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711.2308 | Tridivesh Jena | David Tytler, Mark Gleed, Carl Melis, Angela Chapman, David Kirkman,
Dan Lubin, Pascal Paschos, Tridivesh Jena and Arlin P.S. Crotts | Metal Absorption Systems in Spectra of Pairs of QSOs | 36 pages with 25 figures and 10 Tables Submited to MNRAS | null | 10.1111/j.1365-2966.2008.14159.x | null | astro-ph | null | We present the first large sample of absorption systems in paired QSOs
consisting of 691 absorption systems in the spectra of 310 QSOs including 170
pairings. All these absorption systems have metal lines, usually C IV or Mg II.
We see 17 cases of absorption in one line-of-sight within 200 km/s (1 Mpc) of
absorption in the paired line-of-sight with the probability at least approx 50%
at 100kpc, declining rapidly to 23% at 100 - 200 kpc. We detect clustering on
0.5Mpc scales and see a hint of the "fingers of God" redshift-space distortion.
The distribution matches absorbers arising in galaxies at z=2 with a normal
correlation function and systematic infall velocities but unusually low random
pair-wise velocity differences. Absorption in gas flowing out from galaxies at
a mean velocity of 250 km/s would produce vastly more elongation than we see.
The UV absorption from fast winds that Adelberger et al. 2005 see in spectra of
LBGs is not representative of the absorption that we see. Either the winds are
confined to LBGs, or they can not extend to 40 kpc with large velocities, while
continuing to make UV absorption we see, implying most metals were in place in
the IGM long before z=2. Separately, when we examine the absorption seen when a
sight line passes a second QSO, we see 19 absorbers within 400 km/s of the
partner QSO. The probability of seeing absorption is approximately constant for
impact parameters 0.1 - 1.5 Mpc. Perhaps we do not see a rapid rise in the
probability at small impact parameters because the UV from QSOs destroys some
absorbers near to the QSOs. The 3D distribution of 64 absorbers around 313 QSOs
is to first order isotropic, with just a hint of the anisotropy expected if the
QSO UV emission is beamed, or alternatively QSOs might emit UV isotropically
but for a surprisingly short time of only 0.3Myr.
| [
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] | 2017-02-01T00:00:00 | [
[
"Tytler",
"David",
""
],
[
"Gleed",
"Mark",
""
],
[
"Melis",
"Carl",
""
],
[
"Chapman",
"Angela",
""
],
[
"Kirkman",
"David",
""
],
[
"Lubin",
"Dan",
""
],
[
"Paschos",
"Pascal",
""
],
[
"Jena",
"Tridivesh",
""
],
[
"Crotts",
"Arlin P. S.",
""
]
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711.2309 | Le Hur Karyn | Peter P. Orth, Ivan Stanic, Karyn Le Hur | Dissipative Quantum Ising model in a cold atomic spin-boson mixture | 4 pages, 2 figures, 1 table; Title modified and cosmetic changes | Phys. Rev. A 77, 051601(R) (2008) | 10.1103/PhysRevA.77.051601 | null | cond-mat.other | null | Using cold bosonic atoms with two (hyperfine) ground states, we introduce a
spin-boson mixture which allows to implement the quantum Ising model in a
tunable dissipative environment. The first specie lies in a deep optical
lattice with tightly confining wells and forms a spin array; spin-up/down
corresponds to occupation by one/no atom at each site. The second specie forms
a superfluid reservoir. Different species are coupled coherently via laser
transitions and collisions. Whereas the laser coupling mimics a transverse
field for the spins, the coupling to the reservoir sound modes induces a
ferromagnetic (Ising) coupling as well as dissipation. This gives rise to an
order-disorder quantum phase transition where the effect of dissipation can be
studied in a controllable manner.
| [
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"created": "Fri, 23 Nov 2007 17:32:38 GMT"
},
{
"version": "v3",
"created": "Mon, 24 Mar 2008 15:55:53 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Orth",
"Peter P.",
""
],
[
"Stanic",
"Ivan",
""
],
[
"Hur",
"Karyn Le",
""
]
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711.231 | Simon Kochen | John Conway and Simon Kochen | Thou Shalt Not Clone One Bit! | null | null | null | null | quant-ph | null | We prove a no-triplets theorem for spin 1 particles, which implies a
strengthened form of the no-cloning theorem.
| [
{
"version": "v1",
"created": "Wed, 14 Nov 2007 21:49:32 GMT"
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] | 2007-11-16T00:00:00 | [
[
"Conway",
"John",
""
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[
"Kochen",
"Simon",
""
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] |
711.2311 | Leonardo Pati\~no | Axel de la Macorra, Leonardo Patino (UNAM, Mexico) | Cosmological consequences of scalar mesons from gauge/gravity
correspondence | 14 pages, 9 figures | Nuovo Cim.B124:525-538,2009 | 10.1393/ncb/i2009-10789-3 | null | hep-th astro-ph | null | We consider the spectrum of mesons for the gauge theory dual to a
supergravity configuration of intersecting D3/D7 branes, and use the expression
for the Lagrangian of the scalar mesons to compute explicitly the Lagrangian
for the lightest states in the infrared limit. Assuming that the matter content
of this gauge theory is part of a hidden sector, which interacts with the
standard model only via gravity, we explore the cosmological consequences of
these lightest scalar mesons for a FRW universe. We show that phantom fields
may appear naturally in this kind of scenarios.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 17:51:42 GMT"
}
] | 2009-12-08T00:00:00 | [
[
"de la Macorra",
"Axel",
"",
"UNAM, Mexico"
],
[
"Patino",
"Leonardo",
"",
"UNAM, Mexico"
]
] | [
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] |
711.2312 | Mark Dijkstra | Mark Dijkstra, Abraham Loeb | The Polarization of Scattered Lyman Alpha Radiation Around High-Redshift
Galaxies | 14 pages, 12 figures, matches version published in MNRAS. Discussion
on polarization dependence of phase function added in Appendix | null | 10.1111/j.1365-2966.2008.13066.x | null | astro-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The high-redshift Universe contains luminous Lyman Alpha (hereafter Lya)
emitting sources such as galaxies and quasars. The emitted Lya radiation is
often scattered by surrounding neutral hydrogen atoms. We show that the
scattered Lya radiation obtains a high level of polarization for a wide range
of likely environments of high-redshift galaxies. For example, the
back-scattered Lya flux observed from galaxies surrounded by a superwind-driven
outflow may reach a fractional polarization as high as ~40%. Equal levels of
polarization may be observed from neutral collapsing protogalaxies. Resonant
scattering in the diffuse intergalactic medium typically results in a lower
polarization amplitude (<7%), which depends on the flux of the ionizing
background. Spectral polarimetry can differentiate between Lya scattering off
infalling gas and outflowing gas; for an outflow the polarization should
increase towards longer wavelengths while for infall the opposite is true. Our
numerical results suggest that Lya polarimetry is feasible with existing
instruments, and may provide a new diagnostic of the distribution and
kinematics of neutral hydrogen around high-redshift galaxies. Moreover,
polarimetry may help suppress infrared lines originating in the Earth's
atmosphere, and thus improve the sensitivity of ground-based observations to
high-redshift Lya emitting galaxies outside the currently available redshift
windows.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 19:46:54 GMT"
},
{
"version": "v2",
"created": "Wed, 16 Jul 2008 16:08:57 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Dijkstra",
"Mark",
""
],
[
"Loeb",
"Abraham",
""
]
] | [
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] |
711.2313 | Alexei Moiseev | V.P. Arkhipova (1), T.A. Lozinskaya (1), A.V. Moiseev (2), O.V. Egorov
(1) ((1) Sternberg Astronomical Institute, Moscow, Russia, (2) Special
Astrophysical Observatory, Russia) | The gas emission spectrum in a star-forming region in the BCD galaxy VII
Zw 403 (UGC 6456) | 9 pages, 6 EPS figures | Astron.Rep.51:871-881,2007 | 10.1134/S1063772907110017 | Astron. Reports, 2007, vol. 51, N 11, pp. 871-881 | astro-ph | null | Observations with the 6-m telescope of the Special Astrophysical Observatory
obtained with the MPFS integral-field spectrograph and a longslit spectrograph
with the SCORPIO focal reducer are used to analyze the emission spectrum of the
ionized gas in a star-forming region in the BCD galaxy VII Zw 403. We present
images of the galactic central region in the H-alpha, H-beta, [SII], and [OIII]
emission lines, together with maps of the relative [OIII]/H-beta and
[SII]/H-alpha intensities. We have determined the parameters of the gas in
bright ionized supershells, and estimated the relative abundances of oxygen,
nitrogen, and sulfur; a low relative N/O abundance was detected.
| [
{
"version": "v1",
"created": "Wed, 14 Nov 2007 22:20:38 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Arkhipova",
"V. P.",
""
],
[
"Lozinskaya",
"T. A.",
""
],
[
"Moiseev",
"A. V.",
""
],
[
"Egorov",
"O. V.",
""
]
] | [
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] |
711.2314 | Kevin E. Bassler | Min Liu and Kevin E. Bassler | Finite size effects and symmetry breaking in the evolution of networks
of competing Boolean nodes | 30 pages, 8 figures, 3 tables | null | null | null | cond-mat.stat-mech cond-mat.dis-nn nlin.AO physics.bio-ph physics.soc-ph q-bio.PE | null | The effects of the finite size of the network on the evolutionary dynamics of
a Boolean network are analyzed. In the model considered, Boolean networks
evolve via a competition between nodes that punishes those in the majority. It
is found that finite size networks evolve in a fundamentally different way than
infinitely large networks do. The symmetry of the evolutionary dynamics of
infinitely large networks that selects for canalizing Boolean functions is
broken in the evolutionary dynamics of finite size networks. In finite size
networks there is an additional selection for input inverting Boolean functions
that output a value opposite to the majority of input values. These results are
revealed through an empirical study of the model that calculates the frequency
of occurrence of the different possible Boolean functions. Classes of functions
are found to occur with the same frequency. Those classes depend on the
symmetry of the evolutionary dynamics and correspond to orbits of the relevant
symmetry group. The empirical results match analytic results, determined by
utilizing Polya's theorem, for the number of orbits expected in both finite
size and infinitely large networks. The reason for the symmetry breaking in the
evolutionary dynamics is found to be due to the need for nodes in finite size
networks to behave differently in order to cooperate so that the system
collectively performs as well as possible. The results suggest that both finite
size effects and symmetry are important for understanding the evolution of
real-world complex networks, including genetic regulatory networks.
| [
{
"version": "v1",
"created": "Wed, 14 Nov 2007 22:44:46 GMT"
}
] | 2016-09-08T00:00:00 | [
[
"Liu",
"Min",
""
],
[
"Bassler",
"Kevin E.",
""
]
] | [
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] |
711.2315 | Margaret Reid | E. G. Cavalcanti and M. D. Reid | Uncertainty relations for the realisation of macroscopic quantum
superpositions and EPR paradoxes | 9 pages, 2 figures, to appear Journ Mod Optics work presented at PQE
2007 conference | Journal of Modern Optics, 54, 2373 (2007) | 10.1080/09500340701639623 | null | quant-ph | null | We present a unified approach, based on the use of quantum uncertainty
relations, for arriving at criteria for the demonstration of the EPR paradox
and macroscopic superpositions. We suggest to view each criterion as a means to
demonstrate an EPR-type paradox, where there is an inconsistency between the
assumptions of a form of realism, either macroscopic realism (MR) or local
realism (LR), and the completeness of quantum mechanics.
| [
{
"version": "v1",
"created": "Wed, 14 Nov 2007 22:55:51 GMT"
}
] | 2008-06-18T00:00:00 | [
[
"Cavalcanti",
"E. G.",
""
],
[
"Reid",
"M. D.",
""
]
] | [
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] |
711.2316 | Benjamin Monreal | Benjamin Monreal, Lorne A. Nelson, and Joseph A. Formaggio | Spallation nuclei in substellar objects: a new dark-matter signature? | preprint, 9 pages, 3 figures | null | null | null | astro-ph | null | Although dark matter makes up 80% of the gravitational mass of our Galaxy,
its composition is not known. One hypothesis is that dark matter consists of
massive particles called WIMPs. WIMPs are expected to accumulate and
coannihilate in the cores of stars, but the only signature of this accumulation
has been thought to be hard- to-observe high-energy neutrinos. Here we propose
an entirely new observable signature. WIMP coannihilations in the core of a
very low-mass star, brown dwarf, or planetary-mass object should alter the
star's chemical composition via spallation reactions. Very close to the
Galactic center, these stars may acquire extremely high lithium, beryllium, and
boron abundances, even for models with otherwise- undetectable WIMP-nucleon
cross sections. These abundances should be measurable in certain stellar
systems and phenomena.
| [
{
"version": "v1",
"created": "Wed, 14 Nov 2007 23:06:15 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Monreal",
"Benjamin",
""
],
[
"Nelson",
"Lorne A.",
""
],
[
"Formaggio",
"Joseph A.",
""
]
] | [
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] |
711.2317 | Massimo Persic | Massimo Persic (INAF & INFN, Trieste), Alessandro De Angelis (Udine U.
& INFN, Udine) | Intergalactic absorption and blazar gamma-ray spectra | A&A, in press (accepted Jan 29, 2008): 6 pages, 2 figures. One
source, published subsequent to acceptance, added | null | 10.1051/0004-6361:20079074 | null | astro-ph | null | The distribution of TeV spectral slopes versus redshift for currently known
TeV blazars (16 sources with z<0.21, and one with z>0.25) is essentially a
scatter plot with hardly any hint of a global trend. We suggest that this is
the outcome of two combined effects of intergalactic gamma-gamma absorption,
plus an inherent feature of the SSC (synchro-self-Compton) process of blazar
emission. First, flux dimming introduces a bias that favors detection of
progressively more flaring sources at higher redshifts. According to mainstream
SSC models, more flaring source states imply sources with flatter TeV slopes.
This results in a structured relation between intrinsic TeV slope and redshift.
