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712.0779 | Yair Shokef | Guy Bunin, Yair Shokef, and Dov Levine | Frequency-dependent fluctuation-dissipation relations in granular gases | 6 pages | Phys. Rev. E 77, 051301 (2008) | 10.1103/PhysRevE.77.051301 | null | cond-mat.soft cond-mat.stat-mech | null | The Green-Kubo relation for two models of granular gases is discussed. In the
Maxwell model in any dimension, the effective temperature obtained from the
Green-Kubo relation is shown to be frequency independent, and equal to the
average kinetic energy, known as the granular temperature. In the second model
analyzed, a mean-field granular gas, the collision rate of a particle is taken
to be proportional to its velocity. The Green-Kubo relation in the high
frequency limit is calculated for this model, and the effective temperature in
this limit is shown to be equal to the granular temperature. This result, taken
together with previous results, showing a difference between the effective
temperature at zero frequency (the Einstein relation) and the granular
temperature, shows that the Green-Kubo relation for granular gases is violated.
| [
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] | 2008-05-19T00:00:00 | [
[
"Bunin",
"Guy",
""
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""
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""
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712.078 | Arlene Cristina Aguilar | A. C. Aguilar, J. Papavassiliou | Infrared finite ghost propagator in the Feynman gauge | 22 pages, 9 figures | Phys.Rev.D77:125022,2008 | 10.1103/PhysRevD.77.125022 | null | hep-ph | null | We demonstrate how to obtain from the Schwinger-Dyson equations of QCD an
infrared finite ghost propagator in the Feynman gauge. The key ingredient in
this construction is the longitudinal form factor of the non-perturbative
gluon-ghost vertex, which, contrary to what happens in the Landau gauge,
contributes non-trivially to the gap equation of the ghost. The detailed study
of the corresponding vertex equation reveals that in the presence of a
dynamical infrared cutoff this form factor remains finite in the limit of
vanishing ghost momentum. This, in turn, allows the ghost self-energy to reach
a finite value in the infrared, without having to assume any additional
properties for the gluon-ghost vertex, such as the presence of massless poles.
The implications of this result and possible future directions are briefly
outlined.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 17:02:19 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Aguilar",
"A. C.",
""
],
[
"Papavassiliou",
"J.",
""
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712.0781 | Ana Carolina Bruno Machado Miss | A. C. B. Machado and V. Pleitez | The flavor problem and discrete symmetries | 9 pages, no figures; Report No. corrected; new references added.
Version to be published in PLB | Phys.Lett.B674:223-226,2009 | 10.1016/j.physletb.2009.03.022 | IFT-P.021/2007 | hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this letter we propose a multi-Higgs extension of the standard model with
Abelian and non-Abelian discrete symmetries in which the mass matrices of the
charged fermions obtained from renormalizable interactions are diagonal.
Corrections induced by non-renormalizable interactions deviate these matrices
from the diagonal form. Active neutrinos acquire mass only from
non-renormalizable interactions. The main entries of the neutrino mass matrix
arise only through dimension five operators, while the diagonal entries arise
only from dimension six operators.
| [
{
"version": "v1",
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},
{
"version": "v2",
"created": "Fri, 7 Dec 2007 16:11:37 GMT"
},
{
"version": "v3",
"created": "Fri, 20 Mar 2009 18:37:43 GMT"
}
] | 2009-04-06T00:00:00 | [
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""
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] |
712.0782 | Ebrahim Karimi | Ebrahim Karimi, Gianluigi Zito, Bruno Piccirillo, Lorenzo Marrucci,
and Enrico Santamato | Hypergeometric-Gaussian Modes | null | Optics Letters, (Vol 32) Page 3053-3055 (2007) | 10.1364/OL.32.003053 | null | physics.optics math-ph math.MP | null | We studied a novel family of paraxial laser beams forming an overcomplete yet
nonorthogonal set of modes. These modes have a singular phase profile and are
eigenfunctions of the photon orbital angular momentum. The intensity profile is
characterized by a single brilliant ring with the singularity at its center,
where the field amplitude vanishes. The complex amplitude is proportional to
the degenerate (confluent) hypergeometric function, and therefore we term such
beams hypergeometric gaussian (HyGG) modes. Unlike the recently introduced
hypergeometric modes (Opt. Lett. {\textbf 32}, 742 (2007)), the HyGG modes
carry a finite power and have been generated in this work with a liquid-crystal
spatial light modulator. We briefly consider some sub-families of the HyGG
modes as the modified Bessel Gaussian modes, the modified exponential Gaussian
modes and the modified Laguerre-Gaussian modes.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 17:03:51 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Karimi",
"Ebrahim",
""
],
[
"Zito",
"Gianluigi",
""
],
[
"Piccirillo",
"Bruno",
""
],
[
"Marrucci",
"Lorenzo",
""
],
[
"Santamato",
"Enrico",
""
]
] | [
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] |
712.0783 | Fabio Gastaldello | Fabio Gastaldello (1,2), David A. Buote (1), Fabrizio Brighenti (2,3),
William G. Mathews (3) ((1) UC Irvine, (2) Universita' di Bologna, (3) UC
Santa Cruz) | Trouble for AGN Feedback ? The puzzle of the core of the Galaxy Cluster
AWM 4 | 5 pages, 3 figures (2 in colour), accepted for publication in ApJ
Letters | Astrophys.J. 673 (2008) L17-L20 | 10.1086/527472 | null | astro-ph | null | The core of the relaxed cluster AWM 4 is characterized by a unique
combination of properties which defy a popular scenario for ANG heating of
cluster cores. A flat inner temperature profile is indicative of a past, major
heating episode which completely erased the cool core, as testified by the high
central cooling time (~ 3 Gyr) and by the high central entropy level (~ 60 keV
cm^2). Yet the presence of a 1.4 GHz active central radio galaxy with extended
radio lobes out to 100 kpc, reveals recent feeding of the central massive black
hole. A system like AWM 4 should have no radio emission at all if only feedback
from the cooling hot gas regulates the AGN activity.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 17:15:06 GMT"
}
] | 2014-11-07T00:00:00 | [
[
"Gastaldello",
"Fabio",
""
],
[
"Buote",
"David A.",
""
],
[
"Brighenti",
"Fabrizio",
""
],
[
"Mathews",
"William G.",
""
]
] | [
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] |
712.0784 | Daniela Maionchi | D. O. Maionchi, A. F. Morais, R. N. Costa Filho, J. S. Andrade Jr, H.
J. Herrmann | Model for erosion-deposition patterns | 8 pages, 12 figures, submitted to Phys. Rev. E | null | 10.1103/PhysRevE.77.061402 | null | physics.comp-ph physics.flu-dyn | null | We investigate through computational simulations with a pore network model
the formation of patterns caused by erosion-deposition mechanisms. In this
model, the geometry of the pore space changes dynamically as a consequence of
the coupling between the fluid flow and the movement of particles due to local
drag forces. Our results for this irreversible process show that the model is
capable to reproduce typical natural patterns caused by well known erosion
processes. Moreover, we observe that, within a certain range of porosity
values, the grains form clusters that are tilted with respect to the horizontal
with a characteristic angle. We compare our results to recent experiments for
granular material in flowing water and show that they present a satisfactory
agreement.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 17:25:00 GMT"
},
{
"version": "v2",
"created": "Thu, 6 Dec 2007 16:49:37 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Maionchi",
"D. O.",
""
],
[
"Morais",
"A. F.",
""
],
[
"Filho",
"R. N. Costa",
""
],
[
"Andrade",
"J. S.",
"Jr"
],
[
"Herrmann",
"H. J.",
""
]
] | [
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] |
712.0785 | Sonia L Rueda | Sonia L. Rueda, J. Rafael Sendra | Linear Complete Differential Resultants and the Implicitization of
Linear DPPEs | 26 pages | Journal of Symbolic Computation, 45, 324-341 (2010) | null | null | math.CA | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The linear complete differential resultant of a finite set of linear ordinary
differential polynomials is defined. We study the computation by linear
complete differential resultants of the implicit equation of a system of $n$
linear differential polynomial parametric equations in $n-1$ differential
parameters. We give necessary conditions to ensure properness of the system of
differential polynomial parametric equations.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 17:21:58 GMT"
},
{
"version": "v2",
"created": "Fri, 11 Jul 2008 09:53:34 GMT"
}
] | 2012-04-10T00:00:00 | [
[
"Rueda",
"Sonia L.",
""
],
[
"Sendra",
"J. Rafael",
""
]
] | [
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712.0786 | Wieslaw Kubi\'s | Wieslaw Kubis, Katsuro Sakai | Hausdorff hyperspaces of $R^m$ and their dense subspaces | 21 pages; to appear in J. Math. Soc. Japan | J. Math. Soc. Japan 60 (2008), no. 1, 193--217 | 10.2969/jmsj/06010193 | null | math.GN | null | Let $CLB_H(X)$ denote the hyperspace of closed bounded subsets of a metric
space $X$, endowed with the Hausdorff metric topology. We prove, among others,
that natural dense subspaces of $CLB_H(R^m)$ of all nowhere dense closed sets,
of all perfect sets, of all Cantor sets and of all Lebesgue measure zero sets
are homeomorphic to the Hilbert space $\ell_2$.
Moreover, we investigate the hyperspace $CL_H(R)$ of all nonempty closed
subsets of the real line $R$ with the Hausdorff (infinite-valued) metric. We
show that a nonseparable component of $CL_H(R)$ is homeomorphic to the Hilbert
space $\ell_2(2^{\aleph_0})$ as long as it does not contain any of the sets $R,
[0,\infty), (-\infty,0]$.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 17:23:38 GMT"
}
] | 2012-10-23T00:00:00 | [
[
"Kubis",
"Wieslaw",
""
],
[
"Sakai",
"Katsuro",
""
]
] | [
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] |
712.0787 | Thulsi Wickramasinghe | T. Wickramasinghe | An Approximate Analytical Algorithm for Evaluating the Distances in a
Dark Energy Dominated Universe | null | null | null | null | astro-ph | null | The most recent cosmological observations indicate that the present universe
is flat and vacuum dominated. In such a universe, the distance measurements are
always difficult and involve numerical computations. In this paper, it is shown
that the most fundamental distance measurement of cosmology, the luminosity
distance, for such a universe can be obtained in an approximate analytical way
with very small errors of less than 0.02% up to %z = 5$ for any value of vacuum
energy. The analytical calculation is shown to be exceedingly efficient, as
compared to the traditional numerical methods.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 17:31:47 GMT"
}
] | 2007-12-06T00:00:00 | [
[
"Wickramasinghe",
"T.",
""
]
] | [
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] |
712.0788 | Dennis Gaitsgory | Edward Frenkel and Dennis Gaitsgory | D-modules on the affine flag variety and representations of affine
Kac-Moody algebras | null | null | null | null | math.RT math.AG | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the connection between the category of modules over the affine
Kac-Moody Lie algebra at the critical level, and the category of D-modules on
the affine flag scheme G((t))/I, where I is the Iwahori subgroup.
We prove a localization-type result, which establishes an equivalence between
certain subcategories on both sides.
We also establish an equivalence between a certain subcategory of Kac-Moody
modules, and the category of quasi-coherent sheaves on the scheme of Miura
opers for the Langlands dual group, thereby proving a conjecture of [FG2].
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 17:41:33 GMT"
},
{
"version": "v2",
"created": "Mon, 6 Jul 2009 20:23:16 GMT"
},
{
"version": "v3",
"created": "Tue, 29 Sep 2009 05:38:24 GMT"
}
] | 2009-09-29T00:00:00 | [
[
"Frenkel",
"Edward",
""
],
[
"Gaitsgory",
"Dennis",
""
]
] | [
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] |
712.0789 | Sangchul Oh | Sangchul Oh | Quantum Computational Method of Finding the Ground State Energy and
Expectation Values | 5 pages, 5 figures, accepted for publication in Phys. Rev. A | Phys. Rev. A 77, 012326 (2008) | 10.1103/PhysRevA.77.012326 | null | quant-ph | null | We propose a new quantum computational way of obtaining a ground-state energy
and expectation values of observables of interacting Hamiltonians. It is based
on the combination of the adiabatic quantum evolution to project a ground state
of a non-interacting Hamiltonian onto a ground state of an interacting
Hamiltonian and the phase estimation algorithm to retrieve the ground-state
energy. The expectation value of an observable for the ground state is obtained
with the help of Hellmann-Feynman theorem. As an illustration of our method, we
consider a displaced harmonic oscillator, a quartic anharmonic oscillator,and a
potential scattering model. The results obtained by this method are in good
agreement with the known results.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 18:14:55 GMT"
}
] | 2009-10-31T00:00:00 | [
[
"Oh",
"Sangchul",
""
]
] | [
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] |
712.079 | David Asher Levin | David A. Levin, Malwina J. Luczak, Yuval Peres | Glauber dynamics for the mean-field Ising model: cut-off, critical power
law, and metastability | 40 pages | null | null | null | math.PR | null | We study the Glauber dynamics for the Ising model on the complete graph, also
known as the Curie-Weiss Model. For beta < 1, we prove that the dynamics
exhibits a cut-off: the distance to stationarity drops from near 1 to near 0 in
a window of order n centered at [2(1-beta)]^{-1} n log n. For beta = 1, we
prove that the mixing time is of order n^{3/2}. For beta > 1, we study
metastability. In particular, we show that the Glauber dynamics restricted to
states of non-negative magnetization has mixing time O(n log n).
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 18:15:27 GMT"
},
{
"version": "v2",
"created": "Mon, 10 Dec 2007 22:25:20 GMT"
}
] | 2007-12-11T00:00:00 | [
[
"Levin",
"David A.",
""
],
[
"Luczak",
"Malwina J.",
""
],
[
"Peres",
"Yuval",
""
]
] | [
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] |
712.0791 | Oscar J. C. Dias | Oscar J.C. Dias, Roberto Emparan, Alessandro Maccarrone | Microscopic Theory of Black Hole Superradiance | 33 pages, 1 figure. v2: minor corrections | Phys.Rev.D77:064018,2008 | 10.1103/PhysRevD.77.064018 | null | hep-th | null | We study how black hole superradiance appears in string microscopic models of
rotating black holes. In order to disentangle superradiance from
finite-temperature effects, we consider an extremal, rotating D1-D5-P black
hole that has an ergosphere and is not supersymmetric. We explain how the
microscopic dual accounts for the superradiant ergosphere of this black hole.
