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|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
801.2873 |
Brendon Lovett
|
Avinash Kolli, Simon C. Benjamin, Brendon W. Lovett, Thomas M. Stace
|
Measurement-based approach to entanglement generation in coupled quantum
dots
| null |
Phys. Rev. B 79, 035315 (2009)
|
10.1103/PhysRevB.79.035315
| null |
quant-ph
| null |
Measurements provide a novel mechanism for generating the entanglement
resource necessary for performing scalable quantum computation. Recently, we
proposed a method for performing parity measurements in a coupled quantum dot
system. In this paper we generalise this scheme and perform a comprehensive
analytic and numerical study of environmental factors. We calculate the effects
of possible error sources including non-ideal photon detectors, ineffective
spin-selective excitation and dot distinguishability (both spatial and
spectral). Furthermore, we present an experimental approach for verifying the
success of the parity measurement.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 12:28:54 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Kolli",
"Avinash",
""
],
[
"Benjamin",
"Simon C.",
""
],
[
"Lovett",
"Brendon W.",
""
],
[
"Stace",
"Thomas M.",
""
]
] |
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] |
801.2874 |
Georg Kreyerhoff
|
Saul Barshay and Georg Kreyerhoff
|
Uses of a small field value which falls from a metastable maximum over
cosmological times
|
version accepted for publication in Mod.Phys.Lett. A
|
Mod.Phys.Lett.A23:2897-2905,2008
|
10.1142/S0217732308028338
| null |
astro-ph
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We consider a small, metastable maximum vacuum expectation value $b_0$ of
order of a few eV, for a pseudoscalar Goldstone-like field, which is related to
the scalar inflaton field $\phi$ in an idealized model of a cosmological,
spontaneously-broken chiral symmetry. The b field allows for relating
semi-quantitatively three distinct quantities in a cosmological context.
(1) A very small, residual vacuum energy density or effective cosmological
constant of ~ lambda b_0^4 ~ 2.7 x 10^{-47}GeV^4, for lambda ~ 3 x 10^{-14},
the same as an empirical inflaton self-coupling.
(2) A tiny neutrino mass, less then b_0.
(3) A possible small variation downward of the proton to electron mass ratio
over cosmological time. The latter arises from the motion downward of the $b$
field over cosmological time, toward a nonzero limiting value as $t \to
\infty$. Such behavior is consistent with an equation of motion.
We argue that hypothetical b quanta, potentially inducing new long-range
forces, are absent, because of negative, effective squared mass in an equation
of motion for $b$-field fluctuations.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 12:40:35 GMT"
},
{
"version": "v2",
"created": "Tue, 8 Jul 2008 10:37:11 GMT"
},
{
"version": "v3",
"created": "Tue, 5 Aug 2008 12:48:58 GMT"
}
] | 2009-06-23T00:00:00 |
[
[
"Barshay",
"Saul",
""
],
[
"Kreyerhoff",
"Georg",
""
]
] |
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] |
801.2875 |
Laurent Tournier
|
Laurent Tournier (ICJ)
|
Integrability of exit times and ballisticity for random walks in
Dirichlet environment
| null |
Electronic Journal of Probability 14, 16 (2009) 431-451
|
10.1214/09-AIHP344
| null |
math.PR
| null |
We consider random walks in Dirichlet environment, introduced by Enriquez and
Sabot in 2006. As this distribution on environments is not uniformly elliptic,
the annealed integrability of exit times out of a given finite subset is a
non-trivial property. We provide here an explicit equivalent condition for this
integrability to happen, on general directed graphs. Such integrability
problems arise for instance from the definition of Kalikow auxiliary random
walk. Using our condition, we prove a refined version of the ballisticity
criterion given by Enriquez and Sabot.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 12:43:31 GMT"
}
] | 2013-09-20T00:00:00 |
[
[
"Tournier",
"Laurent",
"",
"ICJ"
]
] |
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] |
801.2876 |
Pierre Hily-Blant
|
Pierre Hily-Blant (IRAM), Malcolm Walmsley (INAF), G. Pineau Des
For\^ets (IAS), David Flower (PHYSICS DEPARTMENT)
|
CN in prestellar cores
|
Accepted for publication in A&A Letters
| null |
10.1051/0004-6361:20079296
| null |
astro-ph
| null |
Determining the structure of and the velocity field in prestellar cores is
essential to understanding protostellar evolution.} {We have observed the dense
prestellar cores L 1544 and L 183 in the $N = 1 \to 0$ rotational transition of
CN and \thcn in order to test whether CN is depleted in the high--density
nuclei of these cores.} {We have used the IRAM 30 m telescope to observe along
the major and minor axes of these cores. We compare these observations with the
1 mm dust emission, which serves as a proxy for the hydrogen column
density.}{We find that while CN\jone is optically thick, the distribution of
\thcn\jone intensity follows the dust emission well, implying that the CN
abundance does not vary greatly with density. We derive an abundance ratio of
$\rm [CN]/[\hh]=\dix{-9}$ in L 183 and 1-3\tdix{-9} in L 1544, which, in the
case of L 183, is similar to previous estimates obtained by sampling
lower--density regions of the core.}{We conclude that CN is not depleted
towards the high--density peaks of these cores and thus behaves like the
N-containing molecules \nnhp and \nhhh. CN is, to our knowledge, the first
C--containing molecule to exhibit this characteristic.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 12:51:04 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Hily-Blant",
"Pierre",
"",
"IRAM"
],
[
"Walmsley",
"Malcolm",
"",
"INAF"
],
[
"Forêts",
"G. Pineau Des",
"",
"IAS"
],
[
"Flower",
"David",
"",
"PHYSICS DEPARTMENT"
]
] |
[
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] |
801.2877 |
David Kuridze
|
D. Kuridze, T. V. Zaqarashvili, B. M. Shergelashvili1, and S. Poedts
|
Acoustic oscillations in a field-free cavity under solar small-scale
bipolar magnetic canopy
|
7 pages, 4 figures, accepted in Annales Geophysicae
| null |
10.5194/angeo-26-2983-2008
| null |
astro-ph
| null |
Observations show the increase of high-frequency wave power near magnetic
network cores and active regions in the solar lower atmosphere. This phenomenon
can be explained by the interaction of acoustic waves with a magnetic field. We
consider small-scale, bipolar, magnetic field canopy structure near the network
cores and active regions overlying field-free cylindrical cavities of the
photosphere. Solving the plasma equations we get the analytical dispersion
relation of acoustic oscillations in the field-free cavity area. We found that
the m = 1 mode, where m is azimuthal wave number, cannot be trapped under the
canopy due to energy leakage upwards. However, higher ($m \geq 2$) harmonics
can be easily trapped leading to the observed acoustic power halos under the
canopy.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:00:47 GMT"
}
] | 2015-05-13T00:00:00 |
[
[
"Kuridze",
"D.",
""
],
[
"Zaqarashvili",
"T. V.",
""
],
[
"Shergelashvili1",
"B. M.",
""
],
[
"Poedts",
"S.",
""
]
] |
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] |
801.2878 |
Pablo Linares
|
A. Ibort, P. Linares, J. G. Llavona
|
Continuous multilinear functionals on $C(K)$-spaces are integral
|
This paper has been withdrawn
| null | null | null |
math.FA
| null |
This paper has been withdrawn by the authors, due to a crucial error.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:00:49 GMT"
},
{
"version": "v2",
"created": "Thu, 24 Jan 2008 09:58:59 GMT"
}
] | 2008-01-24T00:00:00 |
[
[
"Ibort",
"A.",
""
],
[
"Linares",
"P.",
""
],
[
"Llavona",
"J. G.",
""
]
] |
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-0.0232909694,
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-0.1006805152,
0.0567982085
] |
801.2879 |
Amir Kalev
|
Amir Kalev, Sergio Rivera, and Pier A. Mello
|
Quantum Teleportation and Hidden Variables
|
25 pages
| null | null | null |
quant-ph
| null |
In this paper we address the question as to what extent the
quantum-mechanical nature of the process is relevant for teleportation of A
spin-1/2 state. For this purpose we analyze the possibility of underpinning
teleportation with a local-hidden-variable model. The nature of the models,
which we consider as legitimate candidates, guarantees the classical character
of all the probabilities which can be deduced from them. When we try to
describe the teleportation process following two different mathematical routes,
we find two different hidden-variable densities, which thus end up having a
doubtful physical significance within the "reality" that a hidden-variable
model tries to restore. This result we consider as a "no-go theorem" for the
hidden-variable description of the teleportation process. We also show that
this kind of conflict arises when considering successive measurements (one of
which is selective projective) for one spin-1/2 particle.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:07:24 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Kalev",
"Amir",
""
],
[
"Rivera",
"Sergio",
""
],
[
"Mello",
"Pier A.",
""
]
] |
[
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-0.0072004125,
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] |
801.288 |
Winfried Leidemann
|
Sara Della Monaca, Victor D. Efros, Avas Khugaev, Winfried Leidemann,
Giuseppina Orlandini, Edward L. Tomusiak, and Luping P. Yuan
|
The Transverse Electron Scattering Response Function of 3He
|
21 pages, 4 figures
|
Phys.Rev.C77:044007,2008
|
10.1103/PhysRevC.77.044007
| null |
nucl-th
| null |
The transverse response function R_T(q,omega) for 3He is calculated using the
configuration space BonnA nucleon-nucleon potential, the Tucson-Melbourne
three-body force, and the Coulomb potential. Final states are completely taken
into account via the Lorentz integral transform technique. Non-relativistic
one-body currents plus two-body pi- and rho-meson exchange currents as well as
the Siegert operator are included. The response R_T is calculated for q=174,
250, 400, and 500 MeV/c and in the threshold region at q=174, 324, and 487
MeV/c. Strong MEC effects are found in low- and high-energy tails, but due to
MEC there are also moderate enhancements of the quasi-elastic peak (6%-10%).
The calculation is performed both directly and via transformation of electric
multipoles to a form that involves the charge operator. The contribution of the
latter operator is suppressed in and below the quasielastic peak while at
higher energies the charge operator represents almost the whole MEC
contribution at the lowest q value. The effect of the Coulomb force in the
final state interaction is investigated for the threshold region at q=174
MeV/c. Its neglect enhances R_T by more than 10% in the range up to 2 MeV above
threshold. In comparison to experimental data one finds relatively good
agreement at q=250 and 400 MeV/c, while at q=500 MeV/c, presumably due to
relativistic effects, the theoretical quasi-elastic peak position is shifted to
somewhat higher energies. The strong MEC contributions in the threshold region
are nicely confirmed by data at q=324 and 487 MeV/c.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:27:17 GMT"
}
] | 2008-11-26T00:00:00 |
[
[
"Della Monaca",
"Sara",
""
],
[
"Efros",
"Victor D.",
""
],
[
"Khugaev",
"Avas",
""
],
[
"Leidemann",
"Winfried",
""
],
[
"Orlandini",
"Giuseppina",
""
],
[
"Tomusiak",
"Edward L.",
""
],
[
"Yuan",
"Luping P.",
""
]
] |
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] |
801.2881 |
Jeremy Dunning-Davies
|
J. Dunning-Davies
|
Mathematics as the language of physics
|
5 pages
| null | null | null |
physics.gen-ph
| null |
Courses in mathematical methods for physics students are not known for
including too much in the way of mathematical rigour and, in some ways,
understandably so. However, the conditions under which some quite commonly used
mathematical expressions are valid can be of great importance in some physical
circumstances. Here one such expression, which figures frequently in the
manipulations leading to the isothermal compressibility appearing in formulae,
is examined as an illustrative example.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:32:35 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Dunning-Davies",
"J.",
""
]
] |
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] |
801.2882 |
Ioannis Karafyllidis G.
|
Ioannis G. Karafyllidis
|
Quantum Mechanical Model for Information Transfer from DNA to Protein
|
22 pages, 2figures
| null | null | null |
quant-ph
| null |
A model for the information transfer from DNA to protein using quantum
information and computation techniques is presented. DNA is modeled as the
sender and proteins are modeled as the receiver of this information. On the DNA
side, a 64-dimensional Hilbert space is used to describe the information stored
in DNA triplets (codons). A Hamiltonian matrix is constructed for this space,
using the 64 possible codons as base states. The eigenvalues of this matrix are
not degenerate. The genetic code is degenerate and proteins comprise only 20
different amino acids. Since information is conserved, the information on the
protein side is also described by a 64-dimensional Hilbert space, but the
eigenvalues of the corresponding Hamiltonian matrix are degenerate. Each amino
acid is described by a Hilbert subspace. This change in Hilbert space structure
reflects the nature of the processes involved in information transfer from DNA
to protein.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:33:26 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Karafyllidis",
"Ioannis G.",
""
]
] |
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] |
801.2883 |
Roland Triay
|
Roland Triay (CPT), Henri-Hugues Fliche (LMMT)
|
Voids in the distribution of galaxies and the Cosmological constant
|
4 pages, 1 figure
|
Prog.Theor.Phys.Suppl.172:40-43,2008
|
10.1143/PTPS.172.40
|
CPT-P002-2008
|
gr-qc astro-ph
| null |
With the motivation in mind to evaluate the contribution of the cosmological
constant $\Lambda$ on the foam like patterns formation process in the
distribution of galaxies, we investigate the Newtonian dynamics of a spherical
void embedded in an uniform medium which undergoes a Hubble expansion. We use a
covariant approach for deriving the evolution with time of the shell (S) acting
as a boundaries condition for the inside and outside media. As a result, with
the usual values for the cosmological parameters, S expands with a huge initial
burst that freezes up to matching Hubble flow. With respect to Friedmann
comoving frame, its magnification increases nonlinearly with $\Lambda$, with a
maximal growth rate at redshift $z\sim 1.7$. The velocity field inside S shows
an interesting feature which enables us to disentangle a spatially closed from
open universe. Namely, the void region are swept out in the first case, what
can be interpreted as a stability criterion.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:37:04 GMT"
}
] | 2008-11-26T00:00:00 |
[
[
"Triay",
"Roland",
"",
"CPT"
],
[
"Fliche",
"Henri-Hugues",
"",
"LMMT"
]
] |
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] |
801.2884 |
Thomas Wiegelmann
|
T. Wiegelmann, J.K. Thalmann, C.J. Schrijver, M.L. DeRosa, T.R.
Metcalf
|
Preprocessing of Hinode/SOT vector magnetograms for nonlinear force-free
coronal magnetic field modelling
|
2 pages, 1 figure, ASP Conference Series, Hinode Science Meeting,
Dublin, 20-24th August 2007
| null | null | null |
astro-ph
| null |
The solar magnetic field is key to understanding the physical processes in
the solar atmosphere.
