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706.3014
|
Bayesian Calibrated Significance Levels Applied to the Spectral Tilt and
Hemispherical Asymmetry
|
Bayesian model selection provides a formal method of determining the level of
support for new parameters in a model. However, if there is not a specific
enough underlying physical motivation for the new parameters it can be hard to
assign them meaningful priors, an essential ingredient of Bayesian model
selection. Here we look at methods maximizing the prior so as to work out what
is the maximum support the data could give for the new parameters. If the
maximum support is not high enough then one can confidently conclude that the
new parameters are unnecessary without needing to worry that some other prior
may make them significant. We discuss a computationally efficient means of
doing this which involves mapping p-values onto upper bounds of the Bayes
factor (or odds) for the new parameters. A p-value of 0.05 ($1.96\sigma$)
corresponds to odds less than or equal to 5:2 which is below the `weak' support
at best threshold. A p-value of 0.0003 ($3.6\sigma$) corresponds to odds of
less than or equal to 150:1 which is the `strong' support at best threshold.
Applying this method we find that the odds on the scalar spectral index being
different from one are 49:1 at best. We also find that the odds that there is
primordial hemispherical asymmetry in the cosmic microwave background are 9:1
at best.
|
astro-ph gr-qc hep-ph hep-th
|
bayesian model selection provides a formal method of determining the level of support for new parameters in a model however if there is not a specific enough underlying physical motivation for the new parameters it can be hard to assign them meaningful priors an essential ingredient of bayesian model selection here we look at methods maximizing the prior so as to work out what is the maximum support the data could give for the new parameters if the maximum support is not high enough then one can confidently conclude that the new parameters are unnecessary without needing to worry that some other prior may make them significant we discuss a computationally efficient means of doing this which involves mapping pvalues onto upper bounds of the bayes factor or odds for the new parameters a pvalue of 005 196sigma corresponds to odds less than or equal to 52 which is below the weak support at best threshold a pvalue of 00003 36sigma corresponds to odds of less than or equal to 1501 which is the strong support at best threshold applying this method we find that the odds on the scalar spectral index being different from one are 491 at best we also find that the odds that there is primordial hemispherical asymmetry in the cosmic microwave background are 91 at best
|
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|
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|
706.3015
|
Oxide spintronics
|
Concomitant with the development of metal-based spintronics in the late
1980's and 1990's, important advances were made on the growth of high-quality
oxide thin films and heterostructures. While this was at first motivated by the
discovery of high-temperature superconductivity in perovskite Cu oxides, this
technological breakthrough was soon applied to other transition metal oxides,
and notably mixed-valence manganites. The discovery of colossal
magnetoresistance in manganite films triggered an intense research activity on
these materials, but the first notable impact of magnetic oxides in the field
of spintronics was the use of such manganites as electrodes in magnetic tunnel
junctions, yielding tunnel magnetoresistance ratios one order of magnitude
larger than what had been obtained with transition metal electrodes. Since
then, the research on oxide spintronics has been intense with the latest
developments focused on diluted magnetic oxides and more recently on
multiferroics. In this paper, we will review the most important results on
oxide spintronics, emphasizing materials physics as well as spin-dependent
transport phenomena, and finally give some perspectives on how the flurry of
new magnetic oxides could be useful for next-generation spintronics devices.
|
cond-mat.mtrl-sci cond-mat.str-el
|
concomitant with the development of metalbased spintronics in the late 1980s and 1990s important advances were made on the growth of highquality oxide thin films and heterostructures while this was at first motivated by the discovery of hightemperature superconductivity in perovskite cu oxides this technological breakthrough was soon applied to other transition metal oxides and notably mixedvalence manganites the discovery of colossal magnetoresistance in manganite films triggered an intense research activity on these materials but the first notable impact of magnetic oxides in the field of spintronics was the use of such manganites as electrodes in magnetic tunnel junctions yielding tunnel magnetoresistance ratios one order of magnitude larger than what had been obtained with transition metal electrodes since then the research on oxide spintronics has been intense with the latest developments focused on diluted magnetic oxides and more recently on multiferroics in this paper we will review the most important results on oxide spintronics emphasizing materials physics as well as spindependent transport phenomena and finally give some perspectives on how the flurry of new magnetic oxides could be useful for nextgeneration spintronics devices
|
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|
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|
706.3016
|
AC conductivity of graphene: from tight-binding model to 2+1-dimensional
quantum electrodynamics
|
We consider the relationship between the tight-binding Hamiltonian of the
two-dimensional honeycomb lattice of carbon atoms with nearest neighbor hopping
only and the 2+1 dimensional Hamiltonian of quantum electrodynamics which
follows in the continuum limit. We pay particular attention to the symmetries
of the free Dirac fermions including spatial inversion, time reversal, charge
conjugation and chirality. We illustrate the power of such a mapping by
considering the effect of the possible symmetry breaking which corresponds to
the creation of a finite Dirac mass, on various optical properties. In
particular, we consider the diagonal AC conductivity with emphasis on how the
finite Dirac mass might manifest itself in experiment. The optical sum rules
for the diagonal and Hall conductivities are discussed.
|
cond-mat.mes-hall cond-mat.str-el hep-ph
|
we consider the relationship between the tightbinding hamiltonian of the twodimensional honeycomb lattice of carbon atoms with nearest neighbor hopping only and the 21 dimensional hamiltonian of quantum electrodynamics which follows in the continuum limit we pay particular attention to the symmetries of the free dirac fermions including spatial inversion time reversal charge conjugation and chirality we illustrate the power of such a mapping by considering the effect of the possible symmetry breaking which corresponds to the creation of a finite dirac mass on various optical properties in particular we consider the diagonal ac conductivity with emphasis on how the finite dirac mass might manifest itself in experiment the optical sum rules for the diagonal and hall conductivities are discussed
|
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|
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|
706.3017
|
Relativistic Three-Fermion Wave Equations in Reformulated QED and
Relativistic Effects in Muonium Minus
|
The variational method, within the Hamiltonian formalism of reformulated QED
is used to determine relativistic wave equations for a system of three fermions
of arbitrary mass interacting electromagnetically. The interaction kernels of
the equations are, in essence, the invariant $\mathcal{M}$ matrices in lowest
order. The equations are used to obtain relativistic $O(\alpha^2)$ corrections
to the non-relativistic ground state energy levels of the Muonium negative ion
($\mu^+ e^- e^-$) as well as of $\mathrm{Ps}^-$ and $\mathrm{H}^-$, using
approximate variational three-body wave functions. The results are compared
with other calculations, where available. The relativistic correction for
Mu$^-$ is found to be $-1.0773 \times 10^{-4}$ eV.
|
physics.atom-ph physics.chem-ph
|
the variational method within the hamiltonian formalism of reformulated qed is used to determine relativistic wave equations for a system of three fermions of arbitrary mass interacting electromagnetically the interaction kernels of the equations are in essence the invariant mathcalm matrices in lowest order the equations are used to obtain relativistic oalpha2 corrections to the nonrelativistic ground state energy levels of the muonium negative ion mu e e as well as of mathrmps and mathrmh using approximate variational threebody wave functions the results are compared with other calculations where available the relativistic correction for mu is found to be 10773 times 104 ev
|
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|
[-0.11230317898569446, 0.1654355615404818, -0.03390873934361426, 0.13437555053992672, 0.00948300731697065, -0.12594857895472908, -0.03363899217790687, 0.30482120749851066, -0.20717485819705853, -0.31809023908092915, -0.0036550607354215838, -0.3058317150902368, -0.01869963658699656, 0.15234134402171726, 0.08155373453194567, 0.12465881512445562, 0.06961043884375077, 0.06946639797659408, -0.11014598660974526, -0.16570252345363592, 0.30890167443373917, 0.05572886887809956, 0.1977464610382038, 0.06467306661401309, 0.1037452096238221, -0.021889065255356187, 0.04296389522998795, -0.023681193549076423, -0.11635756232534927, 0.06956549554917157, 0.24399396735894055, 0.029617403999117074, 0.20513609968418, -0.4219697401219723, -0.18021186091380728, 0.05694708939386057, 0.11206582880250233, 0.1301134130301173, 0.027401410052370206, -0.33148280755781073, 0.0382020495205378, -0.21244858768220773, -0.18175865154640347, -0.09460981404774037, 0.016344623809095984, 0.0226463159619301, -0.3303064310594517, 0.11034553474746644, -0.019847656222398157, -0.041718883009119, -0.10908192422186189, -0.16539453210505456, -0.03333402165741313, 0.05165448310036285, 0.0288019229374899, 0.07066934352612816, 0.11820390046227212, -0.08974513394173746, -0.12208657478913665, 0.4778390139542228, -0.11611873279074572, -0.24779131191819176, 0.1420837476730858, -0.14219479499768248, -0.09144822242852374, 0.1642622291749599, 0.1778444110087174, 0.148835124525552, -0.1758599782399103, 0.13912095034930982, -0.005457546008698295, 0.10284986565142497, 0.05526784437197242, 0.04517596965089586, 0.11932738750771273, 0.08869800823695008, 0.021536175088555206, 0.0788389353999496, -0.0625140954347729, -0.11011064985045689, -0.3254626423083976, -0.13959578536517203, -0.1807528974479247, 0.09180674793320827, -0.057945167677626516, -0.14529927408176602, 0.34058571772709234, 0.13290127818746603, 0.15357516110673838, 0.010184278133879964, 0.2704119649418977, 0.21660828396595797, 0.039455165661981, 0.07397985094861474, 0.2686870065380764, 0.2044490644041741, 0.045831592831139766, -0.2560789999415112, -0.035144229666056, 0.11464724691548184]
|
706.3018
|
Tomographic Representation of Minisuperspace Quantum Cosmology and
Noether Symmetries
|
The probability representation, in which cosmological quantum states are
described by a standard positive probability distribution, is constructed for
minisuperspace models selected by Noether symmetries. In such a case, the
tomographic probability distribution provides the classical evolution for the
models and can be considered an approach to select "observable" universes. Some
specific examples, derived from Extended Theories of Gravity, are worked out.
We discuss also how to connect tomograms, symmetries and cosmological
parameters.
|
gr-qc hep-th
|
the probability representation in which cosmological quantum states are described by a standard positive probability distribution is constructed for minisuperspace models selected by noether symmetries in such a case the tomographic probability distribution provides the classical evolution for the models and can be considered an approach to select observable universes some specific examples derived from extended theories of gravity are worked out we discuss also how to connect tomograms symmetries and cosmological parameters
|
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|
[-0.07215226635541001, 0.1185313381004699, -0.11894150142085878, 0.16809724335246146, -0.06763594143398821, -0.17264813423309833, -0.0133191462740149, 0.34509263937808066, -0.2491233639725267, -0.28187516492421494, 0.06257857267317452, -0.25345400575873733, -0.119758970831355, 0.1704073926331858, -0.05144029147029944, 0.05406419802712251, -0.004922387199731518, 0.04012633418689852, -0.09638773138022484, -0.26842145810592666, 0.35265941189423405, 0.0798995131036675, 0.2438205724250372, -0.07886114354844984, 0.09449967914197134, -0.0496378381455904, -0.06866223763751045, 0.04278316498695783, -0.16581882473897852, 0.04443044360003064, 0.2569585478883946, 0.18282194531280294, 0.18864169923512086, -0.39699902898338557, -0.2915051059976016, 0.08651493835160891, 0.13485262895079508, 0.1656256771681524, -0.060030338290619524, -0.3428012983178184, 0.03011944589575064, -0.18813868417493898, -0.16951416788801346, -0.1349937405105527, -0.006377163687593316, -0.007230792417867135, -0.2506346497939874, 0.08836962386913126, -0.015827806066874773, -0.01362719285072223, -0.060797160819861785, -0.1020466108831947, -0.05335596877418152, 0.11715973564742567, 0.02677359528622705, -0.027526674125573202, 0.12209186326610307, -0.1397748436931878, -0.1648345595378786, 0.4003216322409372, -0.057977748817879045, -0.29097992355284624, 0.12166054537902547, -0.11386523153377723, -0.1728519657881905, 0.03561198625917712, 0.10591648489696114, 0.11402909355620815, -0.1720882972625837, 0.11346499984041383, -0.015654011973983622, 0.10051785836838288, 0.04526685881237053, 0.02847647990980377, 0.2894185849605766, 0.039515740754822753, 0.008836836381879163, 0.11785632871850457, -0.04975921260065412, -0.16788887272729244, -0.38180702312351905, -0.13169484630016584, -0.1864023834900701, 0.09449077744917204, -0.09654817258108292, -0.11094790362842279, 0.38347783123385415, 0.15808575847190134, 0.1732813066305363, 0.058247153675949126, 0.19199097065306078, 0.14647511862320442, 0.02914944744018251, 0.056820554824622525, 0.20455315769913174, 0.1500275369720814, 0.014682855645245681, -0.1666904523321236, 0.006597778916180338, 0.06469766239393247]
|
706.3019
|
Neutrino Backgrounds to Dark Matter Searches
|
Neutrino coherent scattering cross sections can be as large as 10^{-39} cm^2,
while current dark matter experiments have sensitivities to WIMP coherent
scattering cross sections five orders of magnitude smaller; future experiments
plan to have sensitivities to cross sections as small as 10^{-48} cm^2. With
large target masses and few keV recoil energy detection thresholds, neutral
current coherent scattering of solar neutrinos becomes an irreducible
background in dark matter searches. In the current zero-background analysis
paradigm, neutrino coherent scattering will limit the achievable sensitivity to
dark matter scattering cross sections, at the level of 10^{-46} cm^2.
|
astro-ph hep-ex nucl-ex
|
neutrino coherent scattering cross sections can be as large as 1039 cm2 while current dark matter experiments have sensitivities to wimp coherent scattering cross sections five orders of magnitude smaller future experiments plan to have sensitivities to cross sections as small as 1048 cm2 with large target masses and few kev recoil energy detection thresholds neutral current coherent scattering of solar neutrinos becomes an irreducible background in dark matter searches in the current zerobackground analysis paradigm neutrino coherent scattering will limit the achievable sensitivity to dark matter scattering cross sections at the level of 1046 cm2
|
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|
[-0.07691904799139593, 0.2609200908884001, 0.009503267724843075, 0.17840672264962146, -0.022243845004898805, -0.05955110059585422, -0.03439034308636716, 0.3712222348355378, -0.16629582015351238, -0.3902545514332208, -0.01239409052504925, -0.39621878543403, 0.09683837153716013, 0.22510677605168894, 0.10671989508167219, 0.06621889122955811, 0.022585975192972303, 4.778577325244745e-05, -0.06196101853856817, -0.24915935322981872, 0.2381594679512394, 0.13286160296411254, 0.25138431126833893, 0.1714797490858473, 0.1046070836285556, 0.02277885236981092, -0.023883729891773935, -0.11624291987876252, -0.11256935641449672, 0.05108192074112594, 0.3805679262247092, 0.0721882703431523, 0.044310575009149034, -0.42821288644336164, -0.14382273538528048, 0.17678708180998606, 0.17013067413912117, 0.053640897014702205, -0.03233189724657374, -0.34302702502463944, 0.007952357903680726, -0.2788026232835061, -0.12616228990858266, -0.03754814035346499, 0.01824111980871142, -0.02753894653930426, -0.1977805536783611, 0.10903919744790376, -0.11964950481099852, -0.09277789610617522, -0.0847011591734675, -0.20554630493279546, 0.0025200694750916832, -0.05380898033035919, 0.10336778390531738, -0.03032610464742902, 0.3203308490628842, -0.23694273315292472, -0.13328156480565667, 0.3713463190166901, -0.15188627567355675, -0.08590006015341108, 0.11762281674600672, -0.19221927801845595, -0.090208479622864, 0.32041858611046337, 0.2133248991255338, 0.06989172681096534, -0.1658318285869124, 0.06363798829079315, -0.031996402591175865, 0.21385759119099626, 0.10969496304460336, 0.08296708256239071, 0.3197950921797504, 0.2859754915892457, 0.11280123010995642, -0.11822796753767761, -0.2582451540850646, 0.03538055119376319, -0.3657868411780025, -0.06130465865135193, -0.006484624308844407, 0.13142582953999712, -0.048456505974021034, -0.053901127578380205, 0.26880944467848167, 0.12695412834970435, 0.2546461799283861, -0.0017159173027418244, 0.40660038034669316, 0.14167005154013168, 0.04335803521583633, -0.030649127647241887, 0.3829471878852928, 0.18514244072139263, 0.06342652331659338, -0.14966550265671685, -0.017357543819040682, -0.03085228403566968]
|
706.302
|
Unconventional elasticity in smectic-A elastomers
|
We study two aspects of the elasticity of smectic-$A$ elastomers that make
these materials genuinely and qualitatively different from conventional
uniaxial rubbers. Under strain applied parallel to the layer normal, monodomain
smectic-$A$ elastomers exhibit a drastic change in Young's modulus above a
threshold strain value of about 3%, as has been measured in experiments by
Nishikawa and Finkelmann [Macromol. Chem. Phys. {\bf 200}, 312 (1999)]. Our
theory predicts that such strains induce a transition to a smectic-$C$-like
state and that it is this transition that causes the change in elastic modulus.
We calculate the stress-strain behavior as well as the tilt of the smectic
layers and the molecular orientation for strain along the layer normal, and we
compare our findings with the experimental data. We also study the
electroclinic effect in chiral smectic-$A^\ast$ elastomers. According to
experiments by Lehmann {\em et al}. [Nature {\bf 410}, 447 (2001)] and
K\"{o}hler {\em et al}. [Applied Physics A {\bf 80}, 381 (2003)], this effect
leads in smectic-$A^\ast$ elastomers to a giant or, respectively, at least very
large lateral electrostriction. Incorporating polarization into our theory, we
calculate the height change of smectic-$A^\ast$ elastomer films in response to
a lateral external electric field, and we compare this result to the
experimental findings.
|
cond-mat.soft
|
we study two aspects of the elasticity of smectica elastomers that make these materials genuinely and qualitatively different from conventional uniaxial rubbers under strain applied parallel to the layer normal monodomain smectica elastomers exhibit a drastic change in youngs modulus above a threshold strain value of about 3 as has been measured in experiments by nishikawa and finkelmann macromol chem phys bf 200 312 1999 our theory predicts that such strains induce a transition to a smecticclike state and that it is this transition that causes the change in elastic modulus we calculate the stressstrain behavior as well as the tilt of the smectic layers and the molecular orientation for strain along the layer normal and we compare our findings with the experimental data we also study the electroclinic effect in chiral smecticaast elastomers according to experiments by lehmann em et al nature bf 410 447 2001 and kohler em et al applied physics a bf 80 381 2003 this effect leads in smecticaast elastomers to a giant or respectively at least very large lateral electrostriction incorporating polarization into our theory we calculate the height change of smecticaast elastomer films in response to a lateral external electric field and we compare this result to the experimental findings
|
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|
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|
706.3021
|
Independence property and hyperbolic groups
|
We prove that existentially closed $CSA$-groups have the independence
property. This is done by showing that there exist words having the
independence property relatively to the class of torsion-free hyperbolic
groups.
|
math.LO math.GR
|
we prove that existentially closed csagroups have the independence property this is done by showing that there exist words having the independence property relatively to the class of torsionfree hyperbolic groups
|
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|
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|
706.3022
|
Dynamical tunneling in macroscopic systems
|
We investigate macroscopic dynamical quantum tunneling (MDQT) in the driven
Duffing oscillator, charateristic for Josephson junction physics and
nanomechanics. Under resonant conditions between stable coexisting states of
such systems we calculate the tunneling rate. In macroscopic systems coupled to
a heat bath, MDQT can be masked by driving-induced activation. We compare both
processes, identify conditions under which tunneling can be detected with
present day experimental means and suggest a protocol for its observation.
|
cond-mat.supr-con
|
we investigate macroscopic dynamical quantum tunneling mdqt in the driven duffing oscillator charateristic for josephson junction physics and nanomechanics under resonant conditions between stable coexisting states of such systems we calculate the tunneling rate in macroscopic systems coupled to a heat bath mdqt can be masked by drivinginduced activation we compare both processes identify conditions under which tunneling can be detected with present day experimental means and suggest a protocol for its observation
|
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|
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|
706.3023
|
Impact of the Neutrino Magnetic Moment on the Neutrino Fluxes and the
Electron Fraction in core-collapse Supernovae
|
We explore the effect of the neutrino magnetic moment on neutrino scattering
with matter in a core-collapse Supernova. We study the impact both on the
neutrino fluxes and on the electron fraction. We find that sizeable
modifications require very large magnetic moments both for Dirac and Majorana
neutrinos.
|
astro-ph
|
we explore the effect of the neutrino magnetic moment on neutrino scattering with matter in a corecollapse supernova we study the impact both on the neutrino fluxes and on the electron fraction we find that sizeable modifications require very large magnetic moments both for dirac and majorana neutrinos
|
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|
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|
706.3024
|
On a generalization of Dehn's algorithm
|
Viewing Dehn's algorithm as a rewriting system, we generalise to allow an
alphabet containing letters which do not necessarily represent group elements.