The second effect, spectral steepening by intergalactic absorption, affects
sources progressively with distance and effectively wipes out the intrinsic
slope-redshift correlation.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 20:26:36 GMT"
},
{
"version": "v2",
"created": "Tue, 5 Feb 2008 22:33:24 GMT"
},
{
"version": "v3",
"created": "Mon, 24 Mar 2008 11:40:23 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Persic",
"Massimo",
"",
"INAF & INFN, Trieste"
],
[
"De Angelis",
"Alessandro",
"",
"Udine U.\n & INFN, Udine"
]
] | [
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] |
711.2318 | Sergey Cherkis | Sergey A. Cherkis and Brian Durcan | The 't Hooft-Polyakov Monopole in the Presence of a 't Hooft Operator | 11 pages, 7 figures. Exposition improved, appendix added with
construction details | Phys.Lett.B671:123-127,2009 | 10.1016/j.physletb.2008.11.065 | TCDMATH 07-22, HMI 07-09 | hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We present explicit BPS field configurations representing one nonabelian
monopole with one minimal weight 't Hooft operator insertion. We explore the
SO(3) and SU(2) gauge groups. In the case of SU(2) gauge group the minimal 't
Hooft operator can be completely screened by the monopole. If the gauge group
is SO(3), however, such screening is impossible. In the latter case we observe
a different effect of the gauge symmetry enhancement in the vicinity of the 't
Hooft operator.
| [
{
"version": "v1",
"created": "Wed, 14 Nov 2007 23:30:48 GMT"
},
{
"version": "v2",
"created": "Tue, 2 Dec 2008 18:02:32 GMT"
}
] | 2009-01-16T00:00:00 | [
[
"Cherkis",
"Sergey A.",
""
],
[
"Durcan",
"Brian",
""
]
] | [
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] |
711.2319 | Wen Zhao | Wen Zhao | Statefinder diagnostic for Yang-Mills dark energy model | 13 pages, 3figures, minor typos corrected | Int.J.Mod.Phys.D17:1245-1254,2008 | 10.1142/S0218271808012796 | null | gr-qc astro-ph.CO | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We study the statefinder parameters in the Yang-Mills condensate dark energy
models, and find that the evolving trajectories of these models are different
from those of other dark energy models. We also define two eigenfunctions of
the Yang-Mills condensate dark energy models. The values of these
eigenfunctions are quite close to zero if the equation-of-state of the
Yang-Mills condensate is not far from -1, which can be used to simply
differentiate between the Yang-Mills condensate models and other dark energy
models.
| [
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{
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] | 2009-04-10T00:00:00 | [
[
"Zhao",
"Wen",
""
]
] | [
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711.232 | Tom H. Koornwinder | Tom H. Koornwinder | Zhedanov's Algebra AW(3) and the Double Affine Hecke Algebra in the Rank
One Case. II. The Spherical Subalgebra | This is a contribution to the Proc. of the Seventh International
Conference ''Symmetry in Nonlinear Mathematical Physics'' (June 24-30, 2007,
Kyiv, Ukraine), published in SIGMA (Symmetry, Integrability and Geometry:
Methods and Applications) at http://www.emis.de/journals/SIGMA/ In v2 remarks
about duality anti-algebra isomorphism and about shift operators added | SIGMA 4 (2008), 052, 17 pages | 10.3842/SIGMA.2008.052 | null | math.QA | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | This paper builds on the previous paper arXiv:math/0612730 by the author,
where a relationship between Zhedanov's algebra AW(3) and the double affine
Hecke algebra (DAHA) corresponding to the Askey-Wilson polynomials was
established. It is shown here that the spherical subalgebra of this DAHA is
isomorphic to AW(3) with an additional relation that the Casimir operator
equals an explicit constant. A similar result with q-shifted parameters holds
for the antispherical subalgebra. Some theorems on centralizers and centers for
the algebras under consideration will finally be proved as corollaries of the
characterization of the spherical and antispherical subalgebra.
| [
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},
{
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"created": "Tue, 10 Jun 2008 15:19:44 GMT"
}
] | 2008-06-10T00:00:00 | [
[
"Koornwinder",
"Tom H.",
""
]
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711.2321 | Cora Dvorkin | Cora Dvorkin (U. Chicago), Hiranya V. Peiris (U. Chicago/Cambridge),
and Wayne Hu (U. Chicago) | Testable polarization predictions for models of CMB isotropy anomalies | 17 pages, 15 figures; published in PRD; references added | Phys.Rev.D77:063008,2008 | 10.1103/PhysRevD.77.063008 | null | astro-ph | null | Anomalies in the large-scale CMB temperature sky measured by WMAP have been
suggested as possible evidence for a violation of statistical isotropy on large
scales. In any physical model for broken isotropy, there are testable
consequences for the CMB polarization field. We develop simulation tools for
predicting the polarization field in models that break statistical isotropy
locally through a modulation field. We study two different models: dipolar
modulation, invoked to explain the asymmetry in power between northern and
southern ecliptic hemispheres, and quadrupolar modulation, posited to explain
the alignments between the quadrupole and octopole. For the dipolar case, we
show that predictions for the correlation between the first 10 multipoles of
the temperature and polarization fields can typically be tested at better than
the 98% CL. For the quadrupolar case, we show that the polarization quadrupole
and octopole should be moderately aligned. Such an alignment is a generic
prediction of explanations which involve the temperature field at recombination
and thus discriminate against explanations involving foregrounds or local
secondary anisotropy. Predicted correlations between temperature and
polarization multipoles out to l = 5 provide tests at the ~ 99% CL or stronger
for quadrupolar models that make the temperature alignment more than a few
percent likely. As predictions of anomaly models, polarization statistics move
beyond the a posteriori inferences that currently dominate the field.
| [
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{
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"created": "Fri, 25 Apr 2008 21:51:55 GMT"
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] | 2008-12-18T00:00:00 | [
[
"Dvorkin",
"Cora",
"",
"U. Chicago"
],
[
"Peiris",
"Hiranya V.",
"",
"U. Chicago/Cambridge"
],
[
"Hu",
"Wayne",
"",
"U. Chicago"
]
] | [
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] |
711.2322 | Yoshiaki Koma | Yoshiaki Koma, Miho Koma, Hartmut Wittig | Relativistic corrections to the static potential at O(1/m) and O(1/m^2) | 10 pages, Talk presented at Lattice 2007 (Hadron spectroscopy) | PoSLAT2007:111,2007 | null | MKPH-T-07-15 | hep-lat hep-ph nucl-th | null | We investigate the relativistic corrections to the static potential, i.e. the
O(1/m) potential and the O(1/m^2) velocity-dependent potentials, in SU(3)
lattice gauge theory. They are important ingredients of potential
nonrelativistic QCD for heavy quarkonium. Utilizing the multi-level algorithm,
we obtain remarkably clean signals of these potentials up to r=0.9 fm. We
observe long range nonperturbative contributions to these corrections.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 00:14:22 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Koma",
"Yoshiaki",
""
],
[
"Koma",
"Miho",
""
],
[
"Wittig",
"Hartmut",
""
]
] | [
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711.2323 | Mitsusada M. Sano | Hiroyuki Tomita and Mitsusada M. Sano | Irreversible Circulation of Fluctuation and Entropy Production | 17pages, no figures, to appear in Progreess of Theoretical Physics,
Vol. 119, No.4 | null | 10.1143/PTP.119.515 | null | cond-mat.stat-mech | null | Physical and chemical stochastic processes described by the master equation
are investigated. In this paper, we examine the entropy production both for the
master equation and for the corresponding Fokker-Planck equation. For the
master equation, the exact expression of the entropy production was recently
derived by Gaspard using the Kolmogorov-Sinai entropy ({\em J.Stat.Phys.},
\textbf{117} (2004), 599; [Errata; \textbf{126} (2006), 1109 ]). Although
Gaspard's expression is derived from a stochastic consideration, it should be
noted that Gaspard's expression conincides with the thermodynamical expression.
For the corresponding Fokker-Planck equation, by using the detailed imbalance
relation which appears in the derivation process of the fluctuation theorem
through the Onsger-Machlup theory, the entropy production is expressed in terms
of the {\em irreversible circulation of fluctuation}, which was proposed by
Tomita and Tomita ({\em Prog.Theor.Phys.}, \textbf{51} (1974), 1731). However,
this expression for the corresponding Fokker-Planck equation differs from that
of the entropy production for the master equation. This discrepancy is due to
the difference between the master equation and the corresponding Fokker-Planck
equation, namely the former treats discrete events, but the latter equation is
an approximation of the former one. In fact, in the latter equation, the
original discrete events are smoothed out. To overcome this difficulty, we
propose the {\em path weight principle}. By using this principle, the modified
expression of the entropy production for the corresponding Fokker-Planck
equation coincides with that of the master equation (i.e., the thermodynamical
expression) for a simple chemical reaction system and a diffusion system.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 00:25:01 GMT"
},
{
"version": "v2",
"created": "Wed, 16 Apr 2008 04:56:22 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Tomita",
"Hiroyuki",
""
],
[
"Sano",
"Mitsusada M.",
""
]
] | [
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] |
711.2324 | Igor Belegradek | Igor Belegradek (Georgia Tech) | Rigidity and relative hyperbolicity of real hyperbolic hyperplane
complements | to appear in Pure and Applied Mathematics Quarterly in the special
issue in honor of Farrell and Jones | null | null | null | math.GR math.DG | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | For n>3 we study spaces obtained from finite volume complete real hyperbolic
n-manifolds by removing a compact totally geodesic submanifold of codimension
two. We prove that their fundamental groups are relative hyperbolic, co-Hopf,
biautomatic, residually hyperbolic, not K\"ahler, not isomorphic to lattices in
virtually connected real Lie groups, have no nontrivial subgroups with property
(T), have finite outer automorphism groups, satisfy Mostow-type Rigidity, have
finite asymptotic dimension and rapid decay property, and satisfy Baum-Connes
conjecture. We also characterize those lattices in real Lie groups that are
isomorphic to relatively hyperbolic groups.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 00:28:51 GMT"
},
{
"version": "v2",
"created": "Mon, 14 Jan 2008 19:46:02 GMT"
},
{
"version": "v3",
"created": "Wed, 24 Dec 2008 23:43:06 GMT"
},
{
"version": "v4",
"created": "Sat, 28 Aug 2010 13:04:29 GMT"
}
] | 2010-08-31T00:00:00 | [
[
"Belegradek",
"Igor",
"",
"Georgia Tech"
]
] | [
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] |
711.2325 | Sarah Morrison | S. Morrison, A.S. Parkins | Collective spin systems in dispersive optical cavity QED: Quantum phase
transitions and entanglement | 19 pages, 18 figures, shortened version | Phys. Rev. A 77, 043810 (2008) | 10.1103/PhysRevA.77.043810 | null | quant-ph cond-mat.other | null | We propose a cavity QED setup which implements a dissipative
Lipkin-Meshkov-Glick model -- an interacting collective spin system. By varying
the external model parameters the system can be made to undergo both first-and
second-order quantum phase transitions, which are signified by dramatic changes
in cavity output field properties, such as the probe laser transmission
spectrum. The steady-state entanglement between pairs of atoms is shown to peak
at the critical points and can be experimentally determined by suitable
measurements on the cavity output field. The entanglement dynamics also
exhibits pronounced variations in the vicinities of the phase transitions.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 00:40:43 GMT"
},
{
"version": "v2",
"created": "Wed, 7 May 2008 02:27:41 GMT"
}
] | 2008-05-07T00:00:00 | [
[
"Morrison",
"S.",
""
],
[
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""
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] |
711.2326 | Daniele Fargion | D.Fargion, M. Gaug, P.Oliva | Reflecting on Cherenkov reflections | 4 pages, 4 figures, HEP 2007: The 2007 Europhysics Conference on High
Energy Physics | J.Phys.Conf.Ser.110:062008,2008 | 10.1088/1742-6596/110/6/062008 | null | astro-ph | null | Magic Telescope may observe and reveal at horizons lights from air-shower
Cherenkov reflections. The ground, the sea, the cloudy sky (below the mountain)
may reflect PeVs-EeV UHECR Cherenkov lights observable by MAGIC telescopes.
Even rarest UHE neutrino skimming the atmosphere or skimming the Earth may
induce upward-horizontal airshowers: a new Neutrino Astronomy. These
fluorescence signals or the Cherenkov reflections in upper cloudy sky may flash
in correlated BL-Lac or GRB shining at opposite edges. Geomagnetic splitting of
Horizontal Air-showers may offer a new spectroscopy of UHECR from the knee up
to GZK energy edges.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 20:29:32 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Fargion",
"D.",
""
],
[
"Gaug",
"M.",
""
],
[
"Oliva",
"P.",
""
]
] | [
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] |
711.2327 | David Harrington | D. M. Harrington and J.R. Kuhn | Spectropolarimetric observations of Herbig Ae/Be Stars I: HiVIS
spectropolarimetric calibration and reduction techniques | 35 pages, 44 figures, Accepted by PASP | null | 10.1086/526549 | IfA-07-195 | astro-ph | null | Using the HiVIS spectropolarimeter built for the Haleakala 3.7m AEOS
telescope in Hawaii, we are collecting a large number of high precision
spectropolarimetrc observations of stars. In order to precisely measure very
small polarization changes, we have performed a number of polarization
calibration techniques on the AEOS telescope and HiVIS spectrograph. We have
extended our dedicated IDL reduction package and have performed some hardware
upgrades to the instrument. We have also used the ESPaDOnS spectropolarimeter
on CFHT to verify the HiVIS results with back-to-back observations of MWC 361
and HD163296. Comparision of this and other HiVIS data with stellar
observations from the ISIS and WW spectropolarimeters in the literature further
shows the usefulness of this instrument.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 00:52:58 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Harrington",
"D. M.",
""
],
[
"Kuhn",
"J. R.",
""
]
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] |
711.2328 | Hiroki Takesue | Hiroki Takesue, Yasuhiro Tokura, Hiroshi Fukuda, Tai Tsuchizawa,
Toshifumi Watanabe, Koji Yamada, and Sei-ichi Itabashi | Entanglement generation using silicon wire waveguide | 8 pages, 3 figures. A part of this content was presented at Eur.
Conf. Opt. Commun. ECOC 2007, postdeadline paper 2.3, September 20, 2007,
Berlin | Appl. Phys. Lett. 91, 201108 (2007) | 10.1063/1.2814040 | null | quant-ph | null | We report the first entanglement generation experiment that utilizes a
silicon waveguide. Using spontaneous four-wave mixing in a 1.09-cm-long silicon
wire waveguide, we generated 1.5-um, high-purity time-bin entangled photons
without temperature control, and observed a two-photon interference fringe with
>73% visibility.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 01:15:19 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Takesue",
"Hiroki",
""
],
[
"Tokura",
"Yasuhiro",
""
],
[
"Fukuda",
"Hiroshi",
""
],
[
"Tsuchizawa",
"Tai",
""
],
[
"Watanabe",
"Toshifumi",
""
],
[
"Yamada",
"Koji",
""
],
[
"Itabashi",
"Sei-ichi",
""
]
] | [
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] |
711.2329 | Sumanta Tewari | Sumanta Tewari, Chuanwei Zhang, Victor M. Yakovenko, S. Das Sarma | Time-reversal symmetry breaking by a $(d+id)$ density-wave state in
underdoped cuprate superconductors | 4 pages, 3 eps figures; minor typos corrected, references updated,
new title as suggested by the PRL editor; references updated, final version
as published in PRL | Phys. Rev. Lett. 100, 217004 (2008) | 10.1103/PhysRevLett.100.217004 | null | cond-mat.str-el | null | It was proposed that the $id_{x^2-y^2}$ density-wave state (DDW) may be
responsible for the pseudogap behavior in the underdoped cuprates. Here we show
that the admixture of a small $d_{xy}$ component to the DDW state breaks the
symmetry between the counter-propagating orbital currents of the DDW state and,
thus, violates the macroscopic time-reversal symmetry. This symmetry breaking
results in a non-zero polar Kerr effect, which has recently been observed in
the pseudogap phase.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 15:59:00 GMT"
},
{
"version": "v2",
"created": "Tue, 20 Nov 2007 17:17:16 GMT"
},
{
"version": "v3",
"created": "Wed, 4 Jun 2008 00:29:05 GMT"
}
] | 2008-06-04T00:00:00 | [
[
"Tewari",
"Sumanta",
""
],
[
"Zhang",
"Chuanwei",
""
],
[
"Yakovenko",
"Victor M.",
""
],
[
"Sarma",
"S. Das",
""
]
] | [
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] |
711.233 | Hiromi Saida | Hiromi Saida | Black Hole Evaporation and Generalized 2nd Law with Nonequilibrium
Thermodynamics | Typo is corrected. 10 pages, 2 figures. Based on proceedings and
talks given at: APCTP Jeju Meeting on Gravitation and Cosmology (Jeju, Korea,
2007), Dynamics and Thermodynamics of Black Holes and Naked Singularities II,
(Politecnico di Milano, Italy, 2007) and 16th General Relativity and
Gravitation (Niigata, Japan, 2006) | null | null | null | gr-qc | null | In general, when a black hole evaporates, there arises a net energy flow from
black hole into its outside environment due to Hawking radiation and energy
accretion onto black hole. The existence of energy flow means that the
thermodynamic state of the whole system, which consists of a black hole and its
environment, is in a nonequilibrium state. To know the detail of evaporation
process, the nonequilibrium effects of energy flow should be taken into
account. The nonequilibrium nature of black hole evaporation is a challenging
topic including issues of not only black hole physics but also nonequilibrium
physics. Using the nonequilibrium thermodynamics which has been formulated
recently, this report shows: (1) the self-gravitational effect of black hole
which appears as its negative heat capacity guarantees the validity of
generalized 2nd law without entropy production inside the outside environment,
(2) the nonequilibrium effect of energy flow tends to shorten the evaporation
time (life time) of black hole, and consequently specific nonequilibrium
phenomena are suggested. Finally a future direction of this study is commented.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 02:25:37 GMT"
},
{
"version": "v2",
"created": "Fri, 16 Nov 2007 03:39:06 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Saida",
"Hiromi",
""
]
] | [
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] |
711.2331 | Artem Sabourov | A.V. Sabourov, M.I. Pravdin and S.P. Knurenko | A shape of charged particle lateral distribution in individual EAS
events with energy above 10^19 eV arriving from different celestial regions | 5 pages, 4 figures | null | null | null | astro-ph | null | A shape of lateral distribution for charged particles in events with energy
above 10^19eV is considered. Two methods were used for individual LDF
parametrization. In the first approach, the index of power was determined for
generalized Greisen-Linsley approximation. In second, mean square radius of the
shower was determined for approximation proposed by Lagutin et al. Comparison
of resulted parameters is presented for individual events arrived from
different celestial regions -- Galactic planes and the region with increased
flux of particles with E(0)>=10^19eV (according to Yakutsk array): 1.7h-3.7h
right ascension; 45-60 degrees declination.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 03:19:11 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Sabourov",
"A. V.",
""
],
[
"Pravdin",
"M. I.",
""
],
[
"Knurenko",
"S. P.",
""
]
] | [
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] |
711.2332 | Anton Knigavko | Igor V. Mel'nikov, Anton Knigavko, J. Stewart Aitchison, and Clark A.