Nonlinear force-free codes have been shown to be useful in extrapolating the
coronal field from underlying vector boundary data [see Schrijver et al. 2006
for an overview]. However, we can only measure the magnetic field vector
routinely with high accuracy in the photosphere with, e.g., Hinode/SOT, and
unfortunately these data do not fulfill the force-free consistency condition as
defined by Aly (1989). We must therefore apply some transformations to these
data before nonlinear force-free extrapolation codes can be legitimately
applied. To this end, we have developed a minimization procedure that uses the
measured photospheric field vectors as input to approximate a more
chromospheric like field The method was dubbed preprocessing. See Wiegelmann et
al. 2006 for details]. The procedure includes force-free consistency integrals
and spatial smoothing. The method has been intensively tested with model active
regions [see Metcalf et al. 2008] and been applied to several ground based
vector magnetogram data before. Here we apply the preprocessing program to
photospheric magnetic field measurements with the Hinode/SOT instrument.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:41:58 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Wiegelmann",
"T.",
""
],
[
"Thalmann",
"J. K.",
""
],
[
"Schrijver",
"C. J.",
""
],
[
"DeRosa",
"M. L.",
""
],
[
"Metcalf",
"T. R.",
""
]
] |
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] |
801.2885 |
Wung-Hong Huang
|
Wung-Hong Huang
|
Chiral Dynamics and Meson with Non-commutative Dipole Field in
Gauge/Gravity Dual
|
Latex 12 pages, typos corrected, detail several points
|
Phys.Lett.B665:271-276,2008
|
10.1016/j.physletb.2008.05.069
| null |
hep-th
| null |
Apply the T-duality and smeared twist to the D3-brane solution one can
construct the supergravity backgrounds which may dual to supersymmetric or
non-supersymmetric non-commutative dipole field theory. We introduce D7-brane
probe into the dual supergravity background to study the chiral dynamics and
meson spectrum therein. We first find that the non-commutative dipole field
does not induce the chiral symmetry breaking even if the supersymmetry was
completely broken, contrast to the conventional believing that the chiral
symmetry will be broken in the non-supersymmetric theory. Next, we find that
the dipole field does not modify the meson spectrum in the supersymmetric
theory while it will reduce the meson bound-state energy in the
non-supersymmetric theory. We also evaluate the static quark anti-quark
potential and see that the dipole field has an effect to produce attractive
force between the quark and anti-quark.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:42:38 GMT"
},
{
"version": "v2",
"created": "Mon, 3 Mar 2008 02:49:21 GMT"
},
{
"version": "v3",
"created": "Fri, 25 Apr 2008 23:40:53 GMT"
}
] | 2008-11-26T00:00:00 |
[
[
"Huang",
"Wung-Hong",
""
]
] |
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] |
801.2886 |
Antonella Natta
|
T. Gatti, A. Natta, S. Randich, L. Testi and G. Sacco
|
Accretion properties of T Tauri stars in sigma Ori
|
Astronomy and Astrophysics, accepted
| null |
10.1051/0004-6361:20078971
| null |
astro-ph
| null |
Accretion disks around young stars evolve in time with time scales of few
million years. We present here a study of the accretion properties of a sample
of 35 stars in the ~3 million year old star-forming region sigma Ori. Of these,
31 are objects with evidence of disks, based on their IR excess emission. We
use near-IR hydrogen recombination lines (Pa_gamma) to measure their mass
accretion rate. We find that the accretion rates are significantly lower in
sigma Ori than in younger regions, such as rho-Oph, consistently with viscous
disk evolution. The He I 1.083 micron line is detected (either in absorption or
in emission) in 72% of the stars with disks, providing evidence of
accretion-powered activity also in very low accretors, where other accretion
indicators dissapear.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:51:42 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Gatti",
"T.",
""
],
[
"Natta",
"A.",
""
],
[
"Randich",
"S.",
""
],
[
"Testi",
"L.",
""
],
[
"Sacco",
"G.",
""
]
] |
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0.0439410135,
-0.0456776023,
-0.055465661,
0.103932336,
-0.0164186787,
-0.0984594449,
0.0311533883,
-0.0509663112,
-0.0072489516,
0.0309955161,
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-0.0485982336,
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-0.0579389893,
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-0.0221810024,
-0.0150109865,
-0.0231282339
] |
801.2887 |
Stephen Sangwine
|
Stephen J. Sangwine
|
Canonic form of linear quaternion functions
|
4 pages
| null | null | null |
math.RA
| null |
The general linear quaternion function of degree one is a sum of terms with
quaternion coefficients on the left and right. The paper considers the canonic
form of such a function, and builds on the recent work of Todd Ell, who has
shown that any such function may be represented using at most four quaternion
coefficients. In this paper, a new and simple method is presented for obtaining
these coefficients numerically using a matrix approach which also gives an
alternative proof of the canonic forms.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 13:58:59 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Sangwine",
"Stephen J.",
""
]
] |
[
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-0.1218646392,
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] |
801.2888 |
Philippe Lauren\c{c}ot
|
Jos\'e A. Carrillo, Philippe Lauren\c{c}ot, and Jes\'us Rosado
|
Fermi-Dirac-Fokker-Planck equation: well-posedness and long-time
asymptotics
| null | null | null | null |
math.AP
| null |
A Fokker-Planck type equation for interacting particles with exclusion
principle is analysed. The nonlinear drift gives rise to mathematical
difficulties in controlling moments of the distribution function. Assuming
enough initial moments are finite, we can show the global existence of weak
solutions for this problem. The natural associated entropy of the equation is
the main tool to derive uniform in time a priori estimates for the kinetic
energy and entropy. As a consequence, long-time asymptotics in $L^1$ are
characterized by the Fermi-Dirac equilibrium with the same initial mass. This
result is achieved without rate for any constructed global solution and with
exponential rate due to entropy/entropy-dissipation arguments for initial data
controlled by Fermi-Dirac distributions. Finally, initial data below radial
solutions with suitable decay at infinity lead to solutions for which the
relative entropy towards the Fermi-Dirac equilibrium is shown to converge to
zero without decay rate.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:25:10 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Carrillo",
"José A.",
""
],
[
"Laurençot",
"Philippe",
""
],
[
"Rosado",
"Jesús",
""
]
] |
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] |
801.2889 |
Moshe Schechter
|
M. Schechter and P. C. E. Stamp
|
The low-$T$ phase diagram of ${\rm LiHo_xY_{1-x}F_4}$
|
19 pages, 10 figures, predictions regarding magnetic resonance
experiments are added, presentation improved
|
Phys. Rev. B 78, 054438 (2008)
|
10.1103/PhysRevB.78.054438
| null |
cond-mat.str-el cond-mat.dis-nn
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The ${\rm LiHo_xY_{1-x}F_4}$ compound is widely considered to be the
archetypal dipolar Quantum Ising system, with longitudinal dipolar interactions
$V_{ij}^{zz}$ between ${\rm Ho}$ spins $\{i,j \}$ competing with transverse
field-induced tunneling, to give a T=0 quantum phase transition. By varying the
${\rm Ho}$ concentration x, the typical strength $V_0$ of $V_{ij}^{zz}$ can be
varied over many orders of magnitude; and so can the transverse field
$H_{\perp}$. A new effective Hamiltonian is derived, starting from the
electronuclear degrees of freedom, and valid at low and intermediate
temperatures. For any such dipolar Quantum Ising system, the hyperfine
interaction will dominate the physics at low temperatures, even if its strength
$A_0 < V_0$: one must therefore go beyond an electronic transverse field
Quantum Ising model. We derive the full phase diagram of this system, including
all nuclear levels, as a function of transverse field $H_{\perp}$, temperature
$T$, and dipole concentration x. For ${\rm LiHo_xY_{1-x}F_4}$ we predict a
re-entrant critical field as a function of x. We also predict the phase diagram
for x$=0.045$, and the behavior of the system in magnetic resonance and $\mu$SR
experiments.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:40:31 GMT"
},
{
"version": "v2",
"created": "Wed, 11 Jun 2008 02:46:41 GMT"
}
] | 2008-08-27T00:00:00 |
[
[
"Schechter",
"M.",
""
],
[
"Stamp",
"P. C. E.",
""
]
] |
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-0.0669373721,
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0.0450297147,
0.0421151705,
0.0663058907,
-0.0815100968,
-0.0429166704,
-0.0137712238,
0.0542105287,
0.119399175,
0.0586794987,
-0.0652858019,
0.0736408308,
-0.116873242,
-0.0168072078,
0.1125985757,
0.1590369791,
0.0580965914,
0.0079664225,
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0.1183305159,
-0.1373722106,
0.0529961362,
0.0375733376,
-0.056979347,
-0.0194788724,
0.0500815921,
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0.0136619275,
0.0109173981,
0.0792270377,
-0.0372575969,
-0.0593109839,
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-0.0222355463,
-0.0520246215,
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-0.0989002138,
0.0247007664,
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0.1043406948,
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-0.0950627327,
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] |
801.289 |
Abolfazl Ramezanpour
|
L. Dall'Asta, A. Ramezanpour and R. Zecchina
|
Entropy landscape and non-Gibbs solutions in constraint satisfaction
problems
|
38 pages, 10 figures
|
Phys. Rev. E 77, 031118 (2008)
|
10.1103/PhysRevE.77.031118
| null |
cond-mat.stat-mech cs.CC
| null |
We study the entropy landscape of solutions for the bicoloring problem in
random graphs, a representative difficult constraint satisfaction problem. Our
goal is to classify which type of clusters of solutions are addressed by
different algorithms. In the first part of the study we use the cavity method
to obtain the number of clusters with a given internal entropy and determine
the phase diagram of the problem, e.g. dynamical, rigidity and SAT-UNSAT
transitions. In the second part of the paper we analyze different algorithms
and locate their behavior in the entropy landscape of the problem. For instance
we show that a smoothed version of a decimation strategy based on Belief
Propagation is able to find solutions belonging to sub-dominant clusters even
beyond the so called rigidity transition where the thermodynamically relevant
clusters become frozen. These non-equilibrium solutions belong to the most
probable unfrozen clusters.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:11:10 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Dall'Asta",
"L.",
""
],
[
"Ramezanpour",
"A.",
""
],
[
"Zecchina",
"R.",
""
]
] |
[
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] |
801.2891 |
Jason Kumar
|
Jason Kumar, Arvind Rajaraman and James D. Wells
|
Probing CP-violation at colliders through interference effects in
diboson production and decay
|
4 pages, 1 figure, LaTeX
|
Phys.Rev.D78:035014,2008
|
10.1103/PhysRevD.78.035014
| null |
hep-ph hep-ex
| null |
We define a CP-asymmetric observable that is sensitive to CP-violating
interactions in the gauge-boson sector. We illustrate the utility of this
observable by studying how well the LHC can measure the coefficient of a
particular dimension-six WWZ operator. We find that sensitivity at the 10^{-3}
level is possible at the LHC with 100 fb^{-1} of integrated luminosity, which
would greatly exceed the sensitivity achieved at LEP, and would rival or may
even better the indirect sensitivities inferred from related operators
constrained by electric dipole moment experiments.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 20:06:02 GMT"
}
] | 2008-11-26T00:00:00 |
[
[
"Kumar",
"Jason",
""
],
[
"Rajaraman",
"Arvind",
""
],
[
"Wells",
"James D.",
""
]
] |
[
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] |
801.2892 |
Nikolai Nikolov
|
Nikolai Nikolov and Peter Pflug
|
On the derivatives of the Lempert functions
|
to appear in the Ann. Mat. Pura Appl.
|
Ann. Mat. Pura Appl. 187 (2008), 547-553
| null | null |
math.CV
| null |
We show that if the Kobayashi--Royden metric of a complex manifold is
continuous and positive at a given point and any non-zero tangent vector, then
the "derivatives" of the higher order Lempert functions exist and equal the
respective Kobayashi metrics at the point. It is a generalization of a result
by M. Kobayashi for taut manifolds.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:18:18 GMT"
}
] | 2010-06-23T00:00:00 |
[
[
"Nikolov",
"Nikolai",
""
],
[
"Pflug",
"Peter",
""
]
] |
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] |
801.2893 |
Michael Weyrauch
|
Michael Weyrauch, Dieter Sibold
|
Transport through correlated quantum dots: An investigation using the
functional renormalization group
|
10 figures, accepted by Phys. Rev. B
| null |
10.1103/PhysRevB.77.125309
| null |
cond-mat.mtrl-sci cond-mat.str-el
| null |
Calculations using the (exact) fermionic functional renormalization group are
usually truncated at the second order of the corresponding hierarchy of coupled
ordinary differential equations. We present a method for the systematic
determination of higher order vertex functions. This method is applied to a
study of transport properties of various correlated quantum dot systems. It is
shown that for large Coulomb correlations higher order vertex functions cannot
be neglected, and a static approximation is insufficient.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:26:30 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Weyrauch",
"Michael",
""
],
[
"Sibold",
"Dieter",
""
]
] |
[
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] |
801.2894 |
Daniel Paget
|
Daniel Paget (PMC), Thierry Amand (LPCNO), J.P. Korb (PMC)
|
Light-induced nuclear quadrupolar relaxation in semiconductors
| null | null |
10.1103/PhysRevB.77.245201
| null |
quant-ph cond-mat.mtrl-sci
| null |
Light excitation of a semiconductor, known to dynamically-polarize the
nuclear spins by hyperfine contact interaction with the photoelectrons, also
generates an intrinsic nuclear depolarization mechanism. This novel relaxation
process arises from the modulation of the nuclear quadrupolar Hamiltonian by
photoelectron trapping and recombination at nearby localized states. For nuclei
near shallow donors, the usual diffusion radius is replaced by a smaller,
quadrupolar, radius. If the light excitation conditions correspond to partial
donor occupation by photoelectrons, the nuclear magnetization and the nuclear
field can be decreased by more than one order of magnitude.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:22:27 GMT"
},
{
"version": "v2",
"created": "Tue, 15 Apr 2008 06:24:29 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Paget",
"Daniel",
"",
"PMC"
],
[
"Amand",
"Thierry",
"",
"LPCNO"
],
[
"Korb",
"J. P.",
"",
"PMC"
]
] |
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] |
801.2895 |
Nikolai Nikolov
|
Nikolai Nikolov and Peter Pflug
|
Remarks on Lempert functions of balanced domains
|
to appear in the Monatsh. Math.
|
Monatsh. Math. 156 (2009), 159-165
| null | null |
math.CV
| null |
This note should clarify how the behavior of certain invariant objects
reflects the geometric convexity of balanced domains.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:22:47 GMT"
}
] | 2010-06-23T00:00:00 |
[
[
"Nikolov",
"Nikolai",
""
],
[
"Pflug",
"Peter",
""
]
] |
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] |
801.2896 |
Serge Reynaud
|
Serge Reynaud, Brahim Lamine, Loic Duchayne, Peter Wolf, Marc-Thierry
Jaekel
|
Bounds on gravitational wave backgrounds from large distance clock
comparisons
|
10 pages, 8 figures, minor amendments
|
Phys.Rev.D77:122003,2008
|
10.1103/PhysRevD.77.122003
| null |
gr-qc astro-ph quant-ph
| null |
Our spacetime is filled with gravitational wave backgrounds that constitute a
fluctuating environment created by astrophysical and cosmological sources.
Bounds on these backgrounds are obtained from cosmological and astrophysical
data but also by analysis of ranging and Doppler signals from distant
spacecraft. We propose here a new way to set bounds on those backgrounds by
performing clock comparisons between a ground clock and a remote spacecraft
equipped with an ultra-stable clock, rather than only ranging to an onboard
transponder. This technique can then be optimized as a function of the signal
to be measured and the dominant noise sources, leading to significant
improvements on present bounds in a promising frequency range where different
theoretical models are competing. We illustrate our approach using the SAGAS
project which aims to fly an ultra stable optical clock in the outer solar
system.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:29:54 GMT"
},
{
"version": "v2",
"created": "Fri, 23 May 2008 12:56:17 GMT"
}
] | 2008-11-26T00:00:00 |
[
[
"Reynaud",
"Serge",
""
],
[
"Lamine",
"Brahim",
""
],
[
"Duchayne",
"Loic",
""
],
[
"Wolf",
"Peter",
""
],
[
"Jaekel",
"Marc-Thierry",
""
]
] |
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] |
801.2897 |
Renaud Deguen
|
Renaud Deguen (LGIT), Thierry Alboussi\`ere (LGIT), Daniel Brito
(LGIT)
|
On the existence and structure of a mush at the inner core boundary of
the Earth
| null |
Physics of The Earth and Planetary Interiors 164, 1-2 (2007) 36-49
|
10.1016/j.pepi.2007.05.003
| null |
physics.geo-ph
| null |
It has been suggested about 20 years ago that the liquid close to the inner
core boundary (ICB) is supercooled and that a sizable mushy layer has developed
during the growth of the inner core. The morphological instability of the
liquid-solid interface which usually results in the formation of a mushy zone
has been intensively studied in metallurgy, but the freezing of the inner core
occurs in very unusual conditions: the growth rate is very small, and the
pressure gradient has a key role, the newly formed solid being hotter than the
adjacent liquid. We investigate the linear stability of a solidification front
under such conditions, pointing out the destabilizing role of the thermal and
solutal fields, and the stabilizing role of the pressure gradient. The main
consequence of the very small solidification rate is the importance of
advective transport of solute in liquid, which tends to remove light solute
from the vicinity of the ICB and to suppress supercooling, thus acting against
the destabilization of the solidification front. For plausible phase diagrams
of the core mixture, we nevertheless found that the ICB is likely to be
morphologically unstable, and that a mushy zone might have developed at the
ICB. The thermodynamic thickness of the resulting mushy zone can be
significant, from $\sim100$ km to the entire inner core radius, depending on
the phase diagram of the core mixture. However, such a thick mushy zone is
predicted to collapse under its own weight, on a much smaller length scale
($\lesssim 1$ km). We estimate that the interdendritic spacing is probably
smaller than a few tens of meter, and possibly only a few meters.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:30:59 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Deguen",
"Renaud",
"",
"LGIT"
],
[
"Alboussière",
"Thierry",
"",
"LGIT"
],
[
"Brito",
"Daniel",
"",
"LGIT"
]
] |
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] |
801.2898 |
Dan Maoz
|
Dan Maoz and Filippo Mannucci
|
A Search for the Progenitors of Two Type-Ia Supernovae in NGC 1316
|
MNRAS, in press
| null |
10.1111/j.1365-2966.2008.13403.x
| null |
astro-ph
| null |
Recent evidence of a young progenitor population for many Type-Ia SNe
(SNe-Ia) raises the possibility that evolved intermediate-mass progenitor stars
may be detected in pre-explosion images. NGC 1316, a radio galaxy in the Fornax
cluster, is a prolific producer of SNe-Ia, with four detected since 1980. We
analyze Hubble Space Telescope (HST) pre-explosion images of the sites of two
of the SNe-Ia that exploded in this galaxy, SN2006dd (a normal Type-Ia) and
SN2006mr (likely a subluminous, 1991bg-like, SN-Ia). Astrometric positions are
obtained from optical and near-IR ground-based images of the events. We find no
candidate point sources at either location, and set upper limits on the flux in
B, V, and I from any such progenitors. We also estimate the amount of
extinction that could be present, based on analysis of the surface-brightness
inhomogeneities in the HST images themselves. At the distance of NGC 1316, the
limits correspond to absolute magnitudes of about -5.5, -5.4, and -6.0 mag in
M_B, M_V, and M_I, respectively. Comparison to stellar evolution models argues
against the presence at the SN sites, 3 years prior to the explosion, of normal
stars with initial masses > 6 M_sun at the tip of their asymptotic-giant branch
(AGB) evolution, young post-AGB stars that had initial masses > 4 M_sun, and
post-red-giant stars of initial masses > 9 M_sun.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:31:36 GMT"
},
{
"version": "v2",
"created": "Tue, 4 Mar 2008 12:58:27 GMT"
},
{
"version": "v3",
"created": "Wed, 30 Apr 2008 15:00:47 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Maoz",
"Dan",
""
],
[
"Mannucci",
"Filippo",
""
]
] |
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-0.1557258964,
-0.0556013882,
-0.0294545591,
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-0.0874711201,
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-0.0504297763,
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-0.0110192085,
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-0.0599591918,
-0.0490909331,
-0.0054702261,
-0.0607992522,
-0.0630569085,
-0.0725600719,
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-0.1026971787,
-0.0369100794,
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0.0112029705,
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] |
801.2899 |
Jan Maas
|
Jan Maas
|
Malliavin calculus and decoupling inequalities in Banach spaces
|
17 pages
| null | null | null |
math.FA math.PR
| null |
We develop a theory of Malliavin calculus for Banach space valued random
variables. Using radonifying operators instead of symmetric tensor products we
extend the Wiener-Ito isometry to Banach spaces. In the white noise case we
obtain two sided L^p-estimates for multiple stochastic integrals in arbitrary
Banach spaces. It is shown that the Malliavin derivative is bounded on
vector-valued Wiener-Ito chaoses. Our main tools are decoupling inequalities
for vector-valued random variables. In the opposite direction we use Meyer's
inequalities to give a new proof of a decoupling result for Gaussian chaoses in
UMD Banach spaces.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:34:45 GMT"
},
{
"version": "v2",
"created": "Thu, 14 Feb 2008 14:42:15 GMT"
}
] | 2008-02-14T00:00:00 |
[
[
"Maas",
"Jan",
""
]
] |
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-0.0257725026,
0.0149287404,
0.0575363077,
0.0143221831,
0.0217989329,
-0.0696674585,
-0.0134680513,
-0.0069692214,
-0.0489454716,
0.0380521975,
-0.0579324253,
-0.0592693277,
0.1017035916,
-0.0546644442,
0.0406269692,
0.0887306929,
0.1396320015,
-0.0057344437,
0.1345814764,
0.0084237214,
-0.0557042547,
0.0303526297,
0.0689247325,
0.0878394246,
-0.0897209868,
0.0876908749,
-0.0286938809,
0.0901171044,
-0.0521886982,
-0.0503071323,
-0.0114936447,
0.063577123,
-0.0146687878,
0.0218484476,
-0.0668451041,
-0.0952666551,
-0.0244974941,
0.0036981436,
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0.0317390487,
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0.1091308296,
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0.0234081671,
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0.0229996685
] |
801.29 |
Nathan Ilten
|
Nathan Owen Ilten
|
Calculating Milnor Numbers and Versal Component Dimensions from
P-Resolution Fans
|
8 pages; 2 figures; v2 added section on Milnor numbers, reworked
proof of dimension formula, new example, and new title
|
Bolyai Soc. Math. Stud. 23 (2013) pp. 99-107
|
10.1007/978-3-642-39131-6_3
| null |
math.AG
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We use Altmann's toric fan description of P-resolutions to formulate a new
description of deformation theory invariants for two-dimensional cyclic
quotient singularities. In particular, we show how to calculate the dimensions
of the (reduced) versal base space components as well as Milnor numbers of
smoothings over them.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:40:08 GMT"
},
{
"version": "v2",
"created": "Thu, 2 Apr 2009 10:36:01 GMT"
}
] | 2019-11-26T00:00:00 |
[
[
"Ilten",
"Nathan Owen",
""
]
] |
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0.0641890541,
-0.052536536,
-0.033039324,
0.0180370659,
-0.0913305432,
-0.1192164198,
-0.0430312864,
0.0010450047,
0.0161904152,
-0.0187241938,
0.0708312765,
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-0.0155605488,
-0.0584629998,
0.0245075058
] |
801.2901 |
Haisheng Li Dr.