This extends the class of groups for which the algorithm solves the word
problem to include nilpotent groups, many relatively hyperbolic groups
including geometrically finite groups and fundamental groups of certain
geometrically decomposable manifolds. The class has several nice closure
properties. We also show that if a group has an infinite subgroup and one of
exponential growth, and they commute, then it does not admit such an algorithm.
We dub these Cannon's algorithms.
|
math.GR math.GT
|
viewing dehns algorithm as a rewriting system we generalise to allow an alphabet containing letters which do not necessarily represent group elements this extends the class of groups for which the algorithm solves the word problem to include nilpotent groups many relatively hyperbolic groups including geometrically finite groups and fundamental groups of certain geometrically decomposable manifolds the class has several nice closure properties we also show that if a group has an infinite subgroup and one of exponential growth and they commute then it does not admit such an algorithm we dub these cannons algorithms
|
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|
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|
706.3025
|
Contact Interactions and Resonance-Like Physics at Present and Future
Colliders from Unparticles
|
High scale conformal physics can lead to unusual unparticle stuff at our low
energies. In this paper we discuss how the exchange of unparticles between
Standard Model fields can lead to new contact interaction physics as well as a
pseudoresonance-like structure, an unresonance, that might be observable at the
Tevatron or LHC in, e.g., the Drell-Yan channel. The specific signatures of
this scenario are quite unique and can be used to easily identify this new
physics given sufficient integrated luminosity.
|
hep-ph hep-ex hep-th
|
high scale conformal physics can lead to unusual unparticle stuff at our low energies in this paper we discuss how the exchange of unparticles between standard model fields can lead to new contact interaction physics as well as a pseudoresonancelike structure an unresonance that might be observable at the tevatron or lhc in eg the drellyan channel the specific signatures of this scenario are quite unique and can be used to easily identify this new physics given sufficient integrated luminosity
|
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|
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|
706.3026
|
Precise Determination of the I=2 pipi Scattering Length from
Mixed-Action Lattice QCD
|
The I=2 pipi scattering length is calculated in fully-dynamical lattice QCD
with domain-wall valence quarks on the asqtad-improved coarse MILC
configurations (with fourth-rooted staggered sea quarks) at four light-quark
masses. Two- and three-flavor mixed-action chiral perturbation theory at
next-to-leading order is used to perform the chiral and continuum
extrapolations. At the physical charged pion mass, we find m_pi a_pipi(I=2) =
-0.04330 +- 0.00042, where the error bar combines the statistical and
systematic uncertainties in quadrature.
|
hep-lat hep-ph
|
the i2 pipi scattering length is calculated in fullydynamical lattice qcd with domainwall valence quarks on the asqtadimproved coarse milc configurations with fourthrooted staggered sea quarks at four lightquark masses two and threeflavor mixedaction chiral perturbation theory at nexttoleading order is used to perform the chiral and continuum extrapolations at the physical charged pion mass we find m_pi a_pipii2 004330 000042 where the error bar combines the statistical and systematic uncertainties in quadrature
|
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|
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|
706.3027
|
Final state radiation and a possibility to test a pion-photon
interaction model near two-pion threshold
|
Final state radiation in the process $e^+e^-\to\pi^+\pi^-$ is considered for
the cuts used in the analysis of KLOE data at large angles. By means of a Monte
Carlo event generator FEVA, effects of non-pointlike behaviour of pions are
estimated in the framework of Resonance Perturbation Theory. An additional
complication related with the $\phi$ meson intermediate state is taken into
account and the corresponding contributions (the direct decay
$\phi\to\pi^+\pi^-\gamma$ and the double resonance decay
$\phi\to\rho^\pm\pi^\mp\to\pi^+\pi^-\gamma$) are added to FEVA. A method to
test effects of non-pointlike behaviour of pions in a model-independent way is
proposed.
|
hep-ph
|
final state radiation in the process eetopipi is considered for the cuts used in the analysis of kloe data at large angles by means of a monte carlo event generator feva effects of nonpointlike behaviour of pions are estimated in the framework of resonance perturbation theory an additional complication related with the phi meson intermediate state is taken into account and the corresponding contributions the direct decay phitopipigamma and the double resonance decay phitorhopmpimptopipigamma are added to feva a method to test effects of nonpointlike behaviour of pions in a modelindependent way is proposed
|
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|
[-0.07233111259120051, 0.1717968985129523, -0.15969061548821628, 0.1365128900565752, -0.03496476919390261, -0.08690404270568655, 0.017464284193960743, 0.3166929499556621, -0.22531725708653944, -0.29687070098718527, 0.027256857696920635, -0.33030122506121795, -0.024943627862052786, 0.15537663948618705, 0.07497057626023888, 0.09600132523208028, 0.11303419375067783, 0.02660216957123743, -0.03526666424133711, -0.16164088947698474, 0.31587507219778166, 0.07093404121696949, 0.2257345464617376, 0.06793835160012046, 0.08250530942006865, 0.05402077492326498, -0.05674490513176554, -0.012144389122517573, -0.10439544910720239, 0.04839202569694155, 0.1922654652191947, 0.09031282322377794, 0.2103732902246217, -0.3963822030151884, -0.13754823349623216, 0.08652122539157668, 0.15082887005474832, 0.11039668032737811, -0.049477413069042894, -0.34027889617201357, 0.07682558591477573, -0.18638370147802763, -0.13218300995003018, -0.06972422146548828, -0.029038501686106125, -0.054145173511157434, -0.3468036083401077, 0.07946397267902891, 0.0004747711277256409, 0.027253327166868582, -0.03612543332080046, -0.15880541159874864, -0.009001621733316117, 0.11383571402790646, 0.12337103455114024, 0.03497986119344003, 0.1569997866042993, -0.1339274161391788, -0.12452221076625089, 0.35406861992345917, -0.0722566014362706, -0.20013383015369376, 0.1045422408228559, -0.16618083770800796, -0.10736208963725302, 0.22626435636646217, 0.19648476551390356, 0.10825035981348871, -0.1941767525445256, 0.07691368996036342, 0.0448042428224451, 0.14302499898605878, -0.0007931469991389248, 0.027816324409407876, 0.17915230219562847, 0.1836881004454982, -0.040155773479879524, 0.15908200951396592, -0.10488434392544958, -0.1001347317877743, -0.3828039251681831, -0.11551469882122345, -0.12313411311349935, 0.024734101350057044, -0.05513209393959389, -0.11861401248800879, 0.3703052281298571, 0.0937519034732961, 0.22459551575076248, -0.033618696230567166, 0.3190828410287698, 0.12037061598772804, 0.08532781589569317, 0.005979894463800721, 0.2906606050622132, 0.17023264281710404, 0.09003832606184814, -0.2646294843638316, 0.06075022092813419, 0.0357828545384109]
|
706.3028
|
On the discreteness and rationality of F-jumping coefficients
|
This paper studies the jumping coefficients of principal ideals of regular
local rings.
Recently M. Blickle, M. Mustata and K. Smith showed that, when $R$ is of
essentially finite type over a field and $F$-finite, bounded intervals contain
finitely many jumping coefficients and that those are rational. In a later
paper they extended these results to principal ideals of $F$-finite complete
regular local rings. The aim of this paper is to extend these results on the
discreteness and rationality of jumping coefficients to principal ideals of
arbitrary (i.e. not necessarily $F$-finite) excellent regular local rings
containing fields of positive characteristic.
Our proof uses a very different method: we do not use $D$-modules and instead
we analyze the modules of nilpotents elements in the injective hull or $R$
under some non-standard Frobenius actions. This new method undoubtedly holds a
potential for more applications.
|
math.AC math.AG
|
this paper studies the jumping coefficients of principal ideals of regular local rings recently m blickle m mustata and k smith showed that when r is of essentially finite type over a field and ffinite bounded intervals contain finitely many jumping coefficients and that those are rational in a later paper they extended these results to principal ideals of ffinite complete regular local rings the aim of this paper is to extend these results on the discreteness and rationality of jumping coefficients to principal ideals of arbitrary ie not necessarily ffinite excellent regular local rings containing fields of positive characteristic our proof uses a very different method we do not use dmodules and instead we analyze the modules of nilpotents elements in the injective hull or r under some nonstandard frobenius actions this new method undoubtedly holds a potential for more applications
|
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|
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|
706.3029
|
Using integral transforms to estimate higher order derivatives
|
Integral transformations are used to estimate high order derivatives of
various special functions. Applications are given to numerical integration,
where estimates of high order derivatives of the integrand are needed to
achieve bounds on the error. The main idea is to find a suitable integral
representation of the function whose derivatives are to be estimated,
differentiate repeatedly under the integral sign, and estimate the resulting
integral.
|
math.NA math.HO
|
integral transformations are used to estimate high order derivatives of various special functions applications are given to numerical integration where estimates of high order derivatives of the integrand are needed to achieve bounds on the error the main idea is to find a suitable integral representation of the function whose derivatives are to be estimated differentiate repeatedly under the integral sign and estimate the resulting integral
|
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|
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|
706.303
|
A Comparative Study of Optical and Ultraviolet Effective Temperatures
for DA White Dwarfs from the IUE Archive
|
We present a comparative study of effective temperatures determined from the
hydrogen Balmer lines and from the UV energy distribution for 140 DA white
dwarfs drawn from the IUE archive. Our results indicate that the optical and UV
temperatures of the majority of stars below T~40,000 K and within ~75 pc are in
fairly good agreement given the uncertainties. At higher temperatures and/or
larger distances, however, significant discrepancies are observed. Several
mechanisms are investigated to account for these discrepancies including the
effect of interstellar reddening, the presence of metals in the photosphere,
and the existence of unresolved binary white dwarfs. The results of our
analysis reveal that wavelength-dependent extinction is the most natural
explanation for the observed temperature differences. We also attempt to
predict the differences in optical and UV temperatures expected from unresolved
degenerate binaries by performing an exhaustive simulation of composite model
spectra. In light of these simulations, we then discuss some known double
degenerates and identify new binary candidates by restricting our analysis to
stars located within 75 pc where the effect of interstellar reddening is
significantly reduced.
|
astro-ph
|
we present a comparative study of effective temperatures determined from the hydrogen balmer lines and from the uv energy distribution for 140 da white dwarfs drawn from the iue archive our results indicate that the optical and uv temperatures of the majority of stars below t40000 k and within 75 pc are in fairly good agreement given the uncertainties at higher temperatures andor larger distances however significant discrepancies are observed several mechanisms are investigated to account for these discrepancies including the effect of interstellar reddening the presence of metals in the photosphere and the existence of unresolved binary white dwarfs the results of our analysis reveal that wavelengthdependent extinction is the most natural explanation for the observed temperature differences we also attempt to predict the differences in optical and uv temperatures expected from unresolved degenerate binaries by performing an exhaustive simulation of composite model spectra in light of these simulations we then discuss some known double degenerates and identify new binary candidates by restricting our analysis to stars located within 75 pc where the effect of interstellar reddening is significantly reduced
|
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|
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|
706.3031
|
Duality of antidiagonals and pipe dreams
|
Weighted enumeration of reduced pipe dreams (or rc-graphs) results in a
combinatorial expression for Schubert polynomials. The duality between the set
of reduced pipe dreams and certain antidiagonals has important geometric
implications [A. Knutson and E. Miller, Gr\"obner geometry of Schubert
polynomials, Ann. Math. 161, 1245-1318]. The original proof of the duality was
roundabout, relying on the algebra of certain monomial ideals and a recursive
characterization of reduced pipe dreams. This paper provides a direct
combinatorial proof.
|
math.CO
|
weighted enumeration of reduced pipe dreams or rcgraphs results in a combinatorial expression for schubert polynomials the duality between the set of reduced pipe dreams and certain antidiagonals has important geometric implications a knutson and e miller grobner geometry of schubert polynomials ann math 161 12451318 the original proof of the duality was roundabout relying on the algebra of certain monomial ideals and a recursive characterization of reduced pipe dreams this paper provides a direct combinatorial proof
|
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|
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|
706.3032
|
The Solar Radius in the EUV during the Cycle XXIII
|
Aims. To determine the solar transition region and coronal radius at EUV
wavelengths and its time evolution during Solar Cycle XXIII.
Methods. We use daily 30.4 and 17.1 nm images obtained by the Extreme
Ultraviolet Imager (EIT) aboard the SoHO satellite and derive the solar radius
by fitting a circle to the limb brightness ring.
Results. The weighted mean of the temporal series gives (967''.56 +/- 0''.04)
and (969''.54 +/- 0''.02) at 30.4 and 17.1 nm respectively. No significant
correlation was found with the solar cycle at any of the two wavelengths.
Conclusions. Since the temperature formation of the 30.4 nm line is between
(60 - 80) 10^3 K (Transition Region), the obtained result is bigger than that
derived from present atmospheric models. On the contrary this height is
compatible with radio models.
|
astro-ph
|
aims to determine the solar transition region and coronal radius at euv wavelengths and its time evolution during solar cycle xxiii methods we use daily 304 and 171 nm images obtained by the extreme ultraviolet imager eit aboard the soho satellite and derive the solar radius by fitting a circle to the limb brightness ring results the weighted mean of the temporal series gives 96756 004 and 96954 002 at 304 and 171 nm respectively no significant correlation was found with the solar cycle at any of the two wavelengths conclusions since the temperature formation of the 304 nm line is between 60 80 103 k transition region the obtained result is bigger than that derived from present atmospheric models on the contrary this height is compatible with radio models
|
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|
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|
706.3033
|
Effect of antiferromagnetic spin correlations on lattice distortion and
charge ordering in Pr$_{0.5}$Ca$_{1.5}$MnO$_{4}$
|
We use neutron scattering to study the lattice and magnetic structure of the
layered half-doped manganite Pr$_{0.5}$Ca$_{1.5}$MnO$_4$. On cooling from high
temperature, the system first becomes charge- and orbital- ordered (CO/OO) near
$T_{CO}=300$ K and then develops checkerboard-like antiferromagnetic (AF) order
below $T_{N}=130$ K. At temperatures above $T_{N}$ but below $T_{CO}$
($T_N<T<T_{CO}$), the appearance of short-range AF spin correlations suppresses
the CO/OO induced orthorhombic strain, contrasting with other half-doped
manganites, where AF order has no observable effect on the lattice distortion.
These results suggest that a strong spin-lattice coupling and the competition
between AF exchange and CO/OO ordering ultimately determines the
low-temperature properties of the system.
|
cond-mat.str-el
|
we use neutron scattering to study the lattice and magnetic structure of the layered halfdoped manganite pr_05ca_15mno_4 on cooling from high temperature the system first becomes charge and orbital ordered cooo near t_co300 k and then develops checkerboardlike antiferromagnetic af order below t_n130 k at temperatures above t_n but below t_co t_ntt_co the appearance of shortrange af spin correlations suppresses the cooo induced orthorhombic strain contrasting with other halfdoped manganites where af order has no observable effect on the lattice distortion these results suggest that a strong spinlattice coupling and the competition between af exchange and cooo ordering ultimately determines the lowtemperature properties of the system
|
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|
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|
706.3034
|
Enhancement of the dielectron continuum in sqrt{s_NN} = 200 GeV Au+Au
collisions
|
The PHENIX experiment has measured the dielectron continuum in sqrt{s_NN} =
200 GeV Au+Au collisions. In minimum bias collisions the dielectron yield in
the mass range between 150 and 750 MeV/c^2 is enhanced by a factor of 3.4 +/-
0.2(stat.) +/- 1.3(syst.) +/- 0.7(model) compared to the expectation from our
model of hadron decays. The integrated yield increases faster with the
centrality of the collisions than the number of participating nucleons,
suggesting emission from scattering processes in the hot and dense medium. The
continuum yield between the masses of the phi and the J/psi mesons is
consistent with expectations from correlated c-cbar production, though other
mechanisms are not ruled out.
|
nucl-ex
|
the phenix experiment has measured the dielectron continuum in sqrts_nn 200 gev auau collisions in minimum bias collisions the dielectron yield in the mass range between 150 and 750 mevc2 is enhanced by a factor of 34 02stat 13syst 07model compared to the expectation from our model of hadron decays the integrated yield increases faster with the centrality of the collisions than the number of participating nucleons suggesting emission from scattering processes in the hot and dense medium the continuum yield between the masses of the phi and the jpsi mesons is consistent with expectations from correlated ccbar production though other mechanisms are not ruled out
|
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|
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|
706.3035
|
Massive Clumps in the NGC 6334 Star Forming Region
|
We report observations of dust continuum emission at 1.2 mm toward the star
forming region NGC 6334 made with the SEST SIMBA bolometer array. The
observations cover an area of $\sim 2$ square degrees with approximately
uniform noise. We detected 181 clumps spanning almost three orders of magnitude
in mass (3\Msun$-6\times10^3$ \Msun) and with sizes in the range 0.1--1.0 pc.