The bound 0< omega < m Omega_H on superradiant mode frequencies is argued to be
a consequence of Fermi-Dirac statistics for the spin-carrying degrees of
freedom in the dual CFT. We also compute the superradiant emission rates from
both sides of the correspondence, and show their agreement.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 18:30:42 GMT"
},
{
"version": "v2",
"created": "Wed, 26 Dec 2007 23:04:00 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Dias",
"Oscar J. C.",
""
],
[
"Emparan",
"Roberto",
""
],
[
"Maccarrone",
"Alessandro",
""
]
] | [
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] |
712.0792 | Giovanni Morando | Giovanni Morando | Tempered solutions of $\mathcal D$-modules on complex curves and formal
invariants | 31 pages | null | null | null | math.AG math.CV | null | Let $X$ be a complex analytic curve. In this paper we prove that the
subanalytic sheaf of tempered holomorphic solutions of $\mathcal D_X$-modules
induces a fully faithful functor on a subcategory of germs of formal holonomic
$\mathcal D_X$-modules. Further, given a germ $\mathcal M$ of holonomic
$\mathcal D_X$-module, we obtain some results linking the subanalytic sheaf of
tempered solutions of $\mathcal M$ and the classical formal and analytic
invariants of $\mathcal M$.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 18:53:16 GMT"
}
] | 2007-12-06T00:00:00 | [
[
"Morando",
"Giovanni",
""
]
] | [
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] |
712.0793 | Kambiz Fathi | Kambiz Fathi, John E. Beckman, Andreas A. Lundgren, Claude Carignan,
Olivier Hernandez, Philippe Amram, Philippe Balard, Jacques Boulesteix,
Jean-Luc Gach, Johan H. Knapen, Monica Rela\~no | Spiral inflow feeding the nuclear starburst in M83, observed in H-alpha
emission with the GHAFAS Fabry-Perot interferometer | Accepted for publication in ApJ Letters. High-resolution version can
be found at http://www.astro.su.se/~kambiz/DOC/paper-M83.pdf | null | 10.1086/527473 | null | astro-ph | null | We present observations of the nearby barred starburst galaxy, M83 (NGC5236),
with the new Fabry-Perot interferometer GHAFAS mounted on the 4.2 meter William
Herschel Telescope on La Palma. The unprecedented high resolution observations,
of 16 pc/FWHM, of the H-alpha-emitting gas cover the central two kpc of the
galaxy. The velocity field displays the dominant disk rotation with signatures
of gas inflow from kpc scales down to the nuclear regions. At the inner Inner
Lindblad Resonance radius of the main bar and centerd at the dynamical center
of the main galaxy disk, a nuclear $5.5 (\pm 0.9) \times 10^8 M_\odot$ rapidly
rotating disk with scale length of $60 \pm 20$ pc has formed. The nuclear
starburst is found in the vicinity as well as inside this nuclear disk, and our
observations confirm that gas spirals in from the outer parts to feed the
nuclear starburst, giving rise to several star formation events at different
epochs, within the central 100 pc radius of M83.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 18:40:14 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Fathi",
"Kambiz",
""
],
[
"Beckman",
"John E.",
""
],
[
"Lundgren",
"Andreas A.",
""
],
[
"Carignan",
"Claude",
""
],
[
"Hernandez",
"Olivier",
""
],
[
"Amram",
"Philippe",
""
],
[
"Balard",
"Philippe",
""
],
[
"Boulesteix",
"Jacques",
""
],
[
"Gach",
"Jean-Luc",
""
],
[
"Knapen",
"Johan H.",
""
],
[
"Relaño",
"Monica",
""
]
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] |
712.0794 | Brian DeMarco | M. Pasienski and B. DeMarco | A high-accuracy algorithm for designing arbitrary holographic atom traps | version with high-resolution figures available at
http://research.physics.uiuc.edu/DeMarco/ | null | 10.1364/OE.16.002176 | null | physics.atom-ph | null | We report the realization of a new iterative Fourier-transform algorithm for
creating holograms that can diffract light into an arbitrary two-dimensional
intensity profile. We show that the predicted intensity distributions are
smooth with a fractional error from the target distribution at the percent
level. We demonstrate that this new algorithm outperforms the most frequently
used alternatives typically by one and two orders of magnitude in accuracy and
roughness, respectively. The techniques described in this paper outline a path
to creating arbitrary holographic atom traps in which the only remaining hurdle
is physical implementation.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 18:14:52 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Pasienski",
"M.",
""
],
[
"DeMarco",
"B.",
""
]
] | [
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] |
712.0795 | Alejandro Corsico | A. H. C\'orsico, L. G. Althaus, S. O. Kepler, J. E. S. Costa, and M.
M. Miller Bertolami | Asteroseismological measurements on PG 1159-035, the prototype of the GW
Vir variable stars | 14 pages, 11 figures, 5 tables. To be published in Astronomy &
Astrophysics | null | 10.1051/0004-6361:20078646 | null | astro-ph | null | An asteroseismological study of PG 1159-035, the prototype of the GW Vir
variable stars, has been performed on the basis of detailed and full PG1159
evolutionary models presented by Miller Bertolami & Althaus (2006). We carried
out extensive computations of adiabatic g-mode pulsation periods on PG1159
evolutionary models with stellar masses spanning the range 0.530 to 0.741 Mo.
We derive a stellar mass in the range 0.56-0.59 Mo from the period-spacing data
alone. We also find, on the basis of a period-fit procedure, a seismic model
representative of PG 1159-035 that reproduces the observed period pattern with
an average of the period differences of 0.64-1.03 s, consistent with the
expected model uncertainties. The results of the period-fit analysis carried
out in this work suggest that the surface gravity of PG 1159-035 would be 1
sigma larger than the spectroscopically inferred gravity. For our best-fit
model of PG 1159-035, all of the pulsation modes are characterized by positive
rates of period changes, at odds with the measurements by Costa & Kepler
(2007).
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 18:29:25 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Córsico",
"A. H.",
""
],
[
"Althaus",
"L. G.",
""
],
[
"Kepler",
"S. O.",
""
],
[
"Costa",
"J. E. S.",
""
],
[
"Bertolami",
"M. M. Miller",
""
]
] | [
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0.0072517609,
-0.0110664219,
-0.0929058641,
0.0064608376,
0.111237064,
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-0.0558268428,
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] |
712.0796 | Enrique Fernandez-Martinez | Pilar Coloma, Andrea Donini, Enrique Fernandez-Martinez, Jacobo
Lopez-Pavon | $\theta_{13}$, $\delta$ and the neutrino mass hierarchy at a
$\gamma=350$ double baseline Li/B $\beta$-Beam | 35 pages, 20 figures. Minor changes, matches the published version | JHEP 0805:050,2008 | 10.1088/1126-6708/2008/05/050 | null | hep-ph hep-ex | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We consider a $\beta$-Beam facility where $^8$Li and $^8$B ions are
accelerated at $\gamma = 350$, accumulated in a 10 Km storage ring and let
decay, so as to produce intense $\bar \nu_e$ and $\nu_e$ beams. These beams
illuminate two iron detectors located at $L \simeq 2000$ Km and $L \simeq 7000$
Km, respectively. The physics potential of this setup is analysed in full
detail as a function of the flux. We find that, for the highest flux ($10
\times 10^{18}$ ion decays per year per baseline), the sensitivity to
$\theta_{13}$ reaches $\sin^2 2 \theta_{13} \geq 2 \times10^{-4}$; the sign of
the atmospheric mass difference can be identified, regardless of the true
hierarchy, for $\sin^2 2 \theta_{13} \geq 4\times10^{-4}$; and, CP-violation
can be discovered in 70% of the $\delta$-parameter space for $\sin^2 2
\theta_{13} \geq 10^{-3}$, having some sensitivity to CP-violation down to
$\sin^2 2 \theta_{13} \geq 10^{-4}$ for $|\delta| \sim 90^\circ$.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:51:31 GMT"
},
{
"version": "v2",
"created": "Fri, 7 Mar 2008 16:28:48 GMT"
},
{
"version": "v3",
"created": "Tue, 17 Jun 2008 08:02:01 GMT"
}
] | 2010-02-03T00:00:00 | [
[
"Coloma",
"Pilar",
""
],
[
"Donini",
"Andrea",
""
],
[
"Fernandez-Martinez",
"Enrique",
""
],
[
"Lopez-Pavon",
"Jacobo",
""
]
] | [
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] |
712.0797 | Robert Singleton Jr. Dr. | Robert L. Singleton Jr | Calculating the Charged Particle Stopping Power Exactly to Leading and
Next-to-leading Order | 4 pages, proceedings for the 5th International Conference on Inertial
Fusion Science and Applications (IFSA-07), Kobe, Japan, 9-14 September 2007 | null | 10.1088/1742-6596/112/2/022034 | LA-UR-07-5874 | physics.plasm-ph | null | I will discuss a new method for calculating transport quantities, such as the
charged particle stopping power, in a weakly to moderately coupled plasma. This
method, called dimensional continuation, lies within the framework of
convergent kinetic equations, and it is powerful enough to allow for systematic
perturbative expansions in the plasma coupling constant. In particular, it
provides an exact evaluation of the stopping power to leading and
next-to-leading order in the plasma coupling, with the systematic error being
of cubic order. Consequently, the calculation is near-exact for a weakly
coupled plasma, and quite accurate for a moderately coupled plasma. The leading
order term in this expansion has been known since the classic work of Spitzer.
In contrast, the next-to-leading order term has been calculated only recently
by Brown, Preston, and Singleton (BPS), using the aforementioned method, to
account for all short- and long-distance physics accurate to second order in
the plasma coupling, including an exact treatment of the quantum-to-classical
scattering transition. Preliminary numerical studies suggest that the BPS
stopping power increases the ignition threshold, thereby having potential
adverse implications for upcoming high energy density facilities. Since the key
ideas behind the BPS calculation are possibly unfamiliar to plasma physicists,
and the implications might be important, I will use this opportunity to explain
the method in a pedagogical fashion.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 18:58:47 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Singleton",
"Robert L.",
"Jr"
]
] | [
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712.0798 | Gantumur Tsogtgerel | Michael Holst, Gabriel Nagy, Gantumur Tsogtgerel | Rough solutions of the Einstein constraints on closed manifolds without
near-CMC conditions | 65 pages, 3 figures. To appear in Comm. Math. Phys | null | 10.1007/s00220-009-0743-2 | null | gr-qc math.AP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We consider the conformal decomposition of Einstein's constraint equations
introduced by Lichnerowicz and York, on a closed manifold. We establish
existence of non-CMC weak solutions using a combination of a priori estimates
for the individual Hamiltonian and momentum constraints, barrier constructions
for the Hamiltonian constraint, and topological fixed-point arguments. An
important new feature of these results is the absense of the near-CMC
assumption when the rescaled background metric is in the positive Yamabe class,
if the freely specifiable part of the data given by the matter fields (if
present) and the traceless-transverse part of the rescaled extrinsic curvature
are taken to be sufficiently small. In this case, the mean extrinsic curvature
can be taken to be an arbitrary smooth function without restrictions on the
size of its spatial derivatives, giving what are apparently the first non-CMC
existence results without the near-CMC assumption. Standard bootstrapping
arguments to increase the regularity of the conformal factor are blocked by the
use of a weak background metric. In the CMC case, we recover Maxwell's rough
solution results as a special case. Our results extend the 1996 non-CMC result
of Isenberg and Moncrief in three ways: (1) the near-CMC assumption is removed
in the case of the positive Yamabe class; (2) regularity is extended down to
the maximum allowed by the background metric and the matter; and (3) the result
holds for all three Yamabe classes. This last extension was also accomplished
recently by Allen, Clausen and Isenberg, although their result is restricted to
the near-CMC case and to smoother background metrics and data.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:27:36 GMT"
},
{
"version": "v2",
"created": "Mon, 31 Mar 2008 10:52:21 GMT"
},
{
"version": "v3",
"created": "Thu, 3 Apr 2008 09:19:26 GMT"
},
{
"version": "v4",
"created": "Sat, 12 Apr 2008 07:45:04 GMT"
},
{
"version": "v5",
"created": "Fri, 29 Aug 2008 05:37:58 GMT"
}
] | 2010-01-13T00:00:00 | [
[
"Holst",
"Michael",
""
],
[
"Nagy",
"Gabriel",
""
],
[
"Tsogtgerel",
"Gantumur",
""
]
] | [
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] |
712.0799 | Martin Stringer | M. J. Stringer, A. J. Benson | Modelling the formation and evolution of disk galaxies | 2 pages, 2 figures. to appear in "Pathways through an eclectic
Universe", J. H. Knapen, T. J. Mahoney, and A. Vazdekis (Eds.), ASP Conf.
Ser., 2007 | null | null | null | astro-ph | null | Inspired by recent work on feedback in disk galaxies (Efstathiou 2000, Silk
2003) and on the angular momentum distribution in simulated gas halos (Sharma
and Steinmetz 2005), a fully dynamic model of disk galaxy formation and
evolution has been developed. This is used to demonstrate how observed galactic
systems could have formed from halos similar to those found in simulations and
applies physically motivated models of star formation and feedback to explore
whether the true nature of these processes would be manifest from local and
cosmological observables. This is made possible by computational integration
with the galaxy formation model developed originally by the group at Durham
University (Cole et al. 2000).
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:34:55 GMT"
}
] | 2007-12-06T00:00:00 | [
[
"Stringer",
"M. J.",
""
],
[
"Benson",
"A. J.",
""
]
] | [
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] |
712.08 | Gregg Wade | G.A. Wade, E. Alecian, C. Catala, S. Bagnulo, J.D. Landstreet, J.
Flood, T. Bohm, J.-C. Bouret, J.-F. Donati, C.P. Folsom, J. Grunhut, J.
Silvester | How non-magnetic are "non-magnetic" Herbig Ae/Be stars? | 6 pages, 2 figures. In the proceedings of the "CP/Ap workshop" held
in Vienna, September 2007 | Contrib.Astron.Obs.Skalnate Pleso 38:251-256,2008 | null | null | astro-ph | null | Our recent discovery of magnetic fields in a small number of Herbig Ae/Be
stars has required that we survey a much larger sample of stars. From our FORS1
and ESPaDOnS surveys, we have acquired about 125 observations of some 70 stars
in which no magnetic fields are detected. Using a Monte Carlo approach, we have
performed statistical comparisons of the observed longitudinal fields and LSD
Stokes V profiles of these apparently non-magnetic stars with a variety of
field models. This has allowed us to derive general upper limits on the
presence of dipolar fields in the sample, and to place realistic upper limits
on undetected dipole fields which may be present in individual stars. This
paper briefly reports the results of the statistical modeling, as well as field
upper limits for individual stars of particular interest.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:21:17 GMT"
}
] | 2010-11-26T00:00:00 | [
[
"Wade",
"G. A.",
""
],
[
"Alecian",
"E.",
""
],
[
"Catala",
"C.",
""
],
[
"Bagnulo",
"S.",
""
],
[
"Landstreet",
"J. D.",
""
],
[
"Flood",
"J.",
""
],
[
"Bohm",
"T.",
""
],
[
"Bouret",
"J. -C.",
""
],
[
"Donati",
"J. -F.",
""
],
[
"Folsom",
"C. P.",
""
],
[
"Grunhut",
"J.",
""
],
[
"Silvester",
"J.",
""
]
] | [
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] |
712.0801 | Andrei A. Fedorenko | Andrei A. Fedorenko | Elastic systems with correlated disorder: Response to tilt and
application to surface growth | 15 pages, 8 figures, revtex4 | Phys. Rev. B 77, 094203 (2008) | 10.1103/PhysRevB.77.094203 | null | cond-mat.dis-nn cond-mat.stat-mech | null | We study elastic systems such as interfaces or lattices pinned by correlated
quenched disorder considering two different types of correlations: generalized
columnar disorder and quenched defects correlated as ~ x^{-a} for large
separation x. Using functional renormalization group methods, we obtain the
critical exponents to two-loop order and calculate the response to a transverse
field h. The correlated disorder violates the statistical tilt symmetry
resulting in nonlinear response to a tilt. Elastic systems with columnar
disorder exhibit a transverse Meissner effect: disorder generates the critical
field h_c below which there is no response to a tilt and above which the tilt
angle behaves as \theta ~ (h-h_c)^{\phi} with a universal exponent \phi<1. This
describes the destruction of a weak Bose glass in type-II superconductors with
columnar disorder caused by tilt of the magnetic field. For isotropic
long-range correlated disorder, the linear tilt modulus vanishes at small
fields leading to a power-law response \theta ~ h^{\phi} with \phi>1. The
obtained results are applied to the Kardar-Parisi-Zhang equation with
temporally correlated noise.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:38:49 GMT"
},
{
"version": "v2",
"created": "Sat, 15 Mar 2008 16:42:25 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Fedorenko",
"Andrei A.",
""
]
] | [
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] |
712.0802 | Jo\~ao Penedones | Joao Penedones (Porto University) | High Energy Scattering in the AdS/CFT Correspondence | PhD thesis, 118 pages, 35 figures. v2: Minor corrections and
references added | null | null | null | hep-th | null | This work explores the celebrated AdS/CFT correspondence in the regime of
high energy scattering in Anti--de Sitter (AdS) spacetime. In particular, we
develop the eikonal approximation to high energy scattering in AdS and explore
its consequences for the dual Conformal Field Theory (CFT).
Using position space Feynman rules, we rederive the eikonal approximation for
high energy scattering in flat space. Following this intuitive position space
perspective, we then generalize the eikonal approximation for high energy
scattering in AdS and other spacetimes. Remarkably, we are able to resum, in
terms of a generalized phase shift, ladder and cross ladder Witten diagrams
associated to the exchange of an AdS spin j field, to all orders in the
coupling constant.
By the AdS/CFT correspondence, the eikonal amplitude in AdS is related to the
four point function of CFT primary operators in the regime of large 't Hooft
coupling, including all terms of the 1/N expansion. We then show that the
eikonal amplitude determines the behavior of the CFT four point function for
small values of the cross ratios in a Lorentzian regime and that this controls
its high spin and dimension conformal partial wave decomposition. These results
allow us to determine the anomalous dimension of high spin and dimension double
trace primary operators, by relating it to the AdS eikonal phase shift. Finally
we find that, at large energies and large impact parameters in AdS, the
gravitational interaction dominates all other interactions, as in flat space.
