We consider an alternative scenario of inflation which can account for a spatially open universe. It is similar to the old inflation in which the bubble nucleation occurs in the sea of false vacuum, but differs from it in that the second slow rollover inflation occurs inside a nucleated bubble. Hence our observable universe is entirely contained in one nucleated bubble. The significance of the scenario is that apart from a variance due to model parameters it gives us a definite prediction on the spectrum of the primordial density perturbations, hence is observationally testable. Here we investigate the spectrum of CMB anisotropies on large angular scales. We find that the contribution from peculiar modes which never appear in the usual harmonic analysis is significant in the case \\Omega_0\\lesssim0.1.']",['1995-02-01'] +2564,['eng'],"['Bertolami, O', 'García-Bellido, J']",['Astrophysical and cosmological constraints on a scale dependent gravitational coupling'],['Astrophysics and Astronomy'],"['gravitation, fundamental constant', 'asymptotic freedom', 'astrophysics, galaxy', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'light nucleus, production', 'production, light nucleus', 'astrophysics, pulsar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502010'],"['We study the phenomenological consequences of the recently proposed idea of a running gravitational coupling on macroscopic scales. When applied to the rotation curves of galaxies, we find that their flatness requires the presence of baryonic dark matter. Bounds on the variation of the gravitational coupling from primordial nucleosynthesis and the change of the period of binary pulsars are analysed. We also study constraints on the variations of G with scale from gravitational lensing and the cosmic virial theorem, as well as briefly discuss the implications of such a scenario for structure formation.']",['1995-02-03'] +2565,['eng'],"['Bahcall, J N', 'Kamionkowski, M P', 'Sirlin, A']",['Solar neutrinos'],['Astrophysics and Astronomy'],"['neutrino electron, elastic scattering', 'elastic scattering, neutrino electron', 'neutrino, solar', 'radiative correction', 'quantum electrodynamics, effect', 'energy spectrum, (electron)', '(electron), energy spectrum', 'channel cross section, energy dependence', 'channel cross section, ratio', 'model, solar', 'Feynman graph', 'tables', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502003'],"['Radiative corrections to the electron recoil-energy spectra and to total cross sections are computed for neutrino-electron scattering by solar neutrinos. Radiative corrections change monotonically the electron recoil spectrum for incident \\b8 neutrinos, with the relative probability of observing recoil electrons being reduced by about 4 \\% at the highest electron energies. For p-p and \\be7 neutrinos, the recoil spectra are not affected significantly. Total cross sections for solar neutrino-electron scattering are reduced by about 2 \\% compared to previously computed values. We also calculate the recoil spectra from ^{13}N and ^{15}O neutrinos including radiative corrections.']",['1995-02-02'] +2566,['eng'],"['Wang, Y']",['Simple analytical methods for computing the gravity-wave contribution to the cosmic background radiation anisotropy'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation', 'cosmic radiation, spectra', 'spectra, cosmic radiation', 'spectra, multipole', 'multipole, spectra', 'time dependence', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501116'],"['We present two simple analytical methods for computing the gravity wave contribution to the cosmic background radiation (CBR) anisotropy; one method uses a time-dependent transfer function, the other method uses an approximate gravity-wave mode function which is a simple combination of the lowest order spherical Bessel functions. We compare the CBR anisotropy tensor multipole spectrum computed using our methods with the previous results of highly accurate numerical methods. Our time-dependent transfer function is more accurate than the time-independent transfer function found by Turner, White, and Lidsey; however, we find that the transfer function method is only good for l \\la 120. Using our approximate gravity-wave mode function, we obtain much better accuracy; the tensor multipole spectrum we find differs by less than 5\\% for l\\leq 120, less than 10\\% for l < 160, and less than 25\\% for 160\\leq l \\leq 250 from the numerical result. Our approximate graviton mode function should be quite useful in studying tensor perturbations from inflationary models.']",['1995-02-01'] +2567,['eng'],"['Parsons, P', 'Barrow, John D']",['Generalised scalar field potentials and inflation'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'perturbation, scalar', 'perturbation, tensor', 'density, perturbation', 'gravitational radiation, perturbation', 'potential, inflaton']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501086'],"['We investigate the range of inflationary universe models driven by scalar fields possessing a general interaction potential of the form V(\\phi) = V_0 \\phi^n \\exp(-\\lambda \\phi^m). Power-law, de Sitter and intermediate inflationary universes emerge as special cases together with several new varieties of inflation. Analysing the behaviour of these models at the extrema of \\phi we derive sufficient constraints on the m - n parameter space such that inflation may occur as both an early and late-time phenomenon. We also compute the scalar and tensor perturbations produced in the model and compare these results with recent observations.']",['1995-01-24'] +2568,['eng'],"['Shemi, A']",['Cosmic rays from accreting isolated neutron stars'],['Astrophysics and Astronomy'],"['n, matter', 'matter, magnetic', 'cosmic radiation, galaxy', 'particle, acceleration', 'model, shock waves', 'luminosity', 'photon, cosmic radiation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501081'],"['Interstellar matter that is accreted onto isolated magnetic neutron stars in the Galaxy (\\sim 10^9 by number) is accelerated and reflected back by MHD shocks, which envelope the stars. The integrated power in the Galaxy L_{cr,ns} is \\sgreat 10^{40} {\\rm erg \\ s^{-1} }, the energy distribution is a power law of spectral index > 2, and the particle energy can be raised to 10^6 GeV, consistent with the power and spectrum of primary cosmic rays in the Galaxy. The major contribution for L_{cr,ns} comes from a minority of \\sim 10^7 isolated neutron stars which are located within dense clouds. Sources in these clouds, that are generally spread within the Galactic disk, can explain the concentration of high-energy cosmic rays in the Galactic plane, as deduced from pion decay spectra in gamma-ray observations. The soft X-ray luminosity from these neutron stars is consistent with the Galactic X-ray background. The accretion may be associated with ion-neutral bias, that is further enhanced by ion confinement in frozen-in magnetic fields, which can raise the relative abundance of first ionization potential (FIP) elements in the cosmic rays.']",['1995-01-24'] +2569,['eng'],"['Gilbert, A M', 'Perivolaropoulos, L']",['Spectra and statistics of cosmic string perturbations on the microwave background'],['Astrophysics and Astronomy'],"['astrophysics, string', 'spectra, perturbation', 'perturbation, spectra', 'statistical analysis', 'cosmic radiation, background', 'temperature, fluctuation', 'moment', 'inflationary universe', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502004'],"[""Using Monte Carlo simulations of perturbations induced by cosmic strings on the microwave background, we demonstrate the scale invariance of string fluctuation patterns. By comparing string-induced fluctuation patterns with gaussian random phase ones, we show that the non-gaussian signatures of the string patterns are detectable by tests based on the moments of the distributions only for angular scales smaller than a few arcminutes and for maps based on the gradient of temperature fluctuations. However, we find that tests of the gaussianity of the moments fail when we include a reasonable amount of instrumental noise in a pattern. Signal to noise ratios of 3.3 or greater completely suppress a string pattern's non-gaussian features even at the highest resolutions.""]",['1995-02-02'] +2570,['eng'],"['Stecker, F W', 'De Jager, O C']",['Absorption of high energy gamma-rays by low energy intergalactic photons'],['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'cosmic radiation, background', 'upper limit', 'photon photon, interaction', 'interaction, photon photon', 'photon, absorption', 'absorption, photon', 'energy, density', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501065'],"['Following our previously proposed technique, we have used the recent gamma-ray observations of Mrk 421 to place theoretically significant constraints on and possible estimates of the intergalactic infrared radiation field (IIRF) which are consistent with normal galactic IR production by stars and dust and rule out exotic mechanisms proposed to produce a larger IIRF. Using models for the low energy intergalactic photon spectrum from microwave to UV energies, we calculate the opacity of inter- galactic space to gamma-rays as a function of energy and redshift. These calculations indicate that the GeV gamma-ray burst recently observed by the EGRET experiment on CGRO originates at a redshift less than approximately 1.5.']",['1995-01-19'] +2571,['eng'],"['Stecker, F W', 'Salamon, M H']",['High energy neutrinos from quasars'],['Astrophysics and Astronomy'],"['neutrino, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, particle source', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'astrophysics, quasar', 'p, cosmic radiation', 'cosmic radiation, acceleration', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501064'],"['We review and clarify the assumptions of our basic model for neutrino production in the cores of quasars, as well as those modifications to the model subsequently made by other workers. We also present a revised estimate of the neutrino background flux and spectrum obtained using more recent empirical studies of quasars and their evolution. We compare our results with other thoeretical calculations and experimental upper limits on the AGN neutrino background flux. We also estimate possible neutrino fluxes from the jets of blazars detected recently by the EGRET experiment on the Compton Gamma Ray Observatory. We discuss the theoretical implications of these estimates.']",['1995-01-19'] +2572,['eng'],"['Dar, Arnon', 'Shaviv, N J']",['Origin of the high energy extragalactic diffuse gamma ray background'],['Astrophysics and Astronomy'],"['cosmic radiation, galaxy', 'photon, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, flux', 'flux, cosmic radiation', 'gas', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501079'],"['We show that cosmic rays in external galaxies, groups and clusters rich in gas, with an average flux similar to that observed in the Milky Way, could have produced the observed extragalactic diffuse gamma radiation.']",['1995-01-23'] +2573,['eng'],"['Bottino, A', 'Kim, C W', 'Song, J']",['Effects of the running gravitational constant on the amount of dark matter'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'gravitation, fundamental constant', 'astrophysics, galaxy', 'matter, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501066'],"['The amount of dark matter in the Milky Way and beyond is examined by taking into account the possible running of the gravitational constant G as a function of distance scale. If the running of G, as suggested by the Asymptotically-Free Higher-Derivative quantum gravity, is incorporated into the calculation of the total dark matter in the galactic halo, the amount of dark matter that is necessary to explain the rotation curve is shown to be reduced by one third compared with the standard calculations. However, this running of G alone cannot reproduce the observed flat behavior of the rotation curve. It is also shown that the running of G cannot explain away the presence of most of the dark matter beyond the scale of \\sim 10 Mpc in the Universe. We also present a pedagogical explanation for the running of G(r) in the region of large scales which is clearly a classical domain.']",['1995-01-20'] +2574,['eng'],"['Price, P B']",['Kinetics of conversion of air bubbles to air-hydrate crystals in antarctic ice'],['Astrophysics and Astronomy'],"['solids, water', 'photon, scattering length', 'scattering length, photon', 'temperature, dependence', 'deep underground detector, AMANDA', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501073'],"['The depth-dependence of bubble concentration at pressures above the transition to the air hydrate phase and the optical scattering length due to bubbles in deep ice at the South Pole are modeled using diffusion-growth data from the laboratory, taking into account the dependence of age and temperature on depth in the ice. The model fits the available data on bubbles in cores from Vostok and Byrd and on scattering length in deep ice at the South Pole. It explains why bubbles and air hydrate crystals co-exist in deep ice over a range of depths as great as 800 m and predicts that at depths below \\rm \\sim 1400 m the AMANDA neutrino observatory at the South Pole will operate unimpaired by light scattering from bubbles.']",['1995-01-20'] +2575,['eng'],[],['On the age vs depth and optical clarity of deep ice at South Pole'],['Astrophysics and Astronomy'],"['solids, water', 'photon, absorption', 'absorption, photon', 'photon, scattering length', 'scattering length, photon', 'Cherenkov counter', 'deep underground detector, AMANDA', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501072'],"['The first four strings of phototubes for the AMANDA high-energy neutrino observatory are now frozen in place at a depth of 800 to 1000 m in ice at the South Pole. During the 1995-96 season an additional six strings will be deployed at greater depths. Provided absorption scattering, and refraction of visible light are sufficiently small, the trajectory of a muon into which a neutrino converts can be determined by using the array of phototubes to measure the arrival times of \\v{C}erenkov light emitted by the muon. To help in deciding on the depth for implantation of the six new strings, we discuss models of age vs depth for South Pole ice, we estimate mean free paths for scattering from bubbles and dust as a function of depth, and we assess distortion of light paths due to refraction at crystal boundaries and interfaces between air-hydrate inclusions and normal ice. We conclude that the depth interval 1600 to 1800 m will be suitably transparent for the next six AMANDA strings and, moreover, that the interval 1600 to 2100 m will be suitably transparent for a future 1-km^3 observatory except possibly in a region a few tens of meters thick at a depth corresponding to a peak in the dust concentration at 60 kyr BP.']",['1995-01-23'] +2576,['eng'],"['Vorobev, P V', 'Kolokolov, I V']",['Detectors for the cosmic axionic wind'],['Astrophysics and Astronomy'],"['talk, Moscow 1994/12/04', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'postulated particle, axion', 'axion, solar', 'axion, radiative decay', 'radiative decay, axion', 'coupling, (axion 2photon)', '(axion 2photon), coupling', 'proposed experiment', 'magnetic field', 'radiation, laser']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501042'],"['We propose experimental schemes for detection an axionic condensate supposed to be cosmic dark matter. Various procedures are considered in dependence on the value of the axion mass. There are well known indications that a large part of the Universe mass exists in a form of dark matter: The analysis of rotation curves of galaxies leads to the conclusion that the mass of luminous matter is less than 1/10 part of the total galaxies mass. The existence of the dark matter is supported by the so called ""virial paradoxes"". It turns out that the reach and compact galaxies have unacceptible large \\overline{\\bf v^2} being in the same time stable with respect to anothers characteristics. For such the galaxies to be stable their masses must be one order greater than the observable ones. There are theoretical and observational arguments that this dark matter cannot be usual barionic matter as dust, planets etc. On the other hand there are attractive models where the dark matter is non-relativistic gas of light elementary particles weakly interacting with the ""usual"" matter. Periodicity in the distribution of quasars and distant galaxies with the red shift could be naturally explained in the cosmology with a gas of very light (pseudo)Goldstone bosons filling the Universe. It is well known that during a cooling an ideal Bose gas undergo the Bose condensation. If the decoupling of axions has been enough early in the cosmological evolution the axion gas should be in that moment of time in the Bose condensate state.']",['1995-01-16'] +2577,['eng'],"['Brandenberger, R H', 'Davis, A C', 'Rees, M J']",['Nucleosynthesis constraints on defect-mediated electroweak baryogenesis'],['Astrophysics and Astronomy'],"['astrophysics, string', 'electroweak interaction', 'baryon, production', 'production, baryon', 'topology, defect', 'critical phenomena', 'light nucleus, production', 'production, light nucleus', 'baryon, diffusion', 'neutrino, inflationary universe']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501040'],"['In the defect-mediated electroweak baryogenesis scenario, baryons are produced in well separated regions of space. It is shown that between the electroweak phase transition at a temperature of T \\sim 100 {\\rm GeV} and the end of nucleosynthesis at T \\sim 1 {\\rm KeV} the baryon inhomogeneities dissipate, and that no constraints on defect-mediated electroweak baryogenesis can be derived from considerations of inhomogeneous nucleosynthesis.']",['1995-01-13'] +2578,['eng'],"['Lyth, D H', 'Woszczyna, A']",['Large scale perturbations in the open universe'],['Astrophysics and Astronomy'],"['astrophysics, perturbation', 'field theory, scalar', 'cosmic radiation, anisotropy', 'inflationary universe', 'space-time, Robertson-Walker', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501044'],"['When considering perturbations in an open (Omega<1) universe, cosmologists retain only sub-curvature modes (defined as eigenfunctions of the Laplacian whose eigenvalue is less than -1 in units of the curvature scale, in contrast with the super-curvature modes whose eigenvalue is between -1 and 0). Mathematicians have known for almost half a century that all modes must be included to generate the most general HOMOGENEOUS GAUSSIAN RANDOM FIELD, despite the fact that any square integrable FUNCTION can be generated using only the sub-curvature modes. The former mathematical object, not the latter, is the relevant one for physical applications. The mathematics is here explained in a language accessible to physicists. Then it is pointed out that if the perturbations originate as a vacuum fluctuation of a scalar field there will be no super-curvature modes in nature. Finally the effect on the cmb of any super-curvature contribution is considered, which generalizes to Omega<1 the analysis given by Grishchuk and Zeldovich in 1978. A formula is given, which is used to estimate the effect. In contrast with the case Omega=1, the effect contributes to all multipoles, not just to the quadrupole. It is important to find out whether it has the