We find that the clump mass function $dN/d\log M$ is well fit with a power law
of the mass with exponent -0.6 (or equivalently $dN/dM \propto M^{-1.6}$). The
derived exponent is similar to those obtained from molecular line emission
surveys and is significantly different from that of the stellar initial mass
function. We investigated changes in the mass spectrum by changing the
assumptions on the temperature distribution of the clumps and on the
contribution of free-free emission to the 1.2 mm emission, and found little
changes on the exponent. The Cumulative Mass Distribution Function is also
analyzed giving consistent results in a mass range excluding the high-mass end
where a power-law fit is no longer valid. The masses and sizes of the clumps
observed in NGC 6334 indicate that they are not direct progenitors of stars and
that the process of fragmentation determines the distribution of masses later
on or occurs at smaller spatial scales. The spatial distribution of the clumps
in NGC 6334 reveals clustering which is strikingly similar to that exhibited by
young stars in other star forming regions. A power law fit to the surface
density of companions gives $\Sigma\propto \theta^{-0.62}$.
|
astro-ph
|
we report observations of dust continuum emission at 12 mm toward the star forming region ngc 6334 made with the sest simba bolometer array the observations cover an area of sim 2 square degrees with approximately uniform noise we detected 181 clumps spanning almost three orders of magnitude in mass 3msun6times103 msun and with sizes in the range 0110 pc we find that the clump mass function dndlog m is well fit with a power law of the mass with exponent 06 or equivalently dndm propto m16 the derived exponent is similar to those obtained from molecular line emission surveys and is significantly different from that of the stellar initial mass function we investigated changes in the mass spectrum by changing the assumptions on the temperature distribution of the clumps and on the contribution of freefree emission to the 12 mm emission and found little changes on the exponent the cumulative mass distribution function is also analyzed giving consistent results in a mass range excluding the highmass end where a powerlaw fit is no longer valid the masses and sizes of the clumps observed in ngc 6334 indicate that they are not direct progenitors of stars and that the process of fragmentation determines the distribution of masses later on or occurs at smaller spatial scales the spatial distribution of the clumps in ngc 6334 reveals clustering which is strikingly similar to that exhibited by young stars in other star forming regions a power law fit to the surface density of companions gives sigmapropto theta062
|
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|
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|
706.3036
|
The Hubbard model: bosonic excitations and zero-frequency constants
|
A fully self-consistent calculation of the bosonic dynamics of the Hubbard
model is developed within the Composite Operator Method. From one side we
consider a basic set of fermionic composite operators (Hubbard fields) and
calculate the retarded propagators. On the other side we consider a basic set
of bosonic composite operators (charge, spin and pair) and calculate the causal
propagators. The equations for the Green's functions (GF) (retarded and
causal), studied in the polar approximation, are coupled and depend on a set of
parameters not determined by the dynamics. First, the pair sector is
self-consistently solved together with the fermionic one and the zero-frequency
constants (ZFC) are calculated not assuming the ergodic value, but fixing the
representation of the GF in such a way to maintain the constrains required by
the algebra of the composite fields. Then, the scheme to compute the charge and
spin sectors, ZFCs included, is given in terms of the fermionic and pair
correlators.
|
cond-mat.str-el cond-mat.supr-con
|
a fully selfconsistent calculation of the bosonic dynamics of the hubbard model is developed within the composite operator method from one side we consider a basic set of fermionic composite operators hubbard fields and calculate the retarded propagators on the other side we consider a basic set of bosonic composite operators charge spin and pair and calculate the causal propagators the equations for the greens functions gf retarded and causal studied in the polar approximation are coupled and depend on a set of parameters not determined by the dynamics first the pair sector is selfconsistently solved together with the fermionic one and the zerofrequency constants zfc are calculated not assuming the ergodic value but fixing the representation of the gf in such a way to maintain the constrains required by the algebra of the composite fields then the scheme to compute the charge and spin sectors zfcs included is given in terms of the fermionic and pair correlators
|
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|
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|
706.3037
|
Implicit function density computation
|
If two random variables X and A are functionally related via f(X)=A for some
strictly monotone continuously differentiable function f:R->R, the distribution
of X may easily be computed from the distribution of A.
|
math.GM
|
if two random variables x and a are functionally related via fxa for some strictly monotone continuously differentiable function frr the distribution of x may easily be computed from the distribution of a
|
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|
[-0.09193171340633523, 0.18317026117195687, -0.12387902141464027, 0.06737658268574512, -0.025181980225060022, -0.1781028312433398, 0.026691836389628323, 0.4021262637141979, -0.36900421435182745, -0.18361672222840064, 0.13996239675378258, -0.2685443161824492, -0.1438734701862841, 0.22997074035193885, -0.05094824866815047, 0.045950876492442505, -0.0067716388483390665, 0.06279221656873371, -0.11601921141316945, -0.26331935083550034, 0.3306131378719301, -0.11243200192058628, 0.18942969165403734, -0.004792711499965552, 0.11645675789226186, 0.01681403987899874, -0.005473912524228746, 0.09595196965065869, -0.06946440354328264, 0.1090325044016495, 0.22887876415342995, 0.17434622491992108, 0.2925222010605715, -0.32777017050168733, -0.2087051695438497, 0.17777247074991465, 0.11680073927467068, -0.062200878662141884, 0.0068455029448324985, -0.26297455179420387, 0.09115655807721795, -0.12631968722086062, -0.11417947043523644, -0.06943674467391137, 0.03330825483708671, 0.15287575591355562, -0.35158272251261, 0.04643379051633405, 0.036042406731708485, -0.017631481316956608, -0.01737272639222669, -0.14819200729217494, -0.1145407199069406, 0.0707323017360812, 0.038850164379585876, 0.16740958485752344, 0.14929337950536248, -0.06205074051677278, -0.03294355190838828, 0.2847578642946301, -0.04488035240633921, -0.3436198149327979, 0.14131851164116102, -0.1788568405829596, -0.11832834653217685, 0.17344342225767445, 0.11654071492904966, 0.1823095999883883, -0.21997443120926619, 0.1016151561863918, -0.05092709037390622, 0.17561664043530595, 0.04219362152401696, 0.010647562558226513, 0.20245564350801887, 0.04098524570916638, 0.10843937731150424, 0.12799814958337016, -0.018859101007833626, -0.058126375756480476, -0.3545851549415877, -0.1425870345679648, -0.21402181964367628, 0.10960875028236346, -0.12548166090070453, -0.18818700917516695, 0.3666934185858929, 0.066644251590002, 0.2422553894081802, 0.1263958504987937, 0.19425936246460135, 0.15544412872104935, 0.03042789057574489, 0.06953068898821418, 0.11088206070549363, 0.11755094152988133, 0.010785461671537521, -0.0768271846287517, 0.16810441192126635, 0.05187565012072975]
|
706.3038
|
Separability of a family of one parameter W and GHZ multiqubit states
using Abe-Rajagopal q-conditional entropy approach
|
We employ conditional Tsallis q entropies to study the separability of
symmetric one parameter W and GHZ multiqubit mixed states. The strongest
limitation on separability is realized in the limit q-->infinity, and is found
to be much superior to the condition obtained using the von Neumann conditional
entropy (q=1 case). Except for the example of two qubit and three qubit
symmetric states of GHZ family, the $q$-conditional entropy method leads to
sufficient - but not necessary - conditions on separability.
|
quant-ph
|
we employ conditional tsallis q entropies to study the separability of symmetric one parameter w and ghz multiqubit mixed states the strongest limitation on separability is realized in the limit qinfinity and is found to be much superior to the condition obtained using the von neumann conditional entropy q1 case except for the example of two qubit and three qubit symmetric states of ghz family the qconditional entropy method leads to sufficient but not necessary conditions on separability
|
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|
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|
706.3039
|
The spectral density function of a toric variety
|
For a Kahler manifold (X, \omega) with a holomorphic line bundle L and metric
h such that the Chern form of L is \omega, the spectral measures are the
measures \mu_N = \sum |s_{N,i}|^2 \nu, where \{s_{N,i}\}_i is an
L^2-orthonormal basis for H^0(X, L^{\otimes N}), and \nu is Liouville measure.
We study the asymptotics in N of \mu_N for (X, L) a Hamiltonian toric manifold,
and give a precise expansion in terms of powers 1/N^j and data on the moment
polytope \Delta of the Hamiltonian torus K acting on X. In addition, for an
infinitesimal character k of K and the unique unit eigensection s_{Nk} for the
character Nk of the torus action on H^0(X, L^N), we give a similar expansion
for the measures \mu_{Nk} = |s_{Nk}|^2 \nu. A final remark shows that the
eigenbasis \{s_{k}, k \in \Delta \cap \mathbb{Z}^{\dim K} \} is a
Bohr-Sommerfeld basis in the sense of Tyurin. Some of the present results are
related to work of Shiffman, Tate and Zelditch. The present paper uses no
microlocal analysis, but rather an Euler-Maclaurin formula for Delzant
polytopes.
|
math.SP math-ph math.MP
|
for a kahler manifold x omega with a holomorphic line bundle l and metric h such that the chern form of l is omega the spectral measures are the measures mu_n sum s_ni2 nu where s_ni_i is an l2orthonormal basis for h0x lotimes n and nu is liouville measure we study the asymptotics in n of mu_n for x l a hamiltonian toric manifold and give a precise expansion in terms of powers 1nj and data on the moment polytope delta of the hamiltonian torus k acting on x in addition for an infinitesimal character k of k and the unique unit eigensection s_nk for the character nk of the torus action on h0x ln we give a similar expansion for the measures mu_nk s_nk2 nu a final remark shows that the eigenbasis s_k k in delta cap mathbbzdim k is a bohrsommerfeld basis in the sense of tyurin some of the present results are related to work of shiffman tate and zelditch the present paper uses no microlocal analysis but rather an eulermaclaurin formula for delzant polytopes
|
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|
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|
706.304
|
Experimental observation of strong photon localization in disordered
photonic crystal waveguides
|
We demonstrate experimentally that structural perturbations imposed on
highly-dispersive photonic crystal-based waveguides give rise to spectral
features that bear signatures of Anderson localization. Sharp resonances with
the effective Qs of over 30,000 are found in scattering spectra of disordered
waveguides. The resonances are observed in a ~20-nm bandwidth centered at the
cutoff of slowly-guided Bloch-modes. Their origin can be explained with
interference of coherently scattered electromagnetic waves which results in the
formation of a narrow impurity (or localization) band populated with spectrally
distinct quasistates. Standard photon localization criteria are fulfilled in
the localization band.
|
physics.optics physics.gen-ph
|
we demonstrate experimentally that structural perturbations imposed on highlydispersive photonic crystalbased waveguides give rise to spectral features that bear signatures of anderson localization sharp resonances with the effective qs of over 30000 are found in scattering spectra of disordered waveguides the resonances are observed in a 20nm bandwidth centered at the cutoff of slowlyguided blochmodes their origin can be explained with interference of coherently scattered electromagnetic waves which results in the formation of a narrow impurity or localization band populated with spectrally distinct quasistates standard photon localization criteria are fulfilled in the localization band
|
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|
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|
706.3041
|
Population synthesis of radio and gamma-ray millisecond pulsars from the
Galactic disk
|
We present results of a population synthesis of millisecond pulsars from the
Galactic disk. Excluding globular clusters, we model the spatial distribution
of millisecond pulsars by assuming their birth in the Galactic disk with a
random kick velocity and evolve them to the present within the Galactic
potential. We assume that normal and millisecond pulsars are standard candles
described with a common radio luminosity model that invokes a new relationship
between radio core and cone emission suggested by recent studies. In modeling
the radio emission beams, we explore the relativistic effects of time delay,
aberration and sweepback of the open field lines. While these effects are
essential in understanding pulse profiles, the phase-averaged flux is
adequately described without a relativistic model. We use a polar cap
acceleration model for the gamma-ray emission. We present the preliminary
results of our recent study and the implications for observing millisecond
pulsars with GLAST and AGILE.
|
astro-ph
|
we present results of a population synthesis of millisecond pulsars from the galactic disk excluding globular clusters we model the spatial distribution of millisecond pulsars by assuming their birth in the galactic disk with a random kick velocity and evolve them to the present within the galactic potential we assume that normal and millisecond pulsars are standard candles described with a common radio luminosity model that invokes a new relationship between radio core and cone emission suggested by recent studies in modeling the radio emission beams we explore the relativistic effects of time delay aberration and sweepback of the open field lines while these effects are essential in understanding pulse profiles the phaseaveraged flux is adequately described without a relativistic model we use a polar cap acceleration model for the gammaray emission we present the preliminary results of our recent study and the implications for observing millisecond pulsars with glast and agile
|
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|
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|
706.3042
|
Turbulent transport of material particles: An experimental study of
finite size effects
|
We use an acoustic Lagrangian tracking technique, particularly adapted to
measurements in open flows, and a versatile material particles generator (in
the form of soap bubbles with adjustable size and density) to characterize
Lagrangian statistics of finite sized, neutrally bouyant, particles transported
in an isotropic turbulent flow of air. We vary the size of the particles in a
range corresponding to turbulent inertial scales and explore how the turbulent
forcing experienced by the particles depends on their size. We show that, while
the global shape of the intermittent acceleration probability density function
does not depend significantly on particle size, the acceleration variance of
the particles decreases as they become larger in agreement with the classical
scaling for the spectrum of Eulerian pressure fluctuations in the carrier flow.
|
physics.flu-dyn
|
we use an acoustic lagrangian tracking technique particularly adapted to measurements in open flows and a versatile material particles generator in the form of soap bubbles with adjustable size and density to characterize lagrangian statistics of finite sized neutrally bouyant particles transported in an isotropic turbulent flow of air we vary the size of the particles in a range corresponding to turbulent inertial scales and explore how the turbulent forcing experienced by the particles depends on their size we show that while the global shape of the intermittent acceleration probability density function does not depend significantly on particle size the acceleration variance of the particles decreases as they become larger in agreement with the classical scaling for the spectrum of eulerian pressure fluctuations in the carrier flow
|
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|
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|
706.3043
|
Carbon and Strontium Abundances of Metal-Poor Stars
|
We present carbon and strontium abundances for 100 metal-poor stars measured
from R$\sim $7000 spectra obtained with the Echellette Spectrograph and Imager
at the Keck Observatory. Using spectral synthesis of the G-band region, we have
derived carbon abundances for stars ranging from [Fe/H]$=-1.3$ to
[Fe/H]$=-3.8$. The formal errors are $\sim 0.2$ dex in [C/Fe]. The strontium
abundance in these stars was measured using spectral synthesis of the resonance
line at 4215 {\AA}. Using these two abundance measurments along with the barium
abundances from our previous study of these stars, we show it is possible to
identify neutron-capture-rich stars with our spectra. We find, as in other
studies, a large scatter in [C/Fe] below [Fe/H]$ = -2$. Of the stars with
[Fe/H]$<-2$, 9$\pm$4% can be classified as carbon-rich metal-poor stars. The Sr
and Ba abundances show that three of the carbon-rich stars are
neutron-capture-rich, while two have normal Ba and Sr. This fraction of carbon
enhanced stars is consistent with other studies that include this metallicity
range.
|
astro-ph
|
we present carbon and strontium abundances for 100 metalpoor stars measured from rsim 7000 spectra obtained with the echellette spectrograph and imager at the keck observatory using spectral synthesis of the gband region we have derived carbon abundances for stars ranging from feh13 to feh38 the formal errors are sim 02 dex in cfe the strontium abundance in these stars was measured using spectral synthesis of the resonance line at 4215 aa using these two abundance measurments along with the barium abundances from our previous study of these stars we show it is possible to identify neutroncapturerich stars with our spectra we find as in other studies a large scatter in cfe below feh 2 of the stars with feh2 9pm4 can be classified as carbonrich metalpoor stars the sr and ba abundances show that three of the carbonrich stars are neutroncapturerich while two have normal ba and sr this fraction of carbon enhanced stars is consistent with other studies that include this metallicity range
|
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|
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|
706.3044
|
On McQuillan's "tautological inequality" and the Weyl-Ahlfors theory of
associated curves
|
In 1941, L. Ahlfors gave another proof of a 1933 theorem of H. Cartan on
approximation to hyperplanes of holomorphic curves in P^n. Ahlfors' proof built
on earlier work of H. and J. Weyl (1938), and proved Cartan's theorem by
studying the associated curves of the holomorphic curve. This work has
subsequently been reworked by H.-H. Wu in 1970, using differential geometry, M.
Cowen and P. A. Griffiths in 1976, further emphasizing curvature, and by Y.-T.
Siu in 1987 and 1990, emphasizing meromorphic connections. This paper gives
another variation of the proof, motivated by successive minima as in the proof
of Schmidt's Subspace Theorem, and using McQuillan's "tautological inequality."
In this proof, essentially all of the analysis is encapsulated within a
modified McQuillan-like inequality, so that most of the proof primarily uses
methods of algebraic geometry, in particular flag varieties. A diophantine
conjecture based on McQuillan's inequality is also posed.
|
math.CV math.AG
|
in 1941 l ahlfors gave another proof of a 1933 theorem of h cartan on approximation to hyperplanes of holomorphic curves in pn ahlfors proof built on earlier work of h and j weyl 1938 and proved cartans theorem by studying the associated curves of the holomorphic curve this work has subsequently been reworked by hh wu in 1970 using differential geometry m cowen and p a griffiths in 1976 further emphasizing curvature and by yt siu in 1987 and 1990 emphasizing meromorphic connections this paper gives another variation of the proof motivated by successive minima as in the proof of schmidts subspace theorem and using mcquillans tautological inequality in this proof essentially all of the analysis is encapsulated within a modified mcquillanlike inequality so that most of the proof primarily uses methods of algebraic geometry in particular flag varieties a diophantine conjecture based on mcquillans inequality is also posed
|
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|
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|
706.3045
|
The Future is Now: the Formation of Single Low Mass White Dwarfs in the
Solar Neighborhood
|
Low mass helium-core white dwarfs (M < 0.45 Msun) can be produced from
interacting binary systems, and traditionally all of them have been attributed
to this channel. However, a low mass white dwarf could also result from a
single star that experiences severe mass loss on the first ascent giant branch.
A large population of low mass He-core white dwarfs has been discovered in the
old metal-rich cluster NGC 6791. There is therefore a mechanism in clusters to
produce low mass white dwarfs without requiring binary star interactions, and
we search for evidence of a similar population in field white dwarfs. We argue
that there is a significant field population (of order half of the detected
systems) that arises from old metal rich stars which truncate their evolution
prior to the helium flash from severe mass loss. There is a consistent absence
of evidence for nearby companions in a large fraction of low mass white dwarfs.
The number of old metal-rich field dwarfs is also comparable with the
apparently single low mass white dwarf population, and our revised estimate for
the space density of low mass white dwarfs produced from binary interactions is
also compatible with theoretical expectations. This indicates that this channel
of stellar evolution, hitherto thought hypothetical only, has been in operation
in our own Galaxy for many billions of years. One strong implication of our
model is that single low mass white dwarfs should be good targets for planet
searches because they are likely to arise from metal-rich progenitors. We also
discuss other observational tests and implications, including the potential
impact on SN Ia rates and the frequency of planetary nebulae.
|
astro-ph
|
low mass heliumcore white dwarfs m 045 msun can be produced from interacting binary systems and traditionally all of them have been attributed to this channel however a low mass white dwarf could also result from a single star that experiences severe mass loss on the first ascent giant branch a large population of low mass hecore white dwarfs has been discovered in the old metalrich cluster ngc 6791 there is therefore a mechanism in clusters to produce low mass white dwarfs without requiring binary star interactions and we search for evidence of a similar population in field white dwarfs we argue that there is a significant field population of order half of the detected systems that arises from old metal rich stars which truncate their evolution prior to the helium flash from severe mass loss there is a consistent absence of evidence for nearby companions in a large fraction of low mass white dwarfs the number of old metalrich field dwarfs is also comparable with the apparently single low mass white dwarf population and our revised estimate for the space density of low mass white dwarfs produced from binary interactions is also compatible with theoretical expectations this indicates that this channel of stellar evolution hitherto thought hypothetical only has been in operation in our own galaxy for many billions of years one strong implication of our model is that single low mass white dwarfs should be good targets for planet searches because they are likely to arise from metalrich progenitors we also discuss other observational tests and implications including the potential impact on sn ia rates and the frequency of planetary nebulae
|
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|
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|
706.3046
|
Seismic study of the chemical composition of the solar convection zone
|
Recent downward revision of solar heavy-element abundances using
three-dimensional atmospheric model has introduced serious discrepancies
between standard solar models and helioseismic inferences about solar
structure. In this paper, we investigate the possibility of determining the
heavy-element abundances using helioseismic inversion techniques with the hope
of providing an independent estimate. We use the adiabatic index, Gamma_1
(logarithmic partial derivative of pressure with respect to density at constant
entropy) as a probe to examine the effects of the total heavy-element
abundance, as well as the effects due to the abundance of individual elements.
