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707.083
|
A New Look at Mode Conversion in a Stratified Isothermal Atmosphere
|
Recent numerical investigations of wave propagation near coronal magnetic
null points (McLaughlin and Hood: Astron. Astrophys. 459, 641,2006) have
indicated how a fast MHD wave partially converts into a slow MHD wave as the
disturbance passes from a low-beta plasma to a high-beta plasma. This is a
complex process and a clear understanding of the conversion mechanism requires
the detailed investigation of a simpler model. An investigation of mode
conversion in a stratified, isothermal atmosphere, with a uniform, vertical
magnetic field is carried out, both numerically and analytically. In contrast
to previous investigations of upward-propagating waves (Zhugzhda and Dzhalilov:
Astron. Astrophys. 112, 16, 1982a; Cally: Astrophys. J. 548, 473, 2001), this
paper studies the downward propagation of waves from a low-beta to high-beta
environment. A simple expression for the amplitude of the transmitted wave is
compared with the numerical solution.
|
astro-ph
|
recent numerical investigations of wave propagation near coronal magnetic null points mclaughlin and hood astron astrophys 459 6412006 have indicated how a fast mhd wave partially converts into a slow mhd wave as the disturbance passes from a lowbeta plasma to a highbeta plasma this is a complex process and a clear understanding of the conversion mechanism requires the detailed investigation of a simpler model an investigation of mode conversion in a stratified isothermal atmosphere with a uniform vertical magnetic field is carried out both numerically and analytically in contrast to previous investigations of upwardpropagating waves zhugzhda and dzhalilov astron astrophys 112 16 1982a cally astrophys j 548 473 2001 this paper studies the downward propagation of waves from a lowbeta to highbeta environment a simple expression for the amplitude of the transmitted wave is compared with the numerical solution
|
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|
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|
707.0831
|
Half-space theorem, embedded minimal annuli and minimal graphs in the
Heisenberg group
|
We construct a one-parameter family of properly embedded minimal annuli in
the Heisenberg group Nil_3 endowed with a left-invariant Riemannian metric.
These annuli are not rotationally invariant. This family gives a vertical
half-space theorem and proves that each complete minimal graph in Nil_3 is
entire. Also, the sister surface of an entire minimal graph in Nil_3 is an
entire constant mean curvature 1/2 graph in H^2 x R, and conversely. This gives
a classification of all entire constant mean curvature 1/2 graphs in H^2 x R.
Finally we construct properly embedded constant mean curvature 1/2 annuli in
H^2 x R.
|
math.DG
|
we construct a oneparameter family of properly embedded minimal annuli in the heisenberg group nil_3 endowed with a leftinvariant riemannian metric these annuli are not rotationally invariant this family gives a vertical halfspace theorem and proves that each complete minimal graph in nil_3 is entire also the sister surface of an entire minimal graph in nil_3 is an entire constant mean curvature 12 graph in h2 x r and conversely this gives a classification of all entire constant mean curvature 12 graphs in h2 x r finally we construct properly embedded constant mean curvature 12 annuli in h2 x r
|
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|
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|
707.0832
|
HESS J1616-508: likely powered by PSR J1617-5055
|
HESS J1616-508 is one of the brightest emitters in the TeV sky. Recent
observations with the IBIS/ISGRI telescope on board the INTEGRAL spacecraft
have revealed that a young, nearby and energetic pulsar, PSR J1617-5055, is a
powerful emitter of soft gamma-rays in the 20-100 keV domain. In this paper we
present an analysis of all available data from the INTEGRAL, Swift, BeppoSAX
and XMM-Newton telescopes with a view to assessing the most likely counterpart
to the HESS source. We find that the energy source that fuels the X/gamma-ray
emissions is derived from the pulsar, both on the basis of the positional
morphology, the timing evidence and the energetics of the system. Likewise, the
1.2% of the pulsar's spin down energy loss needed to power the 0.1-10 TeV
emission is also fully consistent with other HESS sources known to be
associated with pulsars. The relative sizes of the X/gamma-ray and VHE sources
are consistent with the expected lifetimes against synchrotron and Compton
losses for a single source of parent electrons emitted from the pulsar. We find
that no other known object in the vicinity could be reasonably considered as a
plausible counterpart to the HESS source. We conclude that there is good
evidence to assume that the HESS J1616-508 source is driven by PSR J1617-5055
in which a combination of synchrotron and inverse Compton processes combine to
create the observed morphology of a broad-band emitter from keV to TeV
energies.
|
astro-ph
|
hess j1616508 is one of the brightest emitters in the tev sky recent observations with the ibisisgri telescope on board the integral spacecraft have revealed that a young nearby and energetic pulsar psr j16175055 is a powerful emitter of soft gammarays in the 20100 kev domain in this paper we present an analysis of all available data from the integral swift bepposax and xmmnewton telescopes with a view to assessing the most likely counterpart to the hess source we find that the energy source that fuels the xgammaray emissions is derived from the pulsar both on the basis of the positional morphology the timing evidence and the energetics of the system likewise the 12 of the pulsars spin down energy loss needed to power the 0110 tev emission is also fully consistent with other hess sources known to be associated with pulsars the relative sizes of the xgammaray and vhe sources are consistent with the expected lifetimes against synchrotron and compton losses for a single source of parent electrons emitted from the pulsar we find that no other known object in the vicinity could be reasonably considered as a plausible counterpart to the hess source we conclude that there is good evidence to assume that the hess j1616508 source is driven by psr j16175055 in which a combination of synchrotron and inverse compton processes combine to create the observed morphology of a broadband emitter from kev to tev energies
|
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|
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|
707.0833
|
Kirzhnits gradient expansion for a D-dimensional Fermi gas
|
For an ideal D-dimensional Fermi gas under generic external confinement we
derive the correcting coefficient $(D-2)/3D$ of the von Weizsacker term in the
kinetic energy density. To obtain this coefficient we use the Kirzhnits
semiclassical expansion of the number operator up to the second order in the
Planck constant $\hbar$. Within this simple and direct approach we determine
the differential equation of the density profile and the density functional of
the Fermi gas. In the case D=2 we find that the Kirzhnits gradient corrections
vanish to all order in $\hbar$.
|
cond-mat.stat-mech cond-mat.other
|
for an ideal ddimensional fermi gas under generic external confinement we derive the correcting coefficient d23d of the von weizsacker term in the kinetic energy density to obtain this coefficient we use the kirzhnits semiclassical expansion of the number operator up to the second order in the planck constant hbar within this simple and direct approach we determine the differential equation of the density profile and the density functional of the fermi gas in the case d2 we find that the kirzhnits gradient corrections vanish to all order in hbar
|
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|
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|
707.0834
|
Interaction, Change, and Wholeness of Material Things
|
Interaction is the mode of being of material things amid other material
things and the driving force of change and wholeness. Through mutual influence,
changes of interacting things become interdependent and their properties
interrelated, which leads to formation of ensembles - material wholes of
correlated things, where the mode of being of a particular component depends on
the modes of being of all other components and vice versa. Every ensemble
attains its wholeness and becomes a physical body through togetherness of
interrelated components coexisting as a collective being with mutually
restrained internal motion. Properties of ensembles on all structural levels of
matter composition emerge through the collective being of components.
|
physics.gen-ph
|
interaction is the mode of being of material things amid other material things and the driving force of change and wholeness through mutual influence changes of interacting things become interdependent and their properties interrelated which leads to formation of ensembles material wholes of correlated things where the mode of being of a particular component depends on the modes of being of all other components and vice versa every ensemble attains its wholeness and becomes a physical body through togetherness of interrelated components coexisting as a collective being with mutually restrained internal motion properties of ensembles on all structural levels of matter composition emerge through the collective being of components
|
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|
[-0.19623726985796733, 0.22353429501419197, -0.08386657625454029, -0.045074222440167365, -0.07783308038398429, -0.11320850755846887, 0.03670116574869974, 0.33688137400895357, -0.2864124139563905, -0.2675478053214546, 0.08755847787122345, -0.3475736016235142, -0.15830982219065642, 0.13703989795909297, 0.011199655979268116, -0.062187109419028275, 0.023187421944587387, 0.0695204225808589, 0.0019020510544241578, -0.19386474297519912, 0.375650887205093, 0.01185852368965883, 0.2800506230861949, 0.00302504595041413, 0.10218956965642671, 0.0034163456002715975, -0.0007369506794795463, 0.028835859931186186, -0.030769230265394545, 0.15990727231359483, 0.17716394189833576, 0.13533629797812965, 0.2663127396566172, -0.4315590003224551, -0.2061269155086915, 0.11048390614989868, 0.1686243481472721, 0.03863187161321683, 0.010687910647700645, -0.24512292467126692, 0.014213032097797151, -0.17785632964741024, -0.14839044608244742, -0.06456523533442696, 0.06089803041821277, 0.09255100208489846, -0.20982898891627513, 0.09259815489079941, 0.07326172228419671, 0.08119055452752272, -0.08604095561787728, -0.08813864410708279, -0.07930119517173066, 0.19837420130648684, 0.06853965088656103, -0.04944604484329897, 0.25024983034947784, -0.18844870791373844, -0.07089219157178714, 0.4202836972005941, 0.011764931715367345, -0.17234806075295503, 0.2924105681573834, -0.10749369489753412, -0.10553684573689545, 0.08529880081725962, 0.1507321095732213, 0.06273913812495906, -0.13176632642366545, 0.01838644933013711, 0.01479355521776058, 0.15251746040626635, 0.04023452647271807, 0.14055797244698084, 0.27066368678222513, 0.1769498534030626, 0.0800392015806008, 0.14723936616361175, -0.010106907049366445, -0.13359716850876188, -0.21460644567937212, -0.17481840604967955, -0.157569005841247, 0.013868064955911703, -0.09829293437562431, -0.19962753361647223, 0.43402721074030354, 0.10807971370889356, 0.21192450188014103, -0.02340154184343259, 0.2956378140855425, 0.061116160601765536, 0.08263695640360108, 0.04705381805952466, 0.2627414850452354, 0.15522292327066814, 0.042955094806125596, -0.2152706132468733, 0.11010073891978849, -0.023324000694426812]
|
707.0835
|
The Euler characteristic of a category as the sum of a divergent series
|
The Euler characteristic of a cell complex is often thought of as the
alternating sum of the number of cells of each dimension. When the complex is
infinite, the sum diverges. Nevertheless, it can sometimes be evaluated; in
particular, this is possible when the complex is the nerve of a finite
category. This provides an alternative definition of the Euler characteristic
of a category, which is in many cases equivalent to the original one
(math.CT/0610260).
|
math.CT math.AT
|
the euler characteristic of a cell complex is often thought of as the alternating sum of the number of cells of each dimension when the complex is infinite the sum diverges nevertheless it can sometimes be evaluated in particular this is possible when the complex is the nerve of a finite category this provides an alternative definition of the euler characteristic of a category which is in many cases equivalent to the original one mathct0610260
|
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|
[-0.15098155475523625, 0.12025970723531114, -0.07243817249262655, 0.08513323308088237, -0.08179639099162651, -0.10540421370643417, -0.03671337923387418, 0.2988560191682867, -0.3306371933163924, -0.21205591889274483, 0.11366346596450722, -0.20468430225485684, -0.17677490576799657, 0.20121517678017956, -0.11012112083718986, -0.044859173304929924, 0.019131380724846513, 0.16177425677007115, -0.035492725391098226, -0.28622280456427784, 0.3408490702339977, -0.009227692703338893, 0.2622225197233461, 0.03714440369701667, 0.12093063474104211, -0.02394284391020601, 0.012753280597059307, 0.07504802939618802, -0.03963072541031382, 0.12787797548682303, 0.2730239258663779, 0.09988051286986652, 0.2835952423456301, -0.36369004946302724, -0.18271480515800617, 0.14773756815623995, 0.18552880352866408, 0.08084573733110635, 0.059826011366739464, -0.1965543588724088, 0.13523670882490035, -0.16693716688157134, -0.1436228853071461, -0.0005650762468576431, 0.05209140942708866, 0.04530976871280251, -0.2655260699134119, 0.0024291050755670548, 0.07616175185083537, 0.0607040670662615, -0.042261769309186854, -0.09463513551934345, -0.006559682984811229, 0.13841128786884224, 0.050796424161416255, 0.03422262098615032, 0.09139064629562199, -0.1431847376673407, -0.07948083142007424, 0.43849229353882774, -0.0006332426910867562, -0.26915385420874666, 0.2056721626604731, -0.11656187075769177, -0.06431858329656157, 0.19061096193822655, 0.05925320995015067, 0.14710740083073442, -0.08920749757207641, 0.09753465834954703, -0.139054395296183, 0.11997191607952118, 0.07409778433675701, 0.0038431193805425552, 0.15879865511748437, 0.19248647495987825, 0.07957772446585491, 0.15468560395026076, -0.06296970272386396, -0.09714116966052963, -0.31964531242595734, -0.24899223361265016, -0.18684758336560145, 0.1302589999914572, -0.10013708085878878, -0.23546191199833677, 0.41944957187248244, 0.07245285307510278, 0.20609189975201278, 0.05868582472966581, 0.3317450546735042, 0.15309300427985806, 0.08181747443882774, -0.015029821727374519, 0.16278600772037297, 0.13950632119903694, 0.027018492689003814, -0.17208092078893772, 0.0852631248370115, 0.10329017107299454]
|
707.0836
|
Repr\'esentations de Springer pour les groupes de r\'eflexions complexes
imprimitifs
|
To a spetsial complex reflection group, equipped with a root lattice in the
sense of Nebe, we attach a certain finite set playing a role which is analogous
to the role of the set of unipotent classes of an algebraic group. In the case
of imprimitive groups, we give a combinatoric parametrization of it in terms of
Malle-Shoji generalized symbols. This result provides a link between the works
of Shoji on Green functions for complex reflection groups and of Broue, Kim,
Malle, Rouquier, et. al. on the cyclotomic Hecke algebras and their families of
characters.
-----
A un groupe de reflexions complexe spetsial, muni d'un reseau radiciel au
sens de Nebe, nous associons un certain ensemble fini qui doit jouer un role
analogue a celui de l'ensemble des classes unipotentes d'un groupe algebrique.
Dans le cas des groupes imprimitifs, nous en donnons un parametrage
combinatoire en termes des symboles generalises de Malle et Shoji. Ce resultat
fournit un lien entre les travaux de Shoji sur les fonctions de Green pour les
groupes de reflexions complexes et ceux de Broue, Kim, Malle, Rouquier, et al.
sur les algebres de Hecke cyclotomiques et leurs familles de caracteres.
|
math.RT
|
to a spetsial complex reflection group equipped with a root lattice in the sense of nebe we attach a certain finite set playing a role which is analogous to the role of the set of unipotent classes of an algebraic group in the case of imprimitive groups we give a combinatoric parametrization of it in terms of malleshoji generalized symbols this result provides a link between the works of shoji on green functions for complex reflection groups and of broue kim malle rouquier et al on the cyclotomic hecke algebras and their families of characters a un groupe de reflexions complexe spetsial muni dun reseau radiciel au sens de nebe nous associons un certain ensemble fini qui doit jouer un role analogue a celui de lensemble des classes unipotentes dun groupe algebrique dans le cas des groupes imprimitifs nous en donnons un parametrage combinatoire en termes des symboles generalises de malle et shoji ce resultat fournit un lien entre les travaux de shoji sur les fonctions de green pour les groupes de reflexions complexes et ceux de broue kim malle rouquier et al sur les algebres de hecke cyclotomiques et leurs familles de caracteres
|
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|
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|
707.0837
|
Explicit Formula for Constructing Binomial Confidence Interval with
Guaranteed Coverage Probability
|
In this paper, we derive an explicit formula for constructing the confidence
interval of binomial parameter with guaranteed coverage probability. The
formula overcomes the limitation of normal approximation which is asymptotic in
nature and thus inevitably introduce unknown errors in applications. Moreover,
the formula is very tight in comparison with classic Clopper-Pearson's approach
from the perspective of interval width. Based on the rigorous formula, we also
obtain approximate formulas with excellent performance of coverage probability.
|
math.ST math.PR stat.ME stat.TH
|
in this paper we derive an explicit formula for constructing the confidence interval of binomial parameter with guaranteed coverage probability the formula overcomes the limitation of normal approximation which is asymptotic in nature and thus inevitably introduce unknown errors in applications moreover the formula is very tight in comparison with classic clopperpearsons approach from the perspective of interval width based on the rigorous formula we also obtain approximate formulas with excellent performance of coverage probability
|
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|
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|
707.0838
|
Membrane instantons from mirror symmetry
|
We use mirror symmetry to determine and sum up a class of membrane instanton
corrections to the hypermultiplet moduli space metric arising in Calabi-Yau
threefold compactifications of type IIA strings. These corrections are mirror
to the D1 and D(-1)-brane instantons on the IIB side and are given explicitly
in terms of a single function in projective superspace. The corresponding
four-dimensional effective action is completely fixed by the Euler number and
the genus zero Gopakumar-Vafa invariants of the mirror Calabi-Yau.
|
hep-th
|
we use mirror symmetry to determine and sum up a class of membrane instanton corrections to the hypermultiplet moduli space metric arising in calabiyau threefold compactifications of type iia strings these corrections are mirror to the d1 and d1brane instantons on the iib side and are given explicitly in terms of a single function in projective superspace the corresponding fourdimensional effective action is completely fixed by the euler number and the genus zero gopakumarvafa invariants of the mirror calabiyau
|
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|
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|
707.0839
|
A Gravitational Wave Background from Reheating after Hybrid Inflation
|
The reheating of the universe after hybrid inflation proceeds through the
nucleation and subsequent collision of large concentrations of energy density
in the form of bubble-like structures moving at relativistic speeds. This
generates a significant fraction of energy in the form of a stochastic
background of gravitational waves, whose time evolution is determined by the
successive stages of reheating: First, tachyonic preheating makes the amplitude
of gravity waves grow exponentially fast. Second, bubble collisions add a new
burst of gravitational radiation. Third, turbulent motions finally sets the end
of gravitational waves production. From then on, these waves propagate
unimpeded to us. We find that the fraction of energy density today in these
primordial gravitational waves could be significant for GUT-scale models of
inflation, although well beyond the frequency range sensitivity of
gravitational wave observatories like LIGO, LISA or BBO. However, low-scale
models could still produce a detectable signal at frequencies accessible to BBO
or DECIGO. For comparison, we have also computed the analogous gravitational
wave background from some chaotic inflation models and obtained results similar
to those found by other groups. The discovery of such a background would open a
new observational window into the very early universe, where the details of the
process of reheating, i.e. the Big Bang, could be explored. Moreover, it could
also serve in the future as a new experimental tool for testing the
Inflationary Paradigm.
|
hep-ph
|
the reheating of the universe after hybrid inflation proceeds through the nucleation and subsequent collision of large concentrations of energy density in the form of bubblelike structures moving at relativistic speeds this generates a significant fraction of energy in the form of a stochastic background of gravitational waves whose time evolution is determined by the successive stages of reheating first tachyonic preheating makes the amplitude of gravity waves grow exponentially fast second bubble collisions add a new burst of gravitational radiation third turbulent motions finally sets the end of gravitational waves production from then on these waves propagate unimpeded to us we find that the fraction of energy density today in these primordial gravitational waves could be significant for gutscale models of inflation although well beyond the frequency range sensitivity of gravitational wave observatories like ligo lisa or bbo however lowscale models could still produce a detectable signal at frequencies accessible to bbo or decigo for comparison we have also computed the analogous gravitational wave background from some chaotic inflation models and obtained results similar to those found by other groups the discovery of such a background would open a new observational window into the very early universe where the details of the process of reheating ie the big bang could be explored moreover it could also serve in the future as a new experimental tool for testing the inflationary paradigm
|
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|
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|
707.084
|
Fredholm Modules on P.C.F. Self-Similar Fractals and their Conformal
Geometry
|
The aim of the present work is to show how, using the differential calculus
associated to Dirichlet forms, it is possible to construct Fredholm modules on
post critically finite fractals by regular harmonic structures. The modules are
d-summable, the summability exponent d coinciding with the spectral dimension
of the generalized laplacian operator associated with the regular harmonic
structures. The characteristic tools of the noncommutative infinitesimal
calculus allow to define a d-energy functional which is shown to be a
self-similar conformal invariant.
|
math.FA math.OA
|
the aim of the present work is to show how using the differential calculus associated to dirichlet forms it is possible to construct fredholm modules on post critically finite fractals by regular harmonic structures the modules are dsummable the summability exponent d coinciding with the spectral dimension of the generalized laplacian operator associated with the regular harmonic structures the characteristic tools of the noncommutative infinitesimal calculus allow to define a denergy functional which is shown to be a selfsimilar conformal invariant
|
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|
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|
707.0841
|
Neutrino masses, mixing and leptogenesis in TeV scale B-L extension of
the standard model
|
We address the issue of the neutrino masses and mixing in TeV scale $B-L$
extension of the Standard Model. We show that if Dirac neutrino masses are of
order $10^{-4}$ Gev, then the measured neutrino masses are correctly obtained.