same l dependence as the data, by evaluating the formula numerically.']",['1995-01-16'] +2579,['eng'],"['Berera, A', 'Fang, L Z']",['Thermally induced density perturbations in the inflation era'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'field theory, scalar', 'temperature, fluctuation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501024'],"['The possibility of thermally induced initial density perturbations in inflationary cosmology is examined. The fluctuation dynamics of a scalar field plus thermal bath system during slow roll is described by a Langevin-like equation. Fluctuation-dissipation arguments show that for a wide parameter range within the standard inflation model, the thermal fluctuations of the scalar field can dominate its quantum fluctuations. The initial amplitude of density perturbations is found to lie in a range which is consistent with the recent observations of cosmic temperature fluctuations.']",['1995-01-10'] +2580,['eng'],"['Faraoni, V', 'Cooperstock, F I', 'Overduin, J M']",['COBE constraints on Kaluza-Klein cosmologies'],['Astrophysics and Astronomy'],"['astrophysics, model', 'Kaluza-Klein model', 'cosmic radiation, background', 'astrophysics, fundamental constant', 'inflationary universe', 'field theory, scalar', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501012'],"['A class of Kaluza-Klein cosmologies recently proposed is compared with observations of the cosmic microwave background. Some models are ruled out, while others turn out to be viable, with the number of extra dimensions being constrained by the COBE and Tenerife experiments.']",['1995-01-05'] +2581,['eng'],"['Biermann, P L']",['The origin of cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, particle source', 'cosmic radiation, acceleration', 'astrophysics, supernova', 'astrophysics, galaxy', 'showers, air', 'transport theory', 'energy spectrum, (electron)', '(electron), energy spectrum', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501003'],"[""We propose that cosmic rays originate mainly in three sites, a) normal supernova explosions into the interstellar medium, b) supernova explosions into stellar winds, and c) hot spots of powerful radio galaxies. The proposal depends on an assumption about the scaling of the turbulent diffusive transport in cosmic ray mediated shock regions; the proposal also uses a specific model for the interstellar transport of cosmic rays. The model has been investigated in some detail and compared to i) the radio data of OB stars, Wolf Rayet stars, radio supernovae, radio supernova remnants, Gamma-ray line and continuum emission from starforming regions, and the cosmic ray electron spectrum, ii) the Akeno air shower data over the particle energy range from 10 TeV to EeV, and iii) the Akeno and Fly's Eye air shower data from 0.1 EeV to above 100 EeV. Here we specifically discuss in some detail the assumptions inherent in the model proposed, concerning the transport of energetic particles, first in the acceleration region, and second in the Galaxy.""]",['1995-01-04'] +2582,['eng'],"['Llorente, A', 'Pérez-Mercader, J']",['Big-bang nucleosynthesis as a probe of the geometry of superspace'],['Astrophysics and Astronomy'],"['Friedman model', 'space-time, Robertson-Walker', 'light nucleus, production', 'production, light nucleus', 'quantum gravity, superspace', 'relativity theory, general', 'elements', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412094'],"['We study the effect from a general ultralocal supermetric on primordial nucleosynthesis for Friedmann-Robertson-Walker Cosmology. The parameter \\lambda of the supermetric changes the effective number of degrees of freedom, g_*, which modifies the Friedmann equation. This modification produces variations in the production of primordial ^4He. The observations of the primordial abundances of light elements (^4He, D, ^3He and ^7Li) allow to estimate bounds on the values of \\lambda consistent with these observations. We obtain 0.87 \\le \\lambda \\le 1.04. In addition we analyze the importance of \\lambda < 1 to explain possible incompatibilities in the standard Big-Bang nucleosynthesis.']",['1995-01-04'] +2583,['eng'],"['Hindmarsh, M B']",['Cosmological perturbations from cosmic strings'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, string', 'perturbation theory', 'topology, defect', 'tensor, energy-momentum', 'density, perturbation', 'scaling']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412079'],"[""Some aspects of the theory of cosmological perturbations from cosmic strings and other topological defects are outlined, with particular reference to a simple example: a spatially flat CDM-dominated universe. The conserved energy-momentum pseudo-tensor is introduced, and the equation for the density perturbation derived from it. It is shown how the scaling hypothesis for defect evolution results in a Harrison-Zel'dovich spectrum for wavelengths well inside the horizon.""]",['1995-01-04'] +2584,['eng'],"['Górski, K M', 'Ratra, B', 'Sugiyama, N', 'Banday, A J']","['COBE-DMR-normalised open inflation, CDM cosmogony']",['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'cosmic radiation, background', 'cosmic radiation, microwaves', 'astrophysics, model', 'production, galaxy', 'galaxy, production', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502034'],"['Fourier analysis on a cut sky of the two-year COBE DMR 53 and 90 GHz sky maps (in galactic coordinates) is used to determine the normalisation of an open inflation model based on the cold dark matter scenario. The normalised model is compared to measures of large-scale structure in the universe. Although the DMR data alone does not provide sufficient discriminative power to prefer a particular value of the mass density parameter, the open model appears to be reasonably consistent with observations when Omega_0 ~ 0.3 - 0.4 and merits further study.']",['1995-02-07'] +2585,['eng'],"['Kawasaki, M', 'Moroi, T']",['Electromagnetic cascade in the early universe and its application to the big-bang nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'cascade, electromagnetic', 'energy spectrum, cascade', 'cascade, energy spectrum', 'Boltzmann equation, solution', 'photon electron, Compton scattering', 'Compton scattering, photon electron', 'photon nucleon, interaction', 'interaction, photon nucleon', 'electron, pair production', 'pair production, electron', 'photon photon, interaction', 'interaction, photon photon', 'light nucleus, photofission', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412055'],['We investigate the electromagnetic cascade initiated by injection of very high energy photons in the early Universe and calculate the cascade spectrum by solving a set of Boltzmann equations numerically. In the calculation we take account of Compton scattering off the background electrons and pair creation off the background nucleons as well as photon-photon processes and inverse Compton scattering. We also apply our cascade spectrum to the big bang nucleosynthesis with photo-dissociation processes due to heavy unstable particles and obtain the constraint on their lifetime and abundance.'],['1994-12-19'] +2586,['eng'],"['Young, K K']",['DUMAND-II'],['Astrophysics and Astronomy'],"['talk', 'deep underground detector, water', 'activity report, DUMAND']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412060'],"['The DUMAND-II detector will search for astronomical sources of high energy neutrinos. Successful deployment of the basic infrastructure, including the shore cable, the underwater junction box, and an environmental module was accomplished in December, 1993. One optical module string was also deployed and operated, logging data for about 10 hours. The underwater cable was connected to the shore station where we were able to successfully exercise system controls and log further environmental data. After this time, water leaking into the electronics control module for the deployed string disabled the string electrical system. The acquired data are consistent with the expected rate of downgoing muons, and our ability to reconstruct muons was demonstrated. The measured acoustical backgrounds are consistent with expectation, which should allow acoustical detection of nearby PeV particle cascades. The disabled string has been recovered and is undergoing repairs ashore. We have identified the source of the water leak and implemented additional testing and QC procedures to ensure no repetition in our next deployment. We will be ready to deploy three strings and begin continuous data taking in 1995.']",['1994-12-19'] +2587,['eng'],"['Hogan, C J']",['Cosmic fluctuations and dark matter from scalar field oscillations'],['Astrophysics and Astronomy'],"['astrophysics, fluctuation', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'field theory, scalar', 'field theory, oscillation', 'Goldstone particle, massless', 'massless, Goldstone particle', 'Higgs particle, massive', 'massive, Higgs particle', 'astrophysics, quasar']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412054'],"[""It is argued that scale-invariant cosmic fluctuations and cosmic dark matter might originate from two different modes of a single scalar field. The dynamical relaxation of a multicomponent classical scalar field in an expanding universe excites two generic types of global modes: massless Goldstone oscillations, which lead to scale-invariant isentropic fluctuations, and massive Higgs modes, which lead to cold dark matter with isocurvature fluctuations in density. Estimates are given of these effects in a simple generic model where the large scale fluctuations and dark matter density match those observed; it is shown that the former requires a heavy scale (\\phi_0\\approx 10^{16}GeV) for the potential minimum, and the latter requires an extremely small self coupling (\\lambda\\approx 10^{-83}). An additional prediction of the model is then the formation of isocurvature fluctuations, leading to the early collapse of dense \\approx 100 \\msol dark matter ``miniclusters'', formation of dense halos on the scale of compact dwarf galaxies, and possibly observable gravitational microlensing of quasars.""]",['1994-12-19'] +2588,['eng'],"['Rivers, R J', 'Evans, T S']",['The production of strings and monopoles at phase transitions'],['Astrophysics and Astronomy'],"['lectures, Cambridge 1994/08/21', 'astrophysics, string', 'topology, defect', 'field theory, relativistic', 'critical phenomena', 'correlation, length', 'field theory, scalar', 'thermodynamics, fluctuation', 'field equations, monopole', 'production, defect', 'defect, production', 'approximation, quenching', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412059'],"['We shall show that the density of defects produced at a second-order phase transition is determined by the correlation length of the fields. This is true both for defects appearing in the Ginzburg regime and for defects produced at a quench, when the Ginzburg regime is irrelevant. (Invited lectures given by R.J.R. to the Nato Advanced Study Institute and Euroconference on Formation and Interaction of Topological Defects, Isaac Newton Institute, Cambridge (UK), September, 1994.)']",['1994-12-19'] +2589,['eng'],"['Rajagopal, M', 'Romani, R W']",['Ultra-low frequency gravitational radiation from massive black hole binaries'],['Astrophysics and Astronomy'],"['black hole, pair', 'astrophysics, galaxy', 'energy loss', 'angular momentum', 'gravitational radiation', 'astrophysics, pulsar', 'energy, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412038'],"[""For massive black hole binaries produced in galactic mergers, we examine the possibility of inspiral induced by interaction with field stars. We model the evolution of such binaries for a range of galaxy core and binary parameters, using numerical results from the literature to compute the binary's energy and angular momentum loss rates due to stellar encounters and including the effect of back-action on the field stars. We find that only a small fraction of binary systems can merge within a Hubble time via unassisted stellar dynamics. External perturbations may, however, cause efficient inspiral. Averaging over a population of central black holes and galaxy mergers, we compute the expected background of gravitational radiation with periods Pw ~1-10y. Comparison with sensitivities from millisecond pulsar timing suggests that the strongest sources may be detectable with modest improvements to present experiments.""]",['1994-12-12'] +2590,['eng'],"['Cervantes-Cota, J L', 'Dehnen, H']",['Induced gravity inflation in the SU(5) GUT'],['Astrophysics and Astronomy'],"['grand unified theory, SU(5)', 'gravitation, induced', 'inflationary universe', 'chaos', 'Higgs particle, mass', 'mass, Higgs particle', 'symmetry breaking', 'boundary condition', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412032'],"['We investigate the cosmological consequences of a theory of induced gravity in which the scalar field is identified with the Higgs field of the first symmetry breaking of a mi\\-ni\\-mal SU(5) GUT. The mass of the X-boson determines a great value for the coupling constant of gravity-particle physics. Because of this fact, a ""slow"" rollover dynamics for the Higgs field is not possible in a ""new"" inflation scenario and, moreover, a contraction era for the scale factor in the early universe exists, \\-after\\- which inflation follows automatically; ""chaotic"" inflation is performed without problems. Inflation is successfully achieved due to the relationship among the masses of particle physics at that scale: The Higgs-, X-boson- and Planck-masses. As a result the particle physics pa\\-ra\\-me\\-ter \\lambda is not fine-tuned as usual in order to predict acceptable values of re-heating temperature and density and gravitational wave perturbations. Moreover, if the coherent Higgs oscillations didn\'t decay they could explain the missing mass problem of cosmology.']",['1994-12-12'] +2591,['eng'],"['Askebjer, P']",['Optical properties of the south pole ice at depths between 0.8 and 1 km'],['Astrophysics and Astronomy'],"['introductory', 'photon, absorption', 'absorption, photon', 'photon, scattering length', 'scattering length, photon', 'deep underground detector, AMANDA', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412028'],"['The optical properties of the ice at the geographical South Pole have been investigated at depths between 0.8 and 1 kilometers. The absorption and scattering lengths of visible light (\\sim515 nm) have been measured {\\it in situ } using the laser calibration setup of the AMANDA neutrino detector. The ice is intrinsically extremely transparent. The measured absorption length is 59 \\pm 3 meters, comparable with the quality of the ultra-pure water used in the IMB and Kamiokande proton-decay and neutrino experiments and more than two times longer than the best value reported for laboratory ice. Due to a residual density of air bubbles at these depths, the trajectories of photons in the medium are randomized. Assuming bubbles are smooth and spherical, the average distance between collisions at 1 km depth is about 25 cm. The measured inverse scattering length on bubbles decreases linearly with increasing depth in the volume of ice investigated.']",['1996-05-21'] +2592,['eng'],"['Wilkes, R J']",['Summary of nuclear and particle astrophysics sessions'],['Astrophysics and Astronomy'],"['conference, review', 'astrophysics', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'showers, air', 'neutrino', 'counters and detectors', 'experimental results']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412018'],"['Astrophysics is gaining increased attention from the particle and nuclear physics communities, as budget cuts, delays, and cancellations limit opportunities for breakthrough research at accelerator laboratories. Observations of cosmic rays (protons and nuclei), gamma rays and neutrinos present a variety of puzzles whose eventual solution will shed light on many issues ranging from the nature of fundamental interactions at extreme energies to the mechanisms of astrophysical sources. Several important detectors are just beginning full-scale operation and others are beginning construction.']",['1994-12-07'] +2593,['eng'],"['Salopek, D S']","['Cosmological inflation, microwave background anisotropies and large scale structure of the universe']",['Astrophysics and Astronomy'],"['talk', 'inflationary universe', 'astrophysics, galaxy', 'density, fluctuation', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitation, quasiclassical', 'relativity theory, general', 'perturbation theory, higher-order', 'Hamilton-Jacobi equation', 'angular correlation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412012'],"[""Cosmological inflation provides the simplest and most promising mechanism for generating fluctuations for structure formation. Using powerful Hamilton-Jacobi methods, I will describe (1) how to compute density fluctuations and cosmic microwave anisotropies arising from inflation, and (2) improvements of the Zel'dovich approximation describing gravitational collapse. I compare these results with the latest cosmological observations.""]",['1994-12-06'] +2594,['eng'],"['Kachelriess, M', 'Berg, D', 'Wunner, G']",['Is Compton scattering in strong magnetic fields really infrared divergent?'],['Astrophysics and Astronomy'],"['Compton scattering', 'magnetic field', 'infrared problem', 'quantum electrodynamics', 'S-matrix']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412013'],"['The infrared behavior of QED changes drastically in the presence of a strong magnetic field: the electron self-energy and the vertex function are infrared {\\em finite}, in contrast with field-free QED, while new infrared divergences appear that are absent in free space. One famous example of the latter is the infrared catastrophe of magnetic Compton scattering, where the cross section for scattering of photons from electrons which undergo a transition to the Landau ground state {\\em diverges} as the frequency of the incoming photon goes to zero. We examine this divergence in more detail and prove that the singularity of the cross section is {\\em removed} as soon as proper account is taken of all quantum electrodynamical processes that become indistinguishable from Compton scattering in the limit of vanishing frequency of the incident photon.']",['1994-12-06'] +2595,['eng'],"['Koranda, S', 'Allen, B']",['CBR anisotropy from inflation-induced gravitational waves in mixed radiation and dust cosmology'],['Astrophysics and Astronomy'],"['inflationary universe', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'gravitational radiation, perturbation', 'temperature, fluctuation', 'Friedman model', 'postulated particle, graviton', 'moment, multipole', 'correlation function, angular correlation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410049'],"['We examine stochastic temperature fluctuations of the cosmic background radiation (CBR) arising via the Sachs-Wolfe effect from gravitational wave perturbations produced in the early universe. We consider spatially flat, perturbed FRW models that begin with an inflationary phase, followed by a mixed phase containing both radiation and dust. The scale factor during the mixed phase takes the form a(\\eta)=c_1\\eta^2+c_2\\eta+c_3, where c_i are constants. During the mixed phase the universe smoothly transforms from being radiation to dust dominated. We find analytic expressions for the graviton mode function during the mixed phase in terms of spheroidal wave