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801.4473 | Predrag Jovanovic | P. Jovanovi\'c, A. F. Zakharov, L. \v{C}. Popovi\'c, T. Petrovi\'c | Microlensing of the X-ray, UV and optical emission regions of quasars:
Simulations of the time-scales and amplitude variations of microlensing
events | 11 pages, 9 figures and 2 tables. Accepted for publication in MNRAS | null | 10.1111/j.1365-2966.2008.13036.x | null | astro-ph | null | We consider the influence of microlensing on different spectral bands of
lensed QSOs. We assumed that the emitting X-ray, UV and optical regions are
different in size, but that the continuum emission in these spectral bands is
originating from an accretion disc. Estimations of the time scales for
microlensing and flux amplification in different bands are given. We found that
the microlensing duration should be shorter in the X-ray (several months) than
in UV/optical emitting region (several years). This result indicates that
monitoring of the X-ray variations in lensed QSOs that show a 'flux anomaly'
can clarify the source of this anomaly.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 11:28:09 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Jovanović",
"P.",
""
],
[
"Zakharov",
"A. F.",
""
],
[
"Popović",
"L. Č.",
""
],
[
"Petrović",
"T.",
""
]
] | [
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801.4474 | Andrew Becker | A.C.Becker, E.Agol, N.M.Silvestri, J.J.Bochanski, C.Laws, A.A.West,
G.Basri, V.Belokurov, D.M.Bramich, J.M.Carpenter, P.Challis, K.R.Covey,
R.M.Cutri, N.W.Evans, M.Fellhauer, A.Garg, G.Gilmore, P.Hewett, P.Plavchan,
D.P.Schneider, C.L.Slesnick, S.Vidrih, L.M.Walkowicz, D.B.Zucker | 2MASS J01542930+0053266 : A New Eclipsing M-dwarf Binary System | 8 figures and 3 tables, accepted for publication in MNRAS | Mon.Not.Roy.Astron.Soc.386:416-424,2008 | 10.1111/j.1365-2966.2008.13040.x | null | astro-ph | null | We report on 2MASS J01542930+0053266, a faint eclipsing system composed of
two M dwarfs. The variability of this system was originally discovered during a
pilot study of the 2MASS Calibration Point Source Working Database. Additional
photometry from the Sloan Digital Sky Survey yields an 8-passband lightcurve,
from which we derive an orbital period of 2.6390157 +/- 0.0000016 days.
Spectroscopic followup confirms our photometric classification of the system,
which is likely composed of M0 and M1 dwarfs. Radial velocity measurements
allow us to derive the masses (M_1 = 0.66 +/- 0.03 M_sun; M_2 = 0.62 +/- 0.03
M_sun) and radii (R_1 = 0.64 +/- 0.08 R_sun; R_2 = 0.61 +/- 0.09 R_sun) of the
components, which are consistent with empirical mass-radius relationships for
low-mass stars in binary systems. We perform Monte Carlo simulations of the
lightcurves which allow us to uncover complicated degeneracies between the
system parameters. Both stars show evidence of H-alpha emission, something not
common in early-type M dwarfs. This suggests that binarity may influence the
magnetic activity properties of low-mass stars; activity in the binary may
persist long after the dynamos in their isolated counterparts have decayed,
yielding a new potential foreground of flaring activity for next generation
variability surveys.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 18:45:16 GMT"
}
] | 2010-04-29T00:00:00 | [
[
"Becker",
"A. C.",
""
],
[
"Agol",
"E.",
""
],
[
"Silvestri",
"N. M.",
""
],
[
"Bochanski",
"J. J.",
""
],
[
"Laws",
"C.",
""
],
[
"West",
"A. A.",
""
],
[
"Basri",
"G.",
""
],
[
"Belokurov",
"V.",
""
],
[
"Bramich",
"D. M.",
""
],
[
"Carpenter",
"J. M.",
""
],
[
"Challis",
"P.",
""
],
[
"Covey",
"K. R.",
""
],
[
"Cutri",
"R. M.",
""
],
[
"Evans",
"N. W.",
""
],
[
"Fellhauer",
"M.",
""
],
[
"Garg",
"A.",
""
],
[
"Gilmore",
"G.",
""
],
[
"Hewett",
"P.",
""
],
[
"Plavchan",
"P.",
""
],
[
"Schneider",
"D. P.",
""
],
[
"Slesnick",
"C. L.",
""
],
[
"Vidrih",
"S.",
""
],
[
"Walkowicz",
"L. M.",
""
],
[
"Zucker",
"D. B.",
""
]
] | [
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801.4475 | Franco Pellegrini | Franco Pellegrini, Simone Montangero, Giuseppe E. Santoro, Rosario
Fazio | Adiabatic quenches through an extended quantum critical region | 4 pages, 4 figures | null | 10.1103/PhysRevB.77.140404 | null | cond-mat.other | null | By gradually changing the degree of the anisotropy in a XXZ chain we study
the defect formation in a quantum system that crosses an extended critical
region. We discuss two qualitatively different cases of quenches, from the
antiferromagnetic to the ferromagnetic phase and from the critical to the
antiferromegnetic phase. By means of time-dependent DMRG simulations, we
calculate the residual energy at the end of the quench as a characteristic
quantity gauging the loss of adiabaticity. We find the dynamical scalings of
the residual energy for both types of quenches, and compare them with the
predictions of the Kibble-Zurek and Landau-Zener theories.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 17:03:36 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Pellegrini",
"Franco",
""
],
[
"Montangero",
"Simone",
""
],
[
"Santoro",
"Giuseppe E.",
""
],
[
"Fazio",
"Rosario",
""
]
] | [
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801.4476 | Nikolai Nikolov | Nikolai Nikolov, Peter Pflug and Pascal J. Thomas | Lipschitzness of the Lempert and Green functions | minor changes | Proc. Amer. Math. Soc. 137 (2009), 2027-2036 | null | null | math.CV | null | Necessary and sufficient conditions for Lipschitzness of the Lempert and
Green functions are found in terms of their boundary behaviors.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:50:47 GMT"
},
{
"version": "v2",
"created": "Tue, 3 Jun 2008 13:12:23 GMT"
}
] | 2010-06-23T00:00:00 | [
[
"Nikolov",
"Nikolai",
""
],
[
"Pflug",
"Peter",
""
],
[
"Thomas",
"Pascal J.",
""
]
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801.4477 | Hossein Farajollahi | Hossein Farajollahi | Time and Observables in Unimodular General Relativity | 16 pages | Gen.Rel.Grav.37:383-390,2005 | 10.1007/s10714-005-0025-z | null | gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A cosmological time variable is emerged from the hamiltonian formulation of
unimodular theory of gravity to measure the evolution of dynamical observables
in the theory. A set of constants of motion has been identified for the theory
on the null hypersurfaces that its evolution is with respect to the volume
clock introduced by the cosmological time variable.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 11:56:09 GMT"
},
{
"version": "v2",
"created": "Thu, 9 Jun 2011 04:52:24 GMT"
}
] | 2015-05-13T00:00:00 | [
[
"Farajollahi",
"Hossein",
""
]
] | [
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801.4478 | Elias C. Vagenas | M. R. Setare, Elias C. Vagenas | Thermodynamical Interpretation of the Interacting Holographic Dark
Energy Model in a non-flat Universe | 12 pages, no figure, LaTeX; v2: 13 pages now, comments and
clarifications added, to appear in Phys. Lett. B | Phys.Lett.B666:111-115,2008 | 10.1016/j.physletb.2008.07.013 | null | hep-th astro-ph gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Motivated by the recent work of Wang, Lin, Pavon, and Abdalla [1], we
generalize their work to the non-flat case. In particular, we provide a
thermodynamical interpretation for the holographic dark energy model in a
non-flat universe. For this case, the characteristic length is no more the
radius of the event horizon (R_E) but the event horizon radius as measured from
the sphere of the horizon (L). Furthermore, when interaction between the dark
components of the holographic dark energy model in the non-flat universe is
present its thermodynamical interpretation changes by a stable thermal
fluctuation. A relation between the interaction term of the dark components and
this thermal fluctuation is obtained. In the limiting case of a flat universe,
i.e. k=0, all results given in [1] are obtained.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:11:21 GMT"
},
{
"version": "v2",
"created": "Wed, 9 Jul 2008 17:41:51 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Setare",
"M. R.",
""
],
[
"Vagenas",
"Elias C.",
""
]
] | [
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801.4479 | Chitta Ranjan Das | C.R. Das, S. Digal and T.R. Govindarajan | Spontaneous symmetry breakdown in fuzzy spheres | 8 pages, 7 figures | Mod.Phys.Lett.A24:2693-2701,2009 | 10.1142/S021773230902859X | CHEP-PKU/1/01-2008, IMSC/2008/01/01 | hep-th hep-lat | null | We study and analyse the questions regarding breakdown of global symmetry on
noncommutative sphere. We demonstrate this by considering a complex scalar
field on a fuzzy sphere and isolating Goldstone modes. We discuss the role of
nonlocal interactions present in these through geometrical considerations.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:21:13 GMT"
},
{
"version": "v2",
"created": "Wed, 13 Feb 2008 09:03:41 GMT"
}
] | 2009-11-19T00:00:00 | [
[
"Das",
"C. R.",
""
],
[
"Digal",
"S.",
""
],
[
"Govindarajan",
"T. R.",
""
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801.448 | Babatunde Okunoye | Babatunde O. Okunoye | Abstractions for biomolecular computations | 9 pages, 2 figures | null | null | null | cs.OH | null | Deoxyribonucleic acid is increasingly being understood to be an informational
molecule, capable of information processing.It has found application in the
determination of non-deterministic algorithms and in the design of molecular
computing devices. This is a theoretical analysis of the mathematical
properties and relations of the molecules which constituting DNA, which
explains in part why DNA is a successful computing molecule.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:12:11 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Okunoye",
"Babatunde O.",
""
]
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801.4481 | Henri Gouin | Henri Gouin (MSNMGP, LMMT) | Energy of interaction between solid surfaces and liquids | 16 pages | The Journal of Physical Chemistry B 102, 7 (1998) 1212-1218 | 10.1021/jp9723426 | null | physics.chem-ph physics.atom-ph | null | We consider the wetting transition on a planar surface in contact with a
semi-infinite fluid. In the classical approach, the surface is assumed to be
solid, and when interaction between solid and fluid is sufficiently
short-range, the contribution of the fluid can be represented by a surface free
energy with a density of the form Phi(rho_s), where rho_s is the limiting
density of the fluid at the surface. In the present paper we propose a more
precise representation of the surface energy that takes into account not only
the value of rho_s but also the contribution from the whole density profile
rho(z) of the fluid, where z is the coordinate normal to the surface. The
specific value of the functional of rho_s at the surface is expressed in
mean-field approximation through the potentials of intermolecular interaction
and some other parameters of the fluid and the solid wall. An extension to the
case of fluid mixtures in contact with a solid surface is proposed.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:21:29 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Gouin",
"Henri",
"",
"MSNMGP, LMMT"
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] |
801.4482 | Christophe Jouvet | Gilles Gr\'egoire (LPL), Bruno Lucas (LCAM), Michel Barat (LCAM),
Jacqueline Fayeton (LCAM), Claude Dedonder-Lardeux (PPM), Christophe Jouvet
(PPM) | Photoinduced dynamics in protonated aromatic amino acid | null | null | 10.1140/epjd/e2008-00085-3 | null | physics.atm-clus | null | UV photoinduced fragmentation of protonated aromatics amino acids have
emerged the last few years, coming from a situation where nothing was known to
what we think a good understanding of the optical properties. We will mainly
focus this review on the tryptophan case. Three groups have mostly done
spectroscopic studies and one has mainly been involved in dynamics studies of
the excited states in the femtosecond/picosecond range and also in the
fragmentation kinetics from nanosecond to millisecond. All these data, along
with high level ab initio calculations, have shed light on the role of the
different electronic states of the protonated molecules upon the fragmentation
mechanisms.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:25:08 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Grégoire",
"Gilles",
"",
"LPL"
],
[
"Lucas",
"Bruno",
"",
"LCAM"
],
[
"Barat",
"Michel",
"",
"LCAM"
],
[
"Fayeton",
"Jacqueline",
"",
"LCAM"
],
[
"Dedonder-Lardeux",
"Claude",
"",
"PPM"
],
[
"Jouvet",
"Christophe",
"",
"PPM"
]
] | [
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] |
801.4483 | Jocelyne Troccaz | Jean-Alexandre Long (TIMC), Vincent Daanen (TIMC), Alexandre
Moreau-Gaudry (TIMC, CHU-Grenoble CIC), Jocelyne Troccaz (TIMC), Jean-Jacques
Rambeaud, Jean-Luc Descotes | Biopsies prostatiques sous guidage \'echographique 3D et temps r\'eel
(4D) sur fant\^ome. Etude comparative versus guidage 2D | null | Progr\`es en Urologie 17, 7 (2007) 1137-1143 | null | null | cs.OH | null | This paper analyzes the impact of using 2D or 3D ultrasound on the efficiency
of prostate biopsies. The evaluation is performed on home-made phantoms. The
study shows that the accuracy is significantly improved.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:26:02 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Long",
"Jean-Alexandre",
"",
"TIMC"
],
[
"Daanen",
"Vincent",
"",
"TIMC"
],
[
"Moreau-Gaudry",
"Alexandre",
"",
"TIMC, CHU-Grenoble CIC"
],
[
"Troccaz",
"Jocelyne",
"",
"TIMC"
],
[
"Rambeaud",
"Jean-Jacques",
""
],
[
"Descotes",
"Jean-Luc",
""
]
] | [
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] |
801.4484 | Maria Lu\'isa Arruda | Lu\'isa Arruda, Fernando Bar\~ao, Patr\'icia Goncalves, Rui Pereira | The Ring Imaging Cherenkov detector of the AMS experiment: test beam
results with a prototype | 4 pages, 5 figures. Contribution to the 10th Topical Seminar on
Innovative Particle and Radiation Detectors (Siena, Italy 2006) | Nucl.Phys.Proc.Suppl.172:32-35,2007 | 10.1016/j.nuclphysbps.2007.07.025 | null | astro-ph | null | The Alpha Magnetic Spectrometer (AMS) to be installed on the International
Space Station (ISS) will be equipped with a proximity Ring Imaging Cherenkov
(RICH) detector for measuring the velocity and electric charge of the charged
cosmic particles. This detector will contribute to the high level of redundancy
required for AMS as well as to the rejection of albedo particles. Charge
separation up to iron and a velocity resolution of the order of 0.1% for singly
charged particles are expected. A RICH protoptype consisting of a detection
matrix with 96 photomultiplier units, a segment of a conical mirror and samples
of the radiator materials was built and its performance was evaluated. Results
from the last test beam performed with ion fragments resulting from the
collision of a 158 GeV/c/nucleon primary beam of indium ions (CERN SPS) on a
lead target are reported. The large amount of collected data allowed to test
and characterize different aerogel samples and the sodium fluoride radiator. In
addition, the reflectivity of the mirror was evaluated. The data analysis
confirms the design goals.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:40:40 GMT"
}
] | 2010-11-26T00:00:00 | [
[
"Arruda",
"Luísa",
""
],
[
"Barão",
"Fernando",
""
],
[
"Goncalves",
"Patrícia",
""
],
[
"Pereira",
"Rui",
""
]
] | [
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] |
801.4485 | Irena Skwirczynska | V. A. Karnaukhov, H. Oeschler, A. Budzanowski, S.P. Avdeyev, A. S.
Botvina, E. A. Cherepanov, W. Karcz, V. V. Kirakosyan, P.A. Rukoyatkin, I.