We propose a mass relation between quarks and leptons that may account for such
small Dirac neutrino masses. We analyze the leptogenesis in this type of models
and provide analytical expressions for the new contributions due to the
predicted extra Higgs and extra neutral gauge boson. We find that thermal
leptogenesis, with a resonant enhancement due to nearly degenerate right-handed
neutrinos, can yield sufficient baryon asymmetry. Finally, we comment on a
possible scheme for non-thermal leptogenesis, which is due to the decay of
extra Higgs into right-handed neutrino.
|
hep-ph
|
we address the issue of the neutrino masses and mixing in tev scale bl extension of the standard model we show that if dirac neutrino masses are of order 104 gev then the measured neutrino masses are correctly obtained we propose a mass relation between quarks and leptons that may account for such small dirac neutrino masses we analyze the leptogenesis in this type of models and provide analytical expressions for the new contributions due to the predicted extra higgs and extra neutral gauge boson we find that thermal leptogenesis with a resonant enhancement due to nearly degenerate righthanded neutrinos can yield sufficient baryon asymmetry finally we comment on a possible scheme for nonthermal leptogenesis which is due to the decay of extra higgs into righthanded neutrino
|
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|
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|
707.0842
|
Classical approximation to quantum cosmological correlations
|
We investigate up to which order quantum effects can be neglected in
calculating cosmological correlation functions after horizon exit. As a toy
model, we study $\phi^3$ theory on a de Sitter background for a massless
minimally coupled scalar field $\phi$. We find that for tree level and one loop
contributions in the quantum theory, a good classical approximation can be
constructed, but for higher loop corrections this is in general not expected to
be possible. The reason is that loop corrections get non-negligible
contributions from loop momenta with magnitude up to the Hubble scale H, at
which scale classical physics is not expected to be a good approximation to the
quantum theory. An explicit calculation of the one loop correction to the two
point function, supports the argument that contributions from loop momenta of
scale $H$ are not negligible. Generalization of the arguments for the toy model
to derivative interactions and the curvature perturbation leads to the
conclusion that the leading orders of non-Gaussian effects generated after
horizon exit, can be approximated quite well by classical methods. Furthermore
we compare with a theorem by Weinberg. We find that growing loop corrections
after horizon exit are not excluded, even in single field inflation.
|
hep-th astro-ph gr-qc hep-ph
|
we investigate up to which order quantum effects can be neglected in calculating cosmological correlation functions after horizon exit as a toy model we study phi3 theory on a de sitter background for a massless minimally coupled scalar field phi we find that for tree level and one loop contributions in the quantum theory a good classical approximation can be constructed but for higher loop corrections this is in general not expected to be possible the reason is that loop corrections get nonnegligible contributions from loop momenta with magnitude up to the hubble scale h at which scale classical physics is not expected to be a good approximation to the quantum theory an explicit calculation of the one loop correction to the two point function supports the argument that contributions from loop momenta of scale h are not negligible generalization of the arguments for the toy model to derivative interactions and the curvature perturbation leads to the conclusion that the leading orders of nongaussian effects generated after horizon exit can be approximated quite well by classical methods furthermore we compare with a theorem by weinberg we find that growing loop corrections after horizon exit are not excluded even in single field inflation
|
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|
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|
707.0843
|
Two chiral nonet model with massless quarks
|
We present a detailed study of a linear sigma model containing one chiral
nonet transforming under U(1)$_A$ as a quark-antiquark composite and another
chiral nonet transforming as a diquark-anti diquark composite (or, equivalently
from a symmetry point of view, as a two meson molecule). The model provides an
intuitive explanation of a current puzzle in low energy QCD: Recent work has
suggested the existence of a lighter than 1 GeV nonet of scalar mesons which
behave like four quark composites. On the other hand, the validity of a
spontaneously broken chiral symmetric description would suggest that these
states be chiral partners of the light pseudoscalar mesons, which are two quark
composites. The model solves the problem by starting with the two chiral nonets
mentioned and allowing them to mix with each other. The input of physical
masses in the SU(3) invariant limit for two scalar octets and an "excited" pion
octet results in a mixing pattern wherein the light scalars have a large four
quark content while the light pseudoscalars have a large two quark content. One
light isosinglet scalar is exceptionally light. In addition, the pion pion
scattering is also studied and the current algebra theorem is verified for
massless pions which contain some four quark admixture.
|
hep-ph
|
we present a detailed study of a linear sigma model containing one chiral nonet transforming under u1_a as a quarkantiquark composite and another chiral nonet transforming as a diquarkanti diquark composite or equivalently from a symmetry point of view as a two meson molecule the model provides an intuitive explanation of a current puzzle in low energy qcd recent work has suggested the existence of a lighter than 1 gev nonet of scalar mesons which behave like four quark composites on the other hand the validity of a spontaneously broken chiral symmetric description would suggest that these states be chiral partners of the light pseudoscalar mesons which are two quark composites the model solves the problem by starting with the two chiral nonets mentioned and allowing them to mix with each other the input of physical masses in the su3 invariant limit for two scalar octets and an excited pion octet results in a mixing pattern wherein the light scalars have a large four quark content while the light pseudoscalars have a large two quark content one light isosinglet scalar is exceptionally light in addition the pion pion scattering is also studied and the current algebra theorem is verified for massless pions which contain some four quark admixture
|
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|
[-0.1066649898842814, 0.3002319979462559, -0.11027230805568937, 0.1225563120091298, -0.08778637145749396, -0.19464814575200062, 0.033878547952685883, 0.32985932357015385, -0.1447132196466344, -0.24960256838532174, 0.009141146949973804, -0.31806483451762924, -0.041276480661759124, 0.054459786954772285, 0.08603866842174948, 0.060104742286285914, 0.00904771153745354, 0.07690550503658428, -0.06220206837867193, -0.20454406564726813, 0.3415977458114137, -0.11350957325610202, 0.21927231259628285, 0.1267387517595749, 0.05404950646404627, 0.011983604695656954, 0.010698463151384379, -0.08471758725517542, -0.006710094296445694, 0.08092867398374727, 0.1691665372309041, 0.0470796100039413, 0.1388398986129801, -0.36574286986412347, -0.19237463569475544, 0.11167395322534125, 0.16781429617380575, 0.13102907868516114, -0.09399316305847746, -0.2951292717302947, 0.08922319439130695, -0.19976829966768658, -0.187226717762991, -0.09567130548915498, -0.0334475311121098, -0.10097544873048943, -0.3058627668592701, 0.06375173223640765, -0.00873216753375631, 0.041339312837535634, -0.05374282350255275, -0.24047277359390892, -0.07978404537383196, 0.02517195756700124, 0.14641293043952328, 0.07689799788713923, 0.14862920758078227, -0.2077673335114251, -0.14148508796551612, 0.456405079478155, -0.09079452918580641, -0.20526168222768584, 0.12946947880656176, -0.09056266864023851, -0.14337367545430896, 0.10744556000035545, 0.1611148015672458, 0.08740002161751227, -0.19924019331985338, 0.07720412190000815, -0.13857385574768022, 0.17850590733643104, 0.11564084784249248, 0.09702666003059074, 0.29532071113910363, 0.19095244080026225, -0.035492175269943936, 0.0917922956565314, -0.013318640857193718, -0.1151969485875705, -0.35564186127017283, -0.13303049345127338, -0.10753904662999338, 0.07618791851269054, -0.0880846480345736, -0.12451031836478607, 0.4394228532595407, 0.06474555621895453, 0.2389538665144628, -0.013462912015153481, 0.30995988846050154, 0.06220866340957132, 0.09015216629252434, 0.058037891922122685, 0.2780636059338787, 0.20593774012247199, 0.12772127238534176, -0.2257642173691954, -0.07939651290321462, 0.07997239256111212]
|
707.0844
|
Spherical Needlets for CMB Data Analysis
|
We discuss Spherical Needlets and their properties. Needlets are a form of
spherical wavelets which do not rely on any kind of tangent plane approximation
and enjoy good localization properties in both pixel and harmonic space;
moreover needlets coefficients are asymptotically uncorrelated at any fixed
angular distance, which makes their use in statistical procedures very
promising. In view of these properties, we believe needlets may turn out to be
especially useful in the analysis of Cosmic Microwave Background (CMB) data on
the incomplete sky, as well as of other cosmological observations. As a final
advantage, we stress that the implementation of needlets is computationally
very convenient and may rely completely on standard data analysis packages such
as HEALPix.
|
astro-ph
|
we discuss spherical needlets and their properties needlets are a form of spherical wavelets which do not rely on any kind of tangent plane approximation and enjoy good localization properties in both pixel and harmonic space moreover needlets coefficients are asymptotically uncorrelated at any fixed angular distance which makes their use in statistical procedures very promising in view of these properties we believe needlets may turn out to be especially useful in the analysis of cosmic microwave background cmb data on the incomplete sky as well as of other cosmological observations as a final advantage we stress that the implementation of needlets is computationally very convenient and may rely completely on standard data analysis packages such as healpix
|
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|
[-0.06168422946643274, 0.046579007161939044, -0.13514567337440864, 0.10900026194132682, -0.1363420180179242, -0.1027987476663222, -0.017418257663247443, 0.43317098369411494, -0.2333329933206156, -0.25258262013479815, 0.15369564509492809, -0.2764998375678877, -0.13349916539707427, 0.25185098547302975, -0.03736509634201589, 0.07109149408100521, 0.05932147844134183, -0.002498530060589566, -0.10346850011521413, -0.21498074113999066, 0.2742012971065054, 0.1512823044085654, 0.3196727706087848, -0.021011209805985375, 0.08714767742973073, 0.0032379212907625962, -0.09250846762462693, 0.025206783829578513, -0.10209486577730138, 0.09677721651357804, 0.26048021902472285, 0.15130624724788813, 0.21127716388742804, -0.4335587200535051, -0.1910116683565459, 0.11863053781059334, 0.1715802386781927, 0.10031153412212192, -0.034957726627106826, -0.26024481180613324, 0.0492684309108388, -0.11771203429138256, -0.1365570703729044, -0.18325896512803827, -0.04318494498492929, 0.08052604081961563, -0.223772064403836, 0.08313772938672011, 0.09571774414852972, 0.045293346884013236, -0.02843532490768959, -0.12921226749954334, -0.021888083030501285, 0.1042181742851133, 0.030144849782257135, -0.00020477157115731073, 0.15185828660456938, -0.08936449504157497, -0.04558778614184614, 0.4110653305675842, -0.04915651198381842, -0.2553257603115418, 0.19590867056424524, -0.16628412865260142, -0.1878446278841061, 0.06862910712627157, 0.20137312814348646, 0.09406762302979448, -0.14812646911211186, 0.11059744789272989, 0.0028992264651914396, 0.15164047030838584, 0.09064308418181993, 0.10030435017996736, 0.26101541167945935, 0.08977770413098446, 0.0743382056164792, 0.11258265490483856, -0.12475728618288887, -0.03525790876819421, -0.313553427993241, -0.10624390267530236, -0.21968570829594067, 0.03499335986456017, -0.1328523870497366, -0.23265555042426211, 0.36796055505470515, 0.14580013754706578, 0.18793561595681488, 0.03555324684110296, 0.3022166333966336, 0.015915453161697013, 0.0757934514677815, 0.02910360905254986, 0.27671511537569055, 0.10749312870646432, 0.08751647726837862, -0.07835138224704602, 0.03416302274139124, 0.04461198120172751]
|
707.0845
|
Logarithmic limit sets of real semi-algebraic sets
|
This paper is about the logarithmic limit sets of real semi-algebraic sets,
and, more generally, about the logarithmic limit sets of sets definable in an
o-minimal, polynomially bounded structure. We prove that most of the properties
of the logarithmic limit sets of complex algebraic sets hold in the real case.
This include the polyhedral structure and the relation with the theory of
non-archimedean fields, tropical geometry and Maslov dequantization.
|
math.AG
|
this paper is about the logarithmic limit sets of real semialgebraic sets and more generally about the logarithmic limit sets of sets definable in an ominimal polynomially bounded structure we prove that most of the properties of the logarithmic limit sets of complex algebraic sets hold in the real case this include the polyhedral structure and the relation with the theory of nonarchimedean fields tropical geometry and maslov dequantization
|
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|
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|
707.0846
|
Solitons in interacting Dicke models of coupled cavities with two-level
systems
|
We consider an array of coupled optical cavities, each containing a
multi-atom ensemble. We show that the nonlinearity inherent in the cooperative
dynamics of the atoms in each ensemble coupled to the respective cavity field
allows for the formation of solitary waves. Such a prediction can be tested in
state-of-the-art semiconducting photonic-crystal microcavities with embedded
impurities.
|
quant-ph
|
we consider an array of coupled optical cavities each containing a multiatom ensemble we show that the nonlinearity inherent in the cooperative dynamics of the atoms in each ensemble coupled to the respective cavity field allows for the formation of solitary waves such a prediction can be tested in stateoftheart semiconducting photoniccrystal microcavities with embedded impurities
|
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|
[-0.18293831787637568, 0.13729823549744782, 0.006263925922602149, -0.0404282758078937, 0.02585000916899714, -0.19001964346638747, -0.039718368537640866, 0.45704987781521467, -0.22729672927276365, -0.23665965330188296, 0.017699067474625605, -0.3072959992945731, -0.1399806951438742, 0.148699813730283, 0.01536548399599269, 0.03415448438110096, 0.09031243384483137, 0.010582057077304594, -0.00702496843795026, -0.19234241010105638, 0.27638867927765076, 0.018899357179179788, 0.31947451039949165, -0.005824484247049051, 0.106405198307974, -0.003932806987514985, 0.11388916030825515, 0.024513983304911693, -0.07992011864618169, 0.13961569589030529, 0.25078190197902067, 0.0029674930930403726, 0.27934908021623933, -0.5154092629839268, -0.24691262641655548, 0.0770960615648489, 0.21080108068417758, 0.19995835520759492, -0.07908745903322208, -0.33065403242861585, -0.01955907912841732, -0.12917279638194096, -0.1377853107239519, -0.01610877677532179, -0.06146469205642851, 0.09318687000112343, -0.27157126686402727, 0.011024832721367213, 0.03131873889027962, -0.007691015999755889, -0.0725996266295884, -0.014106999467393118, 0.007504462950497067, 0.0725260881174888, -0.09699040484390155, -0.02860526631619515, 0.17068815891564423, -0.13956240953744523, -0.13523605983885187, 0.3936064373701811, -0.15960775500363006, -0.17350018147512206, 0.20519949632164622, -0.12590711726807058, -0.054634302422138195, 0.14156650740187615, 0.21165952299322402, 0.06890939575220857, -0.11543728027858638, 0.041292477665202956, -0.046612919125306816, 0.247216032734806, 0.0865205622477723, 0.10055501013994217, 0.27433538329829127, 0.2570187396860482, -0.0005947876821405121, 0.21468775525447978, -0.10132362250338442, -0.08789140197456748, -0.2086180300331242, -0.171587172197178, -0.16396212438121438, 0.06157217427556004, -0.10782234020630962, -0.19761814165394753, 0.40862975595518947, 0.15480755975503208, 0.14764408664112644, -0.06055657402612269, 0.25848836798520225, 0.09265312276381467, 0.10192719131841191, 0.04102109661991043, 0.29210125372212914, 0.15201722105432833, 0.0007848760246166161, -0.3140144952173744, -0.0685331378813966, -0.02916561986785382]
|
707.0847
|
Stochastic Inflationary Scalar Electrodynamics
|
We stochastically formulate the theory of scalar quantum electrodynamics on a
de Sitter background. This reproduces the leading infrared logarithms at each
loop order. It also allows one to sum the series of leading infrared logarithms
to obtain explicit, nonperturbative results about the late time behavior of the
system. One consequence is confirmation of the conjecture by Davis, Dimopoulos,
Prokopec and Tornkvist that super-horizon photons acquire mass during
inflation. We compute a photon mass-suqared of about 3.2991 H^2. The scalar
stays perturbatively light with a mass-squared of about 0.8961 3 e^2 H^2/8pi^2.
Interestingly, the induced change in the cosmological constant is negative, of
about -0.6551 3 G H^4/pi.
|
gr-qc astro-ph hep-ph
|
we stochastically formulate the theory of scalar quantum electrodynamics on a de sitter background this reproduces the leading infrared logarithms at each loop order it also allows one to sum the series of leading infrared logarithms to obtain explicit nonperturbative results about the late time behavior of the system one consequence is confirmation of the conjecture by davis dimopoulos prokopec and tornkvist that superhorizon photons acquire mass during inflation we compute a photon masssuqared of about 32991 h2 the scalar stays perturbatively light with a masssquared of about 08961 3 e2 h28pi2 interestingly the induced change in the cosmological constant is negative of about 06551 3 g h4pi
|
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|
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|
707.0848
|
No-local-broadcasting theorem for quantum correlations
|
We prove that the correlations present in a multipartite quantum state have
an \emph{operational} quantum character as soon as the state does not simply
encode a multipartite classical probability distribution, i.e. does not
describe the joint state of many classical registers. Even unentangled states
may exhibit such \emph{quantumness}, that is pointed out by the new task of
\emph{local broadcasting}, i.e. of locally sharing pre-established
correlations: this task is feasible if and only if correlations are classical
and derive a no-local-broadcasting theorem for quantum correlations. Thus,
local broadcasting is able to point out the quantumness of correlations, as
standard broadcasting points out the quantum character of single system states.
Further, we argue that our theorem implies the standard no-broadcasting theorem
for single systems, and that our operative approach leads in a natural way to
the definition of measures for quantumness of correlations.
|
quant-ph
|
we prove that the correlations present in a multipartite quantum state have an emphoperational quantum character as soon as the state does not simply encode a multipartite classical probability distribution ie does not describe the joint state of many classical registers even unentangled states may exhibit such emphquantumness that is pointed out by the new task of emphlocal broadcasting ie of locally sharing preestablished correlations this task is feasible if and only if correlations are classical and derive a nolocalbroadcasting theorem for quantum correlations thus local broadcasting is able to point out the quantumness of correlations as standard broadcasting points out the quantum character of single system states further we argue that our theorem implies the standard nobroadcasting theorem for single systems and that our operative approach leads in a natural way to the definition of measures for quantumness of correlations
|
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|
[-0.14371194326035355, 0.14377920218649323, -0.14968161332839425, 0.10228033327544783, 0.0013073141403172326, -0.20153498679291512, 0.08702548402547161, 0.31114584553068964, -0.2979515099786627, -0.23972787279500693, 0.0424315018108641, -0.2662915391037646, -0.12447607470001432, 0.18931526456034972, -0.07965828807167438, 0.05765442536684914, 0.08946902441464877, 0.08601313602939363, -0.06544982223936856, -0.23790030302884785, 0.3448283382947894, 0.0141399211547189, 0.29586650971728173, 0.06892169054354662, 0.09106859887201015, 0.05626679335525124, 0.02962537807668897, 0.01358132340364914, -0.04366106288343081, 0.05725051017150796, 0.291958785129954, 0.17175902902195905, 0.2733284392245654, -0.389783037421496, -0.21964095672929956, 0.1715924025621211, 0.13094013337842256, 0.16269441704144297, -0.002524313601273773, -0.3141828634492729, 0.07278602390442097, -0.17563006096431796, -0.10185137373881172, -0.15041689027397745, 0.024216919249949464, -0.03191889491458626, -0.2420039255360978, 0.11228582254978761, 0.1559550978489679, 0.023344352281233972, 0.02038888098415581, -0.034417479477955225, -0.0037357432335831118, 0.1562998698858976, -0.07559715199412481, 0.007664711032386707, 0.11001722162346476, -0.13170746012347873, -0.19235927009604115, 0.38026763150549453, -0.01101695043473518, -0.19890529401701593, 0.17613203111745795, -0.12263911443533025, -0.14553957684235513, 0.03847857451646764, 0.09097760496998503, 0.102539958131999, -0.13220168262099227, 0.050598022287147985, -0.09078520680845216, 0.2112761474818926, 0.026160677592944947, 0.1443811470399732, 0.2149068059372729, 0.06970534333959222, 0.12976462902303826, 0.1574051585520847, -0.06470003574614183, -0.16943017348302933, -0.3189197148709301, -0.20386204724807455, -0.23927015121148873, 0.11671605780978006, -0.047382009883459315, -0.15391085682895736, 0.3701817353957913, 0.14817594903971718, 0.1601734948555426, 0.067608472977198, 0.249394292408344, 0.08645086462754567, 0.06417071240940604, 0.09490675263130444, 0.24934160108408093, 0.10383380957089526, 0.05780222750120405, -0.17316753442223737, 0.09496775478718505, 0.03304160371814193]
|
707.0849
|
Deposition of Atoms on a Quasicrystalline Substrate: Molecular-Dynamics
Study in 3 Dimensions
|
We study the three-dimensional structure formation when atoms are deposited
onto a substrate with a decagonal quasicrystalline order.
Molecular-dynamicscalculations show that the adsorbate layer consists of
ordered nano-scale domains with orientations determined by the underlying
substrate symmetry. Depending on the relative strength of the interactions of
adsorbate atoms with each other and with the substrate atoms, different
morphologies are observed ranging from layer-by-layer growth to cluster
formation. We also find that the film thickness likewise affects the overall
structure of the growing film: Depending on the relative strength of the
interaction between adsorbate atoms, a structural transition of the
configuration of the adsorbate layers closest to the substrate can occur as the
number of deposited layers increases.
|
cond-mat.mtrl-sci cond-mat.soft
|
we study the threedimensional structure formation when atoms are deposited onto a substrate with a decagonal quasicrystalline order moleculardynamicscalculations show that the adsorbate layer consists of ordered nanoscale domains with orientations determined by the underlying substrate symmetry depending on the relative strength of the interactions of adsorbate atoms with each other and with the substrate atoms different morphologies are observed ranging from layerbylayer growth to cluster formation we also find that the film thickness likewise affects the overall structure of the growing film depending on the relative strength of the interaction between adsorbate atoms a structural transition of the configuration of the adsorbate layers closest to the substrate can occur as the number of deposited layers increases
|
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|
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|
707.085
|
Regular and Completely Regular Differential Operators
|
We define the concept of completely regular ordinary differential operators
and give various criteria for operators to belong to this class. We give also
criteria for Birkhof regularity of ordinary differential operators in terms of
the growth of the Green function and basis property.
|
math.SP math.OA
|
we define the concept of completely regular ordinary differential operators and give various criteria for operators to belong to this class we give also criteria for birkhof regularity of ordinary differential operators in terms of the growth of the green function and basis property
|
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|
[-0.10351364024330018, 0.03717617393839498, -0.1004881638123892, 0.11974813088200727, -0.0957153076847452, -0.07649038103950578, -0.005502573192812676, 0.2888689547842152, -0.29449453070586507, -0.2553385400408229, 0.13739454514769361, -0.2541635447983132, -0.1798256187764711, 0.18441038481284713, -0.07238723536910013, 0.07526729385866675, -0.01813089488030866, 0.04458344732086326, -0.11216341396577137, -0.2679059416228949, 0.48179923794990365, -0.06199360747150211, 0.23332482706322227, 0.03334694762909135, 0.10115662445639108, 0.024553495123549256, -0.07879504184563492, -0.007102019305146018, -0.18621237853238748, 0.1551251310941785, 0.26730400739714155, 0.14918139061435712, 0.23529185692584792, -0.4028068089554476, -0.10184863224885492, 0.17714746681930021, 0.07380971781974442, 0.04917626134877981, -0.03712842908016471, -0.23164935209680088, 0.10890056119235449, -0.1674515877005666, -0.2355989510583323, -0.09677951278565668, 0.053207181285806864, 0.08813606255260015, -0.33172127095505943, 0.0640908234995021, 0.1095193682541681, 0.07048327406478483, -0.09561162913586338, -0.08651710925407188, -0.028669539137830047, 0.08339368181606364, -0.048876656176045884, -0.09311989598452698, 0.044886675793244395, -0.0930782271884815, -0.1309573610860118, 0.30969125716838725, -0.07418497952870852, -0.2917743060997752, 0.1654089603378156, -0.19201680398437865, -0.12816554862399435, 0.05853151565764186, 0.17939626152605512, 0.17597084886632686, -0.1978796261774246, 0.11426863249467123, -0.026661025815058585, 0.04098375990640286, 0.06143568436680145, 0.1772653825234535, 0.06482761665139088, 0.0488741077634311, 0.14699139684265436, 0.17733886487088923, 0.05930820621853305, -0.07190124590902827, -0.3531334642970631, -0.2231690603806529, -0.023959909175890824, 0.05911579736789992, -0.05265965719834555, -0.26097644588281943, 0.44457218284870303, 0.11522288345406916, 0.20028302398358666, 0.09838177419679109, 0.17109894832098033, 0.24187789190300676, 0.09481309078546474, -0.025054860697669344, 0.18308383413742102, 0.16944104388117964, 0.11131882448788992, -0.15544920793171366, 0.03612384403687577, 0.22969040367752314]
|
707.0851
|
Determinant of the SU(N) caloron with nontrivial holonomy
|
The 1-loop quantum weight of the SU(N) KvBLL caloron with nontrivial holonomy
is calculated. The latter is the most general self-dual solution with unit
topological charge in the 4d Yang-Mills theory with one compactified dimension
(finite temperature).
|
hep-th
|
the 1loop quantum weight of the sun kvbll caloron with nontrivial holonomy is calculated the latter is the most general selfdual solution with unit topological charge in the 4d yangmills theory with one compactified dimension finite temperature
|
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|
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|
707.0852
|
The CH2CN- molecule: Carrier of the lambda8037 diffuse interstellar
band?