functions. This mode function is used to find an analytic expression for the multipole moments \\langle a_l^2\\rangle of the two-point angular correlation function C(\\gamma) for the CBR anisotropy. The analytic expression for the multipole moments is written in terms of two integrals, which are evaluated numerically. The results are compared to multipoles calculated for models that are {\\it completely} dust dominated at last-scattering. We find that the multipoles \\langle a_l^2\\rangle of the CBR temperature perturbations for l>10 are significantly larger for a universe that contains both radiation and dust at last-scattering. We compare our results with recent, similar numerical work and find good agreement. The spheroidal wave functions may have applications to other problems of cosmological interest.']",['1994-10-18'] +2596,['eng'],"['White, M', 'Gelmini, Graciela B', 'Silk, J']",['Structure formation with decaying neutrinos'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'cosmic radiation, anisotropy', 'neutrino, mass', 'mass, neutrino', 'neutrino, decay', 'decay, neutrino', 'neutrino, lifetime', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411098'],"['We consider the effects of a massive, unstable neutrino on the evolution of large--scale structure and anisotropies in the cosmic microwave background. Comparison with large--scale structure data allows us to rule out a wide range of masses and lifetimes for such neutrinos. We also define a range of masses and lifetimes which delay matter--radiation equality and improve the agreement with the data of Cold Dark Matter models with critical density.']",['1994-11-24'] +2597,['eng'],"['Roberts, D', 'Liddle, A R', 'Lyth, D H']",['False vacuum inflation with a quartic potential'],['Astrophysics and Astronomy'],"['inflationary universe', 'field theory, scalar', 'potential', 'density, perturbation', 'critical phenomena']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411104'],"[""We consider a variant of Hybrid Inflation, where inflation is driven by two interacting scalar fields, one of which has a `Mexican hat' potential and the other a quartic potential. Given the appropriate initial conditions one of the fields can be trapped in a false vacuum state, supported by couplings to the other field. The energy of this vacuum can be used to drive inflation, which ends when the vacuum decays to one of its true minima. Depending on parameters, it is possible for inflation to proceed via two separate epochs, with the potential temporarily steepening sufficiently to suspend inflation. We use numerical simulations to analyse the possibilities, and emphasise the shortcomings of the slow-roll approximation for analysing this scenario. We also calculate the density perturbations produced, which can have a spectral index greater than one.""]",['1994-11-28'] +2598,['eng'],"['Bhattacharjee, P', 'Sigl, G']",['Monopole annihilation and highest energy cosmic rays'],['Astrophysics and Astronomy'],"['cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'p, cosmic radiation', 'neutrino, cosmic radiation', 'photon, cosmic radiation', 'cosmic radiation, production', 'production, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'astrophysics, model', 'critical phenomena', 'postulated particle, magnetic monopole', 'bound state, magnetic monopole', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9412053'],"['Cosmic rays with energies exceeding 10^{20}\\eV have been detected. The origin of these highest energy cosmic rays remains unknown. Established astrophysical acceleration mechanisms encounter severe difficulties in accelerating particles to these energies. Alternative scenarios where these particles are created by the decay of cosmic topological defects have been suggested in literature. In this paper we study the possibility of producing the highest energy cosmic rays through a process that involves formation of metastable magnetic monopole-antimonopole bound states and their subsequent collapse. The annihilation of the heavy monopole-antimonopole pairs constituting the monopolonia can produce energetic nucleons, gamma rays and neutrinos whose expected flux we estimate and discuss in relation to experimental data so far available. The monopoles we consider are the ones that could be produced in the early universe during a phase transition at the grand unification energy scale. We find that observable cosmic ray fluxes can be produced with monopole abundances compatible with present bounds.']",['1994-12-19'] +2599,['eng'],"['Brandenberger, R H']",['Modern cosmology and structure formation'],['Astrophysics and Astronomy'],"['lectures, Boulder 1994/05/29', 'astrophysics, model', 'perturbation', 'inflationary universe', 'finite temperature', 'astrophysics, missing-mass', 'galaxy, production', 'topology, defect', 'string model', 'scaling', 'texture', 'cosmic radiation, background', 'temperature, anisotropy', 'interpretation of experiments', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411049'],"['An introduction to modern cosmology is given, focusing on theories for the origin of structure in the Universe. After a brief review of the theory of growth of cosmological perturbations and a summary of some important observational results, most of the article is devoted to discussions of the inflationary Universe scenario and of topological defect models of structure formation. The final chapter is a summary of the theory of cosmic microwave background temperature fluctuations and of the current observational status.']",['1994-12-01'] +2600,['eng'],"['Masperi, L', 'Savaglio, S']",['Influence of strings with axionic content on the polarization of extragalactic sources'],['Astrophysics and Astronomy'],"['electroweak interaction, string', 'string, electroweak interaction', 'postulated particle, axion', 'photon, cosmic radiation', 'photon, polarization', 'polarization, photon', 'anomaly', 'scattering, photon axion', 'photon axion, scattering', 'perturbation theory', 'approximation, adiabatic']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411047'],"['It is shown that the axion concentrated in electroweak strings which are consequently stabilized may produce a rotation of the polarization angle of radiation from extragalactic sources larger than that caused by a background field, and that axionic walls attached to global strings have an effect which depends on the frequency. We discuss the validity of the classical and quantum treatments of radiation and indicate that the latter produces conversion of linear into circular polarization. We describe possible anomalies in the observations which might suggest these influences of the axion.']",['1994-12-01'] +2601,['eng'],"['Griest, K']",['The particle- and astro-physics of dark matter'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'galaxy, cluster', 'light nucleus, production', 'production, light nucleus', 'axion', 'WIMP', 'astrophysics, MACHO']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411038'],"['We review some recent determinations of the amount of dark matter on galactic, cluster, and large scales, noting some puzzles and their possible resolutions. We discuss the interpretation of big bang nucleosynthesis for dark matter, and then review the motivation for and basic physics of several dark matter candidates, including Machos, Wimps, axions, and neutrinos. Finally, we discuss how the uncertainty in the models of the Milky Way dark halo will affect the dark matter detection experiments.']",['1994-11-10'] +2602,['eng'],"['Primack, Joel R', 'Caldwell, David O', 'Holtzmann, J A', 'Klypin, A A', 'Caldwell, D O']",['Cold + hot dark matter cosmology with m($\\nu_{\\mu}$) $\\appprox$ m($\\nu_{\\tau}$) $\\appprox$ 2.4 eV'],['Astrophysics and Astronomy'],"['astrophysics, model', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, mass', 'mass, neutrino', 'neutrino, oscillation', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411020'],"['Cold + Hot Dark Matter (CHDM) \\Omega=1 cosmological models require a total neutrino mass \\sim 5 eV. Because recent data support the \\nu_\\mu \\to \\nu_\\tau oscillation explanation of the cosmic ray \\nu_\\mu deficit, which requires that m(\\nu_\\mu) \\approx m(\\nu_\\tau) this suggests that m(\\nu_\\mu) \\approx m(\\nu_\\tau) \\approx 2.4 eV. The linear calculations and N-body simulation reported here indicate that an \\Omega=1 CHDM model with two 2.4 eV neutrinos (designated C\\nu^2DM) agrees remarkably well with all available observations, but only if the Hubble parameter h \\approx 0.5. We also show that even one 2.4 eV neutrino raises serious difficulties for low-\\Omega flat CDM models.']",['1994-11-30'] +2603,['eng'],"['Nambu, Y', 'Taruya, A']",['Application of gradient expansion to inflationary universe'],['Astrophysics and Astronomy'],"['inflationary universe', 'perturbation theory', 'field theory, scalar', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9411013'],"['Using the long wave perturbation scheme(gradient expansion), the effect of inhomogeneity on the inflationary phase is investigated. We solved the perturbation equation of which source term comes from inhomogeneity of a scalar field and a seed metric. The result indicates that sub-horizon scale inhomogeneity strongly affects the onset of inflation.']",['1994-11-03'] +2604,['eng'],"['Perivolaropoulos, L']",['Cosmic string theory'],['Astrophysics and Astronomy'],"['lectures', 'astrophysics, string', 'production, string', 'string, production', 'velocity', 'cosmic radiation, background', 'gravitational radiation', 'astrophysics, pulsar', 'topology, defect', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410097'],"['This is a pedagogical introduction to the basics of the cosmic string theory and also a review of the recent progress made with respect to the macrophysical predictions of the theory. Topics covered include, string formation and evolution, large scale structure formation, generation of peculiar velocity flows, cosmic microwave background (CMB) fluctuations, lensing, gravitational waves and constraints from the msec pulsar. Particular emphasis is placed on the signatures predicted on the CMB and the corresponding non-gaussian features.']",['1994-11-01'] +2605,['eng'],"['Sigl, G']",['Neutrino mixing constraints and supernova nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'light nucleus, production', 'production, light nucleus', 'neutrino, interference', 'neutrino, flavor', 'neutrino, oscillation', 'neutrino, polarization', 'polarization, neutrino', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410094'],['We reexamine the constraints on mixing between electron and muon or tau neutrinos from shock-reheating and r-process nucleosynthesis in supernovae. To this end neutrino flavor evolution is described by nonlinear equations following from a quantum kinetic approach. This takes into account neutrino forward scattering off the neutrino background itself. In contrast to other claims in the literature it is shown that a sound self-consistent analytical approximation can in the first place only be performed in the adiabatic limit where phase terms are suppressed. In the cosmologically interesting mass range below about 25\\eV the resulting mixing parameter bounds are between one and two orders of magnitude less restrictive than limits neglecting neutrino contributions. Extensions to the non-adiabatic regime derived in the literature usually neglect coherence effects from phases. To check their importance numerical simulations of the evolution equations were performed in this regime. They indicate that analytical approximations for the flavor conversion efficiencies can indeed be extended by neglecting phase terms. This allows more stringent bounds similar to the ones derived in earlier work. These bounds depend to some extent on the adopted supernova model and tend to be somewhat less restrictive in the mixing angle but simultaneously extend to smaller mixing masses compared to limits neglecting the neutrino induced potential.'],['1994-10-31'] +2606,['eng'],"['Dodelson, S', 'Kosowsky, A']",['Analysis of small and medium-scale cosmic microwave background experiments'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'cosmic radiation, microwaves', 'cosmic radiation, anisotropy', 'astrophysics, model', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410081'],"[""Anisotropies in the temperature of the cosmic microwave background have been detected on a range of scales by several different experiments. These anisotropies reflect the primordial spectrum of metric perturbations in the early universe. In principle, the largest barrier to a clean interpretation of the experimental results is contamination by foreground sources. We address this issue by projecting out likely sources of foreground contamination {}from seven separate small-angle and medium-angle experiments. We then calculate likelihood functions for models with adiabatic perturbations, first for the amplitude of the spectrum while constraining the spectral index to be n=1, and then jointly for the amplitude and spectrum of the fluctuations. All of the experiments are so far consistent with the simplest inflationary models; for n=1 the experiments' combined best-fit quadrupole amplitude is Q_{\\rm rms-ps}= 18^{+3}_{-1} \\,\\,\\mu K, in excellent agreement with the COBE two-year data. In (Q_{\\rm rms-ps}, n) space, the allowed region incorporating intermediate and small-scale experiments is substantially more constrained than {}from COBE alone. We briefly discuss the expected improvement in the data in the near future and corresponding constraints on cosmological models.""]",['1994-10-27'] +2607,['eng'],"['Liddle, A R']",['Inflation as the unique causal mechanism for generating density perturbations on scales well above the Hubble radius'],['Astrophysics and Astronomy'],"['inflationary universe', 'density, perturbation', 'cosmic radiation, background', 'light nucleus, production', 'production, light nucleus', 'causality', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410083'],"['An examination is made of the widely held belief that inflation is the only possible causal mechanism capable of generating density perturbations on scales well in excess of the Hubble radius. A simple proof is given, which relies only on the assumption that our understanding of the universe from nucleosynthesis onwards is correct. No assumption of the underlying gravitational theory is necessary beyond that it is a metric theory.']",['1994-10-28'] +2608,['eng'],"['Gyuk, G', 'Turner, M S']",['MeV tau neutrino'],['Astrophysics and Astronomy'],"['talk', 'neutrino, Majorana', 'neutrino, Dirac', 'neutrino, decay modes', 'decay modes, neutrino', 'astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'helium', 'deuterium', 'baryon, density', 'neutrino, flavor', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, supernova', 'numerical calculations', 'neutrino/tau, mass', 'mass, neutrino/tau', 'neutrino/tau, lifetime']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410065'],"[""Terrestrial and ``Heavenly'' experiments severely constrain the mass and lifetime of an MeV tau neutrino. Irrespective of decay mode, for \\tau_\\nu \\ga 300\\sec the mass of the tau neutrino must be either approximately 30\\MeV or less than 0.4\\MeV (Majorana), 15\\keV (Dirac). If the dominant decay mode includes electromagnetic daughter products, the mass must be less than 0.4\\MeV (Majorana or Dirac) provided \\tau_\\nu \\ga 2.5\\times 10^{-12}\\sec, 15\\keV (Dirac) provided \\tau_\\nu \\ga 10^{-6}\\sec (m_\\nu /\\MeV ). A tau neutrino of mass between 1\\MeV and 30\\MeV can have a host of interesting astrophysical and cosmological consequences: relaxing the big-bang nucleosynthesis bound to the baryon density and the number of neutrino species, allowing big-bang nucleosynthesis to accommodate a low (less than 22\\%) ^4He mass fraction or high (greater than 10^{-4}) deuterium abundance, improving significantly the agreement between the cold dark matter theory of structure formation and observations, and helping to explain how type II supernovae explode. Exploring the MeV mass range not only probes fundamental particle physics, but also interesting astrophysical and cosmological scenarios.""]",['1994-10-23'] +2609,['eng'],"['Mezhlumian, A']",['Stationary universe model'],['Astrophysics and Astronomy'],"['talk, Rome 1994/05/18', 'astrophysics', 'inflationary universe, chaos', 'field theory, scalar', 'Fokker-Planck equation', 'diffusion', 'boundary condition']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410039'],"['This is the text of a talk given at the Rome Conference ""The Birth of the Universe and Fundemental Physics"", May, 1994. We present the recent progress achieved in collaboration with A.Linde and D.Linde towards understanding the true nature of the global spatial structure of the universe as well as the most general stationary characteristics of its time-dependent state with eternally growing total volume.']",['1994-10-17'] +2610,['eng'],"['Long, H N', 'Van Soa, D', 'Tran, T A', 'Tuan, T A']",['Electromagnetic-gravitational cross-sections in external electromagnetic fields'],['Astrophysics and Astronomy'],"['postulated particle, graviton', 'transition, photon graviton', 'electromagnetic field, external field', 'differential cross section']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410003'],['The classical processes: the conversion of photons into gravitons in the static electromagnetic fields are considered by using Feynman perturbation techniques. The differential cross sections are presented for the conversion in the electric field of the flat condesor and the magnetic field of the selenoid. A numerical evaluation shows that the cross sections may have the observable value in the present technical scenario.'],['1994-10-04'] +2611,['eng'],"['Kernan, P J', 'Krauss, L M']",['Yet another paper on SN1987A'],['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, cosmic radiation', 'neutrino, oscillation', 'neutrino, mixing angle', 'numerical calculations, interpretation of experiments', 'neutrino/e, mass', 'mass, neutrino/e', 'astrophysics, supernova', 'neutrino, oscillation', 'upper limit', 'neutrino, counters and detectors', 'neutrino, mixing angle', 'statistical analysis', 'numerical calculations, Monte Carlo', 'interpretation of experiments', 'neutrino/e, mass', 'mass, neutrino/e']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9410010'],"[""We supplement \\ML methods with a \\MC simulation to re-investigate the SN1987A neutrino burst detection by the IMB and Kamiokande experiments. The detector simulations include background in the the latter and ``dead-time'' in the former. We consider simple neutrinosphere cooling models, explored previously in the literature, to explore the case for or against neutrino vacuum mixing and massive neutrinos. In the former case, involving kinematically irrelevant masses, we find that the full range of vacuum mixing angles, 0 \\le \\svac \\le 1, is permitted, and the \\ML mixing angle is \\svac = .45. In the latter case we find that the inclusion of ``dead-time'' reduces previous \\mnue upper bounds by 10\\%, and supplementing the \\ML analysis with a \\MC goodness-of-fit test results in a further 15\\% reduction in the \\mnue upper limit. Our 95\\% C.L. upper limit for \\mnue is 19.6eV, while the best fit value is \\sim 0eV.""]",['1994-10-05'] +2612,['eng'],"['Battye, R A', 'Shellard, E P S']",['String radiative backreaction'],['Astrophysics and Astronomy'],"['string model', 'phi**n model, 4', 'symmetry, U(1)', 