Skwirczynska, E. Norbeck | Critical temperature for the nuclear liquid-gas phase transition (from
multifragmentation and fission) | 15 pages, 8 figures | null | 10.1134/S1063778808120077 | null | nucl-ex | null | Critical temperature Tc for the nuclear liquid-gas phase transition is
stimated both from the multifragmentation and fission data. In the first
case,the critical temperature is obtained by analysis of the IMF yields in
p(8.1 GeV)+Au collisions within the statistical model of multifragmentation
(SMM). In the second case, the experimental fission probability for excited
188Os is compared with the calculated one with Tc as a free parameter. It is
concluded for both cases that the critical temperature is higher than 16 MeV.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:40:46 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Karnaukhov",
"V. A.",
""
],
[
"Oeschler",
"H.",
""
],
[
"Budzanowski",
"A.",
""
],
[
"Avdeyev",
"S. P.",
""
],
[
"Botvina",
"A. S.",
""
],
[
"Cherepanov",
"E. A.",
""
],
[
"Karcz",
"W.",
""
],
[
"Kirakosyan",
"V. V.",
""
],
[
"Rukoyatkin",
"P. A.",
""
],
[
"Skwirczynska",
"I.",
""
],
[
"Norbeck",
"E.",
""
]
] | [
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] |
801.4486 | Vladimir Zirakashvili | V.N.Zirakashvili, V.S.Ptuskin, H.J.Voelk | Modeling Bell's Non-resonant Cosmic Ray Instability | 12 pages, 4 figures, accepted to ApJ | null | 10.1086/529579 | null | astro-ph | null | We have studied the non-resonant streaming instability of charged energetic
particles moving through a background plasma, discovered by Bell (2004). We
confirm his numerical results regarding a significant magnetic field
amplification in the system. A detailed physical picture of the instability
development and of the magnetic field evolution is given.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:43:13 GMT"
},
{
"version": "v2",
"created": "Mon, 4 Feb 2008 11:55:47 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Zirakashvili",
"V. N.",
""
],
[
"Ptuskin",
"V. S.",
""
],
[
"Voelk",
"H. J.",
""
]
] | [
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] |
801.4487 | Charles Hill | Charles D. Hill, Henry L. Haselgrove | Universal quantum dynamics from two 2-local Hamiltonians | null | null | null | null | quant-ph | null | In this paper, we show that the ability to switch globally between two
2-local Hamiltonians on n qubits is sufficient for achieving universal unitary
dynamics on those n qubits. Of the two Hamiltonians used in the construction,
one is comprised of nearest-neighbour two-qubit interactions on a
one-dimensional chain, the other is comprised of single-qubit interactions. We
describe a scheme for choosing the switching times in order to generate
arbitrary one- and two-qubit gates on the n qubits. However the switching
scheme is inefficient, and we leave as an open problem the question of whether
the universality of the Hamiltonians can be exploited in an efficient way.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 12:55:03 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Hill",
"Charles D.",
""
],
[
"Haselgrove",
"Henry L.",
""
]
] | [
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] |
801.4488 | Vladimir Zirakashvili | V.N.Zirakashvili, V.S.Ptuskin | Diffusive Shock Acceleration with Magnetic Amplification by Non-resonant
Streaming Instability in SNRs | 18 pages, 9 figures, accepted to ApJ | null | 10.1086/529580 | null | astro-ph | null | We investigate the diffusive shock acceleration in the presence of the
non-resonant streaming instability introduced by Bell (2004). The numerical MHD
simulations of the magnetic field amplification combined with the analytical
treatment of cosmic ray acceleration permit us to calculate the maximum energy
of particles accelerated by high-velocity supernova shocks. The estimates for
Cas A, Kepler, SN1006, and Tycho historical supernova remnants are given. We
also found that the amplified magnetic field is preferentially oriented
perpendicular to the shock front downstream of the fast shock. This explains
the origin of the radial magnetic fields observed in young supernova remnants.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 13:02:43 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Zirakashvili",
"V. N.",
""
],
[
"Ptuskin",
"V. S.",
""
]
] | [
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] |
801.4489 | Raquel Crespo | R. Crespo, A. Deltuva, E. Cravo, M. Rodriguez-Gallardo, A.C. Fonseca | Multiple scattering effects in quasi free scattering from halo nuclei: a
test to Distorted Wave Impulse Approximation | 7 pages, 16 figures, to be published in Phys. Rev. C | Phys.Rev.C77:024601,2008 | 10.1103/PhysRevC.77.024601 | null | nucl-th | null | Full Faddeev-type calculations are performed for $^{11}$Be breakup on proton
target at 38.4, 100, and 200 MeV/u incident energies. The convergence of the
multiple scattering expansion is investigated. The results are compared with
those of other frameworks like Distorted Wave Impulse Approximation that are
based on an incomplete and truncated multiple scattering expansion.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 13:04:45 GMT"
}
] | 2008-12-18T00:00:00 | [
[
"Crespo",
"R.",
""
],
[
"Deltuva",
"A.",
""
],
[
"Cravo",
"E.",
""
],
[
"Rodriguez-Gallardo",
"M.",
""
],
[
"Fonseca",
"A. C.",
""
]
] | [
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] |
801.449 | Giovanni Manfredi | G. Manfredi, P.-A. Hervieux | Fidelity decay in trapped Bose-Einstein condensates | 4 pages, to appear in Physical Review Letters, February 2008 | null | 10.1103/PhysRevLett.100.050405 | null | quant-ph | null | The quantum coherence of a Bose-Einstein condensate is studied using the
concept of quantum fidelity (Loschmidt echo). The condensate is confined in an
elongated anharmonic trap and subjected to a small random potential such as
that created by a laser speckle. Numerical experiments show that the quantum
fidelity stays constant until a critical time, after which it drops abruptly
over a single trap oscillation period. The critical time depends
logarithmically on the number of condensed atoms and on the perturbation
amplitude. This behavior may be observable by measuring the interference
fringes of two condensates evolving in slightly different potentials.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 13:15:11 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Manfredi",
"G.",
""
],
[
"Hervieux",
"P. -A.",
""
]
] | [
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] |
801.4491 | Thierry Morel | T. Morel (1,2), S. Hubrig (3) and M. Briquet (1) ((1) KU Leuven, (2)
Liege University, (3) ESO) | Nitrogen enrichment, boron depletion and magnetic fields in
slowly-rotating B-type dwarfs | Accepted by A&A. 11 pages, 4 figures (some in colour) | null | 10.1051/0004-6361:20078999 | null | astro-ph | null | Evolutionary models for massive stars, accounting for rotational mixing
effects, do not predict any core-processed material at the surface of B dwarfs
with low rotational velocities. Contrary to theoretical expectations, we
present a detailed and fully-homogeneous, NLTE abundance analysis of 20 early
B-type dwarfs and (sub)giants that reveals the existence of a population of
nitrogen-rich and boron-depleted, yet intrinsically slowly-rotating objects.
The low-rotation rate of several of these stars is firmly established, either
from the occurrence of phase-locked UV wind line-profile variations, which can
be ascribed to rotational modulation, or from theoretical modelling in the
pulsating variables. The observational data presently available suggest a
higher incidence of chemical peculiarities in stars with a (weak) detected
magnetic field. This opens the possibility that magnetic phenomena are
important in altering the photospheric abundances of early B dwarfs, even for
surface field strengths at the one hundred Gauss level. However, further
spectropolarimetric observations are needed to assess the validity of this
hypothesis.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 13:16:43 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Morel",
"T.",
""
],
[
"Hubrig",
"S.",
""
],
[
"Briquet",
"M.",
""
]
] | [
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] |
801.4492 | Athanassios Akylas | A. Akylas and I. Georgantopoulos | Can photo-ionization explain the decreasing fraction of X-ray obscured
AGN with luminosity? | 7 pages 4 figures A&A accepted | null | 10.1051/0004-6361:20077791 | null | astro-ph | null | Chandra and XMM surveys show that the fraction of obscured AGN decreases
rapidly with increasing luminosity. Although this is usually explained by
assuming that the covering factor of the central engine is much smaller at
luminous QSOs, the exact origin of this effect remains unknown. We perform toy
simulations to test whether photo-ionisation of the obscuring screen in the
presence of a strong radiation field can reproduce this effect. In particular,
we create X-ray spectral simulations using a warm absorber model assuming a
range of input column densities and ionization parameters. We fit instead the
simulated spectra with a simple cold absorption power-law model that is the
standard practice in X-ray surveys. We find that the fraction of absorbed AGN
should fall with luminosity as $L^{-0.16\pm0.03}$ in rough agreement with the
observations. Furthermore, this apparent decrease in the obscuring material is
consistent with the dependence of the FeK$\alpha$ narrow-line equivalent width
on luminosity, ie. the X-ray Baldwin effect.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 13:29:30 GMT"
},
{
"version": "v2",
"created": "Wed, 30 Jan 2008 13:31:25 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Akylas",
"A.",
""
],
[
"Georgantopoulos",
"I.",
""
]
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] |
801.4493 | Henrik Beuther | H. Beuther, D. Semenov, Th. Henning, H. Linz | Ethynyl (C2H) in massive star formation: Tracing the initial conditions? | Accepted for Astrophysical Journal Letters, 4 pages, 3 figures, for a
high-resolution version, see http://www.mpia.de/homes/beuther/papers.html | null | 10.1086/533412 | null | astro-ph | null | APEX single-dish observations at sub-millimeter wavelengths toward a sample
of massive star-forming regions reveal that C2H is almost omni-present toward
all covered evolutionary stages from Infrared Dark Clouds via High-Mass
Protostellar Objects to Ultracompact HII regions. High-resolution data from the
Submillimeter Array toward one hot-core like High-Mass Protostellar Object show
a shell-like distribution of C2H with a radius of ~9000AU around the central
submm peak position. These observed features are well reproduced by a 1D cloud
model with power-law density and temperature distributions and a gas-grain
chemical network. The reactive C2H radical (ethynyl) is abundant from the onset
of massive star formation, but later it is rapidly transformed to other
molecules in the core center. In the outer cloud regions the abundance of C2H
remains high due to constant replenishment of elemental carbon from CO being
dissociated by the interstellar UV photons. We suggest that C2H may be a
molecule well suited to study the initial conditions of massive star formation.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 13:32:19 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Beuther",
"H.",
""
],
[
"Semenov",
"D.",
""
],
[
"Henning",
"Th.",
""
],
[
"Linz",
"H.",
""
]
] | [
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] |
801.4494 | Seyed Ahmad Sabok-Sayr | Seyed Ahmad Sabok-Sayr | The simplest and fastest method of solving Exact Differential Equation
by developing the idea of Basic Functions | 8 pages | null | null | null | math.GM | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | This paper concerns exact differential equations. First, I define two types
of functions which I have named Basic Function of Type One and Basic Function
of Type Two. I then derive the property and theorems of these functions.
Finally, by applying the property and theorems of Basic Functions, I establish
the method of solving exact differential equation with n variables which is
significantly simpler and faster than the standard method.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:49:34 GMT"
},
{
"version": "v2",
"created": "Wed, 6 Feb 2008 20:19:18 GMT"
},
{
"version": "v3",
"created": "Wed, 8 Oct 2008 10:45:28 GMT"
}
] | 2008-10-08T00:00:00 | [
[
"Sabok-Sayr",
"Seyed Ahmad",
""
]
] | [
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] |
801.4495 | Lisheng Geng | L. S. Geng, J. Martin Camalich, L. Alvarez-Ruso, and M. J. Vicente
Vacas | Nucleon-to-Delta axial transition form factors in relativistic baryon
chiral perturbation theory | A few clarifying remarks added; version to appear in Physical Review
D | Phys.Rev.D78:014011,2008 | 10.1103/PhysRevD.78.014011 | null | hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We report a theoretical study of the axial Nucleon to Delta(1232)
($N\to\Delta$) transition form factors up to one-loop order in relativistic
baryon chiral perturbation theory. We adopt a formalism in which the $\Delta$
couplings obey the spin-3/2 gauge symmetry and, therefore, decouple the
unphysical spin-1/2 fields. We compare the results with phenomenological form
factors obtained from neutrino bubble chamber data and in quark models.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 13:54:50 GMT"
},
{
"version": "v2",
"created": "Thu, 10 Jul 2008 16:18:06 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Geng",
"L. S.",
""
],
[
"Camalich",
"J. Martin",
""
],
[
"Alvarez-Ruso",
"L.",
""
],
[
"Vacas",
"M. J. Vicente",
""
]
] | [
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] |
801.4496 | Raymond Fresard | Raymond Fresard, Henni Ouerdane, and Thilo Kopp | Barnes slave boson approach to the two-site single impurity Anderson
model with non-local interaction | 6 pages, 2 figures, published version | Europhys. Lett. 82, 31001 (2008) | 10.1209/0295-5075/82/31001 | null | cond-mat.str-el | null | The Barnes slave boson approach to the $U=\infty$ single impurity Anderson
model extended by a non-local Coulomb interaction is revisited. We demonstrate
first that the radial gauge representation facilitates the treatment of such a
non-local interaction by performing the \emph{exact} evaluation of the path
integrals representing the partition function, the impurity hole density and
the impurity hole density autocorrelation function for a two-site cluster. The
free energy is also obtained on the same footing. Next, the exact results are
compared to their approximations at saddle-point level, and it is shown that
the saddle point evaluation recovers the exact answer in the limit of strong
non-local Coulomb interaction, while the agreement between both schemes remains
satisfactory in a large parameter range.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 13:51:05 GMT"
},
{
"version": "v2",
"created": "Wed, 30 Apr 2008 08:15:39 GMT"
}
] | 2008-04-30T00:00:00 | [
[
"Fresard",
"Raymond",
""
],
[
"Ouerdane",
"Henni",
""
],
[
"Kopp",
"Thilo",
""
]
] | [
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] |
801.4497 | Henning Schomerus | Henning Schomerus, Eric Lutz | Controlled decoherence in a quantum L\'evy kicked rotator | 15 pages, 8 figures | Phys. Rev. A 77, 062113 (2008) | 10.1103/PhysRevA.77.062113 | null | quant-ph | null | We develop a theory describing the dynamics of quantum kicked rotators
(modelling cold atoms in a pulsed optical field) which are subjected to
combined amplitude and timing noise generated by a renewal process (acting as
an engineered reservoir). For waiting-time distributions of variable exponent
(L\'evy noise), we demonstrate the existence of a regime of nonexponential loss
of phase coherence. In this regime, the momentum dynamics is subdiffusive,
which also manifests itself in a non-Gaussian limiting distribution and a
fractional power-law decay of the inverse participation ratio. The purity
initially decays with a stretched exponential which is followed by two regimes
of power-law decay with different exponents. The averaged logarithm of the
fidelity probes the sprinkling distribution of the renewal process. These
analytical results are confirmed by numerical computations on quantum kicked
rotators subjected to noise events generated by a Yule-Simon distribution.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:00:46 GMT"
}
] | 2008-07-11T00:00:00 | [
[
"Schomerus",
"Henning",
""
],
[
"Lutz",
"Eric",
""
]
] | [
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] |
801.4498 | Fabien Alet | K.S.D. Beach, Matthieu Mambrini, Fabien Alet | Comment on "Quantum Monte Carlo scheme for frustrated Heisenberg
antiferromagnets" | 2 pages | Phys. Rev. B 77, 146401 (2008) | 10.1103/PhysRevB.77.146401 | null | cond-mat.str-el cond-mat.stat-mech | null | Quantum Monte Carlo methods are sophisticated numerical techniques for
simulating interacting quantum systems. In some cases, however, they suffer
from the notorious "sign problem" and become too inefficient to be useful. A
recent publication [J. Wojtkiewicz, Phys. Rev. B 75, 174421 (2007)] claims to
have solved the sign problem for a certain class of frustrated quantum spin
systems through the use of a bipartite valence bond basis. We show in this
Comment that the apparent positivity of the path integral is due to a
misconception about the resolution of the identity operator in this basis, and
that consequently the sign problem remains a severe obstacle for the simulation
of frustrated quantum magnets.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:12:59 GMT"
}
] | 2008-05-16T00:00:00 | [
[
"Beach",
"K. S. D.",
""
],
[
"Mambrini",
"Matthieu",
""
],
[
"Alet",
"Fabien",
""
]
] | [
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] |
801.4499 | Charles Bordenave | Charles Bordenave | On the birth-and-assassination process, with an application to scotching
a rumor in a network | 16 pages | null | null | null | math.PR | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We give new formulas on the total number of born particles in the stable
birth-and-assassination process, and prove that it has an heavy-tailed
distribution. We also establish that this process is a scaling limit of a
process of rumor scotching in a network, and is related to a predator-prey
dynamics.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:15:17 GMT"
},
{
"version": "v2",
"created": "Mon, 20 Oct 2008 18:24:38 GMT"
}
] | 2008-10-20T00:00:00 | [
[
"Bordenave",
"Charles",
""
]
] | [
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801.45 | Jorge Sotomayor | Jorge Sotomayor | On the motion under focal attraction in a rotating medium | null | null | null | null | math.DS math.CA | null | New results are established here on the phase portraits and bifurcations of
the kinematic model in a system of ODE's, first presented by H.K. Wilson in his
1971 book, and by him attributed to L. Markus (unpublished). A new,
self-sufficient, study which extends Wilson's result and allows an essential
conclusion for the applicability of the model is reported here.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:21:13 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Sotomayor",
"Jorge",
""
]
] | [
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801.4501 | Yonathan Schwarzkopf | Yonathan Schwarzkopf, M. R. Evans and David Mukamel | Zero-Range Processes with Multiple Condensates: Statics and Dynamics | 25 pages, 18 figures | J. Phys. A: Math. Theor. 41 (2008) 205001 | 10.1088/1751-8113/41/20/205001 | null | cond-mat.stat-mech | null | The steady-state distributions and dynamical behaviour of Zero Range
Processes with hopping rates which are non-monotonic functions of the site
occupation are studied. We consider two classes of non-monotonic hopping rates.