|
The hypothesis that the cyanomethyl anion CH2CN- is responsible for the
relatively narrow diffuse interstellar band (DIB) at 8037.8 +- 0.15 Angstroms
is examined with reference to new observational data. The 0_0^0 absorption band
arising from the ^1B_1 - X ^1A' transition from the electronic ground state to
the first dipole-bound state of the anion is calculated for a rotational
temperature of 2.7 K using literature spectroscopic parameters and results in a
rotational contour with a peak wavelength of 8037.78 Angstroms. By comparison
with diffuse band and atomic line absorption spectra of eight heavily-reddened
Galactic sightlines, CH2CN- is found to be a plausible carrier of the
lambda8037 diffuse interstellar band provided the rotational contour is
Doppler-broadened with a b parameter between 16 and 33 km/s that depends on the
specific sightline. Convolution of the calculated CH2CN- transitions with the
optical depth profile of interstellar Ti II results in a good match with the
profile of the narrow lambda8037 DIB observed towards HD 183143, HD 168112 and
Cyg OB2 8a. The rotational level populations may be influenced by nuclear spin
statistics, resulting in the appearance of additional transitions from K_a = 1
of ortho CH2CN- near 8025 and 8050 Angstroms that are not seen in currently
available interstellar spectra. For CH2CN- to be the carrier of the lambda8037
diffuse interstellar band, either a) there must be mechanisms that convert
CH2CN- from the ortho to the para form, or b) the chemistry that forms CH2CN-
must result in a population of K_a'' levels approaching a Boltzmann
distribution near 3 K.
|
astro-ph
|
the hypothesis that the cyanomethyl anion ch2cn is responsible for the relatively narrow diffuse interstellar band dib at 80378 015 angstroms is examined with reference to new observational data the 0_00 absorption band arising from the 1b_1 x 1a transition from the electronic ground state to the first dipolebound state of the anion is calculated for a rotational temperature of 27 k using literature spectroscopic parameters and results in a rotational contour with a peak wavelength of 803778 angstroms by comparison with diffuse band and atomic line absorption spectra of eight heavilyreddened galactic sightlines ch2cn is found to be a plausible carrier of the lambda8037 diffuse interstellar band provided the rotational contour is dopplerbroadened with a b parameter between 16 and 33 kms that depends on the specific sightline convolution of the calculated ch2cn transitions with the optical depth profile of interstellar ti ii results in a good match with the profile of the narrow lambda8037 dib observed towards hd 183143 hd 168112 and cyg ob2 8a the rotational level populations may be influenced by nuclear spin statistics resulting in the appearance of additional transitions from k_a 1 of ortho ch2cn near 8025 and 8050 angstroms that are not seen in currently available interstellar spectra for ch2cn to be the carrier of the lambda8037 diffuse interstellar band either a there must be mechanisms that convert ch2cn from the ortho to the para form or b the chemistry that forms ch2cn must result in a population of k_a levels approaching a boltzmann distribution near 3 k
|
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|
[-0.07388921535854774, 0.1194958077119534, -0.01817655688398645, 0.01446332297304512, -0.03005418977108858, -0.14390781742247147, 0.09102683811492863, 0.44670494265174343, -0.22422741295812312, -0.2935389734270829, 0.0032847301146599448, -0.3011510997330622, -0.007783239828385708, 0.13612207184667655, 0.04768177460246512, -0.05827160184419462, 0.015565216425798892, -0.06573800685665836, -0.037695129333610924, -0.1587926932898838, 0.2673308436263589, 0.057114883662304945, 0.19342897975672266, 0.055209512564784194, 0.028177538687328158, -0.09681411198454, 0.007850640686228871, -0.04595738499275675, -0.149193674914516, 0.09367790333335362, 0.2693930699273811, 0.04929556397219708, 0.1709673917929548, -0.3439304550097043, -0.22286355718628445, 0.04215599795237982, 0.16525419141602007, 0.07196168398617633, -0.0025380635777274, -0.29318413379166036, 0.03438755909086294, -0.11233616309399376, -0.15075493925103237, 0.03199301880603242, 0.06457728241008544, 0.027657732190120788, -0.217081361184336, 0.11139503663654314, -0.02583746489004365, 0.13611968343944422, -0.16210674557609425, -0.1927108139527032, -0.1276479233924802, 0.06629608313105853, 0.009581207617422536, 0.07251107303431675, 0.16320862567850522, -0.0960369051867279, -0.02526812716978528, 0.44855632573839216, -0.1248427594421498, -0.014313044968903774, 0.1837675180969878, -0.19558405726390432, -0.15280309856207747, 0.2624618758813345, 0.05628143293997421, 0.0747606515743962, -0.1258928631413876, 0.03618160055627832, -0.04524920973834389, 0.22052262635302863, 0.05828866923490303, 0.09037203650731253, 0.23294344000400058, 0.0694045309773794, 0.022154098631636726, 0.06557851999657162, -0.23941688452540558, -0.027880809628330762, -0.2142913075143634, -0.1429684441093178, -0.15583745668649615, 0.0767412665069666, -0.07531379644696864, -0.11401791116365949, 0.3378475365729722, 0.07203216875848104, 0.2131623704003037, -0.03514456750717872, 0.24946824264424367, 0.10516899214717486, 0.06467504094175566, 0.09718817318484764, 0.27833995685403584, 0.1724286685099027, 0.0958554568249614, -0.23051809147138902, 0.09637612759483062, -0.013386655494474643]
|
707.0853
|
Spectral isolation of naturally reductive metrics on simple Lie groups
|
We show that within the class of left-invariant naturally reductive metrics
$\mathcal{M}_{\operatorname{Nat}}(G)$ on a compact simple Lie group $G$, every
metric is spectrally isolated. We also observe that any collection of
isospectral compact symmetric spaces is finite; this follows from a somewhat
stronger statement involving only a finite part of the spectrum.
|
math.DG math.SP
|
we show that within the class of leftinvariant naturally reductive metrics mathcalm_operatornamenatg on a compact simple lie group g every metric is spectrally isolated we also observe that any collection of isospectral compact symmetric spaces is finite this follows from a somewhat stronger statement involving only a finite part of the spectrum
|
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|
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|
707.0854
|
Adaptation and Coevolution on an Emergent Global Competitive Landscape
|
Notions of Darwinian selection have been implicit in economic theory for at
least sixty years. Richard Nelson and Sidney Winter have argued that while
evolutionary thinking was prevalent in prewar economics, the postwar
Neoclassical school became almost entirely preoccupied with equilibrium
conditions and their mathematical conditions. One of the problems with the
economic interpretation of firm selection through competition has been a weak
grasp on an incomplete scientific paradigm. As I.F. Price notes, "The
biological metaphor has long lurked in the background of management theory
largely because the message of 'survival of the fittest' (usually wrongly
attributed to Charles Darwin rather than Herbert Spencer) provides a seemingly
natural model for market competition (e.g. Alchian 1950, Merrell 1984,
Henderson 1989, Moore 1993), without seriously challenging the underlying
paradigms of what an organisation is." In this paper we examine the application
of dynamic fitness landscape models to economic theory, particularly the theory
of technology substitution, drawing on recent work by Kauffman, Arthur,
McKelvey, Nelson and Winter, and Windrum and Birchenhall. In particular we use
Professor Post's early work with John Holland on the genetic algorithm to
explain some of the key differences between static and dynamic approaches to
economic modeling.
|
q-fin.GN nlin.AO
|
notions of darwinian selection have been implicit in economic theory for at least sixty years richard nelson and sidney winter have argued that while evolutionary thinking was prevalent in prewar economics the postwar neoclassical school became almost entirely preoccupied with equilibrium conditions and their mathematical conditions one of the problems with the economic interpretation of firm selection through competition has been a weak grasp on an incomplete scientific paradigm as if price notes the biological metaphor has long lurked in the background of management theory largely because the message of survival of the fittest usually wrongly attributed to charles darwin rather than herbert spencer provides a seemingly natural model for market competition eg alchian 1950 merrell 1984 henderson 1989 moore 1993 without seriously challenging the underlying paradigms of what an organisation is in this paper we examine the application of dynamic fitness landscape models to economic theory particularly the theory of technology substitution drawing on recent work by kauffman arthur mckelvey nelson and winter and windrum and birchenhall in particular we use professor posts early work with john holland on the genetic algorithm to explain some of the key differences between static and dynamic approaches to economic modeling
|
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|
[-0.04387219430917363, 0.09726294409981301, -0.13949843460737385, 0.10826511336538767, -0.11815046601557207, -0.15285140585993934, 0.05817962139712193, 0.314985753920103, -0.230441312584076, -0.3364095059826661, 0.11310730784723699, -0.2523154866172319, -0.20533246983149103, 0.14201899058996204, -0.1746781772060484, -0.0006795610877844491, 0.029196090597558014, -0.001683308127688466, 0.04561425116542881, -0.32188842428843323, 0.2591822685995332, 0.13585093746038993, 0.30590059382869944, 0.0692832048589103, 0.08194339181081792, 0.024180515978118607, -0.07836590563140115, -0.002039393518660507, -0.12906692965081176, 0.12826414476510697, 0.28781971173358906, 0.20487520177945148, 0.39644528915526567, -0.45284960722705164, -0.20836169292189427, 0.0775781662765543, 0.06282930729638996, 0.0906252509110892, 0.01331811534708916, -0.2761873816588768, 0.0023996447544144418, -0.19876507864245624, -0.09672537934121922, -0.03130507462602495, 0.08874731071997878, -0.04402899839149286, -0.1715333545387486, 0.058331526883749936, 0.07478351717201964, 0.17907295422869798, -0.03652191645323439, -0.15192688113184635, -0.019171066336102126, 0.11330357783744256, 0.09594803781325838, 0.021660898475536178, 0.09538527628783272, -0.13417762696412464, -0.19011067129657097, 0.3746169399026144, -0.012005747338516247, -0.10036475217896344, 0.23036478977853075, -0.08758299109354672, -0.16768163497139907, 0.045624168028746165, 0.12206243473006209, 0.050757797612263365, -0.17915045484747263, 0.11935508598686906, -0.04443844061061665, 0.09884239705834402, 0.1468517373239385, -0.039204495869712044, 0.1964355057378063, 0.16623457170989114, 0.023173611558047293, 0.043178426513781315, 0.01134514705027053, -0.19276577173165224, -0.1979087052910246, -0.132636232221972, -0.13852727097830703, 0.07276883886383914, -0.015220434603509324, -0.16835742207651794, 0.35503662106885037, 0.16050537951638044, 0.09442634052244725, 0.010743723484962562, 0.24132114516841394, 0.06109479351820897, 0.013666635322495523, 0.05858174555963919, 0.21787721182927225, 0.11626158646607067, 0.18798400187524703, -0.1552779330489578, 0.16587660825808914, 0.09123689371735398]
|
707.0855
|
On the Dynamical Behaviour of Cellular Automata
|
In this paper we study the dynamics of 1- and 2- dimensional cellular
automata, using a 2-adic representation of the states, we give a simple
graphical technique for finding periodic solutions. We also study the
continuity properties of the associated 2-adic system and show how to compute
the entropy.
|
nlin.CG
|
in this paper we study the dynamics of 1 and 2 dimensional cellular automata using a 2adic representation of the states we give a simple graphical technique for finding periodic solutions we also study the continuity properties of the associated 2adic system and show how to compute the entropy
|
[['in', 'this', 'paper', 'we', 'study', 'the', 'dynamics', 'of', '1', 'and', '2', 'dimensional', 'cellular', 'automata', 'using', 'a', '2adic', 'representation', 'of', 'the', 'states', 'we', 'give', 'a', 'simple', 'graphical', 'technique', 'for', 'finding', 'periodic', 'solutions', 'we', 'also', 'study', 'the', 'continuity', 'properties', 'of', 'the', 'associated', '2adic', 'system', 'and', 'show', 'how', 'to', 'compute', 'the', 'entropy']]
|
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|
707.0856
|
Searching for tidal tails - investigating galaxy harassment
|
Galaxy harassment has been proposed as a physical process that
morphologically transforms low surface density disc galaxies into dwarf
elliptical galaxies in clusters. It has been used to link the observed very
different morphology of distant cluster galaxies (relatively more blue galaxies
with 'disturbed' morphologies) with the relatively large numbers of dwarf
elliptical galaxies found in nearby clusters. One prediction of the harassment
model is that the remnant galaxies should lie on low surface brightness tidal
streams or arcs. We demonstrate in this paper that we have an analysis method
that is sensitive to the detection of arcs down to a surface brightness of 29 B
mag/arcsec^2 and then use this method to search for arcs around 46 Virgo
cluster dwarf elliptical galaxies. We find no evidence for tidal streams or
arcs and consequently no evidence for galaxy harassment as a viable explanation
for the relatively large numbers of dwarf galaxies found in the Virgo cluster.
|
astro-ph
|
galaxy harassment has been proposed as a physical process that morphologically transforms low surface density disc galaxies into dwarf elliptical galaxies in clusters it has been used to link the observed very different morphology of distant cluster galaxies relatively more blue galaxies with disturbed morphologies with the relatively large numbers of dwarf elliptical galaxies found in nearby clusters one prediction of the harassment model is that the remnant galaxies should lie on low surface brightness tidal streams or arcs we demonstrate in this paper that we have an analysis method that is sensitive to the detection of arcs down to a surface brightness of 29 b magarcsec2 and then use this method to search for arcs around 46 virgo cluster dwarf elliptical galaxies we find no evidence for tidal streams or arcs and consequently no evidence for galaxy harassment as a viable explanation for the relatively large numbers of dwarf galaxies found in the virgo cluster
|
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|
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|
707.0857
|
Large-scale magnetic fields, curvature fluctuations and the thermal
history of the Universe
|
It is shown that gravitating magnetic fields affect the evolution of
curvature perturbations in a way that is reminiscent of a pristine
non-adiabatic pressure fluctuation. The gauge-invariant evolution of curvature
perturbations is used to constrain the magnetic power spectrum. Depending on
the essential features of the thermodynamic history of the Universe, the
explicit derivation of the bound is modified. The theoretical uncertainty in
the constraints on the magnetic energy spectrum is assessed by comparing the
results obtained in the case of the conventional thermal history with the
estimates stemming from less conventional (but phenomenologically allowed)
post-inflationary evolutions.
|
astro-ph
|
it is shown that gravitating magnetic fields affect the evolution of curvature perturbations in a way that is reminiscent of a pristine nonadiabatic pressure fluctuation the gaugeinvariant evolution of curvature perturbations is used to constrain the magnetic power spectrum depending on the essential features of the thermodynamic history of the universe the explicit derivation of the bound is modified the theoretical uncertainty in the constraints on the magnetic energy spectrum is assessed by comparing the results obtained in the case of the conventional thermal history with the estimates stemming from less conventional but phenomenologically allowed postinflationary evolutions
|
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|
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|
707.0858
|
Tracing Magnetic Fields with Aligned Grains
|
Magnetic fields play a crucial role in various astrophysical processes,
including star formation, accretion of matter, transport processes (e.g.,
transport of heat), and cosmic rays. One of the easiest ways to determine the
magnetic field direction is via polarization of radiation resulting from
extinction on or/and emission by aligned dust grains. Reliability of
interpretation of the polarization maps in terms of magnetic fields depends on
how well we understand the grain-alignment theory. Currently the
grain-alignment theory is a predictive one, and its results nicely match
observations. Among its predictions is a subtle phenomenon of radiative
torques. after having stayed in oblivion for many years after its discovery, is
currently viewed as the most powerful means of alignment. In this article, I
shall review the basic physical processes involved in grain alignment, and the
currently known mechanisms of alignment. I shall also discuss possible niches
for different alignment mechanisms. I shall dwell on the importance of the
concept of grain helicity for understanding of many properties of grain
alignment, and shall demonstrate that rather arbitrarily shaped grains exhibit
helicity when they interact with gaseous flows and radiative fluxes.
|
astro-ph
|
magnetic fields play a crucial role in various astrophysical processes including star formation accretion of matter transport processes eg transport of heat and cosmic rays one of the easiest ways to determine the magnetic field direction is via polarization of radiation resulting from extinction on orand emission by aligned dust grains reliability of interpretation of the polarization maps in terms of magnetic fields depends on how well we understand the grainalignment theory currently the grainalignment theory is a predictive one and its results nicely match observations among its predictions is a subtle phenomenon of radiative torques after having stayed in oblivion for many years after its discovery is currently viewed as the most powerful means of alignment in this article i shall review the basic physical processes involved in grain alignment and the currently known mechanisms of alignment i shall also discuss possible niches for different alignment mechanisms i shall dwell on the importance of the concept of grain helicity for understanding of many properties of grain alignment and shall demonstrate that rather arbitrarily shaped grains exhibit helicity when they interact with gaseous flows and radiative fluxes
|
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|
[-0.11204232187038363, 0.16143357487554777, -0.0556205259748102, 0.10357081616623576, -0.06428496621021214, -0.05940988327172351, -0.0002009923965794677, 0.40402884082121643, -0.2727358704663186, -0.3276853467472256, 0.0698270932843636, -0.23723757625084352, -0.11932075930819075, 0.19427071346896377, -0.019731191413061205, -0.025963459301174663, 0.015206206878796619, -0.03128268389668774, -0.008488170793877646, -0.20836567258546976, 0.3324373815143929, 0.09966555564682358, 0.25001558462372, 0.06259728531305862, 0.07057790071479378, -0.022960136021377846, -0.07654953296893939, -0.015645724209523537, -0.1515875487748417, 0.08916821019639345, 0.19702506568133432, 0.10761474582670445, 0.19192194563142437, -0.4820419378419292, -0.22943503444361935, 0.06423210733841586, 0.15748671546382617, 0.08779828718730827, -0.07412831132943906, -0.18878157614645633, 0.015698320321977776, -0.1173416885876042, -0.1522160656899612, -0.041572834453470806, 0.04636805725033659, 0.02823088687152308, -0.23220156847409354, 0.06683564852573909, 0.08905688350407635, 0.0687048975527685, -0.06927880974309668, -0.11023080835438254, -0.05208226716591613, 0.13237346628046456, 0.10515065278974985, 0.016368835514540818, 0.19916927632701428, -0.1885775388598213, -0.11978779634694882, 0.42583304670026756, -0.03673705338552734, -0.13784496693828027, 0.22410342261073166, -0.18311914865252496, -0.14991366249673507, 0.12842094383506295, 0.16009823526230885, 0.12489868816421591, -0.15744814456897765, 0.03993883567711558, 0.011951933654752327, 0.09847477674708369, 0.0548031353466412, 0.08963236226924362, 0.30597577620805666, 0.16907743580968065, 0.002620213052486991, 0.09535749865207761, -0.11499183185592812, -0.1036722286866435, -0.275163865483859, -0.1521603512941277, -0.13349592830253676, 0.081560146021389, -0.08607904630674879, -0.1350840061086225, 0.3670377247757652, 0.16805239060002175, 0.17360810382929157, -0.03346361372779238, 0.2956908176787556, 0.0395122741387639, 0.061682914341376585, 0.05028653311926652, 0.2825312937465422, 0.17592156043819046, 0.11815832733341, -0.22952969734716344, 0.13711562831911014, 0.005528591142439428]
|
707.0859
|
Coherence and clock shifts in ultracold Fermi gases with resonant
interactions
|
Using arguments based on sum rules, we derive a general result for the
average shifts of rf lines in Fermi gases in terms of interatomic interaction
strengths and two-particle correlation functions. We show that near an
interaction resonance shifts vary inversely with the atomic scattering length,
rather than linearly as in dilute gases, thus accounting for the experimental
observation that clock shifts remain finite at Feshbach resonances.
|
cond-mat.str-el cond-mat.supr-con
|
using arguments based on sum rules we derive a general result for the average shifts of rf lines in fermi gases in terms of interatomic interaction strengths and twoparticle correlation functions we show that near an interaction resonance shifts vary inversely with the atomic scattering length rather than linearly as in dilute gases thus accounting for the experimental observation that clock shifts remain finite at feshbach resonances
|
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|
[-0.14134546493722208, 0.24787371349368947, -0.024703861207270354, 0.06899600376639126, 0.0190975708928682, -0.14809449391661964, 0.08922491369268565, 0.42037005566838964, -0.2212756521297869, -0.22822503192148713, -0.036997153922401146, -0.3094174217210332, -0.08528953995694642, 0.20130367643450067, 0.09510925516430567, -0.0009313142205129808, 0.049304741667583585, 0.02647796084186924, -0.11663479861323792, -0.1809519877685095, 0.33018805778675725, 0.06129466706831286, 0.26680476212901855, 0.16012720802604263, 0.037241701599655314, 0.07843182461836667, 0.05926700867712498, -0.019144301261030026, -0.132216541382611, 0.1042410527189165, 0.23799032182606467, -0.02170118818983936, 0.19176593709931666, -0.40905797357823864, -0.20324697043857912, 0.06061170201178696, 0.20367468687802998, 0.16069681219645401, 0.012079295957697305, -0.2880695867143683, -0.06637288349916909, -0.15674281179724234, -0.15725198766188836, -0.09173982286714573, 0.0727108673248162, 0.08386770640013379, -0.27702127321998576, 0.0983644870888275, 0.022152386237380663, 0.16061119985447, -0.12359769940428408, -0.1390191702530094, 0.08719035206056798, 0.06721148441142555, -0.0014207346726264527, 0.0032721841673074817, 0.1795262310292516, -0.10864766645453759, -0.08314626099482707, 0.3967383781642611, -0.16932589303352003, -0.15758493373087093, 0.1898147900321229, -0.1657348722914484, -0.07074941080341589, 0.1922427483907303, 0.14594742074720005, 0.08253234962640858, -0.10085403151921372, 0.038627913568356535, -0.03168134587302582, 0.18781378534413987, 0.12107141193614077, 0.10238131985794614, 0.2118761436874742, 0.09345597891248207, 0.06611684391469654, 0.10783620023450105, -0.11122729823535392, -0.1024736648307307, -0.29011771700053074, -0.04380676570546521, -0.22136771995852242, -0.011255226945921556, -0.03760288750258476, -0.1631961624040755, 0.32942182405281867, 0.14350564101599714, 0.25373559444491167, 0.07047993751631966, 0.27984192738754315, 0.18862950262342537, 0.09200735873918035, 0.01992461213202619, 0.2754886922975585, 0.14911268367397307, 0.027043952154857453, -0.30748853161792034, 0.04660507513960795, 0.05429153876907345]
|
707.086
|
On the Minimum Number of Transmissions in Single-Hop Wireless Coding
Networks
|
The advent of network coding presents promising opportunities in many areas
of communication and networking. It has been recently shown that network coding
technique can significantly increase the overall throughput of wireless
networks by taking advantage of their broadcast nature. In wireless networks,
each transmitted packet is broadcasted within a certain area and can be
overheard by the neighboring nodes. When a node needs to transmit packets, it
employs the opportunistic coding approach that uses the knowledge of what the
node's neighbors have heard in order to reduce the number of transmissions.
With this approach, each transmitted packet is a linear combination of the
original packets over a certain finite field.