|
Martin Karel and Haisheng Li
|
Some quantum vertex algebras of Zamolodchikov-Faddeev type
|
37 pages
| null | null | null |
math.QA math-ph math.MP
| null |
This is a continuation of a previous study of quantum vertex algebras of
Zamolodchikov-Faddeev type. In this paper, we focus our attention on the
special case associated to diagonal unitary rational quantum Yang-Baxter
operators. We prove that the associated weak quantum vertex algebras, if not
zero, are irreducible quantum vertex algebras with a normal basis in a certain
sense.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 14:57:38 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Karel",
"Martin",
""
],
[
"Li",
"Haisheng",
""
]
] |
[
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] |
801.2902 |
Thomas Wiegelmann
|
T. Wiegelmann
|
Nonlinear force-free modeling of the solar coronal magnetic field
|
33 pages, 3 figures, Review article
|
J.Geophys.Res.113:A03S02,2008
|
10.1029/2007JA012432
| null |
astro-ph
| null |
The coronal magnetic field is an important quantity because the magnetic
field dominates the structure of the solar corona. Unfortunately direct
measurements of coronal magnetic fields are usually not available. The
photospheric magnetic field is measured routinely with vector magnetographs.
These photospheric measurements are extrapolated into the solar corona. The
extrapolated coronal magnetic field depends on assumptions regarding the
coronal plasma, e.g. force-freeness. Force-free means that all non-magnetic
forces like pressure gradients and gravity are neglected. This approach is well
justified in the solar corona due to the low plasma beta. One has to take care,
however, about ambiguities, noise and non-magnetic forces in the photosphere,
where the magnetic field vector is measured. Here we review different numerical
methods for a nonlinear force-free coronal magnetic field extrapolation:
Grad-Rubin codes, upward integration method, MHD-relaxation, optimization and
the boundary element approach. We briefly discuss the main features of the
different methods and concentrate mainly on recently developed new codes.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:10:44 GMT"
}
] | 2009-06-25T00:00:00 |
[
[
"Wiegelmann",
"T.",
""
]
] |
[
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] |
801.2903 |
Mat\'ias Reynoso M
|
Matias M. Reynoso, Gustavo E. Romero, Hugo R. Christiansen
|
Production of gamma rays and neutrinos in the dark jets of the
microquasar SS433
|
10 pages, 13 figures. Accepted for publication in MNRAS
|
Mon.Not.Roy.Astron.Soc.387:1745-1754,2008
|
10.1111/j.1365-2966.2008.13364.x
| null |
astro-ph
| null |
We study the spectral energy distribution of gamma rays and neutrinos in the
precessing microquasar SS433 as a result of pp interactions within its dark
jets. Gamma-ray absorption due to interactions with matter of the extended disk
and of the star is found to be important, as well as absorption caused by the
UV and mid-IR radiation from the equatorial envelopment. We analyze the range
of precessional phases for which this attenuation is at a minimum and the
chances for detection of a gamma-ray signal are enhanced. The power of
relativistic protons in the jets, a free parameter of the model, is constrained
by HEGRA data. This imposes limits on the gamma-ray fluxes to be detected with
instruments such as GLAST, VERITAS and MAGIC II. A future detection of high
energy neutrinos with cubic kilometer telescopes such as IceCube would also
yield important information about acceleration mechanisms that may take place
in the dark jets. Overall, the determination of the ratio of gamma-ray to
neutrino flux will result in a key observational tool to clarify the physics of
heavy jets.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 20:47:37 GMT"
},
{
"version": "v2",
"created": "Tue, 22 Apr 2008 18:04:44 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Reynoso",
"Matias M.",
""
],
[
"Romero",
"Gustavo E.",
""
],
[
"Christiansen",
"Hugo R.",
""
]
] |
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] |
801.2904 |
Tommi Eronen
|
T. Eronen, V.-V. Elomaa, U. Hager, J. Hakala, A. Jokinen, A.
Kankainen, S. Rahaman, J. Rissanen, C. Weber, J. Aysto
|
Preparing isomerically pure beams of short-lived nuclei at JYFLTRAP
|
5 pages, 7 figures, submitted to EMIS2007 Conference proceedings,
Nucl. Instrum. Meth. Phys. Res. B (2007)
|
Nucl.Instrum.Meth.B266:4527-4531,2008
|
10.1016/j.nimb.2008.05.076
| null |
nucl-ex
| null |
A new procedure to prepare isomerically clean samples of ions with a mass
resolving power of more than 100,000 has been developed at the JYFLTRAP tandem
Penning trap system. The method utilises a dipolar rf-excitation of the ion
motion with separated oscillatory fields in the precision trap. During a
subsequent retransfer to the purification trap, the contaminants are rejected
and as a consequence, the remaining bunch is isomerically cleaned. This
newly-developed method is suitable for very high-resolution cleaning and is at
least a factor of five faster than the methods used so far in Penning trap mass
spectrometry.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:26:21 GMT"
}
] | 2008-11-26T00:00:00 |
[
[
"Eronen",
"T.",
""
],
[
"Elomaa",
"V. -V.",
""
],
[
"Hager",
"U.",
""
],
[
"Hakala",
"J.",
""
],
[
"Jokinen",
"A.",
""
],
[
"Kankainen",
"A.",
""
],
[
"Rahaman",
"S.",
""
],
[
"Rissanen",
"J.",
""
],
[
"Weber",
"C.",
""
],
[
"Aysto",
"J.",
""
]
] |
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-0.0916930735,
0.0578273386,
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0.0069821454,
-0.0601170026,
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0.0416399427,
-0.0247336999,
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-0.053833738,
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-0.0349040702,
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-0.0782745704,
-0.0603299923,
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0.0230830126,
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] |
801.2905 |
Mahmoud Abdel-Aty
|
Mahmoud Abdel-Aty
|
A qualitative perspective on the dynamics of a single-Cooper-pair box
with a phase-damped cavity
|
15 pages, 4 figures, some modifications have been done
|
J. Phys. A: Math. Theor. 41 185304 (2008)
| null | null |
quant-ph
| null |
In a recent paper Dajka, et.al., [J. Phys. A \textbf{40}, F879 (2007)]
predicted that some composite systems can be entangled forever even if coupled
with a thermal bath. We analyze the transient entanglement of a
single-Cooper-pair box biased by a classical voltage and irradiated by a
quantized field and find the unusual feature that the phase-damped cavity can
lead to a long-lived entanglement. The results show an asymptotic value of the
idempotency defect (concurrence) which embodies coherence loss (entanglement
survival), independent of the interaction development by dependent critically
on environment.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:08:05 GMT"
},
{
"version": "v2",
"created": "Sat, 3 May 2008 14:20:26 GMT"
}
] | 2008-05-03T00:00:00 |
[
[
"Abdel-Aty",
"Mahmoud",
""
]
] |
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] |
801.2906 |
Marc Ribo
|
M. Ribo
|
TeV Gamma-Ray Astrophysics
|
Invited review at the Frascati Workshop 2007, Vulcano, Italy, May 28
- June 2 on "Multifrequency Behaviour of High Energy Cosmic Sources". ChJAA,
in press. 12 pages, 3 figures
| null | null | null |
astro-ph
| null |
The window of TeV Gamma-Ray Astrophysics was opened less than two decades
ago, when the Crab Nebula was detected for the first time. After several years
of development, the technique used by imaging atmospheric Cherenkov telescopes
like HESS, MAGIC or VERITAS, is now allowing to conduct sensitive observations
in the TeV regime. Water Cherenkov instruments like Milagro are also providing
the first results after years of integration time. Different types of
extragalactic and galactic sources have been detected, showing a variety of
interesting phenomena that are boosting theory in very high energy gamma-ray
astrophysics. Here I review some of the most interesting results obtained up to
now, making special emphasis in the field of X-ray/gamma-ray binaries.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:08:24 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Ribo",
"M.",
""
]
] |
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-0.0575093664,
-0.0193337072,
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-0.0189972445,
0.0363639332,
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0.0380721316,
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0.0056357626,
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0.059062276,
-0.0333875269
] |
801.2907 |
Christoph Schmid
|
Christoph Schmid
|
Mach's principle: Exact frame-dragging via gravitomagnetism in perturbed
Friedmann-Robertson-Walker universes with $K = (\pm 1, 0)$
|
23 pages, no figures. Final published version. Additional material in
Secs. I.A, I.J, III, V.H. Additional references
|
Phys.Rev.D79:064007,2009
|
10.1103/PhysRevD.79.064007
| null |
astro-ph gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We show that the dragging of the axis directions of local inertial frames by
a weighted average of the energy currents in the universe is exact for all
linear perturbations of any Friedmann-Robertson-Walker (FRW) universe with K =
(+1, -1, 0) and of Einstein's static closed universe. This includes FRW
universes which are arbitrarily close to the Milne Universe, which is empty,
and to the de Sitter universe. Hence the postulate formulated by E. Mach about
the physical cause for the time-evolution of the axis directions of inertial
frames is shown to hold in cosmological General Relativity for linear
perturbations. The time-evolution of axis directions of local inertial frames
(relative to given local fiducial axes) is given experimentally by the
precession angular velocity of gyroscopes, which in turn is given by the
operational definition of the gravitomagnetic field. The gravitomagnetic field
is caused by cosmological energy currents via the momentum constraint. This
equation for cosmological gravitomagnetism is analogous to Ampere's law, but it
holds also for time-dependent situtations. In the solution for an open universe
the 1/r^2-force of Ampere is replaced by a Yukawa force which is of identical
form for FRW backgrounds with $K = (-1, 0).$ The scale of the exponential
cutoff is the H-dot radius, where H is the Hubble rate, and dot is the
derivative with respect to cosmic time. Analogous results hold for energy
currents in a closed FRW universe, K = +1, and in Einstein's closed static
universe.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:11:50 GMT"
},
{
"version": "v2",
"created": "Thu, 3 Sep 2009 18:06:52 GMT"
}
] | 2009-09-03T00:00:00 |
[
[
"Schmid",
"Christoph",
""
]
] |
[
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-0.1031273231,
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] |
801.2908 |
Joshua Anderson
|
J.A. Anderson, C.D. Lorenz and A. Travesset
|
Micellar Crystals in Solution from Molecular Dynamics Simulations
|
12 pages, 11 figures. Note that some figures are extremely low
quality to meet arXiv's file size limits
| null |
10.1063/1.2913522
| null |
cond-mat.soft
| null |
Polymers with both soluble and insoluble blocks typically self-assemble into
micelles, aggregates of a finite number of polymers where the soluble blocks
shield the insoluble ones from contact with the solvent. Upon increasing
concentration, these micelles often form gels that exhibit crystalline order in
many systems. In this paper, we present a study of both the dynamics and the
equilibrium properties of micellar crystals of triblock polymers using
molecular dynamics simulations. Our results show that equilibration of single
micelle degrees of freedom and crystal formation occurs by polymer transfer
between micelles, a process that is described by transition state theory. Near
the disorder (or melting) transition, bcc lattices are favored for all
triblocks studied. Lattices with fcc ordering are also found, but only at lower
kinetic temperatures and for triblocks with short hydrophilic blocks. Our
results lead to a number of theoretical considerations and suggest a range of
implications to experimental systems with a particular emphasis on Pluronic
polymers.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:12:25 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Anderson",
"J. A.",
""
],
[
"Lorenz",
"C. D.",
""
],
[
"Travesset",
"A.",
""
]
] |
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] |
801.2909 |
Benne W. Holwerda
|
B. W. Holwerda, P. Kamphuis, R. J. Allen, R. F. Peletier, and P. C.
van der Kruit
|
The Vertical Dust Structure in Spiral Disks
|
4 pages, 3 figures, to appear in the proceedings of ``The Evolving
ISM in the Milky Way and Nearby Galaxies'', Pasadena, 2007
| null | null | null |
astro-ph
| null |
The halo of NGC 891 has been the subject of studies for more than a decade.
One of its most striking features is the large asymmetry in H-$\alpha$
emission. We have taken a quantitative look at this asymmetry at different
wavelengths for the first time. We propose that NGC 891 is intrinsically almost
symmetric, as seen in Spitzer observations, and the large asymmetry in
H-$\alpha$ emission is mostly due to dust attenuation. We quantify the
additional optical depth needed to cause the observed H-$\alpha$ asymmetry. A
comparison of large strips on the North East side of the galaxy with strips
covering the same area in the South West we can quantify and analyze the
asymmetry in the different wavelengths. From the 24 $\mu$m emission we find
that the intrinsic asymmetry in star-formation in NGC 891 is small i.e.,
approximately 30%. The additional asymmetry in H-alpha is modeled as additional
symmetric dust attenuation which extends up to ~ 40'' (1.9 kpc) above the plane
of the galaxy with a mid-plane value of $\tau$=0.8 and a scale height of 0.5
kpc. This observational technique offers the possibility to quantify the
effects of vertical ISM disk stability as an explanation for dust lanes in
massive galaxies Dalcanton et al. (2004).
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:41:46 GMT"
}
] | 2009-09-29T00:00:00 |
[
[
"Holwerda",
"B. W.",
""
],
[
"Kamphuis",
"P.",
""
],
[
"Allen",
"R. J.",
""
],
[
"Peletier",
"R. F.",
""
],
[
"van der Kruit",
"P. C.",
""
]
] |
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] |
801.291 |
Stefan Floerchinger
|
S. Floerchinger and C. Wetterich
|
Functional renormalization for Bose-Einstein Condensation
|
21 pages, 16 figures. Reference added
|
Phys.Rev.A77:053603,2008
|
10.1103/PhysRevA.77.053603
| null |
cond-mat.supr-con cond-mat.str-el hep-th
| null |
We investigate Bose-Einstein condensation for interacting bosons at zero and
nonzero temperature. Functional renormalization provides us with a consistent
method to compute the effect of fluctuations beyond the Bogoliubov
approximation. For three dimensional dilute gases, we find an upper bound on
the scattering length a which is of the order of the microphysical scale -
typically the range of the Van der Waals interaction. In contrast to fermions
near the unitary bound, no strong interactions occur for bosons with
approximately pointlike interactions, thus explaining the high quantitative
reliability of perturbation theory for most quantities. For zero temperature we
compute the quantum phase diagram for bosonic quasiparticles with a general
dispersion relation, corresponding to an inverse microphysical propagator with
terms linear and quadratic in the frequency. We compute the temperature
dependence of the condensate and particle density n, and find for the critical
temperature T_c a deviation from the free theory, Delta T_c/T_c = 2.1 a
n^{1/3}. For the sound velocity at zero temperature we find very good agreement
with the Bogoliubov result, such that it may be used to determine the particle
density accurately.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:34:23 GMT"
},
{
"version": "v2",
"created": "Mon, 26 May 2008 13:35:41 GMT"
}
] | 2009-01-28T00:00:00 |
[
[
"Floerchinger",
"S.",
""
],
[
"Wetterich",
"C.",
""
]
] |
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] |
801.2911 |
Leonardo Gualtieri
|
V. Ferrari, L. Gualtieri, F. Pannarale
|
A Semi-relativistic Model for Tidal Interactions in BH-NS Coalescing
Binaries
|
19 pages, 2 figures; references added
|
Class.Quant.Grav.26:125004,2009
|
10.1088/0264-9381/26/12/125004
| null |
astro-ph gr-qc
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We study the tidal effects of a Kerr black hole on a neutron star in black
hole-neutron star binary systems using a semi-analytical approach which
describes the neutron star as a deformable ellipsoid. Relativistic effects on
the neutron star self-gravity are taken into account by employing a scalar
potential resulting from relativistic stellar structure equations. We calculate
quasi-equilibrium sequences of black hole-neutron star binaries, and the
critical orbital separation at which the star is disrupted by the black hole
tidal field: the latter quantity is of particular interest because when it is
greater than the radius of the innermost stable circular orbit, a short
gamma-ray burst scenario may develop.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:24:17 GMT"
},
{
"version": "v2",
"created": "Fri, 6 Feb 2009 16:04:07 GMT"
},
{
"version": "v3",
"created": "Tue, 16 Mar 2010 15:31:05 GMT"
}
] | 2010-03-18T00:00:00 |
[
[
"Ferrari",
"V.",
""
],
[
"Gualtieri",
"L.",
""
],
[
"Pannarale",
"F.",
""
]
] |
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-0.0732992515,
-0.1588816196,
0.0220821481,
0.09272255,
-0.0177506022,
0.0062351795,
-0.1108476371,
-0.036250174,
0.01067283,
0.0152415503,
-0.003105107,
0.0434153266,
0.0214829706,
-0.0001336054,
-0.0141056115,
0.0874797553,
-0.0135314008,
-0.0163650066
] |
801.2912 |
Iver Brevik
|
Johan S. H{\o}ye, Iver Brevik, Simen A. Ellingsen and Jan B. Aarseth
|
Reply to "Comment on 'Analytic and Numerical Verification of the Nernst
Theorem for Metals'"
|
4 pages, no figures; to appear in Phys. Rev. E
| null |
10.1103/PhysRevE.77.023102
| null |
quant-ph hep-th
| null |
In this Reply to the preceding Comment of Klimchitskaya and Mostepanenko (cf.
also quant-ph/0703214), we summarize and maintain our position that the Drude
dispersion relation when inserted in the Lifshitz formula gives a
thermodynamically satisfactory description of the Casimir force, also in the
limiting case when the relaxation frequency goes to zero (perfect crystals).