The first results in a condensed phase containing a large (but subextensive)
number of mesocondensates each containing a subextensive number of particles.
The second results in a condensed phase containing a finite number of extensive
condensates. We study the scaling behaviour of the peak in the distribution
function corresponding to the condensates in both cases. In studying the
dynamics of the condensate we identify two timescales: one for creation, the
other for evaporation of condensates at a given site. The scaling behaviour of
these timescales is studied within the Arrhenius law approach and by numerical
simulations.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 04:04:06 GMT"
},
{
"version": "v2",
"created": "Wed, 30 Apr 2008 13:17:36 GMT"
}
] | 2008-04-30T00:00:00 | [
[
"Schwarzkopf",
"Yonathan",
""
],
[
"Evans",
"M. R.",
""
],
[
"Mukamel",
"David",
""
]
] | [
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] |
801.4502 | F.-Xavier Desert | F.-X. Desert (1), J. F. Macias-Perez (2), F. Mayet (2), G. Giardino
(7), C. Renault (2), J. Aumont (2), A. Benoit (3), J.-Ph. Bernard (4), N.
Ponthieu (5), and M. Tristram (6) ((1) LAOG Grenoble, (2) LPSC Grenoble, (3)
CRTBT Grenoble, (4) CESR Toulouse, (5) IAS Orsay, (6) LAL Orsay, (7) ESTEC
Noordwijk) | Submillimetre point sources from the Archeops experiment: Very Cold
Clumps in the Galactic Plane | Version matching the published article (English improved). Published
in Astron. Astrophys, 21 pages, 13 figures, 4 tables Full article (with
complete tables) can be retrieved at
http://www.archeops.org/Archeops_Publication | Astron.Astrophys.481:411,2008 | 10.1051/0004-6361:20078701 | null | astro-ph | null | Archeops is a balloon-borne experiment, mainly designed to measure the Cosmic
Microwave Background (CMB) temperature anisotropies at high angular resolution
(~ 12 arcminutes). By-products of the mission are shallow sensitivity maps over
a large fraction of the sky (about 30 %) in the millimetre and submillimetre
range at 143, 217, 353 and 545 GHz. From these maps, we produce a catalog of
bright submillimetre point sources. We present in this paper the processing and
analysis of the Archeops point sources. Redundancy across detectors is the key
factor allowing to sort out glitches from genuine point sources in the 20
independent maps. We look at the properties of the most reliable point sources,
totalling 304. Fluxes range from 1 to 10,000 Jy (at the frequencies covering
143 to 545 GHz). All sources are either planets (2) or of galactic origin.
Longitude range is from 75 to 198 degrees. Some of the sources are associated
with well-known Lynds Nebulae and HII compact regions in the galactic plane. A
large fraction of the sources have an IRAS counterpart. Except for Jupiter,
Saturn, the Crab and Cas A, all sources show a dust-emission-like modified
blackbody emission spectrum. Temperatures cover a range from 7 to 27 K. For the
coldest sources (T<10 K), a steep nu^beta emissivity law is found with a
surprising beta ~ 3 to 4. An inverse relationship between T and beta is
observed. The number density of sources at 353 GHz with flux brighter than 100
Jy is of the order of 1 per degree of Galactic longitude. These sources will
provide a strong check for the calibration of the Planck HFI focal plane
geometry as a complement to planets. These very cold sources observed by
Archeops should be prime targets for mapping observations by the Akari and
Herschel space missions and ground--based observatories.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:52:24 GMT"
},
{
"version": "v2",
"created": "Fri, 9 May 2008 12:29:41 GMT"
}
] | 2009-06-23T00:00:00 | [
[
"Desert",
"F. -X.",
""
],
[
"Macias-Perez",
"J. F.",
""
],
[
"Mayet",
"F.",
""
],
[
"Giardino",
"G.",
""
],
[
"Renault",
"C.",
""
],
[
"Aumont",
"J.",
""
],
[
"Benoit",
"A.",
""
],
[
"Bernard",
"J. -Ph.",
""
],
[
"Ponthieu",
"N.",
""
],
[
"Tristram",
"M.",
""
]
] | [
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] |
801.4503 | Walter Gubler | Walter Gubler | Non-archimedean canonical measures on abelian varieties | Thorough revision according to the comments of the referee. To appear
in Compositio | Compositio Math. 146 (2010) 683-730 | 10.1112/S0010437X09004679 | null | math.NT math.AG | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | For a closed d-dimensional subvariety X of an abelian variety A and a
canonically metrized line bundle L on A, Chambert-Loir has introduced measures
$c_1(L|_X)^{\wedge d}$ on the Berkovich analytic space associated to A with
respect to the discrete valuation of the ground field. In this paper, we give
an explicit description of these canonical measures in terms of convex
geometry. We use a generalization of the tropicalization related to the Raynaud
extension of A and Mumford's construction. The results have applications to the
equidistribution of small points.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:58:58 GMT"
},
{
"version": "v2",
"created": "Wed, 25 Jun 2008 13:53:45 GMT"
},
{
"version": "v3",
"created": "Wed, 9 Dec 2009 11:20:39 GMT"
}
] | 2019-02-20T00:00:00 | [
[
"Gubler",
"Walter",
""
]
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] |
801.4504 | Volodymyr Magas | V.K. Magas, E. Oset, A. Ramos | Critical review of [K- ppn] bound states | 8 pages, 7 figures. New section "Empirical qualitative discussion of
the strength of the reaction" with one new figure is added. Published in PRC | Phys.Rev.C77:065210,2008 | 10.1103/PhysRevC.77.065210 | null | nucl-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We make a thorough study of the process of three body kaon absorption in
nuclei, in connection with a recent FINUDA experiment which claims the
existence of a deeply bound kaonic state from the observation of a peak in the
Lambda d invariant mass distribution following K- absorption on Li6. We show
that the peak is naturally explained in terms of K- absorption from three
nucleons leaving the rest as spectators. We can also reproduce all the other
observables measured in the same experiment and used to support the hypothesis
of the deeply bound kaon state. Our study also reveals interesting aspects of
kaon absorption in nuclei, a process that must be understood in order to make
progress in the search for K- deeply bound states in nuclei.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:28:57 GMT"
},
{
"version": "v2",
"created": "Tue, 1 Jul 2008 10:10:42 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Magas",
"V. K.",
""
],
[
"Oset",
"E.",
""
],
[
"Ramos",
"A.",
""
]
] | [
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] |
801.4505 | Mark J. Reid | Mark J. Reid, Avery E. Broderick, Abraham Loeb, Mareki Honma, Andreas
Brunthaler | Limits on the Position Wander of Sgr A* | 14 pages, 3 figures submitted to ApJ | null | 10.1086/588603 | null | astro-ph | null | We present measurements with the VLBA of the variability in the centroid
position of Sgr A* relative to a background quasar at 7-mm wavelength. We find
an average centroid wander of 71 +/- 45 micro-arcsec for time scales between 50
and 100 min and 113 +/- 50 micro-arcsec for timescales between 100 and 200 min,
with no secular trend. These are sufficient to begin constraining the viability
of the hot-spot model for the radio variability of Sgr A*. It is possible to
rule out hot spots with orbital radii above 15GM_SgrA*/c^2 that contribute more
than 30% of the total 7-mm flux. However, closer or less luminous hot spots
remain unconstrained. Since the fractional variability of Sgr A* during our
observations was ~20% on time scales of hours, the hot-spot model for Sgr A*'s
radio variability remains consistent with these limits. Improved monitoring of
Sgr A*'s centroid position has the potential to place significant constraints
upon the existence and morphology of inhomogeneities in a supermassive black
hole accretion flow.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:30:01 GMT"
},
{
"version": "v2",
"created": "Thu, 27 Mar 2008 11:47:22 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Reid",
"Mark J.",
""
],
[
"Broderick",
"Avery E.",
""
],
[
"Loeb",
"Abraham",
""
],
[
"Honma",
"Mareki",
""
],
[
"Brunthaler",
"Andreas",
""
]
] | [
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] |
801.4506 | Thomas Maier | T.A. Maier, D. Poilblanc, D.J. Scalapino | Pairing Glue in the Hubbard and t-J Models | 5 pages, 4 figures | Phys. Rev. Lett. 100, 237001 (2008) | null | null | cond-mat.supr-con cond-mat.str-el | null | The question of whether one should speak of a "pairing glue" in the Hubbard
and t-J models is basically a question about the dynamics of the pairing
interaction. If the dynamics of the pairing interaction arises from virtual
states, whose energies correspond to the Mott gap, and give rise to the
exchange coupling J, the interaction is instantaneous on the relative time
scales of interest. In this case, while one might speak of an "instantaneous
glue", this interaction differs from the traditional picture of a retarded
pairing interaction. However, if the energies correspond to the spectrum seen
in the dynamic spin susceptibility, then the interaction is retarded and one
speaks of a spin-fluctuation glue which mediates the d-wave pairing. Here we
present results from numerical studies which provide insight into this
question.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:34:30 GMT"
},
{
"version": "v2",
"created": "Mon, 18 Feb 2008 21:06:50 GMT"
}
] | 2008-07-07T00:00:00 | [
[
"Maier",
"T. A.",
""
],
[
"Poilblanc",
"D.",
""
],
[
"Scalapino",
"D. J.",
""
]
] | [
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] |
801.4507 | Vladimir Karmanov | V.A. Karmanov, J.-F. Mathiot, and A.V. Smirnov | Systematic renormalization scheme in light-front dynamics with Fock
space truncation | 32 pages, 14 figures, submitted in Phys. Rev. D | Phys.Rev.D77:085028,2008 | 10.1103/PhysRevD.77.085028 | null | hep-th | null | Within the framework of the covariant formulation of light-front dynamics, we
develop a general non-perturbative renormalization scheme based on the Fock
decomposition of the state vector and its truncation. The counterterms and bare
parameters needed to renormalize the theory depend on the Fock sectors. We
present a general strategy in order to calculate these quantities, as well as
state vectors of physical systems, in a truncated Fock space. The explicit
dependence of our formalism on the orientation of the light front plane is
essential in order to analyze the structure of the counterterms. We apply our
formalism to the two-body (one fermion and one boson) truncation in the Yukawa
model and in QED, and to the three-body truncation in a scalar model. In QED,
we recover analytically, without any perturbative expansion, the
renormalization of the electric charge, according to the requirements of the
Ward identity.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 14:35:17 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Karmanov",
"V. A.",
""
],
[
"Mathiot",
"J. -F.",
""
],
[
"Smirnov",
"A. V.",
""
]
] | [
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] |
801.4508 | Walter Gubler | Walter Gubler | Equidistribution over function fields | 23 pages; reference to X.W.C. Faber added who obtained some of the
results independently. Minor errors corrected. To appear in manuscripta
mathematica | null | null | null | math.NT math.AG | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We prove equidistribution of a generic net of small points in a projective
variety X over a function field K. For an algebraic dynamical system over K, we
generalize this equidistribution theorem to a small generic net of
subvarieties. For number fields, these results were proved by Yuan and we
transfer here his methods to function fields. If X is a closed subvariety of an
abelian variety, then we can describe the equidistribution measure explicitly
in terms of convex geometry.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:01:14 GMT"
},
{
"version": "v2",
"created": "Fri, 1 Feb 2008 14:18:13 GMT"
},
{
"version": "v3",
"created": "Wed, 25 Jun 2008 14:35:35 GMT"
}
] | 2008-06-25T00:00:00 | [
[
"Gubler",
"Walter",
""
]
] | [
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801.4509 | Marcel Vos | Marcel Vos | SiLC simulation status report | proceedings of LCWS07 | ECONF C0705302:TRK24,2007 | null | null | physics.ins-det | null | The SiLC - Silicon for the Linear Collider - collaboration aims to develop
silicon detector technology for tracking in the international linear collider
experiments. The R & D programme involves a substantial effort in simulation of
the response of detector designs. In this contribution, an overview of ongoing
efforts in this area is given.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:04:30 GMT"
}
] | 2009-02-16T00:00:00 | [
[
"Vos",
"Marcel",
""
]
] | [
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] |
801.451 | Elchin Jafarov | E.I. Jafarov, S. Lievens and J. Van der Jeugt | The Wigner distribution function for the one-dimensional parabose
oscillator | 20 pages, 2 EPS figures, published in Journal of Physics A | J. Phys. A: Math. Theor. 41 235301 (2008) | 10.1088/1751-8113/41/23/235301 | null | math-ph math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In the beginning of the 1950's, Wigner introduced a fundamental deformation
from the canonical quantum mechanical harmonic oscillator, which is nowadays
sometimes called a Wigner quantum oscillator or a parabose oscillator. Also, in
quantum mechanics the so-called Wigner distribution is considered to be the
closest quantum analogue of the classical probability distribution over the
phase space. In this article, we consider which definition for such
distribution function could be used in the case of non-canonical quantum
mechanics. We then explicitly compute two different expressions for this
distribution function for the case of the parabose oscillator. Both expressions
turn out to be multiple sums involving (generalized) Laguerre polynomials.
Plots then show that the Wigner distribution function for the ground state of
the parabose oscillator is similar in behaviour to the Wigner distribution
function of the first excited state of the canonical quantum oscillator.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:05:33 GMT"
},
{
"version": "v2",
"created": "Fri, 27 Jun 2008 12:07:42 GMT"
}
] | 2008-06-27T00:00:00 | [
[
"Jafarov",
"E. I.",
""
],
[
"Lievens",
"S.",
""
],
[
"Van der Jeugt",
"J.",
""
]
] | [
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] |
801.4511 | Antonio Sollima | A. Sollima, B. Lanzoni, G. Beccari, F.R. Ferraro, F. Fusi Pecci | A Correlation between Blue Straggler and Binary Fractions in the core of
Galactic Globular Clusters | 5 pages, 2 figures, accepted for publication by A&A | null | 10.1051/0004-6361:20079082 | null | astro-ph | null | Context. Blue Stragglers Stars (BSSs) are thought to form in globular
clusters by two main formation channels: i) mergers induced by stellar
collisions and ii) coalescence or mass-transfer between companions in binary
systems. The detailed study of the BSS properties is therefore crucial for
understanding the binary evolution mechanisms, and the complex interplay
between dynamics and stellar evolution in dense stellar systems. Aims. We
present the first comparison between the BSS specific frequency and the binary
fraction in the core of a sample of Galactic globular clusters, with the aim of
investigating the relative efficiency of the two proposed formation mechanisms.
Methods. We derived the frequency of BSSs in the core of thirteen low-density
Galactic globular clusters by using deep ACS@HST observations and investigated
its correlation with the binary fraction and various other cluster parameters.