In this paper, we focus on the fundamental problem of finding the optimal
encoding for the broadcasted packets that minimizes the overall number of
transmissions. We show that this problem is NP-complete over GF(2) and
establish several fundamental properties of the optimal solution. We also
propose a simple heuristic solution for the problem based on graph coloring and
present some empirical results for random settings.
|
cs.IT cs.NI math.IT
|
the advent of network coding presents promising opportunities in many areas of communication and networking it has been recently shown that network coding technique can significantly increase the overall throughput of wireless networks by taking advantage of their broadcast nature in wireless networks each transmitted packet is broadcasted within a certain area and can be overheard by the neighboring nodes when a node needs to transmit packets it employs the opportunistic coding approach that uses the knowledge of what the nodes neighbors have heard in order to reduce the number of transmissions with this approach each transmitted packet is a linear combination of the original packets over a certain finite field in this paper we focus on the fundamental problem of finding the optimal encoding for the broadcasted packets that minimizes the overall number of transmissions we show that this problem is npcomplete over gf2 and establish several fundamental properties of the optimal solution we also propose a simple heuristic solution for the problem based on graph coloring and present some empirical results for random settings
|
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|
[-0.22632374203021755, 0.032382045487545176, -0.04944971620253372, -0.007941572140142935, -0.08156740480494178, -0.19581275755825284, 0.1357922320107305, 0.3935319143770771, -0.31200217229144817, -0.286469475032804, 0.0812941952873106, -0.2739807730249595, -0.22927417889480817, 0.14164542898652144, -0.13002380951895082, 0.07595796225095083, 0.08152107762527355, 0.10157946943813427, 0.006579703124853867, -0.3139036242218109, 0.28033496731553564, 0.06654787021794949, 0.3521992129390128, 0.055917968591198915, 0.10073989761771042, 0.05781997948757966, -0.02311598529129035, -0.0005239733476297591, -0.06878739186322491, 0.12887075021717465, 0.3214814893885473, 0.2219237038026966, 0.3427010622002523, -0.446555070081641, -0.2869728142071505, 0.11245903914889575, 0.18703851245399247, 0.12199973617085065, -0.04523562463939677, -0.25583377142241015, 0.141397514502883, -0.19491369246018372, -0.029087992771316996, 0.004709272354375571, -0.0222668803729572, 0.06253810894717886, -0.2670600012219934, -0.018461218987629927, -0.015629842041314325, -0.014062980893703008, -0.032802338211860675, -0.07588724901275286, 0.04293496322960974, 0.16819092016935014, 0.01941941594189054, 0.03028295434672724, 0.061547514971938326, -0.09120335583164971, -0.1352906258529794, 0.38810441160405224, 0.026524440056660256, -0.199792720575219, 0.10759782237768047, -0.05085106102342252, -0.12859386481564303, 0.14704199670251744, 0.2265506851148199, 0.07898923226192975, -0.1522363183947329, 0.04238882382262752, -0.06489057922524145, 0.1682785855796696, 0.10161728055920155, 0.10593864615128207, 0.13791053963888605, 0.1953033431884912, 0.16221176064771664, 0.15174943555889928, -0.07659297169514255, -0.09219276828860695, -0.2216020677852529, -0.11844388433118266, -0.242707434908053, 0.022800728138959545, -0.12128030597357958, -0.08438847613549362, 0.4275868976361711, 0.16255970163778824, 0.14812730759678577, 0.11017484687247568, 0.36304744254713034, 0.09850915267386219, 0.07963459399516895, 0.16081816945172084, 0.17912918400229086, 0.10059261364685054, 0.1156025854804532, -0.17312127212327058, 0.10716924311683132, 0.04030872182920575]
|
707.0861
|
Data-driven efficient score tests for deconvolution problems
|
We consider testing statistical hypotheses about densities of signals in
deconvolution models. A new approach to this problem is proposed. We
constructed score tests for the deconvolution with the known noise density and
efficient score tests for the case of unknown density. The tests are
incorporated with model selection rules to choose reasonable model dimensions
automatically by the data. Consistency of the tests is proved.
|
math.ST stat.AP stat.TH
|
we consider testing statistical hypotheses about densities of signals in deconvolution models a new approach to this problem is proposed we constructed score tests for the deconvolution with the known noise density and efficient score tests for the case of unknown density the tests are incorporated with model selection rules to choose reasonable model dimensions automatically by the data consistency of the tests is proved
|
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|
[-0.03952287146105216, 0.0011440213626393906, -0.10255837934270788, 0.12423773178866562, -0.036428692220495294, -0.18413948920340492, 0.06846821809617373, 0.38453316619763006, -0.19395843039338406, -0.3540573203792939, 0.12543326982905945, -0.23591493729215401, -0.11483612751158384, 0.13462178852552406, -0.0786235601712878, 0.12823674836410925, 0.07128722882256484, 0.01987279415703737, -0.0778726651548193, -0.2825295878466792, 0.2675936579990845, 0.09973000580301651, 0.3284701647093663, -0.044016109206355535, 0.11662301289884804, -0.00842848291190771, -0.07096656076610089, 0.03135246448218822, -0.14388799887652007, 0.11042753480768834, 0.2354342234847606, 0.21929452333312768, 0.2933406809774729, -0.37124353068379257, -0.24000221351878, 0.09738040394687023, 0.03856949710931915, 0.08599984467459412, -0.026221706868650822, -0.3139693210582034, 0.09259801915703485, -0.09783690285985358, -0.11602441507319991, -0.12885320155093302, -0.0430868831033317, -0.007614408791638338, -0.41711406510036725, 0.1196029062024676, 0.03194068667407219, 0.019355524825648618, -0.05168921085647665, -0.14357143765888536, 0.06275884815706656, 0.09054599004582717, 0.09800091981350516, -0.030986791018110055, 0.10669510580169467, -0.14699292292890068, -0.12791547136237988, 0.35237314850091933, -0.051455207989336206, -0.2672916310194593, 0.17118782988534523, -0.07769756201081551, -0.19117654962465166, 0.07605156219349457, 0.1759465147096377, 0.11348378627489393, -0.1952960156620695, 0.03778938893139219, -0.04910447377210053, 0.1904990455135703, 0.03549314862690293, -0.062372716817145166, 0.17221237713327775, 0.1952416075536838, 0.01664414441642853, 0.13540175929665565, -0.14567802554856127, -0.03690266487403558, -0.3149304518502994, -0.10680360480283316, -0.19646065607666968, -0.04324337831483437, -0.10430634655752398, -0.13865094021535837, 0.3930141038619555, 0.23877884124477322, 0.13808837134006002, 0.1019052093132184, 0.31688506063073874, 0.1292388893520603, 0.07012277526172021, 0.06016011417556841, 0.19677433589330087, 0.14614184395983243, -0.008209918811917304, -0.14526346511511992, 0.08868792976181095, 0.036982953376494924]
|
707.0862
|
Scheduling in Data Intensive and Network Aware (DIANA) Grid Environments
|
In Grids scheduling decisions are often made on the basis of jobs being
either data or computation intensive: in data intensive situations jobs may be
pushed to the data and in computation intensive situations data may be pulled
to the jobs. This kind of scheduling, in which there is no consideration of
network characteristics, can lead to performance degradation in a Grid
environment and may result in large processing queues and job execution delays
due to site overloads. In this paper we describe a Data Intensive and Network
Aware (DIANA) meta-scheduling approach, which takes into account data,
processing power and network characteristics when making scheduling decisions
across multiple sites. Through a practical implementation on a Grid testbed, we
demonstrate that queue and execution times of data-intensive jobs can be
significantly improved when we introduce our proposed DIANA scheduler. The
basic scheduling decisions are dictated by a weighting factor for each
potential target location which is a calculated function of network
characteristics, processing cycles and data location and size. The job
scheduler provides a global ranking of the computing resources and then selects
an optimal one on the basis of this overall access and execution cost. The
DIANA approach considers the Grid as a combination of active network elements
and takes network characteristics as a first class criterion in the scheduling
decision matrix along with computation and data. The scheduler can then make
informed decisions by taking into account the changing state of the network,
locality and size of the data and the pool of available processing cycles.
|
cs.DC
|
in grids scheduling decisions are often made on the basis of jobs being either data or computation intensive in data intensive situations jobs may be pushed to the data and in computation intensive situations data may be pulled to the jobs this kind of scheduling in which there is no consideration of network characteristics can lead to performance degradation in a grid environment and may result in large processing queues and job execution delays due to site overloads in this paper we describe a data intensive and network aware diana metascheduling approach which takes into account data processing power and network characteristics when making scheduling decisions across multiple sites through a practical implementation on a grid testbed we demonstrate that queue and execution times of dataintensive jobs can be significantly improved when we introduce our proposed diana scheduler the basic scheduling decisions are dictated by a weighting factor for each potential target location which is a calculated function of network characteristics processing cycles and data location and size the job scheduler provides a global ranking of the computing resources and then selects an optimal one on the basis of this overall access and execution cost the diana approach considers the grid as a combination of active network elements and takes network characteristics as a first class criterion in the scheduling decision matrix along with computation and data the scheduler can then make informed decisions by taking into account the changing state of the network locality and size of the data and the pool of available processing cycles
|
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|
[-0.17642501628969467, 0.03230911470522265, -0.08252782724319381, 0.0239220623838342, -0.10112688180189652, -0.16739560254208077, 0.1377779186946967, 0.4265725303455781, -0.27890388987929443, -0.34231094256811684, 0.15333904489849473, -0.2340259133911273, -0.08723941690230502, 0.16414978059714458, -0.11383460093335364, 0.06564860029670623, 0.15351145993193416, 0.030423551892086224, 0.008953933173053126, -0.2835608613242464, 0.25934553256390636, 0.1007728408505698, 0.3350959149975663, 0.030021591742562876, 0.06373752245961137, 0.02649777552931921, -0.04948233106333929, 0.0063574861102974846, -0.047483791706949725, 0.09086620773170424, 0.30051925553304254, 0.20965204468261495, 0.3304652073003845, -0.4964022731176552, -0.1825367586138198, 0.1001071421527358, 0.13002376821696585, 0.049048525098134156, 0.011160678683203945, -0.2582462875893637, 0.07034568272935089, -0.17497904138124987, -0.02023990108841733, -0.07349934536014259, 0.014267667968565387, 0.022010658095782832, -0.3258641967078823, -0.035547306619816484, -0.007222246163042719, 0.008440351298095655, -0.0540153209286731, -0.10528976609930396, -0.0023646969103584144, 0.16594495405175755, 0.04832740149149084, 0.00495566995560775, 0.1825941780524089, -0.12246847440532123, -0.14164420829520558, 0.43040739033182773, 0.034074394778866715, -0.18333065939219198, 0.13257771496912862, -0.043617697564906764, -0.17105508205509865, 0.11311667408533249, 0.25693442973630787, 0.041694354954454685, -0.18573250327948282, 0.004520343334399569, 0.012987247139128497, 0.1556034571140577, 0.041768067812634056, 0.02745408985214779, 0.15952427148663145, 0.24406295083644383, 0.0914786241365169, 0.14352246903558896, -0.059088879378362116, -0.11239394988205124, -0.22389629519393248, -0.1399591998468925, -0.21513186881938362, 0.021249152701402423, -0.11683522380359837, -0.11949270308753367, 0.39264491441431326, 0.15043520315501346, 0.18025704903042503, 0.0920535513576517, 0.3677869068734087, 0.08260773461908175, 0.12266442412148132, 0.16456156864341942, 0.10547792792668138, -0.017300922193941352, 0.15435995966928073, -0.19732317290765303, 0.12481953360770869, 0.00020123844973540027]
|
707.0863
|
Kinetic description of hadron-hadron collisions
|
A transport model based on the mean free path approach to describe pp
collisions is proposed. We assume that hadrons can be treated as bags of
partons similarly to the MIT bag model. When the energy density in the
collision is higher than a critical value, the bags break and partons are
liberated. The partons expand and can make coalescence to form new hadrons. The
results obtained compare very well with available data and some prediction for
higher energies collisions are discussed. Based on the model we suggest that a
QGP could already be formed in the pp collisions at high energies.
|
hep-ph
|
a transport model based on the mean free path approach to describe pp collisions is proposed we assume that hadrons can be treated as bags of partons similarly to the mit bag model when the energy density in the collision is higher than a critical value the bags break and partons are liberated the partons expand and can make coalescence to form new hadrons the results obtained compare very well with available data and some prediction for higher energies collisions are discussed based on the model we suggest that a qgp could already be formed in the pp collisions at high energies
|
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|
[-0.02732918875328466, 0.2453038018132907, -0.17342138124912904, 0.14848362869701767, -0.04556428358031839, -0.08718441216293357, -0.03457889862029868, 0.3823703544022625, -0.1938630111844224, -0.284283179543255, 0.013784688822103335, -0.3388903688219394, 0.015701252200147685, 0.1250699359635987, 0.017367089833772064, 0.049990726712470256, 0.14611068840581448, 0.062275625874891, -0.03394063353520252, -0.22532191915967154, 0.31267795528230424, 0.0915476525311961, 0.25850739382097826, 0.1652592427597162, 0.06307955592637882, 0.026318975265466553, 0.024242043408437396, 0.04118045744047884, -0.11361013042044885, 0.07363272565456938, 0.23958072657970822, 0.05496655437744659, 0.1830573503827384, -0.4298905336444138, -0.23433247556243383, 0.07054379895585132, 0.15811381902655258, 0.14622675721058806, -0.033343224961986294, -0.24856168098345982, 0.11617776118937935, -0.21907191263630474, -0.11855765613362047, -0.0742194394092532, -0.04383025271361511, 0.03432064063792281, -0.28859014384558096, 0.08693645669457813, -0.039940124303422066, -0.012798473257206235, -0.07601396307148331, -0.1947936810616988, -0.06634847529679902, 0.03902514090255935, 0.059232509887877705, 0.08891525143739201, 0.1520058318068657, -0.16654554864861912, -0.12239461078071127, 0.4403289619321917, -0.02204627119413892, -0.16065130029421518, 0.24278879292564942, -0.15957897957231776, -0.09536474460151557, 0.13490454055478468, 0.22631525809707703, 0.11503398966263323, -0.1996479932723542, -0.007951563983749342, -0.0184548492143935, 0.15411679914184645, 0.08818928703583558, 0.023224930514070187, 0.17545851994530975, 0.19331442396494322, -0.03873374907519011, 0.1171639667248682, -0.060963511872150954, -0.09852750470186127, -0.34236739273639577, -0.11235233007099334, -0.18478376680400735, 0.0058806553647360385, -0.06670092726448738, -0.09765601201969035, 0.3187192219067548, 0.1705052650478833, 0.30141098399226574, 0.011556907191726506, 0.262169397326515, 0.1346840457066291, 0.0716965359261296, 0.16181918595205336, 0.25591636430523496, 0.08308224313819379, 0.13794737345739908, -0.17997194801037217, 0.056151883658386914, 0.07801281949779128]
|
707.0864
|
Self-gravitating radiation in AdS(d)
|
We study spherically symmetric equilibrium configurations of self-gravitating
massless thermal radiation in asymptotically anti-de Sitter space. In d=4, it
was shown by Page and Phillips that there is a maximum red-shifted temperature,
maximum mass and maximum entropy. For higher central densities, the
temperature, mass and entropy undergo an infinite series of damped
oscillations, corresponding to unstable configurations. We extend this work to
all dimensions $d\geq 3$. We find that in $4\leq d\leq 10$, the behaviour is
similar to the d=4 case. In $d\geq 11$, the temperature, mass and entropy are
monotonic functions of the central density, asymptoting to their maxima as the
central density goes to infinity. In d=3, an exact solution is given by a slice
of the AdS C-metric.
|
gr-qc hep-th
|
we study spherically symmetric equilibrium configurations of selfgravitating massless thermal radiation in asymptotically antide sitter space in d4 it was shown by page and phillips that there is a maximum redshifted temperature maximum mass and maximum entropy for higher central densities the temperature mass and entropy undergo an infinite series of damped oscillations corresponding to unstable configurations we extend this work to all dimensions dgeq 3 we find that in 4leq dleq 10 the behaviour is similar to the d4 case in dgeq 11 the temperature mass and entropy are monotonic functions of the central density asymptoting to their maxima as the central density goes to infinity in d3 an exact solution is given by a slice of the ads cmetric
|
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|
[-0.13084393940492695, 0.19165194975640357, -0.05678820897909728, 0.09048575204258308, 0.008609952712970331, -0.13177057943299167, -0.009568248267385586, 0.3293854166130143, -0.12860714945526533, -0.24333718972480742, 0.10099394328041726, -0.33130852520188764, -0.08046921590450874, 0.111054721934921, -0.049567636502675774, 0.054356998625434624, -0.05834465875282637, 0.07848584060056889, -0.10781681847042782, -0.261750246136457, 0.3186659947083878, 0.0625430586755522, 0.2579801221231907, 0.04301365850924337, 0.05881074875879894, -0.012488817202970232, 0.028515677764426824, 0.05157167451385955, -0.21325214302012396, 0.015833746930507344, 0.23819457853505435, 0.114935048688434, 0.19575953963097215, -0.3349897008743291, -0.2079855501189951, 0.1426991761069406, 0.1799462225551771, 0.11902169196400791, -0.02745812728520952, -0.20316436348583025, 0.08364375831543906, -0.1796170734946639, -0.23585793700777302, -0.032691189291894684, 0.11359653239761872, -0.03391799404024154, -0.24507722344003185, 0.157761128119016, 0.07702204554287856, 0.007936687747493756, -0.12017616800086434, -0.07150907402719595, -0.1115258929304286, 0.06734448256094225, 0.08261939686384391, 0.057415690082548695, 0.141269715318133, -0.10021356052010943, -0.07427556342483799, 0.29751303215503444, -0.09001559186111058, -0.18330738410615355, 0.1880671805509728, -0.2245619628609212, -0.11900600587394981, 0.17234214078365587, 0.12255391338647705, 0.195640051137071, -0.11864938848644249, 0.14994645400226794, -0.02182438659620248, 0.17047906644384508, 0.16920244696450013, -0.026889887576815017, 0.24689125691055636, 0.07616716735295889, 0.09427680051115857, 0.19045928241454127, -0.032875226137097466, -0.12164000736949734, -0.31554032520444925, -0.16049837537613998, -0.1708034676247592, 0.12259226223677089, -0.18500780610488882, -0.1714444663382832, 0.3158075899647718, 0.11251297255223694, 0.1939263452414023, 0.07238790412887561, 0.22159704938458763, 0.14521776565277472, 0.017738031590942387, 0.1731930650070248, 0.24374867780980738, 0.15792954286987593, 0.12911635929764795, -0.2125482709100855, -0.10048353388012687, 0.10643511342100245]
|
707.0865
|
Spectral properties of singular Sturm-Liouville operators with
indefinite weight sgn x
|
We consider a singular Sturm-Liouville expression with the indefinite weight
sgn x. To this expression there is naturally a self-adjoint operator in some
Krein space associated. We characterize the local definitizability of this
operator in a neighbourhood of $\infty$. Moreover, in this situation, the point
$\infty$ is a regular critical point. We construct an operator $A=(\sgn
x)(-d^2/dx^2+q)$ with non-real spectrum accumulating to a real point. The
obtained results are applied to several classes of Sturm-Liouville operators.
|
math.SP math.CA
|
we consider a singular sturmliouville expression with the indefinite weight sgn x to this expression there is naturally a selfadjoint operator in some krein space associated we characterize the local definitizability of this operator in a neighbourhood of infty moreover in this situation the point infty is a regular critical point we construct an operator asgn xd2dx2q with nonreal spectrum accumulating to a real point the obtained results are applied to several classes of sturmliouville operators
|
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|
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|
707.0866
|
Supersolidity, entropy and frustration
|
We study the properties of t-t'-V model of hard-core bosons on the triangular
lattice that can be realized in optical lattices. By mapping to the spin-1/2
XXZ model in a field, we determine the phase diagram of the t-V model where the
supersolid characterized by the ordering pattern (x,x,-2x') ("ferrimagnetic" or
SS A) is a ground state for chemical potential \mu >3V. By turning on either
temperature or t' at half-filling \mu =3V, we find a first order transition
from SS A to the elusive supersolid characterized by the (x,-x,0) ordering
pattern ("antiferromagnetic" or SS C). In addition, we find a large region
where a superfluid phase becomes a solid upon raising temperature at fixed
chemical potential. This is an analog of the Pomeranchuk effect driven by the
large entropic effects associated with geometric frustration on the triangular
lattice.
|
cond-mat.str-el cond-mat.supr-con
|
we study the properties of ttv model of hardcore bosons on the triangular lattice that can be realized in optical lattices by mapping to the spin12 xxz model in a field we determine the phase diagram of the tv model where the supersolid characterized by the ordering pattern xx2x ferrimagnetic or ss a is a ground state for chemical potential mu 3v by turning on either temperature or t at halffilling mu 3v we find a first order transition from ss a to the elusive supersolid characterized by the xx0 ordering pattern antiferromagnetic or ss c in addition we find a large region where a superfluid phase becomes a solid upon raising temperature at fixed chemical potential this is an analog of the pomeranchuk effect driven by the large entropic effects associated with geometric frustration on the triangular lattice
|
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|
[-0.17996341262714585, 0.2633001970548387, -0.05144386058943211, 0.023177983277254618, -0.029784549737983532, -0.14926685620963143, 0.1289407029069717, 0.35681521224256174, -0.2824472401129163, -0.22500044637717362, 0.09448237458760243, -0.30028078804953373, -0.11883859260621872, 0.09397535358785071, 0.06476569042580735, 0.0006005369566306741, -0.04714832175860478, 0.04277596090906772, -0.1226097851893797, -0.1893340322000069, 0.30251436303302215, -0.011664176245044539, 0.22954862038402454, 0.05446625997875885, 0.05048022880488871, 0.013624761526074692, 0.10909131679521955, 0.03297442862548042, -0.19502952068132404, 0.008644295350203047, 0.17726133695628116, -0.06777808027328465, 0.15973993203859183, -0.3573172089603284, -0.21916398810951607, 0.12266749520010005, 0.12387462957775679, 0.13770986611084285, -0.07300309137950746, -0.3051104715120965, 0.043068708475692656, -0.19628852089543058, -0.13924913259899663, -0.07956376498855272, 0.007190057836587716, -0.01912463730558807, -0.2881513136587497, 0.09474810262369263, 0.0842310634586771, 0.12630965200968194, -0.06312365032584015, -0.12977102300678584, -0.06995586518441206, 0.033309079124592245, -0.01514852246981573, 0.11352563721289777, 0.08691264819893715, -0.1557264144960926, -0.11469437920933832, 0.40752820624038577, -0.07631654059936198, -0.12696792415437708, 0.1786709213629365, -0.1670397103973327, -0.08752401774087785, 0.15064135077409446, 0.13267821723770729, 0.03626340460977045, -0.11156866274625603, 0.11568145881123516, -0.02299209675360201, 0.209584873372122, 0.010081457196856323, -0.004896433693289325, 0.2801916275875292, 0.20577954402044957, 0.07840190842693699, 0.20786146255989518, -0.10850619629828556, -0.11207376444287112, -0.23571036250559965, -0.11856078724984241, -0.24558559952951645, 0.04115642841729889, -0.08548485731665531, -0.17133796543044888, 0.3808550003214159, 0.11135265916464446, 0.23473930966271006, -0.06123523849933206, 0.226297884285315, 0.11610955079389818, 0.035790872885811856, 0.020397391495045165, 0.20877191516827198, 0.11501428152711225, 0.09475842686167554, -0.2903845801500712, 0.03819622666291569, 0.09756131246146085]
|
707.0867
|
Frame dragging and super-energy
|
We show that the vorticity appearing in stationary vacuum spacetimes is
always related to the existence of a flow of super-energy on the plane
orthogonal to the vorticity vector. This result, toghether with the previously
established link between vorticity and super--energy in radiative (Bondi-Sachs)
spacetimes strength further the case for this latter quantity as the cause of
frame dragging.
|
gr-qc math-ph math.MP
|
we show that the vorticity appearing in stationary vacuum spacetimes is always related to the existence of a flow of superenergy on the plane orthogonal to the vorticity vector this result toghether with the previously established link between vorticity and superenergy in radiative bondisachs spacetimes strength further the case for this latter quantity as the cause of frame dragging
|
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|
[-0.20505353702642656, 0.11259469586440314, -0.06192877510132394, 0.05862419678379734, -0.08945218847780409, -0.06805974691001287, -0.0486930582230374, 0.32151833345513725, -0.24848532038977592, -0.20766955879280122, 0.04410941533002434, -0.20893167377591637, -0.10931293476941221, 0.17707300793095412, -0.04412822875241607, 0.04057168308645487, 0.02261180236493632, 0.07618729542088458, -0.059224339545372935, -0.19055337090266206, 0.39251129026130094, 0.07417603039135368, 0.3057880261439388, 0.04501759414008613, 0.09887065095984834, -0.029047156510464217, -0.035597419979887364, 0.053114182852461174, -0.1621452880737429, 0.05120107899341038, 0.1936849646617548, 0.08850721939924662, 0.19657127417316186, -0.35540696268238253, -0.2231783941230279, 0.11156749642963158, 0.12743967878869025, 0.14046102090367762, -0.03599882376838034, -0.2809382209424087, 0.06538680505986183, -0.13067798827916888, -0.1744783821405243, -0.028895808940248218, 0.045554525708243, 0.01530063761619188, -0.23069361815134348, 0.15027720031281144, 0.11478120047535936, 0.023072500807880345, -0.1250193594970693, -0.05968546250961342, -0.07745866900530912, 0.07850370476401206, 0.18986463162779682, 0.10719145318666884, 0.0888712840644106, -0.135430543091527, -0.0834974708367076, 0.39536837448950035, -0.09403108595475806, -0.3220747157110501, 0.1289082421463425, -0.1700482244871683, -0.0720388215761316, 0.09076764743964551, 0.13885948106141413, 0.12126542750935433, -0.07977565739430108, 0.04883879287290718, -0.08304952861646474, 0.0751599104980291, 0.15459507064483427, 0.042807065960714374, 0.2206892093517265, 0.01456197959733969, 0.09424819249533496, 0.1514802921594957, -0.08214827602871268, -0.13326925122755248, -0.3960143698979232, -0.21106518580878186, -0.17339010266153046, 0.07766844903639818, -0.09984291627410191, -0.1936411096840718, 0.3641630190787679, 0.13254941808912207, 0.1531675552033772, 0.03093502792071993, 0.29696850836971556, 0.09802903119529897, 0.050162123184714275, 0.12192488661414738, 0.3495339481949301, 0.2037273610358016, 0.1769993454612539, -0.24395362859970685, 0.006149589802312143, 0.13059546741641173]
|
707.0868
|
Light Nuclei as Quantized Skyrmions
|
We consider the rigid body quantization of Skyrmions with topological charges
1 to 8, as approximated by the rational map ansatz. Novel, general expressions
for the elements of the inertia tensors, in terms of the approximating rational
map, are presented and are used to determine the kinetic energy contribution to
the total energy of the ground and excited states of the quantized Skyrmions.