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:19:33 GMT"
}
] | 2016-08-17T00:00:00 |
[
[
"Høye",
"Johan S.",
""
],
[
"Brevik",
"Iver",
""
],
[
"Ellingsen",
"Simen A.",
""
],
[
"Aarseth",
"Jan B.",
""
]
] |
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] |
801.2913 |
Julia Bernatska
|
Julia Bernatska, Petro Holod
|
Geometry and Topology of Coadjoint Orbits of Semisimple Lie Groups
|
21 pages, 1 figure, submitted to Proceedings of the 9th International
Conference on 'Geometry, Integrability and Quantization', Varna, Bulgaria,
June 8-13, 2007
|
Geometry, Integrability and Quantization IX, 2008, P.146-166
|
10.7546/giq-9-2008-146-166
| null |
math.RT math-ph math.MP
| null |
Orbits of coadjoint representations of classical compact Lie groups have a
lot of applications. They appear in representation theory, geometrical
quantization, theory of magnetism, quantum optics etc. As geometric objects the
orbits were the subject of much study. However, they remain hard for
calculation and application. We propose simple solutions for the following
problems: an explicit parameterization of the orbit by means of a generalized
stereographic projection, obtaining a K\"{a}hlerian structure on the orbit,
introducing basis two-forms for the cohomology group of the orbit.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:26:12 GMT"
},
{
"version": "v2",
"created": "Tue, 29 Jan 2008 16:40:41 GMT"
}
] | 2013-07-09T00:00:00 |
[
[
"Bernatska",
"Julia",
""
],
[
"Holod",
"Petro",
""
]
] |
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] |
801.2914 |
Gleb Oshanin
|
G.Oshanin (LPTMC, University of Paris 6, Paris, France)
|
Asymptotics for the survival probability of a Rouse chain monomer
|
6 pages, submitted to EPL
| null | null | null |
cond-mat.stat-mech math.PR
| null |
We study the long-time asymptotical behavior of the survival probability P_t
of a tagged monomer of an infinitely long Rouse chain in presence of two fixed
absorbing boundaries, placed at x = \pm L. Mean-square displacement of a tagged
monomer obeys \bar{X^2(t)} \sim t^{1/2} at all times, which signifies that its
dynamics is an anomalous diffusion process.
Constructing lower and upper bounds on P_t, which have the same
time-dependence but slightly differ by numerical factors in the definition of
the characteristic relaxation time, we show that P_t is a stretched-exponential
function of time, \ln(P_t) \sim - t^{1/2}/L^2. This implies that the
distribution function of the first exit time from a fixed interval [-L,L] for
such an anomalous diffusion has all moments.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:34:25 GMT"
}
] | 2008-01-28T00:00:00 |
[
[
"Oshanin",
"G.",
"",
"LPTMC, University of Paris 6, Paris, France"
]
] |
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-0.0118827969,
-0.08061032,
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0.022025995,
-0.047504425,
-0.0657300651,
0.0053693382
] |
801.2915 |
Sarah Casewell
|
R.F. Jameson, N. Lodieu, S.L. Casewell, N.P. Bannister, P.D. Dobbie
|
The ages of L dwarfs
|
8 pages, 5 figures. Accepted for publication in MNRAS
| null |
10.1111/j.1365-2966.2008.12973.x
| null |
astro-ph
| null |
We present a new method to derive the age of young (<0.7 Gyr) L dwarfs based
on their near-infrared photometry, colours, and distances. The method is based
on samples of L dwarfs belonging to the Upper Sco association (5 Myr), the
Alpha Per (85 Myr) and Pleiades (125 Myr) clusters, and the Ursa Major (400
Myr) and Hyades (625 Myr) moving groups. We apply our method to a number of
interesting objects in the literature, including a known L dwarf binary, L
dwarf companions, and spectroscopic members of the young sigma Orionis cluster.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:43:29 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Jameson",
"R. F.",
""
],
[
"Lodieu",
"N.",
""
],
[
"Casewell",
"S. L.",
""
],
[
"Bannister",
"N. P.",
""
],
[
"Dobbie",
"P. D.",
""
]
] |
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] |
801.2916 |
Thomas Wiegelmann
|
T. Wiegelmann, T. Neukirch, P. Ruan, B. Inhester
|
Optimization approach for the computation of magnetohydrostatic coronal
equilibria in spherical geometry
|
6 pages, 4 figures
|
Astron.Astrophys.475:701,2007
|
10.1051/0004-6361:20078244
| null |
astro-ph
| null |
Context: This paper presents a method which can be used to calculate models
of the global solar corona from observational data. Aims: We present an
optimization method for computing nonlinear magnetohydrostatic equilibria in
spherical geometry with the aim to obtain self-consistent solutions for the
coronal magnetic field, the coronal plasma density and plasma pressure using
observational data as input. Methods: Our code for the self-consistent
computation of the coronal magnetic fields and the coronal plasma solves the
non-force-free magnetohydrostatic equilibria using an optimization method.
Previous versions of the code have been used to compute non-linear force-free
coronal magnetic fields from photospheric measurements in Cartesian and
spherical geometry, and magnetostatic-equilibria in Cartesian geometry. We test
our code with the help of a known analytic 3D equilibrium solution of the
magnetohydrostatic equations. The detailed comparison between the numerical
calculations and the exact equilibrium solutions is made by using magnetic
field line plots, plots of density and pressure and some of the usual
quantitative numerical comparison measures. Results: We find that the method
reconstructs the equilibrium accurately, with residual forces of the order of
the discretisation error of the analytic solution. The correlation with the
reference solution is better than 99.9% and the magnetic energy is computed
accurately with an error of <0.1%. Conclusions: We applied the method so far to
an analytic test case. We are planning to use this method with real
observational data as input as soon as possible.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:46:44 GMT"
}
] | 2009-06-25T00:00:00 |
[
[
"Wiegelmann",
"T.",
""
],
[
"Neukirch",
"T.",
""
],
[
"Ruan",
"P.",
""
],
[
"Inhester",
"B.",
""
]
] |
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] |
801.2917 |
Matthew R. Burleigh
|
M.R. Burleigh (1), F.J. Clarke (2), E. Hogan (1), C.S. Brinkworth (3),
P. Bergeron (4), P. Dufour (5), P.D. Dobbie (6), A.J. Levan (7), S.T. Hodgkin
(8), D.W. Hoard (3), S. Wachter (3) ((1) Department of Physics and Astronomy,
University of Leicester, UK; (2) Department of Astrophysics, University of
Oxford, UK; (3) Spitzer Science Center, USA; (4) D\'epartment de Physique,
Universit\'e de Montr\'eal, Canada; (5) Department of Astronomy and Steward
Observatory, University of Arizona, USA; (6) Anglo-Australian Observatory,
Australia; (7) Department of Physics, University of Warwick, UK; (8)
Institute of Astronomy, University of Cambridge, UK)
|
The "DODO" survey I: limits on ultra-cool substellar and planetary-mass
companions to van Maanen's star (vMa 2)
|
Accepted for publication in MNRAS Letters
|
Mon.Not.Roy.Astron.Soc.386:L5-L9,2008
|
10.1111/j.1745-3933.2008.00446.x
| null |
astro-ph
| null |
We report limits in the planetary-mass regime for companions around the
nearest single white dwarf to the Sun, van Maanen's star (vMa 2), from deep
J-band imaging with Gemini North and Spitzer IRAC mid-IR photometry. We find no
resolved common proper motion companions to vMa 2 at separations from 3" - 45",
at a limiting magnitude of J~23. Assuming a total age for the system of 4.1
+/-1 Gyr, and utilising the latest evolutionary models for substellar objects,
this limit is equivalent to companion masses >7 +/-1 Mjup (T~300K). Taking into
account the likely orbital evolution of very low mass companions in the
post-main sequence phase, these J-band observations effectively survey orbits
around the white dwarf progenitor from 3 - 50AU. There is no flux excess
detected in any of the complimentary Spitzer IRAC mid-IR filters. We fit a DZ
white dwarf model atmosphere to the optical BVRI, 2MASS JHK and IRAC
photometry. The best solution gives T=6030 +/- 240K, log g=8.10 +/-0.04 and,
hence, M= 0.633 +/-0.022Msun. We then place a 3sigma upper limit of 10 +/-2
Mjup on the mass of any unresolved companion in the 4.5 micron band.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:53:19 GMT"
}
] | 2009-12-08T00:00:00 |
[
[
"Burleigh",
"M. R.",
""
],
[
"Clarke",
"F. J.",
""
],
[
"Hogan",
"E.",
""
],
[
"Brinkworth",
"C. S.",
""
],
[
"Bergeron",
"P.",
""
],
[
"Dufour",
"P.",
""
],
[
"Dobbie",
"P. D.",
""
],
[
"Levan",
"A. J.",
""
],
[
"Hodgkin",
"S. T.",
""
],
[
"Hoard",
"D. W.",
""
],
[
"Wachter",
"S.",
""
]
] |
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] |
801.2918 |
Moncef Derouich
|
M. Derouich
|
Evidence for collisional depolarization of the \ion{Ba}{ii}
${\lambda}4554$ line in the low chromosphere
|
12 pages, 4 figures, accepted for publication in A&A
| null |
10.1051/0004-6361:20078888
| null |
astro-ph
| null |
Context. Rigorous modeling of the \ion{Ba}{ii} ${\lambda}4554$ formation is
potentially interesting since this strongly polarized line forms in the solar
chromosphere where the magnetic field is rather poorly known. Aims. To
investigate the role of isotropic collisions with neutral hydrogen in the
formation of the polarized \ion{Ba}{ii} ${\lambda}4554$ line and, thus, in the
determination of the magnetic field. Methods. Multipole relaxation and transfer
rates of the $d$ and p-states of \ion{Ba}{ii} by isotropic collisions with
neutral hydrogen are calculated. We consider a plane parallel layer of
\ion{Ba}{ii} situated at the low chromosphere and anisotropically illuminated
from below which produces linear polarization in the ${\lambda}4554$ line by
scattering processes. To compute that polarization, we solve the statistical
equilibrium equations for \ion{Ba}{ii} levels including collisions, radiation
and magnetic field effects. Results. Variation laws of the relaxation and
transfer rates with hydrogen number density $n_{\textrm {\scriptsize H}}$ and
temperature are deduced. The polarization of the ${\lambda}4554$ line is
clearly affected due to isotropic collisions with neutral hydrogen although the
collisional depolarization of its upper level $^2P_{3/2}$ is negligible. This
is because the alignment of the metastable levels $^2D_{3/2}$ and $^2D_{5/2}$
of the \ion{Ba}{ii} are vulnerable to collisions. At the height of formation of
the ${\lambda}4554$ line where $n_{\textrm {\scriptsize H}} \sim 2 \times
10^{14}$ cm$^{-3}$, we find that the neglecting of the collisions induces
inaccuracy of $\sim$ 25% on the calculation of the polarization and $\sim$ 35 %
inaccuracy on microturbulent magnetic field determination.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 15:55:46 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Derouich",
"M.",
""
]
] |
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-0.0763546303,
0.0607912391,
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] |
801.2919 |
Yuri Bonder
|
Y. Bonder
|
A Lorentz Invariant Phenomenological Model of Quantum Gravity
|
7 pages. Talk presented at "From Quantum to Emergent Gravity: Theory
and Phenomenology," June 2007, Trieste, Italy
| null | null | null |
gr-qc
| null |
We consider a model of Quantum Gravity phenomenology, based on the idea that
space-time may have some unknown granular structure that respects the Lorentz
symmetry. The proposal involves non-trivial couplings of curvature to matter
fields and leads to a well defined phenomenology. In this manuscript, a brief
description of the model is presented together with some results obtained using
linearized gravity and the Newtonian limit, which could be useful when
comparing with real experiments.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:04:15 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Bonder",
"Y.",
""
]
] |
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] |
801.292 |
Antonella De Ninno
|
A.De Ninno, M. Prosdocimi, V. Ferrari, G. Gerardi, F. Barbaro, T.