Results. We observed a correlation between the BSS specific frequency and the
binary fraction. The significance of the correlation increases by including a
further dependence on the cluster central velocity dispersion. Conclusions. We
conclude that the unperturbed evolution of primordial binaries could be the
dominant BSS formation process, at least in low-density environments.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:05:40 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Sollima",
"A.",
""
],
[
"Lanzoni",
"B.",
""
],
[
"Beccari",
"G.",
""
],
[
"Ferraro",
"F. R.",
""
],
[
"Pecci",
"F. Fusi",
""
]
] | [
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] |
801.4512 | Frank Goldenbaum | A.Budzanowski, M.Fidelus, D.Filges, F.Goldenbaum, H.Hodde, L.Jarczyk,
B.Kamys, M.Kistryn, St.Kistryn, St.Kliczewski, A.Kowalczyk, E.Kozik,
P.Kulessa, H.Machner, A.Magiera, B.Piskor-Ignatowicz, K.Pysz, Z.Rudy,
R.Siudak, M.Wojciechowski | Competition of coalescence and "fireball" processes in nonequilibrium
emission of light charged particles from p+Au collisions | 14 pages, 12 figures, IV tables, \pacs{25.40.-h,25.40.Sc,25.40.Ve} | Phys.Rev.C78:024603,2008 | 10.1103/PhysRevC.78.024603 | null | nucl-ex | null | The energy and angular dependence of double differential cross sections was
measured for p,d,t,He,Li,Be, and B isotopes produced in collisions of 1.2 and
1.9 GeV protons with Au target. The shape of the spectra and angular
distributions almost does not change in the beam energy range from 1.2 to 2.5
GeV, however, the absolute value of the cross sections increases for all
ejectiles. A phenomenological model of two emitting, moving sources reproduces
very well spectra and angular distributions of intermediate mass fragments.
Double differential cross sections for light charged particles (LCP) were
analyzed in the frame of the microscopic model of intranuclear cascade (INC)
with coalescence of nucleons and statistical model for evaporation of particles
from excited residual nuclei. Energy and angular dependencies of data agree
satisfactorily neither with predictions of microscopic intranuclear cascade
calculations for protons, nor with coalescence calculations for other LCP.
Phenomenological inclusion of another reaction mechanism - emission of LCP from
a "fireball", i.e., fast and hot moving source - combined with the microscopic
model calculations of INC, coalescence and evaporation of particles leads to
very good description of the data. It was found that nonequilibrium processes
are very important for production of LCP. They exhaust 40-80% of the total
cross sections - depending on the emitted particles. Coalescence and "fireball"
emission give comparable contributions to the cross sections with exception of
3He data where coalescence clearly dominates. The ratio of sum of all
nonequilibrium processes to those proceeding through stage of statistical
equilibrium does almost not change in the beam energy range from 1.2 GeV to 2.5
GeV for all light charged particles.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:06:16 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Budzanowski",
"A.",
""
],
[
"Fidelus",
"M.",
""
],
[
"Filges",
"D.",
""
],
[
"Goldenbaum",
"F.",
""
],
[
"Hodde",
"H.",
""
],
[
"Jarczyk",
"L.",
""
],
[
"Kamys",
"B.",
""
],
[
"Kistryn",
"M.",
""
],
[
"Kistryn",
"St.",
""
],
[
"Kliczewski",
"St.",
""
],
[
"Kowalczyk",
"A.",
""
],
[
"Kozik",
"E.",
""
],
[
"Kulessa",
"P.",
""
],
[
"Machner",
"H.",
""
],
[
"Magiera",
"A.",
""
],
[
"Piskor-Ignatowicz",
"B.",
""
],
[
"Pysz",
"K.",
""
],
[
"Rudy",
"Z.",
""
],
[
"Siudak",
"R.",
""
],
[
"Wojciechowski",
"M.",
""
]
] | [
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801.4513 | Sanjeev Kumar | Sanjeev Kumar and Arno P. Kampf | Disorder-induced orbital ordering in doped manganites | 7 pages, 7 figures | Phys. Rev. B 77, 134442 (2008) | 10.1103/PhysRevB.77.134442 | null | cond-mat.str-el | null | We study the effect of quenched disorder on the ordering of orbital and
magnetic degrees of freedom in a two-dimensional, two-band double-exchange
model for $e_g$ electrons coupled to Jahn-Teller distortions. Using a
real-space Monte Carlo method, we find that disorder can induce a short-range
ordering of the orbital degrees of freedom near 30% hole doping. The most
striking consequence of this short range ordering is a strong increase in the
low temperature resistivity. The real-space approach allows to analyze the
spatial patterns of the charge, orbital, and magnetic degrees of freedom, and
the correlations among them. The magnetism is inhomogeneous on the nanoscale in
the short-range orbitally ordered state.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:11:03 GMT"
}
] | 2008-05-23T00:00:00 | [
[
"Kumar",
"Sanjeev",
""
],
[
"Kampf",
"Arno P.",
""
]
] | [
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] |
801.4514 | Valeria Kagramanova | Valeria Kagramanova, Jutta Kunz and Claus L\"ammerzahl | Charged particle interferometry in Pleba\'{n}ski--Demia\'{n}ski black
hole space--times | 17 pages, 2 figures, referees' remarks included, to appear in Class.
Quantum Grav. V. 25 | Class.Quant.Grav.25:105023,2008 | 10.1088/0264-9381/25/10/105023 | null | gr-qc | null | The Pleba\'{n}ski--Demia\'{n}ski solution is a very general axially symmetric
analytical solution of the Einstein field equations generalizing the Kerr
solution. This solution depends on seven parameters which under certain
circumstances are related to mass, rotation, cosmological constant, NUT
parameter, electric and magnetic charges, and acceleration. In this paper we
present a general description of matter wave interferometry in the general
Pleba\'{n}ski--Demia\'{n}ski black hole space--time. Particular emphasis is
placed on a gauge invariant description of the symmetries of the gauge field.
We show that it is possible to have access to all parameters separately except
the acceleration. For neutral particles there is only access to a combination
of electric and magnetic charge.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 17:56:23 GMT"
},
{
"version": "v2",
"created": "Wed, 30 Jan 2008 16:26:39 GMT"
},
{
"version": "v3",
"created": "Thu, 1 May 2008 20:32:27 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Kagramanova",
"Valeria",
""
],
[
"Kunz",
"Jutta",
""
],
[
"Lämmerzahl",
"Claus",
""
]
] | [
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] |
801.4515 | Dario Tamascelli | Diego de Falco and Dario Tamascelli | Quantum walks: a Markovian perspective | 12 pages, 3 figures | V. Geffert et al. (Eds.): SOFSEM 2008, LNCS 4910, pp. 519-530,
2008 | 10.1007/978-3-540-77566-9_45 | null | quant-ph | null | For a continuous-time quantum walk on a line the variance of the position
observable grows quadratically in time, whereas, for its classical counterpart
on the same graph, it exhibits a linear, diffusive, behaviour. A quantum walk,
thus, propagates at a rate which is linear in time, as compared to the square
root rate for a classical random walk. Indeed, it has been suggested that there
are graphs that can be traversed by a quantum walker exponentially faster than
by the classical random analogue. In this note we adopt the approach of
exploring the conditions to impose on a Markov process in order to emulate its
quantum counterpart: the central issue that emerges is the problem of taking
into account, in the numerical generation of each sample path, the causative
effect of the ensemble of trajectories to which it belongs. How to deal
numerically with this problem is shown in a paradigmatic example.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:27:09 GMT"
},
{
"version": "v2",
"created": "Wed, 30 Jan 2008 08:43:11 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"de Falco",
"Diego",
""
],
[
"Tamascelli",
"Dario",
""
]
] | [
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] |
801.4516 | Tamar Kashti | Tamar Kashti and Eli Waxman | Searching for a Correlation Between Cosmic-Ray Sources Above 10^{19} eV
and Large-Scale Structure | 17 pages, 8 figures. v2: reference added, typos corrected, accepted
to JCAP | JCAP 0805:006,2008 | 10.1088/1475-7516/2008/05/006 | null | astro-ph hep-ph | null | We study the anisotropy signature which is expected if the sources of ultra
high energy, >10^{19} eV, cosmic-rays (UHECRs) are extragalactic and trace the
large scale distribution of luminous matter. Using the PSCz galaxy catalog as a
tracer of the large scale structure (LSS), we derive the expected all sky
angular distribution of the UHECR intensity. We define a statistic, that
measures the correlation between the predicted and observed UHECR arrival
direction distributions, and show that it is more sensitive to the expected
anisotropy signature than the power spectrum and the two point correlation
function. The distribution of the correlation statistic is not sensitive to the
unknown redshift evolution of UHECR source density and to the unknown strength
and structure of inter-galactic magnetic fields. We show, using this statistic,
that recently published >5.7x10^{19} eV Auger data are inconsistent with
isotropy at ~98% CL, and consistent with a source distribution that traces LSS,
with some preference to a source distribution that is biased with respect to
the galaxy distribution. The anisotropy signature should be detectable also at
lower energy, >4x10^{19} eV. A few fold increase of the Auger exposure is
likely to increase the significance to >99% CL, but not to >99.9% CL (unless
the UHECR source density is comparable or larger than that of galaxies). In
order to distinguish between different bias models, the systematic uncertainty
in the absolute energy calibration of the experiments should be reduced to well
below the current ~25%.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 16:00:44 GMT"
},
{
"version": "v2",
"created": "Mon, 12 May 2008 20:27:21 GMT"
}
] | 2009-02-06T00:00:00 | [
[
"Kashti",
"Tamar",
""
],
[
"Waxman",
"Eli",
""
]
] | [
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] |
801.4517 | Diego Pavon | German Olivares, Fernando Atrio-Brandela, and Diego Pavon | The Integrated Sachs-Wolfe Effect in Interacting Dark Energy Models | 9 pages, 4 figures, PACS: 98.80.Es; 98.80Bp; 98.80.Jk. Version
accepted for publication in the Physical Review | Phys.Rev.D77:103520,2008 | 10.1103/PhysRevD.77.103520 | null | astro-ph gr-qc hep-ph | null | Models with dark energy decaying into dark matter have been proposed in
Cosmology to solve the coincidence problem. We study the effect of such
coupling on the cosmic microwave background temperature anisotropies. The
interaction changes the rate of evolution of the metric potentials, the growth
rate of matter density perturbations and modifies the Integrated Sachs-Wolfe
component of cosmic microwave background temperature anisotropies, enhancing
the effect. Cross-correlation of galaxy catalogs with CMB maps provides a model
independent test to constrain the interaction. We particularize our analysis
for a specific interacting model and show that galaxy catalogs with median
redshifts $z_m=0.1-0.9$ can rule out models with an interaction parameter
strength of $c^2\simeq 0.1$ better than 99.95% confidence level. Values of
$c^2\le 0.01$ are compatible with the data and may account for the possible
discrepancy between the fraction of dark energy derived from WMAP 3yr data and
the fraction obtained from the ISW effect. Measuring the fraction of dark
energy by these two methods could provide evidence of an interaction.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:29:55 GMT"
},
{
"version": "v2",
"created": "Thu, 17 Apr 2008 07:55:13 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Olivares",
"German",
""
],
[
"Atrio-Brandela",
"Fernando",
""
],
[
"Pavon",
"Diego",
""
]
] | [
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] |
801.4518 | Devang Joshi | Devang A. Joshi, R. Nagalakshmi, S. K. Dhar and A. Thamizhavel | Anisotropic magnetization studies of $R_2 Co Ga_8$ (R = Gd, Tb, Dy, Ho,
Er, Tm, Y and Lu) single crystals | In communication with prb | null | null | null | cond-mat.str-el | null | Single crystals of R$_2$CoGa$_8$ series of compounds were grown, for the
first time, by high temperature solution growth (flux) method. These compounds
crystallize in a tetragonal crystal structure with the space group $P4/mmm$. It
has been found that R$_2$CoGa$_8$ phase forms only with the heavier rare
earths, starting from Gd with a relatively large $c/a$ ratio of $\approx$ 2.6.
The resultant anisotropic magnetic properties of the compounds were
investigated along the two principal crystallographic directions of the crystal
viz., along [100] and [001]. The nonmagnetic compounds Y$_2$CoGa$_8$ and
Lu$_2$CoGa$_8$ show diamagnetic behavior down to the lowest temperature (1.8 K)
pointing out the non-magnetic nature of Co in these compounds and a relatively
low density of electronic states at the Fermi level. Compounds with the
magnetic rare earths order antiferromagnetically at temperatures lower than 30
K. The easy axis of magnetization for R$_2$CoGa$_8$ (R = Tb, Dy and Ho) is
found to be along the [001] direction and it changes to [100] direction for
Er$_2$CoGa$_8$ and Tm$_2$CoGa$_8$. The magnetization behavior is analyzed on
the basis of crystalline electric field (CEF) model. The estimated crystal
field parameters explains the magnetocrystalline anisotropy in this series of
compounds.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 06:19:08 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Joshi",
"Devang A.",
""
],
[
"Nagalakshmi",
"R.",
""
],
[
"Dhar",
"S. K.",
""
],
[
"Thamizhavel",
"A.",
""
]
] | [
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] |
801.4519 | Thomas Wiegelmann | T. Wiegelmann, A. Lagg, S.K. Solanki, B. Inhester, J. Woch | Comparing magnetic field extrapolations with measurements of magnetic
loops | 5 pages, 3 figures | Astron.Astrophys.433:701-705,2005 | 10.1051/0004-6361:20042421 | null | astro-ph | null | We compare magnetic field extrapolations from a photospheric magnetogram with
the observationally inferred structure of magnetic loops in a newly developed
active region. This is the first time that the reconstructed 3D-topology of the
magnetic field is available to test the extrapolations. We compare the
observations with potential fields, linear force-free fields and non-linear
force-free fields. This comparison reveals that a potential field extrapolation
is not suitable for a reconstruction of the magnetic field in this young,
developing active region. The inclusion of field-line-parallel electric
currents, the so called force-free approach, gives much better results.
Furthermore, a non-linear force-free computation reproduces the observations
better than the linear force-free approximation, although no free parameters
are available in the former case.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:43:32 GMT"
}
] | 2009-06-25T00:00:00 | [
[
"Wiegelmann",
"T.",
""
],
[
"Lagg",
"A.",
""
],
[
"Solanki",
"S. K.",
""
],
[
"Inhester",
"B.",
""
],
[
"Woch",
"J.",
""
]
] | [
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] |
801.452 | Kees de Jager | Kees de Jager | Recent Experimental Results from JLab | 17 pages, 12 figures, to be published in Progress in Particle and
Nuclear Physics | Prog.Part.Nucl.Phys.61:311-324,2008 | 10.1016/j.ppnp.2007.12.017 | null | nucl-ex | null | Preliminary results of a selected few recent experiments at JLab are
presented.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:43:48 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"de Jager",
"Kees",
""
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] |
801.4521 | Francois Delduc | F. Delduc, E. Ivanov | Gauging isometries in N=4 supersymmetric mechanics | 10 pages, Talk at the International Workshop SQS'07, July 30 - August
4, 2007, Dubna, Russia | null | null | null | hep-th | null | This talk summarizes the study of superfield gaugings of isometries of
extended supersymmetric mechanics in hep-th/0605211, hep-th/0611247 and
arXiv:0706.0706. The gauging procedure provides a manifestly supersymmetric
realization of d=1 automorphic dualities which interrelate various irreducible
off-shell multiplets of d=1 extended supersymmetry featuring the same number of
physical fermions but different divisions of bosonic fields into the physical
and auxiliary subsets. We concentrate on the most interesting N=4 case and
demonstrate that, with a suitable choice of the symmetry to be gauged, all such
multiplets of N=4 supersymmetric mechanics and their generic superfield actions
can be obtained from the "root" multiplet (4,4,0) and the appropriate gauged
subclasses of the generic superfield action of the latter by a simple universal
recipe.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:44:14 GMT"
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] | 2008-01-30T00:00:00 | [
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"F.",
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801.4522 | Jerome Percus | Ora E. Percus and Jerome K. Percus | The Inverse Simpson Paradox (How To Win Without Overtly Cheating) | null | null | null | null | stat.AP | null | Given two sets of data which lead to a similar statistical conclusion, the
Simpson Paradox describes the tactic of combining these two sets and achieving
the opposite conclusion. Depending upon the given data, this may or may not
succeed. Inverse Simpson is a method of decomposing a given set of comparison
data into two disjoint sets and achieving the opposite conclusion for each one.