Our inversion results show that the new, lower, abundance increases the
discrepancy between the Sun and the solar models.
|
astro-ph
|
recent downward revision of solar heavyelement abundances using threedimensional atmospheric model has introduced serious discrepancies between standard solar models and helioseismic inferences about solar structure in this paper we investigate the possibility of determining the heavyelement abundances using helioseismic inversion techniques with the hope of providing an independent estimate we use the adiabatic index gamma_1 logarithmic partial derivative of pressure with respect to density at constant entropy as a probe to examine the effects of the total heavyelement abundance as well as the effects due to the abundance of individual elements our inversion results show that the new lower abundance increases the discrepancy between the sun and the solar models
|
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|
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|
706.3047
|
The Radio Properties of Type Ibc Supernovae
|
Over the past few years, long-duration gamma-ray bursts (GRBs), including the
subclass of X-ray flashes (XRFs), have been revealed to be a rare variety of
Type Ibc supernova (SN Ibc). While all these events result from the death of
massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those
of ordinary Type Ibc SNe by many orders of magnitude. The observed diversity of
stellar death corresponds to large variations in the energy, velocity, and
geometry of the explosion ejecta. Using multi-wavelength (radio, optical,
X-ray) observations of the nearest GRBs, XRFs, and SNe Ibc, I show that while
GRBs and XRFs couple at least 10^48 erg to relativistic material, SNe Ibc
typically couple less than 10^48 erg to their fastest (albeit non-relativistic)
outflows. Specifically, I find that less than 3% of local SNe Ibc show any
evidence for association with a GRB or XRF. Recently, a new class of GRBs and
XRFs has been revealed which are under-luminous in comparison with the
statistical sample of GRBs. Owing to their faint high-energy emission, these
sub-energetic bursts are only detectable nearby (z < 0.1) and are likely 10
times more common than cosmological GRBs. In comparison with local SNe Ibc and
typical GRBs/XRFs, these explosions are intermediate in terms of both
volumetric rate and energetics. Yet the essential physical process that causes
a dying star to produce a GRB, XRF, or sub-energetic burst, and not just a SN,
remains a crucial open question. Progress requires a detailed understanding of
ordinary SNe Ibc which will be facilitated with the launch of wide-field
optical surveys in the near future.
|
astro-ph
|
over the past few years longduration gammaray bursts grbs including the subclass of xray flashes xrfs have been revealed to be a rare variety of type ibc supernova sn ibc while all these events result from the death of massive stars the electromagnetic luminosities of grbs and xrfs exceed those of ordinary type ibc sne by many orders of magnitude the observed diversity of stellar death corresponds to large variations in the energy velocity and geometry of the explosion ejecta using multiwavelength radio optical xray observations of the nearest grbs xrfs and sne ibc i show that while grbs and xrfs couple at least 1048 erg to relativistic material sne ibc typically couple less than 1048 erg to their fastest albeit nonrelativistic outflows specifically i find that less than 3 of local sne ibc show any evidence for association with a grb or xrf recently a new class of grbs and xrfs has been revealed which are underluminous in comparison with the statistical sample of grbs owing to their faint highenergy emission these subenergetic bursts are only detectable nearby z 01 and are likely 10 times more common than cosmological grbs in comparison with local sne ibc and typical grbsxrfs these explosions are intermediate in terms of both volumetric rate and energetics yet the essential physical process that causes a dying star to produce a grb xrf or subenergetic burst and not just a sn remains a crucial open question progress requires a detailed understanding of ordinary sne ibc which will be facilitated with the launch of widefield optical surveys in the near future
|
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|
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|
706.3048
|
A Dark Core in Abell 520
|
The rich cluster Abell 520 (z=0.201) exhibits truly extreme and puzzling
multi-wavelength characteristics. It may best be described as a "cosmic train
wreck." It is a major merger showing abundant evidence for ram pressure
stripping, with a clear offset in the gas distribution compared to the galaxies
(as in the bullet cluster 1E 0657-558). However, the most striking feature is a
massive dark core (721 h_70 M_sun/L_sun) in our weak lensing mass
reconstruction. The core coincides with the central X-ray emission peak, but is
largely devoid of galaxies. An unusually low mass to light ratio region lies
500 kpc to the east, and coincides with a shock feature visible in radio
observations of the cluster. Although a displacement between the X-ray gas and
the galaxy/dark matter distributions may be expected in a merger, a mass peak
without galaxies cannot be easily explained within the current collisionless
dark matter paradigm. Interestingly, the integrated gas mass fraction (~0.15),
mass-to-light ratio (220 h_70 M_sun/L_sun), and position on the X-ray
luminosity-temperature and mass-temperature relations are unremarkable. Thus
gross properties and scaling relations are not always useful indicators of the
dynamical state of clusters.
|
astro-ph
|
the rich cluster abell 520 z0201 exhibits truly extreme and puzzling multiwavelength characteristics it may best be described as a cosmic train wreck it is a major merger showing abundant evidence for ram pressure stripping with a clear offset in the gas distribution compared to the galaxies as in the bullet cluster 1e 0657558 however the most striking feature is a massive dark core 721 h_70 m_sunl_sun in our weak lensing mass reconstruction the core coincides with the central xray emission peak but is largely devoid of galaxies an unusually low mass to light ratio region lies 500 kpc to the east and coincides with a shock feature visible in radio observations of the cluster although a displacement between the xray gas and the galaxydark matter distributions may be expected in a merger a mass peak without galaxies cannot be easily explained within the current collisionless dark matter paradigm interestingly the integrated gas mass fraction 015 masstolight ratio 220 h_70 m_sunl_sun and position on the xray luminositytemperature and masstemperature relations are unremarkable thus gross properties and scaling relations are not always useful indicators of the dynamical state of clusters
|
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|
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|
706.3049
|
Beyond Twisted Tori
|
Exploiting the fact that Kaluza-Klein monopoles and the associated
generalized orbifold planes are sources for geometrical fluxes, omega, we show
that the standard constraint omega.omega=0, valid for superstring
compactifications on twisted tori, can be consistently relaxed. This leads to
novel possibilities for constructing superstring models with fluxes and
localized sources, as well as for stabilizing moduli. This also explains the
ten-dimensional origin of a family of N=4 gauged supergravities, whose
interpretation in type-IIA orientifold compactifications was lacking.
|
hep-th
|
exploiting the fact that kaluzaklein monopoles and the associated generalized orbifold planes are sources for geometrical fluxes omega we show that the standard constraint omegaomega0 valid for superstring compactifications on twisted tori can be consistently relaxed this leads to novel possibilities for constructing superstring models with fluxes and localized sources as well as for stabilizing moduli this also explains the tendimensional origin of a family of n4 gauged supergravities whose interpretation in typeiia orientifold compactifications was lacking
|
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|
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|
706.305
|
Dark matter from "strong gravity" - consistent with CRESST, CoGeNT and
DAMA/LIBRA
|
Kelso, Hooper and Buckley [arXiv:1110.5338] found CRESST, CoGeNT and
DAMA/LIBRA results are consistent with 10 - 15 GeV dark matter particles.
Hennawi and Ostriker [arXiv:astro-ph/0108203] analyzed supermassive black hole
formation in the centers of galaxies, finding a best fit for dark matter
(self-interaction cross-section)/mass ratio = 0.02 cm^{2}/g, with round-off
error of 25%. Combining the Hennawi/Ostriker result with the "strong gravity"
model for dark matter [arXiv:0706.3050] requires dark matter particles with
mass between 10.5 GeV and 17.5 GeV, overlapping the Kelso/Hooper/Buckley dark
matter particle mass range.
|
gr-qc astro-ph hep-th
|
kelso hooper and buckley arxiv11105338 found cresst cogent and damalibra results are consistent with 10 15 gev dark matter particles hennawi and ostriker arxivastroph0108203 analyzed supermassive black hole formation in the centers of galaxies finding a best fit for dark matter selfinteraction crosssectionmass ratio 002 cm2g with roundoff error of 25 combining the hennawiostriker result with the strong gravity model for dark matter arxiv07063050 requires dark matter particles with mass between 105 gev and 175 gev overlapping the kelsohooperbuckley dark matter particle mass range
|
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|
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|
706.3051
|
Molecular Dipolar Crystals as High Fidelity Quantum Memory for Hybrid
Quantum Computing
|
We study collective excitations of rotational and spin states of an ensemble
of polar molecules, which are prepared in a dipolar crystalline phase, as a
candidate for a high fidelity quantum memory. While dipolar crystals are formed
in the high density limit of cold clouds of polar molecules under 1D and 2D
trapping conditions, the crystalline structure protects the molecular qubits
from detrimental effects of short range collisions. We calculate the lifetime
of the quantum memory by identifying the dominant decoherence mechanisms, and
estimate their effects on gate operations, when a molecular ensemble qubit is
transferred to a superconducting strip line cavity (circuit QED). In the case
rotational excitations coupled by dipole-dipole interactions we identify
phonons as the main limitation of the life time of qubits. We study specific
setups and conditions, where the coupling to the phonon modes is minimized.
Detailed results are presented for a 1D dipolar chain.
|
quant-ph cond-mat.other
|
we study collective excitations of rotational and spin states of an ensemble of polar molecules which are prepared in a dipolar crystalline phase as a candidate for a high fidelity quantum memory while dipolar crystals are formed in the high density limit of cold clouds of polar molecules under 1d and 2d trapping conditions the crystalline structure protects the molecular qubits from detrimental effects of short range collisions we calculate the lifetime of the quantum memory by identifying the dominant decoherence mechanisms and estimate their effects on gate operations when a molecular ensemble qubit is transferred to a superconducting strip line cavity circuit qed in the case rotational excitations coupled by dipoledipole interactions we identify phonons as the main limitation of the life time of qubits we study specific setups and conditions where the coupling to the phonon modes is minimized detailed results are presented for a 1d dipolar chain
|
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|
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|
706.3052
|
Two Classes of Hot Jupiters
|
We identify two classes of transiting planet, based on their equilibrium
temperatures and Safronov numbers. We examine various possible explanations for
the dichotomy. It may reflect the influence of planet or planetesimal
scattering in determining when planetary migration stops. Another possibility
is that some planets lose more mass to evaporation than others. If this
evaporation process preferentially removes Helium from the planet, the
consequent reduction in the mean molecular weight may explain why some planets
have anomalously large radii.
|
astro-ph
|
we identify two classes of transiting planet based on their equilibrium temperatures and safronov numbers we examine various possible explanations for the dichotomy it may reflect the influence of planet or planetesimal scattering in determining when planetary migration stops another possibility is that some planets lose more mass to evaporation than others if this evaporation process preferentially removes helium from the planet the consequent reduction in the mean molecular weight may explain why some planets have anomalously large radii
|
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|
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|
706.3053
|
A Survey of Intrinsic Absorption in Active Galaxies using the Far
Ultraviolet Spectroscopic Explorer
|
We present a survey of 72 Seyfert galaxies and quasars observed by the it Far
Ultraviolet Spectroscopic Explorer (FUSE). We have determined that 72 of 253
available active galactic nuclei (AGN) targets are viable targets for detection
of intrinsic absorption lines. We examined these spectra for signs of intrinsic
absorption in the O VI doublet (lambda 1031.9, 1037.6) and Lyman beta (lambda
1025.7). The fraction of Seyfert 1 galaxies and low-redshift quasars at z <
0.15 that show evidence of intrinsic UV absorption is ~50%, which is slightly
lower than Crenshaw et al. (1999) found (60%) based on a smaller sample of
Seyfert 1 galaxies observed with the Hubble Space Telescope (HST). With this
new fraction we find a global covering factor of the absorbing gas with respect
to the central nucleus of ~0.4. Our survey is to date the largest searching for
intrinsic UV absorption with high spectral resolution, and is the first step
toward a more comprehensive study of intrinsic absorption in low-redshift AGN.
|
astro-ph
|
we present a survey of 72 seyfert galaxies and quasars observed by the it far ultraviolet spectroscopic explorer fuse we have determined that 72 of 253 available active galactic nuclei agn targets are viable targets for detection of intrinsic absorption lines we examined these spectra for signs of intrinsic absorption in the o vi doublet lambda 10319 10376 and lyman beta lambda 10257 the fraction of seyfert 1 galaxies and lowredshift quasars at z 015 that show evidence of intrinsic uv absorption is 50 which is slightly lower than crenshaw et al 1999 found 60 based on a smaller sample of seyfert 1 galaxies observed with the hubble space telescope hst with this new fraction we find a global covering factor of the absorbing gas with respect to the central nucleus of 04 our survey is to date the largest searching for intrinsic uv absorption with high spectral resolution and is the first step toward a more comprehensive study of intrinsic absorption in lowredshift agn
|
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|
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|
706.3054
|
The perfect lens on a finite bandwidth
|
The resolution associated with the so-called perfect lens of thickness $d$ is
$-2\pi d/\ln(|\chi+2|/2)$. Here the susceptibility $\chi$ is a Hermitian
function in $H^2$ of the upper half-plane, i.e., a $H^2$ function satisfying
$\chi(-\omega)=\bar{\chi(\omega)}$. An additional requirement is that the
imaginary part of $\chi$ be nonnegative for nonnegative arguments. Given an
interval $I$ on the positive half-axis, we compute the distance in
$L^\infty(I)$ from a negative constant to this class of functions. This result
gives a surprisingly simple and explicit formula for the optimal resolution of
the perfect lens on a finite bandwidth.
|
physics.optics
|
the resolution associated with the socalled perfect lens of thickness d is 2pi dlnchi22 here the susceptibility chi is a hermitian function in h2 of the upper halfplane ie a h2 function satisfying chiomegabarchiomega an additional requirement is that the imaginary part of chi be nonnegative for nonnegative arguments given an interval i on the positive halfaxis we compute the distance in linftyi from a negative constant to this class of functions this result gives a surprisingly simple and explicit formula for the optimal resolution of the perfect lens on a finite bandwidth
|
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|
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|
706.3055
|
A primer on the (2+1) Einstein universe
|
The Einstein universe is the conformal compactification of Minkowski space.
It also arises as the ideal boundary of anti-de Sitter space. The purpose of
this article is to develop the synthetic geometry of the Einstein universe in
terms of its homogeneous submanifolds and causal structure, with particular
emphasis on dimension $2 + 1$, in which there is a rich interplay with
symplectic geometry.
|
math.DG
|
the einstein universe is the conformal compactification of minkowski space it also arises as the ideal boundary of antide sitter space the purpose of this article is to develop the synthetic geometry of the einstein universe in terms of its homogeneous submanifolds and causal structure with particular emphasis on dimension 2 1 in which there is a rich interplay with symplectic geometry
|
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|
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|
706.3056
|
Neutrino-driven explosions twenty years after SN1987A
|
The neutrino-heating mechanism remains a viable possibility for the cause of
the explosion in a wide mass range of supernova progenitors. This is
demonstrated by recent two-dimensional hydrodynamic simulations with detailed,
energy-dependent neutrino transport. Neutrino-driven explosions were not only
found for stars in the range of 8-10 solar masses with ONeMg cores and in case
of the iron core collapse of a progenitor with 11 solar masses, but also for a
``typical'' progenitor model of 15 solar masses. For such more massive stars,
however, the explosion occurs significantly later than so far thought, and is
crucially supported by large-amplitude bipolar oscillations due to the
nonradial standing accretion shock instability (SASI), whose low (dipole and
quadrupole) modes can develop large growth rates in conditions where convective
instability is damped or even suppressed. The dominance of low-mode deformation
at the time of shock revival has been recognized as a possible explanation of
large pulsar kicks and of large-scale mixing phenomena observed in supernovae
like SN 1987A.
|
astro-ph
|
the neutrinoheating mechanism remains a viable possibility for the cause of the explosion in a wide mass range of supernova progenitors this is demonstrated by recent twodimensional hydrodynamic simulations with detailed energydependent neutrino transport neutrinodriven explosions were not only found for stars in the range of 810 solar masses with onemg cores and in case of the iron core collapse of a progenitor with 11 solar masses but also for a typical progenitor model of 15 solar masses for such more massive stars however the explosion occurs significantly later than so far thought and is crucially supported by largeamplitude bipolar oscillations due to the nonradial standing accretion shock instability sasi whose low dipole and quadrupole modes can develop large growth rates in conditions where convective instability is damped or even suppressed the dominance of lowmode deformation at the time of shock revival has been recognized as a possible explanation of large pulsar kicks and of largescale mixing phenomena observed in supernovae like sn 1987a
|
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|
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|
706.3057
|
The characteristic polynomial on compact groups with Haar measure : some
equalities in law
|
This note presents some equalities in law for $Z_N:=\det(\Id-G)$, where $G$
is an element of a subgroup of the set of unitary matrices of size $N$, endowed
with its unique probability Haar measure. Indeed, under some general
conditions, $Z_N$ can be decomposed as a product of independent random
variables, whose laws are explicitly known. Our results can be obtained in two
ways : either by a recursive decomposition of the Haar measure or by previous
results by Killip and Nenciu on orthogonal polynomials with respect to some
measure on the unit circle. This latter method leads naturally to a study of
determinants of a class of principal submatrices.
|
math.PR math-ph math.MP
|
this note presents some equalities in law for z_ndetidg where g is an element of a subgroup of the set of unitary matrices of size n endowed with its unique probability haar measure indeed under some general conditions z_n can be decomposed as a product of independent random variables whose laws are explicitly known our results can be obtained in two ways either by a recursive decomposition of the haar measure or by previous results by killip and nenciu on orthogonal polynomials with respect to some measure on the unit circle this latter method leads naturally to a study of determinants of a class of principal submatrices
|
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|
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|
706.3058
|
Size Effects in the Magnetoresistance of Graphite: Absence of
Magnetoresistance in Micrometer size Samples
|
We present a study of the magnetoresistance of highly oriented pyrolytic
graphite (HOPG) as a function of the sample size. Our results show
unequivocally that the magnetoresistance reduces with the sample size even for
samples of hundreds of micrometers size. This sample size effect is due the
large mean free path and Fermi wavelength of carriers in graphite and may
explain the observed practically absence of magnetoresistance in micrometer
confined small graphene samples where quantum effects should be at hand. These
were not taken into account in the literature yet and ask for a revision of
experimental and theoretical work on graphite.
|
cond-mat.mes-hall cond-mat.mtrl-sci
|
we present a study of the magnetoresistance of highly oriented pyrolytic graphite hopg as a function of the sample size our results show unequivocally that the magnetoresistance reduces with the sample size even for samples of hundreds of micrometers size this sample size effect is due the large mean free path and fermi wavelength of carriers in graphite and may explain the observed practically absence of magnetoresistance in micrometer confined small graphene samples where quantum effects should be at hand these were not taken into account in the literature yet and ask for a revision of experimental and theoretical work on graphite
|
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|
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|
706.3059
|
Jet lag effect and leading hadron production
|
We propose a solution for the long standing puzzle of a too steeply falling
fragmentation function for a quark fragmenting into a pion, calculated by
Berger [1] in the Born approximation. Contrary to the simple anticipation that
gluon resummation worsens the problem, we find good agreement with data. Higher
quark Fock states slow down the quark, an effect which we call jet lag. It can
be also expressed in terms of vacuum energy loss. As a result, the space-time
development of the jet shrinks and the $z$-dependence becomes flatter than in
the Born approximation. The space-time pattern is also of great importance for
in-medium hadronization.
|
hep-ph nucl-th
|
we propose a solution for the long standing puzzle of a too steeply falling fragmentation function for a quark fragmenting into a pion calculated by berger 1 in the born approximation contrary to the simple anticipation that gluon resummation worsens the problem we find good agreement with data higher quark fock states slow down the quark an effect which we call jet lag it can be also expressed in terms of vacuum energy loss as a result the spacetime development of the jet shrinks and the zdependence becomes flatter than in the born approximation the spacetime pattern is also of great importance for inmedium hadronization
|
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|
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|
706.306
|
N-Body Simulations on GPUs
|
Commercial graphics processors (GPUs) have high compute capacity at very low
cost, which makes them attractive for general purpose scientific computing. In
this paper we show how graphics processors can be used for N-body simulations
to obtain improvements in performance over current generation CPUs. We have
developed a highly optimized algorithm for performing the O(N^2) force
calculations that constitute the major part of stellar and molecular dynamics
simulations. In some of the calculations, we achieve sustained performance of
nearly 100 GFlops on an ATI X1900XTX. The performance on GPUs is comparable to
specialized processors such as GRAPE-6A and MDGRAPE-3, but at a fraction of the
cost. Furthermore, the wide availability of GPUs has significant implications
for cluster computing and distributed computing efforts like Folding@Home.
|
cs.CE cs.DC
|
commercial graphics processors gpus have high compute capacity at very low cost which makes them attractive for general purpose scientific computing in this paper we show how graphics processors can be used for nbody simulations to obtain improvements in performance over current generation cpus we have developed a highly optimized algorithm for performing the on2 force calculations that constitute the major part of stellar and molecular dynamics simulations in some of the calculations we achieve sustained performance of nearly 100 gflops on an ati x1900xtx the performance on gpus is comparable to specialized processors such as grape6a and mdgrape3 but at a fraction of the cost furthermore the wide availability of gpus has significant implications for cluster computing and distributed computing efforts like foldinghome
|
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|
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|
706.3061
|
Pump-probe polarized transient hole burning (PTHB) dynamics of hydrated
electron revisited
|
Femtosecond PTHB spectroscopy was expected to demonstrate the existence of
distinct s-p absorption subbands originating from the three nondegenerate
p-like excited states of hydrated electron in anisotropic solvation cavity. Yet
no conclusive experimental evidence either for this subband structure or the
reorientation of the cavity on the picosecond time scale has been obtained. We
demonstrate that rapid reorientation of s-p transition dipole moments in
response to small scale motion of water molecules is the likely culprit. The
polarized bleach is shown to be too small and too short lived to be observed
reliably on the sub-picosecond time scale.
|
physics.chem-ph
|
femtosecond pthb spectroscopy was expected to demonstrate the existence of distinct sp absorption subbands originating from the three nondegenerate plike excited states of hydrated electron in anisotropic solvation cavity yet no conclusive experimental evidence either for this subband structure or the reorientation of the cavity on the picosecond time scale has been obtained we demonstrate that rapid reorientation of sp transition dipole moments in response to small scale motion of water molecules is the likely culprit the polarized bleach is shown to be too small and too short lived to be observed reliably on the subpicosecond time scale
|
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|
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|
706.3062
|
Carbon Detonation and Shock-Triggered Helium Burning in Neutron Star
Superbursts
|
The strong degeneracy of the 12C ignition layer on an accreting neutron star
results in a hydrodynamic thermonuclear runaway, in which the nuclear heating
time becomes shorter than the local dynamical time. We model the resulting
combustion wave during these superbursts as an upward propagating detonation.