Badon, D. Bernardini
|
Effect of ELF e.m. fields on metalloprotein redox-active sites
|
18 pages, 4 figures
| null | null | null |
physics.bio-ph physics.gen-ph
| null |
The peculiarity of the distribution and geometry of metallic ions in enzymes
pushed us to set the hypothesis that metallic ions in active-site act like tiny
antennas able to pick up very feeble e.m. signals. Enzymatic activity of Cu2+,
Zn2+ Superoxide Dismutase (SOD1) and Fe2+ Xanthine Oxidase (XO) has been
studied, following in vitro generation and removal of free radicals. We
observed that Superoxide radicals generation by XO is increased by a weak field
having the Larmor frequency fL of Fe2+ while the SOD1 kinetics is sensibly
reduced by exposure to a weak field having the frequency fL of Cu2+ ion.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:05:10 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"De Ninno",
"A.",
""
],
[
"Prosdocimi",
"M.",
""
],
[
"Ferrari",
"V.",
""
],
[
"Gerardi",
"G.",
""
],
[
"Barbaro",
"F.",
""
],
[
"Badon",
"T.",
""
],
[
"Bernardini",
"D.",
""
]
] |
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] |
801.2921 |
V. M. Krasnov
|
S. O. Katterwe, A. Rydh and V. M. Krasnov
|
Crossover from Thermal Activation to Quantum Interlayer Transport at the
Superconducting Transition Temperature of Bi-2212
|
10 pages, 10 figures
|
Phys. Rev. Lett. 101, 087003 (2008)
| null | null |
cond-mat.supr-con
| null |
We perform a detailed study of temperature, bias and doping dependance of
interlayer transport in the layered high temperature superconductor
Bi$_2$Sr$_2$CaCu$_2$O$_{8+\delta}$. We observe that the shape of interlayer
characteristics in underdoped crystals exhibit a remarkable crossover at the
superconducting transition temperature: from thermal activation-type at
$T>T_c$, to almost $T-$independent quantum tunneling-type, at $T<T_c$. Our data
indicates that the interlayer transport mechanism may change with doping: from
the conventional single quasiparticle tunneling in overdoped, to a
progressively increasing Cooper pair contribution in underdoped crystals.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:29:06 GMT"
}
] | 2008-08-25T00:00:00 |
[
[
"Katterwe",
"S. O.",
""
],
[
"Rydh",
"A.",
""
],
[
"Krasnov",
"V. M.",
""
]
] |
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0.0051930314
] |
801.2922 |
ZhenGang Zhu
|
Zhen-Gang Zhu
|
Selective Spin Injection Controlled by Electrical way in
Ferromagnet/Quantum Dot/Semiconductor system
| null |
Physics Letters A 372, 695 (2008)
|
10.1016/j.physleta.2007.07.081
| null |
cond-mat.mes-hall
| null |
Selective and large polarization of current injected into semiconductor (SC)
is predicted in Ferromagnet (FM)/Quantum Dot (QD)/SC system by varying the gate
voltage above the Kondo temperature. In addition, spin-dependent Kondo effect
is also revealed below Kondo temperature. It is found that Kondo resonances for
up spin state is suppressed with increasing of the polarization P of the FM
lead. While the down one is enhanced. The Kondo peak for up spin is disappear
at P=1.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:16:15 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Zhu",
"Zhen-Gang",
""
]
] |
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-0.0414153486,
-0.0542237051,
0.0435583815,
-0.1393469423,
0.0244829003,
0.0035260359,
-0.0061581032
] |
801.2923 |
Alain Coc
|
Alain Coc
|
Nucleosynthesis in novae: experimental progress in the determination of
nuclear reaction rates
|
Invited contribution to the "Origin of Matter and Evolution of
Galaxies" conference (OMEG07) with additional and color figures
|
AIP Conf.Proc.1016:119-126,2008
|
10.1063/1.2943561
| null |
astro-ph
| null |
The sources of nuclear uncertainties in nova nucleosynthesis have been
identified using hydrodynamical nova models. Experimental efforts have followed
and significantly reduced those uncertainties. This is important for the
evaluation of nova contribution to galactic chemical evolution, gamma--ray
astronomy and possibly presolar grain studies. In particular, estimations of
expected gamma-ray fluxes are essential for the planning of observations with
existing or future satellites.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:29:04 GMT"
}
] | 2009-06-23T00:00:00 |
[
[
"Coc",
"Alain",
""
]
] |
[
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-0.0412695296,
-0.0311979577,
-0.078340359,
0.0280622169,
-0.0182165243,
0.0253250878,
0.0069624064,
0.0512082316,
0.0260160137,
-0.0366190672,
0.0582503602,
-0.1030542403,
-0.0821138769,
-0.105499059,
0.0495074913,
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0.0219501816,
-0.0157318488,
-0.0048398026,
0.037868049,
0.0317028649,
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0.0152800903,
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-0.0218970329,
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-0.0042551728,
-0.0418010131,
-0.1436062753,
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-0.0117125213,
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0.0392233282,
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] |
801.2924 |
Raoyang Zhang
|
Xiaobo Nie, Xiaowen Shan and Chen Hudong
|
Galilean invariance of lattice Boltzmann models
| null | null |
10.1209/0295-5075/81/34005
| null |
physics.flu-dyn physics.comp-ph
| null |
It is well-known that the original lattice Boltzmann (LB) equation deviates
from the Navier-Stokes equations due to an unphysical velocity dependent
viscosity. This unphysical dependency violates the Galilean invariance and
limits the validation domain of the LB method to near incompressible flows. As
previously shown, recovery of correct transport phenomena in kinetic equations
depends on the higher hydrodynamic moments. In this Letter, we give specific
criteria for recovery of various transport coefficients. The Galilean
invariance of a general class of LB models is demonstrated via numerical
experiments.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:23:22 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Nie",
"Xiaobo",
""
],
[
"Shan",
"Xiaowen",
""
],
[
"Hudong",
"Chen",
""
]
] |
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-0.0589996502,
-0.0421426073,
-0.0496086106,
0.0496086106,
0.011511175,
-0.0012950072,
-0.0384226106,
0.0433912762,
-0.0768452212,
0.1079058871,
0.0178195592,
0.1216412559,
-0.0523921065,
0.0587395094,
0.0209152196,
0.09848883,
0.0256627668,
-0.0093129957,
0.1280927211,
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-0.0952110738,
-0.0100934142,
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0.0031639473,
-0.0372259691,
-0.0099958619,
0.0527302884,
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0.0017526902,
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-0.0188341029,
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] |
801.2925 |
Srinivas Raghu
|
S. Raghu, D. Podolsky, A. Vishwanath and David A. Huse
|
A vortex dynamics approach to the Nernst effect in fluctuating
superconductors
|
References added
|
Phys. Rev. B 78, 184520 (2008)
| null | null |
cond-mat.supr-con cond-mat.stat-mech cond-mat.str-el
| null |
We present a new method to study the Nernst effect and diamagetism of an
extreme type-II superconductor dominated by phase fluctuations. We work
directly with vortex variables and our method allows us to tune vortex
parameters (e.g., core energy and number of vortex species). We find that
diamagnetic response and transverse thermoelectric conductivity ($\alpha_{xy}$)
persist well above the Kosterlitz-Thouless transition temperature, and become
more pronounced as the vortex core energy is increased. However, they
\textit{weaken} as the number of internal vortex states are increased. We find
that $\alpha_{xy}$ closely tracks the magnetization $(-M/T)$ over a wide range
of parameters.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:23:36 GMT"
},
{
"version": "v2",
"created": "Fri, 25 Jan 2008 01:32:39 GMT"
}
] | 2008-12-19T00:00:00 |
[
[
"Raghu",
"S.",
""
],
[
"Podolsky",
"D.",
""
],
[
"Vishwanath",
"A.",
""
],
[
"Huse",
"David A.",
""
]
] |
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0.0367579795,
-0.0694094822,
-0.0096840253,
0.0275684856,
0.003280174,
0.0937979519,
0.0496282801,
0.0150612565,
0.0490523726,
-0.1013097987,
0.0802766234,
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0.0427173786,
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-0.0389364175,
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0.0433183275,
-0.0381852314,
-0.0784237012
] |
801.2926 |
Thomas Eckl
|
Thomas Eckl
|
An asymptotic version of Dumnicki's algorithm for linear systems in
$\mathbb{CP}^2$
|
14 pages, 5 figures, references added
| null | null | null |
math.AG
| null |
Using Dumnicki's approach to showing non-specialty of linear systems
consisting of plane curves with prescribed multiplicities in sufficiently
general points on $\mathbb{P}^2$ we develop an asymptotic method to determine
lower bounds for Seshadri constants of general points on $\mathbb{P}^2$. With
this method we prove the lower bound 4/13 for 10 general points on
$\mathbb{P}^2$.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:53:13 GMT"
},
{
"version": "v2",
"created": "Tue, 22 Jan 2008 17:42:44 GMT"
}
] | 2008-01-22T00:00:00 |
[
[
"Eckl",
"Thomas",
""
]
] |
[
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] |
801.2927 |
Bernhard Mehlig
|
K. Gustavsson, B. Mehlig, and M. Wilkinson
|
Collisions of particles advected in random flows
|
24 pages, 3 figures
|
New. J. Phys. 10 (special issue: Focus on Cloud Physics), 075014
(2008)
|
10.1088/1367-2630/10/7/075014
| null |
nlin.CD
| null |
We consider collisions of particles advected in a fluid. As already pointed
out by Smoluchowski [Z. f. physik. Chemie XCII, 129-168, (1917)], macroscopic
motion of the fluid can significantly enhance the frequency of collisions
between the suspended particles. This effect was invoked by Saffman and Turner
[J. Fluid Mech. 1, 16-30, (1956)] to estimate collision rates of small water
droplets in turbulent rain clouds, the macroscopic motion being caused by
turbulence. Here we show that the Saffman-Turner theory is unsatisfactory
because it describes an initial transient only. The reason for this failure is
that the local flow in the vicinity of a particle is treated as if it were a
steady hyperbolic flow, whereas in reality it must fluctuate. We derive exact
expressions for the steady-state collision rate for particles suspended in
rapidly fluctuating random flows and compute how this steady state is
approached. For incompressible flows, the Saffman-Turner expression is an upper
bound.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:25:10 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Gustavsson",
"K.",
""
],
[
"Mehlig",
"B.",
""
],
[
"Wilkinson",
"M.",
""
]
] |
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] |
801.2928 |
Andreas Jacob
|
A. Jacob, P. Ohberg, G. Juzeliunas and L. Santos
|
Cold atom dynamics in non-Abelian gauge fields
|
8 pages, 9 figures
|
Appl.Phys.B89:439-445,2007
|
10.1007/s00340-007-2865-6
| null |
cond-mat.other
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
The dynamics of ultracold neutral atoms subject to a non-Abelian gauge field
is investigated. In particular we analyze in detail a simple experimental
scheme to achieve a constant, but non-Abelian gauge field, and discuss in the
frame of this gauge field the non-Abelian Aharanov-Bohm effect. In the last
part of this paper, we discuss intrinsic non-Abelian effects in the dynamics of
cold atomic wavepackets.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:26:16 GMT"
},
{
"version": "v2",
"created": "Wed, 9 Jul 2008 11:02:45 GMT"
}
] | 2009-03-19T00:00:00 |
[
[
"Jacob",
"A.",
""
],
[
"Ohberg",
"P.",
""
],
[
"Juzeliunas",
"G.",
""
],
[
"Santos",
"L.",
""
]
] |
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-0.0001318924,
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-0.0248232223,
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-0.0384973399,
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-0.0256892908,
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0.1058798879,
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-0.0213833451,
-0.0711883679,
0.0156990103
] |
801.2929 |
Huaxin Lin
|
Huaxin Lin
|
Approximate Unitary Equivalence in Simple C^*-algebras of Tracial Rank
One
|
66 pages
| null | null | null |
math.OA math.FA
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Let $C$ be a unital AH-algebra and let $A$ be a unital separable simple
C*-algebra with tracial rank no more than one. Suppose that $\phi, \psi: C\to
A$ are two unital monomorphisms. With some restriction on $C,$ we show that
$\phi$ and $\psi$ are approximately unitarily equivalent if and only if
[\phi]=[\psi] in KL(C,A)
\tau\circ \phi=\tau\circ \psi for all tracial states of A and
\phi^{\ddag}=\psi^{\ddag}, here \phi^{\ddag} and \psi^{\ddag} are
homomorphisms from $U(C)/CU(C)\to U(A)/CU(A) induced by \phi and \psi,
respectively, and where CU(C) and CU(A) are closures of the subgroup generated
by commutators of the unitary groups of C and B.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:27:28 GMT"
},
{
"version": "v2",
"created": "Fri, 25 Jan 2008 20:51:45 GMT"
},
{
"version": "v3",
"created": "Mon, 28 Jan 2008 01:14:57 GMT"
},
{
"version": "v4",
"created": "Tue, 11 May 2010 15:59:08 GMT"
}
] | 2010-05-12T00:00:00 |
[
[
"Lin",
"Huaxin",
""
]
] |
[
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] |
801.293 |
Yolanda Gomez Dr.
|
Y. Gomez
|
Maser emission in planetary nebulae
|
7 pages, iaus.cls, to appear in IAU Symp. 242 proceedings
(Astrophysical masers and their environments)
| null | null | null |
astro-ph
| null |
Stars at the top of the asymptotic giant branch (AGB) can exhibit maser
emission from molecules like SiO, H2O and OH. As the star evolves to the
planetary nebula phase, mass-loss stops and ionization of the envelope begins,
making the masers disappear progressively. The OH masers in PNe can be present
in the envelope for periods of ~1000 years but the water masers can survive
only hundreds of years. Then, water maser emission is not expected in planetary
nebulae! We discuss the unambiguous detection of water maser emission in two
planetary nebulae: K 3-35 and IRAS 17347-3139.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:27:50 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Gomez",
"Y.",
""
]
] |
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] |
801.2931 |
Jon Feldman
|
Jon Feldman, S. Muthukrishnan, Evdokia Nikolova, Martin Pal
|
A Truthful Mechanism for Offline Ad Slot Scheduling
| null | null | null | null |
cs.GT cs.DS
| null |
We consider the "Offline Ad Slot Scheduling" problem, where advertisers must
be scheduled to "sponsored search" slots during a given period of time.
Advertisers specify a budget constraint, as well as a maximum cost per click,
and may not be assigned to more than one slot for a particular search.
We give a truthful mechanism under the utility model where bidders try to
maximize their clicks, subject to their personal constraints. In addition, we
show that the revenue-maximizing mechanism is not truthful, but has a Nash
equilibrium whose outcome is identical to our mechanism. As far as we can tell,
this is the first treatment of sponsored search that directly incorporates both
multiple slots and budget constraints into an analysis of incentives.
Our mechanism employs a descending-price auction that maintains a solution to
a certain machine scheduling problem whose job lengths depend on the price, and
hence is variable over the auction. The price stops when the set of bidders
that can afford that price pack exactly into a block of ad slots, at which
point the mechanism allocates that block and continues on the remaining slots.
To prove our result on the equilibrium of the revenue-maximizing mechanism, we
first show that a greedy algorithm suffices to solve the revenue-maximizing
linear program; we then use this insight to prove that bidders allocated in the
same block of our mechanism have no incentive to deviate from bidding the fixed
price of that block.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:34:30 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Feldman",
"Jon",
""
],
[
"Muthukrishnan",
"S.",
""
],
[
"Nikolova",
"Evdokia",
""
],
[
"Pal",
"Martin",
""
]
] |
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-0.0237087011,
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-0.0516375229,
-0.0122278705,
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-0.0387674607,
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-0.0144296736,
0.0237873364,
-0.0273390543,
-0.0158713311,
-0.0572993048,
0.0548353828,
0.0107796611,
0.0725546554,
0.0603398904,
0.0671025664,
0.133890599,
0.0023328627,
-0.054520838,
-0.0828821585,
-0.0166576896,
0.0155174695,
0.0564080961,
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-0.0548878051,
-0.0162645094,
-0.0041283807,
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-0.0061696358,
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-0.1004965827,
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-0.0077980524,
-0.0311659984,
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-0.0472339168,
-0.0240494553,
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-0.0121688936,
-0.0449534804,
-0.0607592799,
-0.0544159897,
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-0.0863421336,
-0.0890157521,
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-0.0443243943,
-0.0747040361,
0.0289379824,
0.0028226983,
-0.0254386887
] |
801.2932 |
Martin Kr\"oger
|
I.V. Karlin, M. Colangeli, M. Kroger
|
Exact linear hydrodynamics from the Boltzmann equation
|
4 pages, 3 figures
|
Phys. Rev. Lett. 100, 214503 (2008)
|
10.1103/PhysRevLett.100.214503
| null |
cond-mat.stat-mech
| null |
Exact (to all orders in Knudsen number) equations of linear hydrodynamics are
derived from the Boltzmann kinetic equation with the Bhatnagar-Gross-Krook
collision integral. The exact hydrodynamic equations are cast in a form which
allows us to immediately prove their hyperbolicity, stability, and existence of
an H-theorem.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:32:06 GMT"
}
] | 2008-06-03T00:00:00 |
[
[
"Karlin",
"I. V.",
""
],
[
"Colangeli",
"M.",
""
],
[
"Kroger",
"M.",
""
]
] |
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] |
801.2933 |
Benne W. Holwerda
|
B. W. Holwerda, R. A. Gonzalez, W. C. Keel, D. Calzetti, R. J. Allen
and P. C. van de Kruit
|
Structure and Evolution of the Opacity of Spiral Disks
|
8 pages, 4 figures, to appear in the proceedings of ``The Evolving
ISM in the Milky Way and Nearby Galaxies'', Pasadena, 2007
| null | null |
ismevo-p42
|
astro-ph
| null |
The opacity of a spiral disk due to dust absorption influences every
measurement we make of it in the UV and optical. Two separate techniques
directly measure the total absorption by dust in the disk: calibrated distant
galaxy counts and overlapping galaxy pairs. The main results from both so far
are a semi-transparent disk with more opaque arms, and a relation between
surface brightness and disk opacity. In the Spitzer era, SED models of spiral
disks add a new perspective on the role of dust in spiral disks. Combined with
the overall opacity from galaxy counts, they yield a typical optical depth of
the dusty ISM clouds: 0.4 that implies a size of $\sim$ 60 pc. Work on galaxy
counts is currently ongoing on the ACS fields of M51, M101 and M81. Occulting
galaxies offer the possibility of probing the history of disk opacity from
higher redshift pairs. Evolution in disk opacity could influence distance
measurements (SN1a, Tully-Fisher relation). Here, we present first results from
spectroscopically selected occulting pairs in the SDSS. The redshift range for
this sample is limited, but does offer a first insight into disk opacity
evolution as well as a reference for higher redshift measurements. Spiral disk
opacity has not undergone significant evolution since z=0.2. HST imaging would
help disentangle the effects of spiral arms in these pairs. Many more
mixed-morphology types are being identified in SDSS by the GalaxyZoo project.
The occulting galaxy technique can be pushed to a redshift of 1 using many
pairs identified in the imaging campaigns with HST (DEEP2, GEMS, GOODS,
COSMOS).
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:40:28 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Holwerda",
"B. W.",
""
],
[
"Gonzalez",
"R. A.",
""
],
[
"Keel",
"W. C.",
""
],
[
"Calzetti",
"D.",
""
],
[
"Allen",
"R. J.",
""
],
[
"van de Kruit",
"P. C.",
""
]
] |
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] |
801.2934 |
Lutz D\"umbgen
|
Lutz Duembgen, Bernd-Wolfgang Igl, Axel Munk
|
P-values for classification
|
Published in at http://dx.doi.org/10.1214/08-EJS245 the Electronic
Journal of Statistics (http://www.i-journals.org/ejs/) by the Institute of
Mathematical Statistics (http://www.imstat.org)
|
Electronic Journal of Statistics 2008, Vol. 2, 468-493
|
10.1214/08-EJS245
|
IMS-EJS-EJS_2008_245
|
math.ST stat.ML stat.TH
| null |
Let $(X,Y)$ be a random variable consisting of an observed feature vector
$X\in \mathcal{X}$ and an unobserved class label $Y\in \{1,2,...,L\}$ with
unknown joint distribution. In addition, let $\mathcal{D}$ be a training data
set consisting of $n$ completely observed independent copies of $(X,Y)$. Usual
classification procedures provide point predictors (classifiers)
$\widehat{Y}(X,\mathcal{D})$ of $Y$ or estimate the conditional distribution of
$Y$ given $X$. In order to quantify the certainty of classifying $X$ we propose
to construct for each $\theta =1,2,...,L$ a p-value
$\pi_{\theta}(X,\mathcal{D})$ for the null hypothesis that $Y=\theta$, treating
$Y$ temporarily as a fixed parameter. In other words, the point predictor
$\widehat{Y}(X,\mathcal{D})$ is replaced with a prediction region for $Y$ with
a certain confidence. We argue that (i) this approach is advantageous over
traditional approaches and (ii) any reasonable classifier can be modified to
yield nonparametric p-values. We discuss issues such as optimality, single use
and multiple use validity, as well as computational and graphical aspects.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:44:02 GMT"
},
{
"version": "v2",
"created": "Tue, 3 Jun 2008 09:34:53 GMT"
},
{
"version": "v3",
"created": "Thu, 26 Jun 2008 08:14:11 GMT"
}
] | 2008-06-26T00:00:00 |
[
[
"Duembgen",
"Lutz",
""
],
[
"Igl",
"Bernd-Wolfgang",
""
],
[
"Munk",
"Axel",
""
]
] |
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] |
801.2935 |
Andreas Jacob
|
A. Jacob, P. Ohberg, G. Juzeliunas and L. Santos
|
Landau levels of cold atoms in non-Abelian gauge fields
|
13 pages, 9 figures
|
New J. Phys. 10 (2008) 045022
|
10.1088/1367-2630/10/4/045022
| null |
cond-mat.other
| null |
The Landau levels of cold atomic gases in non-Abelian gauge fields are
analyzed. In particular we identify effects on the energy spectrum and density
distribution which are purely due to the non-Abelian character of the fields.