Therefore, the anomalous dimension of double trace operators, associated to
graviton exchange in AdS, yields a universal prediction for CFT's with AdS
gravitational duals.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:23:26 GMT"
},
{
"version": "v2",
"created": "Wed, 6 Feb 2008 09:43:57 GMT"
}
] | 2008-02-06T00:00:00 | [
[
"Penedones",
"Joao",
"",
"Porto University"
]
] | [
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] |
712.0803 | Junjie Zhu | D0 Collaboration: V. Abazov, et al | Measurement of the shape of the boson transverse momentum distribution
in ppbar -> Z/gamma* -> ee+X events produced at sqrt{s}=1.96 TeV | 7 pages, 4 figures, published in Phys. Rev. Lett 100, 102002 (2008) | Phys.Rev.Lett.100:102002,2008 | 10.1103/PhysRevLett.100.102002 | Fermilab-Pub-07/642-E | hep-ex | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present a measurement of the shape of the Z/gamma* boson transverse
momentum (qT) distribution in ppbar -> Z/gamma* -> ee+X events at a
center-of-mass energy of 1.96 TeV using 0.98 fb-1 of data collected with the D0
detector at the Fermilab Tevatron collider. The data are found to be consistent
with the resummation prediction at low qT, but above the perturbative QCD
calculation in the region of qT>30 GeV/c. Using events with qT<30 GeV/c, we
extract the value of g2, one of the non-perturbative parameters for the
resummation calculation. Data at large boson rapidity y are compared with the
prediction of resummation and with alternative models that employ a resummed
form factor with modifications in the small Bjorken x region of the proton wave
function.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:24:26 GMT"
},
{
"version": "v2",
"created": "Tue, 14 Oct 2008 16:20:25 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"D0 Collaboration",
"",
""
],
[
"Abazov",
"V.",
""
]
] | [
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] |
712.0804 | Gregory Gutin | A. Gupta, G. Gutin, M. Karimi, E.J. Kim, A. Rafiey | Minimum Cost Homomorphisms to Locally Semicomplete and Quasi-Transitive
Digraphs | null | null | null | null | cs.DM | null | For digraphs $G$ and $H$, a homomorphism of $G$ to $H$ is a mapping $f:\
V(G)\dom V(H)$ such that $uv\in A(G)$ implies $f(u)f(v)\in A(H)$. If, moreover,
each vertex $u \in V(G)$ is associated with costs $c_i(u), i \in V(H)$, then
the cost of a homomorphism $f$ is $\sum_{u\in V(G)}c_{f(u)}(u)$. For each fixed
digraph $H$, the minimum cost homomorphism problem for $H$, denoted
MinHOM($H$), can be formulated as follows: Given an input digraph $G$, together
with costs $c_i(u)$, $u\in V(G)$, $i\in V(H)$, decide whether there exists a
homomorphism of $G$ to $H$ and, if one exists, to find one of minimum cost.
Minimum cost homomorphism problems encompass (or are related to) many well
studied optimization problems such as the minimum cost chromatic partition and
repair analysis problems. We focus on the minimum cost homomorphism problem for
locally semicomplete digraphs and quasi-transitive digraphs which are two
well-known generalizations of tournaments. Using graph-theoretic
characterization results for the two digraph classes, we obtain a full
dichotomy classification of the complexity of minimum cost homomorphism
problems for both classes.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:25:40 GMT"
}
] | 2007-12-06T00:00:00 | [
[
"Gupta",
"A.",
""
],
[
"Gutin",
"G.",
""
],
[
"Karimi",
"M.",
""
],
[
"Kim",
"E. J.",
""
],
[
"Rafiey",
"A.",
""
]
] | [
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] |
712.0805 | Sho Yaida | Mauro Brigante, Hong Liu, Robert C. Myers, Stephen Shenker, Sho Yaida | Viscosity Bound Violation in Higher Derivative Gravity | 23 pages, 2 figures; v2: typos corrected, references added, notes
added; v3: subsections IV.C and IV.D eliminated, comments on the null energy
condition eliminated, minor revisions made | Phys.Rev.D77:126006,2008 | 10.1103/PhysRevD.77.126006 | CAS-KITPC/ITP-025, MIT-CTP-3918, SU-ITP-07/22 | hep-th gr-qc hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Motivated by the vast string landscape, we consider the shear viscosity to
entropy density ratio in conformal field theories dual to Einstein gravity with
curvature square corrections. After field redefinitions these theories reduce
to Gauss-Bonnet gravity, which has special properties that allow us to compute
the shear viscosity nonperturbatively in the Gauss-Bonnet coupling. By tuning
of the coupling, the value of the shear viscosity to entropy density ratio can
be adjusted to any positive value from infinity down to zero, thus violating
the conjectured viscosity bound. At linear order in the coupling, we also check
consistency of four different methods to calculate the shear viscosity, and we
find that all of them agree. We search for possible pathologies associated with
this class of theories violating the viscosity bound.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:51:34 GMT"
},
{
"version": "v2",
"created": "Fri, 22 Feb 2008 15:57:16 GMT"
},
{
"version": "v3",
"created": "Fri, 13 Jun 2008 15:39:13 GMT"
}
] | 2010-04-06T00:00:00 | [
[
"Brigante",
"Mauro",
""
],
[
"Liu",
"Hong",
""
],
[
"Myers",
"Robert C.",
""
],
[
"Shenker",
"Stephen",
""
],
[
"Yaida",
"Sho",
""
]
] | [
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] |
712.0806 | Vitor Pereira | Vitor M. Pereira, J. M. B. Lopes dos Santos, A. H. Castro Neto | Modeling disorder in graphene | 16 pages, lower resolution figures | Phys. Rev. B 77, 115109 (2008) | 10.1103/PhysRevB.77.115109 | null | cond-mat.dis-nn cond-mat.mtrl-sci | null | We present a study of different models of local disorder in graphene. Our
focus is on the main effects that vacancies -- random, compensated and
uncompensated --, local impurities and substitutional impurities bring into the
electronic structure of graphene. By exploring these types of disorder and
their connections, we show that they introduce dramatic changes in the low
energy spectrum of graphene, viz. localized zero modes, strong resonances, gap
and pseudogap behavior, and non-dispersive midgap zero modes.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:10:24 GMT"
}
] | 2008-03-25T00:00:00 | [
[
"Pereira",
"Vitor M.",
""
],
[
"Santos",
"J. M. B. Lopes dos",
""
],
[
"Neto",
"A. H. Castro",
""
]
] | [
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] |
712.0807 | Lorenzo Nicolodi | Emilio Musso, Lorenzo Nicolodi | Conformal deformation of spacelike surfaces in Minkowski space | 18 pages, final version to appear in Houston J. Math. | Houston J. Math. 35 (2009) 1029-1049 | null | null | math.DG | null | We address the problem of second order conformal deformation of spacelike
surfaces in compactified Minkowski 4-space. We explain the construction of the
exterior differential system of conformal deformations and discuss its general
and singular solutions. In particular, we show that isothermic surfaces are
singular solutions of the system, which implies that a generic second order
deformable surface is not isothermic. This differs from the situation in
3-dimensional conformal geometry, where isothermic surfaces coincide with
deformable surfaces.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:33:50 GMT"
}
] | 2010-08-03T00:00:00 | [
[
"Musso",
"Emilio",
""
],
[
"Nicolodi",
"Lorenzo",
""
]
] | [
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] |
712.0808 | Hassan Firouzjahi | E.J. Copeland, H. Firouzjahi, T.W.B. Kibble and D.A. Steer | On the Collision of Cosmic Superstrings | 13 pages, 2 figures | Phys.Rev.D77:063521,2008 | 10.1103/PhysRevD.77.063521 | null | hep-th astro-ph | null | We study the formation of three-string junctions between (p,q)-cosmic
superstrings, and collisions between such strings and show that kinematic
constraints analogous to those found previously for collisions of Nambu-Goto
strings apply here too, with suitable modifications to take account of the
additional requirements of flux conservation. We examine in detail several
examples involving collisions between strings with low values of p and q, and
also examine the rates of growth or shrinkage of strings at a junction.
Finally, we briefly discuss the formation of junctions for strings in a warped
space, specifically with a Klebanov-Strassler throat, and show that similar
constraints still apply with changes to the parameters taking account of the
warping and the background flux.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:37:48 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Copeland",
"E. J.",
""
],
[
"Firouzjahi",
"H.",
""
],
[
"Kibble",
"T. W. B.",
""
],
[
"Steer",
"D. A.",
""
]
] | [
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] |
712.0809 | Victor Khalack R | V. Khalack, F. LeBlanc, B. B. Behr, G. A. Wade, D. Bohlender | Vertical stratification of iron abundance in atmospheres of blue
horizontal-branch stars | 2 pages, published in Contrib. Astron. Obs. Skalnate Pleso | Contrib.Astron.Obs.Skalnate Pleso 38:417-418,2008 | null | null | astro-ph | null | The observed slow rotation and abundance peculiarities of certain blue
horizontal branch (BHB) stars suggests that atomic diffusion can be important
in their stellar atmospheres and can lead to vertical abundance stratification
of chemical species in the atmosphere. To verify this hypothesis, we have
undertaken an abundance stratification analysis in the atmospheres of six BHB
stars, based on recently acquired McDonald-CE spectra. Our numerical
simulations show that the iron abundance is vertically stratified in the
atmospheres of two stars in M15: B267 and B279. One star WF2-2541 in M13 also
appears to have vertically stratified iron abundance, while for WF4-3085 the
signatures of iron stratification are less convincing. In all cases the iron
abundances increase towards the lower atmosphere. The other two stars in our
sample, WF4-3485 and B84, do not show any significant variation of iron with
atmospheric depth. Our results support the idea that atomic diffusion dominates
other hydrodynamic processes in the atmospheres of BHB stars.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:47:49 GMT"
}
] | 2010-11-26T00:00:00 | [
[
"Khalack",
"V.",
""
],
[
"LeBlanc",
"F.",
""
],
[
"Behr",
"B. B.",
""
],
[
"Wade",
"G. A.",
""
],
[
"Bohlender",
"D.",
""
]
] | [
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] |
712.081 | Matt Visser | Matt Visser (Victoria University of Wellington) | Emergent rainbow spacetimes: Two pedagogical examples | 16 pages. Based on a talk presented at the conference "Time and
Matter II", Lake Bled, Slovenia, August 2007; V2: more references added | null | null | null | gr-qc | null | There is a possibility that spacetime itself is ultimately an emergent
phenomenon, a near-universal "low-energy long-distance approximation", similar
to the way in which fluid mechanics is the near-universal low-energy
long-distance approximation to quantum molecular dynamics. If so, then direct
attempts to quantize spacetime are misguided - at least as far as fundamental
physics is concerned. Based on this and other considerations, there has
recently been a surge of interest in the notion of energy-dependent and
momentum-dependent "rainbow'' geometries. In the present article I will not
discuss these exotic ideas in any detail, instead I will present two specific
and concrete examples of situations where an energy-dependent "rainbow''
geometry makes perfectly good mathematical and physical sense. These simple
examples will then serve as templates suggesting ways of proceeding in
situations where the underlying physics may be more complex. The specific
models I will deal with are (1) acoustic spacetimes in the presence of
nontrivial dispersion, and (2) a mathematical reinterpretation of Newton's
second law for a non-relativistic conservative force, which is well-known to be
equivalent to the differential geometry of an energy-dependent conformally flat
three-manifold. These two models make it clear that there is nothing wrong with
the concept of an energy-dependent "rainbow'' geometry per se. Whatever
problems may arise in the implementation of any specific
quantum-gravity-inspired proposal for an energy-dependent spacetime are related
to deeper questions regarding the compatibility of that specific proposal with
experimental reality.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:50:37 GMT"
},
{
"version": "v2",
"created": "Thu, 3 Jan 2008 23:33:51 GMT"
}
] | 2008-01-04T00:00:00 | [
[
"Visser",
"Matt",
"",
"Victoria University of Wellington"
]
] | [
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] |
712.0811 | Radim Ba\v{c}a Ing. | R.Baca, V.Snasel, J.Platos, M.Kratky, E.El-Qawasmeh | The Fast Fibonacci Decompression Algorithm | null | null | null | null | cs.PF cs.OH | null | Data compression has been widely applied in many data processing areas.
Compression methods use variable-size codes with the shorter codes assigned to
symbols or groups of symbols that appear in the data frequently. Fibonacci
coding, as a representative of these codes, is used for compressing small
numbers. Time consumption of a decompression algorithm is not usually as
important as the time of a compression algorithm. However, efficiency of the
decompression may be a critical issue in some cases. For example, a real-time
compression of tree data structures follows this issue. Tree's pages are
decompressed during every reading from a secondary storage into the main
memory. In this case, the efficiency of a decompression algorithm is extremely
important. We have developed a Fast Fibonacci decompression for this purpose.
Our approach is up to $3.5\times$ faster than the original implementation.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:55:16 GMT"
},
{
"version": "v2",
"created": "Wed, 19 Dec 2007 08:05:54 GMT"
}
] | 2007-12-19T00:00:00 | [
[
"Baca",
"R.",
""
],
[
"Snasel",
"V.",
""
],
[
"Platos",
"J.",
""
],
[
"Kratky",
"M.",
""
],
[
"El-Qawasmeh",
"E.",
""
]
] | [
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] |
712.0812 | Erin Smith | Erin C. D. Smith, Ian S. McLean | A Survey of 3.3 Micron PAH Emission in Planetary Nebulae | 8 pages, 2 tables, 4 figures, accepted to ApJ | null | 10.1086/527370 | null | astro-ph | null | Results are presented from a pilot survey of 3.3 micron PAH emission from
planetary nebulae using FLITECAM, an instrument intended for airborne astronomy
with SOFIA. The observations were made during ground-based commissioning of
FLITECAM's spectroscopic mode at the 3-m Shane telescope at Lick Observatory.
Direct-ruled KRS-5 grisms were used to give a resolving power (R)~1,700.
Targets were selected from IRAS, KAO and ISO sources with previously observed
PAH emission at longer wavelengths. AGB stars and PN with C/O ratios < 1 were
also added to the target list in order to test PAH detection thresholds. In
all, 20 objects were observed. PAH emission was detected in 11 out of 20
observed targets.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 19:59:27 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Smith",
"Erin C. D.",
""
],
[
"McLean",
"Ian S.",
""
]
] | [
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] |
712.0813 | Gary Felder | Gary N Felder | CLUSTEREASY: A Program for Simulating Scalar Field Evolution on Parallel
Computers | 3 pages, 1 figure | Comput.Phys.Commun.179:604.2008 | 10.1016/j.cpc.2008.06.002 | null | hep-ph hep-lat hep-th | null | We describe a new, parallel programming version of the scalar field
simulation program LATTICEEASY. The new C++ program, CLUSTEREASY, can simulate
arbitrary scalar field models on distributed-memory clusters. The speed and
memory requirements scale well with the number of processors. As with the
serial version of LATTICEEASY, CLUSTEREASY can run simulations in one, two, or
three dimensions, with or without expansion of the universe, with customizable
parameters and output. The program and its full documentation are available on
the LATTICEEASY website at
http://www.science.smith.edu/departments/Physics/fstaff/gfelder/latticeeasy/.
In this paper we provide a brief overview of what CLUSTEREASY does and the ways
in which it does and doesn't differ from the serial version of LATTICEEASY.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:00:31 GMT"
}
] | 2010-05-28T00:00:00 | [
[
"Felder",
"Gary N",
""
]
] | [
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] |
712.0814 | Eric Moulines | Valderio Reisen (UFES), Eric Moulines (LTCI), Philippe Soulier
(MODAL'X), Glaura Franco | Log-average periodogram estimator of the memory parameter | 20 pages | null | null | null | math.ST stat.TH | null | This paper introduces a semiparametric regression estimator of the memory
parameter for long-memory time series process. It is based on the regression in
a neighborhood of the zero-frequency of the periodogram averaged over epochs.
The proposed estimator is theoretically justified and empirical Monte Carlo
investigation gives evidence that the method is very promising to estimate the
long-memory parameter.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:10:03 GMT"
}
] | 2007-12-06T00:00:00 | [
[
"Reisen",
"Valderio",
"",
"UFES"
],
[
"Moulines",
"Eric",
"",
"LTCI"
],
[
"Soulier",
"Philippe",
"",
"MODAL'X"
],
[
"Franco",
"Glaura",
""
]
] | [
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712.0815 | Jason Bell | Jason P. Bell, Pinar Pekcagliyan | Primitivity of finitely presented monomial algebras | 3 figures | null | null | null | math.RA | null | We study prime monomial algebras. Our main result is that a prime finitely
presented monomial algebra is either primitive or it has GK dimension one and
satisfies a polynomial identity. More generally, we show this result holds for
the class of \emph{automaton algebras}; that is, monomial algebras that have a
basis consisting of the set of words recognized by some finite state automaton.