'space-time', 'radiative correction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9408078'],"[""We discuss radiative backreaction for global strings described by the Kalb-Ramond action with an analogous derivation to that for the point electron in classical electrodynamics. We show how local corrections to the equations of motion allow one to separate the self-field of the string from that of the radiation-field. Modifications to this 'local backreaction approximation' circumvent the runaway solutions familiar from electrodynamics, allowing these corrections to be used to evolve string trajectories numerically. Comparisons are made with analytic and numerical radiation calculations from previous work and the merits and limitations of this approach are discussed. Finally, we comment on the relevance of this work to simulations of a cosmological network of global or axion strings. These methods can also be applied to describe graviational, electromagnetic and other forms of string radiative backreaction.""]",['1994-11-30'] +2613,['eng'],"['Salopek, D S', 'Stewart, J M']",['Hypersurface-invariant approach to cosmological perturbations'],['Astrophysics and Astronomy'],"['astrophysics, perturbation', 'gravitation', 'approximation, quasiclassical', 'coupling, matter', 'matter, coupling', 'Hamilton-Jacobi equation, solution', 'field theory, scalar', 'gravitational radiation', 'perturbation theory, linear', 'correlation function, galaxy', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9409055'],"['Using Hamilton-Jacobi theory, we develop a formalism for solving semi-classical cosmological perturbations which does not require an explicit choice of time-hypersurface. The Hamilton-Jacobi equation for gravity interacting with matter (either a scalar or dust field) is solved by making an Ansatz which includes all terms quadratic in the spatial curvature. Gravitational radiation and scalar perturbations are treated on an equal footing. Our technique encompasses linear perturbation theory and it also describes some mild nonlinear effects. As a concrete example of the method, we compute the galaxy-galaxy correlation function as well as large-angle microwave background fluctuations for power-law inflation, and we compare with recent observations.']",['1994-09-23'] +2614,['eng'],"['Cramer, J G', 'Forward, Robert L', 'Morris, M S', 'Visser, M', 'Benford, G', 'Landis, G A']",['Natural wormholes as gravitational lenses'],['Astrophysics and Astronomy'],"['astrophysics, model', 'gravitation, effect', 'wormhole', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9409051'],"['Visser has suggested traversable 3-dimensional wormholes that could plausibly form naturally during Big Bang inflation. A wormhole mouth embedded in high mass density might accrete mass, giving the other mouth a net *negative* mass of unusual gravitational properties. The lensing of such a gravitationally negative anomalous compact halo object (GNACHO) will enhance background stars with a time profile that is observable and qualitatively different from that recently observed for massive compact halo objects (MACHOs) of positive mass. We recommend that MACHO search data be analyzed for GNACHOs.']",['1994-09-21'] +2615,['eng'],"['Will, C M', 'Steinhardt, Paul Joseph']","[""High frequency oscillations of Newton's constant induced by inflation""]",['Astrophysics and Astronomy'],"['inflationary universe', 'gravitation, fundamental constant', 'fundamental constant, oscillation', 'Brans-Dicke model', 'field theory, scalar', 'energy, oscillation', 'relativity theory, general', 'astrophysics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9409041'],"[""We examine the possibility that an epoch of inflationary expansion induces high-frequency oscillations of Newton's constant, G. The effect occurs because inflation can shift the expectation value of a non-minimally coupled, Brans-Dicke-like field away from the minimum of its effective potential. At some time after inflation ends, the field begins to oscillate, resulting in periodic variations in G. We find conditions for which the oscillation energy would be sufficient to close the universe, consistent with all known constraints from cosmology and local tests of general relativity.""]",['1994-09-16'] +2616,['eng'],"['Angelantonj, Carlo', 'Amendola, L', 'Litterio, M', 'Occhionero, F']",['String cosmology and inflation'],['Astrophysics and Astronomy'],"['talk, Rome 1994/05/18', 'astrophysics, string', 'astrophysics, model', 'fundamental constant', 'inflationary universe']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9501008', 'http://www-lib.fnal.gov/archive/1994/pub/Pub-94-315-A.pdf']","[""Following a suggestion by Gasperini and Veneziano, that String Cosmology can be reconciled with Inflation and, hence, with the Standard Big Bang, we display an analytical solution which possesses four interesting properties: (1) it is non-singular; (2) it distinguishes the dynamics of the external scale factor, a(t), from that of the internal one, b(t); (3) it exhibits a non-monotonic behavior of a(t); and (4) it stabilizes both Newton's constant and b(t) (the latter to a finite, non-vanishing value). The interest of the non-monotonic evolution of a(t) consists in the fact that it contains three phases of accelerated expansion, contraction and expansion before the final decelerated expansion which eventually becomes the Standard Big Bang. The total number of e-folds of the three accelerated eras can be calculated and tuned to fit the requests of observational astronomy.""]",['1995-01-05'] +2617,['eng'],"['Protheroe, R J', 'Stanev, T', 'Berezinsky, Veniamin Sergeevich']",['Electromagnetic cascades and cascade nucleosynthesis in the early universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'particle, decay', 'decay, particle', 'cascade, electromagnetic', 'helium, photofission', 'light nucleus, production', 'production, light nucleus', 'energy, cascade', 'channel cross section', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9409004'],"['We describe an exact calculation of electromagnetic cascading in radiation and matter in the early universe initiated by the decay of massive particles or by some other process. If these cascades are initiated after the epoch of big bang nucleosynthesis, then \\gamma-rays in these cascades will photodisintegrate ^4He, producing ^3He and deuterium. Using the observed ^3He and deuterium abundances we are able to place constraints on the cascade energy deposition as a function of cosmic time. In the case of the decay of massive primordial particles, we place limits on the density of massive primordial particles as a function of their mean decay time, and on the expected intensity of decay neutrinos.']",['1994-09-05'] +2618,['eng'],"['Pen, U L', 'Spergel, D N']",['Cosmic microwave anisotropies from topological defects in an open universe'],['Astrophysics and Astronomy'],"['astrophysics, texture', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'cosmic radiation, density', 'Einstein equation', 'propagator', 'topology, defect', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9408103'],"[""We present a general formalism for computing Cosmic Background Radiation (CBR) and density fluctuations in open models with stiff sources. We find analytic Green's functions for the linearized Einstein equations in the presence of stiff sources and use this formalism to estimate the amplitude and harmonic spectrum of microwave background fluctuations produced by topological defects in an open universe. Unlike inflationary models that predict a flat universe and a spectrum of CBR fluctuations that is enhanced at large angular scales, defect models predict that CBR fluctuations are suppressed on angular scales larger than that subtended by the curvature scale. In an \\Omega = 0.2 - 0.4 universe, these models, when normalized to the amplitude of CBR fluctuations observed by COBE, require a moderate bias factor, 2-3, to be compatible with the observed fluctuations in galaxy counts. In these models, accurate predictions can be made which are testable through CBR experiments in the near future. A CBR measurement of \\Omega would then be possible, up to the limit imposed by cosmic variance. We discuss some of the philosophical implications of an open model and propose a solution to the flatness problem.""]",['1994-09-01'] +2619,['eng'],"['Krauss, L M']",['Big bang nucleosynthesis and dark matter'],['Astrophysics and Astronomy'],"['talk, Los Angeles 1994/02/16', 'astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'baryon, matter', 'neutrino, density', 'correlation', 'neutrino, flavor', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9408102'],"['I present a review of Big Bang Nucleosynthesis, concentrating on the statistical analysis of theoretical uncertainties, and on systematic errors in observed abundances. Both have important implications for constraints on the amount of baryonic dark matter and the number of light neutrino species in nature. Without allowing for systematic uncertainties in abundances, we find that homogenous BBN would lead to the constraint \\Omega_B \\le .07 and N_{\\nu} \\le 3.04. Even allowing for maximal systematic uncertainties in ^4He, and ^7Li, we find \\Omega_B \\le .163. For intermediate ranges we provide new analytic fits for the upper limits to N_{\\nu} and \\Omega_B as a function of the helium mass fraction, Y_p.']",['1994-09-01'] +2620,['eng'],"['Battye, R A', 'Shellard, E P S']",['Current status of axion cosmology'],['General Relativity and Cosmology'],"['talk, Los Angeles 1994/02/16', 'astrophysics', 'postulated particle, axion', 'energy, density', 'critical phenomena', 'string model', 'symmetry breaking', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9408035'],"['We review the current status of axion cosmology in the light of recent work. We conclude that in the standard scenario, in which a global string network forms at the Peccei-Quinn phase transition, the largest contribution to the axion density is from loops, even when uncertainties in the nature of the QCD phase transition are taken into account. We also briefly discuss the implications of non-standard scenarios, such as an inflationary epoch and entropy production.']",['1994-08-15'] +2621,['eng'],"['Amendola, L', 'Gottlöber, S', 'Mücket, J P', 'Müller, V']",['Matter distribution for power spectra with broken scale invariance'],['Astrophysics and Astronomy'],"['inflationary universe', 'correlation function', 'angular correlation', 'scaling, violation', 'astrophysics, galaxy', 'moment', 'numerical calculations, interpretation of experiments']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9408104', 'http://fnalpubs.fnal.gov/archive/1994/pub/Pub-94-262-A.pdf']","['To test the primordial power spectra predicted by a double inflationary model with a break of amplitude \\Delta=3 at a scale of 2\\pi/k\\approx 10 \\hm and CDM as dominant matter content, we perform PM simulations with 128^3 particles on a 256^3 grid. The broken scale invariance of the power spectra explains the extra power observed in the large-scale matter distribution. COBE-normalized spectra and a linear biasing with b\\approx 2 are shown to reproduce the reconstructed power spectra from the CfA catalog. Identifying galactic halos with overdensity of approximately two times the cell variance, we can fit the angular correlation function using both the Limber equation and creating a APM-like angular projection with the observed luminosity function. Finally, the higher order moments of the galaxy distribution are shown to fit reasonably well the observed values.']",['1994-09-01'] +2622,['eng'],"['Lai, D', 'Shapiro, S']",['Gravitational radiation from rapidly rotating nascent neutron stars'],['Astrophysics and Astronomy'],"['gravitational radiation', 'n, matter', 'angular momentum', 'model, fluid', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9408053'],"['We study the secular evolution and gravitational wave signature of a newly-formed, rapidly rotating neutron star. The neutron star may arise from core collapse in a massive star or from the accretion-induced collapse of a white dwarf. After a brief dynamical phase, the nascent neutron star settles into an axisymmetric, secularly unstable equilibrium state. Gravitational radiation drives the star to a nonaxisymmetric, stationary equilibrium configuration via the bar-mode instability. The emitted quasi-periodic gravitational waves have a unique signature: the wave frequency sweeps downward from a few hundred Hertz to zero, while the wave amplitude increases from zero to a maximum and then decays back to zero. Such a wave signal could be detected by broad-band gravitational wave interferometers currently being constructed. We also characterize two other types of gravitational wave signals that could arise in principle from a rapidly rotating, secularly unstable neutron star: a high-frequency (f\\go 1000 Hz) wave which increases the pattern-speed of the star, and a wave that actually increases the angular momentum of the star.']",['1994-08-22'] +2623,['eng'],"['MacMinn, D', 'Primack, Joel R']",['Probing the era of galaxy formation via tev gamma ray absorption by the near infrared extragalactic background'],['Astrophysics and Astronomy'],"['production, galaxy', 'galaxy, production', 'photon, cosmic radiation', 'photon, absorption', 'absorption, photon', 'cosmic radiation, flux', 'flux, cosmic radiation', 'cosmic radiation, background', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9408076'],"['We have developed an indirect test of the era of galaxy formation by modeling the extragalactic background light (EBL) in the near infrared portion of the spectrum|a domain difficult to observe directly due to galactic and zodiacal contamination. A new method for probing this spectrum has been suggested by Stecker et al. (1992) which involves the absorption of TeV gamma rays by the EBL. TeV gamma rays have recently been detected from Markarian 421, an active galactic nucleus (AGN) at a redshift of z=0.031. If several more distant TeV sources exist, it should be possible to observe for the first time the EBL, and thus constrain the timescale over which galaxies form. The potential of this technique is illustrated by the constraints it places upon an earlier claim for a detection of the EBL.']",['1994-08-22'] +2624,['eng'],"['Lyth, D H', 'Liddle, A R']",['Interpreting large scale structure observations'],['Astrophysics and Astronomy'],"['talk, Paris 1994/06/02', 'astrophysics', 'density, perturbation', 'adiabatic', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'galaxy, cluster', 'perturbation theory, linear', 'matter, density', 'Friedman model', 'velocity', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9408066'],"[""The standard model of large scale structure is considered, in which the structure originates as a Gaussian adiabatic density perturbation with a nearly scale invariant spectrum. The basic theoretical tool of cosmological perturbation theory is described, as well as the possible origin of the density perturbation as a vacuum fluctuation during inflation. Then, after normalising the spectrum to fit the cosmic microwave background anisotropy measured by COBE, some versions of the standard model are compared with a variety of data coming from observations of galaxies and galaxy clusters. The recent COBE analysis of G\\'{o}rski and collaborators is used, which gives a significantly higher normalization than earlier ones. The comparison with galaxy and cluster data is done using linear theory, supplemented by the Press-Schechter formula when discussing object abundances of rich clusters and of damped Lyman alpha systems. By focussing on the smoothed density contrast as a function of scale, the observational data can be conveniently illustrated on a single figure, facilitating easy comparison with theory. The spectral index is constrained to 0.61 and arise naturally in the recently proposed hybrid inflationary scenario. An observational upper limit on {\\em n} is derived by normalizing the spectrum at the quadrupole scale and considering the possible overproduction of Planck mass relics formed in the final stage of primordial black hole evaporation. In the inflationary Universe with the maximum reheating temperature compatible with the observed quadrupole anisotropy, the upper limit is n=1.4, but it is slightly weaker for lower reheat temperatures. This limit applies over 57 decades of mass and is therefore insensitive to cosmic variance and any gravitational wave contribution to the quadrupole anisotropy. It is also independent of the dark matter content of the Universe and therefore the bias parameter. In some circumstances, there may be an extended dust-like phase between the end of inflation and reheating. In this case, primordial black holes form more abundantly and the upper limit is n=1.3.']",['1994-05-16'] +2649,['eng'],"['Hähnelt, M G']",['Low-frequency gravitational waves from supermassive black holes'],['Astrophysics and Astronomy'],"['black hole, massive', 'massive, black hole', 'gravitational radiation', 'astrophysics, galaxy', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'interference, laser', 'numerical calculations', 'counters and detectors, proposed']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9405032'],"[""Supermassive black holes are investigated as possible sources for low-frequency bursts of gravity waves. The event rate for `known' supermassive black holes at intermediate and high redshifts, inferred from the quasar luminosity function, is low \\sim 0.1 \\yr^{-1}. A space-based interferometer could therefore only see several events per year from supermassive black holes if an additional population of supermassive black holes existed and emitted gravitational waves efficiently. These might reside in the population of dwarf galaxies or in a transient population of small dark matter haloes that have mostly merged into larger haloes hosting the galaxies seen today. The proposed space-based gravitational-wave interferometer LISA/SAGITTARIUS should detect most gravitational-wave events involving supermassive black holes above 10^{4} \\Msol out to redshifts of z \\sim 100.""]",['1994-05-16'] +2650,['eng'],"['Pethick, C J', 'Thorsson, V']","['Neutrino emission from dense matter, and neutron star thermal evolution']",['Astrophysics and Astronomy'],"['talk', 'astrophysics', 'n, matter', 'neutrino, emission', 'emission, neutrino', 'energy loss', 'neutrino, bremsstrahlung', 'bremsstrahlung, neutrino', 'thermodynamics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9502021'],"['A brief review is given of neutrino emission processes in dense matter, with particular emphasis on recent developments. These include direct Urca processes for nucleons and hyperons, which can give rise to rapid energy loss from the stellar core without exotic matter, and the effect of band structure on neutrino bremsstrahlung from electrons in the crust, which results in much lower energy losses by this process than had previously been estimated.']",['1995-02-06'] +2651,['eng'],"['Szabo, A P', 'Protheroe, R J']",['Implications of particle acceleration in active galactic nuclei for cosmic rays and high energy neutrino astronomy'],['Astrophysics and Astronomy'],"['astrophysics, galaxy', 'cosmic radiation, particle source', 'cosmic radiation, acceleration', 'photon, cosmic radiation', 'neutrino, cosmic radiation', 'astrophysics, black hole', 'cosmic radiation, flux', 'flux, cosmic radiation', 'energy loss', 'numerical calculations, Monte Carlo', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9405020'],"[""We