This is always possible; however, the statistical significance of the
conclusions does depend upon the details of the given data.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:45:22 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Percus",
"Ora E.",
""
],
[
"Percus",
"Jerome K.",
""
]
] | [
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801.4523 | Gianluca Geloni | Gianluca Geloni, Evgeni Saldin, Evgeni Schneidmiller and Mikhail
Yurkov | Transverse coherence properties of X-ray beams in third-generation
synchrotron radiation sources | 71 pages, 20 figures - Version accepted for publication in Nuclear
Inst. and Methods in Physics Research, A | Nucl.Instrum.Meth.A588:463-493,2008 | 10.1016/j.nima.2008.01.089 | null | physics.optics physics.acc-ph | null | This article describes a complete theory of spatial coherence for undulator
radiation sources. Current estimations of coherence properties often assume
that undulator sources are quasi-homogeneous, like thermal sources, and rely on
the application of the van Cittert-Zernike theorem for calculating the degree
of transverse coherence. Such assumption is not adequate when treating third
generation light sources, because the vertical(geometrical) emittance of the
electron beam is comparable or even much smaller than the radiation wavelength
in a very wide spectral interval that spans over four orders of magnitude (from
0.1 Angstrom up to 10^3 Angstrom). Sometimes, the so-called Gaussian-Schell
model, that is widely used in statistical optics in the description of
partially-coherent sources, is applied as an alternative to the
quasi-homogeneous model. However, as we will demonstrate, this model fails to
properly describe coherent properties of X-ray beams from non-homogeneous
undulator sources. As a result, a more rigorous analysis is required. We
propose a technique, based on statistical optics and Fourier optics, to
explicitly calculate the cross-spectral density of an undulator source in the
most general case, at any position after the undulator. Our theory, that makes
consistent use of dimensionless analysis, allows relatively easy treatment and
physical understanding of many asymptotes of the parameter space, together with
their region of applicability. Particular emphasis is given to the asymptotic
situation when the horizontal emittance is much larger than the radiation
wavelength, and the vertical emittance is arbitrary. This case is practically
relevant for third generation synchrotron radiation sources.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 08:37:20 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Geloni",
"Gianluca",
""
],
[
"Saldin",
"Evgeni",
""
],
[
"Schneidmiller",
"Evgeni",
""
],
[
"Yurkov",
"Mikhail",
""
]
] | [
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] |
801.4524 | Goncalo Tabuada | Goncalo Tabuada | Homotopy theory of Spectral categories | 19 pages | null | null | null | math.KT math.AT | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We construct a Quillen model structure on the category of spectral
categories, where the weak equivalences are the symmetric spectra analogue of
the notion of equivalence of categories.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:50:08 GMT"
},
{
"version": "v2",
"created": "Fri, 5 Sep 2008 09:35:26 GMT"
},
{
"version": "v3",
"created": "Mon, 23 Feb 2009 10:52:49 GMT"
}
] | 2009-02-23T00:00:00 | [
[
"Tabuada",
"Goncalo",
""
]
] | [
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] |
801.4525 | Sarah Hallerberg | S. Hallerberg and H. Kantz | When are Extreme Events the better predictable, the larger they are? | null | Phys. Rev. E 77, 011108 (2008) | null | null | physics.data-an | null | We investigate the predictability of extreme events in time series. The focus
of this work is to understand under which circumstances large events are better
predictable than smaller events. Therefore we use a simple prediction algorithm
based on precursory structures which are identified using the maximum
likelihood principle. Using the receiver operator characteristic curve as a
measure for the quality of predictions we find that the dependence on the event
magnitude is closely linked to the probability distribution function of the
underlying stochastic process. We evaluate this dependence on the probability
distribution function analytically and numerically. If we assume that the
optimal precursory structures are used to make the predictions, we find that
large increments are better predictable if the underlying stochastic process
has a Gaussian probability distribution function, whereas larger increments are
harder to predict if the underlying probability distribution function has a
power law tail. In the case of an exponential distribution function we find no
significant dependence on the event magnitude. Furthermore we compare these
results with predictions of increments in correlated data, namely, velocity
increments of a free jet flow. The velocity increments in the free jet flow are
in dependence on the time scale either asymptotically Gaussian or
asymptotically exponential distributed. The numerical results for predictions
within free jet data are in good agreement with the previous analytical
considerations for random numbers.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 15:50:16 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Hallerberg",
"S.",
""
],
[
"Kantz",
"H.",
""
]
] | [
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801.4526 | Kurt Hinterbichler | Puneet Batra, Kurt Hinterbichler, Lam Hui, Daniel Kabat | Pseudo-redundant vacuum energy | 39 pages. Appendix added. Version to appear in Phys. Rev. D | Phys.Rev.D78:043507,2008 | 10.1103/PhysRevD.78.043507 | null | hep-th astro-ph gr-qc | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We discuss models that can account for today's dark energy. The underlying
cosmological constant may be Planck scale but starts as a redundant coupling
which can be eliminated by a field redefinition. The observed vacuum energy
arises when the redundancy is explicitly broken, say by a non-minimal coupling
to curvature. We give a recipe for constructing models, including R + 1/R type
models, that realize this mechanism and satisfy all solar system constraints on
gravity. A similar model, based on Gauss-Bonnet gravity, provides a technically
natural explanation for dark energy and exhibits an interesting see-saw
behavior: a large underlying cosmological constant gives rise to both low and
high curvature solutions. Such models could be statistically favored in the
string landscape.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 16:17:05 GMT"
},
{
"version": "v2",
"created": "Tue, 26 Aug 2008 03:26:20 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Batra",
"Puneet",
""
],
[
"Hinterbichler",
"Kurt",
""
],
[
"Hui",
"Lam",
""
],
[
"Kabat",
"Daniel",
""
]
] | [
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801.4527 | Kees de Jager | Kees de Jager | Elastic Form Factors of $^{3,4}$He up to Large $Q^2$ | 3 pages, Proceedings of EFB20 | Few Body Syst.44:199-202,2008 | 10.1007/s00601-008-0290-y | null | nucl-ex | null | Elastic electron scattering off $^3$He and $^4$He has recently been studied
at forward and backward scattering angles in Hall A at JLab. The results will
provide accurate data on the elastic form factors, charge and magnetic for
$^3$He and charge only for $^4$He, up to squared momentum transfer $Q^2$-values
of 3.2 GeV$^2$.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 16:17:36 GMT"
}
] | 2009-01-16T00:00:00 | [
[
"de Jager",
"Kees",
""
]
] | [
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801.4528 | Goetz Seibold | G. Seibold | Slave-boson based configuration-interaction approach for the Hubbard
model | 8 pages, 2 figures | null | 10.1103/PhysRevB.77.235109 | null | cond-mat.str-el | null | Based on the Kotliar-Ruckenstein slave-boson scheme we develop a
configuration-interaction (CI) approach which is suitable to improve the energy
of symmetry-broken saddle-point solutions. The theory is applied to
spin-polaron states in the Hubbard model and compared with analogous results
obtained within the Hartree-Fock approximation. In addition we show that within
the infinite ${\cal D}$ prescription of the Gutzwiller method a CI approach
does not improve the variational result since in the thermodynamic limit matrix
elements between different inhomogeneous states vanish due to an 'orthogonality
catastrophe'.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 16:18:17 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Seibold",
"G.",
""
]
] | [
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] |
801.4529 | Saibal Ray | A. A. Usmani, P. P.Ghosh, Utpal Mukhopadhyay, P. C. Ray and Saibal Ray | The dark energy equation of state | 4 Latex pages, 3 figures, To appear in Mon. Not. R. Astron. Soc. Lett | Mon.Not.Roy.Astron.Soc.Lett.386:L92-95,2008 | 10.1111/j.1745-3933.2008.00468.x | null | gr-qc astro-ph hep-th | null | We perform a study of cosmic evolution with an equation of state parameter
$\omega(t)=\omega_0+\omega_1(t\dot H/H)$ by selecting a phenomenological
$\Lambda$ model of the form, $\dot\Lambda\sim H^3$. This simple proposition
explains both linearly expanding and inflationary Universes with a single set
of equations. We notice that the inflation leads to a scaling in the equation
of state parameter, $\omega(t)$, and hence in equation of state. In this
approach, one of its two parameters have been pin pointed and the other have
been delineated. It has been possible to show a connection between dark energy
and Higgs-Boson.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 16:32:58 GMT"
},
{
"version": "v2",
"created": "Tue, 11 Mar 2008 13:16:32 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Usmani",
"A. A.",
""
],
[
"Ghosh",
"P. P.",
""
],
[
"Mukhopadhyay",
"Utpal",
""
],
[
"Ray",
"P. C.",
""
],
[
"Ray",
"Saibal",
""
]
] | [
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801.453 | Thomas Rivinius | E. Pollmann, Th. Rivinius | H-alpha observations of zeta Tauri | 7 pages, 5 figures, accepted by the IBVS as No. 5813 | null | null | null | astro-ph | null | We report H-alpha observations of zeta Tauri, taken between late 2000 and
early 2006. Next to extending existing long-term montioring of the disk state
of this star we report an intermediate timescale of about 69 days to be present
in the V/R variations of the Halpha line. The observational data will be
published together with this manuscript.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 16:33:00 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Pollmann",
"E.",
""
],
[
"Rivinius",
"Th.",
""
]
] | [
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801.4531 | Gil de Oliveira-Neto | G. Oliveira-Neto and G. F. Sousa | Qualitative and quantitative features of orbits of massive particles and
photons moving in Wyman geometry | 20 pages, 8 ps figures, IOPLaTeX | Braz.J.Phys.38:573-580,2008 | 10.1590/S0103-97332008000500008 | null | gr-qc | null | The Wyman's solution depends on two parameters, the mass $M$ and the scalar
charge $\sigma$. If one fixes $M$ to a positive value, say $M_0$, and let
$\sigma^2$ take values along the real line it describes three different types
of spacetimes. For $\sigma^2 >0$ the spacetimes are naked singularities, for
$\sigma^2 = 0$ one has the Schwarzschild black hole of mass $M_0$ and finally
for $-M_0^2 \leq \sigma^2 < 0$ one has wormhole spacetimes. In the present
work, we shall study qualitative and quantitative features of orbits of massive
particles and photons moving in the naked singularity and wormhole spacetimes
of the Wyman solution. These orbits are the timelike geodesics for massive
particles and null geodesics for photons. Combining the four geodesic equations
with an additional equation derived from the line element, we obtain an
effective potential for the massive particles and a different effective
potential for the photons. We investigate all possible types of orbits, for
massive particles and photons, by studying the appropriate effective potential.
We notice that for certain values of $\sigma^2 >0$, there is an infinity
potential wall that prevents both massive particles and photons ever to reach
the naked singularity. We notice, also, that for certain values of $-M_0^2 \leq
\sigma^2 < 0$, the potential is finite everywhere, which allows massive
particles and photons moving from one wormhole asymptotically flat region to
the other. We also compute the radial timelike and null geodesics for massive
particles and photons, respectively, moving in the naked singularities and
wormholes spacetimes.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 16:36:11 GMT"
}
] | 2011-08-31T00:00:00 | [
[
"Oliveira-Neto",
"G.",
""
],
[
"Sousa",
"G. F.",
""
]
] | [
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] |
801.4532 | Laura Valentina Spinolo | Stefano Bianchini and Laura V. Spinolo | A connection between viscous profiles and singular ODEs | 6 pages, minor changes | null | null | null | math.AP math.CA | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We deal with the viscous profiles for a class of mixed hyperbolic-parabolic
systems. We focus, in particular, on the case of the compressible Navier Stokes
equation in one space variable written in Eulerian coordinates. We describe the
link between these profiles and a singular ordinary differential equation in
the form $$ dV / dt = F(V) / z (V) . $$ Here $V \in R^d$ and the function F
takes values into $R^d$ and is smooth. The real valued function z is as well
regular: the equation is singular in the sense that z (V) can attain the value
0.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 17:23:47 GMT"
},
{
"version": "v2",
"created": "Thu, 2 Apr 2009 13:04:38 GMT"
}
] | 2009-04-02T00:00:00 | [
[
"Bianchini",
"Stefano",
""
],
[
"Spinolo",
"Laura V.",
""
]
] | [
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801.4533 | Michael Shapiro | Derek F. Holt, Sarah Rees and Michael Shapiro | Groups that do and do not have context-sensitive word problem | null | null | null | null | math.GR | null | We prove that a group has word problem that is a growing context-sensitive
language precisely if its word problem can be solved using a non-deterministic
Cannon's algorithm (the deterministic algorithms being defined by Goodman and
Shapiro). We generalise their results to find many examples of groups not
admitting non-deterministic Cannon's algorithms. This adds to the examples of
Kambites and Otto of groups separating context-sensitive and growing
context-sensitive word problems, and provides a new language-theoretic
separation result.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 17:25:23 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Holt",
"Derek F.",
""
],
[
"Rees",
"Sarah",
""
],
[
"Shapiro",
"Michael",
""
]
] | [
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] |
801.4534 | Pasquale Blasi | Pasquale Blasi | Direct Measurements, Acceleration and Propagation of Cosmic Rays | 22 pages, Rapporteur Paper for the OG1 session of the 30th
International Cosmic Ray Conference, Merida, Yucatan, Mexico, July 2007 | null | null | null | astro-ph | null | This paper summarizes highlights of the OG1 session of the 30th International
Cosmic Ray Conference, held in Merida (Yucatan, Mexico). The subsessions
(OG1.1, OG1.2, OG1.3, OG1.4 and OG1.5) summarized here were mainly devoted to
direct measurements, acceleration and propagation of cosmic rays.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 17:34:51 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Blasi",
"Pasquale",
""
]
] | [
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] |
801.4535 | Sergio Colafrancesco | S. Colafrancesco | SZ effect from radio-galaxy lobes: astrophysical and cosmological
relevance | 8 pages, 5 figures, MNRAS in press | null | 10.1111/j.1365-2966.2008.12961.x | null | astro-ph | null | We derive the SZ effect arising in radio-galaxy lobes that are filled with
high-energy, non-thermal electrons. We provide here quantitative estimates for
SZ effect expected from the radio galaxy lobes by normalizing it to the
Inverse-Compton light, observed in the X-ray band, as produced by the
extrapolation to low energies of the radio emitting electron spectrum in these
radio lobes. We compute the spectral and spatial characteristics of the SZ
effect associated to the radio lobes of two distant radio galaxies (3C294 and
3C432) recently observed by Chandra, and we further discuss its detectability
with the next generation microwave and sub-mm experiments with arcsec and $\sim
\mu$K sensitivity. We finally highlight the potential use of the SZE from
radio-galaxy lobes in the astrophysical and cosmological context.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 17:46:40 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Colafrancesco",
"S.",
""
]
] | [
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] |
801.4536 | Oleg Evnin | Ben Craps, Frederik De Roo and Oleg Evnin | Quantum evolution across singularities: the case of geometrical
resolutions | 25 pages, 1 figure | JHEP 0804:036,2008 | 10.1088/1126-6708/2008/04/036 | null | hep-th | null | We continue the study of time-dependent Hamiltonians with an isolated
singularity in their time dependence, describing propagation on singular
space-times. In previous work, two of us have proposed a "minimal subtraction"
prescription for the simplest class of such systems, involving Hamiltonians
with only one singular term. On the other hand, Hamiltonians corresponding to
geometrical resolutions of space-time tend to involve multiple operator
structures (multiple types of dependence on the canonical variables) in an
essential way.