We solve the reactive fluid flow and show that the detonation propagates
through the deepest layers of fuel and drives a shock wave that steepens as it
travels upward into lower density material. The shock is sufficiently strong
upon reaching the freshly accreted H/He layer that it triggers unstable 4He
burning if the superburst occurs during the latter half of the regular Type I
bursting cycle; this is likely the origin of the bright Type I precursor bursts
observed at the onset of superbursts. The cooling of the outermost shock-heated
layers produces a bright, ~0.1s, flash that precedes the Type I burst by a few
seconds; this may be the origin of the spike seen at the burst onset in 4U
1820-30 and 4U 1636-54, the only two bursts observed with RXTE at high time
resolution. The dominant products of the 12C detonation are 28Si, 32S, and
36Ar. Gupta et al. showed that a crust composed of such intermediate mass
elements has a larger heat flux than one composed of iron-peak elements and
helps bring the superburst ignition depth into better agreement with values
inferred from observations.
|
astro-ph
|
the strong degeneracy of the 12c ignition layer on an accreting neutron star results in a hydrodynamic thermonuclear runaway in which the nuclear heating time becomes shorter than the local dynamical time we model the resulting combustion wave during these superbursts as an upward propagating detonation we solve the reactive fluid flow and show that the detonation propagates through the deepest layers of fuel and drives a shock wave that steepens as it travels upward into lower density material the shock is sufficiently strong upon reaching the freshly accreted hhe layer that it triggers unstable 4he burning if the superburst occurs during the latter half of the regular type i bursting cycle this is likely the origin of the bright type i precursor bursts observed at the onset of superbursts the cooling of the outermost shockheated layers produces a bright 01s flash that precedes the type i burst by a few seconds this may be the origin of the spike seen at the burst onset in 4u 182030 and 4u 163654 the only two bursts observed with rxte at high time resolution the dominant products of the 12c detonation are 28si 32s and 36ar gupta et al showed that a crust composed of such intermediate mass elements has a larger heat flux than one composed of ironpeak elements and helps bring the superburst ignition depth into better agreement with values inferred from observations
|
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|
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|
706.3063
|
Self-similar shear-thickening behavior in CTAB/NaSal surfactant
solutions
|
The effect of salt concentration Cs on the critical shear rate required for
the onset of shear thickening and apparent relaxation time of the
shear-thickened phase, has been investigated systematically for dilute
CTAB/NaSal solutions. Experimental data suggest a self-similar behavior of the
critical shear rate and relaxation time as functions of Cs. Specifically, the
former ~ Cs^(-6) whereas the latter ~ Cs^(6) such that an effective Weissenberg
number for the onset of the shear thickened phase is only weakly dependent on
Cs. A procedure has been developed to collapse the apparent shear viscosity
versus shear rate data obtained for various values of Cs into a single master
curve. The effect of Cs on the elastic modulus and mesh size of the
shear-induced gel phase for different surfactant concentrations is discussed.
Experiments performed using different flow cells (Couette and cone-and-plate)
show that the critical shear rate, relaxation time and the maximum viscosity
attained are geometry-independent. The elastic modulus of the gel phase
inferred indirectly by employing simplified hydrodynamic instability analysis
of a sheared gel-fluid interface is in qualitative agreement with that
predicted for an entangled phase of living polymers. A qualitative mechanism
that combines the effect of Cs on average micelle length and Debye parameter
with shear-induced configurational changes of rod-like micelles is proposed to
rationalize the self-similarity of SIS formation.
|
physics.flu-dyn
|
the effect of salt concentration cs on the critical shear rate required for the onset of shear thickening and apparent relaxation time of the shearthickened phase has been investigated systematically for dilute ctabnasal solutions experimental data suggest a selfsimilar behavior of the critical shear rate and relaxation time as functions of cs specifically the former cs6 whereas the latter cs6 such that an effective weissenberg number for the onset of the shear thickened phase is only weakly dependent on cs a procedure has been developed to collapse the apparent shear viscosity versus shear rate data obtained for various values of cs into a single master curve the effect of cs on the elastic modulus and mesh size of the shearinduced gel phase for different surfactant concentrations is discussed experiments performed using different flow cells couette and coneandplate show that the critical shear rate relaxation time and the maximum viscosity attained are geometryindependent the elastic modulus of the gel phase inferred indirectly by employing simplified hydrodynamic instability analysis of a sheared gelfluid interface is in qualitative agreement with that predicted for an entangled phase of living polymers a qualitative mechanism that combines the effect of cs on average micelle length and debye parameter with shearinduced configurational changes of rodlike micelles is proposed to rationalize the selfsimilarity of sis formation
|
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|
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|
706.3064
|
Growing Matter
|
We investigate quintessence cosmologies with a matter component consisting of
particles with an increasing mass. While negligible in early cosmology, the
appearance of a growing matter component has stopped the evolution of the
cosmon field at a redshift around six. In turn, this has triggered the
accelerated expansion of the Universe. We propose to associate growing matter
with neutrinos. Then the presently observed dark energy density and its
equation of state are determined by the neutrino mass.
|
astro-ph hep-ph hep-th
|
we investigate quintessence cosmologies with a matter component consisting of particles with an increasing mass while negligible in early cosmology the appearance of a growing matter component has stopped the evolution of the cosmon field at a redshift around six in turn this has triggered the accelerated expansion of the universe we propose to associate growing matter with neutrinos then the presently observed dark energy density and its equation of state are determined by the neutrino mass
|
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|
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|
706.3065
|
Double Chargino Production in $e^{-}e^{-}$ scattering
|
We point out the production of the charginos and neutralinos in
electron-electron process in several supersymmetric models, in order to show
that the International Linear Collider can discover double charged charginos if
these particles really exist in nature.
|
hep-ph hep-ex
|
we point out the production of the charginos and neutralinos in electronelectron process in several supersymmetric models in order to show that the international linear collider can discover double charged charginos if these particles really exist in nature
|
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|
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|
706.3066
|
Dielectric microscopy with submillimeter resolution
|
In analogy with optical near-field scanning methods, we use tapered
dielectric waveguides as probes for a millimeter wave vector network analyzer.
By scanning thin samples between two such probes we are able to map the
spatially varying dielectric properties of materials with sub-wavelength
resolution; using a 150 GHz probe in transmision mode we see spatial resolution
of around 500 microns. We have applied this method to a variety of highly
heterogeneous materials. Here we show dielectric maps of granite and oil shale.
|
cond-mat.soft cond-mat.mtrl-sci
|
in analogy with optical nearfield scanning methods we use tapered dielectric waveguides as probes for a millimeter wave vector network analyzer by scanning thin samples between two such probes we are able to map the spatially varying dielectric properties of materials with subwavelength resolution using a 150 ghz probe in transmision mode we see spatial resolution of around 500 microns we have applied this method to a variety of highly heterogeneous materials here we show dielectric maps of granite and oil shale
|
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|
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|
706.3067
|
Fitting analysis provides further evidence for eradication of hiv/aids
infection under combined liposome drug delivery treatment
|
It is now evident that the commonly accepted strategy for treatment of
HIV/AIDS by highly active antiretroviral therapy (HAART) will not lead to
eradication of HIV in a reasonable time. This is straightforward from the
typical exponential viral load decay upon treatment revealing initial
considerable but incomplete reduction of plasma HIV RNA with subsequent low
level HIV persistence even in patients on effective antiretroviral therapy.
Here we show that the viral load follows a simple zero trend linear regression
line under different treatment approach recently proposed by us. This
unambiguously indicates a whole body HIV eradication in reasonable time.
|
q-bio.TO
|
it is now evident that the commonly accepted strategy for treatment of hivaids by highly active antiretroviral therapy haart will not lead to eradication of hiv in a reasonable time this is straightforward from the typical exponential viral load decay upon treatment revealing initial considerable but incomplete reduction of plasma hiv rna with subsequent low level hiv persistence even in patients on effective antiretroviral therapy here we show that the viral load follows a simple zero trend linear regression line under different treatment approach recently proposed by us this unambiguously indicates a whole body hiv eradication in reasonable time
|
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|
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|
706.3068
|
A 12um ISOCAM Survey of the ESO-Sculptor Field: Data Reduction and
Analysis
|
We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM
open time observation performed on the ESO-Sculptor Survey field (Arnouts et
al. 1997). A complete catalogue of 142 sources (120 galaxies and 22 stars),
detected with high significance (equivalent to 5sigma), is presented above an
integrated flux density of 0.24mJy. Star/galaxy separation is performed by a
detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and
below this flux density the incompleteness is corrected using two independent
methods. The first method uses stars and the second uses optical counterparts
of the ISOCAM galaxies; these methods yield consistent results. We also apply
an empirical flux density calibration using stars in the field. For each star,
the 12um flux density is derived by fitting optical colours from a multi-band
chi^2 to stellar templates (BaSel-2.0) and using empirical optical-IR
colour-colour relations. This article is a companion analysis to
Rocca-Volmerange 2007 et al. where the 12um faint galaxy counts are presented
and analysed by galaxy type with the evolutionary code PEGASE.3.
|
astro-ph
|
we present a detailed reduction of a midinfrared 12um lw10 filter isocam open time observation performed on the esosculptor survey field arnouts et al 1997 a complete catalogue of 142 sources 120 galaxies and 22 stars detected with high significance equivalent to 5sigma is presented above an integrated flux density of 024mjy stargalaxy separation is performed by a detailed study of colourcolour diagrams the catalogue is complete to 1mjy and below this flux density the incompleteness is corrected using two independent methods the first method uses stars and the second uses optical counterparts of the isocam galaxies these methods yield consistent results we also apply an empirical flux density calibration using stars in the field for each star the 12um flux density is derived by fitting optical colours from a multiband chi2 to stellar templates basel20 and using empirical opticalir colourcolour relations this article is a companion analysis to roccavolmerange 2007 et al where the 12um faint galaxy counts are presented and analysed by galaxy type with the evolutionary code pegase3
|
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|
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|
706.3069
|
Network synchronization: Spectral versus statistical properties
|
We consider synchronization of weighted networks, possibly with asymmetrical
connections. We show that the synchronizability of the networks cannot be
directly inferred from their statistical properties. Small local changes in the
network structure can sensitively affect the eigenvalues relevant for
synchronization, while the gross statistical network properties remain
essentially unchanged. Consequently, commonly used statistical properties,
including the degree distribution, degree homogeneity, average degree, average
distance, degree correlation, and clustering coefficient, can fail to
characterize the synchronizability of networks.
|
cond-mat.dis-nn nlin.AO
|
we consider synchronization of weighted networks possibly with asymmetrical connections we show that the synchronizability of the networks cannot be directly inferred from their statistical properties small local changes in the network structure can sensitively affect the eigenvalues relevant for synchronization while the gross statistical network properties remain essentially unchanged consequently commonly used statistical properties including the degree distribution degree homogeneity average degree average distance degree correlation and clustering coefficient can fail to characterize the synchronizability of networks
|
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|
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|
706.307
|
Potential for the slow-roll inflation, mass scale hierarchy and Dark
Energy from the Type IIA supergravity
|
The magnetic fluxbrane solution with a strongly warped throat is studied in
the Type IIA supergravity theory with co-dimension one local source which
surves as $Z_{2}$-symmetric UV boundary of the throat. Overall volume of extra
space is stabilized since introduction of the local source breaks the no-scale
structure of the theory and evades the no-go theorem. Radion field is defined
as the position of UV boundary "moved" from its stable value fixed by the
anisotropic Israel junction conditions. Analytical expression for the radion
effective potential is received. Potential decreases exponentially (exponent is
equal to 0,21 in Planck units) in the slow-roll region and apparently meets
other demands of the early inflation. Reissner-Nordstrom type deformation of
the elementary fluxbrane solution permits to construct the IR end of the throat
and results in tiny positive non-zero value of the radion potential in its
extremal point seen today as Dark Energy $\rho_{D.E.}$. Expressions for the
mass scale hierarchy and for the "acceleration hierarchy" received in the paper
give the physically interesting relation between two hierarchies: $\rho_{D.E.}
\sim G_{N}^{2}m^{8}$.
|
hep-th
|
the magnetic fluxbrane solution with a strongly warped throat is studied in the type iia supergravity theory with codimension one local source which surves as z_2symmetric uv boundary of the throat overall volume of extra space is stabilized since introduction of the local source breaks the noscale structure of the theory and evades the nogo theorem radion field is defined as the position of uv boundary moved from its stable value fixed by the anisotropic israel junction conditions analytical expression for the radion effective potential is received potential decreases exponentially exponent is equal to 021 in planck units in the slowroll region and apparently meets other demands of the early inflation reissnernordstrom type deformation of the elementary fluxbrane solution permits to construct the ir end of the throat and results in tiny positive nonzero value of the radion potential in its extremal point seen today as dark energy rho_de expressions for the mass scale hierarchy and for the acceleration hierarchy received in the paper give the physically interesting relation between two hierarchies rho_de sim g_n2m8
|
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|
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|
706.3071
|
Extreme values for Benedicks-Carleson quadratic maps
|
We consider the quadratic family of maps given by $f_{a}(x)=1-a x^2$ with
$x\in [-1,1]$, where $a$ is a Benedicks-Carleson parameter. For each of these
chaotic dynamical systems we study the extreme value distribution of the
stationary stochastic processes $X_0,X_1,...$, given by $X_{n}=f_a^n$, for
every integer $n\geq0$, where each random variable $X_n$ is distributed
according to the unique absolutely continuous, invariant probability of $f_a$.
Using techniques developed by Benedicks and Carleson, we show that the limiting
distribution of $M_n=\max\{X_0,...,X_{n-1}\}$ is the same as that which would
apply if the sequence $X_0,X_1,...$ was independent and identically
distributed. This result allows us to conclude that the asymptotic distribution
of $M_n$ is of Type III (Weibull).
|
math.DS math.PR math.ST stat.TH
|
we consider the quadratic family of maps given by f_ax1a x2 with xin 11 where a is a benedickscarleson parameter for each of these chaotic dynamical systems we study the extreme value distribution of the stationary stochastic processes x_0x_1 given by x_nf_an for every integer ngeq0 where each random variable x_n is distributed according to the unique absolutely continuous invariant probability of f_a using techniques developed by benedicks and carleson we show that the limiting distribution of m_nmaxx_0x_n1 is the same as that which would apply if the sequence x_0x_1 was independent and identically distributed this result allows us to conclude that the asymptotic distribution of m_n is of type iii weibull
|
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|
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|
706.3072
|
Efficient vibrational state coupling in an optical tilted-washboard
potential via multiple spatial translations and application to pulse echo
|
We measure the application of simple and compound pulses consisting of
time-dependent spatial translations to coupling vibrational states of ultracold
85Rb atoms in a far-detuned 1D optical lattice. The lattice wells are so
shallow as to support only two bound states, and we prepare the atoms in the
ground state. The lattice is oriented vertically, leading to a tilted-washboard
potential analogous to those encountered in condensed-matter systems.
Experimentally, we find that a square pulse consisting of lattice displacements
and a delay is more efficient than single-step and Gaussian pulses. This is
described as an example of coherent control. It is striking that contrary to
the intuition that soft pulses minimize loss, the Gaussian pulse is
outperformed by the square pulse. Numerical calculations are in strong
agreement with our experimental results and show the superiority of the square
pulse to the single-step pulse for all lattice depths and to the Gaussian pulse
for lattice depths greater than 7 lattice recoil energies. We also compare the
effectiveness of these pulses for reviving oscillations of atoms in vibrational
superposition states using the pulse-echo technique. We find that the square
and Gaussian pulses result in higher echo amplitudes than the single-step
pulse. These improved echo pulses allow us to probe coherence at longer times
than in the past, measuring a plateau which has yet to be explained. In
addition, we show numerically that the vibrational state coupling due to such
lattice manipulations is more efficient in shallow lattices than in deep
lattices.
|
quant-ph
|
we measure the application of simple and compound pulses consisting of timedependent spatial translations to coupling vibrational states of ultracold 85rb atoms in a fardetuned 1d optical lattice the lattice wells are so shallow as to support only two bound states and we prepare the atoms in the ground state the lattice is oriented vertically leading to a tiltedwashboard potential analogous to those encountered in condensedmatter systems experimentally we find that a square pulse consisting of lattice displacements and a delay is more efficient than singlestep and gaussian pulses this is described as an example of coherent control it is striking that contrary to the intuition that soft pulses minimize loss the gaussian pulse is outperformed by the square pulse numerical calculations are in strong agreement with our experimental results and show the superiority of the square pulse to the singlestep pulse for all lattice depths and to the gaussian pulse for lattice depths greater than 7 lattice recoil energies we also compare the effectiveness of these pulses for reviving oscillations of atoms in vibrational superposition states using the pulseecho technique we find that the square and gaussian pulses result in higher echo amplitudes than the singlestep pulse these improved echo pulses allow us to probe coherence at longer times than in the past measuring a plateau which has yet to be explained in addition we show numerically that the vibrational state coupling due to such lattice manipulations is more efficient in shallow lattices than in deep lattices
|
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|
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|
706.3073
|
Tau-function of discrete isomonodromy transformations and probability
|
We introduce the tau-function of a rational d-connection and its isomonodromy
transformations. We show that in a continuous limit our tau-function agrees
with the Jimbo-Miwa-Ueno tau-function, compute the tau-function for the
isomonodromy transformations leading to difference Painleve V and difference
Painleve VI equations, and prove that the gap probability for a wide class of
discrete random matrix type models can be viewed as the tau-function for an
associated d-connection.
|
math.AG math-ph math.MP math.PR
|
we introduce the taufunction of a rational dconnection and its isomonodromy transformations we show that in a continuous limit our taufunction agrees with the jimbomiwaueno taufunction compute the taufunction for the isomonodromy transformations leading to difference painleve v and difference painleve vi equations and prove that the gap probability for a wide class of discrete random matrix type models can be viewed as the taufunction for an associated dconnection
|
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|
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|
706.3074
|
A review of wildland fire spread modelling, 1990-present, 1: Physical
and quasi-physical models
|
In recent years, advances in computational power and spatial data analysis
(GIS, remote sensing, etc) have led to an increase in attempts to model the
spread and behaviour of wildland fires across the landscape. This series of
review papers endeavours to critically and comprehensively review all types of
surface fire spread models developed since 1990. This paper reviews models of a
physical or quasi-physical nature. These models are based on the fundamental
chemistry and/or physics of combustion and fire spread. Other papers in the
series review models of an empirical or quasi-empirical nature, and
mathematical analogues and simulation models. Many models are extensions or
refinements of models developed before 1990. Where this is the case, these
models are also discussed but much less comprehensively.