consider the production of high energy neutrinos and cosmic rays in radio-quiet active galactic nuclei (AGN) or in the central regions of radio-loud AGN. We use a model in which acceleration of protons takes place at a shock in an accretion flow onto a supermassive black hole, and follow the cascade that results from interactions of the accelerated protons in the AGN environment. We use our results to estimate the diffuse high energy neutrino intensity and cosmic ray intensity due to AGN. We discuss our results in the context of high energy neutrino telescopes under construction, and measurements of the cosmic ray composition in the region of the ``knee'' in the energy spectrum at \\sim 10^7 GeV.""]",['1994-05-11'] +2652,['eng'],"['Frieman, Joshua A', 'Harari, D', 'Surpi, G C']",['Time delay induced by gravitational waves upon gravitational lenses'],['Astrophysics and Astronomy'],"['astrophysics, quasar', 'gravitational radiation, effect', 'time delay', 'gravitation, lens']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9405015'],"[""Using Fermat's principle, we analyze the effects of very long wavelength gravitational waves upon the images of a gravitationally lensed quasar. We show that the lens equation in the presence of gravity waves is equivalent to that of a lens with different alignment between source, deflector, and observer in the absence of gravity waves. Contrary to a recent claim, we conclude that measurements of time delays in gravitational lenses cannot serve as a method to detect or constrain a stochastic background of gravitational waves of cosmological wavelengths, because the wave-induced time delay is observationally indistinguishable from an intrinsic time delay due to the lens geometry.""]",['1994-05-11'] +2653,['eng'],"['Pantaleone, J']","[""Neutrino flavor evolution near a supernova's core""]",['Astrophysics and Astronomy'],"['astrophysics, supernova', 'neutrino, flux', 'flux, neutrino', 'neutrino, density', 'phase space', 'density matrix', 'neutrino, flavor', 'light nucleus, production', 'production, light nucleus']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9405008'],"[""In supernovae and in the early universe, neutrino flavor evolution is a many-body phenomena. Here the equations describing the evolution of the density matrices in phase space are derived. Then these equations are applied to neutrino emission from a supernova core. Corrections to adiabatic propagation from a `small' background neutrino density are calculated. It is found that the amount of level crossing is significantly increased. This result indicates that the neutrino mass and mixing parameter region that is reliably disfavored by supernova nucleosynthesis is much smaller than previously calculated.""]",['1994-05-09'] +2654,['eng'],"['Krauss, L M', 'Kernan, P J']",['Recent deuterium observations and big bang nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'deuterium, density', 'baryon, density', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9405004'],"['A new observation of D in a primordial gas cloud, made using the high resolution spectrograph at the Keck telescope, indicates an abundance D/H =(1.9-2.5) \\times 10^{-4} \\cite{SCHR}. Since deuterium is destroyed by stars, and the predicted Big Bang Nucleosynthesis (BBN) abundance falls monotonically with increasing baryon density, deuterium places a reliable upper limit on the baryon density of the universe. Because the new measurement is substationally larger than previous, galactic estimates, it would force a reassessment of BBN predictions--- if it is confirmed. Using a new BBN Monte Carlo code and analysis technique \\cite{KK} we derive constraints implied by a lower limit of D/H =1.9 \\times 10^{-4}. We find \\Omega_B \\le .0068h^{-2}, which is definitively incompatible with baryonic halo dark matter. We also explore implications of combining the D measurement with other light element abundances. ^7Li provides a lower bound, \\Omega_B \\ge .004h^{-2}. Also, the initial ^4He mass fraction (Y_p) would have to be less than 23.5\\%, assuming 3 light neutrino species---in good agreement with present best fits. Finally, observational upper limits of Y_p \\le 24 \\% and ^7Li/H \\le 2.3 \\times 10^{-10} would allow the number of neutrinos to be as big as 3.9.']",['1994-05-03'] +2655,['eng'],"['Altaisky, M V', 'Bednyakov, V A', 'Kovalenko, S G']",['On fractal structure of quantum gravity and relic radiation anisotropy'],['General Theoretical Physics'],"['quantum gravity', 'dimension, 2', 'symmetry, discrete', 'fractals', 'cosmic radiation, background', 'microwaves']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404076'],['It is argued that cosmic microwave background anisotropy detected in COBE cosmic experiment can be considered as a trace of the quantum gravity fractal structure.'],['1994-05-02'] +2656,['eng'],"['Singh, A']",['Quasar production'],"['Other Fields of Physics', 'Astrophysics and Astronomy']","['astrophysics, quasar', 'spatial distribution, quasar', 'critical phenomena', 'neutrino, massive', 'massive, neutrino', 'neutrino, solar', 'neutrino, oscillation', 'topology, defect', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'black hole', 'interpretation of experiments', 'bibliography', 'astrophysics, quasar', 'spatial distribution, quasar', 'critical phenomena', 'neutrino, massive', 'massive, neutrino', 'neutrino, solar', 'neutrino, oscillation', 'topology, defect', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'black hole', 'interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404078'],"['Recent observations of the space distribution of quasars indicate a very notable peak in space density at a redshift of 2 to 3.It is pointed out in this article that this may be the result of a phase transition which has a critical temperature of roughly a few meV (in the cosmological units h=c=k=1 ). It is further pointed out that such a phase transition is natural in the context of massive neutrinos. In fact,the neutrino masses required for quasar production and those required to solve the solar neutrino problem by the MSW mechanism are consistent with each other.']",['1994-05-02'] +2657,['eng'],"['Allen, B', 'Koranda, S']",['Temperature fluctuations in the cosmic background radiation from inflationary cosmological models'],['Other Fields of Physics'],"['astrophysics, model', 'inflationary universe', 'cosmic radiation, background', 'gravitational radiation, perturbation', 'correlation function, angular correlation', 'moment, multipole', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404068'],"['We examine stochastic temperature fluctuations of the cosmic background radiation (CBR) arising via the Sachs-Wolfe effect from gravitational wave perturbations produced in the early universe. These temperature fluctuations are described by an angular correlation function C(\\gamma). A new (more concise and general) derivation of C(\\gamma) is given, and evaluated for inflationary-universe cosmologies. This yields standard results for angles \\gamma greater than a few degrees, but new results for smaller angles, because we do not make standard long-wavelength approximations to the gravitational wave mode functions. The function C(\\gamma) may be expanded in a series of Legendre polynomials; we use numerical methods to compare the coefficients of the resulting expansion in our exact calculation with standard (approximate) results. We also report some progress towards finding a closed form expression for C(\\gamma)']",['1994-04-28'] +2658,['eng'],"['Polarski, D', 'Starobinsky, A A']",['Isocurvature perturbations in multiple inflationary models'],['General Theoretical Physics'],"['inflationary universe, multiple', 'field theory, scalar', 'perturbation', 'astrophysics, missing-mass', 'missing-mass, astrophysics']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404061'],"['Dynamics of long-wave isocurvature perturbations during an inflationary stage in multiple (multi-component) inflationary models is calculated analytically for the case where scalar fields producing this stage interact between themselves through gravity only. This enables to determine correct amplitudes of such perturbations produced by vacuum quantum fluctuations of the scalar fields during the multiple inflationary stage. Exact matching to a post-inflationary evolution that gives the amplitude of isocurvature perturbations in the cold dark matter model with radiation is performed in the case where a massive inflaton field remains uncoupled from usual matter up to the present time. For this model, isocurvature perturbations are smaller than adiabatic ones in the region of the break in the perturbation spectrum which arises due to a transition between the two phases of inflation, but they may be much bigger and have a maximum at much shorter scales. The case of an inflaton with a quartic coupling which remains uncoupled after inflation is considered, too.']",['1994-04-25'] +2659,['eng'],"['Shi, X', 'Schramm, David N', 'Dearborn, D S P']",['On solar model solutions to the solar neutrino problem'],['Other Fields of Physics'],"['neutrino, solar', 'astrophysics, model', 'model, solar', 'neutrino, flux', 'flux, neutrino', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404006'],"[""Given a Kamiokande event rate of larger than 36% (2.sigma.) of the prediction of Bahcall and Pinsonneault's standard solar model, variations of standard solar models yield minimal rates of 3.6 SNU for the Homestake experiment and 114 SNU for GALLEX and SAGE. Therefore, variations of standard solar models as solutions to the solar neutrino problem are so far ruled out by the Homestake experiment and marginally allowed by the gallium experiments. Unless there is a decrease in the .sup(3)He(.sup(4)He,.gamma.).sup(7)Be rate at low energy by a factor of \\ga 2 or an increase in the .sup(3)He(.sup(3)He,2p).sup(4)He rate at low energy by a factor of \\ga 4 with respect to the currently adopted values, the minimal rates that any solar models can possibly yield are 3.0 SNU for the Homestake experiment and 92 SNU for gallium experiments, although a successful model that achieves this extreme has yet to be seen.""]",['1994-04-07'] +2660,['eng'],"['Nagasawa, M', 'Yokoyama, J']",['Numerical analysis of the dynamics of a cosmic string loop as a vortex'],['Astrophysics and Astronomy'],"['space-time', 'gauge field theory, U(1)', 'Higgs model', 'vortex', 'astrophysics, string', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404041'],"['Time evolution of a circular cosmic string loop is investigated by numerically solving the field equations for the scalar and the gauge fields consisting of the vortex. It is shown that the result agrees with an analytic estimate based on the Nambu-Goto action, which supports its validity in analyzing nonstraight and rapidly moving strings.']",['2002-07-16'] +2661,['eng'],"['Ulmer, A']","[""Gamma-rays from grazing incidence cosmic rays in the earth's atmosphere""]",['Other Fields of Physics'],"['cosmic radiation, primary', 'photon, secondary radiation', 'cosmic radiation, secondary radiation', 'experimental methods, satellite', 'satellite, experimental methods', 'background', 'proposed experiment']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404025'],"[""Interactions of grazing incidence, ultra high energy cosmic rays with the earth's atmosphere may provide a new method of studying energetic cosmic rays with gamma-ray satellites. It is found that these cosmic ray interactions may produce gamma-rays on millisecond time scales which may be detectable by satellites. An extremely low gamma-ray background for transient gamma-ray events and a large area of interaction, the earth's surface, make the scheme plausible. The effective cross section of detection of interactions for cosmic rays above 10.sup(20) eV is found to be more than two orders of magnitude higher than earth based detection techniques. This method may eventually offer an efficient way of probing this region of the cosmic ray energy spectrum where events are scarce. In this paper, a conceptual model is presented for the production of short bursts of gamma-rays based on these grazing incidence encounters with the earth's atmosphere.""]",['1994-04-14'] +2662,['eng'],"['Johnson, P A']",['Contribution to the local cosmic-ray flux from the Geminga supernova'],['Other Fields of Physics'],"['astrophysics, supernova', 'cosmic radiation, particle source', 'photon, cosmic radiation', 'flux, cosmic radiation', 'cosmic radiation, flux', 'cosmic radiation, anisotropy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404004'],"['The contribution to the local cosmic-ray flux from the Geminga supernova is calculated assuming shock acceleration to 10.sup(14) eV in a remnant which was formed several 10.sup(5) years ago along with the Geminga pulsar. The particles are propagated to Earth using a simple diffusion model. In the region below the knee in the spectrum, it is found the supernova may contribute 10% of the local cosmic-ray flux, assuming plausible explosion parameters. The contribution to the amplitude of the anisotropy is not in conflict with the data in this energy region.']",['1994-04-07'] +2663,['eng'],"['Bahcall, J N', 'Barnes, C A', 'Christensen-Dalsgaard, J', 'Clevelend, B T', ""Degl'Innocenti, S"", 'Filippone, B W', 'Glasner, A', 'Kavanagh, R W', 'Koonin, S E', 'Lande, K', 'Kanganke, K', 'Parker, P D', 'Pinsonneault, M H', 'Proffitt, C R', 'Shoppa, T']",['Has a standard model solution to the solar neutrino problem been found?'],['Other Fields of Physics'],"['neutrino, solar', 'model, solar', 'nucleus nucleus, nuclear reaction', 'chlorine', 'cross section, energy dependence', 'neutrino, flux', 'flux, neutrino', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404002'],"['The claim by Dar and Shaviv that they have found a standard model solution to the solar neutrino problem is based upon an incorrect assumption made in extrapolating nuclear cross sections and the selective use of a small fraction of the nuclear physics and of the neutrino data. In addition, five different solar model codes show that the rate obtained for the chlorine experiment using the Dar-Shaviv stated parameters differs by at least 14 .sigma. from the observed rate.']",['1994-04-06'] +2664,['eng'],"['Kawasaki, M', 'Moroi, T']",['Gravitino production in the inflationary universe and the effects on big-bang nucleosynthesis'],['Other Fields of Physics'],"['inflationary universe', 'postulated particle, gravitino', 'production, gravitino', 'gravitino, production', 'radiative decay, gravitino', 'gravitino, radiative decay', 'mass, gravitino', 'gravitino, mass', 'temperature, upper limit', 'channel cross section', 'supergravity', 'energy spectrum, (photon)', '(photon), energy spectrum', 'Boltzmann equation, solution', 'postulated particle, photino', 'mass, photino', 'photino, mass', 'light nucleus, photofission', 'light nucleus, production', 'production, light nucleus', 'numerical calculations']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=hep-ph&id=9403364', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9403061']","['Gravitino production and decay in the inflationary universe are reexanimed. Assuming that gravitino mainly decays into photon and photino, we have calculated the upperbound of the reheating temperature. Compared to previous works, we have essentially improved the following two points; (i) the helicity \\pm\\frac{3}{2} gravitino production cross sections are calculated by using the full relevant terms in the supergravity lagrangian, and (ii) high energy photon spectrum is obtained by solving the Boltzmann equations numerically. Photo-dissociation of the light elements (D, T, ^3He, ^4He) leads to the most stringent upperbound of the reheating temperature, which is given by (10^{6}--10^{9})GeV for the gravitino mass 100GeV--1TeV. On the other hand, requiring that the present mass density of photino should be smaller than the critical density, we find that the reheating temperature have to be smaller than (10^{11}--10^{12})GeV for the photino mass (10--100)GeV, irrespectively of the gravitino mass. The effect of other decay channel is also considered.']",['1994-03-28'] +2665,['eng'],"['Sigl, G', 'Schramm, David N', 'Bhattacharjee, P']",['On the origin of highest energy cosmic rays'],['Other Fields of Physics'],"['astrophysics, model', 'cosmic radiation, particle source', 'cosmic radiation, primary', 'model, shock waves', 'relativistic', 'p, cosmic radiation', 'cosmic radiation, spatial distribution', 'magnetic field', 'astrophysics, pulsar', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9403039'],"[""In this paper we show that the conventional diffusive shock acceleration mechanism for cosmic rays associated with relativistic astrophysical shocks in active galactic nuclei (AGNs) has severe difficulties to explain the highest energy cosmic ray events. We show that protons above around 2\\times10^{20}\\eV could have marginally been produced by this mechanism in an AGN or a rich galaxy cluster not further away than around 100\\Mpc. However, for the highest energy Fly's Eye and Yakutsk events this is inconsistent with the observed arrival directions. Galactic and intergalactic magnetic fields appear unable to alter the direction of such energetic particles by more than a few degrees. We also discuss some other options for these events associated with relativistic particles including pulsar acceleration of high Z nuclei. At the present stage of knowledge the concept of topological defects left over from the early universe as the source for such events appears to be a promising option. Such sources are discussed and possible tests of this hypothesis are proposed.""]",['1994-03-18'] +2666,['eng'],"['Peter, P', 'Polarski, D', 'Starobinsky, A A']",['Confrontation of double-inflationary models with observations'],['Other Fields of Physics'],"['inflationary universe', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'field theory, scalar', 'spectra, perturbation', 'perturbation, spectra', 'velocity', 'production, galaxy', 'galaxy, production', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9403037'],"['We consider double-inflationary models with two noninteracting scalar fields, a light scalar field \\phi_l with potential \\frac{1}{2}m_l^2\\phi_l^2 and a heavy scalar field \\phi_h with potential \\frac{\\lambda}{n}\\phi_h^n with n=2,4. CDM with the initial spectrum of adiabatic perturbations produced in these models is compared with observations. These models contain two more free parameters than the standard CDM model with an initial scale-invariant spectrum. We normalize our spectra to COBE DMR and compare the predictions with observations on the biasing factor, large-scale peculiar velocities, quasar and galaxy formation and the Stromlo-APM counts-in-cells analysis. The model with n=4 is excluded by the data while for the n=2 model, taking cosmic variance into account, a small window of parameters compatible with observations is found.']",['1994-03-18'] +2667,['eng'],"['Kolb, E W', 'Tkachev, Igor I']",['Large-amplitude isothermal fluctuations and high-density dark-matter clumps'],['Other Fields of Physics'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'energy, density', 'matter, density', 'radiation, density', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9403011'],"['Large-amplitude isothermal fluctuations in the dark matter energy density, parameterized by $\\Phi\\equiv\\delta\\rhodm/\\rhodm$, are studied within the framework of a spherical collapse model. For $\\Phi \\ga 