We consider some of the general properties of such (near-)singular
Hamiltonian systems, and further specialize to the case of a free scalar field
on a two-parameter generalization of the null-brane space-time. We find that
the singular limit of free scalar field evolution exists for a discrete subset
of the possible values of the two parameters. The coordinates we introduce
reveal a peculiar reflection property of scalar field propagation on the
generalized (as well as the original) null-brane. We further present a simple
family of pp-wave geometries whose singular limit is a light-like hyperplane
(discontinuously) reflecting the positions of particles as they pass through
it.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 17:48:03 GMT"
}
] | 2014-11-18T00:00:00 | [
[
"Craps",
"Ben",
""
],
[
"De Roo",
"Frederik",
""
],
[
"Evnin",
"Oleg",
""
]
] | [
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] |
801.4537 | Theodor Pribulla | Theodor Pribulla, Slavek M. Rucinski | Radial velocity mapping of Paczy\'nski's star AW UMa: Not a contact
binary | 11 figures, accepted for publication in MNRAS, January 28, 2008 | null | 10.1111/j.1365-2966.2008.13033.x | null | astro-ph | null | We present two-dimensional (radial velocity, orbital phase) spectroscopic
results for the very low mass-ratio close binary AW UMa which strongly indicate
that the spectroscopic mass ratio (q_sp = 0.10) does not agree with the
photometrically derived one and that the widely adopted contact binary model
appears to experience serious inconsistencies and limitations for this object.
AW UMa is compared with V566 Oph (q_sp = 0.26) which we found to behave
according to the contact model. Observed broadening functions of AW UMa can be
interpreted by a very strong limb darkening and/or non-solid body rotation of
the dominant primary component; the former assumption is unphysical while the
differential rotation is not supported by an apparent stability of localized,
dark features on the outer side of the primary. There are indications of the
existence of an equatorial belt encompassing the whole system. All deficiencies
in the interpretation and the discrepancy between the photometric and
spectroscopic mass ratio of AW UMa can be solved within a new model of AW UMa
where both components are detached and the system is submerged in a stream of
hot, optically thick matter which mimics the stellar contact. While the masses
and their ratio are correctly given by spectroscopy, the photometric picture is
heavily modified by the matter engulfing both stars in the equatorial plane.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:34:41 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Pribulla",
"Theodor",
""
],
[
"Rucinski",
"Slavek M.",
""
]
] | [
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] |
801.4538 | S. G. Rajeev | S. G. Rajeev | A Relativistic Wave Equation for the Skyrmion | null | AnnalsPhys.323:2873-2880,2008 | 10.1016/j.aop.2008.02.005 | null | hep-th math-ph math.AP math.MP nucl-th | null | We propose a relativistically invariant wave equation for the Skyrme soliton.
It is a differential equation on the space $R^{1,3}\times S^3$ which is
invariant under the Lorentz group and isospin. The internal variable valued in
$SU(2)\approx S^3$ describes the orientation of the soliton. The mass of a
particle of spin and isospin both equal to $j={1\over 2},{3\over 2}...$ is
predicted to be $M=m\sqrt{1+K_2j(j+1)\over 1+K_1j(j+1)}$ which agrees with the
known spectrum for low angular momentum. The iso-scalar magnetic moment is
predicted to be $-{K_1\over 4m}{\mathbf \Sigma}$, where ${\mathbf \Sigma}$ is
the spin.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 17:54:56 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Rajeev",
"S. G.",
""
]
] | [
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] |
801.4539 | Charles Bonatto | Charles Bonatto, Eduardo Bica and Joao F.C. Santos Jr | Discovery of an open cluster with a possible physical association with a
planetary nebula | The paper contains 9 figures and 5 tables. Accepted by MNRAS | null | 10.1111/j.1365-2966.2008.13042.x | null | astro-ph | null | We report the discovery of a new open cluster (OC) in the Galaxy at
$\ell=167.0^\circ$ and $b=-1.0^\circ$. Its field includes the planetary nebula
(PN) PK 167-0.1. We study the possible associations of the PN/OC pairs NGC
2818/NGC 2818A, NGC 2438/M 46 (NGC 2437), PK 6+2.5/NGC 6469, as well as of the
PN PK 167-0.1 with New Cluster 1. The analyses are based on near-infrared
colour-magnitude diagrams (CMDs) and stellar radial density profiles (RDPs).
NGC 6469 is located in a heavily contaminated bulge field. The CMD morphology,
especially for the latter two cases, is defined with a field star
decontamination algorithm applied to the 2MASS \jj, \hh, and \ks photometry.
Field decontamination for the OCs NGC 2818A and M 46 produced better defined
CMDs and more accurate cluster parameters than in the literature. Those pieces
of evidence point to M 46 as physically associated with the PN NGC 2438. The
same occurs for the OC NGC 2818A and the PN NGC 2818, however previous radial
velocity arguments indicate that they are not associated. The OC NGC 6469 does
not appear to be associated with the PN PK 6+2.5, which probably belongs to the
bulge. Finally, the distance of the OC New Cluster 1 is consistent with a
physical association with the PN PK 167-0.1.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 18:14:35 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Bonatto",
"Charles",
""
],
[
"Bica",
"Eduardo",
""
],
[
"Santos",
"Joao F. C.",
"Jr"
]
] | [
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] |
801.454 | Dirk Kussin | Michael Barot, Dirk Kussin, Helmut Lenzing | The cluster category of a canonical algebra | 16 pages. A few minor changes, one reference added. To appear in
Trans. Amer. Math. Soc | Trans. Amer. Math. Soc. 362 (2010), 4313-4330 | null | null | math.RT | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the cluster category of a canonical algebra A in terms of the
hereditary category of coherent sheaves over the corresponding weighted
projective line X. As an application we determine the automorphism group of the
cluster category and show that the cluster-tilting objects form a cluster
structure in the sense of Buan-Iyama-Reiten-Scott. The tilting graph of the
sheaf category always coincides with the tilting or exchange graph of the
cluster category. We show that this graph is connected if the Euler
characteristic of X is non-negative, or equivalently, if A is of tame (domestic
or tubular) representation type.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 19:02:56 GMT"
},
{
"version": "v2",
"created": "Mon, 4 Aug 2008 19:02:39 GMT"
},
{
"version": "v3",
"created": "Thu, 29 Jan 2009 18:54:58 GMT"
}
] | 2020-09-28T00:00:00 | [
[
"Barot",
"Michael",
""
],
[
"Kussin",
"Dirk",
""
],
[
"Lenzing",
"Helmut",
""
]
] | [
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801.4541 | G. S. Paraoanu | G. S. Paraoanu | Microwave-induced coupling of superconducting qubits | 6 pages, 3 figures | Phys. Rev. B 74, 140504(R) (2006) | 10.1103/PhysRevB.74.140504 | null | cond-mat.mes-hall cond-mat.supr-con quant-ph | null | We investigate the quantum dynamics of a system of two coupled
superconducting qubits under microwave irradiation. We find that, with the
qubits operated at the charge co-degeneracy point, the quantum evolution of the
system can be described by a new effective Hamiltonian which has the form of
two coupled qubits with tunable coupling between them. This Hamiltonian can be
used for experimental tests on macroscopic entanglement and for implementing
quantum gates.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 18:38:57 GMT"
},
{
"version": "v2",
"created": "Wed, 30 Jan 2008 06:58:51 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Paraoanu",
"G. S.",
""
]
] | [
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] |
801.4542 | Thomas K. Gaisser | Thomas K. Gaisser | Muons and Neutrinos 2007 | 16 pages, 10 figures. Rapporteur report on sessions HE2, Muons and
Neutrinos, at the 30th International Cosmic Ray Conference, Merida, Yucatan,
July, 2007 | null | null | null | astro-ph | null | This paper is the written version of the rapporteur talk on Section HE-2,
muons and neutrinos, presented at the 30th International Cosmic Ray Conference,
Merida, Yucatan, July 11, 2007. Topics include atmospheric muons and neutrinos,
solar neutrinos and astrophysical neutrinos as well as calculations and
instrumentation related to these topics.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 18:52:50 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Gaisser",
"Thomas K.",
""
]
] | [
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] |
801.4543 | Attila Szolnoki | G. Szabo, A. Szolnoki, and I. Borsos | Self-organizing patterns maintained by competing associations in a
six-species predator-prey model | 6 pages, 8 figures | Phys. Rev. E 77 (2008) 041919 | 10.1103/PhysRevE.77.041919 | null | q-bio.PE cond-mat.stat-mech physics.bio-ph | null | Formation and competition of associations are studied in a six-species
ecological model where each species has two predators and two prey. Each site
of a square lattice is occupied by an individual belonging to one of the six
species. The evolution of the spatial distribution of species is governed by
iterated invasions between the neighboring predator-prey pairs with species
specific rates and by site exchange between the neutral pairs with a
probability $X$. This dynamical rule yields the formation of five associations
composed of two or three species with proper spatiotemporal patterns. For large
$X$ a cyclic dominance can occur between the three two-species associations
whereas one of the two three-species associations prevails in the whole system
for low values of $X$ in the final state. Within an intermediate range of $X$
all the five associations coexist due to the fact that cyclic invasions between
the two-species associations reduce their resistance temporarily against the
invasion of three-species associations.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 19:01:07 GMT"
}
] | 2008-08-26T00:00:00 | [
[
"Szabo",
"G.",
""
],
[
"Szolnoki",
"A.",
""
],
[
"Borsos",
"I.",
""
]
] | [
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801.4544 | Pierre Moulin | Pierre Moulin | A Neyman-Pearson Approach to Universal Erasure and List Decoding | 31 pages, submitted to IEEE Transactions on Information Theory | null | 10.1109/ISIT.2008.4594948 | null | cs.IT math.IT | null | When information is to be transmitted over an unknown, possibly unreliable
channel, an erasure option at the decoder is desirable. Using
constant-composition random codes, we propose a generalization of Csiszar and
Korner's Maximum Mutual Information decoder with erasure option for discrete
memoryless channels. The new decoder is parameterized by a weighting function
that is designed to optimize the fundamental tradeoff between undetected-error
and erasure exponents for a compound class of channels. The class of weighting
functions may be further enlarged to optimize a similar tradeoff for list
decoders -- in that case, undetected-error probability is replaced with average
number of incorrect messages in the list. Explicit solutions are identified.
The optimal exponents admit simple expressions in terms of the sphere-packing
exponent, at all rates below capacity. For small erasure exponents, these
expressions coincide with those derived by Forney (1968) for symmetric
channels, using Maximum a Posteriori decoding. Thus for those channels at
least, ignorance of the channel law is inconsequential. Conditions for
optimality of the Csiszar-Korner rule and of the simpler
empirical-mutual-information thresholding rule are identified. The error
exponents are evaluated numerically for the binary symmetric channel.
| [
{
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"created": "Tue, 29 Jan 2008 19:17:50 GMT"
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] | 2016-11-17T00:00:00 | [
[
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801.4545 | Brant M. Johnson | PHENIX Collaboration, A. Adare, et al | Dihadron azimuthal correlations in Au+Au collisions at sqrt(s_NN)=200
GeV | 421 authors from 58 institutions, 44 pages, 38 figures, 19 tables.
Submitted to Physical Review C. Plain text data tables for the points plotted
in figures for this and previous PHENIX publications are (or will be)
publicly available at http://www.phenix.bnl.gov/papers.html | Phys.Rev.C78:014901,2008 | 10.1103/PhysRevC.78.014901 | null | nucl-ex | null | Azimuthal angle (Delta phi) correlations are presented for a broad range of
transverse momentum (0.4 < pT < 10 GeV/c) and centrality (0-92%) selections for
charged hadrons from di-jets in Au+Au collisions at sqrt(s_NN) = 200 GeV. With
increasing pT, the away-side Delta phi distribution evolves from a broad and
relatively flat shape to a concave shape, then to a convex shape. Comparisons
to p+p data suggest that the away-side distribution can be divided into a
partially suppressed head region centered at Delta phi ~ \pi, and an enhanced
shoulder region centered at Delta phi ~ \pi \pm 1:1. The pT spectrum for the
associated hadrons in the head region softens toward central collisions. The
spectral slope for the shoulder region is independent of centrality and trigger
pT . The properties of the near-side distributions are also modified relative
to those in p + p collisions, reflected by the broadening of the jet shape in
Delta phi and Delta eta, and an enhancement of the per-trigger yield. However,
these modifications seem to be limited to pT < 4 GeV/c, above which both the
dihadron pair shape and per-trigger yield become similar to p + p collisions.
These observations suggest that both the away- and near-side distributions
contain a jet fragmentation component which dominates for pT \ge 5GeV and a
medium-induced component which is important for pT \le 4 GeV/c. We also
quantify the role of jets at intermediate and low pT through the yield of
jet-induced pairs in comparison to binary scaled p + p pair yield. The yield of
jet-induced pairs is suppressed at high pair proxy energy (sum of the pT
magnitudes of the two hadrons) and is enhanced at low pair proxy energy. The
former is consistent with jet quenching; the latter is consistent with the
enhancement of soft hadron pairs due to transport of lost energy to lower pT.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:53:39 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"PHENIX Collaboration",
"",
""
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"Adare",
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801.4546 | Thomas K. Gaisser | Thomas K. Gaisser | RICAP-07: Summary comments | 5 pages, 2 figures. Summary talk at Roma International Conference on
Astroparticle Physics, June 2007 | Nucl.Instrum.Meth.A588:276-280,2008 | 10.1016/j.nima.2008.01.064 | null | astro-ph | null | The Roma International Conference on Astroparticle Physics covered gamma-ray
astronomy, air shower experiments and neutrino astronomy on three successive
days. I organize my brief summary comments into four topics that cut across
these three techniques. They are detector calibration, galactic sources,
extra-galactic sources and cosmology.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 19:27:58 GMT"
}
] | 2009-06-23T00:00:00 | [
[
"Gaisser",
"Thomas K.",
""
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801.4547 | Valenti Bosch-Ramon | V. Bosch-Ramon, D. Khangulyan, F. A. Aharonian | Non-thermal emission from secondary pairs in close TeV binary systems | accepted for publication in Astronomy & Astrophysics, 6 pages, 8
figures | null | 10.1051/0004-6361:20079252 | null | astro-ph | null | Massive hot stars produce dense ultraviolet (UV) photon fields in their
surroundings. If a very high-energy (VHE) gamma-ray emitter is located close to
the star, then gamma-rays are absorbed in the stellar photon field, creating
secondary (electron-positron) pairs. We study the broadband emission of these
secondary pairs in the stellar photon and magnetic fields. Under certain
assumptions on the stellar wind and the magnetic field in the surroundings of a
massive hot star, we calculate the steady state energy distribution of
secondary pairs created in the system and its radiation from radio to
gamma-rays. Under the ambient magnetic field, possibly high enough to suppress
electromagnetic (EM) cascading, the energy of secondary pairs is radiated via
synchrotron and single IC scattering producing radio-to-gamma-ray radiation.
The synchrotron spectral energy distribution (SED) is hard, peaks around X-ray
energies, and becomes softer. The IC SED is hard as well and peaks around 10
GeV, becoming also softer at higher energies due to synchrotron loss dominance.