This proves a special case of a conjecture of the first author and Agata
Smoktunowicz.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:12:05 GMT"
}
] | 2007-12-06T00:00:00 | [
[
"Bell",
"Jason P.",
""
],
[
"Pekcagliyan",
"Pinar",
""
]
] | [
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] |
712.0816 | F. J. Sanchez-Salcedo | F.J. Sanchez-Salcedo, K. Saha, C. A. Narayan | The thickness of HI in galactic discs under MOND: theory and application
to the Galaxy | 13 pages, 4 figures | Mon.Not.Roy.Astron.Soc. 385 (2008) 1585-1596 | 10.1111/j.1365-2966.2008.12941.x | null | astro-ph | null | The outskirts of galaxies are a very good laboratory for testing the nature
of the gravitational field at low accelerations. By assuming that the neutral
hydrogen gas is in hydrostatic equilibrium in the gravitational potential of
the host galaxy, the observed flaring of the gas layer can be used to test
modified gravities. For the first time we construct a simple framework to
derive the scaleheight of the neutral hydrogen gas disc in the MOND scenario
and apply this to the Milky Way. It is shown that using a constant gas velocity
dispersion of ~9 km/s, MOND is able to give a very good fit to the observed HI
flaring beyond a galactocentric distance of 17 kpc up to the last measured
point (~40 kpc). Between 10 and 16 kpc, however, the observed scaleheight is
about 40% more than what MOND predicts for the standard interpolating function
and 70% for the form suggested by Famaey & Binney. Given the uncertainties in
the non-thermal pressure support by cosmic rays and magnetic fields, MOND seems
to be a plausible alternative to dark matter in explaining the Milky Way
flaring. Studying the flaring of extended HI discs in external edge-on galaxies
may be a promising approach to assess the viability of MOND.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:32:38 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Sanchez-Salcedo",
"F. J.",
""
],
[
"Saha",
"K.",
""
],
[
"Narayan",
"C. A.",
""
]
] | [
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] |
712.0817 | Jorge Pullin | Miguel Campiglia, Rodolfo Gambini, Jorge Pullin | Loop quantization of spherically symmetric midi-superspaces : the
interior problem | 12 Pages, to appear in Proceedings of the Third Mexican Meeting on
Mathematical and Experimental Physics, A. Macias, C. Laemmerzahl, A. Camacho,
editors, AIP conference series. Small corrections | AIPConf.Proc.977:52-63,2008 | 10.1063/1.2902798 | LSU-REL-120507 | gr-qc | null | We continue the study of spherically symmetric vacuum space-times in loop
quantum gravity by treating the interior of a black hole. We start from a
midi-superspace approach, but a simple gauge fixing leads to a Kantowski--Sachs
form for the variables. We show that one can solve the quantum theory exactly
in the (periodic) connection representation, including the inner product. The
evolution can be solved exactly by de-parameterizing the theory and can be
easily interpreted as a semi-classical evolution plus quantum corrections. A
relational evolution can also be introduced in a precise manner, suggesting
what may happen in situations where it is not possible to de-parameterize. We
show that the singularity is replaced by a bounce at which quantum effects are
important and that the extent of the region at the bounce where one departs
from classical general relativity depends on the initial data.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:33:28 GMT"
},
{
"version": "v2",
"created": "Thu, 13 Dec 2007 12:40:59 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Campiglia",
"Miguel",
""
],
[
"Gambini",
"Rodolfo",
""
],
[
"Pullin",
"Jorge",
""
]
] | [
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] |
712.0818 | Hema Srinivasan | Sumi Seo and Hema Srinivasan | Multiplicity of Codimension Three Almost Complete Intersections | null | null | null | null | math.AC | null | We establish the upper bound in the multiplicity conjecture of Herzog, Huneke
and Srinivasan for the codimension three almost complete intersections. We also
give some partial results in the case where I is the aci linked to a complete
intersection in one step.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:34:39 GMT"
}
] | 2007-12-06T00:00:00 | [
[
"Seo",
"Sumi",
""
],
[
"Srinivasan",
"Hema",
""
]
] | [
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] |
712.0819 | Michael Hitrik | Michael Hitrik, Karel Pravda-Starov | Spectra and semigroup smoothing for non-elliptic quadratic operators | null | null | null | null | math.SP math.AP | null | We study non-elliptic quadratic differential operators. Quadratic
differential operators are non-selfadjoint operators defined in the Weyl
quantization by complex-valued quadratic symbols. When the real part of their
Weyl symbols is a non-positive quadratic form, we point out the existence of a
particular linear subspace in the phase space, intrinsically associated to the
Weyl symbols, called a singular space, such that when the singular space has a
symplectic structure, the associated heat semigroup is smoothing in every
direction of its symplectic orthogonal complement. When the Weyl symbol of such
an operator is elliptic on the singular space, this space is always symplectic
and we prove that the spectrum of the operator is discrete and can be described
as in the globally elliptic case. We also describe the large time behavior of
contraction semigroups generated by these operators.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:46:10 GMT"
}
] | 2007-12-06T00:00:00 | [
[
"Hitrik",
"Michael",
""
],
[
"Pravda-Starov",
"Karel",
""
]
] | [
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] |
712.082 | Xiaosong Wu | Xiaosong Wu, Mike Sprinkle, Xuebin Li, Fan Ming, Claire Berger, Walt
A. de Heer | The epitaxial-graphene/graphene-oxide junction, an essential step
towards epitaxial graphene electronics | 5 pages, 4 figures | Phys. Rev. Lett. 101, 026801 (2008) | 10.1103/PhysRevLett.101.026801 | null | cond-mat.mes-hall cond-mat.mtrl-sci | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Graphene oxide (GO) flakes have been deposited to bridge the gap between two
epitaxial graphene electrodes to produce all-graphene devices. Electrical
measurements indicate the presence of Schottky barriers (SB) at the
graphene/graphene oxide junctions, as a consequence of the band-gap in GO. The
barrier height is found to be about 0.7 eV, and is reduced after annealing at
180 $^\circ$C, implying that the gap can be tuned by changing the degree of
oxidation. A lower limit of the GO mobility was found to be 850 cm$^2$/Vs,
rivaling silicon. {\it In situ} local oxidation of patterned epitaxial graphene
has been achieved.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 20:40:08 GMT"
},
{
"version": "v2",
"created": "Mon, 7 Jul 2008 15:47:10 GMT"
}
] | 2008-07-07T00:00:00 | [
[
"Wu",
"Xiaosong",
""
],
[
"Sprinkle",
"Mike",
""
],
[
"Li",
"Xuebin",
""
],
[
"Ming",
"Fan",
""
],
[
"Berger",
"Claire",
""
],
[
"de Heer",
"Walt A.",
""
]
] | [
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712.0821 | Marcelo Samuel Berman | Marcelo Samuel Berman | A General Relativistic Rotating Evolutionary Universe | 5 pages including front cover. Published | Astrophys.Space Sci.314:319-321,2008 | 10.1007/s10509-008-9772-0 | null | physics.gen-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We show that when we work with coordinate cosmic time, which is not proper
time, Robertson-Walker's metric, includes a possible rotational state of the
Universe. An exact formula for the angular speed and the temporal metric
coefficient, is found.
| [
{
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"created": "Wed, 5 Dec 2007 20:42:14 GMT"
},
{
"version": "v2",
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] | 2009-01-14T00:00:00 | [
[
"Berman",
"Marcelo Samuel",
""
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712.0822 | Abdelmalek Salem Dr | Abdelmalek Salem and Kouachi Said | Condensation of Determinants | 8 pages | null | null | null | math.CO | null | In this paper we tried to condense the determinant of n square matrix to the
determinant of (n - 1) square matrix with the mathematical proof.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:29:30 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Salem",
"Abdelmalek",
""
],
[
"Said",
"Kouachi",
""
]
] | [
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712.0823 | W. K. M. Rice | W.K.M. Rice, P.J. Armitage, D.F. Hogg | Why are there so few hot Jupiters? | 7 pages, 8 figures, Accepted for publication in MNRAS | null | 10.1111/j.1365-2966.2007.12817.x | null | astro-ph | null | We use numerical simulations to model the migration of massive planets at
small radii and compare the results with the known properties of 'hot Jupiters'
(extrasolar planets with semi-major axes a < 0.1 AU). For planet masses Mp sin
i > 0.5 MJup, the evidence for any `pile-up' at small radii is weak
(statistically insignificant), and although the mass function of hot Jupiters
is deficient in high mass planets as compared to a reference sample located
further out, the small sample size precludes definitive conclusions. We suggest
that these properties are consistent with disc migration followed by entry into
a magnetospheric cavity close to the star. Entry into the cavity results in a
slowing of migration, accompanied by a growth in orbital eccentricity. For
planet masses in excess of 1 Jupiter mass we find eccentricity growth
timescales of a few x 10^5 years, suggesting that these planets may often be
rapidly destroyed. Eccentricity growth appears to be faster for more massive
planets which may explain changes in the planetary mass function at small radii
and may also predict a pile-up of lower mass planets, the sample of which is
still incomplete.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:07:07 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Rice",
"W. K. M.",
""
],
[
"Armitage",
"P. J.",
""
],
[
"Hogg",
"D. F.",
""
]
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] |
712.0824 | Charlie Conroy | Charlie Conroy, Jeremiah P. Ostriker (Princeton) | Thermal Balance in the Intracluster Medium: Is AGN Feedback Necessary? | 16 pages, 8 figures. ApJ in press | null | 10.1086/587861 | null | astro-ph | null | A variety of physical heating mechanisms are combined with radiative cooling
to explore, via one dimensional hydrodynamic simulations, the expected thermal
properties of the intracluster medium (ICM) in the context of the cooling flow
problem. Energy injection from type Ia supernovae, thermal conduction, and
dynamical friction (DF) from orbiting satellite galaxies are considered. The
novel feature of this work is the exploration of a wide range of efficiencies
of each heating process. While the latter two can provide a substantial amount
of energy, neither mechanism operating alone can produce nor maintain an ICM in
thermal balance over cosmological timescales, in stark contrast with
observations. For simulated clusters with initially isothermal temperature
profiles, both mechanisms acting in combination result in long-term thermal
balance for a range of ICM temperatures and for central electron densities less
than n_e~0.02 cm^-3; at greater densities catastrophic cooling invariably
occurs. Furthermore, these heating mechanisms can neither produce nor maintain
clusters with a declining temperature profile in the central regions, implying
that the observed "cooling-core'' clusters, which have such declining
temperature profiles, cannot be maintained with these mechanisms alone. Thus,
while there appears to be an abundant supply of energy capable of heating the
ICM in clusters, it is extremely difficult for the energy deposition to occur
in such a way that the ICM remains in thermal balance over cosmological
time-scales. These results strongly suggest that a more dynamic heating process
such as feedback from a central black hole is required to generate the
properties of observed intracluster media. (ABRIDGED)
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 14:37:20 GMT"
},
{
"version": "v2",
"created": "Mon, 10 Mar 2008 01:00:32 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Conroy",
"Charlie",
"",
"Princeton"
],
[
"Ostriker",
"Jeremiah P.",
"",
"Princeton"
]
] | [
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712.0825 | Tigran Sedrakyan | T. A. Sedrakyan, M. E. Raikh | Interaction effects in 2D electron gas in a random magnetic field:
Implications for composite fermions and quantum critical point | 32 pages, 15 figures, Revtex | Phys. Rev. B 77, 115353 (2008) | 10.1103/PhysRevB.77.115353 | null | cond-mat.mes-hall | null | We consider a clean two-dimensional interacting electron gas subject to a
random perpendicular magnetic field, h({\bf r}). The field is nonquantizing, in
the sense, that {\cal N}_h-a typical flux into the area \lambda_{\text{\tiny
F}}^2 in the units of the flux quantum (\lambda_{\text{\tiny F}} is the de
Broglie wavelength) is small, {\cal N}_h\ll 1. If the spacial scale, \xi, of
change of h({\bf r}) is much larger than \lambda_{\text{\tiny F}}, the
electrons move along semiclassical trajectories. We demonstrate that a weak
field-induced curving of the trajectories affects the interaction-induced
electron lifetime in a singular fashion: it gives rise to the correction to the
lifetime with a very sharp energy dependence. The correction persists within
the interval \omega \sim \omega_0= E_{\text{\tiny F}}{\cal N}_h^{2/3} much
smaller than the Fermi energy, E_{\text{\tiny F}}. It emerges in the third
order in the interaction strength; the underlying physics is that a small phase
volume \sim (\omega/E_{\text{\tiny F}})^{1/2} for scattering processes,
involving {\em two} electron-hole pairs, is suppressed by curving. Even more
surprising effect that we find is that {\em disorder-averaged} interaction
correction to the density of states, \delta\nu(\omega), exhibits {\em
oscillatory} behavior, periodic in \bigl(\omega/\omega_0\bigr)^{3/2}. In our
calculations of interaction corrections random field is incorporated via the
phases of the Green functions in the coordinate space. We discuss the relevance
of the new low-energy scale for realizations of a smooth random field in
composite fermions and in disordered phase of spin-fermion model of
ferromagnetic quantum criticality.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:56:02 GMT"
},
{
"version": "v2",
"created": "Sun, 30 Mar 2008 07:56:29 GMT"
}
] | 2008-03-30T00:00:00 | [
[
"Sedrakyan",
"T. A.",
""
],
[
"Raikh",
"M. E.",
""
]
] | [
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] |
712.0826 | Sergei Zharikov | S.V. Zharikov (1), Yu.A. Shibanov (2), R.E. Mennickent (3), V.N.
Komarova (4) ((1) IA UNAM, Mexico, (2) Ioffe Physical Technical Inst. RAS,
St. Petersburg, Russia, (3) Universidad de Concepcion, Concepcion, Chile, (4)
Special Astrophysical Observatory, RAS, Russia) | Possible optical detection of a fast, nearby radio pulsar PSR B1133+16 | 11 pages, 6 figures, A&A, accepted | null | 10.1051/0004-6361:20077728 | null | astro-ph | null | Aims: We performed deep optical observations of the field of an old,
fast-moving radio pulsar PSR B1133+16 in an attempt to detect its optical
counterpart and a bow shock nebula.
Methods: The observations were carried out using the direct imaging mode of
FORS1 at the ESO VLT/UT1 telescope in the B, R, and H_alpha bands. We also
used archival images of the same field obtained with the VLT in the B band and
with the Chandra/ACIS in X-rays.
Results: In the B band we detected a faint (B=28.1+/-0.3) source that may be
the optical counterpart of PSR B1133+16, as it is positionally consistent with
the radio pulsar and with the X-ray counterpart candidate published earlier.
Its upper limit in the R band implies a color index B-R <0.5, which is
compatible with the index values for most pulsars identified in the optical
range. The derived optical luminosity and its ratio to the X-ray luminosity of
the candidate are consistent with expected values derived from a sample of
pulsars detected in both spectral domains. No Balmer bow shock was detected,
implying a low density of ambient matter around the pulsar. However, in the
X-ray and H_alpha images we found the signature of a trail extending ~4"-5"
behind the pulsar and coinciding with the direction of its proper motion. If
confirmed by deeper studies, this is the first time such a trail has been seen
in the optical and X-ray wavelengths.
Conclusions: Further observations at later epochs are necessary to confirm
the identification of the pulsar by the candidate's proper motion measurements.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:07:06 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Zharikov",
"S. V.",
""
],
[
"Shibanov",
"Yu. A.",
""
],
[
"Mennickent",
"R. E.",
""
],
[
"Komarova",
"V. N.",
""
]
] | [
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] |
712.0827 | Michael Munn | Michael Munn | Volume growth and the topology of manifolds with nonnegative Ricci
curvature | v3 is based on the earlier v1. The current version simplifies the
argument of Lemma 2.4 and corrects some minor typos. We also include further
discussion describing the main ideas behind Lemma 3.4 and Lemma 3.5. This
article was accepted for publication and will appear in the Journal of
Geometric Analysis | null | null | null | math.DG | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Let $M^n$ be a complete, open Riemannian manifold with $\Ric \geq 0$. In
1994, Grigori Perelman showed that there exists a constant $\delta_{n}>0$,
depending only on the dimension of the manifold, such that if the volume growth
satisfies $\alpha_M := \lim_{r \to \infty} \frac{\Vol(B_p(r))}{\omega_n r^n}
\geq 1-\delta_{n}$, then $M^n$ is contractible. Here we employ the techniques
of Perelman to find specific lower bounds for the volume growth, $\alpha(k,n)$,
depending only on $k$ and $n$, which guarantee the individual $k$-homotopy
group of $M^n$ is trivial.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:16:17 GMT"
},
{
"version": "v2",
"created": "Thu, 19 Jun 2008 16:17:58 GMT"
},
{
"version": "v3",
"created": "Thu, 17 Dec 2009 16:52:14 GMT"
}
] | 2009-12-17T00:00:00 | [
[
"Munn",
"Michael",
""
]
] | [
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] |
712.0828 | Mark R. Krumholz | Mark R. Krumholz (1) and Ian A. Bonnell (2) ((1) Princeton University,
(2) University of St. Andrews) | Models for the Formation of Massive Stars | 25 pages, 4 figures, CUP press format. To be published in "Structure
Formation in the Universe", ed. G. Chabrier. This version is has a slightly
revised discussion of massive binaries | null | null | null | astro-ph | null | The formation of massive stars is currently an unsolved problems in
astrophysics. Understanding the formation of massive stars is essential because
they dominate the luminous, kinematic, and chemical output of stars.