1$, a fluctuation collapses in the radiation-dominated epoch and produces a dense dark-matter object. The final density of the virialized object is found to be $\\rho_F \\approx 140\\, \\Phi^3 (\\Phi+1) \\rhoeq$, where $\\rhoeq$ is the matter density at equal matter and radiation energy density. This expression is valid for the entire range of possible values of $\\Phi$, both for $\\Phi \\gg 1$ and $\\Phi \\ll 1$. Some astrophysical consequences of high-density dark-matter clumps are discussed.']",['1994-03-08'] +2668,['eng'],"['Kolb, E W']",['Particle physics and cosmology'],['Other Fields of Physics'],"['lectures', 'astrophysics, model', 'cosmic radiation, background', 'light nucleus, production', 'production, light nucleus', 'inflationary universe', 'critical phenomena', 'gravitation, stability', 'numerical calculations, interpretation of experiments', 'bibliography']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9403007', 'http://fnalpubs.fnal.gov/archive/1994/conf/Conf-94-058-A.pdf']","['Lectures presented at the 42nd Scottish Universities Summer School in Physics, St. Andrews, Scotland, August 1993.']",['1994-03-04'] +2669,['eng'],"['Borrill, J']",['Numerical methods in cosmological global texture simulations'],['General Theoretical Physics'],"['astrophysics, texture', 'topology, defect', 'cosmic radiation, anisotropy', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9403006'],"['Numerical simulations of the evolution of a global topological defect field have two characteristic length scales --- one macrophysical, of order the field correlation length, and the other microphysical, of order the field width. The situation currently of most interest to particle cosmologists involves the behaviour of a GUT-scale defect field at the epoch of decoupling, where the ratio of these scales is typically of order $10^{50}$. Such a ratio is unrealisable in numerical work, and we consider the approximations which may be employed to deal with this. Focusing on the case of global texture we outline the implementation of the associated algorithms, and in particular note the subtleties involved in handling texture unwinding events. Comparing the results in each approach then establishes that, subject to certain constraints on the minimum grid resolution, the methods described are both robust and consistent with one another.']",['1994-03-04'] +2670,['eng'],"['Dodelson, S', 'Knox, L', 'Kolb, E W']",['Testing inflation with the cosmic microwave background'],['Other Fields of Physics'],"['inflationary universe, validity test', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'perturbation, scalar', 'perturbation, tensor', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9403004'],"['Cosmic microwave background (CMB) anisotropy may result from both scalar and tensor perturbations. For a sufficiently narrow range of angular scales, CMB perturbations can be characterized by four parameters. Results from the Cosmic Background Explorer fix one combination of the parameters, reducing the parameters to three. If CMB perturbations are from inflation, there is an additional relation, reducing the parameters to two. An appropriate combination of a medium-angle and a small-angle CMB observation can test the inflation hypothesis because inflation cannot explain a high signal in one experiment and a low signal in the other.']",['1994-03-04'] +2671,['eng'],"['Kolb, E W', 'Vadas, S L']",['Relating spectral indices to tensor and scalar amplitudes in inflation'],['General Theoretical Physics'],"['inflationary universe', 'density, perturbation', 'perturbation, scalar', 'perturbation, tensor', 'correction, higher-order', 'potential', 'chaos']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9403001'],"['Within an expansion in slow-roll inflation parameters, we derive second-order expressions relating the ratio of tensor to scalar density perturbations and the spectral index of the scalar spectrum. We find that ""corrections"" to previously derived formulae can dominate if the tensor to scalar ratio is small. For instance, if $V V\'\'/(V\')^2\\neq 1$ or if $m_{Pl}^2/(4\\pi) ~|V\'\'\'/V\'|\\ga 1$, where $V(\\phi)$ is the inflaton potential and $m_{Pl}$ is the Plank mass, then the previously used simple relations between the indices and the tensor to scalar ratio fails. This failure occurs in particular for natural inflation, Coleman-Weinberg inflation, and ""chaotic"" inflation.']",['1994-03-02'] +2672,['eng'],"['Nagasawa, M', 'Kawasaki, M']",['Collapse of axionic domain wall and axion emission'],['Other Fields of Physics'],"['domain wall, axion', 'string model, axion', 'emission, axion', 'axion, emission', 'energy, density', 'mass, density', 'density, mass', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402066'],['We examine the collapse of an axion domain wall bounded by an axionic string. It is found that the collapse proceeds quickly and axion domain walls disappear. However axions are emitted in the collapse and its energy density increases during radiation dominated era and contributes significantly to the present mass density of the universe. In particular the axion emitted from the wall can account for the dark matter in the universe for $F_a\\gsim 10^{10}\\GeV$.'],['1994-02-28'] +2673,['eng'],"['Spergel, D N', 'Pen, U L']",['Topological defects in an open universe'],['Astrophysics and Astronomy'],"['talk', 'astrophysics, model', 'astrophysics, galaxy', 'topology, defect', 'cosmic radiation, background', 'density, perturbation', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402044'],"['(To appear in Nuclear Physics B Supplements Proceedings section) This talk will explore the evolution of topological defects in an open universe. The rapid expansion of the universe in an open model slows defects and suppresses the generation of CBR fluctuations at large angular scale as does the altered relationship between angle and length in an open universe. Defect models, when normalized to COBE in an open universe, predict a galaxy power spectrum consistent with the galaxy power spectrum inferred from the galaxy surveys and do not require an extreme bias. Neither defect models in a flat universe nor standard inflationary models can fit either the multipole spectrum or the power spectrum inferred from galaxy surveys.']",['1996-04-15'] +2674,['eng'],"['Bayin, S S', 'Cooperstock, F I', 'Faraoni, V']",['A singularity-free cosmological model with a conformally coupled scalar field'],['General Theoretical Physics'],"['astrophysics, model', 'relativity theory, general', 'inflationary universe', 'field theory, scalar', 'coupling, conformal', 'conformal, coupling', 'critical phenomena', 'boundary condition', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402033'],"['We explore the possibility of describing our universe with a singularity-free, closed, spatially homogeneous and isotropic cosmological model, using only general relativity and a suitable equation of state which produces an inflationary era. A phase transition to a radiation-dominated era occurs as a consequence of boundary conditions expressing the assumption that the temperature cannot exceed the Planck value. We find that over a broad range of initial conditions, the predicted value of the Hubble parameter is approximately $47$ km$\\cdot$~s$^{- 1}\\cdot$~Mpc$^{-1}$. Inflation is driven by a scalar field, which must be conformally coupled to the curvature if the Einstein equivalence principle has to be satisfied. The form of the scalar field potential is derived, instead of being assumed a priori.']",['1994-02-14'] +2675,['eng'],"['Spergel, D N', 'Pen, U L', 'Kamionkowski, M P', 'Sugiyama, N']",['Microwave background fluctuations in an open universe'],['Astrophysics and Astronomy'],"['astrophysics, model', 'cosmic radiation, background', 'topology, defect', 'astrophysics, galaxy', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402060'],"['( to appear in: Proceedings of the Nishonomiya Yukawa Memorial Symposium Edited by M. Sasaki) There are several models for generating fluctuations in an open universe that are compatible with the microwave background fluctuations detected by COBE {\\it and} observations of large scale structure. Topological defects, such as strings and textures, appear to be more successful in a low-\\Omega model than in an \\Omega = 1 model. These models predict that the cosmic microwave background (CMB) fluctuations are non-Gaussian with distinctive signatures that may lead to their confirmation. If there exists a mechanism for generating scale invariant mass fluctuations, (\\delta M/M)^2 \\propto M^{-4/3}, then these models are also compatible with COBE. Both models predict mass fluctuations on the 8/h Mpc scale, \\sigma_8, \\sim 0.5 - 1 for \\Omega h \\sim 0.2 - 0.3. A variety of observations of large-scale structure, clusters and galaxies, as well as the age problem, suggest that the low-\\Omega models are attractive.']",['1996-04-15'] +2676,['eng'],"['Dodelson, S', 'Gyuk, G', 'Turner, M S']",['Is a massive tau neutrino just what cold dark matter needs?'],['Particle Physics - Phenomenology'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'perturbation, density', 'energy, density', 'cosmic radiation, anisotropy', 'light nucleus, production', 'production, light nucleus', 'numerical calculations, interpretation of experiments', 'neutrino/tau, massive', 'massive, neutrino/tau']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402028'],"['The cold dark matter (CDM) scenario for structure formation in the Universe is very attractive and has many successes; however, when its spectrum of density perturbations is normalized to the COBE anisotropy measurement the level of inhomogeneity predicted on small scales is too large. This can be remedied by a tau neutrino of mass $1\\MeV - 10\\MeV$ and lifetime $0.1\\sec - 100\\sec$ whose decay products include electron neutrinos because it allows the total energy density in relativistic particles to be doubled without interfering with nucleosynthesis. The anisotropies predicted on the degree scale for "".tau.CDM"" are larger than standard CDM. Experiments at $e^\\pm$ colliders may be able to probe such a mass range.']",['1994-02-14'] +2677,['eng'],"['Anderson, W J', 'Haubold, H J', 'Mathai, A M']",['Astrophysical thermonuclear functions'],['Other Fields of Physics'],"['talk', 'phi**n model, 4', 'finite temperature', 'renormalization group', 'perturbation theory, higher-order', 'higher-order, 2', 'mass']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402020'],['As theoretical knowledge and experimental verification of nuclear cross sections increases it becomes possible to refine analytic representations for nuclear reaction rates. In this paper mathematical/statistical techniques for deriving closed-form representations of thermonuclear functions are summarized and numerical results for them are given.The purpose of the paper is also to compare numerical results for approximate and closed-form representations of thermonuclear functions.'],['1994-02-09'] +2678,['eng'],"['Linde, Andrei D']",['Monopoles as big as a universe'],['General Theoretical Physics'],"['inflationary universe', 'field equations, monopole', 'domain wall', 'topology, defect', 'fractals, defect', 'field theory, scalar', 'Higgs model', 'gauge field theory, O(3)']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402031'],"['We show that, contrary to the standard belief, primordial monopoles expand exponentially during inflation in the new inflationary universe scenario. Moreover, inflation of monopoles continues without an end even when inflation ends in the surrounding space. Therefore primordial monopoles (as well as other topological defects produced during inflation) can serve as seeds for the process of eternal self-reproduction of inflationary universe.']",['1994-02-14'] +2679,['eng'],"['Liddle, A R', 'Turner, M S']",['Second-order reconstruction of the inflationary potential'],['General Theoretical Physics'],"['inflationary universe', 'potential', 'perturbation, scalar', 'perturbation, tensor', 'cosmic radiation, anisotropy', 'Pade approximation', 'correction', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402021'],"['To first order in the deviation from scale invariance the inflationary potential and its first two derivatives can be expressed in terms of the spectral indices of the scalar and tensor perturbations, $n$ and $n_T$, and their contributions to the variance of the quadrupole CBR temperature anisotropy, $S$ and $T$. In addition, there is a ""consistency relation"" between these quantities: $7 n_T = - T/S$. We derive the second-order expressions for the inflationary potential and its first two derivatives and the first-order expression for its third derivative, in terms of $n$, $n_T$, $S$, $T$, and $dn/d\\ln\\lambda$. We also obtain the second-order consistency relation, $n_T = -(1/7) (T/S) [ 1 + 0.11 T/S + 0.15 (n-1)]$. As an example we consider the exponential potential, the only known case where exact analytic solutions for the perturbation spectra exist. We reconstruct the potential via Taylor expansion (with coefficients calculated at both first and second order), and introduce the Pad\\\'{e} approximant as a greatly improved alternative.']",['1994-02-09'] +2680,['eng'],"['Kernan, P J', 'Krauss, L M']",['Refined big bang nucleosynthesis constraints on $\\Omega$sub(baryon) and N$_{\\nu}$'],['Other Fields of Physics'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'light nucleus, density', 'density, upper limit', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'neutrino, flavor', 'numerical calculations, Monte Carlo', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9402010'],"['We include correlations between elemental abundances in a Monte Carlo statistical analysis of BBN predictions, which, along with updated reaction rates and an improved BBN code, lead to tightened constraints on $\\Omega_{B}$ and $N_{\\nu}$. Observational upper limits on the primordial \\he and $\\rm {D + {^3He}}$ fractions of $24 \\%$ (by weight) and $ 10^{-4}$ respectively lead to the limits: $0.015 \\le \\Omega_{B} \\le 0.070$, and $N_{\\nu} \\le 3.04$. The former limit appears to be incompatible with purely baryonic galactic halo dark matter, while the latter puts qualitatively new constraints on neutrinos, and physics beyond the standard model.']",['1994-02-04'] +2681,['eng'],"['Dar, Arnon', 'Shaviv, G']",['A standard model solution to the solar neutrino problem?'],"['Other Fields of Physics', 'Astrophysics and Astronomy']","['neutrino, solar', 'neutrino, flux', 'flux, neutrino', 'plasma, effect', 'interpretation of experiments', 'neutrino, solar', 'neutrino, flux', 'flux, neutrino', 'plasma, effect', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401043'],"['An imroved standard solar model, with more accurate input parameters and more accurate treatment of plasma physics effects, predicts a solar neutrino flux which is consistent within experimental uncertainties with the solar neutrino observations after 1986.']",['1996-04-15'] +2682,['eng'],"['Bar-Kana, R']",['Limits on direct detection of gravitational waves'],['Other Fields of Physics'],"['gravitational radiation, counters and detectors', 'gravitational radiation, energy spectrum', 'energy spectrum, gravitational radiation', 'energy, density', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'inflationary universe', 'interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401050'],"['We compute energy density and strain induced by a primordial spectrum of gravitational waves on terrestrial- and space-based detectors (e.g., LIGO) as constrained by the COBE detection of microwave background anisotropy. For the case where the spectrum is created during inflation, we find new, stricter upper bounds on the induced strain, making detection unlikely. However, detectors might be useful for discovering (or ruling out) exotic, non-inflationary sources.']",['1994-01-31'] +2683,['eng'],"['García-Bellido, J']",['Jordan-Brans-Dicke stochastic inflation'],"['General Theoretical Physics', 'Astrophysics and Astronomy']","['inflationary universe, stochastic', 'Brans-Dicke model', 'postulated particle, inflaton', 'postulated particle, dilaton', 'field theory, scalar', 'perturbation theory', 'background field', 'bibliography', 'inflationary universe, stochastic', 'Brans-Dicke model', 'postulated particle, inflaton', 'postulated particle, dilaton', 'field theory, scalar', 'perturbation theory', 'background field', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401042'],"['We study stochastic inflation in the presence of a dynamical gravitational constant. We describe the Arnowitt--Deser--Misner formalism for Jordan--Brans--Dicke theory of gravity with an inflaton field. The inflaton and dilaton scalar fields can be separated into coarse-grained background fields and quantum fluctuations. We compute the amplitude of the perturbations generated by those quantum fluctuations in JBD theory with an arbitrary potential for the inflaton field. The effect of the quantum fluctuations on the background fields is equivalent to a Brownian motion of the scalar fields, which can be described with the use of a Fokker--Planck diffusion equation. The probability to find a given value of the fields in the comoving frame can be written as a Gaussian distribution centered on their classical trajectory, with decreasing dispersion along both field directions. We also calculate the condition for the Universe to enter a self-regenerating inflationary phase. The probability distribution in the physical frame, which takes into account the expansion of the proper volume of the inflationary domains, will be concentrated at the Planck boundary and will move along it towards large values of the fields.']",['1996-04-15'] +2684,['eng'],"['Vachaspati, T']",['Topological defects in cosmology'],['Other Fields of Physics'],"['lectures', 'astrophysics, string', 'defect, topological', 'magnetic field', 'domain wall', 'field equations, monopole', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401039'],['The scenario of a cosmology with topological defects is surveyed starting from the field theoretic aspects and ending with a description of large-scale structure formation and magnetic field generation.'],['1994-01-25'] +2685,['eng'],"['Copeland, E J', 'Liddle, A R', 'Lyth, D H', 'Stewart, E D', 'Wands, D']",['False vacuum inflation with Einstein gravity'],['General Theoretical Physics'],"['inflationary universe', 'chaos', 'field theory, scalar', 'vacuum state', 'postulated particle, inflaton', 'critical phenomena', 'production, bubble', 'bubble, production', 'density, perturbation', 'astrophysics, string', 'defect, topological', 'supergravity', 'numerical calculations', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401011'],"['We investigate chaotic inflation models with two scalar fields, such that one field (the inflaton) rolls while the other is trapped in a false vacuum state. The false vacuum becomes unstable when the inflaton field falls below some critical value, and a first or second order transition to the true vacuum ensues. Particular attention is paid to Linde\'s second-order ""Hybrid Inflation""; with the false vacuum dominating, inflation differs from the usual true vacuum case both in its cosmology and in its relation to particle physics. The spectral index of the adiabatic density perturbation can be very close to 1, or it can be around ten percent higher. The energy scale at the end of inflation can be anywhere between $10^{16}$\\,GeV and $10^{11}$\\,GeV, though reheating is prompt so