We investigate in detail non-Abelian generalizations of both the Landau and the
symmetric gauge. Finally, we discuss how these non-Abelian Landau and symmetric
gauges may be generated by means of realistically feasible lasers in a tripod
scheme.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:45:35 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Jacob",
"A.",
""
],
[
"Ohberg",
"P.",
""
],
[
"Juzeliunas",
"G.",
""
],
[
"Santos",
"L.",
""
]
] |
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-0.079003334,
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] |
801.2936 |
So Matsuura
|
Poul H. Damgaard and So Matsuura
|
Geometry of Orbifolded Supersymmetric Lattice Gauge Theories
|
10 pages, no figure, latex2e
|
Phys.Lett.B661:52-56,2008
|
10.1016/j.physletb.2008.01.044
| null |
hep-th hep-lat
| null |
We prove that the prescription for construction of supersymmetric lattice
gauge theories by orbifolding and deconstruction directly leads to Catterall's
geometrical discretization scheme in general. These two prescriptions always
give the same lattice discretizations when applied to theories of p-form
fields. We also show that the geometrical discretization scheme can be applied
to more general theories.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:51:17 GMT"
}
] | 2008-11-26T00:00:00 |
[
[
"Damgaard",
"Poul H.",
""
],
[
"Matsuura",
"So",
""
]
] |
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0.0812346265,
-0.0800812989,
-0.0591709018,
-0.0983841643,
0.0225150306
] |
801.2937 |
Philip Lockett
|
Philip Lockett and Moshe Elitzur
|
The Effect of 53 micron IR Radiation on 18 cm OH Megamaser Emission
|
Accepted to ApJ, 26 pages including 1 table and 7 figures
| null |
10.1086/533429
| null |
astro-ph
| null |
OH megamasers (OHMs) emit primarily in the main lines at 1667 and 1665 MHz,
and differ from their Galactic counterparts due to their immense luminosities,
large linewidths and 1667/1665 MHz flux ratios, which are always greater than
one. We find that these maser properties result from strong 53 micron radiative
pumping combined with line overlap effects caused by turbulent linewidths of
about 20 km/s; pumping calculations that do not include line overlap are
unreliable. A minimum dust temperature of about 45 K is needed for inversion,
and maximum maser efficiency occurs for dust temperatures in the range 80 - 140
K. We find that warmer dust can support inversion at lower IR luminosities, in
agreement with observations. Our results are in good agreement with a clumpy
model of OHMs, with clouds sizes about 1 pc and OH column densities about 5e16
cm^2, that is able to explain both the diffuse and compact emission observed
for OHMs. We suggest that all OH main line masers may be pumped by far-IR
radiation, with the major differences between OHMs and Galactic OH masers
caused by differences in linewidth produced by line overlap. Small Galactic
maser linewidths tend to produce stronger 1665 MHz emission. The large OHM
linewidths lead to inverted ground state transitions having approximately the
same excitation temperature, producing 1667/1665 MHz flux ratios greater than
one and weak satellite line emission. Finally, the small observed ratio of
pumping radiation to dense molecular gas, as traced by HCN and HCO$^+$, is a
possible reason for the lack of OH megamaser emission in NGC 6240.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 16:53:42 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Lockett",
"Philip",
""
],
[
"Elitzur",
"Moshe",
""
]
] |
[
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] |
801.2938 |
Benne W. Holwerda
|
B. W. Holwerda, R. S. de Jong, A. Seth, J. J. Dalcanton, M. Regan, E.
Bell and S. Bianchi
|
Spitzer's View of Edge-on Spirals
|
4 pages, 4 figures, to appear in the proceedings of ``The Evolving
ISM in the Milky Way and Nearby Galaxies'', Pasadena, 2007
| null | null |
ismevo-p43
|
astro-ph
| null |
Edge-on spiral galaxies offer a unique perspective on disks. One can
accurately determine the height distribution of stars and ISM and the
line-of-sight integration allows for the study of faint structures. The Spitzer
IRAC camera is an ideal instrument to study both the ISM and stellar structure
in nearby galaxies; two of its channels trace the old stellar disk with little
extinction and the 8 micron channel is dominated by the smallest dust grains
(Polycyclic Aromatic Hydrocarbons, PAHs).
Dalcanton et al. (2004) probed the link between the appearance of dust lanes
and the disk stability. In a sample of bulge-less disks they show how in
massive disks the ISM collapses into the characteristic thin dust lane. Less
massive disks are gravitationally stable and their dust morphology is
fractured. The transition occurs at 120 km/s for bulgeless disks.
Here we report on our results of our Spitzer/IRAC survey of nearby edge-on
spirals and its first results on the NIR Tully-Fischer relation, and ISM disk
stability.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:02:18 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Holwerda",
"B. W.",
""
],
[
"de Jong",
"R. S.",
""
],
[
"Seth",
"A.",
""
],
[
"Dalcanton",
"J. J.",
""
],
[
"Regan",
"M.",
""
],
[
"Bell",
"E.",
""
],
[
"Bianchi",
"S.",
""
]
] |
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] |
801.2939 |
Maurice Pouzet
|
Moncef Bouaziz, Miguel Couceiro and Maurice Pouzet
|
Irreducible Boolean Functions
|
10 pages, ROGICS08,Mahdia 12-15 may 2008
| null | null | null |
math.CO
| null |
This paper is a contribution to the study of a quasi-order on the set
$\Omega$ of Boolean functions, the \emph{simple minor} quasi-order. We look at
the join-irreducible members of the resulting poset $\tilde{\Omega}$. Using a
two-way correspondence between Boolean functions and hypergraphs,
join-irreducibility translates into a combinatorial property of hypergraphs. We
observe that among Steiner systems, those which yield join-irreducible members
of $\tilde{\Omega}$ are the -2-monomorphic Steiner systems. We also describe
the graphs which correspond to join-irreducible members of $\tilde{\Omega}$.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:20:35 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Bouaziz",
"Moncef",
""
],
[
"Couceiro",
"Miguel",
""
],
[
"Pouzet",
"Maurice",
""
]
] |
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-0.0594963469,
0.0081183482
] |
801.294 |
Marc Ribo
|
M. Ribo, J.M. Paredes, J. Moldon, J. Marti, M. Massi
|
The changing milliarcsecond radio morphology of the gamma-ray binary LS
5039
|
To be published in A&A main journal. 5 pages, 1 figure. A reference
has been corrected
|
Astron.Astrophys. 481 (2008) 17-20
|
10.1051/0004-6361:20078390
| null |
astro-ph
| null |
Context. LS 5039 is one of the few TeV emitting X-ray binaries detected so
far. The powering source of its multiwavelength emission can be accretion in a
microquasar scenario or wind interaction in a young nonaccreting pulsar
scenario.
Aims. To present new high-resolution radio images and compare them with the
expected behavior in the different scenarios.
Methods. We analyze Very Long Baseline Array (VLBA) radio observations that
provide morphological and astrometric information at milliarcsecond scales.
Results. We detect a changing morphology between two images obtained five
days apart. In both runs there is a core component with a constant flux
density, and an elongated emission with a position angle (PA) that changes by
12+/-3 degrees between both runs. The source is nearly symmetric in the first
run and asymmetric in the second one. The astrometric results are not
conclusive.
Conclusions. A simple and shockless microquasar scenario cannot easily
explain the observed changes in morphology. An interpretation within the young
nonaccreting pulsar scenario requires the inclination of the binary system to
be very close to the upper limit imposed by the absence of X-ray eclipses.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:11:53 GMT"
},
{
"version": "v2",
"created": "Fri, 1 Feb 2008 16:34:56 GMT"
}
] | 2008-03-20T00:00:00 |
[
[
"Ribo",
"M.",
""
],
[
"Paredes",
"J. M.",
""
],
[
"Moldon",
"J.",
""
],
[
"Marti",
"J.",
""
],
[
"Massi",
"M.",
""
]
] |
[
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-0.0371451415,
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] |
801.2941 |
Francis J. O'Brien Jr.
|
Francis J. O'Brien Jr
|
Summary Of Four Generalized Exponential Models (GEM) For Continuous
Probability Distributions
|
66 pages v5; minor typos corrected and formu;and reference formulas
added
| null | null | null |
math.GM
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
Four new probability models are derived which generalize the common
univariate continuous distributions. Classical distributional measures are
derived from Hoel, et al., Introduction to Probability Theory, 1971. Measures
include probability density function, moments generating function, cumulative
distribution function,derivatives, inverse distributions, skewness, kurtosis,
change of variable distributions, log distributions. Maximum likelihood
estimation technique is briefly outlined. Appendices describe applications.
Errata/addenda sheet included.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:12:57 GMT"
},
{
"version": "v2",
"created": "Tue, 22 Jan 2008 12:14:43 GMT"
},
{
"version": "v3",
"created": "Fri, 22 Jan 2010 13:11:35 GMT"
},
{
"version": "v4",
"created": "Mon, 25 Jan 2010 13:15:24 GMT"
},
{
"version": "v5",
"created": "Thu, 8 May 2014 11:14:50 GMT"
}
] | 2014-05-09T00:00:00 |
[
[
"O'Brien",
"Francis J.",
"Jr"
]
] |
[
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-0.0604398549,
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] |
801.2942 |
Yuval Peres
|
Fedor Nazarov, Yuval Peres and Alexander Volberg
|
The power law for the Buffon needle probability of the four-corner
Cantor set
|
16 pages, 2 figures
| null | null | null |
math.CA math.MG
| null |
Let $C_n$ be the $n$-th generation in the construction of the middle-half
Cantor set. The Cartesian square $K_n$ of $C_n$ consists of $4^n$ squares of
side-length $4^{-n}$. The chance that a long needle thrown at random in the
unit square will meet $K_n$ is essentially the average length of the
projections of $K_n$, also known as the Favard length of $K_n$. A classical
theorem of Besicovitch implies that the Favard length of $K_n$ tends to zero.
It is still an open problem to determine its exact rate of decay. Until
recently, the only explicit upper bound was $\exp(- c\log_* n)$, due to Peres
and Solomyak. ($\log_* n$ is the number of times one needs to take log to
obtain a number less than 1 starting from $n$). We obtain a power law bound by
combining analytic and combinatorial ideas.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:24:01 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Nazarov",
"Fedor",
""
],
[
"Peres",
"Yuval",
""
],
[
"Volberg",
"Alexander",
""
]
] |
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] |
801.2943 |
Samuel Meek
|
Samuel A. Meek, Hendrick L. Bethlem, Horst Conrad, Gerard Meijer
|
Trapping molecules on a chip in traveling potential wells
|
4 pages, 3 figures
|
Phys. Rev. Lett. 100, 153003 (2008)
|
10.1103/PhysRevLett.100.153003
| null |
physics.atom-ph
| null |
A microstructured array of over 1200 electrodes on a substrate has been
configured to generate an array of local minima of electric field strength with
a periodicity of $120 \mu$m about $25 \mu$m above the substrate. By applying
sinusoidally varying potentials to the electrodes, these minima can be made to
move smoothly along the array. Polar molecules in low field seeking quantum
states can be trapped in these traveling potential wells. This is
experimentally demonstrated by transporting metastable CO molecules in 30 mK
deep wells that move at constant velocities above the substrate.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:26:10 GMT"
},
{
"version": "v2",
"created": "Wed, 23 Apr 2008 09:30:53 GMT"
}
] | 2008-04-23T00:00:00 |
[
[
"Meek",
"Samuel A.",
""
],
[
"Bethlem",
"Hendrick L.",
""
],
[
"Conrad",
"Horst",
""
],
[
"Meijer",
"Gerard",
""
]
] |
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] |
801.2944 |
Georges Meynet
|
Georges Meynet
|
Physics of rotation in stellar models
|
32 pages, 7 figures, lectures, CNRS school, will be published by
Springer
| null |
10.1007/978-3-540-87831-5_6
| null |
astro-ph
| null |
In these lecture notes, we present the equations presently used in stellar
interior models in order to compute the effects of axial rotation. We discuss
the hypotheses made. We suggest that the effects of rotation might play a key
role at low metallicity.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:33:13 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Meynet",
"Georges",
""
]
] |
[
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] |
801.2945 |
Emre Tuna
|
S. Emre Tuna
|
Synchronizing discrete-time neutrally stable linear systems via
partial-state coupling
|
14 pages, to appear in Automatica
| null | null | null |
math.DS math.OC
| null |
A basic result in synchronization of linear systems via output coupling is
presented. For identical discrete-time linear systems that are detectable from
their outputs and neutrally stable, it is shown that a linear output feedback
law exists under which the coupled systems globally asymptotically synchronize
for all fixed connected (asymmetrical) network topologies. An algorithm is
provided to compute such feedback law based on individual system parameters. A
dual problem is also presented and solved.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:39:40 GMT"
},
{
"version": "v2",
"created": "Sat, 19 Jan 2008 16:46:11 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Tuna",
"S. Emre",
""
]
] |
[
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0.0054101762,
0.0553775243
] |
801.2946 |
Amelia Sparavigna
|
Amelia Sparavigna, Rory A. Wolf
|
Fourier optics for polymeric substrates and coating textures analysis
|
7 pages, 9 figures
| null | null | null |
physics.pop-ph
| null |
Several devices for substrate texture detection based on diffractive optics,
for paper, textiles and non-wovens have been proposed in the past for direct
inspection during the production processes. In spite of the presence of devices
totally based on image processing, the use of diffractive optics cannot be
considered surpassed for many reasons. Compared with image processing
procedures, it is less sensitive to vibrations and does not suffer from the
presence of ambient light. Based on transmitted light, it can give information
on changes in refractive indexes, thickness variation and surface conditions.
We study the use of optical Fourier spectrum to identify textures of polymer
films. As the power spectrum reveals, the texture is seldom homogeneous. Here
we report investigation on several substrates and on thin ink coatings on
substrate. Role of bulk and surface conditions is analysed.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:43:20 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Sparavigna",
"Amelia",
""
],
[
"Wolf",
"Rory A.",
""
]
] |
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] |
801.2947 |
Nouicer Rachid
|
Rachid Nouicer (for the PHENIX Collaboration)
|
Silicon Vertex Tracker for PHENIX Upgrade at RHIC: Capabilities and
Detector Technology
|
13 pages, the 16th International Workshop on Vertex detectors,
September 23-28 2007, Lake Placid, NY, U.S.A. accepted for publication in
Proceeding of Science (PoS)
| null | null | null |
nucl-ex
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
From the wealth of data obtained from the first three years of RHIC
operation, the four RHIC experiments, BRAHMS, PHENIX, PHOBOS and STAR, have
concluded that a high density partonic matter is formed at central Au+Au
collisions at 200 GeV. The research focus now shifts from initial discovery to
a detailed exploration of partonic matter. Particles carrying heavy flavor,
i.e. charm or beauty quarks, are powerful tool for study the properties of the
hot and dense medium created in high-energy nuclear collisions at RHIC. At the
relatively low transverse momentum region, the collective motion of the heavy
flavor will be a sensitive signal for the thermalization of light flavors. An
upgrade of RHIC (RHIC-II) is intended for the second half of the decade, with a
luminosity increase to about 20-40 times the design value of 8x1026 cm-2 s-1
for Au+Au, and 2x1032 cm-2 s-1 for polarized proton beams. The PHENIX
collaboration plans to upgrade its experiment to exploit with an enhanced
detector new physics then in reach. For this purpose, we are constructing the
Silicon Vertex Tracker (VTX). The VTX detector will provide us the tool to
measure new physics observables that are not accessible at the present RHIC or
available only with very limited accuracy. The VTX detector consists of four
layers of barrel detectors located in the region of pseudorapidity |eta| < 1.2
and covers almost 2 azimuthal angle. The pseudorapidity is defined as eta =
-ln[tan(/2)], where is the emission angle relative to the beam axis. In this
paper, we will provide details of the physics capability added to PHENIX by the
new central silicon vertex tracker, the status of the project, including
technology choices used in the design, performance of individual silicon sensor
and silicon detector prototype.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:43:32 GMT"
},
{
"version": "v2",
"created": "Wed, 10 Sep 2008 14:43:09 GMT"
}
] | 2019-08-13T00:00:00 |
[
[
"Nouicer",
"Rachid",
"",
"for the PHENIX Collaboration"
]
] |
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] |
801.2948 |
Alberto Robledo
|
A. Robledo, L. G. Moyano
|
q-Deformed Statistical-Mechanical Property in the Dynamics of
Trajectories en route to the Feigenbaum Attractor
|
16 pages, 24 figures. Final published version. Minor corrections and
typos added
|
Phys. Rev. E 77, 036213 (2008)
|
10.1103/PhysRevE.77.036213
| null |
cond-mat.stat-mech nlin.CD
| null |
We demonstrate that the dynamics towards and within the Feigenbaum attractor
combine to form a q-deformed statistical-mechanical construction. The rate at
which ensemble trajectories converge to the attractor (and to the repellor) is
described by a q-entropy obtained from a partition function generated by
summing distances between neighboring positions of the attractor. The values of
the q-indices involved are given by the unimodal map universal constants, while
the thermodynamic structure is closely related to that formerly developed for
multifractals. As an essential component in our demonstration we expose, at a
previously unknown level of detail, the features of the dynamics of
trajectories that either evolve towards the Feigenbaum attractor or are
captured by its matching repellor. The dynamical properties of the family of
periodic superstable cycles in unimodal maps are seen to be key ingredients for
the comprehension of the discrete scale invariance features present at the
period-doubling transition to chaos. We make clear the dynamical origin of the
anomalous thermodynamic framework existing at the Feigenbaum attractor.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 17:45:40 GMT"
},
{
"version": "v2",
"created": "Wed, 26 Mar 2008 11:22:10 GMT"
}
] | 2008-05-14T00:00:00 |
[
[
"Robledo",
"A.",
""
],
[
"Moyano",
"L. G.",
""
]
] |
[
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] |
801.2949 |
Claudio Coriano
|
Claudio Coriano, Marco Guzzi and Simone Morelli
|
Unitarity Bounds for Gauged Axionic Interactions and the Green-Schwarz
Mechanism
|
50 pages, 28 figures
|
Eur.Phys.J.C55:629-652,2008
|
10.1140/epjc/s10052-008-0616-4
| null |
hep-ph
| null |
We analyze the effective actions of anomalous models in which a
four-dimensional version of the Green-Schwarz mechanism is invoked for the
cancellation of the anomalies, and we compare it with those models in which
gauge invariance is restored by the presence of a Wess-Zumino term. Some issues
concerning an apparent violation of unitarity of the mechanism, which requires
Dolgov-Zakharov poles, are carefully examined, using a class of amplitudes
studied in the past by Bouchiat-Iliopoulos-Meyer (BIM), and elaborating on
previous studies. In the Wess-Zumino case we determine explicitly the unitarity
bound using a realistic model of intersecting branes (the Madrid model) by
studying the corresponding BIM amplitudes. This is shown to depend
significantly on the St\"uckelberg mass and on the coupling of the extra
anomalous gauge bosons and allows one to identify Standard-Model-like regions
(which are anomaly-free) from regions where the growth of certain amplitudes is
dominated by the anomaly, separated by an inflection point which could be
studied at the LHC. The bound can even be around 5-10 TeV's for a $Z'$ mass
around 1 TeV and varies sensitively with the anomalous coupling. The results
for the WZ case are quite general and apply to all the models in which an
axion-like interaction is introduced as a generalization of the Peccei-Quinn
mechanism, with a gauged axion.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 19:09:54 GMT"
},
{
"version": "v2",
"created": "Sun, 20 Jan 2008 10:51:24 GMT"
},
{
"version": "v3",
"created": "Fri, 15 Feb 2008 16:01:33 GMT"
},
{
"version": "v4",
"created": "Sat, 16 Feb 2008 18:36:18 GMT"
},
{
"version": "v5",
"created": "Fri, 9 May 2008 14:16:42 GMT"
}
] | 2008-11-26T00:00:00 |
[
[
"Coriano",
"Claudio",
""
],
[
"Guzzi",
"Marco",
""
],
[
"Morelli",
"Simone",
""
]
] |
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] |
801.295 |
Timothy Dulaney
|
Timothy R. Dulaney, Moira I. Gresham, Mark B. Wise
|
Classical stability of a homogeneous, anisotropic inflating space-time
|
12 pages, no figures; references added, content in section V revised
and some clarification made in text; minor typos corrected, v4 closely
resembles version published in Phys. Rev. D; in v5 - incorrect argument in
section V removed and one reference added
|
Phys.Rev.D77:083510,2008; Erratum-ibid.D79:029903,2009
|
10.1103/PhysRevD.77.083510 10.1103/PhysRevD.79.029903
|
CALT-68-2669
|
astro-ph hep-ph
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We study the classical stability of an anisotropic space-time seeded by a
spacelike, fixed norm, dynamical vector field in a vacuum-energy-dominated
inflationary era. It serves as a model for breaking isotropy during the
inflationary era. We find that, for a range of parameters, the linear
differential equations for small perturbations about the background do not have
a growing mode. We also examine the energy of fluctuations about this
background in flat-space. If the kinetic terms for the vector field do not take
the form of a field strength tensor squared then there is a negative energy
mode and the background is unstable. For the case where the kinetic term is of
the form of a field strength tensor squared we show that perturbations about
the background have positive energy at lowest order.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 18:05:43 GMT"
},
{
"version": "v2",
"created": "Wed, 6 Feb 2008 07:30:52 GMT"
},
{
"version": "v3",
"created": "Wed, 27 Feb 2008 21:26:05 GMT"
},
{
"version": "v4",
"created": "Tue, 13 May 2008 19:59:32 GMT"
},
{
"version": "v5",
"created": "Thu, 13 Nov 2008 00:23:25 GMT"
}
] | 2014-11-18T00:00:00 |
[
[
"Dulaney",
"Timothy R.",
""
],
[
"Gresham",
"Moira I.",
""
],
[
"Wise",
"Mark B.",
""
]
] |
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] |
801.2951 |
Vu Le Anh
|
Le Anh Vu and Duong Quang Hoa
|
The Topology of Foliations Formed by the Generic K-Orbits of a Subclass
of the Indecomposable MD5-Groups
|
20 pages, no figure
| null |
10.1007/s11425-009-0017-7
| null |
math.DG math.GT
| null |
The present paper is a continuation of [13], [14] of the authors.