Furthermore, their feedback is likely to play a dominant role in the evolution
of molecular clouds and any subsequent star formation therein. Although
significant progress has been made observationally and theoretically, we still
do not have a consensus as to how massive stars form. There are two contending
models to explain the formation of massive stars, Core Accretion and
Competitive Accretion. They differ primarily in how and when the mass that
ultimately makes up the massive star is gathered. In the core accretion model,
the mass is gathered in a prestellar stage due to the overlying pressure of a
stellar cluster or a massive pre-cluster cloud clump. In contrast, competitive
accretion envisions that the mass is gathered during the star formation process
itself, being funneled to the centre of a stellar cluster by the gravitational
potential of the stellar cluster. Although these differences may not appear
overly significant, they involve significant differences in terms of the
physical processes involved. Furthermore, the differences also have important
implications in terms of the evolutionary phases of massive star formation, and
ultimately that of stellar clusters and star formation on larger scales. Here
we review the dominant models, and discuss prospects for developing a better
understanding of massive star formation in the future.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:18:04 GMT"
},
{
"version": "v2",
"created": "Mon, 17 Dec 2007 16:27:54 GMT"
}
] | 2007-12-17T00:00:00 | [
[
"Krumholz",
"Mark R.",
""
],
[
"Bonnell",
"Ian A.",
""
]
] | [
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] |
712.0829 | Aditi Sen De | Aditi Sen De, Ujjwal Sen, Jan Wehr, Maciej Lewenstein | Classical Spin Models with Broken Continuous Symmetry: Random Field
Induced Order and Persistence of Spontaneous Magnetization | 12 pages, 12 figures, RevTeX4 | Phys. Rev. B 90, 174408 (2014) | 10.1103/PhysRevB.90.174408 | null | cond-mat.other cond-mat.dis-nn | null | We consider a classical spin model, of two-dimensional spins, with continuous
symmetry, and investigate the effect of a symmetry breaking unidirectional
quenched disorder on the magnetization of the system. We work in the mean field
regime. We show, by numerical simulations and by perturbative calculations in
the low as well as in the high temperature limits, that although the continuous
symmetry of the magnetization is lost, the system still magnetizes, albeit with
a lower value as compared to the case without disorder. The critical
temperature at which the system starts magnetizing, also decreases with the
introduction of disorder. However, with the introduction of an additional
constant magnetic field, the component of magnetization in the direction that
is transverse to the disorder field increases with the introduction of the
quenched disorder. We discuss the same effects also for three-dimensional
spins.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:41:20 GMT"
}
] | 2014-11-19T00:00:00 | [
[
"De",
"Aditi Sen",
""
],
[
"Sen",
"Ujjwal",
""
],
[
"Wehr",
"Jan",
""
],
[
"Lewenstein",
"Maciej",
""
]
] | [
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] |
712.083 | Paolo Berra Dr. | Paolo Berra | Design, construction and tests of a 3 GHz proton linac booster (LIBO)
for cancer therapy | PhD Thesis, Lyon University, UCBL and TERA 2005, Published by ANRT
Granoble 2006, CDS CERN-THESIS-2007-054 and CERN EDMS-2006 at
https://edms.cern.ch/document/787414/2 | null | null | UCBL N d'ordre: 163-2005 | physics.acc-ph physics.med-ph | null | In the last ten years the use of proton beams in radiation therapy has become
a clinical tool for treatment of deep-seated tumours. LIBO is a RF compact and
low cost proton linear accelerator (SCL type) for hadrontherapy. It is
conceived by TERA Foundation as a 3 GHz Linac Booster, to be mounted downstream
of an existing cyclotron in order to boost the energy of the proton beam up to
200 MeV, needed for deep treatment (~25 cm) in the human body. With this
solution it is possible to transform a low energy commercial cyclotron,
normally used for eye melanoma therapy, isotope production and nuclear physics
research, into an accelerator for deep-seated tumours. A prototype module of
LIBO has been built and successfully tested with full RF power at CERN and with
proton beam at INFN Laboratori Nazionali del Sud (LNS) in Catania, within an
international collaboration between TERA Foundation, CERN, the Universities and
INFN groups of Milan and Naples. The mid-term aim of the project is the
technology transfer of the accumulated know-how to a consortium of companies
and to bring this novel medical tool to hospitals. The design, construction and
tests of the LIBO prototype are described in detail.
| [
{
"version": "v1",
"created": "Sun, 2 Dec 2007 14:52:16 GMT"
}
] | 2009-09-29T00:00:00 | [
[
"Berra",
"Paolo",
""
]
] | [
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712.0831 | Asle Sudbo | Jacob Linder and Asle Sudb\o | Tunneling conductance in $s$- and d-wave superconductor-graphene
junctions: Extended Blonder-Tinkham-Klapwijk formalism | 14 pages, 16 figures. High-resolution figures available in the
published version | Phys. Rev. B 77, 064507 (2008) | 10.1103/PhysRevB.77.064507 | null | cond-mat.supr-con | null | We investigate the conductance spectra of a normal/superconductor graphene
junction using the extended Blonder-Tinkham-Klapwijk formalism, considering
pairing potentials that are both conventional (isotropic s-wave) and
unconventional (anisotropic d-wave). In particular, we study the full crossover
from normal to specular Andreev reflection without restricting ourselves to
special limits and approximations, thus expanding results obtained in previous
work. In addition, we investigate in detail how the conductance spectra are
affected if it is possible to induce an unconventional pairing symmetry in
graphene, for instance a d-wave order parameter. We also discuss the recently
reported conductance-oscillations that take place in normal/superconductor
graphene junctions, providing both analytical and numerical results.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:55:11 GMT"
},
{
"version": "v2",
"created": "Mon, 18 Feb 2008 07:59:06 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Linder",
"Jacob",
""
],
[
"Sudbø",
"Asle",
""
]
] | [
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0.0978927836,
-0.0412510261,
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] |
712.0832 | Junfang Li | Junfang Li | First variation of the Log Entropy functional along the Ricci flow | 4 pages. One remark improved | null | null | null | math.DG math.AP | null | In this note, we establish the first variation formula of the adjusted log
entropy functional $\mathcal Y_a$ introduced by Ye in \cite{Y2}. As a direct
consequence, we also obtain the monotonicity of $\mathcal Y_a$ along the Ricci
flow.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:49:26 GMT"
},
{
"version": "v2",
"created": "Fri, 7 Dec 2007 20:57:37 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Li",
"Junfang",
""
]
] | [
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] |
712.0833 | William Heinzer | William J. Heinzer, Louis J. Ratliff Jr and David E. Rush | Projective equivalence of ideals in Noetherian integral domains | 20 pages | null | null | null | math.AC | null | Let I be a nonzero proper ideal in a Noetherian integral domain R. In this
paper we establish the existence of a finite separable integral extension
domain A of R and a positive integer m such that all the Rees integers of IA
are equal to m. Moreover, if R has altitude one, then all the Rees integers of
J = Rad(IA) are equal to one and the ideals J^m and IA have the same integral
closure. Thus Rad(IA) = J is a projectively full radical ideal that is
projectively equivalent to IA. In particular, if R is Dedekind, then there
exists a Dedekind domain A having the following properties: (i) A is a finite
separable integral extension of R; and (ii) there exists a radical ideal J of A
and a positive integer m such that IA = J^m.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 21:59:10 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Heinzer",
"William J.",
""
],
[
"Ratliff",
"Louis J.",
"Jr"
],
[
"Rush",
"David E.",
""
]
] | [
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] |
712.0834 | Angela Zalucha | A. Zalucha, A. Fitzsimmons, J. L. Elliot, J. Thomas-Osip, H. B.
Hammel, V. S. Dhillon, T. R. Marsh, F. W. Taylor, P. G. J. Irwin | The 2003 Nov 14 occultation by Titan of TYC 1343-1865-1. II. Analysis of
light curves | 58 pages, 14 figures, 5 tables, accepted to Icarus | Icarus192:503-518,2007 | 10.1016/j.icarus.2007.08.008 | null | astro-ph | null | We observed a stellar occultation by Titan on 2003 November 14 from La Palma
Observatory using ULTRACAM with three Sloan filters: u', g', and i' (358, 487,
and 758 nm, respectively). The occultation probed latitudes 2 degrees S and 1
degrees N during immersion and emersion, respectively. A prominent central
flash was present in only the i' filter, indicating wavelength-dependent
atmospheric extinction. We inverted the light curves to obtain six lower-limit
temperature profiles between 335 and 485 km (0.04 and 0.003 mb) altitude. The
i' profiles agreed with the temperature measured by the Huygens Atmospheric
Structure Instrument [Fulchignoni, M. et al., 2005. Nature 438, 785-791] above
415 km (0.01 mb). The profiles obtained from different wavelength filters
systematically diverge as altitude decreases, which implies significant
extinction in the light curves. Applying an extinction model [Elliot, J.L.,
Young, L.A., 1992. Astron. J. 103, 991-1015] gave the altitudes of line of
sight optical depth equal to unity: 396 +/- 7 km and 401 +/- 20 km (u'
immersion and emersion); 354 +/- 7 km and 387 +/- 7 km (g' immersion and
emersion); and 336 +/- 5 km and 318 +/- 4 km (i' immersion and emersion).
Further analysis showed that the optical depth follows a power law in
wavelength with index 1.3 +/- 0.2. We present a new method for determining
temperature from scintillation spikes in the occulting body's atmosphere.
Temperatures derived with this method are equal to or warmer than those
measured by the Huygens Atmospheric Structure Instrument. Using the highly
structured, three-peaked central flash, we confirmed the shape of Titan's
middle atmosphere using a model originally derived for a previous Titan
occultation [Hubbard, W.B. et al., 1993. Astron. Astrophys. 269, 541-563].
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:00:38 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Zalucha",
"A.",
""
],
[
"Fitzsimmons",
"A.",
""
],
[
"Elliot",
"J. L.",
""
],
[
"Thomas-Osip",
"J.",
""
],
[
"Hammel",
"H. B.",
""
],
[
"Dhillon",
"V. S.",
""
],
[
"Marsh",
"T. R.",
""
],
[
"Taylor",
"F. W.",
""
],
[
"Irwin",
"P. G. J.",
""
]
] | [
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] |
712.0835 | Alexey Kuzmenko | A. B. Kuzmenko, E. van Heumen, F. Carbone, D. van der Marel | Universal dynamical conductance in graphite | 4 pages, 4 figures | Phys. Rev. Lett. 100, 117401 (2008) | 10.1103/PhysRevLett.100.117401 | null | cond-mat.str-el | null | We find experimentally that the optical sheet conductance of graphite per
graphene layer is very close to $(\pi/2)e^2/h$, which is the theoretically
expected value of dynamical conductance of isolated monolayer graphene. Our
calculations within the Slonczewski-McClure-Weiss model explain well why the
interplane hopping leaves the conductance of graphene sheets in graphite almost
unchanged for photon energies between 0.1 and 0.6 eV, even though it
significantly affects the band structure on the same energy scale. The f-sum
rule analysis shows that the large increase of the Drude spectral weight as a
function of temperature is at the expense of the removed low-energy optical
spectral weight of transitions between hole and electron bands.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:03:52 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Kuzmenko",
"A. B.",
""
],
[
"van Heumen",
"E.",
""
],
[
"Carbone",
"F.",
""
],
[
"van der Marel",
"D.",
""
]
] | [
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] |
712.0836 | Andrew Adamatzky | Andrew Adamatzky, Larry Bull, Pierre Collet, Emmanuel Sapin | Evolving localizations in reaction-diffusion cellular automata | Accepted for publication in Int. J. Modern Physics C | International Journal of Modern Physics C (IJMPC) Volume: 19,
Issue: 4 (April 2008) pp. 557-567 | 10.1142/S0129183108012376 | null | cs.AI | null | We consider hexagonal cellular automata with immediate cell neighbourhood and
three cell-states. Every cell calculates its next state depending on the
integral representation of states in its neighbourhood, i.e. how many
neighbours are in each one state. We employ evolutionary algorithms to breed
local transition functions that support mobile localizations (gliders), and
characterize sets of the functions selected in terms of quasi-chemical systems.
Analysis of the set of functions evolved allows to speculate that mobile
localizations are likely to emerge in the quasi-chemical systems with limited
diffusion of one reagent, a small number of molecules is required for
amplification of travelling localizations, and reactions leading to stationary
localizations involve relatively equal amount of quasi-chemical species.
Techniques developed can be applied in cascading signals in nature-inspired
spatially extended computing devices, and phenomenological studies and
classification of non-linear discrete systems.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:07:04 GMT"
}
] | 2010-11-23T00:00:00 | [
[
"Adamatzky",
"Andrew",
""
],
[
"Bull",
"Larry",
""
],
[
"Collet",
"Pierre",
""
],
[
"Sapin",
"Emmanuel",
""
]
] | [
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] |
712.0837 | Peter Sin | Peter Sin and John G. Thompson | The Divisor Matrix, Dirichlet Series and SL(2,Z) | 29 pages. The current version V4 is the combination of two papers,
previously called parts I and II, with the same title. Part II had been
posted as arXiv:0803.1121v5. Some additional remarks added in section 10. V6.
Minor errors corrected | The legacy of Alladi Ramakrishnan in the mathematical sciences (K.