Our results are compared to the experimentally determined energy levels of the
corresponding nuclei, and the energies and spins of a few as yet unobserved
states are predicted.
|
hep-th nucl-th
|
we consider the rigid body quantization of skyrmions with topological charges 1 to 8 as approximated by the rational map ansatz novel general expressions for the elements of the inertia tensors in terms of the approximating rational map are presented and are used to determine the kinetic energy contribution to the total energy of the ground and excited states of the quantized skyrmions our results are compared to the experimentally determined energy levels of the corresponding nuclei and the energies and spins of a few as yet unobserved states are predicted
|
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|
[-0.11865185449861891, 0.17501600657635788, -0.015651017637247897, 0.09154645464086271, -0.001790619767424497, -0.08016640288182177, 0.032109507564250586, 0.33382642834068654, -0.25154589719886145, -0.33681421115953514, 0.05044116094007392, -0.3032620731372755, -0.07769681625886933, 0.14695805028735937, 0.004080303719492404, 0.06182496025544274, -0.0035123105063666026, 0.07675555220979093, -0.07365654431447223, -0.18777119680717178, 0.3221094642794924, 0.04037030524277425, 0.24371817789889955, 0.06531090575915116, 0.1387607476182773, -0.045559452836411996, 0.022273877134116795, 0.02128708469527927, -0.13776666364008253, 0.17269954414255304, 0.2499205151388606, 0.017297538304394417, 0.1637718660736477, -0.446485898570045, -0.16329737969131752, 0.08787820671408714, 0.12591139219220276, 0.14492646434119197, -0.01342555446611656, -0.29120010296701565, 0.11046528471070904, -0.18174179083575587, -0.16129707568069243, -0.1456754173121446, 0.029945138759992936, 0.06311784834079034, -0.2290769207936067, 0.07518676787123575, 0.02614533082469479, 0.03206270776566241, -0.15179024918700804, -0.17815975412844096, -0.08149299033467176, 0.14572019150971874, 0.06620048750115169, 0.008140489807004457, 0.13877264952675983, -0.1396828814010535, -0.12633610737336043, 0.3954045767793534, -0.016550468705635476, -0.2395986551684353, 0.14514324735276973, -0.12434939700844032, -0.064147312879808, 0.14912380534735928, 0.13701722640953548, 0.14663160602807754, -0.10912944807333279, 0.05506222641126222, -0.01360283259834562, 0.12057512698203816, 0.041626064628772025, 0.04983117756661498, 0.20194007031578612, 0.08663064889241379, 0.029898913075717595, 0.14279582496005838, -0.09926827181806112, -0.10782465628593914, -0.3124012626646148, -0.13722897537953252, -0.23707775360070538, 0.037439500575291586, -0.03476958270990648, -0.1314945928445393, 0.43956026173411655, 0.06690527026920201, 0.21432576815669352, 0.05825936605969628, 0.25292457910868654, 0.16291386402112298, 0.0422093109457989, 0.052161643167722274, 0.2814354749810933, 0.1723705798177724, 0.04221023555722211, -0.22371110450578752, 0.0016643146288345804, 0.0637257060875277]
|
707.0869
|
Convexity of the self-energy functional in the variational cluster
approximation
|
In the variational cluster approximation (VCA) (or variational cluster
perturbation theory), widely used to study the Hubbard model, a fundamental
problem that renders variational solutions difficult in practice is its known
lack of convexity at stationary points, i.e. the physical solutions can be
saddle points rather than extrema of the self-energy functional. Here we
suggest two different approaches to construct a convex functional of the
self-energy. In the first approach, one can show analytically that in the
approximation where the irreducible particle-hole vertex depends only on center
of mass coordinates, the functional is convex away from phase transitions in
the corresponding channel. Numerical tests on a tractable version of that
functional show that convexity can be a nuisance when looking for instabilities
both in the pairing and particle-hole channels. Therefore, an alternative
phenomenological functional is proposed. Convexity is explicitly enforced only
with respect to a restricted set of variables, such as the cluster chemical
potential that is known to be otherwise problematic. Numerical tests show that
our functional is convex at the physical solutions of VCA and allows
second-order phase transitions in the pairing channel as well. This opens the
way to the use of more efficient algorithms to find solutions of the VCA
equations.
|
cond-mat.str-el cond-mat.supr-con
|
in the variational cluster approximation vca or variational cluster perturbation theory widely used to study the hubbard model a fundamental problem that renders variational solutions difficult in practice is its known lack of convexity at stationary points ie the physical solutions can be saddle points rather than extrema of the selfenergy functional here we suggest two different approaches to construct a convex functional of the selfenergy in the first approach one can show analytically that in the approximation where the irreducible particlehole vertex depends only on center of mass coordinates the functional is convex away from phase transitions in the corresponding channel numerical tests on a tractable version of that functional show that convexity can be a nuisance when looking for instabilities both in the pairing and particlehole channels therefore an alternative phenomenological functional is proposed convexity is explicitly enforced only with respect to a restricted set of variables such as the cluster chemical potential that is known to be otherwise problematic numerical tests show that our functional is convex at the physical solutions of vca and allows secondorder phase transitions in the pairing channel as well this opens the way to the use of more efficient algorithms to find solutions of the vca equations
|
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|
[-0.11502356460579194, 0.047237749311507954, -0.1387427081535684, 0.11621498290915042, -0.08367987485011903, -0.13427971323452345, 0.08839966471409198, 0.35014833980126353, -0.29791234619915485, -0.24777210945087463, 0.07373482556388963, -0.27582884056375806, -0.16598129684911905, 0.14514725224410252, -0.021417193745671793, 0.06462885855509695, 0.03446235806999228, 0.039071654355744036, -0.11252597644925118, -0.21317992509320016, 0.3297785578783965, -0.006986524793887284, 0.2491598340353315, 0.05635840041653776, 0.05844652824467275, 0.0054392792199306735, 0.055603578714540275, 0.041864529701812966, -0.09786278576605738, 0.08153035226618735, 0.27443206718464086, 0.09116156283175436, 0.29776217448184406, -0.43949801429379276, -0.2199723596207616, 0.07647560695413409, 0.16360569564943633, 0.12935474006368256, -0.017636546599692892, -0.2613437053792905, 0.07725378144617624, -0.1505042267690708, -0.15499562210198947, -0.12852882123892992, -0.022316718160560946, 0.02718284446746111, -0.2904046553891243, 0.11029532404343893, -0.0006903107381687022, 0.010563955783117107, -0.09625312517959307, -0.11993527081000005, -0.034113446893965504, 0.06808470815218554, 0.061135518109115695, 0.061077187131954036, 0.111024699332874, -0.11768746186933685, -0.09134863210279813, 0.3947174638328029, -0.012555174843944814, -0.24636544283570314, 0.2072299028934184, -0.11099535796745885, -0.14121518360632584, 0.11776998266123417, 0.12393996158569325, 0.13611824235356434, -0.18793847876545552, 0.12796743421236098, -0.025275637777295055, 0.16801048052190554, 0.023951415142907603, 0.010405596594394344, 0.14571159950077034, 0.13630084771117787, 0.12872894177349603, 0.13540742334898379, -0.06487377661212189, -0.1476643525245713, -0.3285268842628816, -0.1154828034550031, -0.2102982500267056, 0.0018128642721510514, -0.10304280704713609, -0.19714841785398454, 0.378514164223949, 0.14916937318971243, 0.15174995032479852, 0.04701881026394847, 0.28411515125686804, 0.15869124200906343, 0.07144935947002434, 0.07791603691421631, 0.2517398715030584, 0.1388610426245666, 0.0074514948649377355, -0.22537667071446776, 0.06442834912435856, 0.0770277297919298]
|
707.087
|
Two-Dimensional Dynamics of Ultracold Atoms in Optical Lattices
|
We analyze the dynamics of ultracold atoms in optical lattices induced by a
sudden shift of the underlying harmonic trapping potential. In order to study
the effect of strong interactions, dimensionality and lattice topology on
transport properties, we consider bosonic atoms with arbitrarily strong
repulsive interactions, on a two-dimensional square lattice and a hexagonal
lattice. On the square lattice we find insulating behavior for weakly
interacting atoms and slow relaxation for strong interactions, even when a Mott
plateau is present, which in one dimension blocks the dynamics. On the
hexagonal lattice the center of mass relaxes to the new equilibrium for any
interaction strength.
|
cond-mat.other
|
we analyze the dynamics of ultracold atoms in optical lattices induced by a sudden shift of the underlying harmonic trapping potential in order to study the effect of strong interactions dimensionality and lattice topology on transport properties we consider bosonic atoms with arbitrarily strong repulsive interactions on a twodimensional square lattice and a hexagonal lattice on the square lattice we find insulating behavior for weakly interacting atoms and slow relaxation for strong interactions even when a mott plateau is present which in one dimension blocks the dynamics on the hexagonal lattice the center of mass relaxes to the new equilibrium for any interaction strength
|
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|
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|
707.0871
|
Optimal Linear Precoding Strategies for Wideband Non-Cooperative Systems
based on Game Theory-Part II: Algorithms
|
In this two-part paper, we address the problem of finding the optimal
precoding/multiplexing scheme for a set of non-cooperative links sharing the
same physical resources, e.g., time and bandwidth. We consider two alternative
optimization problems: P.1) the maximization of mutual information on each
link, given constraints on the transmit power and spectral mask; and P.2) the
maximization of the transmission rate on each link, using finite order
constellations, under the same constraints as in P.1, plus a constraint on the
maximum average error probability on each link. Aiming at finding decentralized
strategies, we adopted as optimality criterion the achievement of a Nash
equilibrium and thus we formulated both problems P.1 and P.2 as strategic
noncooperative (matrix-valued) games. In Part I of this two-part paper, after
deriving the optimal structure of the linear transceivers for both games, we
provided a unified set of sufficient conditions that guarantee the uniqueness
of the Nash equilibrium. In this Part II, we focus on the achievement of the
equilibrium and propose alternative distributed iterative algorithms that solve
both games. Specifically, the new proposed algorithms are the following: 1) the
sequential and simultaneous iterative waterfilling based algorithms,
incorporating spectral mask constraints; 2) the sequential and simultaneous
gradient projection based algorithms, establishing an interesting link with
variational inequality problems. Our main contribution is to provide sufficient
conditions for the global convergence of all the proposed algorithms which,
although derived under stronger constraints, incorporating for example spectral
mask constraints, have a broader validity than the convergence conditions known
in the current literature for the sequential iterative waterfilling algorithm.
|
cs.IT cs.GT math.IT
|
in this twopart paper we address the problem of finding the optimal precodingmultiplexing scheme for a set of noncooperative links sharing the same physical resources eg time and bandwidth we consider two alternative optimization problems p1 the maximization of mutual information on each link given constraints on the transmit power and spectral mask and p2 the maximization of the transmission rate on each link using finite order constellations under the same constraints as in p1 plus a constraint on the maximum average error probability on each link aiming at finding decentralized strategies we adopted as optimality criterion the achievement of a nash equilibrium and thus we formulated both problems p1 and p2 as strategic noncooperative matrixvalued games in part i of this twopart paper after deriving the optimal structure of the linear transceivers for both games we provided a unified set of sufficient conditions that guarantee the uniqueness of the nash equilibrium in this part ii we focus on the achievement of the equilibrium and propose alternative distributed iterative algorithms that solve both games specifically the new proposed algorithms are the following 1 the sequential and simultaneous iterative waterfilling based algorithms incorporating spectral mask constraints 2 the sequential and simultaneous gradient projection based algorithms establishing an interesting link with variational inequality problems our main contribution is to provide sufficient conditions for the global convergence of all the proposed algorithms which although derived under stronger constraints incorporating for example spectral mask constraints have a broader validity than the convergence conditions known in the current literature for the sequential iterative waterfilling algorithm
|
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|
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|
707.0872
|
Hydrodynamics of fluid-solid coexistence in dense shear granular flow
|
We consider dense rapid shear flow of inelastically colliding hard disks.
Navier-Stokes granular hydrodynamics is applied accounting for the recent
finding \cite{Luding,Khain} that shear viscosity diverges at a lower density
than the rest of constitutive relations. New interpolation formulas for
constitutive relations between dilute and dense cases are proposed and
justified in molecular dynamics (MD) simulations. A linear stability analysis
of the uniform shear flow is performed and the full phase diagram is presented.
It is shown that when the inelasticity of particle collision becomes large
enough, the uniform sheared flow gives way to a two-phase flow, where a dense
"solid-like" striped cluster is surrounded by two fluid layers. The results of
the analysis are verified in event-driven MD simulations, and a good agreement
is observed.
|
cond-mat.soft
|
we consider dense rapid shear flow of inelastically colliding hard disks navierstokes granular hydrodynamics is applied accounting for the recent finding citeludingkhain that shear viscosity diverges at a lower density than the rest of constitutive relations new interpolation formulas for constitutive relations between dilute and dense cases are proposed and justified in molecular dynamics md simulations a linear stability analysis of the uniform shear flow is performed and the full phase diagram is presented it is shown that when the inelasticity of particle collision becomes large enough the uniform sheared flow gives way to a twophase flow where a dense solidlike striped cluster is surrounded by two fluid layers the results of the analysis are verified in eventdriven md simulations and a good agreement is observed
|
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|
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|
707.0873
|
ExoPTF Science Uniquely Enabled by Far-IR Interferometry: Probing the
Formation of Planetary Systems, and Finding and Characterizing Exoplanets
|
By providing sensitive sub-arcsecond images and integral field spectroscopy
in the 25 - 400 micron wavelength range, a far-IR interferometer will
revolutionize our understanding of planetary system formation, reveal
otherwise-undetectable planets through the disk perturbations they induce, and
spectroscopically probe the atmospheres of extrasolar giant planets in orbits
typical of most of the planets in our solar system. The technical challenges
associated with interferometry in the far-IR are greatly relaxed relative to
those encountered at shorter wavelengths or when starlight nulling is required.
A structurally connected far-IR interferometer with a maximum baseline length
of 36 m can resolve the interesting spatial structures in nascent and developed
exoplanetary systems and measure exozodiacal emission at a sensitivity level
critical to TPF-I mission planning. The Space Infrared Interferometric
Telescope was recommended in the Community Plan for Far-IR/Submillimeter Space
Astronomy, studied as a Probe-class mission, and estimated to cost 800M
dollars. The scientific communities in Europe, Japan, and Canada have also
demonstrated a keen interest in far-IR interferometry through mission planning
workshops and technology research, suggesting the possibility of an
international collaborative effort.
|
astro-ph
|
by providing sensitive subarcsecond images and integral field spectroscopy in the 25 400 micron wavelength range a farir interferometer will revolutionize our understanding of planetary system formation reveal otherwiseundetectable planets through the disk perturbations they induce and spectroscopically probe the atmospheres of extrasolar giant planets in orbits typical of most of the planets in our solar system the technical challenges associated with interferometry in the farir are greatly relaxed relative to those encountered at shorter wavelengths or when starlight nulling is required a structurally connected farir interferometer with a maximum baseline length of 36 m can resolve the interesting spatial structures in nascent and developed exoplanetary systems and measure exozodiacal emission at a sensitivity level critical to tpfi mission planning the space infrared interferometric telescope was recommended in the community plan for farirsubmillimeter space astronomy studied as a probeclass mission and estimated to cost 800m dollars the scientific communities in europe japan and canada have also demonstrated a keen interest in farir interferometry through mission planning workshops and technology research suggesting the possibility of an international collaborative effort
|
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|
[-0.0975129202068757, 0.15194207019020348, -0.06612934295277474, 0.07494226675598993, -0.11451413893367106, -0.06633963992141416, 0.042462128849889515, 0.4005821389040915, -0.18052554299520845, -0.37339687328996124, 0.10568138673746337, -0.2733778222806036, -0.10198551996895192, 0.22641572220866585, -0.08595426032046057, 0.05244219705355906, 0.12702493974412818, -0.1093682647284152, 0.019892903691023527, -0.25287597300036707, 0.2298422880059024, 0.16392030102190283, 0.1865902614390404, 0.005571156821745095, 0.061269201792113606, -0.07956929405688146, -0.09077584636160883, -0.05486166310703151, -0.15379654991803532, 0.0975827042481699, 0.37005302189784534, 0.16564028191388094, 0.2840732622064261, -0.38585104275031784, -0.22535304399601863, 0.05237948252046007, 0.13338538845882641, -0.013396229389739238, 0.009210358665845656, -0.32937793248454056, -0.003544713359978576, -0.1710669050561422, -0.1952951620438131, 0.027188829929662584, 0.06270743028450189, 0.016151292783623865, -0.21417422481050574, -0.035576945151193175, -0.034908516048827, 0.15186420527397324, -0.09586709733436799, -0.12700666911968445, -0.035888149155077584, 0.11482303129922793, -0.03997651195004951, 0.07840089956354376, 0.15690150966941468, -0.12267941617180651, -0.07386968175796424, 0.394180547527569, -0.07653735191192962, 0.016526519757627093, 0.21759571206603345, -0.24784121571087653, -0.13978623543829147, 0.16707134991621145, 0.16785800478310656, 0.1113196639238862, -0.1692527555877844, 0.03342444521386839, 0.03845722040971794, 0.2148395829812997, 0.11587258790077715, 0.12399974521144298, 0.36628144722179334, 0.19871694018596014, 0.12353287781799202, 0.096562902066241, -0.2181566212813654, -0.04844879859798301, -0.17156498595851205, -0.12403076375429492, -0.1485071742267869, 0.031056853019060845, -0.0533257658761238, -0.07279764183094505, 0.3399440963949224, 0.17013999686942607, 0.08767132105379455, -0.00451619108602152, 0.34367544860658, -0.0028951645501242096, 0.1305150417328186, 0.03566812096153107, 0.30743461781797016, 0.09803880531588138, 0.16923679785781914, -0.2143052371592382, 0.04786093729300856, -0.04179782727022924]
|
707.0874
|
Isometry theorem for the Segal-Bargmann transform on noncompact
symmetric spaces of the complex type
|
We consider the Segal-Bargmann transform for a noncompact symmetric space of
the complex type. We establish isometry and surjectivity theorems for the
transform, in a form as parallel as possible to the results in the compact
case. The isometry theorem involves integration over a tube of radius R in the
complexification, followed by analytic continuation with respect to R. A
cancellation of singularities allows the relevant integral to have a
nonsingular extension to large R, even though the function being integrated has
singularities.
|
math-ph math.MP math.RT
|
we consider the segalbargmann transform for a noncompact symmetric space of the complex type we establish isometry and surjectivity theorems for the transform in a form as parallel as possible to the results in the compact case the isometry theorem involves integration over a tube of radius r in the complexification followed by analytic continuation with respect to r a cancellation of singularities allows the relevant integral to have a nonsingular extension to large r even though the function being integrated has singularities
|
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|
[-0.16049306595092078, 0.019154857625309604, -0.10864303783928773, 0.08190396531339152, -0.11529522793120649, -0.11733367706435811, -0.021176047714326126, 0.35910659902785197, -0.2478489236210484, -0.183781855838536, 0.17534419703605889, -0.244199002691978, -0.13069796830370842, 0.2090344514293843, -0.08600846281645438, 0.02610703869386161, 0.022216947477153807, 0.08521290552095477, -0.15045042785167895, -0.21122263083571052, 0.3609083775004529, 0.004485719769923802, 0.21198539541338582, 0.032439311943858504, 0.10380562804975962, 0.06778522313247065, -0.04394620537536264, -0.011151703372275099, -0.1217562557893794, 0.10681043175352087, 0.2735960447644613, 0.09249133422847343, 0.2292639330346474, -0.38052892011691286, -0.18531130217240158, 0.1551768182922738, 0.15559503308171968, 0.009313589220036226, -0.033308663450361015, -0.2702066920086158, 0.1066240557014987, -0.13964137108435473, -0.2149000542002719, -0.07620754684265478, 0.05880514471735581, -0.007831388456096133, -0.2781002260520157, 0.04096392855743866, 0.09283435683562813, 0.034226256209504174, -0.06050851097378139, -0.033560413328638995, 0.029928915039916713, 0.06775776301903358, 0.03765943005515532, 0.0825055434848238, 0.08460274189486201, -0.06767641573426235, -0.0691377658660647, 0.3619073673364628, -0.0903213353636843, -0.25392781635634154, 0.1450838722591569, -0.1611231620962092, -0.12164119098627243, 0.13143123100590276, 0.1078890822603401, 0.13202536404581675, -0.06681424792833536, 0.21389385097287034, -0.03827858036131519, 0.06863153032419911, 0.10911275583308146, 0.015195687312677682, 0.14468108828976212, 0.10783161750941324, 0.10069890975312565, 0.18626691409700877, -0.030214911988790494, -0.0804865630911607, -0.36517602008913297, -0.22969306695712619, -0.15709058753024024, 0.13351872779361634, -0.12279984942361774, -0.20553677944264498, 0.3845178464522967, 0.03316953072481486, 0.20916411709264818, 0.09243674483150244, 0.24857644018638564, 0.09568852082972067, 0.1265495099935187, 0.04219977696796497, 0.17364853408456926, 0.20943051046433758, 0.06776277184374532, -0.14152250370061226, -0.05456016502758286, 0.15862327244087873]
|
707.0875
|
Theory and Numerics of Gravitational Waves from Preheating after
Inflation
|
Preheating after inflation involves large, time-dependent field
inhomogeneities, which act as a classical source of gravitational radiation.