the reheat temperature can\'t be far below $10^{11}\\,$GeV. Topological defects are almost inevitably produced at the end of inflation, and if the inflationary energy scale is near its upper limit they can have significant effects. Because false vacuum inflation occurs with the inflaton field far below the Planck scale, it is easier to implement in the context of supergravity than standard chaotic inflation. That the inflaton mass is small compared with the inflationary Hubble parameter is still a problem for generic supergravity theories, but remarkably this can be avoided in a natural way for a class of supergravity models which follow from orbifold compactification of superstrings. This opens up the prospect of a truly realistic, superstring']",['1994-01-12'] +2686,['eng'],"['Durrer, R']",['Light deflection in perturbed Friedmann universes'],['General Theoretical Physics'],"['Friedman model', 'photon', 'perturbation theory', 'invariance, gauge', 'gravitational radiation']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401033'],"['In this letter a new formula for light deflection is derived using only physically observable concepts. The general result is specialized to cosmological perturbation theory and expressed in terms of gauge-invariant perturbation variables. The resulting scalar, vector and tensor equations are supplemented by simple examples for illustration. The gravity wave example may be of more than academic interest and even represent a new way to detect gravitational waves.']",['1994-01-19'] +2687,['eng'],"['Adams, F C', 'Freese, Katherine']",['The scalar field potential in inflationary models'],['General Theoretical Physics'],"['inflationary universe', 'field theory, scalar', 'potential', 'spectra, density', 'density, spectra', 'perturbation, scalar', 'perturbation, tensor', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401006'],"['In this paper, we present quantitative constraints on the scalar field potential for a general class of inflationary models. (1) We first consider the reconstruction of the inflationary potential for given primordial density fluctuation spectra. Our work differs from previous work on reconstruction in that we find a semi-analytic solution for the potential for the case of density fluctuations with power-law spectra. In addition, for the case of more general spectra, we show how constraints on the density fluctuation spectra imply corresponding constraints on the potential. We present a series of figures which show how the shape of the potential depends on the shape of the perturbation spectrum and on the relative contribution of tensor modes. (2) We show that the average ratio $\\rave$ of the amplitude of tensor perturbations (gravity wave perturbations) to scalar density perturbations is bounded from above: $\\rave \\le$ 1.6. We also show that the ratio $\\rave$ is proportional to the change $\\Delta \\phi$ in the field: $\\rave \\approx 0.42 \\Delta \\phi/\\mp$. Thus, if tensor perturbations are important for the formation of structure, then the width $\\Delta \\phi$ must be comparable to the Planck mass. (3) We constrain the change $\\Delta V$ of the potential and the change $\\Delta \\phi$ of the inflation field during the portion of inflation when cosmological structure is produced. We find both upper and lower bounds for $\\Delta \\phi$ and for $\\Delta V$. In addition, these constraints are then used to derive a bound on the scale $\\Lambda$, which is the scale of the height of the potential']",['1994-01-10'] +2688,['eng'],"['Lyth, D H']",['Introduction to cosmology'],['General Theoretical Physics'],"['lectures', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'cosmic radiation, anisotropy', 'inflationary universe', 'astrophysics, fundamental constant', 'astrophysics, galaxy', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312022'],"['These notes form an introduction to cosmology with special emphasis on large scale structure, the cmb anisotropy and inflation. In some places a basic familiarity with particle physics is assumed, but otherwise no special knowledge is needed. Most of the material in the first two sections can be found in several texts, except that the discussion of dark matter and the cosmological constant is more up to date. Most of that in the remaining sections can be found in a review of structure formation and inflation done with Andrew Liddle, which describes original work by various authors including ourselves and Ewan Stewart. The reader is referred to these works for more detail, and a very complete list of references.']",['1993-12-13'] +2689,['eng'],"['Ma Chung Pei', 'Bertschinger, E']",['Cosmological perturbation theory in the synchronous vs. conformal Newtonian gauge'],['General Theoretical Physics'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'gravitation', 'perturbation theory', 'invariance, gauge', 'transformation, gauge', 'Boltzmann equation', 'Einstein equation', 'tensor, energy-momentum', 'model, fluid', 'density, perturbation', 'astrophysics, horizon', 'neutrino, phase space', 'photon', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401007'],"['We present a systematic treatment of the linear theory of scalar gravitational perturbations in the synchronous gauge and the conformal Newtonian (or longitudinal) gauge. We first derive the transformation law relating the two gauges. We then write down in parallel in both gauges the coupled, linearized Boltzmann, Einstein and fluid equations that govern the evolution of the metric perturbations and the density fluctuations of the particle species. The particle species considered include cold dark matter (CDM), baryons, photons, massless neutrinos, and massive neutrinos (a hot dark matter or HDM candidate), where the CDM and baryon components are treated as fluids while a detailed phase-space description is given to the photons and neutrinos. The linear evolution equations presented are applicable to any $\\Omega=1$ model with CDM or a mixture of CDM and HDM. Isentropic initial conditions on super-horizon scales are derived. The equations are solved numerically in both gauges for a CDM+HDM model with $\\Omega_{\\rm cold}=0.65,$ $\\Omega_{\\rm hot}=0.3$, and $\\Omega_{\\rm baryon}=0.05$. We discuss the evolution of the metric and the density perturbations and compare their different behaviors outside the horizon in the two gauges. In a companion paper we integrate the geodesic equations for the neutrino particles in the perturbed conformal Newtonian background metric computed here. The purpose is to obtain an accurate sampling of the neutrino phase space for the HDM initial conditions in $N$-body simulations of the CDM+HDM models.']",['1994-01-10'] +2690,['eng'],"['Giudice, Gian F', 'Mollerach, S', 'Roulet, Esteban']",['Can EROS/MACHO be detecting the galactic spheroid instead of the galactic halo?'],['Other Fields of Physics'],"['astrophysics, galaxy', 'astrophysics, model', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312047'],"['Models of our galaxy based on dynamical observations predict a spheroid component much heavier than accounted for by direct measurements of star counts and high velocity stars. If, as first suggested by Caldwell and Ostriker, this discrepancy is due to a large population of faint low-mass stars or dark objects in the spheroid, the spheroid could be responsible for microlensing events for sources in the LMC. We show that, although the rate of events is lower than predicted by a galactic halo made of microlensing objects, it is still significant for EROS/MACHO observations. Because of the different matter distributions in the halo and spheroid components, a comparison between microlensing event rates in the LMC, future measurements of microlensing in the galactic bulge and, possibly, in M31 can provide information about the amounts of dark objects in the different galactic components. If the EROS/MACHO collaborations find a deficiency with respect to their halo expectation, when more statistics are available, their detected events could be interpreted as coming from spheroid microlenses, allowing for a galactic halo composed entirely of non-baryonic dark matter.']",['1993-12-20'] +2691,['eng'],"['Elizondo, D', 'Yepes, G']",['Can conformal Weyl gravity be considered a viable cosmological theory?'],['General Theoretical Physics'],"['gravitation, Weyl', 'invariance, conformal', 'astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'field equations, solution', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312064'],['We present exact analytical solutions to the Conformal Weyl Gravity cosmological equations that are valid for both the matter and radiation dominated eras. The Primordial Nucleosynthesis process is also exhaustively studied. The main conclusion of our work is that cosmological models derived from this theory are not likely to reproduce the observational properties of our Universe. They fail to fulfill simultaneously the observational constraints on present cosmological parameters and on primordial light element abundances.'],['1994-01-10'] +2692,['eng'],"['Aharonian, F A', 'Coppi, P S', 'Völk, H J']",['Very high energy gamma-rays from AGN'],['Other Fields of Physics'],"['photon, cosmic radiation', 'cosmic radiation, particle source', 'astrophysics, galaxy', 'cosmic radiation, background', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312045'],"['Recent high energy gamma-ray observations (E > 100 MeV) of blazar AGN show emission spectra with no clear upper energy cutoff. AGN, considered to be possible sources for the highest energy cosmic rays, may have emission extending well into the VHE (very high energy, E > 100 GeV) domain. Because VHE gamma-rays are absorbed by pair production on the intergalactic background radiation, much of this emission is not visible. Electromagnetic cascades initiated by absorbed VHE gamma-rays, however, may be observable. Since the velocities of e+e- pairs produced in a cascade are likely to be isotropized by an ambient random magnetic field, extended ""halos"" (R > 1 Mpc) of pairs will be formed around AGN with VHE emission. Cascade radiation from these pair halos is emitted isotropically and is observable below a few TeV. The halo radiation can be distinguished by its characteristic variation in spectrum and intensity with angular distance from the central source. This variation depends weakly on the details of the central source model, e.g., the orientation and beaming/opening angle of an emitting jet. Limiting or determining the intensity of the pair halo can thus serve as a model-independent bound on or measure of the VHE power of AGN. Next-generation Cherenkov telescopes may be able to image a pair halo.']",['1993-12-20'] +2693,['eng'],"['Gangui, A', 'Lucchin, F', 'Matarrese, S', 'Mollerach, S']",['The three-point correlation function of the cosmic microwave background in inflationary models'],['Other Fields of Physics'],"['inflationary universe, stochastic', 'cosmic radiation, background', 'cosmic radiation, anisotropy', 'correlation function', 'vertex function', 'temperature', 'potential, gravitation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312033'],"['We analyze the temperature three-point correlation function and the skewness of the Cosmic Microwave Background (CMB), providing general relations in terms of multipole coefficients. We then focus on applications to large angular scale anisotropies, such as those measured by the {\\em COBE} DMR, calculating the contribution to these quantities from primordial, inflation generated, scalar perturbations, via the Sachs--Wolfe effect. Using the techniques of stochastic inflation we are able to provide a {\\it universal} expression for the ensemble averaged three-point function and for the corresponding skewness, which accounts for all primordial second-order effects. These general expressions would moreover apply to any situation where the bispectrum of the primordial gravitational potential has a {\\em hierarchical} form. Our results are then specialized to a number of relevant models: power-law inflation driven by an exponential potential, chaotic inflation with a quartic and quadratic potential and a particular case of hybrid inflation. In all these cases non-Gaussian effects are small: as an example, the {\\em mean} skewness is much smaller than the cosmic {\\em rms} skewness implied by a Gaussian temperature fluctuation field.']",['1993-12-16'] +2694,['eng'],"['Jetzer, Philippe', 'Massó, E']",['On the mass of the dark compact halo objects'],"['Other Fields of Physics', 'Other Fields of Physics']","['astrophysics, MACHO', 'mass, MACHO', 'MACHO, mass', 'numerical calculations, interpretation of experiments', 'astrophysics, MACHO', 'mass, MACHO', 'MACHO, mass', 'numerical calculations, interpretation of experiments']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=hep-ph&id=9312321', 'http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312050']","['Recently the French EROS collaboration and the American-Australian MACHO collaboration have reported the observation of altogether three possible microlensing events by monitoring over several years the brightness of millions of stars in the Large Magellanic Cloud. For each of these events, assuming they are due to microlensing, we compute the most likely mass for the dark compact halo object, which acted as gravitational lens. The most likely masses are 0.12, 0.31 and 0.38 $M_{\\odot}$. The average mass calculated using the method of moments turns out to be 0.14 $M_{\\odot}$.']",['1993-12-14'] +2695,['eng'],"['Starkman, G D', 'Kaiser, N', 'Malaney, R A']",['Mixed dark matter from neutrino lasing'],['Other Fields of Physics'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'production, missing-mass', 'missing-mass, production', 'neutrino, massive', 'massive, neutrino', 'neutrino, decay', 'decay, neutrino', 'Boltzmann equation', 'spin, polarization', 'polarization, spin', 'postulated particle, Majoron', 'Majoron, singlet', 'neutrino --> boson fermion']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312020'],"['We investigate the production of dark matter with non-standard momentum distributions arising from the decay of a relativistic massive neutrino into a lighter fermion and boson H --> F + B. We develop the Boltzmann equations for this process, paying particular attention to spin polarisation effects. Such decays can, under certain circumstances, lead to a process of runaway stimulated decays or ""neutrino-lasing"" resulting, for suitable boson mass, in the production of mixed-dark-matter. We discuss a number of variations on the model; we show how the yield of cold particles can be increased by a simple modification to our original proposal. We discuss the singlet-majoron model as a possible framework for these decays.']",['1993-12-13'] +2696,['eng'],"['Bahcall, J N']",['Solar neutrinos'],['Other Fields of Physics'],"['talk, Paris 1993/09/22', 'neutrino, solar', 'model, solar', 'neutrino, flux', 'flux, neutrino', 'numerical calculations, interpretation of experiments', 'bibliography']","['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312002', 'http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=scan&id=P00020232']","['The four operating solar neutrino experiments confirm the hypothesis that the energy source for solar luminosity is hydrogen fusion. However, the measured rate for each of the four solar neutrino experiments differs significantly (by factors of 2.0 to 3.5) from the corresponding theoretical prediction that is based upon the standard solar model and the simplest version of the standard electroweak theory. If standard electroweak theory is correct, the energy spectrum for \\b8 neutrinos created in the solar interior must be the same (to one part in $10^5$) as the known laboratory \\b8 neutrino energy spectrum. Direct comparison of the chlorine and the Kamiokande experiments, both sensitive to \\b8 neutrinos, suggests that the discrepancy between theory and observations depends upon neutrino energy, in conflict with standard expectations. Monte Carlo studies with 1000 implementations of the standard solar model confirm that the chlorine and the Kamiokande experiments cannot be reconciled unless new weak interaction physics changes the shape of the \\b8 neutrino energy spectrum. The results of the two gallium solar neutrino experiments strengthen the conclusion that new physics is required and help determine a relatively small allowed region for the MSW neutrino parameters.']",['1994-01-21'] +2697,['eng'],"['Hirai, T', 'Maeda, K I']",['Gauge-invariant cosmological perturbations in generalized Einstein theories'],['General Theoretical Physics'],"['astrophysics, perturbation', 'invariance, gauge', 'relativity theory, general', 'Brans-Dicke model', 'field theory, scalar', 'transformation, conformal', 'density, perturbation', 'production, galaxy', 'galaxy, production', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9404023'],"['Using the covariant approach and conformal transformations, we present a gauge-invariant formalism for cosmological perturbations in generalized Einstein theories (GETs), including the Brans-Dicke theory, theories with a non-minimally coupled scalar field and certain curvature-squared theories. We find an enhancement in the growth rate of density perturbations in the Brans-Dicke theory, and discuss attractive features of GETs in the structure formation process.']",['1994-04-13'] +2698,['eng'],"['Gondolo, P']",['Dark matter annihilations in the large magellanic cloud'],['Particle Physics - Phenomenology'],"['talk', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'photon, cosmic radiation', 'cluster, galaxy', 'postulated particle, WIMP', 'annihilation, WIMP', 'WIMP, annihilation', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312011'],"['The flat rotation curve obtained for the outer star clusters of the Large Magellanic Cloud is suggestive of an LMC dark matter halo. From the composite HI and star cluster rotation curve, I estimate the parameters of an isothermal dark matter halo added to a ""maximum disk"". I then examine the possibility of detecting high energy gamma-rays from non-baryonic dark matter annihilations in the central region of the Large Magellanic Cloud.']",['1993-12-07'] +2699,['eng'],"['Olesen, M L', 'Madsen, J']",['Nucleation of quark matter bubbles in neutron stars'],['Other Fields of Physics'],"['astrophysics', 'n, matter', 'quark, matter', 'matter, strangeness', 'production, bubble', 'bubble, production', 'mean field approximation', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9401002'],"['The thermal nucleation of quark matter bubbles inside neutron stars is examined for various temperatures which the star may realistically encounter during its lifetime. It is found that for a bag constant less than a critical value, a very large part of the star will be converted into the quark phase within a fraction of a second. Depending on the equation of state for neutron star matter and strange quark matter, all or some of the outer parts of the star may subsequently be converted by a slower burning or a detonation.']",['1994-01-10'] +2700,['eng'],"['Fuller, G M', 'Jedamzik, K', 'Mathews, G J', 'Olinto, A V']",['On constraining electroweak-baryogenesis with inhomogeneous primordial nucleosynthesis'],['Astrophysics and Astronomy'],"['astrophysics', 'light nucleus, production', 'production, light nucleus', 'electroweak interaction, critical phenomena', 'critical phenomena, electroweak interaction', 'baryon number', 'baryon, bubble']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9407034'],['Primordial