Alladi, J. Klauder, C. R. Rao, Eds.), Developments in Mathematics, Springer
(2010) | null | null | math.NT math.GR | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | A representation of SL(2,Z) by integer matrices acting on the space of
analytic ordinary Dirichlet series is constructed, in which the standard
unipotent element acts as multiplication by the Riemann zeta function. It is
then shown that the Dirichlet series in the orbit of the zeta function are
related to it by algebraic equations.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:10:09 GMT"
},
{
"version": "v2",
"created": "Tue, 25 Dec 2007 18:27:48 GMT"
},
{
"version": "v3",
"created": "Wed, 9 Apr 2008 04:57:56 GMT"
},
{
"version": "v4",
"created": "Tue, 10 Jun 2008 19:24:59 GMT"
},
{
"version": "v5",
"created": "Thu, 17 Jul 2008 14:41:03 GMT"
},
{
"version": "v6",
"created": "Fri, 18 Jul 2008 21:34:06 GMT"
}
] | 2020-01-30T00:00:00 | [
[
"Sin",
"Peter",
""
],
[
"Thompson",
"John G.",
""
]
] | [
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] |
712.0838 | Mohammad H. S. Amin | R. Harris, M.W. Johnson, S. Han, A.J. Berkley, J. Johansson, P. Bunyk,
E. Ladizinsky, S. Govorkov, M.C. Thom, S. Uchaikin, B. Bumble, A. Fung, A.
Kaul, A. Kleinsasser, M.H.S. Amin, D.V. Averin | Probing Noise in Flux Qubits via Macroscopic Resonant Tunneling | 4 pages 4 figures | Phys. Rev. Lett. 101, 117003 (2008) | 10.1103/PhysRevLett.101.117003 | null | cond-mat.mes-hall cond-mat.supr-con | null | Macroscopic resonant tunneling between the two lowest lying states of a
bistable RF-SQUID is used to characterize noise in a flux qubit. Measurements
of the incoherent decay rate as a function of flux bias revealed a Gaussian
shaped profile that is not peaked at the resonance point, but is shifted to a
bias at which the initial well is higher than the target well. The r.m.s.
amplitude of the noise, which is proportional to the decoherence rate 1/T_2^*,
was observed to be weakly dependent on temperature below 70 mK. Analysis of
these results indicates that the dominant source of low frequency (1/f) flux
noise in this device is a quantum mechanical environment in thermal
equilibrium.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 01:06:18 GMT"
},
{
"version": "v2",
"created": "Fri, 8 Feb 2008 23:10:07 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Harris",
"R.",
""
],
[
"Johnson",
"M. W.",
""
],
[
"Han",
"S.",
""
],
[
"Berkley",
"A. J.",
""
],
[
"Johansson",
"J.",
""
],
[
"Bunyk",
"P.",
""
],
[
"Ladizinsky",
"E.",
""
],
[
"Govorkov",
"S.",
""
],
[
"Thom",
"M. C.",
""
],
[
"Uchaikin",
"S.",
""
],
[
"Bumble",
"B.",
""
],
[
"Fung",
"A.",
""
],
[
"Kaul",
"A.",
""
],
[
"Kleinsasser",
"A.",
""
],
[
"Amin",
"M. H. S.",
""
],
[
"Averin",
"D. V.",
""
]
] | [
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] |
712.0839 | Jonathan Devor | Jonathan Devor, David Charbonneau, Francis T. O'Donovan, Georgi
Mandushev and Guillermo Torres | Identification, Classifications, and Absolute Properties of 773
Eclipsing Binaries Found in the TrES Survey | 64 pages, 23 figures, accepted for publication in AJ, see
http://www.cfa.harvard.edu/~jdevor/Catalog.html for the catalog | null | 10.1088/0004-6256/135/3/850 | null | astro-ph | null | In recent years we have witnessed an explosion of photometric time-series
data, collected for the purpose of finding a small number of rare sources, such
as transiting extrasolar planets and gravitational microlenses. Once combed,
these data are often set aside, and are not further searched for the many other
variable sources that they undoubtedly contain. To this end, we describe a
pipeline that is designed to systematically analyze such data, while requiring
minimal user interaction. We ran our pipeline on a subset of the Trans-Atlantic
Exoplanet Survey dataset, and used it to identify and model 773 eclipsing
binary systems. For each system we conducted a joint analysis of its light
curve, colors, and theoretical isochrones. This analysis provided us with
estimates of the binary's absolute physical properties, including the masses
and ages of their stellar components, as well as their physical separations and
distances. We identified three types of eclipsing binaries that are of
particular interest and merit further observations. The first category includes
11 low-mass candidates, which may assist current efforts to explain the
discrepancies between the observation and the models of stars at the bottom of
the main-sequence. The other two categories include 34 binaries with eccentric
orbits, and 20 binaries with abnormal light curves. Finally, this uniform
catalog enabled us to identify a number of relations that provide further
constraints on binary population models and tidal circularization theory.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 02:28:25 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Devor",
"Jonathan",
""
],
[
"Charbonneau",
"David",
""
],
[
"O'Donovan",
"Francis T.",
""
],
[
"Mandushev",
"Georgi",
""
],
[
"Torres",
"Guillermo",
""
]
] | [
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] |
712.084 | Leonid (Aryeh) Kontorovich | Leonid (Aryeh) Kontorovich | A Universal Kernel for Learning Regular Languages | 7 pages | The 5th International Workshop on Mining and Learning with Graphs,
2007 | null | null | cs.LG cs.DM | null | We give a universal kernel that renders all the regular languages linearly
separable. We are not able to compute this kernel efficiently and conjecture
that it is intractable, but we do have an efficient $\eps$-approximation.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:25:03 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Leonid",
"",
"",
"Aryeh"
],
[
"Kontorovich",
"",
""
]
] | [
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] |
712.0841 | Gondran Michel | Michel Gondran, Alexandre Gondran | Numerical Simulation of the Double Slit Interference with Ultracold
Atoms | 25 pages, 15 figures | Am. J. Phys. 73, 2005 | null | null | quant-ph | null | We present a numerical simulation of the double slit interference experiment
realized by F. Shimizu, K. Shimizu and H. Takuma with ultracold atoms. We show
how the Feynman path integral method enables the calculation of the
time-dependent wave function. Because the evolution of the probability density
of the wave packet just after it exits the slits raises the issue of the
interpreting the wave/particle dualism, we also simulate trajectories in the de
Broglie-Bohm interpretation.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:29:01 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Gondran",
"Michel",
""
],
[
"Gondran",
"Alexandre",
""
]
] | [
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] |
712.0842 | Bernardo Cervantes-Sodi | B. Cervantes-Sodi, X. Hernandez, Changbom Park and Juhan Kim | Environment and mass dependencies of galactic $\lambda$ spin parameter:
cosmological simulations and observed galaxies compared | 11 pages, 5 figures. Matches MNRAS published version | 2008, MNRAS, 388, 863 | 10.1111/j.1365-2966.2008.13449.x | null | astro-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We use a sample of galaxies from the Sloan Digital Sky Survey (SDSS) to
search for correlations between the $\lambda$ spin parameter and the
environment and mass of galaxies. In order to calculate the total value of
$\lambda$ for each observed galaxy, we employed a simple model of the dynamical
structure of the galaxies, which allows a rough estimate of the value of
$\lambda$ using only readily obtainable observables from the luminous galaxies.
Use of a large volume-limited sample (upwards of 11,000) allows reliable
inferences of mean values and dispersions of $\lambda$ distributions. We find,
in agreement with some N-body cosmological simulations, no significant
dependence of $\lambda$ on the environmental density of the galaxies. For the
case of mass, our results show a marked correlation with $\lambda$, in the
sense that low-mass galaxies present both higher mean values of $\lambda$ and
associated dispersions, than high-mass galaxies. These results provide
interesting constrain on the mechanisms of galaxy formation and acquisition of
angular momentum, a valuable test for cosmological models.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:32:23 GMT"
},
{
"version": "v2",
"created": "Tue, 13 May 2008 17:27:31 GMT"
},
{
"version": "v3",
"created": "Mon, 28 Jul 2008 17:06:27 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Cervantes-Sodi",
"B.",
""
],
[
"Hernandez",
"X.",
""
],
[
"Park",
"Changbom",
""
],
[
"Kim",
"Juhan",
""
]
] | [
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] |
712.0843 | Adam Sorini | A. P. Sorini and J. J. Rehr and Z. H. Levine | The Magic Angle "Mystery" in Electron Energy Loss Spectroscopy:
Relativistic and Dielectric Corrections | 10 pages (double column), 6 figures | null | 10.1103/PhysRevB.77.115126 | null | cond-mat.mtrl-sci | null | Recently it has been demonstrated that a careful treatment of both
longitudinal and transverse matrix elements in electron energy loss spectra can
explain the mystery of relativistic effects on the {\it magic angle}. Here we
show that there is an additional correction of order $(Z\alpha)^2$ where $Z$ is
the atomic number and $\alpha$ the fine structure constant, which is not
necessarily small for heavy elements. Moreover, we suggest that macroscopic
electrodynamic effects can give further corrections which can break the
sample-independence of the magic angle.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 22:39:51 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Sorini",
"A. P.",
""
],
[
"Rehr",
"J. J.",
""
],
[
"Levine",
"Z. H.",
""
]
] | [
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712.0844 | A. B. Dieker | A. B. Dieker and J. Moriarty | Reflected Brownian motion in a wedge: sum-of-exponential stationary
densities | null | Electronic Communications in Probability, 14, p. 1-16, 2009 | null | null | math.PR | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We give necessary and sufficient conditions for the stationary density of
semimartingale reflected Brownian motion in a wedge to be written as a finite
sum of terms of exponential product form. Relying on geometric ideas
reminiscent of the reflection principle, we give an explicit formula for the
density in such cases.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 23:05:34 GMT"
},
{
"version": "v2",
"created": "Mon, 22 Dec 2008 14:16:16 GMT"
}
] | 2011-07-18T00:00:00 | [
[
"Dieker",
"A. B.",
""
],
[
"Moriarty",
"J.",
""
]
] | [
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712.0845 | Dmitri Averin V. | M.H.S. Amin and Dmitri V. Averin | Macroscopic Resonant Tunneling in the Presence of Low Frequency Noise | 4 pages, 1 figure | Phys. Rev. Lett. 100, 197001 (2008) | 10.1103/PhysRevLett.100.197001 | null | cond-mat.mes-hall cond-mat.supr-con | null | We develop a theory of macroscopic resonant tunneling of flux in a
double-well potential in the presence of realistic flux noise with significant
low-frequency component. The rate of incoherent flux tunneling between the
wells exhibits resonant peaks, the shape and position of which reflect
qualitative features of the noise, and can thus serve as a diagnostic tool for
studying the low-frequency flux noise in SQUID qubits. We show, in particular,
that the noise-induced renormalization of the first resonant peak provides
direct information on the temperature of the noise source and the strength of
its quantum component.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 23:25:04 GMT"
},
{
"version": "v2",
"created": "Tue, 13 May 2008 20:02:32 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Amin",
"M. H. S.",
""
],
[
"Averin",
"Dmitri V.",
""
]
] | [
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] |
712.0846 | Kai Miller | Kai J. Miller, Larry B. Sorensen, Jeffrey G. Ojemann, Marcel den Nijs | ECoG observations of power-law scaling in the human cortex | 4 pages, 4 figures | null | null | null | q-bio.NC cond-mat.other | null | We report the results of our search for power-law electrical signals in the
human brain, using subdural electrocorticographic recordings from the surface
of the cortex. The power spectral density (PSD) of these signals has the
power-law form $ P(f)\sim f^{-\chi} $ from 80 to 500 Hz. This scaling index
$\chi = 4.0\pm 0.1$ is universal, across subjects, area in the cortex, and
local neural activity levels. The shape of the PSD does not change with local
cortex activity, only its amplitude increases. We observe a knee in the spectra
at $f_0\simeq 70$ Hz, implying the existence of a characteristic time scale
$\tau=(2\pi f_0)^{-1}\simeq 2-4$ msec. For $f<f_0$ we find evidence for a
power-law with $\chi_L\simeq 2.0\pm 0.4$.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 23:04:04 GMT"
}
] | 2007-12-11T00:00:00 | [
[
"Miller",
"Kai J.",
""
],
[
"Sorensen",
"Larry B.",
""
],
[
"Ojemann",
"Jeffrey G.",
""
],
[
"Nijs",
"Marcel den",
""
]
] | [
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712.0847 | Ashley Ruiter | Ashley J. Ruiter (1,2), Krzysztof Belczynski (3,1), Matthew
Benacquista (4), and Kelly Holley-Bockelmann (5) ((1) NMSU, (2) CfA, (3)
LANL, (4) CGWA at UTB, (5) Vanderbilt) | The Contribution of Halo White Dwarf Binaries to the LISA Signal | 8 pages, 3 figures, ApJ submitted | null | null | LA-UR-07-7963 | astro-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | Galactic double white dwarfs were postulated as a source of confusion limited
noise for LISA, the future space-based gravitational wave observatory. Until
very recently, the Galactic population consisted of a relatively well studied
disk population, a somewhat studied smaller bulge population and a mostly
unknown, but potentially large halo population. It has been argued that the
halo population may produce a signal that is much stronger (factor of ~5 in
spectral amplitude) than the disk population. However, this surprising result
was not based on an actual calculation of a halo white dwarf population but was
derived on (i) the assumption that one can extrapolate the halo population
properties from those of the disk population and (ii) the postulated
(unrealistically) high number of white dwarfs in the halo. We perform the first
calculation of a halo white dwarf population using population synthesis models.
Our comparison with the signal arising from double white dwarfs in the Galactic
disk+bulge clearly shows that it is impossible for the double white dwarf halo
signal to exceed that of the rest of the Galaxy. Using microlensing results to
give an upper limit on the content of white dwarfs in the halo (~30 % baryonic
mass in white dwarfs), our predicted halo signal is a factor of 10 lower than
the disk+bulge signal. Even in the implausible case where all of the baryonic
halo mass is found in white dwarfs, the halo signal does not become comparable
to that of the disk+bulge, and thus would still have a negligible effect on the
detection of other LISA sources.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 23:13:06 GMT"
},
{
"version": "v2",
"created": "Wed, 15 Oct 2008 23:39:44 GMT"
}
] | 2008-10-16T00:00:00 | [
[
"Ruiter",
"Ashley J.",
""
],
[
"Belczynski",
"Krzysztof",
""
],
[
"Benacquista",
"Matthew",
""
],
[
"Holley-Bockelmann",
"Kelly",
""
]
] | [
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712.0848 | Ashkan Nikeghbali | Paul Bourgade, Ashkan Nikeghbali and Alain Rouault | Ewens measures on compact groups and hypergeometric kernels | New version of the previous paper "Hua-Pickrell measures on general
compact groups". The article has been completely re-written (the presentation
has changed and some proofs have been simplified). New references added. | null | null | null | math.PR math-ph math.MP | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | On unitary compact groups the decomposition of a generic element into product
of reflections induces a decomposition of the characteristic polynomial into a
product of factors. When the group is equipped with the Haar probability
measure, these factors become independent random variables with explicit
distributions. Beyond the known results on the orthogonal and unitary groups
(O(n) and U(n)), we treat the symplectic case. In U(n), this induces a family
of probability changes analogous to the biassing in the Ewens sampling formula
known for the symmetric group. Then we study the spectral properties of these
measures, connected to the pure Fisher-Hartvig symbol on the unit circle. The
associated orthogonal polynomials give rise, as $n$ tends to infinity to a
limit kernel at the singularity.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 23:17:56 GMT"
},
{
"version": "v2",
"created": "Wed, 24 Mar 2010 09:52:26 GMT"
}
] | 2010-03-25T00:00:00 | [
[
"Bourgade",
"Paul",
""
],
[
"Nikeghbali",
"Ashkan",
""
],
[
"Rouault",
"Alain",
""
]
] | [
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712.0849 | Percy Deift | Percy Deift | Some open problems in random matrix theory and the theory of integrable
systems | null | null | null | null | math-ph math.MP | null | We describe a list of open problems in random matrix theory and integrable
systems which was presented at the conference ``Integrable Systems, Random
Matrices, and Applications'' at the Courant Institute in May 2006.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 19:26:32 GMT"
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] | 2007-12-07T00:00:00 | [
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712.085 | Sergey Cherkis | Sergey A. Cherkis and Brian Durcan | Singular Monopoles via the Nahm Transform | 10 pages, LaTeX | JHEP0804:070,2008 | 10.1088/1126-6708/2008/04/070 | TCDMATH 07-23, HMI 07-10 | hep-th | null | We present explicit expressions for the fields of a charge one BPS monopole
with two Dirac singularities. These are solutions of the nonlinear Bogomolny
equations with the gauge group U(2) or SO(3). We derive these expressions by
applying the technique of the Nahm transform. By exploring various limits we
find a number of other solutions.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 23:37:26 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Cherkis",
"Sergey A.",
""
],
[
"Durcan",
"Brian",
""
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712.0851 | Amnon Harel | D0 Collaboration: V.M. Abazov, et al | First measurement of the forward-backward charge asymmetry in top quark
pair production | 8 pages, 4 figures (5 .eps files), submitted to Phys. Rev. Lett | Phys.Rev.Lett.100:142002,2008 | 10.1103/PhysRevLett.100.142002 | FERMILAB-PUB-07-645-E | hep-ex | null | We present the first measurement of the integrated forward-backward charge
asymmetry in top-antitop quark pair (ttbar) production in proton-antiproton
collisions in the lepton plus jets final state. Using a b-jet tagging algorithm
and kinematic reconstruction assuming ttbar+X production and decay, a sample of
0.9fb-1 of data, collected by the D0 experiment at the Fermilab Tevatron
Collider, is used to measure the asymmetry for different jet multiplicities.
The result is also used to set upper limits on ttbar+X production via a Z'
resonance.
| [
{
"version": "v1",
"created": "Wed, 5 Dec 2007 23:45:34 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"D0 Collaboration",
"",
""
],
[
"Abazov",
"V. M.",
""
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] |
712.0852 | Chun Hay Kom | B. C. Allanach, C. H. Kom | Lepton number violating mSUGRA and neutrino masses | 36 pages, 7 figures. References updated. A factor of 2 typo in
eq.(2.19) is removed. All numerical results remain unchanged | JHEP 0804:081,2008 | 10.1088/1126-6708/2008/04/081 | DAMTP-2007-106 | hep-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We perform a quantitative study of neutrino phenomenology in the framework of
minimal supergravity (mSUGRA) with grand unified theory (GUT)-scale tri-linear
lepton number violation. We show that only two non-zero GUT scale lepton number
violating parameters and three charged lepton mixing angles are sufficient to
account for current neutrino oscillation data. This allows collider studies to
be performed in a manageable parameter space. We discuss some phenomenological
consequences of the models, including tuning issues.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 00:12:28 GMT"
},
{
"version": "v2",
"created": "Thu, 24 Jan 2008 15:19:04 GMT"
},
{
"version": "v3",
"created": "Wed, 12 Mar 2008 16:31:27 GMT"
},
{
"version": "v4",
"created": "Wed, 16 Sep 2009 21:26:44 GMT"
}
] | 2009-09-17T00:00:00 | [
[
"Allanach",
"B. C.",
""
],
[
"Kom",
"C. H.",
""
]
] | [
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] |
712.0853 | Kaitlin Kratter | Kaitlin M. Kratter (1), Christopher D. Matzner (1), Mark. R. Krumholz
(2) ((1) Univ. Toronto (2) Princeton University) | Embedded, Accreting Disks in Massive Star Formation | 8 pages, 3 figures, to appear in ASP conference proceedings of
"Massive Star Formation: Observations Confront Theory", Heidelberg 2007, ed.