Merchant | Generation of slow intense optical solitons in a resonance photonic
crystal | null | null | 10.1140/epjst/e2007-00733-8 | null | physics.optics | null | We demonstrate interesting and previously unforeseen properties of a pair of
gap solitons in a resonant photonic crystal which are predicted and explained
in a physically transparent form using both analytical and numerical methods.
The most important result is the fact that an oscillating gap soliton created
by the presence of a localized population inversion inside the crystal can be
manipulated by means of a proper choice of bit rate, phase and amplitude
modulation. Developing this idea, we are able to obtain qualitatively different
regimes of a resonant photonic crystal operation. In particular, a noteworthy
observation is that both the delay time and amplitude difference must exceed a
certain level to ensure effective control over the soliton dynamics.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 03:34:18 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Mel'nikov",
"Igor V.",
""
],
[
"Knigavko",
"Anton",
""
],
[
"Aitchison",
"J. Stewart",
""
],
[
"Merchant",
"Clark A.",
""
]
] | [
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] |
711.2333 | Christopher J. Conselice | Christopher J. Conselice, Sheena Rajgor, Robert Myers (Nottingham) | The Structures of Distant Galaxies I: Galaxy Structures and the Merger
Rate to z~3 in the Hubble Ultra-Deep Field | MNRAS, submitted | null | 10.1111/j.1365-2966.2008.13069.x | null | astro-ph | null | This paper begins a series in which we examine the structures of distant
galaxies to directly determine the history of their formation modes. We start
this series by examining the structures of z_F850LP < 27 galaxies in the Hubble
Ultra-Deep field, the deepest high-resolution optical image taken to date. We
investigate a few basic features of galaxy structure using this image. These
include: (1) The agreement of visual eye-ball classifications and
non-parametric quantitative (CAS, Gini/M_20) methods; (2) How distant galaxy
quantitative structures can vary as a function of rest-frame wavelength; and
(3) The evolution of distant galaxy structures up to z~3. One of our major
conclusions is that the majority of galaxies with z_850 < 27 are peculiar in
appearance, and that galaxy assembly is rapidly occurring at these magnitudes,
even up to the present time. We find a general agreement between galaxy
classification by eye and through quantitative methods, as well as a general
agreement between the CAS and the Gini/M_20 parameters. We find that the
Gini/M_20 method appears to find a larger number of galaxy mergers than the CAS
system, but contains a larger contamination from non-mergers. We furthermore
calculate the merger rate of galaxies in the UDF up to z~3, finding an increase
with redshift as well as stellar mass, confirming previous work in the Hubble
Deep Field. We find that massive galaxies with M_{*} > 10^10 M_0 undergo
4.3_+0.8^-0.8 major galaxy mergers at z < 3, with all of this merging occurring
at z > 1.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 03:52:39 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Conselice",
"Christopher J.",
"",
"Nottingham"
],
[
"Rajgor",
"Sheena",
"",
"Nottingham"
],
[
"Myers",
"Robert",
"",
"Nottingham"
]
] | [
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] |
711.2334 | Zoran \v{S}uni\'c | Titu Andreescu and Zoran Sunic | Encouraging the grand coalition in convex cooperative games | null | null | null | null | math.OC | null | A solution function for convex transferable utility games encourages the
grand coalition if no player prefers (in a precise sense defined in the text)
any coalition to the grand coalition. We show that the Shapley value encourages
the grand coalition in all convex games and the tau-value encourages the grand
coalitions in convex games up to three (but not more than three) players.
Solution functions that encourage the grand coalition in convex games always
produce allocations in the core, but the converse is not necessarily true.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 04:13:49 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Andreescu",
"Titu",
""
],
[
"Sunic",
"Zoran",
""
]
] | [
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] |
711.2335 | Bo-Qiang Ma | Bo-Qiang Ma | Melosh rotation: source of the proton's missing spin | 5 latex pages | J.Phys.G17:L53-L58,1991 | 10.1088/0954-3899/17/5/001 | null | hep-ph | null | It is shown that the observed small value of the integrated spin structure
function for protons could be naturally understood within the naive quark model
by considering the effect from Melosh rotation. The key to this problem lies in
the fact that the deep inelastic process probes the light-cone quarks rather
than the instant-form quarks, and that the spin of the proton is the sum of the
Melosh rotated light-cone spin of the individual quarks rather than simply the
sum of the light-cone spin of the quarks directly.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 04:22:59 GMT"
}
] | 2010-04-15T00:00:00 | [
[
"Ma",
"Bo-Qiang",
""
]
] | [
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-0.0678418577,
-0.0201829523,
0.0007978485,
0.0344184339,
0.0896869302,
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0.0199907329,
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] |
711.2336 | Yasuo Yoshida | Yasuo Yoshida, Tatsuya Kawae, Yuko Hosokoshi, Katsuya Inoue, Nobuya
Maeshima, Koichi Okunishi, Kiyomi Okamoto, and Toru Sakai | Magnetic Field versus Temperature Phase Diagram of the Spin-1/2
Alternating Chain Compound F5PNN | 5 pages, 5 figures (Submitted to Physical Review B) | null | null | null | cond-mat.str-el | null | We have measured the specific heat of the S = 1/2 alternating Heisenberg
antiferromagnetic chain compound pentafluorophenyl nitronyl nitroxide in
magnetic fields using a single crystal and powder. A sharp peak due to
field-induced magnetic ordering (FIMO) is observed in both samples. The H-T
phase boundary of the FIMO of the single crystal is symmetric with respect to
the central field of the gapless field region HC1 < H < HC2, whereas it is
distorted for the powder whose ordering temperatures are lower. An analysis
employing calculations based on the finite temperature density matrix
renormalization group indicates the possibility of novel incommensurate
ordering due to frustration in the powder around the central field.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 05:12:06 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Yoshida",
"Yasuo",
""
],
[
"Kawae",
"Tatsuya",
""
],
[
"Hosokoshi",
"Yuko",
""
],
[
"Inoue",
"Katsuya",
""
],
[
"Maeshima",
"Nobuya",
""
],
[
"Okunishi",
"Koichi",
""
],
[
"Okamoto",
"Kiyomi",
""
],
[
"Sakai",
"Toru",
""
]
] | [
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] |
711.2337 | Stefan C. Keller | Stefan C. Keller, Simon Murphy, Sayuri Prior, Gary DaCosta, and Brian
Schmidt | Revealing Substructure in the Galactic Halo - The SEKBO RR Lyrae Survey | 59 pages, 21 figures. ApJ accepted | null | 10.1086/526516 | null | astro-ph | null | We present a search for RR Lyrae variable stars from archival observations of
the Southern Edgeworth-Kuiper Belt Object survey. The survey covers 1675 square
degrees along the ecliptic to a mean depth of V=19.5, i.e. a heliocentric
distance of ~50kpc for RR Lyrae stars. The survey reveals 2016 RR Lyrae
candidates. Follow-up photometric monitoring of a subset of these candidates
shows (24+/-12)% contamination by non-RR Lyrae variables. We derive a map of
over-density of RR Lyraes in the halo that reveals a series of structures
coincident with the leading and trailing arms of debris from the Sagittarius
dwarf galaxy. One of the regions of over-density is found on the trailing arm,
200 deg. from the main body of the Sagittarius dwarf at a distance of ~45kpc.
This distant detection of the stellar population of the outer trailing arm of
Sagittarius offers a tight constraint on the motion of the dwarf galaxy. A
distinctly separate region of over-density is seen towards the Virgo Over
Density.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 05:32:53 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Keller",
"Stefan C.",
""
],
[
"Murphy",
"Simon",
""
],
[
"Prior",
"Sayuri",
""
],
[
"DaCosta",
"Gary",
""
],
[
"Schmidt",
"Brian",
""
]
] | [
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] |
711.2338 | Sergey Golovin | Sergey V. Golovin | On the hierarchy of partially invariant submodels of differential
equations | null | J. Phys. A: Math. Theor. 2008 41 265501 | 10.1088/1751-8113/41/26/265501 | null | math-ph math.MP | null | It is noticed, that partially invariant solution (PIS) of differential
equations in many cases can be represented as an invariant reduction of some
PIS of the higher rank. This introduce a hierarchic structure in the set of all
PISs of a given system of differential equations. By using this structure one
can significantly decrease an amount of calculations required in enumeration of
all PISs for a given system of partially differential equations. An equivalence
of the two-step and the direct ways of construction of PISs is proved. In this
framework the complete classification of regular partially invariant solutions
of ideal MHD equations is given.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 05:20:51 GMT"
}
] | 2010-08-05T00:00:00 | [
[
"Golovin",
"Sergey V.",
""
]
] | [
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0.0317397788,
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] |
711.2339 | Teruhisa Baba | T. Baba, T. Yokoya, S. Tsuda, T. Kiss, T. Shimojima, K. Ishizaka, H.
Takeya, K. Hirata, T. Watanabe, M. Nohara, H. Takagi, N. Nakai, K. Machida,
T. Togashi, S. Watanabe, X.-Y. Wang, C. T. Chen, S. Shin | Bulk electronic structure of the antiferromagnetic superconducting phase
in ErNi2B2C | 11 pages, 4 figures | Phys. Rev. Lett. 100, 017003 (2008) | 10.1103/PhysRevLett.100.017003 | null | cond-mat.supr-con | null | We have performed temperature (T) - dependent laser-photoemission
spectroscopy of antiferromagnetic (AF) superconductor ErNi2B2C to study the
electronic-structure evolution reflecting the interplay between
antiferromagnetism and superconductivity. The spectra at the superconducting
(SC) phase show a very broad spectral shape. T-dependent SC gap shows a sudden
deviation from the BCS prediction just below TN. This observation can be well
explained by the theoretical model and thus represents characteristic bulk
electronic structure of the AF SC phase for the first time.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 05:25:24 GMT"
},
{
"version": "v2",
"created": "Fri, 11 Jan 2008 05:35:17 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Baba",
"T.",
""
],
[
"Yokoya",
"T.",
""
],
[
"Tsuda",
"S.",
""
],
[
"Kiss",
"T.",
""
],
[
"Shimojima",
"T.",
""
],
[
"Ishizaka",
"K.",
""
],
[
"Takeya",
"H.",
""
],
[
"Hirata",
"K.",
""
],
[
"Watanabe",
"T.",
""
],
[
"Nohara",
"M.",
""
],
[
"Takagi",
"H.",
""
],
[
"Nakai",
"N.",
""
],
[
"Machida",
"K.",
""
],
[
"Togashi",
"T.",
""
],
[
"Watanabe",
"S.",
""
],
[
"Wang",
"X. -Y.",
""
],
[
"Chen",
"C. T.",
""
],
[
"Shin",
"S.",
""
]
] | [
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] |
711.234 | Felipe Cervantes-Sodi | F. Cervantes-Sodi, G. Cs\'anyi, S. Piscanec, A. C. Ferrari | Edge-functionalized and substitutional doped graphene nanoribbons:
electronic and spin properties | 12 pages, 5 figures | Phys. Rev. B 77, 165427 (2008) | 10.1103/PhysRevB.77.165427 | null | cond-mat.mtrl-sci | null | Graphene nanoribbons are the counterpart of carbon nanotubes in
graphene-based nanoelectronics. We investigate the electronic properties of
chemically modified ribbons by means of density functional theory. We observe
that chemical modifications of zigzag ribbons can break the spin degeneracy.
This promotes the onset of a semiconducting-metal transition, or of an
half-semiconducting state, with the two spin channels having a different
bandgap, or of a spin-polarized half-semiconducting state -where the spins in
the valence and conduction bands are oppositely polarized. Edge
functionalization of armchair ribbons gives electronic states a few eV away
from the Fermi level, and does not significantly affect their bandgap. N and B
produce different effects, depending on the position of the substitutional
site. In particular, edge substitutions at low density do not significantly
alter the bandgap, while bulk substitution promotes the onset of
semiconducting-metal transitions. Pyridine-like defects induce a
semiconducting-metal transition.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 17:31:30 GMT"
}
] | 2009-09-29T00:00:00 | [
[
"Cervantes-Sodi",
"F.",
""
],
[
"Csányi",
"G.",
""
],
[
"Piscanec",
"S.",
""
],
[
"Ferrari",
"A. C.",
""
]
] | [
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] |
711.2341 | Nikodem Poplawski | Nikodem J. Poplawski | Conservation laws for a general Lorentz connection | 7 pages | null | null | null | gr-qc math-ph math.MP | null | We derive conservation laws for energy-momentum (canonical and dynamical) and
angular momentum for a general Lorentz connection.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 06:00:00 GMT"
}
] | 2008-01-03T00:00:00 | [
[
"Poplawski",
"Nikodem J.",
""
]
] | [
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] |
711.2342 | Shunsuke Takagi | Shunsuke Takagi | Adjoint ideals along closed subvarieties of higher codimension | 17 pages; v.2: minor changes, to appear in Crelles Journal | null | null | null | math.AG math.AC | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper, we introduce a notion of adjoint ideal sheaves along closed
subvarieties of higher codimension and study its local properties using
characteristic $p$ methods. When $X$ is a normal Gorenstein closed subvariety
of a smooth complex variety $A$, we formulate a restriction property of the
adjoint ideal sheaf $\adj_X(A)$ of $A$ along $X$ involving the l.c.i. ideal
sheaf $\mathcal{D}_X$ of $X$. The proof relies on a modification of generalized
test ideals of Hara and Yoshida.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 05:39:51 GMT"
},
{
"version": "v2",
"created": "Wed, 17 Dec 2008 09:03:46 GMT"
}
] | 2008-12-17T00:00:00 | [
[
"Takagi",
"Shunsuke",
""
]
] | [
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] |
711.2343 | Mohan Sarovar | Mohan Sarovar, Kevin C. Young, Thomas Schenkel, and K. Birgitta Whaley | Quantum non-demolition measurements of single donor spins in
semiconductors | 8+ pages. 4 figures. Published version | Phys. Rev. B, 78, 245302 (2008) | 10.1103/PhysRevB.78.245302 | null | cond-mat.mes-hall quant-ph | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We propose a technique for measuring the state of a single donor electron
spin using a field-effect transistor induced two-dimensional electron gas and
electrically detected magnetic resonance techniques. The scheme is facilitated
by hyperfine coupling to the donor nucleus. We analyze the potential
sensitivity and outline experimental requirements. Our measurement provides a
single-shot, projective, and quantum non-demolition measurement of an
electron-encoded qubit state.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 06:08:35 GMT"
},
{
"version": "v2",
"created": "Wed, 11 Jun 2008 16:59:50 GMT"
},
{
"version": "v3",
"created": "Mon, 5 Jan 2009 03:38:28 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Sarovar",
"Mohan",
""
],
[
"Young",
"Kevin C.",
""
],
[
"Schenkel",
"Thomas",
""
],
[
"Whaley",
"K. Birgitta",
""
]
] | [
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] |
711.2344 | Morbidelli Alessandro | Alessandro Morbidelli (OCA), Aurelien Crida, Frederic Masset, Richard
P. Nelson | Building Giant-Planet Cores at a Planet Trap | in press in Astronomy and Astrophysics | null | 10.1051/0004-6361:20078546 | null | astro-ph | null | A well-known bottleneck for the core-accretion model of giant-planet
formation is the loss of the cores into the star by Type-I migration, due to
the tidal interactions with the gas disk. It has been shown that a steep
surface-density gradient in the disk, such as the one expected at the boundary
between an active and a dead zone, acts as a planet trap and prevents isolated
cores from migrating down to the central star. We study the relevance of the
planet trap concept for the accretion and evolution of systems of multiple
planetary embryos/cores. We performed hydrodynamical simulations of the
evolution of systems of multiple massive objects in the vicinity of a planet
trap. The planetary embryos evolve in 3 dimensions, whereas the disk is modeled
with a 2D grid. Synthetic forces are applied onto the embryos to mimic the
damping effect that the disk has on their inclinations. Systems with two
embryos tend to acquire stable, separated and non-migrating orbits, with the
more massive embryo placed at the planet trap and the lighter one farther out
in the disk. Systems of multiple embryos are intrinsically unstable.