The resulting spectrum might be probed by direct detection experiments if
inflation occurs at a low enough energy scale. In this paper, we develop a
theory and algorithm to calculate, analytically and numerically, the spectrum
of energy density in gravitational waves produced from an inhomogeneous
background of stochastic scalar fields in an expanding universe. We derive some
generic analytical results for the emission of gravity waves by stochastic
media of random fields, which can test the validity/accuracy of numerical
calculations. We contrast our method with other numerical methods in the
literature, and then we apply it to preheating after chaotic inflation. In this
case, we are able to check analytically our numerical results, which differ
significantly from previous works. We discuss how the gravity wave spectrum
builds up with time and find that the amplitude and the frequency of its peak
depend in a relatively simple way on the characteristic spatial scale amplified
during preheating. We then estimate the peak frequency and amplitude of the
spectrum produced in two models of preheating after hybrid inflation, which for
some parameters may be relevant for gravity wave interferometric experiments.
|
astro-ph gr-qc hep-ph hep-th
|
preheating after inflation involves large timedependent field inhomogeneities which act as a classical source of gravitational radiation the resulting spectrum might be probed by direct detection experiments if inflation occurs at a low enough energy scale in this paper we develop a theory and algorithm to calculate analytically and numerically the spectrum of energy density in gravitational waves produced from an inhomogeneous background of stochastic scalar fields in an expanding universe we derive some generic analytical results for the emission of gravity waves by stochastic media of random fields which can test the validityaccuracy of numerical calculations we contrast our method with other numerical methods in the literature and then we apply it to preheating after chaotic inflation in this case we are able to check analytically our numerical results which differ significantly from previous works we discuss how the gravity wave spectrum builds up with time and find that the amplitude and the frequency of its peak depend in a relatively simple way on the characteristic spatial scale amplified during preheating we then estimate the peak frequency and amplitude of the spectrum produced in two models of preheating after hybrid inflation which for some parameters may be relevant for gravity wave interferometric experiments
|
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|
[-0.11743914049458254, 0.17187583419506375, -0.10860179238287467, 0.0882392737819765, -0.06745770171381019, -0.09523729755189912, -0.00873181086407488, 0.36104215946268714, -0.23329145265536685, -0.2905316831328415, 0.09841992061360386, -0.219511983386273, -0.16632778793395603, 0.2327455762461782, 0.020921886752914693, 0.013172737892781353, 0.03821977305001226, 0.024296019400648884, -0.042744143507007525, -0.22972109198129823, 0.32386798475091366, 0.11872344138674218, 0.2205741976495612, 0.03693729941159707, 0.058912766849612955, -0.04537295276445928, -0.042095414644997255, 0.009785074483731697, -0.14754964192438752, 0.047551550991888264, 0.2068710313737199, 0.1275983987665125, 0.23944915001156736, -0.46071771429530506, -0.27398953402502085, 0.11529810074028637, 0.15358487787751682, 0.18285822254134482, -0.0705380274442809, -0.27280476458916636, 0.05358935766876331, -0.17012220059792177, -0.1335772276566974, -0.06795281164114148, -0.010365240580374788, 0.008033020564084276, -0.28860127861815704, 0.11907351582214751, 0.0044281272174047275, -0.024533222979165468, -0.059703271607226084, -0.02396171779504844, -0.013050891361497527, 0.04835012009633439, 0.10070940264479315, 0.018289976936806306, 0.14935607666590164, -0.13771190073712744, -0.07980367464410242, 0.3647422385608475, -0.16454579582520454, -0.14355433181276903, 0.17235447902214057, -0.165545915375037, -0.14067645747159502, 0.14600306177360414, 0.17507034251604028, 0.13483174323077654, -0.10642192657839672, 0.08291696128277727, 0.034899298174638216, 0.16080034685233985, 0.10829294238037664, 0.016430386335226557, 0.2572091453263692, 0.12073344083243678, 0.007796254800976681, 0.1344928988499287, -0.09395017116926978, -0.0677855489156186, -0.33415786944916975, -0.06416970900411309, -0.1727633176353104, 0.03228638013936648, -0.0992659933537043, -0.153224955441366, 0.4321631436727097, 0.20788775245673963, 0.17889025796943442, 0.0637596856396682, 0.3021389546441694, 0.15643238176630692, 0.015759188131305384, 0.08340309799667173, 0.2932271025355176, 0.12873340789297494, 0.12493430311032319, -0.21955069053282714, -0.029180837935066137, 0.013214265105309965]
|
707.0876
|
Quasi-Local Linear Momentum in Black-Hole Binaries
|
We propose a quasi-local formula for the linear momentum of black-hole
horizons inspired by the formalism of quasi-local horizons. We test this
formula using two complementary configurations: (i) by calculating the large
orbital linear momentum of the two black holes in an unequal-mass, zero-spin,
quasi-circular binary and (ii) by calculating the very small recoil momentum
imparted to the remnant of the head-on collision of an equal-mass,
anti-aligned-spin binary. We obtain results consistent with the horizon
trajectory in the orbiting case, and consistent with the net radiated linear
momentum for the much smaller head-on recoil velocity.
|
gr-qc astro-ph
|
we propose a quasilocal formula for the linear momentum of blackhole horizons inspired by the formalism of quasilocal horizons we test this formula using two complementary configurations i by calculating the large orbital linear momentum of the two black holes in an unequalmass zerospin quasicircular binary and ii by calculating the very small recoil momentum imparted to the remnant of the headon collision of an equalmass antialignedspin binary we obtain results consistent with the horizon trajectory in the orbiting case and consistent with the net radiated linear momentum for the much smaller headon recoil velocity
|
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|
[-0.17703906078129372, 0.15994828104003125, -0.08061725740628119, 0.1003537390943359, -0.07457186288152019, -0.09249173478778214, -0.0249547884611294, 0.2954791834023088, -0.15759043236996265, -0.2880370242005967, -0.0005765037804326795, -0.3045604961349609, -0.006163706881628233, 0.2168491401491647, -0.02154488085788932, 0.07589164990535442, 0.10005906435284526, 0.003946553222200972, -0.16136526762250256, -0.19050296075998785, 0.3918129243749253, 0.13444294257366912, 0.1424629782980427, -0.010523251356913689, 0.17822688303273568, 0.10037911859182443, -0.021665349255930236, 0.04142986131990527, -0.17536719150326036, 0.0669639117104259, 0.2032447027146539, 0.10102630728617945, 0.18198816682428165, -0.4037263898297827, -0.12125808354145154, 0.05755539496052772, 0.1393786085140396, 0.18028875085663923, -0.10296599631831843, -0.25292588711934205, 0.05241020470659467, -0.34128363982358195, -0.17421180261992553, -0.02651580429061296, 0.10886013051098649, 0.015078432907528699, -0.21407614440280706, 0.14827455155194758, 0.10010854643026486, -0.02551784739889046, -0.17258145256919113, -0.09424488582063784, -0.0477688531094092, 0.021226043074807906, 0.12889418359647722, 0.01582193989405765, 0.11868985731432095, -0.057578253909014165, -0.11983944172475566, 0.3466975165511224, -0.04131507941650504, -0.21912875522839578, 0.15639578578795524, -0.24513845878004276, -0.04467057483023072, 0.14811373739800554, 0.18864798064695354, 0.2412456827624602, -0.1668992249155479, 0.02399516772315342, 0.010088656721834807, 0.1133265603888542, 0.12295801615580282, 0.018447396365251948, 0.36441440507769585, 0.11120330756084319, 0.014393852468817792, 0.15456285515423626, -0.17984898185773573, -0.119067646503607, -0.2951774753709423, -0.12347446827369184, -0.21455010162428656, 0.06008806507390468, -0.17015134050737463, -0.12374384845904213, 0.31470398584559084, 0.07741285488938299, 0.2544584086838555, 0.055552045874139096, 0.3035518016458809, 0.14039569570029037, 0.049053523699416124, 0.14023402267868848, 0.3398886691144806, 0.10817928115609399, 0.10138375238773037, -0.2974483034613126, -0.04855179644506821, 0.08845466452630911]
|
707.0877
|
Signatures of Extra Gauge Bosons in the Littlest Higgs Model with
T-parity at Future Colliders
|
We study the collider signatures of a T-odd gauge boson $W_{H}$ pair
production in the Littlest Higgs Model with T-parity (LHT) at Large Hadron
Collider (LHC) and Linear Collider (LC). At the LHC, we search for the $W_{H}$
boson using its leptonic decay, i.e. $pp\to W_{H}^{+}W_{H}^{-}\to
A_{H}A_{H}\ell^{+}\nu_{\ell}\ell^{\prime-}\bar{\nu}_{\ell^{\prime}}$, which
gives rise to a collider signature of $\ell^{+}\ell^{\prime-}+\met$. We
demonstrate that the LHC not only has a great potential of discovering the
$W_{H}$ boson in this channel, but also can probe enormous parameter space of
the LHT. Due to four missing particles in the final state, one cannot
reconstruct the mass of $W_{H}$ at the LHC. But such a mass measurement can be
easily achieved at the LC in the process of $e^{+}e^{-}\to
W_{H}^{+}W_{H}^{-}\to A_{H}A_{H}W^{+}W^{-}\to A_{H}A_{H}jjjj$. We present an
algorithm of measuring the mass and spin of the $W_{H}$ boson at the LC.
Furthermore, we illustrate that the spin correlation between the $W$ boson and
its mother particle ($W_{H}$) can be used to distinguish the LHT from other new
physics models.
|
hep-ph
|
we study the collider signatures of a todd gauge boson w_h pair production in the littlest higgs model with tparity lht at large hadron collider lhc and linear collider lc at the lhc we search for the w_h boson using its leptonic decay ie ppto w_hw_hto a_ha_hellnu_ellellprimebarnu_ellprime which gives rise to a collider signature of ellellprimemet we demonstrate that the lhc not only has a great potential of discovering the w_h boson in this channel but also can probe enormous parameter space of the lht due to four missing particles in the final state one cannot reconstruct the mass of w_h at the lhc but such a mass measurement can be easily achieved at the lc in the process of eeto w_hw_hto a_ha_hwwto a_ha_hjjjj we present an algorithm of measuring the mass and spin of the w_h boson at the lc furthermore we illustrate that the spin correlation between the w boson and its mother particle w_h can be used to distinguish the lht from other new physics models
|
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|
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|
707.0878
|
Risk Analysis in Robust Control -- Making the Case for Probabilistic
Robust Control
|
This paper offers a critical view of the "worst-case" approach that is the
cornerstone of robust control design. It is our contention that a blind
acceptance of worst-case scenarios may lead to designs that are actually more
dangerous than designs based on probabilistic techniques with a built-in risk
factor. The real issue is one of modeling. If one accepts that no mathematical
model of uncertainties is perfect then a probabilistic approach can lead to
more reliable control even if it cannot guarantee stability for all possible
cases. Our presentation is based on case analysis. We first establish that
worst-case is not necessarily "all-encompassing." In fact, we show that for
some uncertain control problems to have a conventional robust control solution
it is necessary to make assumptions that leave out some feasible cases. Once we
establish that point, we argue that it is not uncommon for the risk of
unaccounted cases in worst-case design to be greater than that of the accepted
risk in a probabilistic approach. With an example, we quantify the risks and
show that worst-case can be significantly more risky. Finally, we join our
analysis with existing results on computational complexity and probabilistic
robustness to argue that the deterministic worst-case analysis is not
necessarily the better tool.
|
math.OC cs.SY math.ST stat.TH
|
this paper offers a critical view of the worstcase approach that is the cornerstone of robust control design it is our contention that a blind acceptance of worstcase scenarios may lead to designs that are actually more dangerous than designs based on probabilistic techniques with a builtin risk factor the real issue is one of modeling if one accepts that no mathematical model of uncertainties is perfect then a probabilistic approach can lead to more reliable control even if it cannot guarantee stability for all possible cases our presentation is based on case analysis we first establish that worstcase is not necessarily allencompassing in fact we show that for some uncertain control problems to have a conventional robust control solution it is necessary to make assumptions that leave out some feasible cases once we establish that point we argue that it is not uncommon for the risk of unaccounted cases in worstcase design to be greater than that of the accepted risk in a probabilistic approach with an example we quantify the risks and show that worstcase can be significantly more risky finally we join our analysis with existing results on computational complexity and probabilistic robustness to argue that the deterministic worstcase analysis is not necessarily the better tool
|
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|
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|
707.0879
|
Escape of Ionizing Radiation from High Redshift Galaxies
|
We model the escape of ionizing radiation from high-redshift galaxies using
high-resolution Adaptive Mesh Refinement N-body + hydrodynamics simulations.
Our simulations include time-dependent and spatially-resolved transfer of
ionizing radiation in three dimensions, including effects of dust absorption.
For galaxies of total mass M > 10^11 Msun and star formation rates SFR ~ 1-5
Msun/yr, we find angular averaged escape fractions of 0.01-0.03 over the entire
redshift interval studied (3<z<9). In addition, we find that the escape
fraction varies by more than an order of magnitude along different
lines-of-sight within individual galaxies, from the largest values near
galactic poles to the smallest along the galactic disk. The escape fraction
declines steeply at lower masses and SFR. We show that the low values of escape
fractions are due to a small fraction of young stars located just outside the
edge of HI disk. We compare our predicted escape fraction of ionizing photons
with previous results, and find a general agreement with both other simulation
results and available direct detection measurements at z ~ 3. We also compare
our simulations with a novel method to estimate the escape fraction in galaxies
from the observed distribution of neutral hydrogen column densities along the
lines of sights to long duration gamma-ray bursts. Using this method we find
escape fractions of the GRB host galaxies of 2-3%, consistent with our
theoretical predictions. [abridged]
|
astro-ph
|
we model the escape of ionizing radiation from highredshift galaxies using highresolution adaptive mesh refinement nbody hydrodynamics simulations our simulations include timedependent and spatiallyresolved transfer of ionizing radiation in three dimensions including effects of dust absorption for galaxies of total mass m 1011 msun and star formation rates sfr 15 msunyr we find angular averaged escape fractions of 001003 over the entire redshift interval studied 3z9 in addition we find that the escape fraction varies by more than an order of magnitude along different linesofsight within individual galaxies from the largest values near galactic poles to the smallest along the galactic disk the escape fraction declines steeply at lower masses and sfr we show that the low values of escape fractions are due to a small fraction of young stars located just outside the edge of hi disk we compare our predicted escape fraction of ionizing photons with previous results and find a general agreement with both other simulation results and available direct detection measurements at z 3 we also compare our simulations with a novel method to estimate the escape fraction in galaxies from the observed distribution of neutral hydrogen column densities along the lines of sights to long duration gammaray bursts using this method we find escape fractions of the grb host galaxies of 23 consistent with our theoretical predictions abridged
|
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|
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|
707.088
|
Defects Can Increase the Melting Temperature of DNA-Nanoparticle
Assemblies
|
DNA-gold nanoparticle assemblies have shown promise as an alternative
technology to DNA microarrays for DNA detection and RNA profiling.
Understanding the effect of DNA sequences on the melting temperature of the
system is central to developing reliable detection technology. We studied the
effects of DNA base-pairing defects, such as mismatches and deletions, on the
melting temperature of DNA-nanoparticle assemblies. We found that, contrary to
the general assumption that defects lower the melting temperature of DNA, some
defects increase the melting temperature of DNA-linked nanoparticle assemblies.
The effects of mismatches and deletions were found to depend on the specific
base pair, the sequence, and the location of the defects. Our results
demonstrate that the surface-bound DNA exhibit hybridization behavior different
from that of free DNA. Such findings indicate that a detailed understanding of
DNA-nanoparticle assembly phase behavior is required for quantitative
interpretation of DNA-nanoparticle aggregation.
|
physics.bio-ph
|
dnagold nanoparticle assemblies have shown promise as an alternative technology to dna microarrays for dna detection and rna profiling understanding the effect of dna sequences on the melting temperature of the system is central to developing reliable detection technology we studied the effects of dna basepairing defects such as mismatches and deletions on the melting temperature of dnananoparticle assemblies we found that contrary to the general assumption that defects lower the melting temperature of dna some defects increase the melting temperature of dnalinked nanoparticle assemblies the effects of mismatches and deletions were found to depend on the specific base pair the sequence and the location of the defects our results demonstrate that the surfacebound dna exhibit hybridization behavior different from that of free dna such findings indicate that a detailed understanding of dnananoparticle assembly phase behavior is required for quantitative interpretation of dnananoparticle aggregation
|
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|
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|
707.0881
|
SN 1993J VLBI (IV): A Geometric Determination of the Distance to M81
with the Expanding Shock Front Method
|
We compare the angular expansion velocities, determined with VLBI, with the
linear expansion velocities measured from optical spectra for supernova 1993J
in the galaxy M81, over the period from 7 d to ~9 yr after shock breakout. We
estimate the distance to SN 1993J using the Expanding Shock Front Method (ESM).
We find the best distance estimate is obtained by fitting the angular velocity
of a point halfway between the contact surface and outer shock front to the
maximum observed hydrogen gas velocity. We obtain a direct, geometric, distance
estimate for M81 of D=3.96+-0.05+-0.29 Mpc with statistical and systematic
error contributions, respectively, corresponding to a total standard error of
$+-0.29 Mpc. The upper limit of 4.25 Mpc corresponds to the hydrogen gas with
the highest observed velocity reaching no farther out than the contact surface
a few days after shock breakout. The lower limit of 3.67 Mpc corresponds to
this hydrogen gas reaching as far out as the forward shock for the whole
period, which would mean that Rayleigh-Taylor fingers have grown to the forward
shock already a few days after shock breakout. Our distance estimate is 9+-13 %
larger than that of 3.63+-0.34 Mpc from the HST Key Project, which is near our
lower limit but within the errors.
|
astro-ph
|
we compare the angular expansion velocities determined with vlbi with the linear expansion velocities measured from optical spectra for supernova 1993j in the galaxy m81 over the period from 7 d to 9 yr after shock breakout we estimate the distance to sn 1993j using the expanding shock front method esm we find the best distance estimate is obtained by fitting the angular velocity of a point halfway between the contact surface and outer shock front to the maximum observed hydrogen gas velocity we obtain a direct geometric distance estimate for m81 of d396005029 mpc with statistical and systematic error contributions respectively corresponding to a total standard error of 029 mpc the upper limit of 425 mpc corresponds to the hydrogen gas with the highest observed velocity reaching no farther out than the contact surface a few days after shock breakout the lower limit of 367 mpc corresponds to this hydrogen gas reaching as far out as the forward shock for the whole period which would mean that rayleightaylor fingers have grown to the forward shock already a few days after shock breakout our distance estimate is 913 larger than that of 363034 mpc from the hst key project which is near our lower limit but within the errors
|
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|
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|
707.0882
|
An algebraic theory of infinite classical lattices III: Theory of single
measurements
|
This is the third in a series of papers dealing with the algebraic theory of
infinite classical lattices. This paper presents a theory of single
measurements on a lattice which we represent as comprising a finite
subvolume--the system of measurement--immersed in an infinite surround or
``heat bath'' which determines the system's state. We consider the class of all
stationary distributions on the set of microcanonical states of the infinite
lattice. The theory addresses the question, ``For a lattice initially in state
A, say, what is the probability that measurement of a certain quantity will
take a value in (a,b)?'' Discussion includes description of the source of
randomness in a measurement as well as characterization of the given states A.
|
math-ph math.MP
|
this is the third in a series of papers dealing with the algebraic theory of infinite classical lattices this paper presents a theory of single measurements on a lattice which we represent as comprising a finite subvolumethe system of measurementimmersed in an infinite surround or heat bath which determines the systems state we consider the class of all stationary distributions on the set of microcanonical states of the infinite lattice the theory addresses the question for a lattice initially in state a say what is the probability that measurement of a certain quantity will take a value in ab discussion includes description of the source of randomness in a measurement as well as characterization of the given states a
|
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|
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|
707.0883
|
The Space Infrared Interferometric Telescope (SPIRIT): High-resolution
imaging and spectroscopy in the far-infrared
|
We report results of a recently-completed pre-Formulation Phase study of
SPIRIT, a candidate NASA Origins Probe mission. SPIRIT is a spatial and
spectral interferometer with an operating wavelength range 25 - 400 microns.
SPIRIT will provide sub-arcsecond resolution images and spectra with resolution
R = 3000 in a 1 arcmin field of view to accomplish three primary scientific
objectives: (1) Learn how planetary systems form from protostellar disks, and
how they acquire their inhomogeneous composition; (2) characterize the family
of extrasolar planetary systems by imaging the structure in debris disks to
understand how and where planets of different types form; and (3) learn how
high-redshift galaxies formed and merged to form the present-day population of
galaxies. Observations with SPIRIT will be complementary to those of the James
Webb Space Telescope and the ground-based Atacama Large Millimeter Array. All
three observatories could be operational contemporaneously.
|
astro-ph
|
we report results of a recentlycompleted preformulation phase study of spirit a candidate nasa origins probe mission spirit is a spatial and spectral interferometer with an operating wavelength range 25 400 microns spirit will provide subarcsecond resolution images and spectra with resolution r 3000 in a 1 arcmin field of view to accomplish three primary scientific objectives 1 learn how planetary systems form from protostellar disks and how they acquire their inhomogeneous composition 2 characterize the family of extrasolar planetary systems by imaging the structure in debris disks to understand how and where planets of different types form and 3 learn how highredshift galaxies formed and merged to form the presentday population of galaxies observations with spirit will be complementary to those of the james webb space telescope and the groundbased atacama large millimeter array all three observatories could be operational contemporaneously
|
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|
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|
707.0884
|
The Effective Field Theory of Codimension-two Branes
|
Distributional sources of matter on codimension-two and higher branes are
only well-defined as regularized objects. Nevertheless, intuition from
effective field theory suggests that the low-energy physics on such branes
should be independent of any high-energy regularization scheme. In this paper,
we address this issue in the context of a scalar field model where matter
fields (the standard model) living on such a brane interact with bulk fields
(gravity). The low-energy effective theory is shown to be consistent and
independent of the regularization scheme, provided the brane couplings are
renormalized appropriately at the classical level. We perform explicit
computations of the classical renormalization group flows at tree and one-loop
level, demonstrate that the theory is renormalizable against codimension-two
divergences, and extend the analysis to several physical applications such as
electrodynamics and brane localized kinetic terms.
|
hep-th
|
distributional sources of matter on codimensiontwo and higher branes are only welldefined as regularized objects nevertheless intuition from effective field theory suggests that the lowenergy physics on such branes should be independent of any highenergy regularization scheme in this paper we address this issue in the context of a scalar field model where matter fields the standard model living on such a brane interact with bulk fields gravity the lowenergy effective theory is shown to be consistent and independent of the regularization scheme provided the brane couplings are renormalized appropriately at the classical level we perform explicit computations of the classical renormalization group flows at tree and oneloop level demonstrate that the theory is renormalizable against codimensiontwo divergences and extend the analysis to several physical applications such as electrodynamics and brane localized kinetic terms
|
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|
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|
707.0885
|
Observation of a uniform temperature dependence in the electrical
resistance across the structural phase transition in thin film vanadium oxide
($VO_{2}$)
|
An electrical study of thin $VO_{2}$ films in the vicinity of the structural
phase transition at $68^{0}C$ shows (a) that the electrical resistance $R$
follows $log (R)$ $\propto$ $-T$ over the $T$-range, $20 < T < 80 ^{0}C$
covering both sides of the structural transition, and (b) a history dependent
hysteresis loop in $R$ upon thermal cycling. These features are attributed here
to transport through a granular network.
|
cond-mat.mes-hall cond-mat.mtrl-sci
|
an electrical study of thin vo_2 films in the vicinity of the structural phase transition at 680c shows a that the electrical resistance r follows log r propto t over the trange 20 t 80 0c covering both sides of the structural transition and b a history dependent hysteresis loop in r upon thermal cycling these features are attributed here to transport through a granular network
|
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|
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|
707.0886
|
Radiative torques: Analytical Model and Basic Properties
|
We attempt to get a physical insight into grain alignment processes by
studying basic properties of radiative torques (RATs). For this purpose we
consider a simple toy model of a helical grain that reproduces well the basic
features of RATs. The model grain consists of a spheroidal body with a mirror
attached at an angle to it. Being very simple, the model allows analytical
description of RATs that act upon it. We show a good correspondence of RATs
obtained for this model and those of irregular grains calculated by DDSCAT. Our
analysis of the role of different torque components for grain alignment reveals
that one of the three RAT components does not affect the alignment, but induces
only for grain precession. The other two components provide a generic alignment
with grain long axes perpendicular to the radiation direction, if the radiation
dominates the grain precession, and perpendicular to magnetic field, otherwise.