H. Beuther | null | null | null | astro-ph | null | Recent advances in our understanding of massive star formation have made
clear the important role of protostellar disks in mediating accretion. Here we
describe a simple, semi-analytic model for young, deeply embedded, massive
accretion disks. Our approach enables us to sample a wide parameter space of
stellar mass and environmental variables, providing a means to make predictions
for a variety of sources that next generation telescopes like ALMA and the EVLA
will observe. Moreover we include, at least approximately, multiple mechanisms
for angular momentum transport, a comprehensive model for disk heating and
cooling, and a realistic estimate for the angular momentum in the gas
reservoir. We make predictions for the typical sizes, masses, and temperatures
of the disks, and describe the role of gravitational instabilities in
determining the binarity fraction and upper mass cut-off.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 20:10:23 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Kratter",
"Kaitlin M.",
"",
"Univ. Toronto"
],
[
"Matzner",
"Christopher D.",
"",
"Univ. Toronto"
],
[
"Krumholz",
"Mark. R.",
"",
"Princeton University"
]
] | [
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] |
712.0854 | Yin-Zhong Wu | Yin-Zhong Wu and Yong-Mei Tao | Simulations on the electromechanical poling of ferroelectric ceramics | 11 pages, 2 figures | Journal of Applied Physics 102, 114104(2007) | 10.1063/1.2817624 | null | cond-mat.mtrl-sci cond-mat.soft | null | Based on the two-step-switching model, the process of electromechanical
poling of a ferroelectric ceramics is simulated. A difference of the remnant
polarizations between two poling protocols (mechanical stress is applied before
and after the application of poling field) is found from our simulations, which
is also observed in experiment. An explanation is given to illustrate why the
remnant polarization for the case that mechanical stress is loaded after the
application of electric field is larger than the case that mechanical stress is
loaded before the application of electric field. Our simulation results supply
a proof for the validity of the two-step-switching model in the
electromechanical poling of polycrystalline ferroelectric ceramics.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 00:06:49 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Wu",
"Yin-Zhong",
""
],
[
"Tao",
"Yong-Mei",
""
]
] | [
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712.0855 | Sofia Quaglioni | S. Quaglioni, P. Navratil | Ab initio no-core shell model and microscopic reactions: recent
achievements | 3 pages, 2 figures, proceedings of the 20th European Conference on
Few-Body Problems in Physics (EFB20) | Few Body Syst.44:337-339,2008 | 10.1007/s00601-008-0322-7 | UCRL-PROC-237032 | nucl-th | null | We report on recent microscopic calculations of reaction properties based
upon the nuclear structure of the ab initio no-core shell model (NCSM).
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 00:10:41 GMT"
}
] | 2009-01-16T00:00:00 | [
[
"Quaglioni",
"S.",
""
],
[
"Navratil",
"P.",
""
]
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712.0856 | Robert Finkelstein j | Robert J. Finkelstein | The Strong and Gravitational Couplings of Knotted Solitons | LaTex file; 23 pages | null | null | UCLA/07/TEP/28 | hep-th | null | We extend our earlier study of the electroweak interactions of quantum knots
to their gravitational and strong interactions. The knots are defined by
appropriate quantum groups and are intended to describe all knotted field
structures that conserve mass and spin, charge and hypercharge, as well as
color charge and color hypercharge. As sources of the gravitational fields the
knots are described as representations of the quantum group $SL_q(2)$ and as
sources of the electroweak and strong fields they are described by $SU_q(2)$.
When the point sources of the standard theory are replaced by the quantum
knots, the interaction terms of the new Lagrangian density acquire knot form
factors and the standard local gauge invariance is supplemented by an
additional global $U(1)\times U(1)$ invariance of the $SU_q(2)$ algebra.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 00:17:43 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Finkelstein",
"Robert J.",
""
]
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712.0857 | Balu Nadiga | Balu Nadiga | On Zonal Jets in Oceans | null | Geophysical Research Letters, Volume 33, Issue 10, L10601, 2006 | null | null | physics.flu-dyn physics.ao-ph | null | We find that in parameter regimes relevant to the recently observed
alternating zonal jets in oceans, the formation of these jets can be explained
as due to an arrest of the turbulent inverse-cascade of energy by {\em free}
Rossby waves (as opposed to Rossby {\em basin} modes) and a subsequent
redirection of that energy into zonal modes. This mechanism, originally studied
in the context of alternating jets in Jovian atmospheres and two dimensional
turbulence in zonally-periodic configurations survives in spite of the presence
of the meridional boundaries in the oceanic context.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 00:17:56 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Nadiga",
"Balu",
""
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] |
712.0858 | Gennady Kovalev V. | Gennady V. Kovalev | Volume Reflection and Refraction of Relativistic Particles in Bent
Crystals | 13 pages, no fig | JETP Lett.87:87-91,2008 | 10.1007/s11448-008-2005-5 | null | physics.acc-ph physics.class-ph | null | The quasi-channeling of positive and negative relativistic particles in a
bent crystal is studied using the classical deflection function. It was shown
that the potential scattering in a central field of bounded ring-like
potentials may produce the ``reflected'' and ``refracted'' fractions of
scattered particles. For particles with positive charge the ``reflected''
fraction is mainly presented; at the same time we predict that for particles
with negative charge the ``refracted'' fraction should dominate. The effect of
``empty core'' for central scattering is also discussed. The average deflection
angles for volume ``reflection'' and ``refraction'' are derived for accepted
potential model of the crystal. The calculated average ``reflection'' angle is
in satisfactory agreement with recent experimental data \cite{ivanov_2006}
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 00:30:27 GMT"
}
] | 2009-12-10T00:00:00 | [
[
"Kovalev",
"Gennady V.",
""
]
] | [
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] |
712.0859 | Edo Noordermeer | E.Noordermeer, M.R.Merrifield, L.Coccato, M.Arnaboldi, M.Capaccioli,
N.G.Douglas, K.C.Freeman, O.Gerhard, K.Kuijken, F.De Lorenzi, N.R.Napolitano
and A.J. Romanowsky | Testing the nature of S0 galaxies using planetary nebula kinematics in
NGC 1023 | Accepted for publication in MNRAS. Version with full resolution
figure 1 can be found at
http://www.nottingham.ac.uk/~ppzmrm/N1023_PNS.accepted.pdf | null | 10.1111/j.1365-2966.2007.12809.x | null | astro-ph | null | We investigate the manner in which lenticular galaxies are formed by studying
their stellar kinematics: an S0 formed from a fading spiral galaxy should
display similar cold outer disc kinematics to its progenitor, while an S0
formed in a minor merger should be more dominated by random motions. In a pilot
study to attempt to distinguish between these scenarios, we have measured the
planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the
Planetary Nebula Spectrograph, we have detected and measured the line-of-sight
velocities of 204 candidate PNe in the field of this galaxy. Out to
intermediate radii, the system displays the kinematics of a normal
rotationally-supported disc system. After correction of its rotational
velocities for asymmetric drift, the galaxy lies just below the spiral galaxy
Tully-Fisher relation, as one would expect for a fading system. However, at
larger radii the kinematics undergo a gradual but major transition to random
motion with little rotation. This transition does not seem to reflect a change
in the viewing geometry or the presence of a distinct halo component, since the
number counts of PNe follow the same simple exponential decline as the stellar
continuum with the same projected disc ellipticity out to large radii. The
galaxy's small companion, NGC 1023A, does not seem to be large enough to have
caused the observed modification either. This combination of properties would
seem to indicate a complex evolutionary history in either the transition to
form an S0 or in the past life of the spiral galaxy from which the S0 formed.
More data sets of this type from both spirals and S0s are needed in order to
definitively determine the relationship between these types of system.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 00:47:15 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Noordermeer",
"E.",
""
],
[
"Merrifield",
"M. R.",
""
],
[
"Coccato",
"L.",
""
],
[
"Arnaboldi",
"M.",
""
],
[
"Capaccioli",
"M.",
""
],
[
"Douglas",
"N. G.",
""
],
[
"Freeman",
"K. C.",
""
],
[
"Gerhard",
"O.",
""
],
[
"Kuijken",
"K.",
""
],
[
"De Lorenzi",
"F.",
""
],
[
"Napolitano",
"N. R.",
""
],
[
"Romanowsky",
"A. J.",
""
]
] | [
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712.086 | Rachel Kuzio de Naray | Rachel Kuzio de Naray, Stacy S. McGaugh, W.J.G. de Blok | Mass Models for Low Surface Brightness Galaxies with High Resolution
Optical Velocity Fields | Accepted for publication in ApJ; 23 pages, 17 color figures; High
resolution images at http://www.astro.umd.edu/~kuzio/PAPERS/massmodels.html | Astrophys.J.676:920-943,2008 | 10.1086/527543 | null | astro-ph | null | We present high-resolution optical velocity fields from DensePak integral
field spectroscopy, along with derived rotation curves, for a sample of low
surface brightness galaxies. In the limit of no baryons, we fit the NFW and
pseudoisothermal halo models to the data and find the rotation curve shapes and
halo central densities to be better described by the isothermal halo. For those
galaxies with photometry, we present halo fits for three assumptions of the
stellar mass-to-light ratio. We find that the velocity contribution from the
baryons is significant enough in the maximum disk case that maximum disk and
the NFW halo are mutually exclusive. We find a substantial cusp mass excess at
the centers of the galaxies, with at least two times more mass expected in the
cuspy CDM halo than is allowed by the data. We also find that to reconcile the
data with LCDM, ~20 km/s noncircular motions are needed and/or the power
spectrum has a lower amplitude on the scales we probe.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 01:02:19 GMT"
}
] | 2010-11-11T00:00:00 | [
[
"de Naray",
"Rachel Kuzio",
""
],
[
"McGaugh",
"Stacy S.",
""
],
[
"de Blok",
"W. J. G.",
""
]
] | [
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] |
712.0861 | Yin-Zhong Wu | Yong-Mei Tao, Yin-Zhong Wu | Effects of anisotropic in-plane strains on the phase diagram of
BaxSr1-xTiO3 thin film | 12 pages, 4 figures | Journal Applied Physics 101,024111(2007) | 10.1063/1.2430642 | null | cond-mat.mtrl-sci cond-mat.soft | null | Based on Landau-Devonshire (LD) phenomenological theory, phase diagram of
epitaxial BST50/50 thin films on anisotropic in-plane strains is investigated.
Different from BaTiO3 thin films, the paraelectric phase appears under the
anisotropic misfit strains on BST50/50 thin films at the room temperature. The
pyroelectric property of the BST films is also calculated, we find that the
position of pyroelectric peak greatly depends on anisotropic misfit strains.
Keywords: anisotropic in-plane strains; BST thin films; phase diagram
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 01:42:04 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Tao",
"Yong-Mei",
""
],
[
"Wu",
"Yin-Zhong",
""
]
] | [
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] |
712.0862 | Igor Rumanov | Igor Rumanov | The correspondence between Tracy-Widom (TW) and Adler-Shiota-van
Moerbeke (ASvM) approaches in random matrix theory: the Gaussian case | 20 pages, submitted to Journal of Mathematical Physics | Journal of Mathematical Physics, 49 (2008), 043503 | 10.1063/1.2890428 | null | math-ph math.MP | null | Two approaches (TW and ASvM) to derivation of integrable differential
equations for random matrix probabilities are compared. Both methods are
rewritten in such a form that simple and explicit relations between all TW
dependent variables and $\tau$-functions of ASvM are found, for the example of
finite size Gaussian matrices. Orthogonal function systems and Toda lattice are
seen as the core structure of both approaches and their relationship.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 01:59:35 GMT"
}
] | 2010-06-24T00:00:00 | [
[
"Rumanov",
"Igor",
""
]
] | [
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] |
712.0863 | Lin-Tian Luh | Lin-Tian Luh | An Improved Error Bound for Gaussian Interpolation | 11 pages | null | null | null | math.NA | null | An error bound for Gaussian Interpolation which is better than the current
exponential-type error bound is presented.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 02:16:26 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Luh",
"Lin-Tian",
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712.0864 | Lin-Tian Luh | Lin-Tian Luh | A New Error Bound for Shifted Surface Spline Interpolation | 12 pages | null | null | null | math.NA | null | A New Error Bound for shifted surface spline interpolation is presented. This
error bound probably is the most powerful one up to now.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 02:22:54 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Luh",
"Lin-Tian",
""
]
] | [
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712.0865 | Yu-Liang Liu | Yu-Liang Liu | Rigorous description of exchange-correlation energy of many-electron
systems | 9pages | null | null | null | cond-mat.mtrl-sci cond-mat.str-el | null | With the eigenfunctional theory, we study a general interacting electron
system, and give a rigorous expression of its ground state energy which is
composed of two parts, one part is contributed by the non-interacting
electrons, and another one is represented by the correlation functions that are
controlled by the electron correlation. Moreover, according to the rigorous
expression of the ground state energy, an effective method beyond the local
density approximation of the density functional theory is proposed.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 02:27:05 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Liu",
"Yu-Liang",
""
]
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712.0866 | Alexander Stoimenow | A. Stoimenow | Alexander polynomials and hyperbolic volume of arborescent links | 31 pages | null | null | null | math.GT | null | We realize a given (monic) Alexander polynomial by a (fibered) hyperbolic
arborescent knot and link of any number of components, and by infinitely many
such links of at least 4 components. As a consequence, a Mahler measure
minimizing polynomial, if it exists, is realized as the Alexander polynomial of
a fibered hyperbolic link of at least 2 components. For given polynomial, we
give also an upper bound on the minimal hyperbolic volume of knots/links, and
contrarily, construct knots of arbitrarily large volume, which are arborescent,
or have given free genus at least 2.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 02:40:01 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Stoimenow",
"A.",
""
]
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712.0867 | Thomas Mehen | Thomas Mehen (Duke U.) | On Non-Relativistic Conformal Field Theory and Trapped Atoms: Virial
Theorems and the State-Operator Correspondence in Three Dimensions | 23 pages, 3 .ps figures | null | 10.1103/PhysRevA.78.013614 | null | cond-mat.other hep-th nucl-th | null | The field theory of nonrelativistic fermions interacting via contact
interactions can be used to calculate the properties of few-body systems of
cold atoms confined in harmonic traps. The state-operator correspondence of
Non-Relativistic Conformal Field Theory (NRCFT) shows that the energy
eigenvalues (in oscillator units) of N harmonically trapped fermions can be
calculated from the scaling dimensions of N-fermion operators in the NRCFT.
They are also in one-to-one correspondence with zero-energy, scale-invariant
solutions to the N-body problem in free space. We show that these two mappings
of the trapped fermion problem to free space problems are related by an
automorphism of the SL(2,R) algebra of the conformal symmetry of fermions at
the unitary limit. This automorphism exchanges the internal Hamiltonian of the
gas with the trapping potential and hence provides a novel method for deriving
virial theorems for trapped Fermi gases at the unitary limit. We also show that
the state-operator correspondence can be applied directly in three spatial
dimensions by calculating the scaling dimensions of two- and three-fermion
operators and finding agreement with known exact results for energy levels of
two and three trapped fermions at the unitary limit.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 05:36:27 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Mehen",
"Thomas",
"",
"Duke U."