Consequently, a long phase of mutual scattering can lead to accreting
collisions among embryos; some embryos are injected into the inner part of the
disk, where they can be evacuated into the star by Type I migration. The system
can resume a stable, non-migrating configuration only when the number of
surviving embryos decreases to a small value (~2-4). This can explain the
limited number of giant planets in our solar system. These results should apply
in general to any case in which the Type-I migration of the inner embryo is
prevented by some mechanism, and not solely to the planet trap scenario.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 06:10:00 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Morbidelli",
"Alessandro",
"",
"OCA"
],
[
"Crida",
"Aurelien",
""
],
[
"Masset",
"Frederic",
""
],
[
"Nelson",
"Richard P.",
""
]
] | [
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] |
711.2345 | Anne-Laure Fougeres | Anne-Laure Foug\`eres (MODAL'X), John P. Nolan, Holger Rootz\'en | Models for dependent extremes using stable mixtures | null | Scandinavian Journal of Statistics 36 (2009) 42-59 | 10.1111/j.1467-9469.2008.00613.x | null | stat.ME math.ST stat.TH | null | This paper unifies and extends results on a class of multivariate Extreme
Value (EV) models studied by Hougaard, Crowder, and Tawn. In these models both
unconditional and conditional distributions are EV, and all lower-dimensional
marginals and maxima belong to the class. This leads to substantial economies
of understanding, analysis and prediction. One interpretation of the models is
as size mixtures of EV distributions, where the mixing is by positive stable
distributions. A second interpretation is as exponential-stable location
mixtures (for Gumbel) or as power-stable scale mixtures (for non-Gumbel EV
distributions). A third interpretation is through a Peaks over Thresholds model
with a positive stable intensity. The mixing variables are used as a modeling
tool and for better understanding and model checking. We study extreme value
analogues of components of variance models, and new time series, spatial, and
continuous parameter models for extreme values. The results are applied to data
from a pitting corrosion investigation.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 06:13:08 GMT"
}
] | 2013-09-30T00:00:00 | [
[
"Fougères",
"Anne-Laure",
"",
"MODAL'X"
],
[
"Nolan",
"John P.",
""
],
[
"Rootzén",
"Holger",
""
]
] | [
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] |
711.2346 | Emma Jin | Emma Y. Jin and Christian M. Reidys | $k$-noncrossing RNA structures with arc-length $\ge 3$ | 17 pages, 4 figures | null | null | null | q-bio.BM | null | In this paper we enumerate $k$-noncrossing RNA pseudoknot structures with
given minimum arc- and stack-length. That is, we study the numbers of RNA
pseudoknot structures with arc-length $\ge 3$, stack-length $\ge \sigma$ and in
which there are at most $k-1$ mutually crossing bonds, denoted by ${\sf
T}_{k,\sigma}^{[3]}(n)$. In particular we prove that the numbers of 3, 4 and
5-noncrossing RNA structures with arc-length $\ge 3$ and stack-length $\ge 2$
satisfy ${\sf T}_{3,2}^{[3]}(n)^{}\sim K_3 n^{-5} 2.5723^n$, ${\sf
T}^{[3]}_{4,2}(n)\sim K_4 n^{-{21/2}} 3.0306^n$, and ${\sf
T}^{[3]}_{5,2}(n)\sim K_5 n^{-18} 3.4092^n$, respectively, where $K_3,K_4,K_5$
are constants. Our results are of importance for prediction algorithms for RNA
pseudoknot structures.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 06:34:09 GMT"
},
{
"version": "v2",
"created": "Tue, 4 Dec 2007 09:37:37 GMT"
}
] | 2007-12-04T00:00:00 | [
[
"Jin",
"Emma Y.",
""
],
[
"Reidys",
"Christian M.",
""
]
] | [
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] |
711.2347 | Dr. Alok Banerjee | A. Banerjee, Kranti Kumar and P. Chaddah | Recrystallization of glass: homogeneous vs. heterogeneous nucleation in
La(0.5)Ca(0.5)MnO3 | null | null | null | null | cond-mat.str-el cond-mat.mtrl-sci cond-mat.stat-mech | null | We probe through magnetization and resistivity measurements a kinetically
arrested glass-like but long-range ordered magnetic state. The transformation
kinetics of the magnetic field-temperature induced broad first-order transition
from ferromagnetic-metallic (FMM) to antiferromagnetic-insulating (AFI) state
gets hindered at low temperature in a La(0.5)Ca(0.5)MnO3 sample. A fraction of
high-temperature FMM phase persists to the lowest temperature, albeit as a
non-ergodic state. We present a phenomenology for this glass-like but
long-range order FMM phase which devitrifies on heating and converts to
equilibrium AFI phase. The residual kinetically arrested FMM phase can be
`recrystallized' to AFI state by annealing and more efficiently by successive
annealing, presumably by heterogeneous nucleation. This glass-like state shows
a stimulating feature that when the fraction of glass is larger the
`recrystallization' is easier.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 14:01:05 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Banerjee",
"A.",
""
],
[
"Kumar",
"Kranti",
""
],
[
"Chaddah",
"P.",
""
]
] | [
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] |
711.2348 | Artem Sabourov | S.P. Knurenko, A.A. Ivanov, A.V. Sabourov and I.Ye. Sleptsov | Average mass composition of primary cosmic rays in the superhigh energy
region by Yakutsk complex EAS array data | 5 pages, 2 figures | null | null | null | astro-ph | null | The characteristics relating to the lateral and longitudinal development of
EAS in the energy region of 10^15-10^19eV have been analyzed in the framework
of the QGSJET model and of mass composition of primary cosmic rays. It is found
that at E(0) >= 5*10^15eV the mean mass composition of primary cosmic rays
begins to vary as indicated by a rise of <ln A> with increasing energy. The
maximum value of <ln A> is observed at E(0) ~ (5-50)*10^16eV. It is confirmed
by data of many compact EAS arrays and does not contradict an anomalous
diffusion model of cosmic ray propagation in our Galaxy. In the superhigh
energy region (>=10^18eV) the value <ln A> begins to decrease, i.e. the mass
composition becomes lighter and consists of protons and nuclei of He and C. It
does not contradict our earlier estimations for the mass composition and points
to a growing role of the metagalactic component of cosmic rays in the superhigh
energy region.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 06:50:43 GMT"
},
{
"version": "v2",
"created": "Mon, 19 Nov 2007 01:42:12 GMT"
}
] | 2007-11-19T00:00:00 | [
[
"Knurenko",
"S. P.",
""
],
[
"Ivanov",
"A. A.",
""
],
[
"Sabourov",
"A. V.",
""
],
[
"Sleptsov",
"I. Ye.",
""
]
] | [
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] |
711.2349 | Samuel M\"uller | Samuel Mueller, A.H. Welsh | Robust model selection in generalized linear models | 24 pages, 1 figure, submitted to JASA | null | null | null | stat.ME | null | In this paper, we extend to generalized linear models (including logistic and
other binary regression models, Poisson regression and gamma regression models)
the robust model selection methodology developed by Mueller and Welsh (2005;
JASA) for linear regression models. As in Mueller and Welsh (2005), we combine
a robust penalized measure of fit to the sample with a robust measure of out of
sample predictive ability which is estimated using a post-stratified m-out-of-n
bootstrap. A key idea is that the method can be used to compare different
estimators (robust and nonrobust) as well as different models. Even when
specialized back to linear regression models, the methodology presented in this
paper improves on that of Mueller and Welsh (2005). In particular, we use a new
bias-adjusted bootstrap estimator which avoids the need to centre the
explanatory variables and to include an intercept in every model. We also use
more sophisticated arguments than Mueller and Welsh (2005) to establish an
essential monotonicity condition.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 06:56:50 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Mueller",
"Samuel",
""
],
[
"Welsh",
"A. H.",
""
]
] | [
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] |
711.235 | Joel Hass | Joel Hass and Tahl Nowik | Unknot diagrams requiring a quadratic number of Reidemeister moves to
untangle | null | null | null | null | math.GT | null | We present a sequence of diagrams of the unknot for which the minimum number
of Reidemeister moves required to pass to the trivial diagram is quadratic with
respect to the number of crossings. These bounds apply both in $S^2$ and in
$\R^2$.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 06:58:57 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Hass",
"Joel",
""
],
[
"Nowik",
"Tahl",
""
]
] | [
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] |
711.2351 | Dan Butnariu | Dan Butnariu, Gabor Kassay | A Proximal-Projection Method for Finding Zeros of Set-Valued Operators | 38 pages | null | null | null | nlin.SI | null | In this paper we study the convergence of an iterative algorithm for finding
zeros with constraints for not necessarily monotone set-valued operators in a
reflexive Banach space. This algorithm, which we call the proximal-projection
method is, essentially, a fixed point procedure and our convergence results are
based on new generalizations of Lemma Opial. We show how the
proximal-projection method can be applied for solving ill-posed variational
inequalities and convex optimization problems with data given or computable by
approximations only. The convergence properties of the proximal-projection
method we establish also allow us to prove that the proximal point method (with
Bregman distances), whose convergence was known to happen for maximal monotone
operators, still converges when the operator involved in it is monotone with
sequentially weakly closed graph.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 07:18:11 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Butnariu",
"Dan",
""
],
[
"Kassay",
"Gabor",
""
]
] | [
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] |
711.2352 | Carey Lisse | Carey Lisse, Mark Sykes, David Trilling, Josh Emery, Yanga Fernandez,
Heidi Hammel, Bidushi Bhattacharya, Erin Ryan, John Stansberry | Planetary Science Goals for the Spitzer Warm Era | 29 pages, 17 figures, to appear in "Science Opportunities for the
Warm Spitzer Mission" | null | 10.1063/1.2806779 | null | astro-ph | null | The overarching goal of planetary astronomy is to deduce how the present
collection of objects found in our Solar System were formed from the original
material present in the proto-solar nebula. As over two hundred exo-planetary
systems are now known, and multitudes more are expected, the Solar System
represents the closest and best system which we can study, and the only one in
which we can clearly resolve individual bodies other than planets. In this
White Paper we demonstrate how to use Spitzer Space Telescope InfraRed Array
Camera Channels 1 and 2 (3.6 and 4.5 um) imaging photometry with large
dedicated surveys to advance our knowledge of Solar System formation and
evolution. There are a number of vital, key projects to be pursued using
dedicated large programs that have not been pursued during the five years of
Spitzer cold operations. We present a number of the largest and most important
projects here; more will certainly be proposed once the warm era has begun,
including important observations of newly discovered objects.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 07:28:16 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Lisse",
"Carey",
""
],
[
"Sykes",
"Mark",
""
],
[
"Trilling",
"David",
""
],
[
"Emery",
"Josh",
""
],
[
"Fernandez",
"Yanga",
""
],
[
"Hammel",
"Heidi",
""
],
[
"Bhattacharya",
"Bidushi",
""
],
[
"Ryan",
"Erin",
""
],
[
"Stansberry",
"John",
""
]
] | [
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] |
711.2353 | Bhola Dwivedi | K.A.P. Singh, R. Erdelyi, and B.N. Dwivedi | Effect of the steady flow on spatial damping of small-amplitude
prominence oscillations | 17 pages; 6 figures, Submitted in A&A | null | null | null | astro-ph | null | Aims. Taking account of steady flow in solar prominences, we study its
effects on spatial damping of small-amplitude non-adiabatic magnetoacoustic
waves in a homogeneous, isothermal, and unbounded prominence plasma. Methods.
We model the typical feature of observed damped oscillatory motion in
prominences, removing the adiabaticity assumption through thermal conduction,
radiation and heating. Invoking steady flow in MHD equations, we linearise them
under small-amplitude approximation and obtain a new general dispersion
relation for linear non-adiabatic magnetoacoustic waves in prominences Results.
The presence of steady flow breaks the symmetry of forward and backward
propagating MHD wave modes in prominences. The steady flow has dramatic
influence on the propagation and damping of magnetoacoustic and thermal waves.
Depending upon the direction and strength of flow the magnetoacoustic and
thermal modes can show both the features of wave amplification and damping. At
the wave period of 5 min where the photospheric power is maximum, the slow mode
shows wave amplification. However, in the absence of steady flow the slow mode
wave shows damping. Conclusions. For the wave period between 5 min and 15 min,
the amplification length for slow mode, in the case of prominence regime 1.1,
varies between 3.4*10^11 m to 2*10^12 m. Dramatic influence of steady flow on
small-amplitude prominence oscillations is likely to play an important role in
both wave detection and prominence seismology.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 07:51:54 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Singh",
"K. A. P.",
""
],
[
"Erdelyi",
"R.",
""
],
[
"Dwivedi",
"B. N.",
""
]
] | [
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] |
711.2354 | Svetlana Roudenko | Lars Diening, Peter H\"ast\"o and Svetlana Roudenko | Function spaces of variable smoothness and integrability | null | null | null | null | math.CA | null | In this article we introduce Triebel--Lizorkin spaces with variable
smoothness and integrability. Our new scale covers spaces with variable
exponent as well as spaces of variable smoothness that have been studied in
recent years. Vector-valued maximal inequalities do not work in the generality
which we pursue, and an alternate approach is thus developed. Applying it, we
give molecular and atomic decomposition results and show that our space is
well-defined, i.e., independent of the choice of basis functions.