Specifically, the paper considers the MD5-foliations associated to connected
and simply connected MD5-groups such that their Lie algebras have 4-dimensional
commutative derived ideal. In the paper, we give the topological classification
of all considered MD5-foliations. A description of these foliations by certain
fibrations or suitable actions of $\mathbb{R}^{2}$ and the Connes' C*-algebras
of the foliations which come from fibrations are also given in the paper.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 18:21:15 GMT"
},
{
"version": "v2",
"created": "Sat, 23 Feb 2008 02:10:48 GMT"
}
] | 2015-05-13T00:00:00 |
[
[
"Vu",
"Le Anh",
""
],
[
"Hoa",
"Duong Quang",
""
]
] |
[
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-0.089091152,
0.0281262156
] |
801.2952 |
Alexander Fetter
|
Alexander L. Fetter
|
Rotating trapped Bose-Einstein condensates
|
44 pages, 18 figures, submitted to Reviews of Modern Physics
|
Rev. Mod. Phys. 81, 647 (2009).
|
10.1007/s11490-008-1001-6
| null |
cond-mat.stat-mech
| null |
After reviewing the ideal Bose-Einstein gas in a box and in a harmonic trap,
I discuss the effect of interactions on the formation of a Bose-Einstein
condensate (BEC), along with the dynamics of small-amplitude perturbations (the
Bogoliubov equations). When the condensate rotates with angular velocity Omega,
one or several vortices nucleate, with many observable consequences. With more
rapid rotation, the vortices form a dense triangular array, and the collective
behavior of these vortices has additional experimental implications. For Omega
near the radial trap frequency omega_perp, the lowest-Landau-level
approximation becomes applicable, providing a simple picture of such rapidly
rotating condensates. Eventually, as Omega approaches omega_perp, the rotating
dilute gas is expected to undergo a quantum phase transition from a superfluid
to various highly correlated (nonsuperfluid) states analogous to those familiar
from the fractional quantum Hall effect for electrons in a strong perpendicular
magnetic field.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 18:33:23 GMT"
}
] | 2015-05-13T00:00:00 |
[
[
"Fetter",
"Alexander L.",
""
]
] |
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] |
801.2953 |
Guillaume Morin
|
Jacky Cresson (LMA - Pau, Imcce), Guillaume Morin (IMCCE, Ceremade)
|
Mould Calculus for Hamiltonian Vector Fields
|
30 pages
| null | null | null |
math.DS
| null |
We present the general framework of \'Ecalle's moulds in the case of
linearization of a formal vector field without and within resonances. We
enlighten the power of moulds by their universality, and calculability. We
modify then \'Ecalle's technique to fit in the seek of a formal normal form of
a Hamiltonian vector field in cartesian coordinates. We prove that mould
calculus can also produce successive canonical transformations to bring a
Hamiltonian vector field into a normal form. We then prove a Kolmogorov theorem
on Hamiltonian vector fields near a diophantine torus in action-angle
coordinates using moulds techniques.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 18:34:58 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Cresson",
"Jacky",
"",
"LMA - Pau, Imcce"
],
[
"Morin",
"Guillaume",
"",
"IMCCE, Ceremade"
]
] |
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-0.0769849718,
0.0555558726
] |
801.2954 |
Francois Demontoux
|
Fran\c{c}ois Demontoux (LPIOM, IMS), Gilles Ruffi\'e (IMS), Jean
Pierre Wigneron (EPHYSE - UR1263), Maria-Jos\'e Escorihuela (CESBIO)
|
Am\'elioration de l'\'etude de l'\'etude de l'humidit\'e de sols par
radiom\'etrie. Caract\'erisation et mod\'elisation di\'electriques de profils
g\'eologiques
| null |
Dans actes des journ\'ees nationales micro-ondes - Journ\'ees
Nationales Micro-ondes, Nancy : France (2005)
| null | null |
physics.geo-ph
| null |
The surface soil moisture is a key variable to describe the exchange of water
and energy between the land and the atmosphere. In hydrology, and meteorology,
the amount of water in the upper soil layers permits (0-5 cm from the surface)
the evaluation of the relationship between the real evaporation and the
potential evaporation of the bare soil. It is also possible to determine the
distribution of rainfall or other variables such as hydraulic conductivity.
Studies have shown that microwave sensors could be used to scan the surface
soil moisture. The solution choose by the team associated with the SMOS mission
(Soil Moisture and Ocean Salinity) is to use a radiometer (1.4 GHz) to identify
soil microwave emissions . The measurements are made on the site of CESBIO in
Toulouse where a 1.4 GHz radiometer is installed . The effect of vegetation
cover, soil temperatures, snow cover, topography or moisture variations have an
important role in the broadcast microwave surface. Other parameters such as the
presence of inclusions in the ground (holes, stones), or soil texture can also
disrupt measurements. The aim of the work that we present in this paper is to
develop a numerical model to simulate complex geological structures. This model
must take into account all parameters that can affect the equivalent
permittivity measured by the radiometer (surface, moisture variation ,...
inclusions). The purpose of this model is to calculate the equivalent
permittivity of these geological structures in order to be able to associate
with each radiometer measurement an equivalent moisture.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 18:38:38 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Demontoux",
"François",
"",
"LPIOM, IMS"
],
[
"Ruffié",
"Gilles",
"",
"IMS"
],
[
"Wigneron",
"Jean Pierre",
"",
"EPHYSE - UR1263"
],
[
"Escorihuela",
"Maria-José",
"",
"CESBIO"
]
] |
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] |
801.2955 |
Colas Bardavid
|
Colas Bardavid (IRMAR)
|
Profinite completion and double-dual : isomorphisms and counter-examples
| null | null | null | null |
math.GR
| null |
We define, for any group $G$, finite approximations ; with this tool, we give
a new presentation of the profinite completion $\hat{\pi} : G \to \hat{G}$ of
an abtract group $G$. We then prove the following theorem : if $k$ is a finite
prime field and if $V$ is a $k$-vector space, then, there is a natural
isomorphism between $\hat{V}$ (for the underlying additive group structure) and
the additive group of the double-dual $V^{**}$. This theorem gives
counter-examples concerning the iterated profinite completions of a group.
These phenomena don't occur in the topological case.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 18:40:56 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Bardavid",
"Colas",
"",
"IRMAR"
]
] |
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] |
801.2956 |
Wytse van Dijk
|
F.M. Toyama, W. van Dijk, Y. Nogami, M. Tabuchi, and Y. Kimura
|
Multi-phase matching in the Grover algorithm
|
10 pages, 8 figures
| null |
10.1103/PhysRevA.77.042324
| null |
quant-ph
| null |
Phase matching has been studied for the Grover algorithm as a way of
enhancing the efficiency of the quantum search. Recently Li and Li found that a
particular form of phase matching yields, with a single Grover operation, a
success probability greater than 25/27 for finding the equal-amplitude
superposition of marked states when the fraction of the marked states stored in
a database state is greater than 1/3. Although this single operation eliminates
the oscillations of the success probability that occur with multiple Grover
operations, the latter oscillations reappear with multiple iterations of Li and
Li's phase matching. In this paper we introduce a multi-phase matching subject
to a certain matching rule by which we can obtain a multiple Grover operation
that with only a few iterations yields a success probability that is almost
constant and unity over a wide range of the fraction of marked items. As an
example we show that a multi-phase operation with six iterations yields a
success probability between 99.8% and 100% for a fraction of marked states of
1/10 or larger.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 18:49:52 GMT"
},
{
"version": "v2",
"created": "Mon, 24 Mar 2008 18:43:51 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Toyama",
"F. M.",
""
],
[
"van Dijk",
"W.",
""
],
[
"Nogami",
"Y.",
""
],
[
"Tabuchi",
"M.",
""
],
[
"Kimura",
"Y.",
""
]
] |
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] |
801.2957 |
Gigliola Staffilani
|
Alexandru D. Ionescu and Gigliola Staffilani
|
Semilinear Schr\"odinger Flows on Hyperbolic Spaces: Scattering in H^1
| null | null | null | null |
math.AP
| null |
We prove global well-posedness and scattering in $H^1$ for the defocusing
nonlinear Schr\"{o}dinger equations \begin{equation*} \begin{cases}
&(i\partial_t+\Delta_\g)u=u|u|^{2\sigma}; &u(0)=\phi, \end{cases}
\end{equation*} on the hyperbolic spaces $\H^d$, $d\geq 2$, for exponents
$\sigma\in(0,2/(d-2))$. The main unexpected conclusion is scattering to linear
solutions in the case of small exponents $\sigma$; for comparison, on Euclidean
spaces scattering in $H^1$ is not known for any exponent $\sigma\in(1/d,2/d]$
and is known to fail for $\sigma\in(0,1/d]$. Our main ingredients are certain
noneuclidean global in time Strichartz estimates and noneuclidean Morawetz
inequalities.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 19:05:55 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Ionescu",
"Alexandru D.",
""
],
[
"Staffilani",
"Gigliola",
""
]
] |
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] |
801.2958 |
Ay\c{s}e \c{S}ahin
|
Ayse A. Sahin
|
The Z^d Alpern multi-tower theorem for rectangles: a tiling approach
|
14 pages, 3 figures
| null | null | null |
math.DS
| null |
We provide a proof of the Alpern multi-tower theorem for Z^d actions. We
reformulate the theorem as a problem of measurably tiling orbits of a Z^d
action by a collection of rectangles whose corresponding sides have no
non-trivial common divisors. We associate to such a collection of rectangles a
special family of generalized domino tilings. We then identify an intrinsic
dynamic property of these tilings, viewed as symbolic dynamical systems, which
allows for a multi-tower decomposition.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 19:30:27 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Sahin",
"Ayse A.",
""
]
] |
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] |
801.2959 |
Mark Veraar
|
Tuomas Hytonen, Mark Veraar
|
On Besov regularity of Brownian motions in infinite dimensions
|
to appear in Probab. Math. Statist (2008)
| null | null | null |
math.PR math.FA
| null |
We extend to the vector-valued situation some earlier work of Ciesielski and
Roynette on the Besov regularity of the paths of the classical Brownian motion.
We also consider a Brownian motion as a Besov space valued random variable. It
turns out that a Brownian motion, in this interpretation, is a Gaussian random
variable with some pathological properties. We prove estimates for the first
moment of the Besov norm of a Brownian motion. To obtain such results we
estimate expressions of the form $\E \sup_{n\geq 1}\|\xi_n\|$, where the
$\xi_n$ are independent centered Gaussian random variables with values in a
Banach space. Using isoperimetric inequalities we obtain two-sided inequalities
in terms of the first moments and the weak variances of $\xi_n$.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 19:34:06 GMT"
}
] | 2008-01-21T00:00:00 |
[
[
"Hytonen",
"Tuomas",
""
],
[
"Veraar",
"Mark",
""
]
] |
[
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] |
801.296 |
Jairo Bochi
|
Jairo Bochi
|
$C^1$-Generic Symplectic Diffeomorphisms: Partial Hyperbolicity and Zero
Center Lyapunov Exponents
|
Final version. To appear in Journal of the Institute of Mathematics
of Jussieu
|
J. Inst. Math. Jussieu, 9 (2010), 49-93
|
10.1017/S1474748009000061
| null |
math.DS math.PR math.SG
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We prove that if $f$ is a $C^1$-generic symplectic diffeomorphism then the
Oseledets splitting along almost every orbit is either trivial or partially
hyperbolic. In addition, if $f$ is not Anosov then all the exponents in the
center bundle vanish. This establishes in full a result announced by R.
Ma\~{n}\'{e} in the ICM 1983. The main technical novelty is a probabilistic
method for the construction of perturbations, using random walks.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 19:57:35 GMT"
},
{
"version": "v2",
"created": "Thu, 1 May 2008 23:09:10 GMT"
},
{
"version": "v3",
"created": "Sat, 3 May 2008 20:10:07 GMT"
},
{
"version": "v4",
"created": "Sun, 3 Aug 2008 08:45:41 GMT"
},
{
"version": "v5",
"created": "Sun, 14 Sep 2008 22:52:13 GMT"
}
] | 2010-05-03T00:00:00 |
[
[
"Bochi",
"Jairo",
""
]
] |
[
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] |
801.2961 |
Andrea Donarini
|
Georg Begemann, Dana Darau, Andrea Donarini, Milena Grifoni
|
Symmetry fingerprints of a benzene single-electron transistor
|
4 pages, 4 figures
|
Phys. Rev. B 77, 201406(R) (2008)
|
10.1103/PhysRevB.77.201406
| null |
cond-mat.mes-hall
| null |
The interplay between Coulomb interaction and orbital symmetry produces
specific transport characteristics in molecular single electron transistors
(SET) that can be considered as the fingerprints of the contacted molecule.