|
physics.geo-ph physics.ao-ph physics.flu-dyn
|
in recent years advances in computational power and spatial data analysis gis remote sensing etc have led to an increase in attempts to model the spread and behaviour of wildland fires across the landscape this series of review papers endeavours to critically and comprehensively review all types of surface fire spread models developed since 1990 this paper reviews models of a physical or quasiphysical nature these models are based on the fundamental chemistry andor physics of combustion and fire spread other papers in the series review models of an empirical or quasiempirical nature and mathematical analogues and simulation models many models are extensions or refinements of models developed before 1990 where this is the case these models are also discussed but much less comprehensively
|
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|
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|
706.3075
|
Stochastic Lorentz forces on a point charge moving near the conducting
plate
|
The influence of quantized electromagnetic fields on a nonrelativistic
charged particle moving near a conducting plate is studied. We give a
field-theoretic derivation of the nonlinear, non-Markovian Langevin equation of
the particle by the method of Feynman-Vernon influence functional. This
stochastic approach incorporates not only the stochastic noise manifested from
electromagnetic vacuum fluctuations, but also dissipation backreaction on a
charge in the form of the retarded Lorentz forces. Since the imposition of the
boundary is expected to anisotropically modify the effects of the fields on the
evolution of the particle, we consider the motion of a charge undergoing
small-amplitude oscillations in the direction either parallel or normal to the
plane boundary. Under the dipole approximation for nonrelativistic motion,
velocity fluctuations of the charge are found to grow linearly with time in the
early stage of the evolution at the rather different rate, revealing strong
anisotropic behavior. They are then asymptotically saturated as a result of the
fluctuation-dissipation relation, and the same saturated value is found for the
motion in both directions. The observational consequences are discussed. plane
boundary. Velocity fluctuations of the charge are found to grow linearly with
time in the early stage of the evolution at the rate given by the relaxation
constant, which turns out to be smaller in the parallel case than in the
perpendicular one in a similar configuration. Then, they are asymptotically
saturated as a result of the fluctuation-dissipation relation. For the
electron, the same saturated value is obtained for motion in both directions,
and is mainly determined by its oscillatory motion. Possible observational
consequences are discussed.
|
hep-th quant-ph
|
the influence of quantized electromagnetic fields on a nonrelativistic charged particle moving near a conducting plate is studied we give a fieldtheoretic derivation of the nonlinear nonmarkovian langevin equation of the particle by the method of feynmanvernon influence functional this stochastic approach incorporates not only the stochastic noise manifested from electromagnetic vacuum fluctuations but also dissipation backreaction on a charge in the form of the retarded lorentz forces since the imposition of the boundary is expected to anisotropically modify the effects of the fields on the evolution of the particle we consider the motion of a charge undergoing smallamplitude oscillations in the direction either parallel or normal to the plane boundary under the dipole approximation for nonrelativistic motion velocity fluctuations of the charge are found to grow linearly with time in the early stage of the evolution at the rather different rate revealing strong anisotropic behavior they are then asymptotically saturated as a result of the fluctuationdissipation relation and the same saturated value is found for the motion in both directions the observational consequences are discussed plane boundary velocity fluctuations of the charge are found to grow linearly with time in the early stage of the evolution at the rate given by the relaxation constant which turns out to be smaller in the parallel case than in the perpendicular one in a similar configuration then they are asymptotically saturated as a result of the fluctuationdissipation relation for the electron the same saturated value is obtained for motion in both directions and is mainly determined by its oscillatory motion possible observational consequences are discussed
|
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|
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|
706.3076
|
On the Performance of Joint Fingerprint Embedding and Decryption Scheme
|
Till now, few work has been done to analyze the performances of joint
fingerprint embedding and decryption schemes. In this paper, the security of
the joint fingerprint embedding and decryption scheme proposed by Kundur et al.
is analyzed and improved. The analyses include the security against
unauthorized customer, the security against authorized customer, the
relationship between security and robustness, the relationship between
secu-rity and imperceptibility and the perceptual security. Based these
analyses, some means are proposed to strengthen the system, such as multi-key
encryp-tion and DC coefficient encryption. The method can be used to analyze
other JFD schemes. It is expected to provide valuable information to design JFD
schemes.
|
cs.MM cs.CR
|
till now few work has been done to analyze the performances of joint fingerprint embedding and decryption schemes in this paper the security of the joint fingerprint embedding and decryption scheme proposed by kundur et al is analyzed and improved the analyses include the security against unauthorized customer the security against authorized customer the relationship between security and robustness the relationship between security and imperceptibility and the perceptual security based these analyses some means are proposed to strengthen the system such as multikey encryption and dc coefficient encryption the method can be used to analyze other jfd schemes it is expected to provide valuable information to design jfd schemes
|
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|
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|
706.3077
|
Exact solution of the Faddeev-Volkov model
|
The Faddeev-Volkov model is an Ising-type lattice model with positive
Boltzmann weights where the spin variables take continuous values on the real
line. It serves as a lattice analog of the sinh-Gordon and Liouville models and
intimately connected with the modular double of the quantum group U_q(sl_2).
The free energy of the model is exactly calculated in the thermodynamic limit.
In the quasi-classical limit c->infinity the model describes quantum
fluctuations of discrete conformal transformations connected with the
Thurston's discrete analogue of the Riemann mappings theorem. In the
strongly-coupled limit c->1 the model turns into a discrete version of the D=2
Zamolodchikov's ``fishing-net'' model.
|
cond-mat.stat-mech hep-th math-ph math.MP
|
the faddeevvolkov model is an isingtype lattice model with positive boltzmann weights where the spin variables take continuous values on the real line it serves as a lattice analog of the sinhgordon and liouville models and intimately connected with the modular double of the quantum group u_qsl_2 the free energy of the model is exactly calculated in the thermodynamic limit in the quasiclassical limit cinfinity the model describes quantum fluctuations of discrete conformal transformations connected with the thurstons discrete analogue of the riemann mappings theorem in the stronglycoupled limit c1 the model turns into a discrete version of the d2 zamolodchikovs fishingnet model
|
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|
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|
706.3078
|
Index Theorem in Finite Noncommutative Geometry
|
Index theorem is formulated in noncommutative geometry with finite degrees of
freedom by using Ginsparg-Wilson relation. It is extended to the case where the
gauge symmetry is spontaneously broken. Dynamical analysis about topological
aspects in gauge theory is also shown.
|
hep-th hep-lat
|
index theorem is formulated in noncommutative geometry with finite degrees of freedom by using ginspargwilson relation it is extended to the case where the gauge symmetry is spontaneously broken dynamical analysis about topological aspects in gauge theory is also shown
|
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|
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|
706.3079
|
Revisiting the QCD corrections to the R-parity violating processes
$p\bar{p}/pp \to e\mu+X$
|
We present the theoretical predictions up to QCD NLO for the cross section of
high-mass electron-muon pair production at the Tevatron and the LHC,
considering only the dominant contributions from the third-generation
sneutrino. The dependence of the renormalization and factorization scales on
the total cross section, and the effects on the K-factor due to the uncertainty
of parton distribution function(PDF) have been carefully investigated. By
considering soft-gluon resummation effects to all order in $\alpha_s$ of
leading logarithm, we present the transverse momentum distributions of the
final $e\mu$ pair.
|
hep-ph
|
we present the theoretical predictions up to qcd nlo for the cross section of highmass electronmuon pair production at the tevatron and the lhc considering only the dominant contributions from the thirdgeneration sneutrino the dependence of the renormalization and factorization scales on the total cross section and the effects on the kfactor due to the uncertainty of parton distribution functionpdf have been carefully investigated by considering softgluon resummation effects to all order in alpha_s of leading logarithm we present the transverse momentum distributions of the final emu pair
|
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|
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|
706.308
|
Does a black hole rotate in Chern-Simons modified gravity?
|
Rotating black hole solutions in the (3+1)-dimensional Chern-Simons modified
gravity theory are discussed by taking account of perturbation around the
Schwarzschild solution. The zenith-angle dependence of a metric function
related to the frame-dragging effect is determined from a constraint equation
independently of a choice of the embedding coordinate. We find that at least
within the framework of the first-order perturbation method, the black hole
cannot rotate for finite black hole mass if the embedding coordinate is taken
to be a timelike vector. However, the rotation can be permitted in the limit of
$M/r \to 0$ (where $M$ is the black hole mass and $r$ is the radius). For a
spacelike vector, the rotation can also be permitted for any value of the black
hole mass.
|
gr-qc
|
rotating black hole solutions in the 31dimensional chernsimons modified gravity theory are discussed by taking account of perturbation around the schwarzschild solution the zenithangle dependence of a metric function related to the framedragging effect is determined from a constraint equation independently of a choice of the embedding coordinate we find that at least within the framework of the firstorder perturbation method the black hole cannot rotate for finite black hole mass if the embedding coordinate is taken to be a timelike vector however the rotation can be permitted in the limit of mr to 0 where m is the black hole mass and r is the radius for a spacelike vector the rotation can also be permitted for any value of the black hole mass
|
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|
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|
706.3081
|
Strong Uniqueness of the Ricci Flow
|
In this paper, we derive some local a priori estimates for Ricci flow. This
gives rise to some strong uniqueness theorems. As a corollary, let $g(t)$ be a
smooth complete solution to the Ricci flow on $\mathbb{R}^{3}$, with the
canonical Euclidean metric $E$ as initial data, then $g(t)$ is trivial, i.e.
$g(t)\equiv E$.
|
math.DG math.AP
|
in this paper we derive some local a priori estimates for ricci flow this gives rise to some strong uniqueness theorems as a corollary let gt be a smooth complete solution to the ricci flow on mathbbr3 with the canonical euclidean metric e as initial data then gt is trivial ie gtequiv e
|
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|
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|
706.3082
|
Configurations of Extremal Even Unimodular Lattices
|
We extend the results of Ozeki on the configurations of extremal even
unimodular lattices. Specifically, we show that if L is such a lattice of rank
56, 72, or 96, then L is generated by its minimal-norm vectors.
|
math.NT
|
we extend the results of ozeki on the configurations of extremal even unimodular lattices specifically we show that if l is such a lattice of rank 56 72 or 96 then l is generated by its minimalnorm vectors
|
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|
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|
706.3083
|
Perturbative spectrum of a Yukawa-Higgs model with Ginsparg-Wilson
fermions
|
A Yukawa-Higgs model with Ginsparg-Wilson (GW) fermions, proposed recently by
Bhattacharya, Martin and Poppitz as a possible lattice formulation of chiral
gauge theories, is studied. A simple argument shows that the gauge boson always
acquires mass by the St\"uckelberg (or, in a broad sense, Higgs) mechanism,
regardless of strength of interactions. The gauge symmetry is spontaneously
broken. When the gauge coupling constant is small, the physical spectrum of the
model consists of massless fermions, massive fermions and \emph{massive} vector
bosons.
|
hep-lat hep-th
|
a yukawahiggs model with ginspargwilson gw fermions proposed recently by bhattacharya martin and poppitz as a possible lattice formulation of chiral gauge theories is studied a simple argument shows that the gauge boson always acquires mass by the stuckelberg or in a broad sense higgs mechanism regardless of strength of interactions the gauge symmetry is spontaneously broken when the gauge coupling constant is small the physical spectrum of the model consists of massless fermions massive fermions and emphmassive vector bosons
|
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|
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|
706.3084
|
VLA H53alpha observations of the central region of the Super Star
Cluster Galaxy NGC 5253
|
We present observations in the H53alpha line and radio continuum at 43 GHz
carried out with the VLA in the D array (2'' angular resolution) toward the
starburst galaxy NGC 5253. VLA archival data have been reprocessed to produce a
uniform set of 2, 1.3 and 0.7 cm high angular (0.''2 X 0.''1) radio continuum
images. The RRL H53alpha, a previously reported measurement of the H92alpha RRL
flux density and the reprocessed high angular resolution radio continuum flux
densities have been modeled using a collection of HII regions. Based on the
models, the ionized gas in the nuclear source has an electron density of ~6 X
10^4 cm^-3 and an volume filling factor of 0.05. A Lyman continuum photon
production rate of 2 X 10^52 s^-1 is necessary to sustain the ionization in the
nuclear region. The number of required O7 stars in the central 1.5 pc of the
supernebula is ~ 2000. The H53alpha velocity gradient 10 km s^-1 arcsec^-1)
implies a dynamical mass of ~3X10^5 Msun; this mass suggests the supernebula is
confined by gravity.
|
astro-ph
|
we present observations in the h53alpha line and radio continuum at 43 ghz carried out with the vla in the d array 2 angular resolution toward the starburst galaxy ngc 5253 vla archival data have been reprocessed to produce a uniform set of 2 13 and 07 cm high angular 02 x 01 radio continuum images the rrl h53alpha a previously reported measurement of the h92alpha rrl flux density and the reprocessed high angular resolution radio continuum flux densities have been modeled using a collection of hii regions based on the models the ionized gas in the nuclear source has an electron density of 6 x 104 cm3 and an volume filling factor of 005 a lyman continuum photon production rate of 2 x 1052 s1 is necessary to sustain the ionization in the nuclear region the number of required o7 stars in the central 15 pc of the supernebula is 2000 the h53alpha velocity gradient 10 km s1 arcsec1 implies a dynamical mass of 3x105 msun this mass suggests the supernebula is confined by gravity
|
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|
[-0.08764848253188327, 0.10648771846122558, -0.006522912481820888, 0.03401120537918442, -0.0035500633794899013, -0.05566833175213436, 0.04845386421815916, 0.4469996760493483, -0.09440040339673446, -0.3504094406499379, 0.07211799366500186, -0.28112089686857705, 0.09463113043933515, 0.14309332189507337, -0.003073623812187262, -0.03309585194934202, 0.01129253009275999, -0.10271684380131774, -0.035788685407500125, -0.1930751046648683, 0.23061378391205586, 0.11086789534998719, 0.1823107408973473, 0.03690213013165207, 0.12256230340955715, -0.15798103103721092, -0.09362291806974099, -0.04588708931326189, -0.15055064340413082, 0.04822892660740763, 0.22636257532934162, 0.1007209785563067, 0.2101598669753664, -0.33926570330831135, -0.21077995148781073, 0.042124831564830274, 0.18197641366648235, -0.006915826644134623, 0.004905330400189004, -0.27988836796298117, 0.04734038857912475, -0.2241859350734475, -0.20881961498525925, 0.12579847356325694, 0.09302432229940844, 0.016879893812901257, -0.21661031679038636, 0.1801883511870983, -0.04594948507771981, 0.11360225028660022, -0.09726506321749184, -0.14767288506316784, -0.06521518389953682, 0.02199998198325788, -0.049788432332041506, 0.16342032135104423, 0.21226886299766853, -0.11292781868972022, -0.010576962869064037, 0.3589637958979107, -0.06872301042511192, -0.011054734370004966, 0.20156792043020355, -0.2714514422127236, -0.19845738956725903, 0.3048477529055989, 0.11714713870523238, 0.09293729540811248, -0.12356517270778898, 0.04254061690153321, -0.06833643935731909, 0.2932699218019314, 0.07293640411808155, 0.06415506690055653, 0.2795427758458324, 0.08957292977455919, 0.04061123714993962, 0.07028928501941581, -0.33725750794374937, 0.02768531514712694, -0.23644254599854653, -0.08890826313423035, -0.13189735436356964, 0.18601919667774133, -0.15668772428199934, -0.05437992021854205, 0.2901684475999156, 0.05566106187655929, 0.24523668287491257, 0.009839803524135443, 0.2920798075554723, 0.09249047418093555, 0.0865717187777839, 0.15467118836187926, 0.2979005898285488, 0.2345789293626281, 0.12416252822599332, -0.2070409508318831, -0.03359077850208533, 0.001495157240159725]
|
706.3085
|
The optical spectrum of R Coronae Borealis close to 2003 decline
|
Two sets of high-resolution spectra of R CrB obtained during the 2003 light
decline are described. The first set was obtained on the descending branch of
the light curve when V ~12.0 and the second one in the recovery phase with V
~7.5. The usual sharp and broad emissions are described and the lines radial
velocities measured. C_2 Swan system (0,0) band was found to be in emission for
the first set. The other C_2 bands were in absorption. Few CN red system (5,1)
band rotational lines and low excitation FeI lines were in absorption. A table
with measured radial velocities of various spectral features is presented.
|
astro-ph
|
two sets of highresolution spectra of r crb obtained during the 2003 light decline are described the first set was obtained on the descending branch of the light curve when v 120 and the second one in the recovery phase with v 75 the usual sharp and broad emissions are described and the lines radial velocities measured c_2 swan system 00 band was found to be in emission for the first set the other c_2 bands were in absorption few cn red system 51 band rotational lines and low excitation fei lines were in absorption a table with measured radial velocities of various spectral features is presented
|
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|
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|
706.3086
|
Estimates of Gromov's box distance
|
In 1999, M. Gromov introduced the box distance function $\sikaku$ on the
space of all mm-spaces. In this paper, by using the method of T. H. Colding
(cf. \cite[Lemma 5.10]{Colding}), we estimate
$\sikaku(\mathbb{S}^n,\mathbb{S}^m)$ and $\sikaku (\mathbb{C}P^n,
\mathbb{C}P^m)$, where $\mathbb{S}^n$ is the $n$-dimensional unit sphere in
$\mathbb{R}^{n+1}$ and $\mathbb{C}P^n$ is the $n$-dimensional complex
projective space equipped with the Fubini-Study metric. In paticular, we give
the complete answer to an Exercise of Gromov's Green book (cf. \cite[Section
$3{1/2}.18$]{gromov}). We also estimate $\sikaku \big(SO(n), SO(m)\big)$ from
below, where SO(n) is the special orthogonal group.
|
math.MG
|
in 1999 m gromov introduced the box distance function sikaku on the space of all mmspaces in this paper by using the method of t h colding cf citelemma 510colding we estimate sikakumathbbsnmathbbsm and sikaku mathbbcpn mathbbcpm where mathbbsn is the ndimensional unit sphere in mathbbrn1 and mathbbcpn is the ndimensional complex projective space equipped with the fubinistudy metric in paticular we give the complete answer to an exercise of gromovs green book cf citesection 31218gromov we also estimate sikaku bigson sombig from below where son is the special orthogonal group
|
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|
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|
706.3087
|
Stark units and main conjectures for totally real fields
|
Main theorem of [Buyukboduk, arXiv:0706.0377v1] suggests that it should be
possible to lift the Kolyvagin systems of Stark units constructed in
[Buyukboduk, arXiv:math/0703426v1] to a Kolyvagin system over the cyclotomic
Iwasawa algebra. This is what we prove in this paper. This construction gives
the first example towards a more systematic study of Kolyvagin system theory
over an Iwasawa algebra when the core Selmer rank is greater than one. As a
result of this construction, we reduce the main conjectures of Iwasawa theory
for totally real fields to a statement of local Iwasawa theory. This statement,
however, turns out to be interesting in its own right as it suggests a relation
between solutions to $p$-adic and complex Stark conjectures.
|
math.NT
|
main theorem of buyukboduk arxiv07060377v1 suggests that it should be possible to lift the kolyvagin systems of stark units constructed in buyukboduk arxivmath0703426v1 to a kolyvagin system over the cyclotomic iwasawa algebra this is what we prove in this paper this construction gives the first example towards a more systematic study of kolyvagin system theory over an iwasawa algebra when the core selmer rank is greater than one as a result of this construction we reduce the main conjectures of iwasawa theory for totally real fields to a statement of local iwasawa theory this statement however turns out to be interesting in its own right as it suggests a relation between solutions to padic and complex stark conjectures
|
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|
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|
706.3088
|
Quantum and thermal fluctuations in a two-dimensional correlated band
ferromagnet -- Goldstone-mode preserving investigation with self-energy and
vertex corrections
|
Ferromagnetism in the t-t' Hubbard model is investigated on a square lattice.