As in the classical case, a unified scale of spaces permits clearer results
in cases where smoothness and integrability interact, such as Sobolev embedding
and trace theorems. As an application of our decomposition, we prove optimal
trace theorems in the variable indices case.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 07:59:57 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Diening",
"Lars",
""
],
[
"Hästö",
"Peter",
""
],
[
"Roudenko",
"Svetlana",
""
]
] | [
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] |
711.2355 | Selcuk Bilir | S. Karaali, S. Bilir, E. Yaz, E. Hamzaoglu, R. Buser | Volume limited dependent Galactic model parameters | 12 pages, including 8 figures and 5 tables, accepted for publication
in PASA | null | 10.1071/AS07006 | null | astro-ph | null | We estimated 34 sets of Galactic model parameters for three intermediate
latitude fields with Galactic longitudes l=60, l=90, and l=180, and we
discussed their dependence on the volume. Also, we confirmed the variation of
these parameters with absolute magnitude and Galactic longitude. The star
samples in two fields are restricted with bright and unit absolute magnitude
intervals, (4,5], and (5,6], whereas for the third field a larger absolute
magnitude interval is adopted, (4,10]. The limiting apparent magnitudes of star
samples are g=15 and g=22.5 mag which provide space densities within distances
in the line of sight 0.9 and 25 kpc. The Galactic model parameters for the thin
disc are not volume dependent. However, the ones for thick disc and halo do
show spectacular trends in their variations with volume, except for the
scalelength of the thick disc. The local space density of the thick disc
increases, whereas the scaleheight of the same Galactic component decreases
monotonically. However, both model parameters approach asymptotic values at
large distances. The axial ratio of the halo increases abruptly for the volumes
where thick disc is dominant, whereas it approaches an asymptotic value
gradually for larger volumes, indicating a continuous transition from disclike
structure to a spherical one at the outermost region of the Galaxy. The
variation of the Galactic model parameters with absolute magnitude can be
explained by their dependence on the stellar luminosity, whereas the variation
with volume and Galactic longitude at short distances is a bias in analysis.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 08:02:52 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Karaali",
"S.",
""
],
[
"Bilir",
"S.",
""
],
[
"Yaz",
"E.",
""
],
[
"Hamzaoglu",
"E.",
""
],
[
"Buser",
"R.",
""
]
] | [
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] |
711.2356 | Anna Lytova | J. L. Lebowitz, A. Lytova, L. Pastur | On a Random Matrix Models of Quantum Relaxation | 21 pages | null | null | null | math-ph math.MP | null | Earlier two of us (J.L. and L.P.) considered a matrix model for a two-level
system interacting with a $n\times n$ reservoir and assuming that the
interaction is modelled by a random matrix. We presented there a formula for
the reduced density matrix in the limit $n\to \infty $ as well as several its
properties and asymptotic forms in various regimes. In this paper we give the
proofs of the assertions, and present also a new fact about the model.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 08:03:37 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Lebowitz",
"J. L.",
""
],
[
"Lytova",
"A.",
""
],
[
"Pastur",
"L.",
""
]
] | [
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] |
711.2357 | Marcin Wie\'sniak | Marcin Wiesniak | Quantum Wire as Open System | New results, new references added, clearer plots | null | null | null | quant-ph | null | The faithful exchange of quantum information will soon become one of the
challenges of the emerging quantum information technology. One of the possible
solutions is to transfer a superposition through a chain of properly coupled
spins. Such a system is called a quantum wire. We discuss the transfer in a
quantum wire \cite{christ,niko1,niko2}, when the process of thermalization of
the state takes place together with the free evolution. We investigate which
encoding scheme is more faithful in certain thermal conditions.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 08:08:25 GMT"
},
{
"version": "v2",
"created": "Fri, 2 May 2008 04:56:52 GMT"
}
] | 2008-05-02T00:00:00 | [
[
"Wiesniak",
"Marcin",
""
]
] | [
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] |
711.2358 | Mehdi Kargarian | M. Kargarian, R. Jafari, A. Langari | The renormalization of entanglement in the anisotropic Heisenberg (XXZ)
model | 9 pages, 7 figures | Phys. Rev. A 77, 032346 (2008) | 10.1103/PhysRevA.77.032346 | null | quant-ph | null | We have applied our recent approach (Kargarian, et.al Phys. Rev. A 76, 60304
(R) (2007)) to study the quantum information properties of the anisotropic
s=1/2 Heisenberg chain. We have investigated the underlying quantum information
properties like the evolution of concurrence, entanglement entropy, nonanalytic
behaviours and the scaling close to the quantum critical point of the model.
Both the concurrence and the entanglement entropy develop two saturated values
after enough iterations of the renormalization of coupling constants. This
values are associated with the two different phases, i.e Neel and spin liquid
phases. The nonanalytic behaviour comes from the divergence of the first
derivative of both measures of entanglement as the size of system becomes
large. The renormalization scheme demonstrates how the minimum value of the
first derivative and its position scales with an exponent of the system size.
It is shown that this exponent is directly related to the critical properties
of the model, i.e. the exponent governing the divergence of the correlation
length close to the quantum critical point. We also use a renormalization
method based on the quantum group concept in order to get more insight about
the critical properties of the model and the renormalization of entanglement.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 08:13:55 GMT"
},
{
"version": "v2",
"created": "Wed, 16 Jan 2008 06:32:30 GMT"
},
{
"version": "v3",
"created": "Wed, 2 Apr 2008 21:14:02 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Kargarian",
"M.",
""
],
[
"Jafari",
"R.",
""
],
[
"Langari",
"A.",
""
]
] | [
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711.2359 | Javier Vijande Asenjo | J. Vijande, A. Valcarce, F. Fernandez | B meson spectroscopy | 8 pages, 5 tables. Accepted for publication in Physical Review D | Phys.Rev.D77:017501,2008 | 10.1103/PhysRevD.77.017501 | null | hep-ph hep-ex | null | We study the $B$ meson spectroscopy allowing the mixture of conventional $P$
wave quark-antiquark states and four-quark components. A similar picture was
used to describe the new $D_J$ and $D_{sJ}$ open charm mesons. The four-quark
components shift the masses of some positive parity $B_{sJ}$ states below their
corresponding isospin preserving two-meson threshold and therefore they are
expected to be narrow. Electromagnetic decay widths are analyzed.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 08:15:18 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Vijande",
"J.",
""
],
[
"Valcarce",
"A.",
""
],
[
"Fernandez",
"F.",
""
]
] | [
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] |
711.236 | Etienne Birmel\'e | E. Birmel\'e | Every longest circuit of a 3-connected, $K_{3,3}$-minor free graph has a
chord | accepted by Journal of Graph Theory | Journal of Graph Theory, 58 (4): 293-298, 2008 | 10.1002/jgt.20312 | null | math.CO | null | Carsten Thomassen conjectured that every longest circuit in a 3-connected
graph has a chord. We prove the conjecture for graphs having no $K_{3,3}$
minor, and consequently for planar graphs.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 08:23:49 GMT"
},
{
"version": "v2",
"created": "Mon, 31 Mar 2008 14:12:03 GMT"
}
] | 2011-09-07T00:00:00 | [
[
"Birmelé",
"E.",
""
]
] | [
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711.2361 | Rashid Nazmitdinov | R.G. Nazmitdinov, J. Kvasil, and A. Tsvetkov | Reflection symmetry instability at high spins in 162,164Yb | 6 pages, 7 figures | Phys.Lett.B657:159-164,2007 | 10.1016/j.physletb.2007.10.004 | null | nucl-th nucl-ex | null | A shape evolution of 162,164Yb in yrast states is traced using the
self-consistent Skyrme Hartree-Fock calculations. We found that nonaxial
octupole deformations (in particular, Y_{31} term) become favorable at large
rotational frequencies (> 0.4 MeV) in 162Yb, while in 164Yb a nonaxial
quadrupole shape is dominant at fast rotation. The cranked Nilsson model and
random phase approximation are used to understand the dynamics of octupole
correlations in both nuclei. We demonstrate that the disappearance of one of
the octupole vibrational modes in the rotating frame gives rise to the nonaxial
octupole deformations in 162Yb, while the octupole modes are nonzero in 164Yb.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 08:38:12 GMT"
}
] | 2010-11-05T00:00:00 | [
[
"Nazmitdinov",
"R. G.",
""
],
[
"Kvasil",
"J.",
""
],
[
"Tsvetkov",
"A.",
""
]
] | [
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] |
711.2362 | Zhongmu Li | Zhongmu Li, Zhanwen Han | How binary interactions affect spectral stellar population synthesis | 28 pages, 13 figures, Accepted for publication in ApJ | null | 10.1086/590228 | null | astro-ph | null | Single-star stellar population (ssSSP) models are usually used for stellar
population studies. However, more than 50% of stars are in binaries and evolve
differently from single stars. This suggests that the effects of binary
interactions should be considered when modeling the stellar populations of
galaxies and star clusters. Via a rapid spectral stellar population synthesis
(RPS) model, we give detailed studies of the effects of binary interactions on
the Lick indices and colours of stellar populations, and on the determination
of the stellar ages and metallicities of populations.
The results show that binary interactions make stellar populations less
luminous, bluer, with larger age-sensitive Lick index (Hbeta) and less
metallicity-sensitive indices (e.g., Mgb, Fe5270 and Fe5335) compared to
ssSSPs. It also shows that when ssSSP models are used to determine the ages and
metallicities of stellar populations, lower ages or metallicities will be
obtained, taking two line indices (Hbeta and [MgFe]) and two colours (e.g., u-R
and R-K), respectively. Some relations for linking the stellar-population
parameters obtained by ssSSPs to those obtained by binary-star stellar
populations (bsSSPs) are presented in the work. This can help us to get some
absolute values for stellar-population parameters and is useful for absolute
studies. However, it is found that the relative luminosity-weighted stellar
ages and metallicities obtained via ssSSPs and bsSSPs are similar. This
suggests that ssSSPs can be used for most stellar population studies, except in
some special cases.
| [
{
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"created": "Tue, 1 Apr 2008 01:02:20 GMT"
},
{
"version": "v3",
"created": "Tue, 20 May 2008 07:25:33 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Li",
"Zhongmu",
""
],
[
"Han",
"Zhanwen",
""
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711.2363 | Gajendra Pandey | Gajendra Pandey (1), David L. Lambert (2), N. Kameswara Rao (1) ((1)
Indian Institute of Astrophysics, Bangalore, India, (2) The W.J. McDonald
Observatory, University of Texas at Austin, TX, USA) | Fluorine in R Coronae Borealis Stars | 25 pages, 7 figures, accepted to ApJ | null | 10.1086/526492 | null | astro-ph | null | Neutral fluorine (F I) lines are identified in the optical spectra of several
R Coronae Borealis stars (RCBs) at maximum light. These lines provide the first
measurement of the fluorine abundance in these stars. Fluorine is enriched in
some RCBs by factors of 800 to 8000 relative to its likely initial abundance.
The overabundances of fluorine are evidence for the synthesis of fluorine.
These results are discussed in the light of the scenario that RCBs are formed
by accretion of an He white dwarf by a C-O white dwarf. Sakurai's object (V4334
Sgr), a final He-shell flash product, shows no detectable F I lines.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 09:00:20 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Pandey",
"Gajendra",
""
],
[
"Lambert",
"David L.",
""
],
[
"Rao",
"N. Kameswara",
""
]
] | [
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] |
711.2364 | Kenji Fukushima | Kenji Fukushima | Randomness in infinitesimal extent in the McLerran-Venugopalan model | 11 pages, 11 figures, typos corrected; Introduction and Discussion
sections extended | Phys.Rev.D77:074005,2008 | 10.1103/PhysRevD.77.074005 | YITP-07-79 | hep-ph | null | We study discrepancy between the analytical definition and the numerical
implementation of the McLerran-Venugopalan (MV) model. The infinitesimal extent
of a fast-moving nucleus should retain longitudinal randomness in the color
source distribution even when the longitudinal extent approximates zero due to
the Lorentz contraction, which is properly taken into account in the analytical
treatment. We point out that the longitudinal randomness is lost in numerical
simulations because of lack of the path-ordering of the Wilson line along the
longitudinal direction. We quantitatively investigate how much the results with
and without longitudinal randomness differ from each other. We finally mention
that the discrepancy could be absorbed in a choice of the model parameter in
the physical unit, and nevertheless, it is important for a full theory
approach.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 18:15:08 GMT"
},
{
"version": "v2",
"created": "Sun, 20 Jan 2008 15:00:03 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Fukushima",
"Kenji",
""
]
] | [
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711.2365 | Otmar Stahl | O. Stahl, S. Casassus, T.L. Wilson | Interstellar 12C/13C from CH+ absorption lines: Results from an extended
survey | 11 pages, 16 figures, 2 tables, A&A submitted | null | 10.1051/0004-6361:20078747 | null | astro-ph | null | The 12C/13C isotope ratio in the interstellar medium (ISM), and its evolution
with time, is an important tracer of stellar yields. Spatial variations of this
ratio can be used to study mixing in the ISM. We want to determine this ratio
and its spatial variations in the local ISM from CH+ absorption lines in the
optical towards early-type stars. The aim is to determine the average value for
the local ISM and study possible spatial variations. We observed a large number
of early-type stars with Feros to extend the sample of suitable target stars
for CH+ isotope studies. The best suited targets were observed with Uves with
higher signal-to-noise ratio and spectral resolution to determine the isotope
ratio from the interstellar CH+ lines. This study significantly expands the
number of 13CH+ detections. We find an average ratio of <R> = 76.27 +- 1.94 or,
for f = 1/R, <f> = (120.46 +- 3.02) 10^{-4}. The scatter in f is 6.3
sigma(<f>). This findings strengthens the case for chemical inhomogeneity in
the local ISM, with important implications for the mixing in the ISM. Given the
large scatter, the present-day value in the ISM is not significantly larger
than the solar value, which corresponds to the local value 4.5 Gyr ago.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 09:20:20 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Stahl",
"O.",
""
],
[
"Casassus",
"S.",
""
],
[
"Wilson",
"T. L.",
""
]
] | [
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711.2366 | Isabel M. C. Salavessa | Guanghan Li, Isabel Salavessa | Forced Convex Mean Curvature Flow in Euclidean Spaces | 22 Pages | Manuscripta Math. 126 (2008) 333 - 351 | 10.1007/s00229-008-0181-z | null | math.DG math.AP | null | In this paper, we consider the mean curvature flow of convex hypersurfaces in
Euclidean spaces with a general forcing term. We show that the flow may shrink
to a point in finite time if the forcing term is small, or exist for all times
and expand to infinity if the forcing term is large enough. The flow can also
converge to a round sphere for some special forcing term and initial
hypersurface. Furthermore, the normalization of the flow is carried out so that
long time existence and convergence of the rescaled flow are studied. Our work
extends Huisken's well-known mean curvature flow and McCoy's mixed volume
preserving mean curvature flow.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 09:18:53 GMT"
}
] | 2008-06-17T00:00:00 | [
[
"Li",
"Guanghan",
""
],
[
"Salavessa",
"Isabel",
""
]
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711.2367 | Slavko Bogdanov | Slavko Bogdanov, Jonathan E. Grindlay (Harvard) | An X-ray View of Radio Millisecond Pulsars | 5 pages, 5 figures, To appear in the proceedings of "40 Years of
Pulsars: Millisecond Pulsars, Magnetars, and More", August 12-17, 2007,
McGill University, Montreal, Canada | AIPConf.Proc.983:64-68,2008 | 10.1063/1.2900321 | null | astro-ph | null | In recent years, X-ray observations with Chandra and XMM-Newton have
significantly increased our understanding of rotation-powered (radio)
millisecond pulsars (MSPs). Deep Chandra studies of several globular clusters
have detected X-ray counterparts to a host of MSPs, including 19 in 47 Tuc
alone. These surveys have revealed that most MSPs exhibit thermal emission from
their heated magnetic polar caps. Realistic models of this thermal X-ray
emission have provided important insight into the basic physics of pulsars and
neutron stars. In addition, intrabinary shock X-ray radiation observed in
``black-widow'' and peculiar globular cluster ``exchanged'' binary MSPs give
interesting insight into MSP winds and relativistic shock. Thus, the X-ray band
contains valuable information regarding the basic properties of MSPs that are
not accesible by radio timing observations.