Specifically we predict, for a benzene SET, selective conductance suppression
and the appearance of negative differential conductance when changing the
contacts from para to meta configuration. Both effects originate from
destructive interference in transport involving states with orbital degeneracy.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 19:47:10 GMT"
}
] | 2008-07-04T00:00:00 |
[
[
"Begemann",
"Georg",
""
],
[
"Darau",
"Dana",
""
],
[
"Donarini",
"Andrea",
""
],
[
"Grifoni",
"Milena",
""
]
] |
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0.0048401388,
-0.0227958877,
-0.1328983009,
0.1381985396,
-0.0328319669,
-0.0068706656,
0.0018464915,
0.029936472
] |
801.2962 |
Y. Jack Ng
|
Y. Jack Ng
|
Spacetime foam: from entropy and holography to infinite statistics and
nonlocality
|
28 pages, LaTeX; added references, minor changes; invited review
article for the special issue in Entropy (http://www.mdpi.org) on "Quantum
spaces: where locality is not necessary, causality might not be, but entropy
certainly is," edited by P.A. Zizzi
| null |
10.3390/e10040441
| null |
hep-th astro-ph gr-qc quant-ph
| null |
Due to quantum fluctuations, spacetime is foamy on small scales. The degree
of foaminess is found to be consistent with holography, a principle prefigured
in the physics of black hole entropy. It has bearing on the ultimate accuracies
of clocks and measurements and the physics of quantum computation. Consistent
with existing archived data on active galactic nuclei from the Hubble Space
Telescope, the application of the holographic spacetime foam model to cosmology
requires the existence of dark energy which, we argue, is composed of an
enormous number of inert "particles" of extremely long wavelength. We suggest
that these "particles" obey infinite statistics in which all representations of
the particle permutation group can occur, and that the nonlocality present in
systems obeying infinite statistics may be related to the nonlocality present
in holographic theories. We also propose to detect spacetime foam by looking
for halos in the images of distant quasars, and argue that it does not modify
the GZK cutoff in the ultra-high energy cosmic ray spectrum and its
contributions to time-of-flight differences of high energy gamma rays from
distant GRB are too small to be detectable.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 20:16:20 GMT"
},
{
"version": "v2",
"created": "Thu, 28 Feb 2008 19:21:53 GMT"
}
] | 2015-05-13T00:00:00 |
[
[
"Ng",
"Y. Jack",
""
]
] |
[
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] |
801.2963 |
Richard A. Wade
|
M. A. Stark (1), Richard A. Wade (2), John R. Thorstensen (3),
Christopher S. Peters (3), Horace A. Smith (4), Robert D. Miller (4), and E.
M. Green (5) ((1) U. of Wyoming, (2) Pennsylvania State U., (3) Dartmouth
College, (4) Michigan State U., (5) U. of Arizona)
|
A New, Bright, Short-Period, Emission Line Binary in Ophiuchus
|
To be published in AJ, 16 pages, 6 figures. Uses AAS Latex
| null |
10.1088/0004-6256/135/3/991
| null |
astro-ph
| null |
The 11th magnitude star LS IV -08 3 has been classified previously as an OB
star in the Luminous Stars survey, or alternatively as a hot subdwarf. It is
actually a binary star. We present spectroscopy, spectroscopic orbital
elements, and time series photometry, from observations made at the Kitt Peak
National Observatory 2.1m, Steward Observatory 2.3m, MDM Observatory 1.3m and
2.4m, Hobby-Eberly 9.2m, and Michigan State University 0.6m telescopes. The
star exhibits emission of varying strength in the cores of H and He I
absorption lines. Emission is also present at 4686 Angstroms (He II) and near
4640/4650 Angstroms (N III/C III). Time-series spectroscopy collected from 2005
July to 2007 June shows coherent, periodic radial velocity variations of the
H-alpha line, which we interpret as orbital motion with a period of
0.1952894(10) days. High-resolution spectra show that there are two emission
components, one broad and one narrow, moving in antiphase, as might arise from
an accretion disk and the irradiated face of the mass donor star. Less
coherent, low-amplitude photometric variability is also present on a timescale
similar to the orbital period. Diffuse interstellar bands indicate considerable
reddening, which however is consistent with a distance of ~100-200 pc. The star
is the likely counterpart of a weak ROSAT X-ray source, whose properties are
consistent with accretion in a cataclysmic variable (CV) binary system. We
classify LS IV -08 3 as a new member of the UX UMa subclass of CV stars.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 20:21:04 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Stark",
"M. A.",
""
],
[
"Wade",
"Richard A.",
""
],
[
"Thorstensen",
"John R.",
""
],
[
"Peters",
"Christopher S.",
""
],
[
"Smith",
"Horace A.",
""
],
[
"Miller",
"Robert D.",
""
],
[
"Green",
"E. M.",
""
]
] |
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] |
801.2964 |
Natalia Berloff
|
Natalia G. Berloff
|
Vortex Splitting in Subcritical Nonlinear Schrodinger Equation
|
Invited submission to the special issue on Vortex Rings, Journal of
Fluid Dynamics Research
| null |
10.1088/0169-5983/41/5/051403
| null |
cond-mat.other physics.flu-dyn
| null |
Vortices and axisymmetric vortex rings are considered in the framework of the
subcritical nonlinear Schrodinger equations. The higher order nonlinearity
present in such systems models many-body interactions in superfluid systems and
allows one to study the effects of negative pressure on vortex dynamics. We
find the critical pressure for which the straight-line vortex becomes unstable
to radial expansion of the core. The energy of the straight-line vortices and
energy, impulse and velocity of vortex rings are calculated. The effect of a
varying pressure on the vortex core is studied. It is shown that under the
action of the periodically varying pressure field a vortex ring may split into
many vortex rings and the conditions for which this happens are elucidated.
These processes are also relevant to experiments in Bose-Einstein condensates
where the strength and the sign of two-body interactions can be changed via
Feshbach resonance.
|
[
{
"version": "v1",
"created": "Thu, 17 Jan 2008 22:31:18 GMT"
}
] | 2015-05-13T00:00:00 |
[
[
"Berloff",
"Natalia G.",
""
]
] |
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] |
801.2965 |
R. G. Vishwakarma
|
Jayant V. Narlikar, Geoffrey Burbidge and R.G. Vishwakarma
|
Cosmology and Cosmogony in a Cyclic Universe
|
51 pages including 1 figure
|
J.Astrophys.Astron.28:67-99,2007
|
10.1007/s12036-007-0007-5
| null |
astro-ph gr-qc hep-th
| null |
In this paper we discuss the properties of the quasi-steady state
cosmological model (QSSC) developed in 1993 in its role as a cyclic model of
the universe driven by a negative energy scalar field. We discuss the origin of
such a scalar field in the primary creation process first described by F. Hoyle
and J. V. Narlikar forty years ago. It is shown that the creation processes
which takes place in the nuclei of galaxies are closely linked to the high
energy and explosive phenomena, which are commonly observed in galaxies at all
redshifts.
The cyclic nature of the universe provides a natural link between the places
of origin of the microwave background radiation (arising in hydrogen burning in
stars), and the origin of the lightest nuclei (H, D, He$^3$ and He$^4$). It
also allows us to relate the large scale cyclic properties of the universe to
events taking place in the nuclei of galaxies. Observational evidence shows
that ejection of matter and energy from these centers in the form of compact
objects, gas and relativistic particles is responsible for the population of
quasi-stellar objects (QSOs) and gamma-ray burst sources in the universe.
In the later parts of the paper we briefly discuss the major unsolved
problems of this integrated cosmological and cosmogonical scheme. These are the
understanding of the origin of the intrinsic redshifts, and the periodicities
in the redshift distribution of the QSOs.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 20:38:18 GMT"
}
] | 2015-05-13T00:00:00 |
[
[
"Narlikar",
"Jayant V.",
""
],
[
"Burbidge",
"Geoffrey",
""
],
[
"Vishwakarma",
"R. G.",
""
]
] |
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] |
801.2966 |
Joseph Lazio
|
J. Lazio (NRL)
|
Radio Wavelength Transients: Current and Emerging Prospects
|
to appear in proceedings of Hot-wiring the Transient Universe, 2008
March issue of Astronomische Nachrichten
| null |
10.1002/asna.200710935
|
NRL/JA/7210-07-0327
|
astro-ph
| null |
Known classes of radio wavelength transients range from the nearby--stellar
flares and radio pulsars--to the distant Universe--\gamma-ray burst afterglows.
Hypothesized classes of radio transients include analogs of known objects,
e.g., extrasolar planets emitting Jovian-like radio bursts and giant-pulse
emitting pulsars in other galaxies, to the exotic, prompt emission from
\gamma-ray bursts, evaporating black holes, and transmitters from other
civilizations. A number of instruments and facilities are either under
construction or in early observational stages and are slated to become
available in the next few years. With a combination of wide fields of view and
wavelength agility, the detection and study of radio transients will improve
immensely.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 20:58:04 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Lazio",
"J.",
"",
"NRL"
]
] |
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] |
801.2967 |
Roberta Humphreys
|
Roberta M. Humphreys, Kris Davidson, and Michael Koppleman
|
The Early Spectra of Eta Carinae 1892 to 1941 and the Onset of Its High
Excitation Emission Spectrum
|
41 pages, 12 figures
| null |
10.1088/0004-6256/135/4/1249
| null |
astro-ph
| null |
The observed behavior of eta Car from 1860 to 1940 has not been considered in
most recent accounts, nor has it been explained in any quantitative model. We
have used modern digital processing techniques to examine Harvard
objective-prism spectra made from 1892 to 1941. Relatively high-excitation He I
4471 and [Fe III] 4658 emission, conspicuous today, were weak and perhaps
absent throughout those years. Feast et al. noted this qualitative fact for
other pre-1920 spectra, but we quantify it and extend it to a time only three
years before Gaviola's first observations of the high-excitation features.
Evidently the supply of helium-ionizing photons(lambda < 504A) grew rapidly
between 1941 and 1944. The apparent scarcity of such far-UV radiation before
1944 is difficult to explain in models that employ a hot massive secondary
star,} because no feasible dense wind or obscuration by dust would have hidden
the photoionization caused by the proposed companion during most of its orbital
period. We also discuss the qualitative near-constancy of the spectrum from
1900 to 1940, and eta Car's photometric and spectroscopic transition between
1940 and 1953.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 20:39:49 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Humphreys",
"Roberta M.",
""
],
[
"Davidson",
"Kris",
""
],
[
"Koppleman",
"Michael",
""
]
] |
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] |
801.2968 |
Eric Linder
|
Eric V. Linder
|
Mapping the Cosmological Expansion
|
49 pages, 29 figures; Review invited for Reports on Progress in
Physics; v2 minor changes to match accepted version
|
Rept.Prog.Phys.71:056901,2008
|
10.1088/0034-4885/71/5/056901
| null |
astro-ph
| null |
The ability to map the cosmological expansion has developed enormously,
spurred by the turning point one decade ago of the discovery of cosmic
acceleration. The standard model of cosmology has shifted from a matter
dominated, standard gravity, decelerating expansion to the present search for
the origin of acceleration in the cosmic expansion. We present a wide ranging
review of the tools, challenges, and physical interpretations. The tools
include direct measures of cosmic scales through Type Ia supernova luminosity
distances, and angular distance scales of baryon acoustic oscillation and
cosmic microwave background density perturbations, as well as indirect probes
such as the effect of cosmic expansion on the growth of matter density
fluctuations. Accurate mapping of the expansion requires understanding of
systematic uncertainties in both the measurements and the theoretical
framework, but the result will give important clues to the nature of the
physics behind accelerating expansion and to the fate of the universe.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 21:00:08 GMT"
},
{
"version": "v2",
"created": "Fri, 7 Mar 2008 16:55:10 GMT"
}
] | 2009-06-23T00:00:00 |
[
[
"Linder",
"Eric V.",
""
]
] |
[
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] |
801.2969 |
Steven Bickerton
|
S.J. Bickerton, J.J. Kavelaars, and D.L. Welch
|
A Search for sub-km KBOs with the Method of Serendipitous Stellar
Occultations
|
Accepted for publication in AJ
| null |
10.1088/0004-6256/135/3/1039
| null |
astro-ph
| null |
The results of a search for sub-km Kuiper Belt Objects (KBOs) with the method
of serendipitous stellar occultations are reported. Photometric time series
were obtained on the 1.8m telescope at the Dominion Astrophysical Observatory
(DAO) in Victoria, BC, and were analyzed for the presence of occultation
events. Observations were performed at 40 Hz and included a total of 5.0
star-hours for target stars in the ecliptic open cluster M35 (beta=0.9deg), and
2.1 star-hours for control stars in the off-ecliptic open cluster M34
(beta=25.7deg). To evaluate the recovery fraction of the analysis method, and
thereby determine the limiting detectable size, artificial occultation events
were added to simulated time series (1/f scintillation-like power-spectra), and
to the real data. No viable candidate occultation events were detected. This
limits the cumulative surface density of KBOs to 3.5e10 deg^{-2} (95%
confidence) for KBOs brighter than m_R=35.3 (larger than ~860m in diameter,
assuming a geometric albedo of 0.04 and a distance of 40 AU). An evaluation of
TNO occultations reported in the literature suggests that they are unlikely to
be genuine, and an overall 95%-confidence upper limit on the surface density of
2.8e9 deg^{-2} is obtained for KBOs brighter than m_R=35 (larger than ~1 km in
diameter, assuming a geometric albedo of 0.04 and a distance of 40 AU) when all
existing surveys are combined.
|
[
{
"version": "v1",
"created": "Sat, 19 Jan 2008 21:43:58 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Bickerton",
"S. J.",
""
],
[
"Kavelaars",
"J. J.",
""
],
[
"Welch",
"D. L.",
""
]
] |
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] |
801.297 |
Subir Sachdev
|
Markus Mueller and Subir Sachdev
|
Collective cyclotron motion of the relativistic plasma in graphene
|
16 pages, 2 figures; calculation of giant Nernst effect in graphene
added
|
Phys.Rev.B78:115419,2008
|
10.1103/PhysRevB.78.115419
| null |
cond-mat.str-el hep-th
|
http://arxiv.org/licenses/nonexclusive-distrib/1.0/
|
We present a theory of the finite temperature thermo-electric response
functions of graphene, in the hydrodynamic regime induced by electron-electron
collisions. In moderate magnetic fields, the Dirac particles undergo a
collective cyclotron motion with a temperature-dependent relativistic cyclotron
frequency proportional to the net charge density of the Dirac plasma. In
contrast to the undamped cyclotron pole in Galilean-invariant systems (Kohn's
theorem), here there is a finite damping induced by collisions between the
counter-propagating particles and holes. This cyclotron motion shows up as a
damped pole in the frequency dependent conductivities, and should be readily
detectable in microwave measurements at room temperature. We also discuss the
large Nernst effect to be expected in graphene.
|
[
{
"version": "v1",
"created": "Mon, 21 Jan 2008 20:24:35 GMT"
},
{
"version": "v2",
"created": "Wed, 19 Mar 2008 02:27:45 GMT"
},
{
"version": "v3",
"created": "Fri, 19 Sep 2008 20:52:18 GMT"
}
] | 2008-11-07T00:00:00 |
[
[
"Mueller",
"Markus",
""
],
[
"Sachdev",
"Subir",
""
]
] |
[
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] |
801.2971 |
Isabelle Dicaire
|
I. Dicaire (1), C. Carignan (1), P. Amram (2), O. Hernandez (1), L.
Chemin (3), O. Daigle (1, 2), M.-M. de Denus-Baillargeon (1, 4), C. Balkowski
(3), A. Boselli (2), K. Fathi (5) and R. C. Kennicutt (6) ((1) Universit\'e
de Montr\'eal, (2) LAM, (3) Observatoire de Paris-GEPI, (4) Institut Fresnel,
(5) IAC, (6) IoA)
|
H-alpha Kinematics of the SINGS Nearby Galaxies Survey. II
|
18 pages, 5 figures, 4 tables. Accepted for publication in MNRAS. All
high-res. figures are available at
http://www.astro.umontreal.ca/fantomm/singsII/
| null |
10.1111/j.1365-2966.2008.12868.x
| null |
astro-ph
| null |
This is the second part of an H-alpha kinematics follow-up survey of the
Spitzer Infrared Nearby Galaxies Survey (SINGS) sample. The aim of this program
is to shed new light on the role of baryons and their kinematics and on the
dark/luminous matter relation in the star forming regions of galaxies, in
relation with studies at other wavelengths. The data for 37 galaxies are
presented. The observations were made using Fabry-Perot interferometry with the
photon-counting camera FaNTOmM on 4 different telescopes, namely the
Canada-France-Hawaii 3.6m, the ESO La Silla 3.6m, the William Herschel 4.2m,
and the Observatoire du mont Megantic 1.6m telescopes. The velocity fields are
computed using custom IDL routines designed for an optimal use of the data. The
kinematical parameters and rotation curves are derived using the GIPSY
software. It is shown that non-circular motions associated with galactic bars
affect the kinematical parameters fitting and the velocity gradient of the
rotation curves. This leads to incorrect determinations of the baryonic and
dark matter distributions in the mass models derived from those rotation
curves.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 21:00:40 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Dicaire",
"I.",
""
],
[
"Carignan",
"C.",
""
],
[
"Amram",
"P.",
""
],
[
"Hernandez",
"O.",
""
],
[
"Chemin",
"L.",
""
],
[
"Daigle",
"O.",
""
],
[
"de Denus-Baillargeon",
"M. -M.",
""
],
[
"Balkowski",
"C.",
""
],
[
"Boselli",
"A.",
""
],
[
"Fathi",
"K.",
""
],
[
"Kennicutt",
"R. C.",
""
]
] |
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] |
801.2972 |
Brad Hansen
|
Brad Hansen (UCLA)
|
On the Absorption and Redistribution of Energy in Irradiated Planets
|
42 pages, 25 figures. Submitted to ApJ in June
| null |
10.1086/591964
| null |
astro-ph
| null |
We present a sequence of toy models for irradiated planet atmospheres, in
which the effects of geometry and energy redistribution are modelled
self-consistently. We use separate but coupled grey atmosphere models to treat
the ingoing stellar irradiation and outgoing planetary reradiation. We
investigate how observed quantities such as full phase secondary eclipses and
orbital phase curves depend on various important parameters, such as the depth
at which irradiation is absorbed and the depth at which energy is
redistributed. We also compare our results to the more detailed radiative
transfer models in the literature, in order to understand how those map onto
the toy model parameter space. Such an approach can prove complementary to more
detailed calculations, in that they demonstrate, in a simple way, how the
solutions change depending on where, and how, energy redistribution occurs. As
an example of the value of such models, we demonstrate how energy
redistribution and temperature equilibration at moderate optical depths can
lead to temperature inversions in the planetary atmosphere, which may be of
some relevance to recent observational findings.
|
[
{
"version": "v1",
"created": "Fri, 18 Jan 2008 21:42:39 GMT"
}
] | 2009-11-13T00:00:00 |
[
[
"Hansen",
"Brad",
"",
"UCLA"
]
] |
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