Correlation effects in the form of self-energy and vertex corrections are
systematically incorporated within a spin-rotationally-symmetric scheme which
explicitly preserves the Goldstone mode and is therefore in accord with the
Mermin-Wagner theorem. Interplay of band dispersion and correlation effects on
ferromagnetic-state stability are highlighted with respect to both long- and
short-wavelength fluctuations, which are shown to have substantially different
behaviour. Our approach provides a novel understanding of the enhancement of
ferromagnetism near van Hove filling for t'~0.5 in terms of strongly suppressed
saddle-point contribution to the destabilizing exchange part of spin stiffness.
Finite-temperature electron spin dynamics is investigated directly in terms of
spectral-weight transfer across the Fermi energy due to electron-magnon
coupling. Relevant in the context of recent magnetization measurements on
ultrathin films, the role of strong thermal spin fluctuations in low dimensions
is highlighted, in the anisotropy-stabilized ordered state, by determining the
thermal decay of magnetization and T_c within a renormalized spin-fluctuation
theory.
|
cond-mat.str-el
|
ferromagnetism in the tt hubbard model is investigated on a square lattice correlation effects in the form of selfenergy and vertex corrections are systematically incorporated within a spinrotationallysymmetric scheme which explicitly preserves the goldstone mode and is therefore in accord with the merminwagner theorem interplay of band dispersion and correlation effects on ferromagneticstate stability are highlighted with respect to both long and shortwavelength fluctuations which are shown to have substantially different behaviour our approach provides a novel understanding of the enhancement of ferromagnetism near van hove filling for t05 in terms of strongly suppressed saddlepoint contribution to the destabilizing exchange part of spin stiffness finitetemperature electron spin dynamics is investigated directly in terms of spectralweight transfer across the fermi energy due to electronmagnon coupling relevant in the context of recent magnetization measurements on ultrathin films the role of strong thermal spin fluctuations in low dimensions is highlighted in the anisotropystabilized ordered state by determining the thermal decay of magnetization and t_c within a renormalized spinfluctuation theory
|
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|
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|
706.3089
|
Can Chandra resolve the remaining cosmic X-ray background?
|
The deepest extragalactic X-ray observation, the 2 Ms Chandra Deep Field
North (CDF-N), resolves ~80% of the total extragalactic cosmic X-ray background
(CXB) in the 1-2 keV band. Recent work has shown that 70% of the remaining CXB
flux is associated with sources detected by the Hubble Space Telescope (HST).
This paper uses the existing CDF-N data to constrain the X-ray flux
distribution of these X-ray undetected HST sources, by comparing the number of
0.5-2 keV X-ray counts at the HST positions to those expected for model flux
distributions. In the simple case where all the undetected HST X-ray sources
have the same 0.5-2 keV flux, the data are best fit by 1.5-3 counts per source
in 2 Ms, compared to a detection limit (at 10% completeness) of 9 counts.
Assuming a more realistic power-law logN-logS distribution [N(>S) S^-alpha],
the data favor a relatively steep flux distribution, with alpha=1.1^+0.5_-0.3
(limits are 99% confidence). This slope is very similar to that previously
found for faint normal and starburst galaxies in the CDF-N. These results
suggest deeper Chandra observations will detect a new population of faint X-ray
sources, but extremely deep exposures are needed to resolve the remainder of
the soft CXB. In the most optimistic scenario, when the HST sources have the
flattest allowed flux distribution and all the sources without HST counterparts
are detected, observations 5 times more sensitive than the existing ones would
resolve at most ~60% of the remaining soft CXB.
|
astro-ph
|
the deepest extragalactic xray observation the 2 ms chandra deep field north cdfn resolves 80 of the total extragalactic cosmic xray background cxb in the 12 kev band recent work has shown that 70 of the remaining cxb flux is associated with sources detected by the hubble space telescope hst this paper uses the existing cdfn data to constrain the xray flux distribution of these xray undetected hst sources by comparing the number of 052 kev xray counts at the hst positions to those expected for model flux distributions in the simple case where all the undetected hst xray sources have the same 052 kev flux the data are best fit by 153 counts per source in 2 ms compared to a detection limit at 10 completeness of 9 counts assuming a more realistic powerlaw lognlogs distribution ns salpha the data favor a relatively steep flux distribution with alpha1105_03 limits are 99 confidence this slope is very similar to that previously found for faint normal and starburst galaxies in the cdfn these results suggest deeper chandra observations will detect a new population of faint xray sources but extremely deep exposures are needed to resolve the remainder of the soft cxb in the most optimistic scenario when the hst sources have the flattest allowed flux distribution and all the sources without hst counterparts are detected observations 5 times more sensitive than the existing ones would resolve at most 60 of the remaining soft cxb
|
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|
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|
706.309
|
Flexible-to-semiflexible chain crossover on the pressure-area isotherm
of lipid bilayer
|
We found theoretically that competition between ~Kq^4 and ~Qq^2 terms in the
Fourier transformed conformational energy of a single lipid chain, in
combination with inter-chain entropic repulsion in the hydrophobic part of the
lipid (bi)layer, may cause a crossover on the bilayer pressure-area isotherm
P(A)~(A-A_0)^{-n}. The crossover manifests itself in the transition from n=5/3
to n=3. Our microscopic model represents a single lipid molecule as a worm-like
chain with finite irreducible cross-section area A_0, flexural rigidity K and
stretching modulus Q in a parabolic potential with self-consistent curvature
B(A) formed by entropic interactions between hydrocarbon chains in the lipid
layer. The crossover area per lipid A* obeys relation Q^2/(KB(A*))~1 . We
predict a peculiar possibility to deduce effective elastic moduli K and Q of
the individual hydrocarbon chain from the analysis of the isotherm possessing
such crossover. Also calculated is crossover-related behavior of the area
compressibility modulus K_a, equilibrium area per lipid A_t, and chain order
parameter S.
|
q-bio.QM q-bio.BM
|
we found theoretically that competition between kq4 and qq2 terms in the fourier transformed conformational energy of a single lipid chain in combination with interchain entropic repulsion in the hydrophobic part of the lipid bilayer may cause a crossover on the bilayer pressurearea isotherm paaa_0n the crossover manifests itself in the transition from n53 to n3 our microscopic model represents a single lipid molecule as a wormlike chain with finite irreducible crosssection area a_0 flexural rigidity k and stretching modulus q in a parabolic potential with selfconsistent curvature ba formed by entropic interactions between hydrocarbon chains in the lipid layer the crossover area per lipid a obeys relation q2kba1 we predict a peculiar possibility to deduce effective elastic moduli k and q of the individual hydrocarbon chain from the analysis of the isotherm possessing such crossover also calculated is crossoverrelated behavior of the area compressibility modulus k_a equilibrium area per lipid a_t and chain order parameter s
|
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|
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|
706.3091
|
On the well-posedness of the Cauchy problem for the generalized
Korteweg-de Vries-Burgers equation
|
Considered is the generalized Korteweg-de Vries-Burgers equation $$
u_{t}+u_{xxx}+uu_{x}+|D_{x}|^{2\alpha}u=0,\quad t\in \mathbb{R}^{+}, x\in
\mathbb{R}, $$ with $0\leq \alpha\le 1$. We prove a sharp results on the
associated Cauchy problem in the Sobolev space $ {H}^s(\mathbb{R})$. For
$s>-\min\{\frac {3+2\alpha}4, 1\}$ we give the well-posedness of solutions of
the Cauchy problem, while for $\frac 12\le\alpha\le 1$ and for $s<-\min\{\frac
{3+2\alpha}4, 1\}$ we show some ill-posedness issues.
|
math.AP
|
considered is the generalized kortewegde vriesburgers equation u_tu_xxxuu_xd_x2alphau0quad tin mathbbr xin mathbbr with 0leq alphale 1 we prove a sharp results on the associated cauchy problem in the sobolev space hsmathbbr for sminfrac 32alpha4 1 we give the wellposedness of solutions of the cauchy problem while for frac 12lealphale 1 and for sminfrac 32alpha4 1 we show some illposedness issues
|
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|
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|
706.3092
|
On $(2k)$-Minimal Submanifolds
|
Recall that a submanifold of a Riemannian manifold is said to be minimal if
its mean curvature is zero. It is classical that minimal submanifolds are the
critical points of the volume function. In this paper, we examine the critical
points of the total $(2k)$-th Gauss-Bonnet curvature function, called
$(2k)$-minimal submanifolds. We prove that they are characterized by the
vanishing of a higher mean curvature, namely the $(2k+1)$-Gauss-Bonnet
curvature. Furthermore, we show that several properties of usual minimal
submanifolds can be naturally generalized to $(2k)$-minimal submanifolds.
|
math.DG
|
recall that a submanifold of a riemannian manifold is said to be minimal if its mean curvature is zero it is classical that minimal submanifolds are the critical points of the volume function in this paper we examine the critical points of the total 2kth gaussbonnet curvature function called 2kminimal submanifolds we prove that they are characterized by the vanishing of a higher mean curvature namely the 2k1gaussbonnet curvature furthermore we show that several properties of usual minimal submanifolds can be naturally generalized to 2kminimal submanifolds
|
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|
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|
706.3093
|
Addendum: "On the nature of the phase transition in the itinerant
helimagnet MnSi", arXiv:cond-mat/0702460v1 [cond-mat.str-el]
|
New high resolution data for heat capacity, heat capacity under applied
magnetic fields and resistivity of high quality single crystal of MnSi are
reported. Striking mirror symmetry between temperature derivative of
resistivity and thermal expansion coefficient of MnSi is displayed. Close
similarity between variation of the heat capacity and the temperature
derivative of resistivity through the phase transition is observed. It is shown
that the heat capacity and thermal expansion coefficient of the helical phase
are not influenced by moderate magnetic field.
|
cond-mat.str-el
|
new high resolution data for heat capacity heat capacity under applied magnetic fields and resistivity of high quality single crystal of mnsi are reported striking mirror symmetry between temperature derivative of resistivity and thermal expansion coefficient of mnsi is displayed close similarity between variation of the heat capacity and the temperature derivative of resistivity through the phase transition is observed it is shown that the heat capacity and thermal expansion coefficient of the helical phase are not influenced by moderate magnetic field
|
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|
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|
706.3094
|
Direct-current control of radiation-induced differential
magnetoresistance oscillations in two-dimensional electron systems
|
Magnetoresistance oscillations in two-dimensional electron systems driven
simultaneously by a strong direct current and a microwave irradiation, are
analyzed within a unified microscopic scheme treating both excitations on an
equal footing. The microwave-induced resistance oscillations are described by a
parameter $\epsilon_\omega$ proportional to the radiation frequency, while the
dc-induced resistance oscillations are governed by a parameter $\epsilon_j$
proportional to the current density. In the presence of both a microwave
radiation and a strong dc, the combined parameter $\epsilon_\omega+\epsilon_j$
is shown to control the main resistance oscillations, in agreement with the
recent measurement [Zhang {\it et al.} Phys. Rev. Lett. {\bf 98}, 106804
(2007)]
|
cond-mat.mes-hall
|
magnetoresistance oscillations in twodimensional electron systems driven simultaneously by a strong direct current and a microwave irradiation are analyzed within a unified microscopic scheme treating both excitations on an equal footing the microwaveinduced resistance oscillations are described by a parameter epsilon_omega proportional to the radiation frequency while the dcinduced resistance oscillations are governed by a parameter epsilon_j proportional to the current density in the presence of both a microwave radiation and a strong dc the combined parameter epsilon_omegaepsilon_j is shown to control the main resistance oscillations in agreement with the recent measurement zhang it et al phys rev lett bf 98 106804 2007
|
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|
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|
706.3095
|
Channeling Effect and Improvement of the Efficiency of Charged Particle
Registration with Crystal Scintillators
|
The importance is emphasized of taking into account the channeling along the
low index crystallographic axes and planes of a part of low-energy (1-10 keV)
recoil ions in measurements of their parameters with crystal scintillators of
the type of NaI(Tl) etc. Because the nucleus stopping power in channels is low
as compared with electronic stopping power, the light yield of the scintillator
must be, accordingly, higher in the given case than that for ions having higher
energy (tens keV and more), which lose most part of their energy via nuclear
collisions outside channels. Hence, in particular, it follows that the DAMA/NaI
observations in Gran Sasso of the annual modulation of the signal frequency in
a narrow range of scintillations with an amplitude of 2-6 keV electron
equivalent may be due to incidence onto the Earth of exceedingly massive
particles (of the type of Planckian objects) from elongated Earth-crossing
heliocentric orbits at a velocity of 30-50 km/s. In NaI(Tl), these particles
create the iodine recoil ions with just the energy of 2-6 keV.
|
physics.ins-det hep-ph
|
the importance is emphasized of taking into account the channeling along the low index crystallographic axes and planes of a part of lowenergy 110 kev recoil ions in measurements of their parameters with crystal scintillators of the type of naitl etc because the nucleus stopping power in channels is low as compared with electronic stopping power the light yield of the scintillator must be accordingly higher in the given case than that for ions having higher energy tens kev and more which lose most part of their energy via nuclear collisions outside channels hence in particular it follows that the damanai observations in gran sasso of the annual modulation of the signal frequency in a narrow range of scintillations with an amplitude of 26 kev electron equivalent may be due to incidence onto the earth of exceedingly massive particles of the type of planckian objects from elongated earthcrossing heliocentric orbits at a velocity of 3050 kms in naitl these particles create the iodine recoil ions with just the energy of 26 kev
|
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|
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|
706.3096
|
The frequency separations of stellar p-modes
|
Aims. The purpose of this work is to investigate a new frequency separation
of stellar p-modes and its characteristics. Methods. Frequency separations are
deduced from the asymptotic formula of stellar p-modes. Then, using the
theoretical adiabatic frequencies of stellar model, we compute the frequency
separations. Results. A new separation $\sigma_{l-1 l+1}(n)$, which is similar
to the scaled small separation $d_{l l+2}(n)/(2l+3)$, is obtained from the
asymptotic formula of stellar p-modes. The separations $\sigma_{l-1 l+1}(n)$
and $d_{l l+2}(n)/(2l+3)$ have the same order. And like the small separation,
$\sigma_{l-1 l+1}(n)$ is mainly sensitive to the conditions in the stellar
core. However, with the decrease of the central hydrogen abundance of stars,
the $\sigma_{02}$ and $\sigma_{13}$ more and more deviate from the scaled small
separation. This characteristic could be used to extract the information on the
central hydrogen abundance of stars.
|
gr-qc
|
aims the purpose of this work is to investigate a new frequency separation of stellar pmodes and its characteristics methods frequency separations are deduced from the asymptotic formula of stellar pmodes then using the theoretical adiabatic frequencies of stellar model we compute the frequency separations results a new separation sigma_l1 l1n which is similar to the scaled small separation d_l l2n2l3 is obtained from the asymptotic formula of stellar pmodes the separations sigma_l1 l1n and d_l l2n2l3 have the same order and like the small separation sigma_l1 l1n is mainly sensitive to the conditions in the stellar core however with the decrease of the central hydrogen abundance of stars the sigma_02 and sigma_13 more and more deviate from the scaled small separation this characteristic could be used to extract the information on the central hydrogen abundance of stars
|
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|
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|
706.3097
|
The nature of the fluorescent iron line in V 1486 Ori
|
The fluorescent 6.4 keV iron line provides information on cool material in
the vicinity of hard X-ray sources as well as on the characteristics of the
X-ray sources themselves. First discovered in the X-ray spectra of the flaring
Sun, X-ray binaries and active galactic nuclei (AGN), the fluorescent line was
also observed in a number of stellar X-ray sources. The young stellar object
(YSO) V1486 Ori was observed in the framework of the Chandra Ultra Deep Project
(COUP) as the source COUP 331. We investigate its spectrum, with emphasis on
the strength and time variability of the fluorescent iron K-alpha line, derive
and analyze the light curve of COUP 331 and proceed with a time-resolved
spectral analysis of the observation. The light curve of V 1486 Ori shows two
major flares, the first one lasting for (approx) 20 ks with a peak X-ray
luminosity of 2.6*10^{32} erg/s (dereddened in the 1-10 keV band) and the
second one -- only partially observed -- for >60 ks with an average X-ray
luminosity of 2.4*10^{31} erg/s (dereddened). The spectrum of the first flare
is very well described by an absorbed thermal model at high temperature, with a
pronounced 6.7 keV iron line complex, but without any fluorescent K-alpha line.
The X-ray spectrum of the second flare is characterized by even higher
temperatures (>= 10 keV) without any detectable 6.7 keV Fe XXV feature, but
with a very strong fluorescent iron K-alpha line appearing predominantly in the
20 ks rise phase of the flare. Preliminary model calculations indicate that
photoionization is unlikely to account for the entire fluorescent emission
during the rise phase.
|
astro-ph
|
the fluorescent 64 kev iron line provides information on cool material in the vicinity of hard xray sources as well as on the characteristics of the xray sources themselves first discovered in the xray spectra of the flaring sun xray binaries and active galactic nuclei agn the fluorescent line was also observed in a number of stellar xray sources the young stellar object yso v1486 ori was observed in the framework of the chandra ultra deep project coup as the source coup 331 we investigate its spectrum with emphasis on the strength and time variability of the fluorescent iron kalpha line derive and analyze the light curve of coup 331 and proceed with a timeresolved spectral analysis of the observation the light curve of v 1486 ori shows two major flares the first one lasting for approx 20 ks with a peak xray luminosity of 261032 ergs dereddened in the 110 kev band and the second one only partially observed for 60 ks with an average xray luminosity of 241031 ergs dereddened the spectrum of the first flare is very well described by an absorbed thermal model at high temperature with a pronounced 67 kev iron line complex but without any fluorescent kalpha line the xray spectrum of the second flare is characterized by even higher temperatures 10 kev without any detectable 67 kev fe xxv feature but with a very strong fluorescent iron kalpha line appearing predominantly in the 20 ks rise phase of the flare preliminary model calculations indicate that photoionization is unlikely to account for the entire fluorescent emission during the rise phase
|
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|
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|
706.3098
|
Bayesian analysis of joint strong gravitational lensing and dynamic
galactic mass in SLACS: evidence of line-of-sight contamination
|
We readdress the calculation of the mass of early-type galaxies using strong
gravitational lensing and stellar dynamics. Our sample comprises 27 galaxies in
the Sloan Lens ACS (SLACS) Survey. Comparing the mass estimates from these two
independent methods in a Bayesian framework, we find evidence of significant
line-of-sight mass contamination. Assuming a power-law mass distribution, the
best fit density profile is given by $\rho \propto r^{-1.69\pm0.05}$. We show
that neglecting the line-of-sight mass contamination produces an overestimate
of the mass attributed to the lens-galaxy by the lensing method, which
introduces a bias in favor of a SIS profile when using the joint lensing and
dynamic analysis to determine the slope of the density profile. We suggest that
the line-of-sight contamination could also be important for other astrophysical
and cosmological uses of joint lensing and dynamical measurements.
|
astro-ph
|
we readdress the calculation of the mass of earlytype galaxies using strong gravitational lensing and stellar dynamics our sample comprises 27 galaxies in the sloan lens acs slacs survey comparing the mass estimates from these two independent methods in a bayesian framework we find evidence of significant lineofsight mass contamination assuming a powerlaw mass distribution the best fit density profile is given by rho propto r169pm005 we show that neglecting the lineofsight mass contamination produces an overestimate of the mass attributed to the lensgalaxy by the lensing method which introduces a bias in favor of a sis profile when using the joint lensing and dynamic analysis to determine the slope of the density profile we suggest that the lineofsight contamination could also be important for other astrophysical and cosmological uses of joint lensing and dynamical measurements
|
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|
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|
706.3099
|
An Improved Process for Fabricating High-Mobility Organic Molecular
Crystal Field-Effect Transistors
|
In this paper we present an improved process for producing elastomer
transistor stamps and high-mobility organic field-effect transistors (FETs)
based on semiconducting acene molecular crystals. In particular, we have
removed the need to use a silanized Si wafer for curing the stamps and to
handle a fragile micron-thickness polydimethylsiloxane (PDMS) insulating film
and laminate it, bubble free, against the PDMS transistor stamp. We find that
despite the altered design, rougher PDMS surface, and lamination and
measurement of the device in air, we still achieve electrical mobilities of
order 10 cm^2/Vs, comparable to the current state of the art in organic FETs.