| [
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711.2368 | Alexander Zaitsev | Alexander Zaitsev | Sending and Searching for Interstellar Messages | 6 pages, 3 figures, to appear in the proceedings of "International
Asronautical Congress 2007", Hyderbad, India | null | 10.1016/j.actaastro.2008.05.014 | null | physics.pop-ph | null | There is a close interrelation between Searching for Extraterrestrial
Intelligence (SETI) and Messaging to Extraterrestrial Intelligence (METI). For
example, the answers to the questions "Where to search" and "Where to send" are
equivalent, in that both require an identical selection from the same target
star lists. Similar considerations lead to a strategy of time synchronization
between sending and searching. Both SETI and METI use large reflectors. The
concept of "magic frequencies" may be applicable to both SETI and METI. Efforts
to understand an alien civilization's Interstellar Messages (IMs), and efforts
to compose our own IMs so they will be easily understood by unfamiliar
Extraterrestrials, are mutually complementary. Furthermore, the METI-question:
"How can we benefit from sending IMs, if a response may come only thousands of
years later?" begs an equivalent SETI-question: "How can we benefit from
searching, if it is impossible now to perceive the motivations and feelings of
those who may have sent messages in the distant past?" A joint consideration of
the theoretical and the practical aspects of both sending and searching for
IMs, in the framework of a unified, disciplined scientific approach, can be
quite fruitful. We seek to resolve the cultural disconnect between those who
advocate sending interstellar messages, and others who anathematize those who
would transmit.
| [
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711.2369 | Moulin Emmanuel | HESS Collaboration: F. Aharonian, et al | Observations of the Sagittarius Dwarf galaxy by the H.E.S.S. experiment
and search for a Dark Matter signal | 21 pages, 4 figures, 2 tables; Accepted for publication in
Astroparticle Physics | Astropart.Phys.29:55-62,2008; Erratum-ibid.33:274-275,2010 | 10.1016/j.astropartphys.2007.11.007 10.1016/j.astropartphys.2010.01.007 | null | astro-ph | null | Observations of the Sagittarius dwarf spheroidal (Sgr dSph) galaxy were
carried out with the H.E.S.S. array of four imaging air Cherenkov telescopes in
June 2006. A total of 11 hours of high quality data are available after data
selection. There is no evidence for a very high energy gamma-ray signal above
the energy threshold at the target position. A 95% C.L. flux limit of 3.6 x
10-12 cm-2s-1 above 250 GeV has been derived. Constraints on the
velocity-weighted cross section <sigma v> are calculated in the framework of
Dark Matter particle annihilation using realistic models for the Dark Matter
halo profile of Sagittarius dwarf galaxy. Two different models have been
investigated encompassing a large class of halo types. A 95% C.L. exclusion
limit on <sigma v> of the order of 2 x 10-25 cm3s-1 is obtained for a core
profile in the 100 GeV - 1 TeV neutralino mass range.
| [
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] |
711.237 | Ryutin Roman | V. A. Petrov and R. A. Ryutin (IHEP, Serpukhov, Russia) | Patterns of the Exclusive Double Diffraction | 12 pages, 7 figures, to be published | J.Phys.G35:065004,2008 | 10.1088/0954-3899/35/6/065004 | null | hep-ph | null | We consider Exclusive Double Diffractive Events (EDDE) as a powerfull tool to
study the picture of the $pp$ interaction. Calculations of the cross-sections
for the process $p+p\to p+M+p$ are presented in the convenient form for further
experimental applications. We propose measurements of t-distributions in the
joint CMS-TOTEM experiment. It is shown that important information on the
interaction region could be extracted from the diffractive pattern.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 10:20:38 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Petrov",
"V. A.",
"",
"IHEP, Serpukhov, Russia"
],
[
"Ryutin",
"R. A.",
"",
"IHEP, Serpukhov, Russia"
]
] | [
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] |
711.2371 | Shoulan Gao | Shoulan Gao, Cuipo Jiang | Representations for the non-graded Virasoro-like algebra | 29 pages; | null | null | null | math.RT math.RA | null | It is proved that an irreducible module over the non-graded Virasoro-like
algebra, which satisfies a natural condition, is a GHW module or uniformly
bounded. Furthermore, the classification of some uniformly bounded modules is
given.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 10:38:49 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Gao",
"Shoulan",
""
],
[
"Jiang",
"Cuipo",
""
]
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711.2372 | Luis Paris | Luis Paris | Braid groups and Artin groups | null | In: Handbook on Teichm\"uller theory (A. Papadopoulos, ed.),
Volume II, EMS Publishing House, Z\"urich 2008 | null | null | math.GR math.GT | null | This article is a survey on the braid groups, the Artin groups, and the
Garside groups. It is a presentation, accessible to non-experts, of various
topological and algebraic aspects of these groups. It is also a report on three
points of the theory: the faithful linear representations, the cohomology, and
the geometrical representations.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 10:42:13 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Paris",
"Luis",
""
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] |
711.2373 | Stanislav Volkov | Mikhail Menshikov, Stanislav Volkov | Urn-related random walk with drift $\rho x^{\alpha} / t^{\beta}$ | 23 pages | null | null | null | math.PR | null | We study a one-dimensional random walk whose expected drift depends both on
time and the position of a particle. We establish a non-trivial phase
transition for the recurrence vs. transience of the walk, and show some
interesting applications to Friedman's urn, as well as showing the connection
with Lamperti's walk with asymptotically zero drift.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 10:51:38 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Menshikov",
"Mikhail",
""
],
[
"Volkov",
"Stanislav",
""
]
] | [
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] |
711.2374 | Alexander Chernyatiev | A.Ya. Belov, A.L.Chernyat'ev | Describing the set of words generated by interval exchange
transformation | 17 pages, this paper was submitted at scientific council of MSU,
date: September 21, 2007 | Comm. in Algebra, 2010, 38, N. 7, 2588--2605 | 10.1080/00927870903032932 | VINITI 1048-B2007 | math.DS math.CO | null | Let $W$ be an infinite word over finite alphabet $A$. We get combinatorial
criteria of existence of interval exchange transformations that generate the
word W.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 10:54:42 GMT"
},
{
"version": "v2",
"created": "Thu, 31 Jan 2008 15:52:48 GMT"
}
] | 2017-11-30T00:00:00 | [
[
"Belov",
"A. Ya.",
""
],
[
"Chernyat'ev",
"A. L.",
""
]
] | [
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711.2375 | Roee Teper | Roee Teper | The induced capacity and Choquet integral monotone convergece | null | null | null | null | math.CA | null | Given a probability measure over a state space, a partial collection
(sub-$\sigma$-algebra) of events whose probabilities are known, induces a
capacity over the collection of all possible events. The \emph{induced
capacity} of an event $F$ is the probability of the maximal (with respect to
inclusion) event contained in $F$ whose probability is known. The Choquet
integral with respect to the induced capacity coincides with the integral with
respect to a \emph{probability specified on a sub-algebra} (Lehrer
\cite{Lehrer2}). We study Choquet integral monotone convergence and apply the
results to the integral with respect to the induced capacity. The paper
characterizes the properties of sub-$\sigma$-algebras and of induced capacities
which yield integral monotone convergence.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 10:59:26 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Teper",
"Roee",
""
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] |
711.2376 | Marian Lazar | M. Lazar, P.K. Shukla, and A. Smolyakov | Surface waves on a quantum plasma half-space | null | submmitted to Physics of Plasmas on October 22, 2007 | 10.1063/1.2825278 | null | physics.plasm-ph physics.gen-ph | null | Surface modes are coupled electromagnetic/electrostatic excitations of free
electrons near the vacuum-plasma interface and can be excited on a sufficiently
dense plasma half-space. They propagate along the surface plane and decay in
either sides of the boundary. In such dense plasma models, which are of
interest in electronic signal transmission or in some astrophysical
applications, the dynamics of the electrons is certainly affected by the
quantum effects. Thus, the dispersion relation for the surface wave on a
quantum electron plasma half-space is derived by employing the quantum
hydrodynamical (QHD) and Maxwell-Poison equations. The QHD include quantum
forces involving the Fermi electron temperature and the quantum Bohm potential.
It is found that, at room temperature, the quantum effects are mainly relevant
for the electrostatic surface plasma waves in a dense gold metallic plasma.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:14:04 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Lazar",
"M.",
""
],
[
"Shukla",
"P. K.",
""
],
[
"Smolyakov",
"A.",
""
]
] | [
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] |
711.2377 | Masaki Kobayashi | M. Kobayashi, Y. Ooki, M. Takizawa, G. S. Song, A. Fujimori, Y.
Takeda, K. Terai, T. Okane, S.-I. Fujimori, Y. Saitoh, H. Yamagami, M. Seki,
T. Kawai, H. Tabata | Photoemission and x-ray absorption studies of valence states in
(Ni,Zn,Fe,Ti)$_{3}$O$_{4}$ thin films exhibiting photo-induced magnetization | 4 pages, 4 figures | Appl. Phys. Lett. 92, 082502 (2008) | 10.1063/1.2885080 | null | cond-mat.mtrl-sci cond-mat.str-el | null | By means of photoemission and x-ray absorption spectroscopy, we have studied
the electronic structure of (Ni,Zn,Fe,Ti)$_{3}$O$_{4}$ thin films, which
exhibits a cluster glass behavior with a spin-freezing temperature $T_f$ of
$\sim 230$ K and photo-induced magnetization (PIM) below $T_f$. The Ni and Zn
ions were found to be in the divalent states. Most of the Fe and Ti ions in the
thin films were trivalent (Fe$^{3+}$) and tetravalent (Ti$^{4+}$),
respectively. While Ti doping did not affect the valence states of the Ni and
Zn ions, a small amount of Fe$^{2+}$ ions increased with Ti concentration,
consistent with the proposed charge-transfer mechanism of PIM.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 15:49:59 GMT"
}
] | 2008-04-21T00:00:00 | [
[
"Kobayashi",
"M.",
""
],
[
"Ooki",
"Y.",
""
],
[
"Takizawa",
"M.",
""
],
[
"Song",
"G. S.",
""
],
[
"Fujimori",
"A.",
""
],
[
"Takeda",
"Y.",
""
],
[
"Terai",
"K.",
""
],
[
"Okane",
"T.",
""
],
[
"Fujimori",
"S. -I.",
""
],
[
"Saitoh",
"Y.",
""
],
[
"Yamagami",
"H.",
""
],
[
"Seki",
"M.",
""
],
[
"Kawai",
"T.",
""
],
[
"Tabata",
"H.",
""
]
] | [
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711.2378 | Sudhir Vempati | Ranjan Laha and Sudhir K. Vempati | Results from MiniBooNE | 16 pages; Added comments and references. Accepted for publication in
Current Science | Curr.Sci.94:211-217,2008 | null | IISc/CHEP/13/07 | physics.pop-ph hep-ex hep-ph | null | The long awaited experimental results from MiniBooNE have recently been
announced. This experiment tests whether neutrino oscillations can occur at a
higher mass squared difference $\sim1 {eV}^2$ compared to well established
observations of solar and atmospheric neutrinos. The LSND experiment has
previously claimed to have observed neutrino oscillations at $\Delta m^2 \sim 1
{eV}^2$, however the results being controversial, required an independent
confirmation. The MiniBooNE results settle this controversy by observing null
oscillations at the said mass squared difference. These results have strong
implications on existence of sterile neutrinos, CPT violation and mass varying
neutrinos. We review the present status of neutrino masses and mixing in the
light of this recent result.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:22:23 GMT"
},
{
"version": "v2",
"created": "Mon, 31 Dec 2007 11:56:49 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Laha",
"Ranjan",
""
],
[
"Vempati",
"Sudhir K.",
""
]
] | [
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] |
711.2379 | Zhuo Li | Zhuo Li and Eli Waxman | Prompt optical emission from residual collisions in GRB outflows | 5 pages, 1 fig, ApJL accepted version, minor changes-- add
demonstration of gamma-ray emission radius, and comments on earlier work | ApJ 674 (2008) L65 | 10.1086/529042 | null | astro-ph | null | The prompt gamma-ray emission in gamma-ray bursts is believed to be produced
by internal shocks within a relativistic unsteady outflow. The recent detection
of prompt optical emission accompanying the prompt gamma-ray emission appears
to be inconsistent with this model since the out flowing plasma is expected to
be highly optically thick to optical photons. We show here that fluctuations in
flow properties on short, ~ 1 ms, time scale, which drive the gamma-ray
producing collisions at small radii, are expected to lead to "residual"
collisions at much larger radii, where the optical depth to optical photons is
low. The late residual collisions naturally account for the relatively bright
optical emission. The apparent simultaneity of gamma-ray and optical emission
is due to the highly relativistic speed with which the plasma expands. Residual
collisions may also account for the X-ray emission during the early "steep
decline" phase, where the radius is inferred to be larger than the gamma-ray
emission radius. Finally, we point out that inverse-Compton emission from
residual collisions at large radii is expected to contribute significantly to
the emission at high energy, and may therefore "smear" the pair production
spectral cut-off.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:22:49 GMT"
},
{
"version": "v2",
"created": "Thu, 15 Nov 2007 21:49:05 GMT"
},
{
"version": "v3",
"created": "Thu, 3 Jan 2008 11:34:02 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Li",
"Zhuo",
""
],
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"Eli",
""
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711.238 | Pavel Kurakin | P. V. Kurakin | Hidden time interpretation of quantum mechanics and "no protocol"
argument | 8 pages, 7 figures. Reported at the International Symposium "Quantum
Informatics - 2007", 1 - 5 Oct., Lipki, Russia. Discusses arguments raised at
"Are superluminal signals an acceptable hypothesis? - Difficulties in
building communication protocol with them", quant-ph/0610159 | null | 10.1117/12.801906 | null | physics.gen-ph | null | Previously suggested hidden time interpretation of quantum mechanics allows
to reproduce the same predictions as standard quantum mechanics provides, since
it is based on Feynman many - paths formulation of QM. While new experimental
consequences of this interpretation are under investigation, some advantages
can be enumerated. (1) The interpretation is much field theoretic - like in
classical sense, so it is local in mathematical sense, though quantum
(physical) non-locality is preserved. (2) The interpretation is based on one
type of mathematical objects, rather than two different (Hilbert space vectors
and operators). (3) The interpretation, as it was argued, overcomes the problem
of hidden variables in a radically new way, with no conflict to Bell's theorem.