The radio emission from secondary pairs is moderate and detectable as a
point-like and/or extended source. In X-rays, the secondary pair synchrotron
component may be dominant. At energies <10 GeV, the secondary pair IC radiation
may be the dominant primary gamma-ray emission and possibly detectable by the
next generation of instruments.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 19:42:28 GMT"
},
{
"version": "v2",
"created": "Sun, 3 Feb 2008 18:32:33 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Bosch-Ramon",
"V.",
""
],
[
"Khangulyan",
"D.",
""
],
[
"Aharonian",
"F. A.",
""
]
] | [
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801.4548 | Masaki Tsukamoto | Masaki Tsukamoto | Macroscopic dimension of the $\ell^p$-ball with respect to the
$\ell^q$-norm | 10 pages | Journal of Mathematics of Kyoto University, 48-2 (2008), 445-454 | null | null | math.MG | null | We show estimates of the "macroscopic dimension" of the $\ell^p$-ball with
respect to the $\ell^q$-norm.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 19:52:03 GMT"
}
] | 2009-01-26T00:00:00 | [
[
"Tsukamoto",
"Masaki",
""
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] |
801.4549 | Haruka Tanji | Haruka Tanji (1 and 2), Jonathan Simon (1 and 2), Saikat Ghosh (1) and
Vladan Vuleti\'c (1) ((1) Department of Physics, MIT-Harvard Center for
Ultracold Atoms, and Research Laboratory of Electronics, Massachusetts
Institute of Technology, Cambridge, Massachusetts, USA, (2) Department of
Physics, Harvard University, Cambridge, Massachusetts, USA) | Simplified measurement of the Bell parameter within quantum mechanics | 4 pages, 1 figure. Submitted to Physical Review A | null | null | null | quant-ph | null | We point out that, if one accepts the validity of quantum mechanics, the Bell
parameter for the polarization state of two photons can be measured in a
simpler way than by the standard procedure [Clauser, Horne, Shimony, and Holt,
Phys. Rev. Lett. 23, 880 (1969)]. The proposed method requires only two
measurements with parallel linear-polarizer settings for Alice and Bob at 0 and
45 degrees, and yields a significantly smaller statistical error for a large
Bell parameter.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:53:19 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Tanji",
"Haruka",
"",
"1 and 2"
],
[
"Simon",
"Jonathan",
"",
"1 and 2"
],
[
"Ghosh",
"Saikat",
""
],
[
"Vuletić",
"Vladan",
""
]
] | [
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] |
801.455 | A. S. Denikin | A.S. Denikin, V.I. Zagrebaev, P. Descouvemont | Generalized optical potential for weakly bound nuclei. I. Two-cluster
projectiles | 35 pages, 11 figures | Phys.Rev.C79:024605,2009 | 10.1103/PhysRevC.79.024605 | null | nucl-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A generalized optical potential for elastic scattering induced by light
nuclei is calculated within the Feshbach projection operator method. The model
explicitly takes into account the contribution of the projectile break-up
continuum treated within a microscopic few-cluster model. In this work we
formulate the model, deriving an explicit expression for the optical potential,
and show ability of the model applying it to deuteron elastic scattering.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:12:10 GMT"
},
{
"version": "v2",
"created": "Fri, 12 Dec 2008 07:51:45 GMT"
}
] | 2009-04-28T00:00:00 | [
[
"Denikin",
"A. S.",
""
],
[
"Zagrebaev",
"V. I.",
""
],
[
"Descouvemont",
"P.",
""
]
] | [
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] |
801.4551 | Fernando C. Lombardo | F.C. Lombardo, F. D. Mazzitelli, and P.I. Villar | Exploring the quantum vacuum with cylinders | 11 pages, 6 figures, Proceedings of QFEXT07. To be published in J.
Phys. A | null | 10.1088/1751-8113/41/16/164009 | null | quant-ph hep-ph hep-th | null | We review recent work on the Casimir interaction energy between cylindrical
shells. We include proposals for future experiments involving cylinders, such
us a null experiment using quasi-concentric cylinders, a cylinder in front a
conducting plate, and a cylindrical version of the rack and pinion powered by
Casimir lateral force. We also present an exact formula for the theoretical
evaluation of the vacuum interaction energy between eccentric cylindrical
shells, and describe improved analytical and numerical evaluations for the
particular case of concentric cylinders.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:13:00 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Lombardo",
"F. C.",
""
],
[
"Mazzitelli",
"F. D.",
""
],
[
"Villar",
"P. I.",
""
]
] | [
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] |
801.4552 | Randall McEntaffer | Randall L. McEntaffer and Webster Cash | Soft X-ray Spectroscopy of the Cygnus Loop Supernova Remnant | null | ApJ, 680, 328-335, 2008 | 10.1086/587936 | null | astro-ph | null | The Cygnus X-ray Emission Spectroscopic Survey (CyXESS) sounding rocket
payload was launched from White Sands Missile Range on 2006 November 20 and
obtained a high resolution spectrum of the Cygnus Loop supernova remnant in the
soft X-rays. The novel X-ray spectrograph incorporated a wire-grid collimator
feeding an array of gratings in the extreme off-plane mount which ultimately
dispersed the spectrum onto Gaseous Electron Multiplier (GEM) detectors. This
instrument recorded 65 seconds of usable data between 43-49.5 \AA in two
prominent features. The first feature near 45 \AA is dominated by the He-like
triplet of \ion{O}{7} in second order with contributions from \ion{Mg}{10} and
\ion{Si}{9}-\ion{Si}{12} in first order, while the second feature near 47.5 \AA
is first order \ion{S}{9} and \ion{S}{10}. Fits to the spectra give an
equilibrium plasma at $\log(T)=6.2$ ($kT_e=0.14$ keV) and near cosmic
abundances. This is consistent with previous observations, which demonstrated
that the soft x-ray emission from the Cygnus Loop is dominated by interactions
between the initial blast wave with the walls of a precursor formed cavity
surrounding the Cygnus Loop and that this interaction can be described using
equilibrium conditions.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:14:21 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"McEntaffer",
"Randall L.",
""
],
[
"Cash",
"Webster",
""
]
] | [
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801.4553 | Claus Lammerzahl | Ertan G\"okl\"u and Claus L\"ammerzahl | Metric fluctuations and the Weak Equivalence Principle | 10 pages, to appear in Class. Quantum Grav. (2008) | Class.Quant.Grav.25:105012,2008 | 10.1088/0264-9381/25/10/105012 | null | gr-qc quant-ph | null | We describe space--time fluctuations by means of small fluctuations of the
metric on a given background metric. From a minimally coupled Klein--Gordon
equation we obtain within a weak-field approximation up to second order and an
averaging procedure over a finite space--time scale given by the quantum
particle in the non--relativistic limit a modified Schr\"odinger equation. The
dominant modification consists in an anomalous inertial mass tensor which
depends on the type of particle and on the fluctuation scenario. The scenario
considered in this paper is a most simple picture of spacetime fluctuations and
gives an existence proof for an apparent violation of the weak equivalence
principle and, in general, for a violation of Lorentz invariance.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:26:21 GMT"
},
{
"version": "v2",
"created": "Wed, 30 Jan 2008 10:44:09 GMT"
},
{
"version": "v3",
"created": "Wed, 9 Apr 2008 07:52:03 GMT"
},
{
"version": "v4",
"created": "Thu, 24 Apr 2008 12:27:42 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Göklü",
"Ertan",
""
],
[
"Lämmerzahl",
"Claus",
""
]
] | [
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] |
801.4554 | John F. Gunion | Spencer Chang, Radovan Dermisek, John F. Gunion and Neal Weiner | Nonstandard Higgs Boson Decays | 53 pages, review intended for Annual Reviews of Nuclear Science.
Final corrections and references now included | Ann.Rev.Nucl.Part.Sci.58:75-98,2008 | 10.1146/annurev.nucl.58.110707.171200 | null | hep-ph | null | This review summarizes the motivations for and phenomenological consequences
of nonstandard Higgs boson decays, with emphasis on final states containing a
pair of non-Standard-Model particles that subsequently decay to Standard Model
particles. Typically these non-Standard-Model particles are part of a
``hidden'' sector, for example a pair of neutral Higgs bosons or a pair of
unstable neutralinos. We emphasize that such decays allow for a Higgs
substantially below the Standard Model Higgs LEP limit of 114 GeV. This in turn
means that the ``fine-tuning'' problems of many Beyond the Standard Model (BSM)
theories, in particular supersymmetric models, can be eliminated while
achieving excellent consistency with precision electroweak data which favor a
Higgs boson with mass below $100\gev$ and standard $WW$, $ZZ$, and top
couplings.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:47:14 GMT"
},
{
"version": "v2",
"created": "Thu, 7 Feb 2008 08:02:36 GMT"
}
] | 2008-11-07T00:00:00 | [
[
"Chang",
"Spencer",
""
],
[
"Dermisek",
"Radovan",
""
],
[
"Gunion",
"John F.",
""
],
[
"Weiner",
"Neal",
""
]
] | [
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] |
801.4555 | Brant M. Johnson | PHENIX Collaboration, A. Adare, et al | Energy dependence of pi-zero production in Cu+Cu collisions at
sqrt(s_NN) = 22.4, 62.4, and 200 GeV | 431 authors from 63 institutions, 7 pages, 3 figures, 2 tables.
Submitted to Physical Review Letters. Plain text data tables for the points
plotted in figures for this and previous PHENIX publications are (or will be)
publicly available at http://www.phenix.bnl.gov/papers.html | Phys.Rev.Lett.101:162301,2008 | 10.1103/PhysRevLett.101.162301 | null | nucl-ex | null | Neutral pion transverse momentum (pT) spectra at mid-rapidity (|y| < 0.35)
were measured in Cu+Cu collisions at \sqrt s_NN = 22.4, 62.4, and 200 GeV.
Relative to pi -zero yields in p+p collisions scaled by the number of inelastic
nucleon-nucleon collisions (Ncoll) at the respective energies, the pi-zero
yields for pT \ge 2 GeV/c in central Cu+Cu collisions at 62.4 and 200 GeV are
suppressed, whereas an enhancement is observed at 22.4 GeV. A comparison with a
jet quenching model suggests that final state parton energy loss dominates in
central Cu+Cu collisions at 62.4 GeV and 200 GeV, while the enhancement at 22.4
GeV is consistent with nuclear modifications in the initial state alone.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:48:28 GMT"
}
] | 2010-03-19T00:00:00 | [
[
"PHENIX Collaboration",
"",
""
],
[
"Adare",
"A.",
""
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801.4556 | German Andres Enciso | Winfried Just and German Enciso | Large attractors in cooperative bi-quadratic Boolean networks. Part II | 14 pages | null | null | null | q-bio.MN q-bio.QM | null | Boolean networks have been the object of much attention, especially since S.
Kauffman proposed them in the 1960's as models for gene regulatory networks.
These systems are characterized by being defined on a Boolean state space and
by simultaneous updating at discrete time steps. Of particular importance for
biological applications are networks in which the indegree for each variable is
bounded by a fixed constant, as was stressed by Kauffman in his original
papers.
An important question is which conditions on the network topology can rule
out exponentially long periodic orbits in the system. In this paper we consider
cooperative systems, i.e. systems with positive feedback interconnections among
all variables, which in a continuous setting guarantees a very stable dynamics.
In Part I of this paper we presented a construction that shows that for an
arbitrary constant 0<c<2 and sufficiently large n there exist n-dimensional
Boolean cooperative networks in which both the indegree and outdegree of each
for each variable is bounded by two (bi-quadratic networks) and which
nevertheless contain periodic orbits of length at least c^n.
In this part, we prove an inverse result showing that for sufficiently large
n and for 0<c<2 sufficiently close to 2, any n-dimensional cooperative,
bi-quadratic Boolean network with a cycle of length at least c^n must have a
large proportion of variables with indegree 1. Such systems therefore share a
structural similarity to the systems constructed in Part I.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:50:32 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Just",
"Winfried",
""
],
[
"Enciso",
"German",
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801.4557 | Nick Dungey | Nick Dungey | Subordinated discrete semigroups of operators | 28 pages | null | null | null | math.FA math.PR | null | Given a power-bounded linear operator T in a Banach space and a probability F
on the non-negative integers, one can form a `subordinated' operator S = \sum_k
F(k) T^k. We obtain asymptotic properties of the subordinated discrete
semigroup (S^n: n=1,2,...) under certain conditions on F. In particular, we
study probabilities F with the property that S satisfies the Ritt resolvent
condition whenever T is power-bounded. Examples and counterexamples of this
property are discussed. The hypothesis of power-boundedness of T can sometimes
be replaced by the weaker Kreiss resolvent condition.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:52:09 GMT"
}
] | 2008-01-30T00:00:00 | [
[
"Dungey",
"Nick",
""
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] |
801.4558 | Douglas Natelson | Daniel R. Ward, Naomi J. Halas, Jacob W. Ciszek, James M. Tour,
Yanpeng Wu, Peter Nordlander, Douglas Natelson | Simultaneous measurements of electronic conduction and Raman response in
molecular junctions | 16 pages, 5 figures + supporting material of 15 pages, 10 figures | Nano Lett. 8, 919-924 (2008) | 10.1021/nl073346h | null | cond-mat.mes-hall | null | Electronic conduction through single molecules is affected by the molecular
electronic structure as well as by other information that is extremely
difficult to assess, such as bonding geometry and chemical environment. The
lack of an independent diagnostic technique has long hampered single-molecule
conductance studies. We report simultaneous measurement of the conductance and
the Raman spectra of nanoscale junctions used for single-molecule electronic
experiments. Blinking and spectral diffusion in the Raman response of both
para-mercaptoaniline and a fluorinated oligophenylyne ethynylene correlate in
time with changes in the electronic conductance. Finite difference time domain
calculations confirm that these correlations do not result from the conductance
modifying the Raman enhancement. Therefore, these observations strongly imply
that multimodal sensing of individual molecules is possible in these
mass-producible nanostructures.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 20:57:37 GMT"
}
] | 2009-05-21T00:00:00 | [
[
"Ward",
"Daniel R.",
""
],
[
"Halas",
"Naomi J.",
""
],
[
"Ciszek",
"Jacob W.",
""
],
[
"Tour",
"James M.",
""
],
[
"Wu",
"Yanpeng",
""
],
[
"Nordlander",
"Peter",
""
],
[
"Natelson",
"Douglas",
""
]
] | [
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] |
801.4559 | Elizabeth R. Stanway | Elizabeth R. Stanway (Bristol), Malcolm N. Bremer (Bristol), Valentina
Squitieri (Bristol), Laura S. Douglas (Bristol, Paris), Matthew D. Lehnert
(Paris) | A Limit on the Number Density of Bright z~7 Galaxies | 8 pages, accepted for publication in MNRAS | null | 10.1111/j.1365-2966.2008.13030.x | null | astro-ph | null | We present a survey of bright optical dropout sources in two deep,
multiwavelength surveys comprising eleven widely-separated fields, aimed at
constraining the galaxy luminosity function at z~7 for sources at 5-10L*(z=6).
Our combined survey area is 225 arcmin^2 to a depth of J=24.2 (AB, 3 sigma) and
135 arcmin^2 to J=25.3 (AB, 4 sigma). We find that infrared data longwards of 2
microns is essential for classifying optical dropout sources, and in particular
for identifying cool Galactic star contaminants. Our limits on the number
density of high redshift sources are consistent with current estimates of the
Lyman break galaxy luminosity function at z=6.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:00:09 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Stanway",
"Elizabeth R.",
"",
"Bristol"
],
[
"Bremer",
"Malcolm N.",
"",
"Bristol"
],
[
"Squitieri",
"Valentina",
"",
"Bristol"
],
[
"Douglas",
"Laura S.",
"",
"Bristol, Paris"
],
[
"Lehnert",
"Matthew D.",
"",
"Paris"
]
] | [
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0.0145576578
] |
801.456 | Roberto Decarli | R. Decarli, M. Dotti, M. Fontana, F. Haardt | Are the black hole masses in Narrow Line Seyfert 1 galaxies actually
small? | 5 pages, 3 figures. Accepted for publication in MNRAS Letters. Wrong
version was uploaded! Check for the correct one in the replacement | null | 10.1111/j.1745-3933.2008.00451.x | null | astro-ph | null | Narrow Line Seyfert 1 galaxies (NLS1s) are generally considered peculiar
objects among the broad class of Type 1 active galactic nuclei, due to the
relatively small width of the broad lines, strong X-ray variability, soft X-ray
continua, weak [OIII], and strong FeII line intensities. The mass M_BH of the
central massive black hole (MBH) is claimed to be lighter than expected from
known MBH-host galaxy scaling relations, while the accretion rate onto the MBH
larger than the average value appropriate to Seyfert 1 galaxies. In this
Letter, we show that NLS1 peculiar M_BH and L/L_Edd turn out to be fairly
standard, provided that the broad line region is allowed to have a disc-like,
rather than isotropic, geometry. Assuming that NLS1s are rather ``normal''
Seyfert 1 objects seen along the disc axis, we could estimate the typical
inclination angles from the fraction of Seyfert 1 classified as NLS1s, and
compute the geometrical factor relating the observed FWHM of broad lines to the
virial mass of the MBH. We show that the geometrical factor can fully account
for the "black hole mass deficit" observed in NLS1s, and that L/L_Edd is (on
average) comparable to the value of the more common broad line Seyfert 1
galaxies.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:00:19 GMT"
},
{
"version": "v2",
"created": "Fri, 1 Feb 2008 11:26:43 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Decarli",
"R.",
""
],
[
"Dotti",
"M.",
""
],
[
"Fontana",
"M.",
""
],
[
"Haardt",
"F.",
""
]
] | [
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801.4561 | Hannah Jang-Condell | H. Jang-Condell | Planet Shadows in Protoplanetary Disks. I: Temperature Perturbations | 14 pages, 14 figures. To appear in ApJ | null | 10.1086/533583 | null | astro-ph | null | Planets embedded in optically thick passive accretion disks are expected to
produce perturbations in the density and temperature structure of the disk. We
calculate the magnitudes of these perturbations for a range of planet masses
and distances. The model predicts the formation of a shadow at the position of
the planet paired with a brightening just beyond the shadow. We improve on
previous work on the subject by self-consistently calculating the temperature
and density structures under the assumption of hydrostatic equilibrium and
taking the full three-dimensional shape of the disk into account rather than
assuming a plane-parallel disk. While the excursion in temperatures is less
than in previous models, the spatial size of the perturbation is larger. We
demonstrate that a self-consistent calculation of the density and temperature
structure of the disk has a large effect on the disk model. In addition, the
temperature structure in the disk is highly sensitive to the angle of incidence
of stellar irradition at the surface, so accurately calculating the shape of
the disk surface is crucial for modeling the thermal structure of the disk.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:09:48 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Jang-Condell",
"H.",
""
]
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801.4562 | Jonathan Braithwaite | Jonathan Braithwaite (CITA) | Non-dipolar magnetic fields in Ap stars | 6 pages, 2 figures. To appear in the proceedings of the CP/Ap-star
workshop, Vienna, September 2007 | null | null | null | astro-ph | null | An arbitrary initial magnetic field in an A star evolves into a stable
equilibrium. Simulations are presented of the formation of non-axisymmetric
equilibria consisting of twisted flux tubes meandering under the surface of the
star, and analytic arguments are given relating the stability and form of these
equilibria. These results may help to explain observations of Ap stars with
very non-dipolar fields. This work is also applicable to other essentially
non-convective stars such as white dwarfs and neutron stars.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:00:58 GMT"
}
] | 2008-01-31T00:00:00 | [
[
"Braithwaite",
"Jonathan",
"",
"CITA"
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] |
801.4563 | Ariyeh Maller | Ariyeh H. Maller, Andreas A. Berlind, Michael Blanton, David W. Hogg | Intrinsic Properties of Low-z SDSS Galaxies | 2 pages, 1 figure to appear in the proceedings of "Formation and
Evolution of Galaxy Disks", Rome, October 2007, Eds. J. Funes and E. M.