Our device shows hole conduction with a threshold voltage of order -9V, which
corresponds to a trap density of 1.4 x 10^10 cm^-2.
|
cond-mat.soft cond-mat.mtrl-sci
|
in this paper we present an improved process for producing elastomer transistor stamps and highmobility organic fieldeffect transistors fets based on semiconducting acene molecular crystals in particular we have removed the need to use a silanized si wafer for curing the stamps and to handle a fragile micronthickness polydimethylsiloxane pdms insulating film and laminate it bubble free against the pdms transistor stamp we find that despite the altered design rougher pdms surface and lamination and measurement of the device in air we still achieve electrical mobilities of order 10 cm2vs comparable to the current state of the art in organic fets our device shows hole conduction with a threshold voltage of order 9v which corresponds to a trap density of 14 x 1010 cm2
|
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|
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|
706.31
|
Cooling a Micromechanical Beam by Coupling it to a Transmission Line
|
We study a method to cool down the vibration mode of a micro-mechanical beam
using a capacitively-coupled superconducting transmission line. The Coulomb
force between the transmission line and the beam is determined by the driving
microwave on the transmission line and the displacement of the beam. When the
frequency of the driving microwave is smaller than that of the transmission
line resonator, the Coulomb force can oppose the velocity of the beam. Thus,
the beam can be cooled. This mechanism, which may enable to prepare the beam in
its quantum ground state of vibration, is feasible under current experimental
conditions.
|
cond-mat.mes-hall cond-mat.supr-con
|
we study a method to cool down the vibration mode of a micromechanical beam using a capacitivelycoupled superconducting transmission line the coulomb force between the transmission line and the beam is determined by the driving microwave on the transmission line and the displacement of the beam when the frequency of the driving microwave is smaller than that of the transmission line resonator the coulomb force can oppose the velocity of the beam thus the beam can be cooled this mechanism which may enable to prepare the beam in its quantum ground state of vibration is feasible under current experimental conditions
|
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|
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|
706.3101
|
The Penna Model of Biological Aging
|
This review deals with computer simulation of biological ageing, particularly
with the Penna model of 1995.
|
q-bio.PE
|
this review deals with computer simulation of biological ageing particularly with the penna model of 1995
|
[['this', 'review', 'deals', 'with', 'computer', 'simulation', 'of', 'biological', 'ageing', 'particularly', 'with', 'the', 'penna', 'model', 'of', '1995']]
|
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|
706.3102
|
Complete Hamiltonian description of wave-like features in classical and
quantum physics
|
The analysis of the Helmholtz equation is shown to lead to an exact
Hamiltonian system of equations describing in terms of ray trajectories a very
wide family of wave-like phenomena (including diffraction and interference)
going much beyond the limits of the ordinary geometrical optics approximation,
which is contained as a simple limiting case. Due to the fact that the time
independent Schroedinger equation is itself a Helmoltz-like equation, the same
mathematical solutions holding for a classical optical beam turn out to apply
to a quantum particle beam, leading to a complete system of Hamiltonian
equations which provide a set of particle trajectories and motion laws
containing as a limiting case the ones encountered in classical Mechanics.
|
quant-ph
|
the analysis of the helmholtz equation is shown to lead to an exact hamiltonian system of equations describing in terms of ray trajectories a very wide family of wavelike phenomena including diffraction and interference going much beyond the limits of the ordinary geometrical optics approximation which is contained as a simple limiting case due to the fact that the time independent schroedinger equation is itself a helmoltzlike equation the same mathematical solutions holding for a classical optical beam turn out to apply to a quantum particle beam leading to a complete system of hamiltonian equations which provide a set of particle trajectories and motion laws containing as a limiting case the ones encountered in classical mechanics
|
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|
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|
706.3103
|
Production of high energy particles in laser and Coulomb fields and
e^+e^- antenna
|
A strong laser field and the Coulomb field of a nucleus can produce
e^{+}e^{-} pairs. It is shown for the first time that there is a large
probability that electrons and positrons created in this process collide after
one or several oscillations of the laser field. These collisions can take place
at high energy resulting in several phenomena. The quasielastic collision
e^{+}e^{-} -> e^{+}e^{-} allows acceleration of leptons in the laser field to
higher energies. The inelastic collisions allow production of high energy
photons e^{+}e^{-}-> 2 gamma and muons, e^{+}e^{-} -> mu^{+}mu^{-}. The yield
of high-energy photons and muons produced via this mechanism exceeds
exponentially their production through conventional direct creation in laser
and Coulomb fields. A relation of the phenomena considered with the
antenna-mechanism of multiphoton absorption in atoms is discussed.
|
physics.atom-ph
|
a strong laser field and the coulomb field of a nucleus can produce ee pairs it is shown for the first time that there is a large probability that electrons and positrons created in this process collide after one or several oscillations of the laser field these collisions can take place at high energy resulting in several phenomena the quasielastic collision ee ee allows acceleration of leptons in the laser field to higher energies the inelastic collisions allow production of high energy photons ee 2 gamma and muons ee mumu the yield of highenergy photons and muons produced via this mechanism exceeds exponentially their production through conventional direct creation in laser and coulomb fields a relation of the phenomena considered with the antennamechanism of multiphoton absorption in atoms is discussed
|
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|
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|
706.3104
|
Group Testing with Random Pools: optimal two-stage algorithms
|
We study Probabilistic Group Testing of a set of N items each of which is
defective with probability p. We focus on the double limit of small defect
probability, p<<1, and large number of variables, N>>1, taking either p->0
after $N\to\infty$ or $p=1/N^{\beta}$ with $\beta\in(0,1/2)$. In both settings
the optimal number of tests which are required to identify with certainty the
defectives via a two-stage procedure, $\bar T(N,p)$, is known to scale as
$Np|\log p|$. Here we determine the sharp asymptotic value of $\bar
T(N,p)/(Np|\log p|)$ and construct a class of two-stage algorithms over which
this optimal value is attained. This is done by choosing a proper bipartite
regular graph (of tests and variable nodes) for the first stage of the
detection. Furthermore we prove that this optimal value is also attained on
average over a random bipartite graph where all variables have the same degree,
while the tests have Poisson-distributed degrees. Finally, we improve the
existing upper and lower bound for the optimal number of tests in the case
$p=1/N^{\beta}$ with $\beta\in[1/2,1)$.
|
cs.DS cond-mat.dis-nn cond-mat.stat-mech cs.IT math.IT
|
we study probabilistic group testing of a set of n items each of which is defective with probability p we focus on the double limit of small defect probability p1 and large number of variables n1 taking either p0 after ntoinfty or p1nbeta with betain012 in both settings the optimal number of tests which are required to identify with certainty the defectives via a twostage procedure bar tnp is known to scale as nplog p here we determine the sharp asymptotic value of bar tnpnplog p and construct a class of twostage algorithms over which this optimal value is attained this is done by choosing a proper bipartite regular graph of tests and variable nodes for the first stage of the detection furthermore we prove that this optimal value is also attained on average over a random bipartite graph where all variables have the same degree while the tests have poissondistributed degrees finally we improve the existing upper and lower bound for the optimal number of tests in the case p1nbeta with betain121
|
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|
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|
706.3105
|
Hadronic Final States
|
In this summary we give a concise overview of the experimental and
theoretical results, which were presented during the QCD and Hadronic Final
State Working Group sessions at the DIS 2007 workshop.
|
hep-ph
|
in this summary we give a concise overview of the experimental and theoretical results which were presented during the qcd and hadronic final state working group sessions at the dis 2007 workshop
|
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|
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|
706.3106
|
Tuning the domain wall orientation in thin magnetic strips by induced
anisotropy
|
We report on a method to tune the orientation of in-plane magnetic domains
and domain walls in thin ferromagnetic strips by manipulating the magnetic
anisotropy. Uniaxial in-plane anisotropy is induced in a controlled way by
oblique evaporation of magnetic thin strips. A direct correlation between the
magnetization direction and the domain wall orientation is found experimentally
and confirmed by micromagnetic simulations. The domain walls in the strips are
always oriented along the oblique evaporation-induced easy axis, in spite of
the shape anisotropy. The controlled manipulation of domain wall orientations
could open new possibilities for novel devices based on domain-wall
propagation.
|
cond-mat.other
|
we report on a method to tune the orientation of inplane magnetic domains and domain walls in thin ferromagnetic strips by manipulating the magnetic anisotropy uniaxial inplane anisotropy is induced in a controlled way by oblique evaporation of magnetic thin strips a direct correlation between the magnetization direction and the domain wall orientation is found experimentally and confirmed by micromagnetic simulations the domain walls in the strips are always oriented along the oblique evaporationinduced easy axis in spite of the shape anisotropy the controlled manipulation of domain wall orientations could open new possibilities for novel devices based on domainwall propagation
|
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|
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|
706.3107
|
Spinorial Characterization of Surfaces into 3-dimensional homogeneous
Manifolds
|
We give a spinorial characterization of isometrically immersed surfaces into
3-dimensional homogeneous manifolds with 4-dimensional isometry group in terms
of the existence of a particular spinor, called generalized Killing spinor.
This generalizes results by T. Friedrich for $\R^3$ and B. Morel for $\Ss^3$
and $\HH^3$. The main argument is the interpretation of the energy-momentum
tensor of a genralized Killing spinor as the second fondamental form up to a
tensor depending on the structure of the ambient space
|
math.DG
|
we give a spinorial characterization of isometrically immersed surfaces into 3dimensional homogeneous manifolds with 4dimensional isometry group in terms of the existence of a particular spinor called generalized killing spinor this generalizes results by t friedrich for r3 and b morel for ss3 and hh3 the main argument is the interpretation of the energymomentum tensor of a genralized killing spinor as the second fondamental form up to a tensor depending on the structure of the ambient space
|
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|
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|
706.3108
|
Mapped Chebyshev pseudospectral method to study multiple scale phenomena
|
In the framework of mapped pseudospectral methods, we introduce a new
polynomial-type mapping function in order to describe accurately the dynamics
of systems developing almost singular structures. Using error criteria related
to the spectral interpolation error, the new polynomial-type mapping is
compared against previously proposed mappings for the study of collapse and
shock wave phenomena. As a physical application, we study the dynamics of two
coupled beams, described by coupled nonlinear Schr\"odinger equations and
modeling beam propagation in an atomic coherent media, whose spatial sizes
differs up to several orders of magnitude. It is demonstrated, also by
numerical simulations, that the accuracy properties of the new polynomial-type
mapping outperforms in orders of magnitude the ones of the other studied
mapping functions.
|
physics.comp-ph physics.optics
|
in the framework of mapped pseudospectral methods we introduce a new polynomialtype mapping function in order to describe accurately the dynamics of systems developing almost singular structures using error criteria related to the spectral interpolation error the new polynomialtype mapping is compared against previously proposed mappings for the study of collapse and shock wave phenomena as a physical application we study the dynamics of two coupled beams described by coupled nonlinear schrodinger equations and modeling beam propagation in an atomic coherent media whose spatial sizes differs up to several orders of magnitude it is demonstrated also by numerical simulations that the accuracy properties of the new polynomialtype mapping outperforms in orders of magnitude the ones of the other studied mapping functions
|
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|
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|
706.3109
|
Itinerant ferromagnetism in the multiorbital Hubbard model: a dynamical
mean-field study
|
In order to resolve the long-standing issue of how the itinerant
ferromagnetism is affected by the lattice structure and Hund's coupling, we
have compared various three-dimensional lattice structures in the single- and
multiorbital Hubbard models with the dynamical mean-field theory with an
improved quantum Monte Carlo algorithm that preserves the spin-SU(2) symmetry.
The result indicates that {\it both} the lattice structure and the d-orbital
degeneracy are essential for the ferromagnetism in the parameter region
representing a transition metal. Specifically, (a) Hund's coupling, despite the
common belief, is important, which is here identified to come from
particle-hole scatterings, and (b) the ferromagnetism is a correlation effect
(outside the Stoner picture) as indicated from the band-filling dependence.
|
cond-mat.str-el
|
in order to resolve the longstanding issue of how the itinerant ferromagnetism is affected by the lattice structure and hunds coupling we have compared various threedimensional lattice structures in the single and multiorbital hubbard models with the dynamical meanfield theory with an improved quantum monte carlo algorithm that preserves the spinsu2 symmetry the result indicates that it both the lattice structure and the dorbital degeneracy are essential for the ferromagnetism in the parameter region representing a transition metal specifically a hunds coupling despite the common belief is important which is here identified to come from particlehole scatterings and b the ferromagnetism is a correlation effect outside the stoner picture as indicated from the bandfilling dependence
|
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|
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|
706.311
|
Interstellar Dust in the Solar System
|
The Ulysses spacecraft has been orbiting the Sun on a highly inclined ellipse
almost perpendicular to the ecliptic plane (inclination 79 deg, perihelion
distance 1.3 AU, aphelion distance 5.4 AU) since it encountered Jupiter in
1992. The in-situ dust detector on board continuously measured interstellar
dust grains with masses up to 10^-13 kg, penetrating deep into the solar
system. The flow direction is close to the mean apex of the Sun's motion
through the solar system and the grains act as tracers of the physical
conditions in the local interstellar cloud (LIC). While Ulysses monitored the
interstellar dust stream at high ecliptic latitudes between 3 and 5 AU,
interstellar impactors were also measured with the in-situ dust detectors on
board Cassini, Galileo and Helios, covering a heliocentric distance range
between 0.3 and 3 AU in the ecliptic plane. The interstellar dust stream in the
inner solar system is altered by the solar radiation pressure force,
gravitational focussing and interaction of charged grains with the time varying
interplanetary magnetic field. We review the results from in-situ interstellar
dust measurements in the solar system and present Ulysses' latest interstellar
dust data. These data indicate a 30 deg shift in the impact direction of
interstellar grains w.r.t. the interstellar helium flow direction, the reason
of which is presently unknown.
|
astro-ph
|
the ulysses spacecraft has been orbiting the sun on a highly inclined ellipse almost perpendicular to the ecliptic plane inclination 79 deg perihelion distance 13 au aphelion distance 54 au since it encountered jupiter in 1992 the insitu dust detector on board continuously measured interstellar dust grains with masses up to 1013 kg penetrating deep into the solar system the flow direction is close to the mean apex of the suns motion through the solar system and the grains act as tracers of the physical conditions in the local interstellar cloud lic while ulysses monitored the interstellar dust stream at high ecliptic latitudes between 3 and 5 au interstellar impactors were also measured with the insitu dust detectors on board cassini galileo and helios covering a heliocentric distance range between 03 and 3 au in the ecliptic plane the interstellar dust stream in the inner solar system is altered by the solar radiation pressure force gravitational focussing and interaction of charged grains with the time varying interplanetary magnetic field we review the results from insitu interstellar dust measurements in the solar system and present ulysses latest interstellar dust data these data indicate a 30 deg shift in the impact direction of interstellar grains wrt the interstellar helium flow direction the reason of which is presently unknown
|
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|
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|
706.3111
|
Wave-front engineering by Huygens-Fresnel principle for nonlinear
optical interactions in domain engineered structures
|
The wave-front engineering for nonlinear optical interactions was discussed.
Using Huygens-Fresnel principle we developed a general theory and technique for
domain engineering with conventional quasi-phase-matching structures being the
special cases. By Fourier analysis we put forward the concept of local
quasi-phase matching, which suggests that the quasi-phase matching is fulfilled
only locally not globally. Experiments on focal effect of second-harmonic wave
agreed well with the theoretical prediction. The proposed scheme combines three
optical functions: generation, focusing and beam splitting of second-harmonic
wave, thus making the device more compact. Further the proposed scheme can be
used to perform the integration of multi-functional optical properties in
nonlinear photonics, as well as expand the use of nonlinear optical devices.
|
physics.optics
|
the wavefront engineering for nonlinear optical interactions was discussed using huygensfresnel principle we developed a general theory and technique for domain engineering with conventional quasiphasematching structures being the special cases by fourier analysis we put forward the concept of local quasiphase matching which suggests that the quasiphase matching is fulfilled only locally not globally experiments on focal effect of secondharmonic wave agreed well with the theoretical prediction the proposed scheme combines three optical functions generation focusing and beam splitting of secondharmonic wave thus making the device more compact further the proposed scheme can be used to perform the integration of multifunctional optical properties in nonlinear photonics as well as expand the use of nonlinear optical devices
|
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|
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|
706.3112
|
Almost-Commutative Geometries Beyond the Standard Model III: Vector
Doublets
|
We will present a new extension of the standard model of particle physics in
its almostcommutative formulation. This extension has as its basis the algebra
of the standard model with four summands [11], and enlarges only the particle
content by an arbitrary number of generations of left-right symmetric doublets
which couple vectorially to the U(1)_YxSU(2)_w subgroup of the standard model.
As in the model presented in [8], which introduced particles with a new colour,
grand unification is no longer required by the spectral action. The new model
may also possess a candidate for dark matter in the hundred TeV mass range with
neutrino-like cross section.
|
hep-th
|
we will present a new extension of the standard model of particle physics in its almostcommutative formulation this extension has as its basis the algebra of the standard model with four summands 11 and enlarges only the particle content by an arbitrary number of generations of leftright symmetric doublets which couple vectorially to the u1_yxsu2_w subgroup of the standard model as in the model presented in 8 which introduced particles with a new colour grand unification is no longer required by the spectral action the new model may also possess a candidate for dark matter in the hundred tev mass range with neutrinolike cross section
|
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|
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|
706.3113
|
Bursty stellar populations and obscured AGN in galaxy bulges
|
[Abridged] We investigate trends between the recent star formation history
and black hole growth in galaxy bulges in the Sloan Digital Sky Survey (SDSS).
The galaxies lie at 0.01<z<0.07 where the fibre aperture covers only the
central 0.6-4.0kpc diameter of the galaxy. We find strong trends between black
hole growth, as measured by dust-attenuation-corrected OIII luminosity, and the
recent star formation history of the bulges. We conclude that our results
support the popular hypothesis for black hole growth occurring through gas
inflow into the central regions of galaxies, followed by a starburst and
triggering of the AGN. However, while this is a significant pathway for the
growth of black holes, it is not the dominant one in the present-day Universe.
More unspectacular processes are apparently responsible for the majority of
this growth.
In order to arrive at these conclusions we have developed a set of new high
signal-to-noise ratio (SNR) optical spectral indicators, designed to allow a
detailed study of stellar populations which have undergone recent enhanced star
formation. Working in the rest-frame wavelength range 3750-4150AA, ideally
suited to many recent and ongoing spectroscopic surveys at low and high
redshift, the first two indices are equivalent to the previously well studied
4000AA break strength and Hdelta equivalent width. The primary advantage of
this new method is a greatly improved SNR for the latter index, allowing the
present study to use spectra with SNR-per-pixel as low as 8.
|
astro-ph
|
abridged we investigate trends between the recent star formation history and black hole growth in galaxy bulges in the sloan digital sky survey sdss the galaxies lie at 001z007 where the fibre aperture covers only the central 0640kpc diameter of the galaxy we find strong trends between black hole growth as measured by dustattenuationcorrected oiii luminosity and the recent star formation history of the bulges we conclude that our results support the popular hypothesis for black hole growth occurring through gas inflow into the central regions of galaxies followed by a starburst and triggering of the agn however while this is a significant pathway for the growth of black holes it is not the dominant one in the presentday universe more unspectacular processes are apparently responsible for the majority of this growth in order to arrive at these conclusions we have developed a set of new high signaltonoise ratio snr optical spectral indicators designed to allow a detailed study of stellar populations which have undergone recent enhanced star formation working in the restframe wavelength range 37504150aa ideally suited to many recent and ongoing spectroscopic surveys at low and high redshift the first two indices are equivalent to the previously well studied 4000aa break strength and hdelta equivalent width the primary advantage of this new method is a greatly improved snr for the latter index allowing the present study to use spectra with snrperpixel as low as 8
|
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|
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|
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