nucleosynthesis calculations are shown to be able to provide constraints on electroweak baryogenesis which produce a highly inhomogeneous distribution of the baryon-to-photon ratio. Such baryogenesis scenarios overproduce 4He and/or 7Li and can be ruled out whenever a fraction f<3*10e-6(100 GeV/T)^3 of nucleated bubbles of broken-symmetry phase contributes > 10% of the baryon number within the horizon volume.'],['1994-07-13'] +2701,['eng'],"['Biermann, P L', 'Strom, R G']","['Cosmic Rays, III. The CR spectrum between 1 GeV and 10^4 GeV and the radio emission from supernova remnants']",['Astrophysics and Astronomy'],"['cosmic radiation, acceleration', 'shock waves', 'astrophysics, supernova', 'magnetic field', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9303013'],"['We develop a theory to account for the cosmic ray spectrum between 1 GeV and 10^4 GeV following the earlier papers of this series. We use the basic concept that the cosmic ray particles are accelerated in a supernova shock that travels through the interstellar medium. Physically important ingredients besides the presence of a strong shock are diffusion, drifts, convection, adiabatic cooling, the injection history, and the topology of the magnetic field, here assumed for simplicity to be homogeneous in the interstellar medium. The result is a spectrum, which for strong shocks in a gas with adiabatic index 5/3 yields a spectrum of E^-2.42. Interstellar turbulence with a Kolmogorov spectrum then leads by leakage from the galactic disk to a spectrum which is E^-2.75, as observed. We argue that the ratio of cosmic ray electrons to protons is determined by the amount of expansion which takes place from the cessation of electron injection to the break-up of the shell by cooling instabilities. Since the highest particle energy reached derives from geometrical arguments, it depends on the charge of the nucleus and so higher Z elements are predicted to reach higher energies.']",['2002-03-13'] +2702,['eng'],"['Jedamzik, K', 'Fuller, G M', 'Mathews, G J', 'Kajino, T']",['Enhanced heavy-element formation in baryon-inhomogeneous big-bang models'],['Other Fields of Physics'],"['astrophysics, model', 'light nucleus, production', 'production, light nucleus', 'baryon, density', 'inflationary universe', 'neutrino', 'critical phenomena', 'numerical calculations, interpretation of experiments', 'bibliography']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312066'],"['We show that primordial nucleosynthesis in baryon inhomogeneous big-bang models can lead to significant heavy-element production while still satisfying all the light-element abundance constraints including the low lithium abundance observed in population II stars. The parameters which admit this solution arise naturally from the process of neutrino induced inflation of baryon inhomogeneities prior to the epoch of nucleosynthesis. These solutions entail a small fraction of baryons (\\le 2\\%) in very high density regions with local baryon-to-photon ratio $\\eta^h\\approx 10^{-4}$, while most baryons are at a baryon-to-photon ratio which optimizes the agreement with light-element abundances. The model would imply a unique signature of baryon inhomogeneities in the early universe, evidenced by the existence of primordial material containing heavy-element products of proton and alpha- burning reactions with an abundance of $[Z]\\sim -6 to -4$.']",['1994-01-12'] +2703,['eng'],"['Jedamzik, K', 'Fuller, G M']",['The evolution of non-linear sub-horizon scale entropy fluctuations in the early universe'],['General Theoretical Physics'],"['astrophysics, model', 'inflationary universe', 'astrophysics, horizon', 'entropy', 'light nucleus, production', 'production, light nucleus', 'model, hydrodynamical', 'thermodynamics', 'numerical calculations']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312063'],"['We examine the damping of non-linear sub-horizon scale entropy fluctuations in early epochs of the universe ($T\\approx 100$ GeV to $T\\approx 1$keV) by neutrino, baryon, and photon induced dissipative processes. Results of numerical evolution calculations are presented for broad ranges of initial fluctuation amplitudes and length scales. These calculations include a detailed treatment of neutrino inflation, neutron and proton diffusion, photon diffusive heat transport, and hydrodynamic expansion with photon-electron Thomson drag. Neutrino inflation is treated both in the diffusive heat transport regime where neutrinos are optically thick on the length scales of the fluctuations, and in the homogeneous heating regime where neutrinos are optically thin on these scales. We find considerable convergence in amplitude evolution for appreciable ranges in initial fluctuation length scales and amplitudes. Fluctuations produced with the right characteristics at very early times ($T$ $^>_{\\sim}$ 100 GeV) are found to survive through the nucleosynthesis epoch.']",['1994-01-10'] +2704,['eng'],"['Melott, A L', 'Splinter, R J', 'Persic, M', 'Salucci, P']",['Decaying neutrinos in galaxy clusters'],['Particle Physics - Phenomenology'],"['neutrino, astrophysics', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, galaxy', 'galaxy, cluster', 'neutrino, flux', 'flux, neutrino', 'neutrino, radiative decay', 'radiative decay, neutrino', 'photon, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'neutrino, density', 'numerical calculations, interpretation of experiments']",['http://preprints.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9312014'],"[""Davidsen et al. (1991) have argued that the failure to detect uv photons from the dark matter DM) in cluster A665 excludes the decaying neutrino hypothesis. Sciama et al. (1993) argued that because of high central concentration the DM in that cluster must be baryonic. We study the DM profile in clusters of galaxies simulated using the Harrison--Zel'dovich spectrum of density fluctuations, and an amplitude previously derived from numerical simulations (Melott 1984b; Anninos et al. 1991) and in agreement with microwave background fluctuations (Smoot et al. 1992). We find that with this amplitude normalization cluster neutrino DM densities are comparable to observed cluster DM values. We conclude that given this normalization, the cluster DM should be at least largely composed of neutrinos. The constraint of Davidsen et al. can be somewhat weakened by the presence of baryonic DM; but it cannot be eliminated given our assumptions.""]",['1993-08-26'] +2705,['eng'],"['Loeb, A']",['Are Gamma-Ray Bursts at Cosmological Distances Optically-Thin?'],['Astrophysics and Astronomy'],"['cosmic radiation, spatial distribution', 'photon, cosmic radiation', 'cosmic radiation, flux', 'flux, cosmic radiation', 'postulated particle, axion', 'mass, axion', 'axion, mass', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'astrophysics, supernova', 'interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9308048'],"['The observed spatial distribution of $\\gamma-$ray bursts indicates that they probably originate at cosmological distances. At this distance scale their variability timescale and flux above MeV imply an initial optical-depth to pair production $> 10^{10}$. This appears to be in conflict with their highly non-thermal spectra. We show that this difficulty can be removed if axion bursts from supernovae are converted to $\\gamma-$rays over cosmological distances. Nonthermal bursts with the relevant flux, duration, variability and spectra are obtained just for the range of axion masses of $10^{-5}-10^{-4}{\\rm eV}$ that accounts for the cold dark matter in the universe. The observed rate of $\\gamma-$ray bursts implies that axions should be converted efficiently to photons in only one out of $\\sim 10^{4}$ supernovae.']",['2002-03-18'] +2706,['eng'],"['Cheng, B', 'Schramm, David N', 'Truran, J W']",['Interaction Rates at High Magnetic Field Strengths and High Degeneracy'],['Astrophysics and Astronomy'],"['charged particle, relativistic', 'magnetic field', 'astrophysics', 'weak interaction', 'strong interaction']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9308035'],"['In this paper, we have derived the the effects of strong magnetic fields ${\\bf \\vec B}$ on nucleon and particle reaction rates of astrophysical significance. We have explored the sensitivity to the presence of arbitrary degeneracy and polarization. The possible astrophysical applications of our results are discussed.']",['2002-03-18'] +2707,['eng'],"['Bahcall, J N']",['Solar Neutrino Experiments'],['Astrophysics and Astronomy'],"['talk', 'neutrino, solar', 'model, solar', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9307013'],"['Physics beyond the simplest version of the standard electroweak model is required to reconcile the results of the chlorine and the Kamiokande solar neutrino experiments. None of the 1000 solar models in a full Monte Carlo simulation is consistent with the results of the chlorine or the Kamiokande experiments. Even if the solar models are forced articficially to have a ${}^8 B$ neutrino flux in agreement with the Kamiokande experiment, none of the fudged models agrees with the chlorine observations. This comparison shows that consistency of the chlorine and Kamiokande experiments requires some physical process that changes the shape of the ${}^8 B$ neutrino energy spectrum. The GALLEX and SAGE experiments, which currently have large statistical uncertainties, differ from the predictions of the standard solar model by $2 \\sigma$ and $3 \\sigma$, respectively. The possibility that the neutrino experiments are incorrect is briefly discussed.']",['2002-03-15'] +2708,['eng'],"['Ma Chung Pei', 'Bertschinger, E']",['A Calculation of the Full Neutrino Phase Space in Cold+Hot Dark Matter Models'],['Astrophysics and Astronomy'],"['astrophysics, missing-mass', 'missing-mass, astrophysics', 'gravitation', 'perturbation theory, relativistic', 'invariance, gauge', 'transformation, gauge', 'invariance, conformal', 'Boltzmann equation', 'Einstein equation', 'model, fluid', 'neutrino, phase space', 'neutrino, massive', 'massive, neutrino', 'many-body problem', 'neutrino, density', 'density, perturbation', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9308006'],"['This paper presents a general-relativistic N-body technique for evolving the phase space distribution of massive neutrinos in linear perturbation theory. The method provides a much more accurate sampling of the neutrino phase space for the HDM initial conditions of N-body simulations in a cold+hot dark matter universe than previous work. Instead of directly sampling the phase space at the end of the linear era, we first compute the evolution of the metric perturbations by numerically integrating the coupled, linearized Einstein, Boltzmann, and fluid equations for all particle species. We then sample the phase space shortly after neutrino decoupling at redshift z=10^9 when the distribution is Fermi-Dirac. To follow the trajectory of each neutrino, we subsequently integrate the geodesic equations for each neutrino in the perturbed background spacetime from z=10^9 to z=13.55, using the linearized metric found in the previous calculation to eliminate discreteness noise. The positions and momenta resulting from this integration represent a fair sample of the full neutrino phase space and can be used as HDM initial conditions for N-body simulations of nonlinear structure evolution in this model. A total of 21 million neutrino particles are used in a 100 Mpc box, with Omega_cdm=0.65, Omega_hdm=0.30, Omega_baryon=0.05, and Hubble constant H_0=50. We find that correlations develop in the neutrino densities and momenta which are absent when only the zeroth-order Fermi-Dirac distribution is considered.']",['2002-03-18'] +2709,['eng'],"['Bruni, M', 'Lyth, D H']","['Peculiar Velocity, Cosmic Perturbation Theory and the CMB Anisotropy']",['Astrophysics and Astronomy'],"['relativity theory, general', 'astrophysics, model', 'energy, density', 'perturbation theory', 'cosmic radiation, background', 'microwaves', 'anisotropy']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9307036'],"['This is a somewhat extended version of the original July 93 report. It is proved that the cosmological density perturbation is associated with a peculiar velocity field. This allows a simple formulation of cosmological perturbation theory, which works entirely with quasi-Newtonian fluid flow equations. As an illustration, the large scale cosmic microwave background anisotropy (Sachs-Wolfe effect) is calculated without any reference to the metric perturbation. In addition, assuming the usual adiabatic initial condition on the density perturbation, we show that the dipole of the anisotropy measures our peculiar velocity relative to the average peculiar velocity within the last scattering surface of the microwave background, thus defining its frame of reference.']",['2002-03-15'] +2710,['eng'],"['Shi, X', 'Schramm, David N', 'Fields, B D']",['Constraints on Neutrino Oscillations from Big Bang Nucleosynethesis'],['Astrophysics and Astronomy'],"['astrophysics', 'light nucleus, production', 'production, light nucleus', 'neutrino, oscillation', 'neutrino, mixing angle', 'temperature, high', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9307027'],"['We discuss in detail the effect of neutrino oscillations in Big Bang nucleosynthesis, between active and sterile neutrinos, as well as between active and active neutrinos. We calculate the constraints on mixings between active and sterile neutrinos from the present observation of the primordial helium abundance and discuss the potential implications on various astrophysical and cosmological problems of such oscillations. In particular, we show that large angle sterile neutrino mixing seems to be excluded as a MSW solution to the solar neutrino situation or a solution to the atmospheric neutrino mixing hinted at in some underground experiments. We show how with this constraint, the next generation of solar neutrino experiments should be able to determine the resolution of the solar neutrino problem. It is also shown how sterile neutrinos remain a viable dark matter candidate.']",['2002-03-15'] +2711,['eng'],"['Crittenden, R', 'Davis, R L', 'Steinhardt, Paul Joseph']",['Polarization of the Microwave Background due to Primordial Gravitational Waves'],['Astrophysics and Astronomy'],"['cosmic radiation, background', 'polarization', 'gravitational radiation', 'energy, density', 'ionization', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9306027'],"['The contribution of gravitational wave (tensor metric) and energy density (scalar metric) fluctuations to the cosmic microwave background polarization is computed by numerically solving the relativistic radiation transfer equations. We find that the tensor contribution is significant only at large angular scales (multipoles $\\ell \\lta 40$). For standard recombination, the tensor contribution can dominate at $\\ell \\lta 40$; however, the effect would be difficult to detect since the total (scalar plus tensor) polarization is $< 1$\\%. For models with late reionization, the total large angular scale polarization is large ($\\sim 7-9$\\%), but the tensor fraction is negligibly small. Hence, polarization may be useful for discriminating ionization history, but is much less promising as a means for detecting tensor fluctuations.']",['2002-03-15'] +2712,['eng'],"['Kochanek, C S', 'Piran, T']",['Gravitational Waves and $\\gamma$-Ray Bursts'],['Astrophysics and Astronomy'],"['gravitational radiation, counters and detectors', 'photon, cosmic radiation', 'cosmic radiation, particle source', 'proposed experiment', 'numerical calculations']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9305015'],"['Coalescing binaries in distant galaxies are one of the most promising sources of gravitational waves detectable by the LIGO project.$^{[1-5]}$ They are also a copious source of neutrinos,$^{[1]}$ however these neutrino pulses are far too weak to be detected on earth. Several years ago Eichler \\etal$\\,']",['2002-03-15'] +2713,['eng'],"['Rachen, J P', 'Stanev, T', 'Biermann, P L']","['Extragalactic ultra high energy cosmic rays, II. Comparison with experimental data']",['Astrophysics and Astronomy'],"['photon, cosmic radiation', 'p, cosmic radiation', 'nucleus, cosmic radiation', 'cosmic radiation, energy spectrum', 'energy spectrum, cosmic radiation', 'cosmic radiation, background', 'cosmic radiation, flux', 'flux, cosmic radiation', 'astrophysics', 'magnetic field', 'cosmic radiation, acceleration', 'shock waves', 'numerical calculations, interpretation of experiments']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9302005'],"['We compare the expected contribution of FR-II hot spots to the ultra-high energy cosmic ray spectrum (Rachen & Biermann 1993, A&A in press, BB paper astro-ph/9301010) to improved experimental results. We introduce a ""world data set"" of UHE cosmic rays by comparing the data of various experiments, extracting relative systematic errors in the energy derivation and averaging over energy bins. Since the contribution of FR-II hot spots is expected to be dominated by protons, we can also compare it to the recent experimental results for the proton component of cosmic rays between 0.1 and 1 EeV from both the Fly\'s Eye and the Akeno airshower detector (Gaisser et al. 1993, Phys Rev D in press, and Stanev et al. 1992, A&A submitted). The result is striking: Our prediction for energies below 1 EeV fits very well to the data for the proton component, while explaining the total flux at highest energies as well. The result is consistent with the expectation of a galactic component, consisting of heavy nuclei only, that has a slope of about -3.1 and cuts off at 5 EeV, as predicted by Biermann 1993 (A&A in press, BB paper astro-ph/9301008)']",['2002-03-13'] +2714,['eng'],"['Turner, M S']",['Dark Matter'],['Astrophysics and Astronomy'],"['review, Irvine 1992/03', 'astrophysics, missing-mass', 'missing-mass, astrophysics', 'postulated particle, axion', 'neutrino, production', 'production, neutrino', 'sparticle, neutral particle', 'bibliography']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9302003'],['Talk presented at NAS Special Colloquium on Physical Cosmology'],['2002-03-13'] +2715,['eng'],"['Hu, Y', 'Turner, M S', 'Weinberg, Erick J']",['Dynamical Solutions to the Horizon and Flatness Problems'],['Astrophysics and Astronomy'],"['inflationary universe', 'entropy, production', 'production, entropy', 'field theory, action', 'approximation, adiabatic']",['http://documents.cern.ch/cgi-bin/setlink?base=preprint&categ=astro-ph&id=9302002'],"['We discuss in some detail the requirements on an early-Universe model that solves the horizon and flatness problems during the epoch of classical cosmology ($t\\ge t_i\\gg 10^{-43}\\sec$). We show that a dynamical resolution of the horizon problem requires superluminal expansion (or very close to it) and that a truly satisfactory resolution of the flatness problem requires entropy production. This implies that a proposed class of adiabatic models in which the Planck mass varies by many orders of magnitude cannot fully resolve the flatness problem. Furthermore, we show that, subject to minimal assumptions, such models cannot solve the horizon problem either. Because superluminal expansion and entropy production are the two generic features of inflationary models, our results suggest that inflation, or something very similar, may be the only dynamical solution to the horizon and flatness problems.']",['2002-03-13']