We study a self-similar scaling of RATs as a function of $\lambda/a_{eff}$. We
show that the self-similarity is useful for studying grain alignment by a broad
spectrum of radiation, i.e. interstellar radiation field.
|
astro-ph
|
we attempt to get a physical insight into grain alignment processes by studying basic properties of radiative torques rats for this purpose we consider a simple toy model of a helical grain that reproduces well the basic features of rats the model grain consists of a spheroidal body with a mirror attached at an angle to it being very simple the model allows analytical description of rats that act upon it we show a good correspondence of rats obtained for this model and those of irregular grains calculated by ddscat our analysis of the role of different torque components for grain alignment reveals that one of the three rat components does not affect the alignment but induces only for grain precession the other two components provide a generic alignment with grain long axes perpendicular to the radiation direction if the radiation dominates the grain precession and perpendicular to magnetic field otherwise we study a selfsimilar scaling of rats as a function of lambdaa_eff we show that the selfsimilarity is useful for studying grain alignment by a broad spectrum of radiation ie interstellar radiation field
|
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|
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|
707.0887
|
Di-lepton ttH At The CMS
|
In keeping with the "find the Higgs" bandwagon, due to embark together with
the Large Hadron Collider (LHC), we investigate discovery prospects with Higgs
produced in conjunction with two top quarks decaying in the dilepton channel.
The following is a brief account of adventures along the way; the interested
reader may find more in our CMS note.
|
hep-ex
|
in keeping with the find the higgs bandwagon due to embark together with the large hadron collider lhc we investigate discovery prospects with higgs produced in conjunction with two top quarks decaying in the dilepton channel the following is a brief account of adventures along the way the interested reader may find more in our cms note
|
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|
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|
707.0888
|
Cosmic String Loops and Gravitational Radiation
|
Understanding of the signatures of cosmic string networks is limited by a
large uncertainty in the sizes at which cosmic string loops form. We review
cosmic string network evolution, and the gravitational signatures, with
emphasis on this uncertainty. We then review a recent analytic model of cosmic
string networks. In combination with recent simulations, this suggests that 90%
of the string goes into very small loops, at the gravitational radiation scale,
and 10% into loops near the Hubble scale. We discuss cosmic string signatures
in such a scenario, and the `inverse problem' of determining the microscopic
cosmic string properties from observations.
|
astro-ph gr-qc hep-ph hep-th
|
understanding of the signatures of cosmic string networks is limited by a large uncertainty in the sizes at which cosmic string loops form we review cosmic string network evolution and the gravitational signatures with emphasis on this uncertainty we then review a recent analytic model of cosmic string networks in combination with recent simulations this suggests that 90 of the string goes into very small loops at the gravitational radiation scale and 10 into loops near the hubble scale we discuss cosmic string signatures in such a scenario and the inverse problem of determining the microscopic cosmic string properties from observations
|
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|
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|
707.0889
|
Deformation theory of representations of prop(erad)s
|
We study the deformation theory of morphisms of properads and props thereby
extending to a non-linear framework Quillen's deformation theory for
commutative rings. The associated chain complex is endowed with a Lie algebra
up to homotopy structure. Its Maurer-Cartan elements correspond to deformed
structures, which allows us to give a geometric interpretation of these
results.
To do so, we endow the category of prop(erad)s with a model category
structure. We provide a complete study of models for prop(erad)s. A new
effective method to make minimal models explicit, that extends Koszul duality
theory, is introduced and the associated notion is called homotopy Koszul.
As a corollary, we obtain the (co)homology theories of (al)gebras over a
prop(erad) and of homotopy (al)gebras as well. Their underlying chain complex
is endowed with a canonical Lie algebra up to homotopy structure in general and
a Lie algebra structure only in the Koszul case. In particular, we explicit the
deformation complex of morphisms from the properad of associative bialgebras.
For any minimal model of this properad, the boundary map of this chain complex
is shown to be the one defined by Gerstenhaber and Schack. As a corollary, this
paper provides a complete proof of the existence of a Lie algebra up to
homotopy structure on the Gerstenhaber-Schack bicomplex associated to the
deformations of associative bialgebras.
|
math.QA math.AT
|
we study the deformation theory of morphisms of properads and props thereby extending to a nonlinear framework quillens deformation theory for commutative rings the associated chain complex is endowed with a lie algebra up to homotopy structure its maurercartan elements correspond to deformed structures which allows us to give a geometric interpretation of these results to do so we endow the category of properads with a model category structure we provide a complete study of models for properads a new effective method to make minimal models explicit that extends koszul duality theory is introduced and the associated notion is called homotopy koszul as a corollary we obtain the cohomology theories of algebras over a properad and of homotopy algebras as well their underlying chain complex is endowed with a canonical lie algebra up to homotopy structure in general and a lie algebra structure only in the koszul case in particular we explicit the deformation complex of morphisms from the properad of associative bialgebras for any minimal model of this properad the boundary map of this chain complex is shown to be the one defined by gerstenhaber and schack as a corollary this paper provides a complete proof of the existence of a lie algebra up to homotopy structure on the gerstenhaberschack bicomplex associated to the deformations of associative bialgebras
|
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|
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|
707.089
|
Are there Hilbert-style Pure Type Systems?
|
For many a natural deduction style logic there is a Hilbert-style logic that
is equivalent to it in that it has the same theorems (i.e. valid judgements
with empty contexts). For intuitionistic logic, the axioms of the equivalent
Hilbert-style logic can be propositions which are also known as the types of
the combinators I, K and S. Hilbert-style versions of illative combinatory
logic have formulations with axioms that are actual type statements for I, K
and S. As pure type systems (PTSs)are, in a sense, equivalent to systems of
illative combinatory logic, it might be thought that Hilbert-style PTSs (HPTSs)
could be based in a similar way. This paper shows that some PTSs have very
trivial equivalent HPTSs, with only the axioms as theorems and that for many
PTSs no equivalent HPTS can exist. Most commonly used PTSs belong to these two
classes. For some PTSs however, including lambda* and the PTS at the basis of
the proof assistant Coq, there is a nontrivial equivalent HPTS, with axioms
that are type statements for I, K and S.
|
cs.LO
|
for many a natural deduction style logic there is a hilbertstyle logic that is equivalent to it in that it has the same theorems ie valid judgements with empty contexts for intuitionistic logic the axioms of the equivalent hilbertstyle logic can be propositions which are also known as the types of the combinators i k and s hilbertstyle versions of illative combinatory logic have formulations with axioms that are actual type statements for i k and s as pure type systems ptssare in a sense equivalent to systems of illative combinatory logic it might be thought that hilbertstyle ptss hptss could be based in a similar way this paper shows that some ptss have very trivial equivalent hptss with only the axioms as theorems and that for many ptss no equivalent hpts can exist most commonly used ptss belong to these two classes for some ptss however including lambda and the pts at the basis of the proof assistant coq there is a nontrivial equivalent hpts with axioms that are type statements for i k and s
|
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|
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|
707.0891
|
The Nash Equilibrium Revisited: Chaos and Complexity Hidden in
Simplicity
|
The Nash Equilibrium is a much discussed, deceptively complex, method for the
analysis of non-cooperative games. If one reads many of the commonly available
definitions the description of the Nash Equilibrium is deceptively simple in
appearance. Modern research has discovered a number of new and important
complex properties of the Nash Equilibrium, some of which remain as
contemporary conundrums of extraordinary difficulty and complexity. Among the
recently discovered features which the Nash Equilibrium exhibits under various
conditions are heteroclinic Hamiltonian dynamics, a very complex asymptotic
structure in the context of two-player bi-matrix games and a number of
computationally complex or computationally intractable features in other
settings. This paper reviews those findings and then suggests how they may
inform various market prediction strategies.
|
cs.GT cs.CC
|
the nash equilibrium is a much discussed deceptively complex method for the analysis of noncooperative games if one reads many of the commonly available definitions the description of the nash equilibrium is deceptively simple in appearance modern research has discovered a number of new and important complex properties of the nash equilibrium some of which remain as contemporary conundrums of extraordinary difficulty and complexity among the recently discovered features which the nash equilibrium exhibits under various conditions are heteroclinic hamiltonian dynamics a very complex asymptotic structure in the context of twoplayer bimatrix games and a number of computationally complex or computationally intractable features in other settings this paper reviews those findings and then suggests how they may inform various market prediction strategies
|
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|
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|
707.0892
|
Ground State of the Kagome Lattice Heisenberg Antiferromagnet
|
Using series expansions around the dimer limit, we show that the ground state
of the Heisenberg Antiferromagnet on the Kagome Lattice appears to be a Valence
Bond Crystal (VBC) with a 36-site unit cell, and an energy per site of
$E/J=-0.433\pm0.001$. It is a honeycomb lattice of `perfect hexagons' as
discussed by Nikolic and Senthil. The energy difference between the ground
state and other ordered states with the maximum number of `perfect hexagons',
such as a stripe-ordered state, is of order $0.001 J$. The energy of the
36-site system with periodic boundary conditions is further lowered by an
amount of $0.005\pm 0.001 J$, consistent with Exact Diagonalization. Every unit
cell of the VBC has two singlet states whose degeneracy is not lifted to $6th$
order in the expansion. We estimate this energy difference to be smaller than
$0.001 J$. Two leading orders of perturbation theory find the lowest-energy
triplet excitations to be dispersionless and confined to the `perfect
hexagons'.
|
cond-mat.str-el
|
using series expansions around the dimer limit we show that the ground state of the heisenberg antiferromagnet on the kagome lattice appears to be a valence bond crystal vbc with a 36site unit cell and an energy per site of ej0433pm0001 it is a honeycomb lattice of perfect hexagons as discussed by nikolic and senthil the energy difference between the ground state and other ordered states with the maximum number of perfect hexagons such as a stripeordered state is of order 0001 j the energy of the 36site system with periodic boundary conditions is further lowered by an amount of 0005pm 0001 j consistent with exact diagonalization every unit cell of the vbc has two singlet states whose degeneracy is not lifted to 6th order in the expansion we estimate this energy difference to be smaller than 0001 j two leading orders of perturbation theory find the lowestenergy triplet excitations to be dispersionless and confined to the perfect hexagons
|
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|
[-0.15982381186809888, 0.21676246339479716, -0.004470481366737728, 0.004707646976072329, -0.014436177480787894, -0.11106571008208072, 0.09666339868744894, 0.37239824150166934, -0.26138032141444123, -0.27121905244554684, 0.09196115517469752, -0.3407607349703551, -0.04607181235366341, 0.08449147234242231, 0.046493152927631023, -0.01689721904042515, 0.03135129948188165, 0.06341762520865223, -0.0854582398177783, -0.26025501626193714, 0.24764267920225763, 0.020166522218211063, 0.28668089379288797, 0.0696037545189214, 0.06530070880125426, 0.009808213347687748, 0.1525502456797014, -0.000961148417347176, -0.18730090607342698, 0.11716742351410946, 0.20952754545583135, -0.051932367582206325, 0.18339527592917157, -0.4209881550207909, -0.16383489387800954, 0.055560659839635256, 0.10513493375612458, 0.12835796167896052, 0.02273933240879849, -0.24536164974049327, 0.04771908979334981, -0.19193947019209717, -0.1591748802264215, -0.06531056235249638, -0.01147198539440799, -0.006920235975983606, -0.2655477506215358, 0.12492698700920601, 0.053713626647961275, 0.06993566475998444, -0.08443405431440207, -0.1530874700642897, -0.144075734606072, 0.07109061143046637, 0.02242206966142603, 0.09777094794520337, 0.038247126708871974, -0.08075253228296579, -0.15065451848890135, 0.4219118263869054, -0.0532410484283553, -0.16295674906533425, 0.13949272909148294, -0.17515323334966731, -0.07301513806792201, 0.1781218868152351, 0.039952716032327834, 0.07568779415235956, -0.07773636901383377, 0.08133209127618392, -0.05501648982183023, 0.22230630991594855, 0.08836454159586103, 0.034644147695582, 0.23409126354915322, 0.14981752608985802, 0.11179511266268173, 0.16821498397825238, -0.11246299067701979, -0.14349705279525962, -0.2432327489754197, -0.16916191921002902, -0.26457441722748765, 0.05464328133071414, -0.09065721218680346, -0.19218759344309377, 0.37816591076790146, 0.05397479516412517, 0.19090485451505726, -0.04431273049087661, 0.1810275211954003, 0.122264530715847, 0.05112527507197136, 0.0554555204213496, 0.20833462068757672, 0.16474503503703056, 0.025028571845358533, -0.25043976631988385, -0.01870366960918163, 0.09500055711354562]
|
707.0893
|
Unparticle physics and Higgs phenomenology
|
Recently, conceptually new physics beyond the Standard Model has been
proposed, where a hidden conformal sector provides ``unparticle'' which couples
to the Standard Model sector through higher dimensional operators in low energy
effective theory. Among several possibilities, we focus on operators involving
unparticle, the Higgs doublet and the gauge bosons. Once the Higgs doublet
develops the vacuum expectation value, the conformal symmetry is broken and as
a result, the mixing between unparticle and Higgs boson emerges. We find that
this mixing can cause sizable shifts for the couplings between Higgs boson and
a pair of gluons and photons, because these couplings exist only at the loop
level in the Standard Model. These Higgs couplings are the most important ones
for the Higgs boson search at the CERN Large Hadron Collider, and the
unparticle physics effects may be observed together with the discovery of Higgs
boson.
|
hep-ph hep-ex hep-th
|
recently conceptually new physics beyond the standard model has been proposed where a hidden conformal sector provides unparticle which couples to the standard model sector through higher dimensional operators in low energy effective theory among several possibilities we focus on operators involving unparticle the higgs doublet and the gauge bosons once the higgs doublet develops the vacuum expectation value the conformal symmetry is broken and as a result the mixing between unparticle and higgs boson emerges we find that this mixing can cause sizable shifts for the couplings between higgs boson and a pair of gluons and photons because these couplings exist only at the loop level in the standard model these higgs couplings are the most important ones for the higgs boson search at the cern large hadron collider and the unparticle physics effects may be observed together with the discovery of higgs boson
|
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|
[-0.0817596846966651, 0.30992614884443326, -0.05264479275471692, 0.1875650859726914, -0.1236659021951772, -0.23812360653396825, 0.008383356094970528, 0.2934494321716243, -0.2129684778331811, -0.2827405971892435, 0.0009919228080403188, -0.2871020132868454, -0.06813043042182408, 0.10376908689223487, 0.09854123093637412, 0.06078771569621589, 0.03989712288282041, 0.02541788632114386, -0.03529249349817762, -0.2511558278624354, 0.32324097776817606, 0.02267450033847628, 0.23357708401464183, 0.10506379042655743, 0.11316662643281422, 0.023750615375244925, 0.026522143509495874, -0.10454936548264633, -0.07123892467397723, 0.11876317379948009, 0.16758219836087063, 0.03335266108624637, 0.15784512798077074, -0.31740928884467173, -0.16761587440550071, 0.17869093357745944, 0.15391813405179258, 0.13848148249170003, -0.08198655143556795, -0.3435610878803157, 0.047411134370185175, -0.212688440731566, -0.08429796001472478, -0.08561894153084221, -0.0931941302685902, -0.1812155950043736, -0.33005429810105724, 0.07613862412720758, -0.06589921716889688, 0.04926321221322849, 0.04779901968732733, -0.16016366511888416, -0.10746280475166337, -0.0015990645496238923, 0.20675070380414676, 0.01109746575158828, 0.14568394918781544, -0.2496014667601136, -0.19005935454484205, 0.4018999696548643, -0.14292652784236545, -0.16848753076528425, 0.20749047136833443, -0.18623793337911623, -0.17173667999369832, 0.0998184101078017, 0.21163566866969882, 0.01979688072641348, -0.1624263280906297, 0.2621705118624959, -0.04396042170581119, 0.1391488109956142, 0.026242266553614675, 0.09943676683088315, 0.2956793411956008, 0.16842003064230085, 0.041235101438159574, 0.06388916298666776, -0.04838996992831857, -0.1346081925395491, -0.45310151397154247, -0.15546269481680516, -0.050415994891704154, 0.027715017130309393, -0.0742833867374053, -0.09374935188539454, 0.42234038132531887, 0.15030172844678324, 0.2413320492118083, -0.024205461617334393, 0.25734648764261914, 0.13437242694439944, 0.1644461782482565, 0.03166306726825183, 0.3827497229397554, 0.15149415113304837, 0.13516215412427895, -0.20294358080598238, -0.03470260118744497, 0.12333042900688175]
|
707.0894
|
Hybrid compactifications and brane gravity in six dimensions
|
We consider a six-dimensional axisymmetric Einstein-Maxwell model of warped
braneworlds. The bulk is bounded by two branes, one of which is a conical
3-brane and the other is a 4-brane wrapped around the axis of symmetry. The
latter brane is assumed to be our universe. If the tension of the 3-brane is
fine-tuned, it folds the internal two-dimensional space in a narrow cone,
making sufficiently small the Kaluza-Klein circle of the 4-brane. An arbitrary
energy-momentum tensor can be accommodated on this ring-like 4-brane. We study
linear perturbations sourced by matter on the brane, and show that weak gravity
is apparently described by a four-dimensional scalar-tensor theory. The extra
scalar degree of freedom can be interpreted as the fluctuation of the internal
space volume (or that of the circumference of the ring), the effect of which
turns out to be suppressed at long distances. Consequently, four-dimensional
Einstein gravity is reproduced on the brane. We point out that as in the
Randall-Sundrum model, the brane bending mode is crucial for recovering the
four-dimensional tensor structure in this setup.
|
hep-th gr-qc
|
we consider a sixdimensional axisymmetric einsteinmaxwell model of warped braneworlds the bulk is bounded by two branes one of which is a conical 3brane and the other is a 4brane wrapped around the axis of symmetry the latter brane is assumed to be our universe if the tension of the 3brane is finetuned it folds the internal twodimensional space in a narrow cone making sufficiently small the kaluzaklein circle of the 4brane an arbitrary energymomentum tensor can be accommodated on this ringlike 4brane we study linear perturbations sourced by matter on the brane and show that weak gravity is apparently described by a fourdimensional scalartensor theory the extra scalar degree of freedom can be interpreted as the fluctuation of the internal space volume or that of the circumference of the ring the effect of which turns out to be suppressed at long distances consequently fourdimensional einstein gravity is reproduced on the brane we point out that as in the randallsundrum model the brane bending mode is crucial for recovering the fourdimensional tensor structure in this setup
|
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|
[-0.185981692150976, 0.165695197468267, -0.08609530970253135, 0.08501067769115749, -0.11641877836187962, -0.14854299748416946, -0.07123175385574788, 0.2939399050929668, -0.21499895751052958, -0.2374676091183739, 0.09373125375251137, -0.23496548559871205, -0.1124765237168917, 0.09890498565404084, -0.050096254076131365, -0.04292334840879035, -0.017575067179595037, 0.054906173228201544, -0.041508407976256094, -0.24254770896566863, 0.38532979396140116, 0.0624836667530789, 0.24043037540236997, 0.03365675258630125, 0.10222837457157849, -0.04547704130130693, 0.02723277341151102, 0.08913795031383581, -0.1118881314647214, 0.08823269406407648, 0.17800573748561213, 0.05160663926455362, 0.15090139035204297, -0.4257182892919941, -0.25498618015130475, 0.08678008339219642, 0.16944584808846808, 0.15645872698488264, 0.0062959199931356125, -0.3052453304566866, 0.08221965907300315, -0.1593283705688009, -0.19135585079890338, -0.033799402585745236, 0.0007057069530922242, -0.12385686855916654, -0.227641489017432, 0.0929467702960458, 0.03522866451848214, -0.016175929964943367, -0.06851128045077944, -0.03848010784316681, -0.12148006398638245, 0.023264062026018193, 0.1454557377602958, 0.06711531803541054, 0.16885429164143384, -0.12571251647914944, -0.07570442099280296, 0.40466717510240746, -0.1353285695976493, -0.26951816752394236, 0.10459628519443372, -0.15501683261060284, -0.07510751220053696, 0.11358862432032103, 0.11580278678130443, 0.18293725519800896, -0.11097659233630773, 0.20608756539815493, -0.06675015939320227, 0.16229651736003606, 0.11862710354299369, 0.010293516431622927, 0.343798714494121, 0.14823507934025573, 0.055317104884207685, 0.16438711055723781, -0.0575165545570516, -0.11279854444596409, -0.3987419866025448, -0.1363690018664453, -0.17612792829111806, 0.10881160779602149, -0.17479801279560805, -0.18373589639932933, 0.3626019772226838, 0.03536015090900368, 0.19208364186356033, 0.0006034956750227138, 0.2389249600025571, 0.05124022738560929, 0.09272031659863635, 0.0695469782777681, 0.31966378384558164, 0.10898103599240792, 0.07079307002541926, -0.23212077904132788, -0.08972970324860151, 0.08601196238727095]
|
707.0895
|
Segmentation and Context of Literary and Musical Sequences
|
We test a segmentation algorithm, based on the calculation of the
Jensen-Shannon divergence between probability distributions, to two symbolic
sequences of literary and musical origin. The first sequence represents the
successive appearance of characters in a theatrical play, and the second
represents the succession of tones from the twelve-tone scale in a keyboard
sonata. The algorithm divides the sequences into segments of maximal
compositional divergence between them. For the play, these segments are related
to changes in the frequency of appearance of different characters and in the
geographical setting of the action. For the sonata, the segments correspond to
tonal domains and reveal in detail the characteristic tonal progression of such
kind of musical composition.
|
cs.CL physics.data-an
|
we test a segmentation algorithm based on the calculation of the jensenshannon divergence between probability distributions to two symbolic sequences of literary and musical origin the first sequence represents the successive appearance of characters in a theatrical play and the second represents the succession of tones from the twelvetone scale in a keyboard sonata the algorithm divides the sequences into segments of maximal compositional divergence between them for the play these segments are related to changes in the frequency of appearance of different characters and in the geographical setting of the action for the sonata the segments correspond to tonal domains and reveal in detail the characteristic tonal progression of such kind of musical composition
|
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|
[-0.1277735023151921, 0.0809814009580093, -0.10981886321837722, 0.082760899870292, -0.054360680881401766, -0.05152111004673592, 0.016399738746290297, 0.3753693262115121, -0.30197678187295146, -0.3179962430351778, 0.04202924967925672, -0.28369072539245954, -0.19291282475561553, 0.17757207977221065, -0.08874040099832675, 0.017107567840012845, 0.036910066915595015, 0.08424829590215308, -0.03522770466363948, -0.18344836116119279, 0.34445040493231754, -0.006544888096497111, 0.2779673515244529, -0.01785195029705115, 0.11098294115179906, -0.018797067184325146, -0.06720912097345876, -0.05461551560008007, -0.06643950479591022, 0.1602809550924576, 0.2582830546444039, 0.16022038822006637, 0.2726904176499533, -0.3999939342555792, -0.14629621634502774, 0.09966713209919956, 0.09769020390939777, 0.0672334556022416, 0.029044263084095134, -0.28861336942924104, 0.07505226824736304, -0.0831795728188413, -0.02014379465709562, -0.020804604159101195, 0.021930376529369664, 0.047359353870801306, -0.24517950822963663, 0.06577864163757666, 0.11062119794888017, 0.12073433755330093, -0.06562397581241701, -0.12439730881470377, 0.02526471621721335, 0.25144311370247086, 0.07783040300659512, 0.009229259063368259, 0.07281483996902471, -0.12949344903716575, -0.1204012330338035, 0.3657078411106182, -0.03864965819672722, -0.17780367862028273, 0.15255978772133263, -0.13291967351232534, -0.1230435142941449, 0.12471205238657801, 0.1815828841969209, 0.09764516619236573, -0.08693200095819877, 0.001066784979775548, -0.009491149611447168, 0.17582169337117154, 0.15664322640868308, 0.028095018734102663, 0.22496785819530488, 0.15433337926540686, -0.0037754780800162775, 0.1832129258217047, -0.11332960199670987, -0.11317236713012276, -0.30094266378361245, -0.17614447199132133, -0.1675653959745946, -0.05064050998164179, -0.11857877128261506, -0.22315339924686628, 0.4662620704783046, 0.13299852199650006, 0.22337963592423046, 0.05515227710585231, 0.2373729148555709, 0.03685738299163464, 0.08486943188548574, 0.01153649993483787, 0.12131427348307941, 0.05229360200059802, 0.08078119211384784, -0.23821963272487703, 0.10939090329262874, 0.12950958516853658]
|
707.0896
|
Shocked Molecular Hydrogen in the 3C 326 Radio Galaxy System
|
The Spitzer spectrum of the giant FR II radio galaxy 3C 326 is dominated by
very strong molecular hydrogen emission lines on a faint IR continuum. The H2
emission originates in the northern component of a double-galaxy system
associated with 3C 326. The integrated luminosity in H2 pure-rotational lines
is 8.0E41 erg/s, which corresponds to 17% of the 8-70 micron luminosity of the
galaxy. A wide range of temperatures (125-1000 K) is measured from the H2 0-0
S(0)-S(7) transitions, leading to a warm H2 mass of 1.1E9 Msun. Low-excitation
ionic forbidden emission lines are consistent with an optical LINER
classification for the active nucleus, which is not luminous enough to power
the observed H2 emission. The H2 could be shock-heated by the radio jets, but
there is no direct indication of this. More likely, the H2 is shock-heated in a
tidal accretion flow induced by interaction with the southern companion galaxy.