Corsini | null | null | null | astro-ph | null | Galaxies are seen from different viewing angles and their observed properties
change as a function of viewing angle. In many circumstances we would rather
know the intrinsic properties of galaxies - those properties that do not depend
on viewing angle. For a large sample of galaxies it is possible to recover the
intrinsic properties of galaxies, statistically, by looking for correlations
with galaxy inclination, and then applying a correction to remove those
dependencies. Studying the intrinsic properties of galaxies can give a
different impression of the galaxy population and help avoid the mistake of
connecting observed properties to quantities that don't depend on inclination
like halo mass.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:00:53 GMT"
}
] | 2008-01-31T00:00:00 | [
[
"Maller",
"Ariyeh H.",
""
],
[
"Berlind",
"Andreas A.",
""
],
[
"Blanton",
"Michael",
""
],
[
"Hogg",
"David W.",
""
]
] | [
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] |
801.4564 | Roman Buniy | Micheal S. Berger and Roman V. Buniy | Entanglement Entropy and Spatial Geometry | published version | JHEP0807:095,2008 | 10.1088/1126-6708/2008/07/095 | null | hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The entanglement entropy in a quantum field theory between two regions of
space has been shown in simple cases to be proportional to the volume of the
hypersurface separating the regions. We prove that this is true for a free
scalar field in an arbitrary geometry with purely spatial curvature and obtain
a complete asymptotic expansion for the entropy.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:01:26 GMT"
},
{
"version": "v2",
"created": "Mon, 28 Jul 2008 03:28:21 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Berger",
"Micheal S.",
""
],
[
"Buniy",
"Roman V.",
""
]
] | [
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] |
801.4565 | Thomas Kitching | T. D. Kitching, A. F. Heavens, L. Verde, P. Serra, A. Melchiorri | Finding Evidence for Massive Neutrinos using 3D Weak Lensing | 9 pages, 2 Figures, 2 Tables, submitted to Physical Review D | Phys.Rev.D77:103008,2008 | 10.1103/PhysRevD.77.103008 | null | astro-ph | null | In this paper we investigate the potential of 3D cosmic shear to constrain
massive neutrino parameters. We find that if the total mass is substantial
(near the upper limits from LSS, but setting aside the Ly alpha limit for now),
then 3D cosmic shear + Planck is very sensitive to neutrino mass and one may
expect that a next generation photometric redshift survey could constrain the
number of neutrinos N_nu and the sum of their masses m_nu to an accuracy of
dN_nu ~ 0.08 and dm_nu ~ 0.03 eV respectively. If in fact the masses are close
to zero, then the errors weaken to dN_nu ~ 0.10 and dm_nu~0.07 eV. In either
case there is a factor 4 improvement over Planck alone. We use a Bayesian
evidence method to predict joint expected evidence for N_nu and m_nu. We find
that 3D cosmic shear combined with a Planck prior could provide `substantial'
evidence for massive neutrinos and be able to distinguish `decisively' between
many competing massive neutrino models. This technique should `decisively'
distinguish between models in which there are no massive neutrinos and models
in which there are massive neutrinos with |N_nu-3| > 0.35 and m_nu > 0.25 eV.
We introduce the notion of marginalised and conditional evidence when
considering evidence for individual parameter values within a multi-parameter
model.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:19:58 GMT"
}
] | 2009-06-23T00:00:00 | [
[
"Kitching",
"T. D.",
""
],
[
"Heavens",
"A. F.",
""
],
[
"Verde",
"L.",
""
],
[
"Serra",
"P.",
""
],
[
"Melchiorri",
"A.",
""
]
] | [
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] |
801.4566 | Wei Song | Wei Li, Wei Song and Andrew Strominger | Chiral Gravity in Three Dimensions | 21 pages, published version, typos corrected, more reference added | JHEP 0804:082,2008 | 10.1088/1126-6708/2008/04/082 | null | hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Three dimensional Einstein gravity with negative cosmological constant
-1/\ell^2 deformed by a gravitational Chern-Simons action with coefficient
1/\mu is studied in an asymptotically AdS_3 spacetime. It is argued to violate
unitary or positivity for generic \mu due to negative-energy massive gravitons.
However at the critical value \mu\ell=1, the massive gravitons disappear and
BTZ black holes all have mass and angular momentum related by \ell M=J. The
corresponding chiral quantum theory of gravity is conjectured to exist and be
dual to a purely right-moving boundary CFT with central charges
(c_L,c_R)=(0,3\ell /G).
| [
{
"version": "v1",
"created": "Wed, 30 Jan 2008 20:53:45 GMT"
},
{
"version": "v2",
"created": "Mon, 21 Jul 2008 20:04:17 GMT"
}
] | 2010-04-06T00:00:00 | [
[
"Li",
"Wei",
""
],
[
"Song",
"Wei",
""
],
[
"Strominger",
"Andrew",
""
]
] | [
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] |
801.4567 | Bettina Posselt | B. Posselt, S.B. Popov, F. Haberl, J. Truemper, R. Turolla, R.
Neuhaeuser, P.A. Boldin | The needle in the haystack - Where to look for more isolated cooling
neutron stars | 18 pages, 14 figures; added Erratum after bug in code was discovered,
updated results in Appendix, main conclusions do not change | Astron.Astrophys.482:617,2008 | 10.1051/0004-6361:20078430 | null | astro-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Context: Isolated cooling neutron stars with thermal X-ray emission remain
rarely detected objects despite many searches investigating the ROSAT data.
Aims: We simulate the population of close-by young cooling neutron stars to
explain the current observational results. Given the inhomogeneity of the
neutron star distribution on the sky it is particularly interesting to identify
promising sky regions with respect to on-going and future searches.
Methods: Applying a population synthesis model the inhomogeneity of the
progenitor distribution and the inhomogeneity of the X-ray absorbing
interstellar medium are considered for the first time. The total number of
observable neutron stars is derived with respect to ROSAT count rates. In
addition, we present sky maps of neutron star locations and discuss age and
distance distributions of the simulated neutron stars. Implications for future
searches are discussed.
Results: With our advanced model we can successfully explain the observed
logN - logS distribution of close-by neutron stars. Cooling neutron stars will
be most abundant in the directions of rich OB associations. New candidates are
expected to be identified behind the Gould Belt, in particular in the
Cygnus-Cepheus region. They are expected to be on average younger and then
hotter than the known population of isolated cooling neutron stars. In
addition, we propose to use data on runaway stars to search for more
radio-quiet cooling neutron stars.
| [
{
"version": "v1",
"created": "Wed, 30 Jan 2008 14:57:34 GMT"
},
{
"version": "v2",
"created": "Wed, 24 Mar 2010 17:50:14 GMT"
}
] | 2014-11-18T00:00:00 | [
[
"Posselt",
"B.",
""
],
[
"Popov",
"S. B.",
""
],
[
"Haberl",
"F.",
""
],
[
"Truemper",
"J.",
""
],
[
"Turolla",
"R.",
""
],
[
"Neuhaeuser",
"R.",
""
],
[
"Boldin",
"P. A.",
""
]
] | [
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] |
801.4568 | Ariyeh Maller | Ariyeh H. Maller | Halo Mergers, Galaxy Mergers, and Why Hubble Type Depends on Mass | 4 pages, 2 figures, to appear in the proceedings of "Formation and
Evolution of Galaxy Disks", Rome, October 2007, Eds. J. Funes and E. M.
Corsini | null | null | null | astro-ph | null | In the CDM cosmological framework structures grow from merging with smaller
structures. Merging should have observable effects on galaxies including
destroying disks and creating spheroids. This proceeding aims to give a brief
overview of how mergers occur in cosmological simulations. In this regard it is
important to understand that dark matter halo mergers are not galaxy mergers; a
theory of galaxy formation is necessary to connect the two. Mergers of galaxies
in hydrodynamical simulations show a stronger dependence on mass than halo
mergers in N-body simulations. If one knows how to connect galaxies to dark
matter halos then the halo merger rate can be converted into a galaxy merger
rate. When this is done it becomes clear that major mergers are many times more
common in more massive galaxies offering a possible explanation of why Hubble
type depends on galaxy mass.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:07:47 GMT"
}
] | 2008-01-31T00:00:00 | [
[
"Maller",
"Ariyeh H.",
""
]
] | [
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] |
801.4569 | Christopher Lee | Christian W. Bauer, Sean Fleming, Christopher Lee, and George Sterman | Factorization of e+e- Event Shape Distributions with Hadronic Final
States in Soft Collinear Effective Theory | 21 pages. Journal version. Defined an explicit thrust axis operator;
clarified meaning of a delta function operator | Phys.Rev.D78:034027,2008 | 10.1103/PhysRevD.78.034027 | UCB-PTH-08/02, YITP-SB-08-02 | hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present a new analysis of two-jet event shape distributions in soft
collinear effective theory. Extending previous results, we observe that a large
class of such distributions can be expressed in terms of vacuum matrix elements
of operators in the effective theory. We match these matrix elements to the
full theory in the two-jet limit without assuming factorization of the complete
set of hadronic final states into independent sums over partonic collinear and
soft states. We also briefly discuss the relationship of this approach to
diagrammatic factorization in the full theory.
| [
{
"version": "v1",
"created": "Wed, 30 Jan 2008 20:09:50 GMT"
},
{
"version": "v2",
"created": "Wed, 24 Sep 2008 21:32:08 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Bauer",
"Christian W.",
""
],
[
"Fleming",
"Sean",
""
],
[
"Lee",
"Christopher",
""
],
[
"Sterman",
"George",
""
]
] | [
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] |
801.457 | Martin Pessah | Martin E. Pessah (Institute for Advanced Study), Chi-kwan Chan
(Harvard-Smithsonian Center for Astrophysics) | Viscous, Resistive Magnetorotational Modes | ApJ, submitted, 17 pages (emulateapj style), 12 figures. Comments
welcomed | null | 10.1086/589915 | null | astro-ph | null | We carry out a comprehensive analysis of the behavior of the
magnetorotational instability (MRI) in viscous, resistive plasmas. We find
exact, non-linear solutions of the non-ideal magnetohydrodynamic (MHD)
equations describing the local dynamics of an incompressible, differentially
rotating background threaded by a vertical magnetic field when disturbances
with wavenumbers perpendicular to the shear are considered. We provide a
geometrical description of these viscous, resistive MRI modes and show how
their physical structure is modified as a function of the Reynolds and magnetic
Reynolds numbers. We demonstrate that when finite dissipative effects are
considered, velocity and magnetic field disturbances are no longer orthogonal
(as it is the case in the ideal MHD limit) unless the magnetic Prandtl number
is unity. We generalize previous results found in the ideal limit and show that
a series of key properties of the mean Reynolds and Maxwell stresses also hold
for the viscous, resistive MRI. In particular, we show that the Reynolds stress
is always positive and the Maxwell stress is always negative. Therefore, even
in the presence of viscosity and resistivity, the total mean angular momentum
transport is always directed outwards. We also find that, for any combination
of the Reynolds and magnetic Reynolds numbers, magnetic disturbances dominate
both the energetics and the transport of angular momentum and that the total
mean energy density is an upper bound for the total mean stress responsible for
angular momentum transport. The ratios between the Maxwell and Reynolds
stresses and between magnetic and kinetic energy densities increase with
decreasing Reynolds numbers for any magnetic Reynolds number; the lowest limit
of both ratios is reached in the ideal MHD regime.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:15:06 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Pessah",
"Martin E.",
"",
"Institute for Advanced Study"
],
[
"Chan",
"Chi-kwan",
"",
"Harvard-Smithsonian Center for Astrophysics"
]
] | [
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] |
801.4571 | Yongyi Mao Dr | Ronghui Tu, Yongyi Mao and Jiying Zhao | Is SP BP? | 77 page double-spaced single-column submitted version to IEEE
Transactions on Information Theory | null | null | null | cs.IT math.IT | null | The Survey Propagation (SP) algorithm for solving $k$-SAT problems has been
shown recently as an instance of the Belief Propagation (BP) algorithm. In this
paper, we show that for general constraint-satisfaction problems, SP may not be
reducible from BP. We also establish the conditions under which such a
reduction is possible. Along our development, we present a unification of the
existing SP algorithms in terms of a probabilistically interpretable iterative
procedure -- weighted Probabilistic Token Passing.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:35:13 GMT"
}
] | 2008-01-31T00:00:00 | [
[
"Tu",
"Ronghui",
""
],
[
"Mao",
"Yongyi",
""
],
[
"Zhao",
"Jiying",
""
]
] | [
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] |
801.4572 | Lucas Cieza | Lucas A. Cieza | The Evolution of Primordial Circumstellar Disks | 15 pages and 5 figures, invited review talk, to appear in the ASP
conference proceedings of the "Frank N. Bash Symposium 2007: New Horizons in
Astronomy", editors: A. Frebel, J. Maund, J. Shen, M. Siegel | null | null | null | astro-ph | null | Circumstellar disks are an integral part of the star formation process and
the sites where planets are formed. Understanding the physical processes that
drive their evolution, as disks evolve from optically thick to optically thin,
is crucial for our understanding of planet formation. Disks evolve through
various processes including accretion onto the star, dust settling and
coagulation, dynamical interactions with forming planets, and
photo-evaporation. However, the relative importance and timescales of these
processes are still poorly understood. In this review, I summarize current
models of the different processes that control the evolution of primordial
circumstellar disks around low-mass stars. I also discuss recent observational
developments on circumstellar disk evolution with a focus on new Spitzer
results on transition objects.
| [
{
"version": "v1",
"created": "Tue, 29 Jan 2008 21:55:35 GMT"
},
{
"version": "v2",
"created": "Thu, 31 Jan 2008 20:42:57 GMT"
}
] | 2016-09-08T00:00:00 | [
[
"Cieza",
"Lucas A.",
""
]
] | [
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