]
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712.0868 | Hernando Quevedo | Hernando Quevedo and Alejandro Vazquez | The geometry of thermodynamics | 8 pages, no figures, prepared for Proceedings of the III Mexican
Meeting on Mathematical and Experimental Physics | AIP Conf.Proc.977:165-172,2008 | 10.1063/1.2902782 | null | math-ph gr-qc math.MP physics.chem-ph | null | We present a review of the main aspects of geometrothermodynamics, an
approach which allows us to associate a specific Riemannian structure to any
classical thermodynamic system. In the space of equilibrium states, we consider
a Legendre invariant metric, which is given in terms of the fundamental
equation of the corresponding thermodynamic system, and analyze its geometric
properties in the case of the van der Waals gas, and black holes. We conclude
that the geometry of this particular metric reproduces the thermodynamic
behavior of the van der Waals gas, and the Reissner-Nordstr\"om black hole, but
it is not adequate for the thermodynamic description of Kerr black holes.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 03:22:21 GMT"
}
] | 2011-04-11T00:00:00 | [
[
"Quevedo",
"Hernando",
""
],
[
"Vazquez",
"Alejandro",
""
]
] | [
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] |
712.0869 | Jonathan Harrison | J. M. Harrison | Quantum graphs with spin Hamiltonians | 17 pages, typos corrected, references and comments added | P Exner, JP Keating, P Kuchment, T Sunada, A Teplyaev (Eds)
Analysis on graphs and its applications, Proceedings of Symposia in Pure
Mathematics 77 (AMS 2008) 261-277 | null | null | math-ph math.MP | null | The article surveys quantization schemes for metric graphs with spin.
Typically quantum graphs are defined with the Laplace or Schrodinger operator
which describe particles whose intrinsic angular momentum (spin) is zero.
However, in many applications, for example modeling an electron (which has
spin-1/2) on a network of thin wires, it is necessary to consider operators
which allow spin-orbit interaction. The article presents a review of
quantization schemes for graphs with three such Hamiltonian operators, the
Dirac, Pauli and Rashba Hamiltonians. Comparing results for the trace formula,
spectral statistics and spin-orbit localization on quantum graphs with spin
Hamiltonians.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 05:23:34 GMT"
},
{
"version": "v2",
"created": "Wed, 30 Jan 2008 16:58:22 GMT"
}
] | 2010-12-06T00:00:00 | [
[
"Harrison",
"J. M.",
""
]
] | [
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712.087 | Janos Zsargo | J. Zsargo, D. J. Hillier, L. N. Georgiev | Axi-symmetric Models of B[e] Supergiants: I. The Effective Temperature
and Mass-loss Dependence of the Hydrogen and Helium Ionization Structure | Accepted for publication in A&A | null | 10.1051/0004-6361:20078293 | null | astro-ph | null | We calculate the hydrogen and helium ionization in B[e] envelopes and explore
their dependence on mass-loss and effective temperature. We also present
simulated observations of the Halpha emission line and the C IV 1550 doublet,
and study their behavior. This paper reports our first results in an ongoing
study of B[e] supergiants, and provides a glimpse on the ionization of the most
important elements in self-consistent numerical simulations.
Our newly developed 2D stellar atmosphere code, ASTAROTH, was used for the
numerical simulations. The code self-consistently solves for the continuum
radiation, non-LTE level populations, and electron temperature in axi-symmetric
stellar envelopes. Observed profiles were calculated by an auxiliary program
developed separately from ASTAROTH.
In all but one of our models, H remained fully ionized. Due to ionizations
from excited states it is much more difficult to get a H neutral disk than
indicated by previous analytical calculations. Near the poles, the ionization
is high in all models, while helium recombined in the equatorial regions for
all but our lowest mass-loss rate. Although the model parameters were not
adjusted to provide fits to any particular star, the theoretical profiles show
some features seen in the profiles of R126. These include the partially
resolved double peaked profile of Halpha, and the weak emission associated with
the UV C IV resonance line.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 03:59:54 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Zsargo",
"J.",
""
],
[
"Hillier",
"D. J.",
""
],
[
"Georgiev",
"L. N.",
""
]
] | [
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712.0871 | Anant Sahai | Anant Sahai | Balancing forward and feedback error correction for erasure channels
with unreliable feedback | 20 pages, 6 pages, submitted to IEEE Transactions on Information
Theory, an earlier version was presented at ITA '07 in UCSD | null | null | null | cs.IT math.IT | null | The traditional information theoretic approach to studying feedback is to
consider ideal instantaneous high-rate feedback of the channel outputs to the
encoder. This was acceptable in classical work because the results were
negative: Shannon pointed out that even perfect feedback often does not improve
capacity and in the context of symmetric DMCs, Dobrushin showed that it does
not improve the fixed block-coding error exponents in the interesting high rate
regime. However, it has recently been shown that perfect feedback does allow
great improvements in the asymptotic tradeoff between end-to-end delay and
probability of error, even for symmetric channels at high rate. Since gains are
claimed with ideal instantaneous feedback, it is natural to wonder whether
these improvements remain if the feedback is unreliable or otherwise limited.
Here, packet-erasure channels are considered on both the forward and feedback
links. First, the feedback channel is considered as a given and a strategy is
given to balance forward and feedback error correction in the suitable
information-theoretic limit of long end-to-end delays. At high enough rates,
perfect-feedback performance is asymptotically attainable despite having only
unreliable feedback! Second, the results are interpreted in the zero- sum case
of "half-duplex" nodes where the allocation of bandwidth or time to the
feedback channel comes at the direct expense of the forward channel. It turns
out that even here, feedback is worthwhile since dramatically lower asymptotic
delays are possible by appropriately balancing forward and feedback error
correction.
The results easily generalize to channels with strictly positive
zero-undeclared-error capacities.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 04:08:57 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Sahai",
"Anant",
""
]
] | [
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] |
712.0872 | Peng Wang | Peng Wang, Tom Abel (KIPAC, Stanford; Kitp, Ucsb) | Magnetohydrodynamic Simulations of Disk Galaxy Formation: the
Magnetization of The Cold and Warm Medium | 13 pages, 14 figures. Higher resolution figure version can be found
at http://www.stanford.edu/~pengwang/mhddisk.pdf | Astrophys.J.696:96-109,2009 | 10.1088/0004-637X/696/1/96 | null | astro-ph | null | Using magnetohydrodynamic (MHD) adaptive mesh refinement simulations, we
study the formation and early evolution of disk galaxies with a magnetized
interstellar medium. For a $10^{10}$ \msun halo with initial NFW dark matter
and gas profiles, we impose a uniform $10^{-9}$ G magnetic field and follow its
collapse, disk formation and evolution up to 1 Gyr. Comparing to a purely
hydrodynamic simulation with the same initial condition, we find that a
protogalactic field of this strength does not significantly influence the
global disk properties. At the same time, the initial magnetic fields are
quickly amplified by the differentially rotating turbulent disk. After the
initial rapid amplification lasting $\sim500$ Myr, subsequent field
amplification appears self-regulated. As a result, highly magnetized material
begin to form above and below the disk. Interestingly, the field strengths in
the self-regulated regime agrees well with the observed fields in the Milky Way
galaxy both in the warm and the cold HI phase and do not change appreciably
with time. Most of the cold phase shows a dispersion of order ten in the
magnetic field strength. The global azimuthal magnetic fields reverse at
different radii and the amplitude declines as a function of radius of the disk.
By comparing the estimated star formation rate (SFR) in hydrodynamic and MHD
simulations, we find that after the magnetic field strength saturates, magnetic
forces provide further support in the cold gas and lead to a decline of the
SFR.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 04:48:52 GMT"
}
] | 2009-04-17T00:00:00 | [
[
"Wang",
"Peng",
"",
"KIPAC, Stanford; Kitp, Ucsb"
],
[
"Abel",
"Tom",
"",
"KIPAC, Stanford; Kitp, Ucsb"
]
] | [
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] |
712.0873 | Anant Sahai | Cheng Chang and Anant Sahai | The price of ignorance: The impact of side-information on delay for
lossless source-coding | 25 pages, 17 figures. Submitted to the IEEE Transactions on
Information Theory | null | null | null | cs.IT math.IT | null | Inspired by the context of compressing encrypted sources, this paper
considers the general tradeoff between rate, end-to-end delay, and probability
of error for lossless source coding with side-information. The notion of
end-to-end delay is made precise by considering a sequential setting in which
source symbols are revealed in real time and need to be reconstructed at the
decoder within a certain fixed latency requirement. Upper bounds are derived on
the reliability functions with delay when side-information is known only to the
decoder as well as when it is also known at the encoder.
When the encoder is not ignorant of the side-information (including the
trivial case when there is no side-information), it is possible to have
substantially better tradeoffs between delay and probability of error at all
rates. This shows that there is a fundamental price of ignorance in terms of
end-to-end delay when the encoder is not aware of the side information. This
effect is not visible if only fixed-block-length codes are considered. In this
way, side-information in source-coding plays a role analogous to that of
feedback in channel coding.
While the theorems in this paper are asymptotic in terms of long delays and
low probabilities of error, an example is used to show that the qualitative
effects described here are significant even at short and moderate delays.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 04:38:03 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Chang",
"Cheng",
""
],
[
"Sahai",
"Anant",
""
]
] | [
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712.0874 | Hironori Matsumoto | Hironori Matsumoto (1), Hideki Uchiyama (1), Makoto Sawada (1),
Takeshi G. Tsuru (1), Katsuji Koyama (1), Hideaki Katagiri (2), Ryo Yamazaki
(2), Aya Bamba (3), Kazunori Kohri (4), Koji Mori (5), Yasunobu Uchiyama (3)
((1) Kyoto University, (2) Hiroshima University, (3) ISAS/JAXA, (4) Lancaster
University, (5) Miyazaki University) | Discovery of Extended X-Ray emission from the unidentified TeV source
HESS J1614-518 using the Suzaku Satellite | Accepted for publication in PASJ vol. 60 Suzaku Special Issue 2 | null | 10.1093/pasj/60.sp1.S163 | null | astro-ph | null | We report the Suzaku results of HESS J1614-518, which is the brightest
extended TeV gamma-ray source discovered in the Galactic plane survey conducted
using the H.E.S.S. telescope. We discovered three X-ray objects in the field of
view of the X-ray Imaging Spectrometer (XIS), which were designated as Suzaku
J1614-5141 (src A), Suzaku J1614-5152 (src B), and Suzaku J1614-5148 (src C).
Src A is an extended source located at the peak position of HESS J1614-518, and
therefore it is a plausible counterpart to HESS J1614-518. The X-ray flux in
the 2-10 keV band is 5e-13 erg/s/cm^2, which is an order of magnitude smaller
than the TeV flux. The photon index is 1.7, which is smaller than the canonical
value of synchrotron emissions from high-energy electrons found in some
supernova remnants. These findings present a challenge to models in which the
origin of the TeV emission is the inverse Compton scattering of the cosmic
microwave background by accelerated electrons that emit X-rays via synchrotron
emission. Src B is located at a relatively dim region in the TeV band image;
however, its hydrogen column density is the same as that of src A. Therefore,
src B may also be physically related to HESS J1614-518. Src C is a foreground
late-type B star. We also discovered a soft extended X-ray emission near HESS
J1614-518.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 04:45:59 GMT"
}
] | 2017-01-18T00:00:00 | [
[
"Matsumoto",
"Hironori",
""
],
[
"Uchiyama",
"Hideki",
""
],
[
"Sawada",
"Makoto",
""
],
[
"Tsuru",
"Takeshi G.",
""
],
[
"Koyama",
"Katsuji",
""
],
[
"Katagiri",
"Hideaki",
""
],
[
"Yamazaki",
"Ryo",
""
],
[
"Bamba",
"Aya",
""
],
[
"Kohri",
"Kazunori",
""
],
[
"Mori",
"Koji",
""
],
[
"Uchiyama",
"Yasunobu",
""
]
] | [
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712.0875 | Milton da Costa Lopes Fo. | Milton C. Lopes Filho | Boundary layers and the vanishing viscosity limit for incompressible 2D
flow | 28 pages | null | null | null | math.AP | null | This manuscript is a survey on results related to boundary layers and the
vanishing viscosity limit for incompressible flow. It is the lecture notes for
a 10 hour minicourse given at the Morningside Center, Academia Sinica, Beijing,
PRC from 11/28 to 12/07, 2007. The main topics covered are: a derivation of
Prandtl's boundary layer equation; an outline of the rigorous theory of
Prandtl's equation, without proofs; Kato's criterion for the vanishing
viscosity limit; the vanishing viscosity limit with Navier friction condition;
rigorous boundary layer theory for the Navier friction condition and boundary
layers for flows in a rotating cylinder.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 05:13:57 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Filho",
"Milton C. Lopes",
""
]
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] |
712.0876 | Marco Ghiotti | Marco Ghiotti | Gauge fixing and BRST formalism in non-Abelian gauge theories | Jan 2007. 146pp. Ph.D. Thesis (Advisor: L. von Smekal and A.G.
Williams) | null | null | null | hep-th | null | In this Thesis we present a comprehensive study of perturbative and
non-perturbative non-Abelian gauge theories in the light of gauge-fixing
procedures, focusing our attention on the BRST formalism in Yang-Mills theory.
We propose first a model to re-write the Faddeev-Popov quantisation method in
terms of group-theoretical techniques and then we give a possible way to solve
the no-go theorem of Neuberger for lattice Yang-Mills theory with double BRST
symmetry. In the final part we present a study of the Batalin-Vilkovisky
quantisation method for non-linear gauges in non-Abelian gauge theories.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 05:36:59 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Ghiotti",
"Marco",
""
]
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712.0877 | Masayoshi Nobukawa | Masayoshi Nobukawa, Takeshi Go Tsuru, Yojiro Takikawa, Yoshiaki Hyodo,
Tatsuya Inui, Hiroshi Nakajima, Hironori Matsumoto and Katsuji Koyama,
Hiroshi Murakami, and Shigeo Yamauchi | Suzaku Spectroscopy of an X-Ray Reflection Nebula and a New Supernova
Remnant Candidate in the Sgr B1 Region | 10 pages, 10 figures | null | 10.1093/pasj/60.sp1.S191 | null | astro-ph | null | We made a 100 ks observation of the Sagittarius (Sgr) B1 region at (l, b) =
(0.5, -0.1) near to the Galactic center (GC) with the Suzaku/XIS. Emission
lines of S XV, Fe I, Fe XXV, and Fe XXVI were clearly detected in the spectrum.
We found that the Fe XXV and Fe XXVI line emissions smoothly distribute over
the Sgr B1 and B2 regions connecting from the GC. This result suggests that the
GC hot plasma extends at least up to the Sgr B region with a constant
temperature. There are two diffuse X-ray sources in the observed region. One of
the two (G0.42-0.04) is newly discovered, and exhibits a strong S XV Ka
emission line, suggesting a candidate for a supernova remnant located in the GC
region. The other one (M0.51-0.10), having a prominent Fe I Ka emission line
and a strongly absorbed continuum, is likely to be an X-ray reflection nebula.
There is no near source bright enough to irradiate M0.51-0.10. However, the Fe
I Ka emission can be explained if Sgr A* was ~ 10^6 times brighter 300 years
ago, the light travel time for 100 pc to M0.51-0.10, than it is at present.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 06:33:23 GMT"
}
] | 2017-01-18T00:00:00 | [
[
"Nobukawa",
"Masayoshi",
""
],
[
"Tsuru",
"Takeshi Go",
""
],
[
"Takikawa",
"Yojiro",
""
],
[
"Hyodo",
"Yoshiaki",
""
],
[
"Inui",
"Tatsuya",
""
],
[
"Nakajima",
"Hiroshi",
""
],
[
"Matsumoto",
"Hironori",
""
],
[
"Koyama",
"Katsuji",
""
],
[
"Murakami",
"Hiroshi",
""
],
[
"Yamauchi",
"Shigeo",
""
]
] | [
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] |
712.0878 | Lev Magarill Dr. | A.V. Chaplik, L.I. Magarill, R.Z. Vitlina | Friedel oscillations of screening in nanotubes | 3 pages | null | null | null | cond-mat.other | null | In 3D and 2D electronic systems the singular contribution to the static
permittivity $\epsilon$ (Kohn singularity) is a small correction to the regular
part of $\epsilon$ but it results in the leading term in asymptotic behavior of
the screened potential (Friedel oscillations). In the present letter we show
that for nanotubes quite different results are valid: $\epsilon$ becomes
infinitely large at the singular point and the Friedel oscillations do not play
the dominant role in the screening at the large distances. Moreover, the zero
and highest cylindrical harmonics of the effective potential are screened by
quite different mechanisms.
| [
{
"version": "v1",
"created": "Thu, 6 Dec 2007 06:12:14 GMT"
}
] | 2007-12-07T00:00:00 | [
[
"Chaplik",
"A. V.",
""
],
[
"Magarill",
"L. I.",
""
],
[
"Vitlina",
"R. Z.",
""
]
] | [
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] |
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