Recently an important argument against hidden variables - like formulations of
quantum theory was risen - "no protocol" argument. It is argued in the paper,
that hidden time interpretation successfully overcomes this argument.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:33:08 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Kurakin",
"P. V.",
""
]
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711.2381 | Fernando Casas | Fernando Casas | Sufficient conditions for the convergence of the Magnus expansion | 20 pages | J. Phys. A: Math. Theor. 40 (2007), 15001-15017 | 10.1088/1751-8113/40/50/006 | null | math.CA | null | Two different sufficient conditions are given for the convergence of the
Magnus expansion arising in the study of the linear differential equation $Y' =
A(t) Y$. The first one provides a bound on the convergence domain based on the
norm of the operator $A(t)$. The second condition links the convergence of the
expansion with the structure of the spectrum of $Y(t)$, thus yielding a more
precise characterization. Several examples are proposed to illustrate the main
issues involved and the information on the convergence domain provided by both
conditions.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:34:47 GMT"
}
] | 2009-04-11T00:00:00 | [
[
"Casas",
"Fernando",
""
]
] | [
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] |
711.2382 | Nicolas Vergne | Nicolas Vergne (1) and Miguel Abadi (2) ((1) Laboratoire Statistique
et G\'enome France, (2) Universidade de Campinas Brazil) | Poisson approximation for search of rare words in DNA sequences | 29 pages, 0 figures | null | null | null | math.PR math.ST stat.AP stat.TH | null | Using recent results on the occurrence times of a string of symbols in a
stochastic process with mixing properties, we present a new method for the
search of rare words in biological sequences generally modelled by a Markov
chain. We obtain a bound on the error between the distribution of the number of
occurrences of a word in a sequence (under a Markov model) and its Poisson
approximation. A global bound is already given by a Chen-Stein method. Our
approach, the psi-mixing method, gives local bounds. Since we only need the
error in the tails of distribution, the global uniform bound of Chen-Stein is
too large and it is a better way to consider local bounds. We search for two
thresholds on the number of occurrences from which we can regard the studied
word as an over-represented or an under-represented one. A biological role is
suggested for these over- or under-represented words. Our method gives such
thresholds for a panel of words much broader than the Chen-Stein method.
Comparing the methods, we observe a better accuracy for the psi-mixing method
for the bound of the tails of distribution. We also present the software PANOW
(available at http://stat.genopole.cnrs.fr/software/panowdir/) dedicated to the
computation of the error term and the thresholds for a studied word.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:37:37 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Vergne",
"Nicolas",
""
],
[
"Abadi",
"Miguel",
""
]
] | [
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] |
711.2383 | Barbara Cerato | Barbara Cerato, Guido Masera and Emanuele Viterbo | Decoding the Golden Code: a VLSI design | 25 pages, 10 figures | null | null | null | cs.AR | null | The recently proposed Golden code is an optimal space-time block code for 2 X
2 multiple-input multiple-output (MIMO) systems. The aim of this work is the
design of a VLSI decoder for a MIMO system coded with the Golden code. The
architecture is based on a rearrangement of the sphere decoding algorithm that
achieves maximum-likelihood (ML) decoding performance. Compared to other
approaces, the proposed solution exhibits an inherent flexibility in terms of
modulation schemes QAM modulation size and this makes our architecture
particularly suitable for adaptive modulation schemes.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:55:30 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Cerato",
"Barbara",
""
],
[
"Masera",
"Guido",
""
],
[
"Viterbo",
"Emanuele",
""
]
] | [
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] |
711.2384 | Andrea Tomadin | Andrea Tomadin, Marco Polini, M.P. Tosi, Rosario Fazio | Nonequilibrium pairing instability in ultracold Fermi gases with
population imbalance | 10 pages, 6 figures. High-quality figures can be requested to the
authors | Phys. Rev. A 77, 033605 (2008) | 10.1103/PhysRevA.77.033605 | null | cond-mat.str-el cond-mat.supr-con | null | We present detailed numerical and analytical investigations of the
nonequilibrium dynamics of spin-polarized ultracold Fermi gases following a
sudden switching-on of the atom-atom pairing coupling strength. Within a
time-dependent mean-field approach we show that on increasing the imbalance it
takes longer for pairing to develop, the period of the nonlinear oscillations
lengthens, and the maximum value of the pairing amplitude decreases. As
expected, dynamical pairing is suppressed by the increase of the imbalance.
Eventually, for a critical value of the imbalance the nonlinear oscillations do
not even develop. Finally, we point out an interesting temperature-reentrant
behavior of the exponent characterizing the initial instability.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:41:07 GMT"
}
] | 2008-03-06T00:00:00 | [
[
"Tomadin",
"Andrea",
""
],
[
"Polini",
"Marco",
""
],
[
"Tosi",
"M. P.",
""
],
[
"Fazio",
"Rosario",
""
]
] | [
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] |
711.2385 | Marian Lazar | M. Lazar | Fast magnetization in counterstreaming plasmas with temperature
anisotropies | null | null | 10.1016/j.physleta.2007.11.063 | null | physics.plasm-ph physics.gen-ph | null | Counterstreaming plasmas exhibits an electromagnetic unstable mode of
filamentation type, which is responsible for the magnetization of plasma
system. It is shown that filamentation instability becomes significantly faster
when plasma is hotter in the streaming direction. This is relevant for
astrophysical sources, where strong magnetic fields are expected to exist and
explain the nothermal emission observed.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 11:49:30 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Lazar",
"M.",
""
]
] | [
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711.2386 | Hajime Takami | Hajime Takami and Katsuhiko Sato | Distortion of Ultra-high-energy sky by Galactic Magnetic Field | 9 pages, 6 figures, submitted to ApJ | Astrophys.J.681:1279-1287,2008 | 10.1086/588513 | null | astro-ph | null | We investigate the deflections of UHE protons by Galactic magnetic field(GMF)
using four conventional GMF models in order to discuss the positional
correlation between the arrival distribution of UHECRs and their sources. UHE
protons coming from the direction around the Galactic center are highly
deflected above $8^{\circ}$ by the dipole magnetic field during their
propagation in Galactic space. However, in bisymmetric spiral field models,
there are directions with the deflection angle below $1^{\circ}$. One of these
directions is toward Centaurus A, the nearest radio-loud active galactic nuclei
that is one of possible candidates of UHECR sources. On the other hand, UHE
protons arriving from the direction of the anti-Galactic center are less
deflected, especially in bisymmetric spiral field models. Thus, the northern
hemisphere, not including the Galactic center, is suitable for the studies of
correlation with sources. The dependence on model parameters is also
investigated. The deflection angles of UHE protons are dependent on the pitch
angle of the spiral field. We also investigate distortion of the supergalactic
plane by GMF. Since the distortion in the direction around Galactic center
strongly depends on the GMF model, we can obtain information on GMF around
Galactic center if Pierre Auger Observatory finds the significant positional
correlation around the supergalactic plane.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 12:03:06 GMT"
}
] | 2009-02-10T00:00:00 | [
[
"Takami",
"Hajime",
""
],
[
"Sato",
"Katsuhiko",
""
]
] | [
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] |
711.2387 | Marek Karliner | Itay Hen and Marek Karliner | Hexagonal Structure of Baby Skyrmion Lattices | RevTeX, 7 pages, 6 figures | Phys.Rev.D77:054009,2008 | 10.1103/PhysRevD.77.054009 | null | hep-th | null | We study the zero-temperature crystalline structure of baby Skyrmions by
applying a full-field numerical minimization algorithm to baby Skyrmions placed
inside different parallelogramic unit-cells and imposing periodic boundary
conditions. We find that within this setup, the minimal energy is obtained for
the hexagonal lattice, and that in the resulting configuration the Skyrmion
splits into quarter-Skyrmions. In particular, we find that the energy in the
hexagonal case is lower than the one obtained on the well-studied rectangular
lattice, in which splitting into half-Skyrmions is observed.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 14:41:51 GMT"
},
{
"version": "v2",
"created": "Tue, 20 Nov 2007 14:23:33 GMT"
},
{
"version": "v3",
"created": "Wed, 16 Jan 2008 11:21:27 GMT"
},
{
"version": "v4",
"created": "Mon, 28 Jan 2008 23:13:11 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Hen",
"Itay",
""
],
[
"Karliner",
"Marek",
""
]
] | [
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] |
711.2388 | Sylvain Joubaud | Sylvain Joubaud (Phys-ENS), Nicolas Garnier (Phys-ENS), Sergio
Ciliberto (Phys-ENS) | Fluctuations of the total entropy production in stochastic systems | 6 p | null | 10.1209/0295-5075/82/30007 | null | cond-mat.stat-mech | null | Fluctuations of the excess heat in an out of equilibrium steady state are
experimentally investigated in two stochastic systems : an electric circuit
with an imposed mean current and a harmonic oscillator driven out of
equilibrium by a periodic torque. In these two linear systems, we study excess
heat that represents the difference between the dissipated heat out of
equilibrium and the dissipated heat at equilibrium. Fluctuation theorem holds
for the excess heat in the two experimental systems for all observation times
and for all fluctuation magnitudes.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 12:13:19 GMT"
},
{
"version": "v2",
"created": "Fri, 16 Nov 2007 13:48:36 GMT"
},
{
"version": "v3",
"created": "Mon, 14 Jan 2008 11:26:34 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Joubaud",
"Sylvain",
"",
"Phys-ENS"
],
[
"Garnier",
"Nicolas",
"",
"Phys-ENS"
],
[
"Ciliberto",
"Sergio",
"",
"Phys-ENS"
]
] | [
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711.2389 | Rudra Prakash Malik | R. P. Malik (Bhu), B. P. Mandal (Bhu) | Superfield approach to symmetry invariance in QED with complex scalar
fields | LaTeX file, 14 pages, minor changes in the title and text, version to
appear in ``Pramana - Journal of Physics'' | Pramana 72: 805-818, 2009 | 10.1007/s12043-009-0073-0 | null | hep-th | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | We show that the Grassmannian independence of the super Lagrangian density,
expressed in terms of the superfields defined on a (4, 2)-dimensional
supermanifold, is a clear-cut proof for the Becchi-Rouet-Stora-Tyutin (BRST)
and anti-BRST invariance of the corresoponding four (3 + 1)-dimensional (4D)
Lagrangian density that describes the interaction between the U(1) gauge field
and the charged complex scalar fields. The above 4D field theoretical model is
considered on a (4, 2)-dimensional supermanifold parametrized by the ordinary
four spacetime variables x^\mu (with \mu = 0, 1, 2, 3) and a pair of
Grassmannian variables \theta and \bar\theta (with \theta^2 = \bar\theta^2 = 0,
\theta \bar\theta + \bar\theta \theta = 0). Geometrically, the (anti-)BRST
invariance is encoded in the translation of the super Lagrangian density along
the Grassmannian directions of the above supermanifold such that the outcome of
this shift operation is zero.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 14:09:34 GMT"
},
{
"version": "v2",
"created": "Thu, 19 Feb 2009 13:15:16 GMT"
}
] | 2015-05-13T00:00:00 | [
[
"Malik",
"R. P.",
"",
"Bhu"
],
[
"Mandal",
"B. P.",
"",
"Bhu"
]
] | [
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] |
711.239 | Alexander Silenko | Alexander J. Silenko | Potential for measurement of the tensor magnetic polarizability of the
deuteron in storage ring experiments | Corrected text, 8 pages | Phys.Rev.C77:021001,2008 | 10.1103/PhysRevC.77.021001 | null | nucl-th | null | General formulas describing deuteron spin dynamics in storage rings with
allowance for the tensor electric and magnetic polarizabilities are derived. It
is found that an initially tensor-polarized deuteron beam can acquire a final
horizontal vector polarization of the order of 1%. This effect allows one to
measure the tensor magnetic polarizability of the deuteron in storage ring
experiments. We also confirm an existence of the effect found by Baryshevsky
and Gurinovich, hep-ph/0506135 and Baryshevsky, hep-ph/0510158; hep-ph/0603191
that the tensor magnetic polarizability of the deuteron causes the spin
rotation with two frequencies and experiences beating for polarized deuteron
beams in storage rings.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 12:19:52 GMT"
},
{
"version": "v2",
"created": "Fri, 22 Feb 2008 07:18:50 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Silenko",
"Alexander J.",
""
]
] | [
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711.2391 | Joao Lopes Dias | Joao Lopes Dias | Local conjugacy classes for analytic torus flows | inc bibl | null | null | null | math.DS | null | If a real-analytic flow on the multidimensional torus close enough to linear
has a unique rotation vector which satisfies an arithmetical condition Y, then
it is analytically conjugate to linear. We show this by proving that the orbit
under renormalization of a constant Y vector field attracts all nearby orbits
with the same rotation vector.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 12:34:00 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Dias",
"Joao Lopes",
""
]
] | [
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711.2392 | Margit Haberreiter Dr. | Margit Haberreiter, Alexander G. Kosovichev, Werner Schmutz | Solving the discrepancy between the seismic and photospheric solar
radius | submitted to ApJL | null | 10.1086/529492 | null | astro-ph | null | Two methods are used to observationally determine the solar radius: One is
the observation of the intensity profile at the limb, the other one uses f-mode
frequencies to derive a 'seismic' solar radius which is then corrected to
optical depth unity. The two methods are inconsistent and lead to a difference
in the solar radius of $\sim$0.3 Mm. Because of the geometrical extention of
the solar photosphere and the increased path lengths of tangential rays the Sun
appears to be larger to an observer who measures the extent of the solar disk.
Based on radiative transfer calculations we show that this discrepancy can be
explained by the difference between the height at disk center where
$\tau_{\mathrm{5000}}=1$ ($\tau_{\mathrm{Ross}}=2/3$) and the inflection point
of the intensity profile on the limb. We calculate the intensity profile of the
limb for the MDI continuum and the continuum at 5000 {\AA} for two atmosphere
structures and compare the position of the inflection points with the radius at
$\tau_{\mathrm{5000}}=1$ ($\tau_{\mathrm{Ross}}=2/3$). The calculated
difference between the 'seismic' radius and the inflection point is $0.347\pm
0.06$ Mm with respect to $\tau_{\mathrm{5000}}=1$ and $0.333\pm 0.08$ Mm with
respect to $\tau_{\mathrm{Ross}}=2/3$. We conclude that the standard solar
radius in evolutionary models has to be lowered by $0.333\pm 0.08$ Mm and is
695.66 Mm. Furthermore, this correction reconciles inflection point
measurements and the 'seismic' radii within the uncertainty.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 19:10:09 GMT"
},
{
"version": "v2",
"created": "Fri, 16 Nov 2007 09:47:26 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Haberreiter",
"Margit",
""
],
[
"Kosovichev",
"Alexander G.",
""
],
[
"Schmutz",
"Werner",
""
]
] | [
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711.2393 | Eduard Aschenbach | Bernd Aschenbach | Grazing Incidence Reflection and Scattering of MeV Protons | 7 pages, 3 figures, updated version of a paper accepted for
publication in the SPIE Conference Proceedings 6688, 2007 | null | 10.1117/12.735589 | null | astro-ph | null | Treating protons as de Broglie waves shows that up to a few MeV energies
protons experience total external reflection using the index of refraction
concept for the target earlier applied to electrons. Angular scattering
distributions can be explained by random surface scattering as known for
X-rays. Applied to the {\it{Chandra}} and {\it{XMM-Newton}} X-ray telescopes
the calculated reflection efficiencies can explain the observed degradation of
the X-ray CCDs for both missions. Some discussion about the possibility of
realizing imaging sub-MeV and MeV proton optics is presented.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 12:37:54 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Aschenbach",
"Bernd",
""
]
] | [
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711.2394 | Antonio Alarcon | Antonio Alarcon | Compact complete minimal immersions in R^3 | 16 pages. Main theorem improved. To appear in Trans. Amer. Math. Soc | null | null | null | math.DG | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | In this paper we find, for any arbitrary finite topological type, a compact
Riemann surface $\mathcal{M},$ an open domain $M\subset\mathcal{M}$ with the
fixed topological type, and a conformal complete minimal immersion $X:M\to\R^3$
which can be extended to a continuous map $X:\bar{M}\to\R^3,$ such that
$X_{|\partial M}$ is an embedding and the Hausdorff dimension of $X(\partial
M)$ is $1.$
We also prove that complete minimal surfaces are dense in the space of
minimal surfaces spanning a finite set of closed curves in $\R^3$, endowed with
the topology of the Hausdorff distance.
| [
{
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"created": "Mon, 28 Jan 2008 11:26:10 GMT"
},
{
"version": "v4",
"created": "Tue, 10 Feb 2009 15:55:20 GMT"
}
] | 2009-02-10T00:00:00 | [
[
"Alarcon",
"Antonio",
""
]
] | [
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711.2395 | Andreas Wirzba | Andreas Wirzba | The Casimir effect as scattering problem | 14 pages, 2 figures, plenary talk at QFEXT07, Leipzig, September
2007, some typos corrected | J.Phys.A41:164003,2008 | 10.1088/1751-8113/41/16/164003 | FZJ-IKP-TH-2007-28 | quant-ph hep-th nlin.CD nucl-th | null | We show that Casimir-force calculations for a finite number of
non-overlapping obstacles can be mapped onto quantum-mechanical billiard-type
problems which are characterized by the scattering of a fictitious point
particle off the very same obstacles. With the help of a modified Krein trace
formula the genuine/finite part of the Casimir energy is determined as the
energy-weighted integral over the log-determinant of the multi-scattering
matrix of the analog billiard problem. The formalism is self-regulating and
inherently shows that the Casimir energy is governed by the infrared end of the
multi-scattering phase shifts or spectrum of the fluctuating field. The
calculation is exact and in principle applicable for any separation(s) between
the obstacles. In practice, it is more suited for large- to medium-range
separations. We report especially about the Casimir energy of a fluctuating
massless scalar field between two spheres or a sphere and a plate under
Dirichlet and Neumann boundary conditions. But the formalism can easily be
extended to any number of spheres and/or planes in three or arbitrary
dimensions, with a variety of boundary conditions or non-overlapping
potentials/non-ideal reflectors.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 15:27:04 GMT"
},
{
"version": "v2",
"created": "Mon, 11 Feb 2008 13:40:03 GMT"
}
] | 2008-11-26T00:00:00 | [
[
"Wirzba",
"Andreas",
""
]
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] |
711.2396 | Nicolas Rey | Nicolas Rey (LPMCN), Alfonso Munoz, Placida Rodriguez-Hernandez,
Alfonso San Miguel (LPMCN) | First-principles study of lithium-doped carbon clathrates under pressure | null | null | 10.1088/0953-8984/20/21/215218 | null | cond-mat.mtrl-sci | null | We present a theoretical study on the behavior under pressure of the two
hypothetical C$_{46}$ and Li$_8$C$_{46}$ type-I carbon clathrates in order to
bring new informations concerning their synthesis. Using \textit{ab initio}
calculations, we have explored the energetic and structural properties under
pressure of these two carbon based cage-like materials. These low-density
meta-stable phases show large negative pressure transitions compared to diamond
which represent a serious obstacle for their synthesis. However, we evidence
that a minimum energy barrier can be reached close to 40 GPa, suggesting that
the synthesis of the Li-clathrate under extreme conditions of pressure and
temperature may be possible. Electronic band structure with related density of
states behavior under pressure as well as the dependence of the active Raman
modes with pressure are also examined.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:05:39 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Rey",
"Nicolas",
"",
"LPMCN"
],
[
"Munoz",
"Alfonso",
"",
"LPMCN"
],
[
"Rodriguez-Hernandez",
"Placida",
"",
"LPMCN"
],
[
"Miguel",
"Alfonso San",
"",
"LPMCN"
]
] | [
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] |
711.2397 | Nikolaus Witte Dr. | Ewgenij Gawrilow, Michael Joswig, Thilo R\"orig, and Nikolaus Witte | Drawing polytopal graphs with polymake | 18 pages, 17 examples, 13 figures, 0 theorems | null | null | null | math.CO | null | This note wants to explain how to obtain meaningful pictures of (possibly
high-dimensional) convex polytopes, triangulated manifolds, and other objects
from the realm of geometric combinatorics such as tight spans of finite metric
spaces and tropical polytopes. In all our cases we arrive at specific,
geometrically motivated, graph drawing problems. The methods displayed are
implemented in the software system polymake.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:10:18 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Gawrilow",
"Ewgenij",
""
],
[
"Joswig",
"Michael",
""
],
[
"Rörig",
"Thilo",
""
],
[
"Witte",
"Nikolaus",
""
]
] | [
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] |
711.2398 | Jonathan Irwin | Jonathan Irwin, Simon Hodgkin, Suzanne Aigrain, Jerome Bouvier, Leslie
Hebb, Mike Irwin, Estelle Moraux | The Monitor project: Rotation of low-mass stars in NGC 2362 -- testing
the disc regulation paradigm at 5 Myr | 13 pages, 17 figures, 1 table. Accepted for publication in MNRAS | null | 10.1111/j.1365-2966.2007.12725.x | null | astro-ph | null | We report on the results of a time-series photometric survey of NGC 2362,
carried out using the CTIO 4m Blanco telescope and Mosaic-II detector as part
of the Monitor project. Rotation periods were derived for 271 candidate cluster
members over the mass range 0.1 <~ M/Msol <~ 1.2. The rotation period
distributions show a clear mass-dependent morphology, qualitatively similar to
that in NGC 2264, as would be expected from the age of this cluster. Using
models of angular momentum evolution, we show that angular momentum losses over
the ~1-5 Myr age range appear to be needed in order to reproduce the evolution
of the slowest rotators in the sample from the ONC to NGC 2362, as found by
many previous studies. By incorporating Spitzer IRAC mid-IR measurements, we
found that 3-4 objects showing mid-IR excesses indicative of the presence of
circumstellar discs were all slow rotators, as would be expected in the disc
regulation paradigm for early pre-main sequence angular momentum evolution, but
this result is not statistically significant at present, given the extremely
limited sample size.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 20:50:26 GMT"
}
] | 2009-11-13T00:00:00 | [
[
"Irwin",
"Jonathan",
""
],
[
"Hodgkin",
"Simon",
""
],
[
"Aigrain",
"Suzanne",
""
],
[
"Bouvier",
"Jerome",
""
],
[
"Hebb",
"Leslie",
""
],
[
"Irwin",
"Mike",
""
],
[
"Moraux",
"Estelle",
""
]
] | [
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] |
711.2399 | Alexander Tiskin | Vladimir Deineko and Alexander Tiskin | Minimum-weight double-tree shortcutting for Metric TSP: Bounding the
approximation ratio | null | null | null | null | cs.DS | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | The Metric Traveling Salesman Problem (TSP) is a classical NP-hard
optimization problem. The double-tree shortcutting method for Metric TSP yields
an exponentially-sized space of TSP tours, each of which approximates the
optimal solution within at most a factor of 2. We consider the problem of
finding among these tours the one that gives the closest approximation, i.e.\
the \emph{minimum-weight double-tree shortcutting}. Previously, we gave an
efficient algorithm for this problem, and carried out its experimental
analysis. In this paper, we address the related question of the worst-case
approximation ratio for the minimum-weight double-tree shortcutting method. In
particular, we give lower bounds on the approximation ratio in some specific
metric spaces: the ratio of 2 in the discrete shortest path metric, 1.622 in
the planar Euclidean metric, and 1.666 in the planar Minkowski metric. The
first of these lower bounds is tight; we conjecture that the other two bounds
are also tight, and in particular that the minimum-weight double-tree method
provides a 1.622-approximation for planar Euclidean TSP.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:19:01 GMT"
},
{
"version": "v2",
"created": "Tue, 16 Dec 2008 11:58:25 GMT"
},
{
"version": "v3",
"created": "Sun, 28 Dec 2008 17:28:18 GMT"
}
] | 2008-12-30T00:00:00 | [
[
"Deineko",
"Vladimir",
""
],
[
"Tiskin",
"Alexander",
""
]
] | [
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] |
711.24 | Jinshan Zhang | Jinshan Zhang | Constituting Atoms of a $\sigma$ Algebra via Its Generator | 8 pages | null | null | null | math.PR math.GM | http://arxiv.org/licenses/nonexclusive-distrib/1.0/ | To constitute atoms of a $\sigma$ algebra is not a easy task due to the large
number of its elements. However, determining them via generators seems a
feasible and simple way since most $\sigma$ algebras are generated by their
smaller proper subsets. Precisely, under some conditions each atom of a
$\sigma$ algebra equals the intersection of the elements containing a point of
the atom in the generator. In this paper, a very weak sufficient condition for
determining atoms by the generator is presented. The condition, though not
being a necessary one, is shown to be almost the weakest one in the sense that
it can hardly be improved.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:21:41 GMT"
},
{
"version": "v2",
"created": "Tue, 29 Jan 2008 07:05:05 GMT"
},
{
"version": "v3",
"created": "Thu, 11 Dec 2008 15:21:40 GMT"
}
] | 2008-12-11T00:00:00 | [
[
"Zhang",
"Jinshan",
""
]
] | [
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] |
711.2401 | Genkai Zhang | Siddhartha Sahi and Genkai Zhang | Biorthogonal Expansion of Non-Symmetric Jack Functions | This is a contribution to the Proceedings of the 2007 Midwest
Geometry Conference in honor of Thomas P. Branson, published in SIGMA
(Symmetry, Integrability and Geometry: Methods and Applications) at
http://www.emis.de/journals/SIGMA/ | SIGMA 3 (2007), 106, 9 pages | 10.3842/SIGMA.2007.106 | null | math.CA math.RT | null | We find a biorthogonal expansion of the Cayley transform of the non-symmetric
Jack functions in terms of the non-symmetric Jack polynomials, the coefficients
being Meixner-Pollaczek type polynomials. This is done by computing the
Cherednik-Opdam transform of the non-symmetric Jack polynomials multiplied by
the exponential function.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:21:45 GMT"
}
] | 2008-04-25T00:00:00 | [
[
"Sahi",
"Siddhartha",
""
],
[
"Zhang",
"Genkai",
""
]
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] |
711.2402 | J. Schaffner-Bielich | Irina Sagert, Mirjam Wietoska, Jurgen Schaffner-Bielich, Christian
Sturm | Neutron star versus heavy-ion data: is the nuclear equation of state
hard or soft? | 10 pages, 3 figures, talk given at the International Symposium on
Exotic States of Nuclear Matter (EXOCT07), Catania, Italy, June 11-15, 2007 | null | null | null | astro-ph nucl-th | null | Recent astrophysical observations of neutron stars and heavy-ion data are
confronted with our present understanding of the equation of state of dense
hadronic matter. Emphasis is put on the possible role of the presence of
hyperons in the interior of compact stars. We argue that data from low-mass
pulsars provide an important cross-check between high-density astrophysics and
heavy-ion physics.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:21:55 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Sagert",
"Irina",
""
],
[
"Wietoska",
"Mirjam",
""
],
[
"Schaffner-Bielich",
"Jurgen",
""
],
[
"Sturm",
"Christian",
""
]
] | [
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711.2403 | Jens Wirth | Fumihiko Hirosawa and Jens Wirth | $C^m$-theory of damped wave equations with stabilisation | 13 pages | J. Math. Anal. Appl. 343(2):1022-1035, 2008 | 10.1016/j.jmaa.2008.02.024 | null | math.AP | null | The aim of this note is to extend the energy decay estimates from [J. Wirth,
J. Differential Equations 222 (2006) 487--514] to a broader class of
time-dependent dissipation including very fast oscillations. This is achieved
using stabilisation conditions on the coefficient in the spirit of [F.
Hirosawa, Math. Ann. 339/4 (2007) 819--839].
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:23:49 GMT"
}
] | 2010-05-17T00:00:00 | [
[
"Hirosawa",
"Fumihiko",
""
],
[
"Wirth",
"Jens",
""
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] |
711.2404 | Yota Takamura | Yota Takamura, Ryosho Nakane, Hiro Munekata and Satoshi Sugahara | Characterization of half-metallic L2_1-phase Co_2FeSi full-Heusler alloy
films formed by rapid thermal annealing | 18 pages, 5 figures | J. Appl. Phys. 103 (2008) 07D719 | 10.1063/1.2838648 | null | cond-mat.mtrl-sci | null | The authors developed a preparation technique of Co_2FeSi full-Heusler alloy
films with the L2_1-ordered structure on silicon-on-insulator (SOI) substrates,
employing rapid thermal annealing (RTA). The Co_2FeSi full-Heusler alloy films
were successfully formed by RTA-induced silicidation reaction between an
ultrathin SOI (001) layer and Fe/Co layers deposited on it. The highly
(110)-oriented L2_1-phase polycrystalline full-Heusler alloy films were
obtained at the RTA temperature of 700 C. Crystallographic and magnetic
properties of the RTA-formed full-Heusler alloy films were qualitatively the
same as those of bulk full-Heusler alloy. This technique is compatible with
metal source/drain formation process in advanced CMOS technology and would be
applicable to the fabrication of the half-metallic source/drain of MOSFET type
of spin transistors.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 14:02:14 GMT"
}
] | 2010-05-26T00:00:00 | [
[
"Takamura",
"Yota",
""
],
[
"Nakane",
"Ryosho",
""
],
[
"Munekata",
"Hiro",
""
],
[
"Sugahara",
"Satoshi",
""
]
] | [
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] |
711.2405 | Natalia Babych | Natalia O. Babych, Ilia V. Kamotski and Valery P. Smyshlyaev | Homogenization of spectral problems in bounded domains with doubly high
contrasts | 23 pages, 2 figures | null | null | null | math.SP math.AP | null | Homogenization of a spectral problem in a bounded domain with a high contrast
in both stiffness and density is considered. For a special critical scaling,
two-scale asymptotic expansions for eigenvalues and eigenfunctions are
constructed. Two-scale limit equations are derived and relate to certain
non-standard self-adjoint operators. In particular they explicitly display the
first two terms in the asymptotic expansion for the eigenvalues, with a
surprising bound for the error of order \epsilon^{5/4} proved.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:26:21 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Babych",
"Natalia O.",
""
],
[
"Kamotski",
"Ilia V.",
""
],
[
"Smyshlyaev",
"Valery P.",
""
]
] | [
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] |
711.2406 | Matthias Bergner | Matthias Bergner, Jens Dittrich | On Surfaces of Prescribed Weighted Mean Curvature | null | null | null | null | math.DG math.AP | null | Utilizing a weight matrix we study surfaces of prescribed weighted mean
curvature which yield a natural generalisation to critical points of
anisotropic surface energies. We first derive a differential equation for the
normal of immersions with prescribed weighted mean curvature, generalising a
result of Clarenz and von der Mosel. Next we study graphs of prescribed
weighted mean curvature, for which a quasilinear elliptic equation is proved.
Using this equation, we can show height and boundary gradient estimates.
Finally, we solve the Dirichlet problem for graphs of prescribed weighted mean
curvature.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:31:37 GMT"
}
] | 2007-11-16T00:00:00 | [
[
"Bergner",
"Matthias",
""
],
[
"Dittrich",
"Jens",
""
]
] | [
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] |
711.2407 | S. A. Tarasenko | S.A. Tarasenko | Electron scattering in quantum wells subjected to an in-plane magnetic
field | 5 pages, 1 figure | Phys. Rev. B 77, 085328 (2008) | 10.1103/PhysRevB.77.085328 | null | cond-mat.mes-hall cond-mat.mtrl-sci | null | It is shown that the electron scattering by static defects, acoustic or
optical phonons in quantum wells subjected to an in-plane magnetic field is
asymmetric. The probability of scattering contains terms which are proportional
to both the electron wave vector and the magnetic field components. The terms
under study are caused by the lack of an inversion center in quantum wells due
to structure or bulk inversion asymmetry although they are of pure diamagnetic
origin. Such a magnetic field induced asymmetry of scattering can be
responsible for a number of phenomena. In particular, the asymmetry of
inelastic electron-phonon interaction leads to an electric current flow if only
the electron gas is driven out of thermal equilibrium with the crystal lattice.
| [
{
"version": "v1",
"created": "Thu, 15 Nov 2007 13:35:15 GMT"
}
] | 2009-11-13T00:00:00 | [
[
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