The latter scenario is supported by an irregular morphology, tidal bridge, and
possible tidal tail imaged with IRAC at 3-9 micron. Unlike ULIRGs, which in
some cases exhibit H2 line luminosities of comparable strength, 3C 326 shows
little star-formation activity (~0.1 Msun/yr). This may represent an important
stage in galaxy evolution. Starburst activity and efficient accretion onto the
central supermassive black hole may be delayed until the shock-heated H2 can
kinematically settle and cool
|
astro-ph
|
the spitzer spectrum of the giant fr ii radio galaxy 3c 326 is dominated by very strong molecular hydrogen emission lines on a faint ir continuum the h2 emission originates in the northern component of a doublegalaxy system associated with 3c 326 the integrated luminosity in h2 purerotational lines is 80e41 ergs which corresponds to 17 of the 870 micron luminosity of the galaxy a wide range of temperatures 1251000 k is measured from the h2 00 s0s7 transitions leading to a warm h2 mass of 11e9 msun lowexcitation ionic forbidden emission lines are consistent with an optical liner classification for the active nucleus which is not luminous enough to power the observed h2 emission the h2 could be shockheated by the radio jets but there is no direct indication of this more likely the h2 is shockheated in a tidal accretion flow induced by interaction with the southern companion galaxy the latter scenario is supported by an irregular morphology tidal bridge and possible tidal tail imaged with irac at 39 micron unlike ulirgs which in some cases exhibit h2 line luminosities of comparable strength 3c 326 shows little starformation activity 01 msunyr this may represent an important stage in galaxy evolution starburst activity and efficient accretion onto the central supermassive black hole may be delayed until the shockheated h2 can kinematically settle and cool
|
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|
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|
707.0897
|
Orbital Solution & Fundamental Parameters of sigma Scorpii
|
The first orbital solution for the spectroscopic pair in the multiple star
system sigma Scorpii, determined from measurements with the Sydney University
Stellar Interferometer (SUSI), is presented. The primary component is of beta
Cephei variable type and has been one of the most intensively studied examples
of its class. The orbital solution, when combined with radial velocity results
found in the literature, yields a distance of 174(+23,-18) pc, which is
consistent with, but more accurate than the Hipparcos value. For the primary
component we determine 18.4+/-5.4 M_sun, -4.12+/-0.34 mag and 12.7+/-1.8 R_sun
for the mass, absolute visual magnitude and radius respectively. A B1 dwarf
spectral type and luminosity class for the secondary is proposed from the mass
determination of 11.9+/-3.1 M_sun and the estimated system age of 10 Myr.
|
astro-ph
|
the first orbital solution for the spectroscopic pair in the multiple star system sigma scorpii determined from measurements with the sydney university stellar interferometer susi is presented the primary component is of beta cephei variable type and has been one of the most intensively studied examples of its class the orbital solution when combined with radial velocity results found in the literature yields a distance of 1742318 pc which is consistent with but more accurate than the hipparcos value for the primary component we determine 18454 m_sun 412034 mag and 12718 r_sun for the mass absolute visual magnitude and radius respectively a b1 dwarf spectral type and luminosity class for the secondary is proposed from the mass determination of 11931 m_sun and the estimated system age of 10 myr
|
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|
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|
707.0898
|
Entanglement and Irreversibility in the Approach to Thermal Equilibrium
|
When a physical system is put in contact with a very large thermal bath, it
undergoes a dissipative (i.e., an apparently irreversible) process that leads
to thermal equilibrium. This dynamical process can be described fully within
quantum physics, involving only unitary, therefore reversible, maps. The
information, initially present in the system, is not erased, but is diluted in
the bath because of entanglement. Irreversibility may arise if, after quantum
information has been thus diluted, some classical information is lost. This
paper reviews a model for thermalization that displays these features. Two new
analytical results are provided for the zero-temperature channels: a new
quantitative measure of entanglement, and a study of irreversibility in the
case where the lost classical information is the label of the particles in the
bath.
|
quant-ph
|
when a physical system is put in contact with a very large thermal bath it undergoes a dissipative ie an apparently irreversible process that leads to thermal equilibrium this dynamical process can be described fully within quantum physics involving only unitary therefore reversible maps the information initially present in the system is not erased but is diluted in the bath because of entanglement irreversibility may arise if after quantum information has been thus diluted some classical information is lost this paper reviews a model for thermalization that displays these features two new analytical results are provided for the zerotemperature channels a new quantitative measure of entanglement and a study of irreversibility in the case where the lost classical information is the label of the particles in the bath
|
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|
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|
707.0899
|
Broken SU(3) Flavor Symmetry and Tribimaximal Neutrino Mixing
|
Recent work on a lepton mass matrix model based on an SU(3) flavor symmetry
which is broken into S_4 is reviewed. The flavor structures of the masses and
mixing are caused by VEVs of SU(2)_L-singlet scalars \phi which are nonets
({\bf 8}+{\bf 1}) of the SU(3) flavor symmetry, and which are broken into {\bf
2}+{\bf 3}+{\bf 3}' and {\bf 1} of S_4. If we require the invariance under the
transformation (\phi^{(8)},\phi^{(1)}) \to (-\phi^{(8)},+\phi^{(1)}) for the
superpotential of the nonet field \phi^{(8+1)}, the model leads to a beautiful
relation for the charged lepton masses. The observed tribimaximal neutrino
mixing is understood by assuming two SU(3) singlet right-handed neutrinos
\nu_R^{(\pm)} and an SU(3) triplet scalar \chi.
|
hep-ph
|
recent work on a lepton mass matrix model based on an su3 flavor symmetry which is broken into s_4 is reviewed the flavor structures of the masses and mixing are caused by vevs of su2_lsinglet scalars phi which are nonets bf 8bf 1 of the su3 flavor symmetry and which are broken into bf 2bf 3bf 3 and bf 1 of s_4 if we require the invariance under the transformation phi8phi1 to phi8phi1 for the superpotential of the nonet field phi81 the model leads to a beautiful relation for the charged lepton masses the observed tribimaximal neutrino mixing is understood by assuming two su3 singlet righthanded neutrinos nu_rpm and an su3 triplet scalar chi
|
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|
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|
707.09
|
Traversable Wormholes Construction in (2+1) Gravity
|
Wormholes have been always an interesting object in gravity theories. In this
paper we make a little review of the principal properties of these objects and
the exotic matter they need to exist. Then, we obtain two specific solutions in
the formalism of (2+1)-dimensional gravity with negative cosmological constant.
The obtained geometries correspond to traversable wormholes with an exterior
geometry correspondient to the well known BTZ black hole solution. We also
discuss the distribution of exotic matter that these wormholes need.
|
gr-qc
|
wormholes have been always an interesting object in gravity theories in this paper we make a little review of the principal properties of these objects and the exotic matter they need to exist then we obtain two specific solutions in the formalism of 21dimensional gravity with negative cosmological constant the obtained geometries correspond to traversable wormholes with an exterior geometry correspondient to the well known btz black hole solution we also discuss the distribution of exotic matter that these wormholes need
|
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|
[-0.14701947165012824, 0.07139587569727154, -0.13583228839561343, 0.1429647504526656, -0.1466666805325076, -0.17530691252904945, -0.06381785092962673, 0.3607757463818416, -0.17300584679469466, -0.3392782268463634, 0.09852679059404182, -0.2837179092573933, -0.15491317196283488, 0.12568790074437858, -0.08888253693003208, 0.07044494450674392, -0.04106384043698199, 0.048681554768700154, -0.10402036839950597, -0.23673110423842444, 0.4287707624491304, 0.03414584638085216, 0.20325778853148221, 0.018885433854302393, 0.07094119518005755, -0.09076641169958748, 0.008892657759133726, 0.06971366368234158, -0.24529145761562177, 0.07915292187244631, 0.23078690865659154, 0.13813920560933185, 0.16307082605198958, -0.45217491295188667, -0.24926073075621388, 0.13995214985479834, 0.1680963176127989, 0.20038191641215236, -0.12153347102430416, -0.3065765318693593, 0.08201073164818809, -0.2397509943926707, -0.19085095924092457, -0.08502759693656117, 0.043318926414940506, -0.02327766567468643, -0.11983536313055083, 0.04681287260573299, 0.04415297570085386, -0.06706276878539938, -0.13886249572387896, -0.07406293821113649, -0.0022878885880345478, 0.09069057150627487, 0.16300550636369734, -0.02486480484949425, 0.11044859082321637, -0.17546590394631495, -0.13285198431112805, 0.3591359636746347, -0.04624864622019231, -0.26261900770477953, 0.19254794214793947, -0.20132070920953993, -0.1299139522423502, 0.05479892433504574, 0.12227145044016652, 0.20737462057732045, -0.1347109247930348, 0.13698907459547627, -0.03603056968422606, 0.13142834698082878, 0.12089733493048697, 0.06787366049247794, 0.3895568343345076, 0.06793797542341054, 0.026583581071463414, 0.1376627870660741, -0.00646721053053625, -0.07895597337046638, -0.3840078839799389, -0.1862413593331894, -0.09486560215591452, 0.08167990435904357, -0.13637527067312477, -0.2210669042658992, 0.29909248660551385, 0.13811051633401802, 0.16076040901825764, -0.023145647102501242, 0.21941254844423383, 0.031173517392016948, 0.031087223114445804, 0.1097352435812354, 0.32673476776108146, 0.12842347273544874, 0.12121000186889433, -0.17807246713637143, -0.07677505542524159, 0.02588990443618968]
|
707.0901
|
Effect of time delay on feedback control of a flashing ratchet
|
It was recently shown that the use of feedback control can improve the
performance of a flashing ratchet. We investigate the effect of a time delay in
the implementation of feedback control in a closed-loop collective flashing
ratchet, using Langevin dynamics simulations. Surprisingly, for a large
ensemble, a well-chosen delay time improves the ratchet performance by allowing
the system to synchronize into a quasi-periodic stable mode of oscillation that
reproduces the optimal average velocity for a periodically flashing ratchet.
For a small ensemble, on the other hand, finite delay times significantly
reduce the benefit of feedback control for the time-averaged velocity, because
the relevance of information decays on a time scale set by the diffusion time
of the particles. Based on these results, we establish that experimental use of
feedback control is realistic.
|
cond-mat.stat-mech
|
it was recently shown that the use of feedback control can improve the performance of a flashing ratchet we investigate the effect of a time delay in the implementation of feedback control in a closedloop collective flashing ratchet using langevin dynamics simulations surprisingly for a large ensemble a wellchosen delay time improves the ratchet performance by allowing the system to synchronize into a quasiperiodic stable mode of oscillation that reproduces the optimal average velocity for a periodically flashing ratchet for a small ensemble on the other hand finite delay times significantly reduce the benefit of feedback control for the timeaveraged velocity because the relevance of information decays on a time scale set by the diffusion time of the particles based on these results we establish that experimental use of feedback control is realistic
|
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|
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|
707.0902
|
Flow Representation of the Bose-Hubbard Hamiltonian : General Case
|
In this paper the explicit flow representation to the Bose-Hubbard
Hamiltonian is given in the general case. This representation may be useful in
creating cat states for the system of atoms trapped in the optical ring.
|
quant-ph math-ph math.MP
|
in this paper the explicit flow representation to the bosehubbard hamiltonian is given in the general case this representation may be useful in creating cat states for the system of atoms trapped in the optical ring
|
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|
[-0.12439511592189471, 0.13937081039572755, -0.06776605502495335, 0.02239149491651915, 0.02009408944286406, -0.14729469067727527, -0.03136802376441968, 0.36485039277209175, -0.28026559286647373, -0.2032438400718901, 0.055626515868223377, -0.238523249165155, -0.13636365129301944, 0.1689852396440175, -0.09116824990875709, 0.026470180083480146, 0.09365541337885791, 0.05843447838884054, -0.03791742564903365, -0.21975094464141876, 0.3174792614041103, 0.03681516476596395, 0.23619627272192803, 0.027033648712353572, 0.034057918211652174, 0.02895985199009172, 0.09778652421664447, -0.03338025991494457, -0.09001447022375134, 0.19747349101655548, 0.2886913215043023, 0.059056289597517915, 0.21240246712437105, -0.46489213722654515, -0.20718640327039692, 0.1529797757199655, 0.2195787900644872, 0.2449799736754762, -0.03688595945843392, -0.33825578591656974, -0.023568781066892877, -0.20272782796786892, -0.1805270985286269, -0.08454316683734457, 0.06837384801151024, -0.02117043177390264, -0.2715424533105559, 0.052434248603983886, 0.07891739444231563, 0.10617334302514791, -0.1038300902582705, 0.007535569337455349, 0.026110024398399725, 0.10123975039459765, -0.09388143453462464, 0.03401609907288932, 0.07363904360681772, -0.16235145795831663, -0.037528437588156924, 0.41601526080113316, -0.07073187328771585, -0.22608374535209602, 0.1617144937109616, -0.14736395900965565, -0.0977739625506931, 0.06678012686057223, 0.17131600722980997, 0.09839099842227167, -0.1314827387428118, 0.07663170613038044, -0.13097331186549532, 0.12403747408340375, 0.04189624676170448, 0.0724032533358291, 0.21719882399257687, 0.1513509398791939, 0.05920800455512815, 0.2234610318846535, -0.025750332098040316, -0.11531720796806945, -0.30888481557162273, -0.21024071885686782, -0.22119610477238894, 0.04156367198771073, -0.04929765457442651, -0.12598921976880068, 0.4730876882870992, 0.15564551242277957, 0.154017708885173, -0.04535305763905247, 0.278880312676645, 0.18805851513105962, 0.0374537192336801, 0.07476122311264691, 0.23132455649061334, 0.09819339241625534, 0.08139531054378797, -0.22968019731342793, -0.004076238876829545, 0.10581648432546192]
|
707.0903
|
Loss-tolerant operations in parity-code linear optics quantum computing
|
A heavy focus for optical quantum computing is the introduction of
error-correction, and the minimisation of resource requirements. We detail a
complete encoding and manipulation scheme designed for linear optics quantum
computing, incorporating scalable operations and loss-tolerant architecture.
|
quant-ph
|
a heavy focus for optical quantum computing is the introduction of errorcorrection and the minimisation of resource requirements we detail a complete encoding and manipulation scheme designed for linear optics quantum computing incorporating scalable operations and losstolerant architecture
|
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|
[-0.18332760862540454, 0.09060446441626961, -0.08662259500277669, 0.03784285310815137, -0.04689910752992881, -0.31112907755825864, 0.07458240280270968, 0.3864261874634969, -0.2603465282162161, -0.3035189146911235, 0.11345347059939645, -0.1741438969038427, -0.15900189683337598, 0.22772951031986036, -0.09778896561137547, 0.2016788363750828, 0.08274693135172129, -0.06075109727680683, -0.12693172970198488, -0.2746532218726842, 0.22019299835358797, 0.10728137451836742, 0.3597090712895519, 0.04083330994226823, 0.14916587140607207, 0.10574366863032705, -0.06900406408270723, -0.03584291863769881, -0.07258441691335879, 0.2444425477388952, 0.2811873532635601, 0.18288890983125097, 0.3029032718929413, -0.44681290424379866, -0.17827433957963398, 0.062093519250323116, 0.08409018103817575, 0.1969529269508233, -0.11472177635388155, -0.2417154329779901, 0.030122264447671018, -0.21418185492879466, -0.04088548360098349, -0.1746044336377006, -0.0038381650014535375, -0.03515785262233725, -0.2774703205612145, -0.07251824860117938, 0.048011770631235684, 0.08667441853322089, 0.037155963556295704, -0.03247280676211966, 0.10301108533320458, 0.08764919805291452, -0.2314599800278972, -0.020123725634460386, 0.1690916493289957, -0.16777035089111642, -0.20243783630920867, 0.409948271062029, 0.027485921121153393, -0.1766563480915992, 0.09460993532679583, 0.03696801548970765, -0.15709839257607727, 0.031155686629445928, 0.20172730120094984, 0.09957869404828862, -0.1507608777059144, 0.12038460872166692, 0.07703469894630344, 0.1605703710382314, 0.03959043327669956, 0.23205033970359518, 0.19008138236638747, 0.2470848700521808, 0.0867319634493661, 0.18695389001483195, -0.06882511177345325, -0.15635309424741486, -0.3004414544832942, -0.2139161688422686, -0.2038315236078281, 0.019903220505894798, -0.0397585640944032, -0.1428012317536693, 0.39663534890582686, 0.10685269323814857, 0.07645578258425782, 0.055340566525333805, 0.4180616818760571, 0.10689665864858973, 0.09023807464185857, 0.14171421423701472, 0.1484580732097751, 0.1428245856965843, 0.128102286228616, -0.26269204727079914, -0.001179681919319065, 0.04515940147010904]
|
707.0904
|
Brown representability for space-valued functors
|
In this paper we prove two theorems which resemble the classical
cohomological and homological Brown representability theorems. The main
difference is that our results classify small contravariant functors from
spaces to spaces up to weak equivalence of functors.
In more detail, we show that every small contravariant functor from spaces to
spaces which takes coproducts to products up to homotopy and takes homotopy
pushouts to homotopy pullbacks is naturally weekly equivalent to a
representable functor.
The second representability theorem states: every contravariant continuous
functor from the category of finite simplicial sets to simplicial sets taking
homotopy pushouts to homotopy pullbacks is equivalent to the restriction of a
representable functor. This theorem may be considered as a contravariant analog
of Goodwillie's classification of linear functors.
|
math.AT
|
in this paper we prove two theorems which resemble the classical cohomological and homological brown representability theorems the main difference is that our results classify small contravariant functors from spaces to spaces up to weak equivalence of functors in more detail we show that every small contravariant functor from spaces to spaces which takes coproducts to products up to homotopy and takes homotopy pushouts to homotopy pullbacks is naturally weekly equivalent to a representable functor the second representability theorem states every contravariant continuous functor from the category of finite simplicial sets to simplicial sets taking homotopy pushouts to homotopy pullbacks is equivalent to the restriction of a representable functor this theorem may be considered as a contravariant analog of goodwillies classification of linear functors
|
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|
[-0.13410083157472283, 0.03125761883829029, -0.13143924263591367, 0.17800028319188935, -0.13866959327471354, -0.13584953751189693, -0.0056491641678862396, 0.3533628003882064, -0.4919270650754052, -0.14244127933183806, 0.0353400312625097, -0.1894721025281826, -0.10899794262443338, 0.1516000614670526, -0.2963742746355673, -0.06782094466184536, 0.08017676283094671, 0.0685468862479132, -0.09520824640358408, -0.28414154943499353, 0.5010671258092888, -0.09813031229010273, 0.2172976655298161, 0.049785559230874625, 0.1369504781041835, -0.048540914457501666, -0.01539807160565209, -0.006342113521250505, -0.11743873458380544, 0.12666968364154005, 0.40775632279204027, 0.07518893670132984, 0.22019556597074225, -0.34475118003460775, -0.02712603829680912, 0.2272331972659055, 0.0698925589414073, 0.02087004063463199, 0.06445598974201974, -0.3738310295908201, 0.15510775913454353, -0.195582082671594, -0.054750385093352484, -0.14464475952028746, 0.08643445838242769, 0.032084721538628784, -0.2732339610360683, -0.11022277977017145, 0.15744034717265035, 0.12611623591322813, -0.161320366310857, -0.03286291711452988, -0.14229479585135837, 0.10565616967787425, -0.01359383548392103, 0.061164983319148665, 0.13752698239536146, -0.023296064524460706, -0.14069206070064777, 0.4036336218968274, -0.0751994070568828, -0.19086703489865026, 0.17746488064163243, -0.12366567380095442, -0.22780666986457823, 0.16294319641911575, -0.04485890016170038, 0.16225149236514322, -0.02773048163902375, 0.19454031817581235, -0.14944295204364724, 0.07015484421243591, 0.17295403885955532, 0.05707670036598199, 0.09204725479526867, 0.07171824660585, 0.06363421704454889, 0.17832638155537536, 0.07742052653761235, -0.0753562994537905, -0.3606148443274921, -0.17586364349230163, -0.05427817930091893, 0.1747596029177188, -0.10256008152646245, -0.21528221583444504, 0.3376012145571651, 0.12814935418681406, 0.10965721018710023, 0.2718309643622037, 0.29313563747752097, 0.011082814227143724, 0.06988800801486979, -0.051398207452298415, 0.15641477203837806, 0.3493204843778644, 0.013300881660994022, 0.01455485775870564, -0.09783048404290551, 0.33337793929686377]
|
707.0905
|
Muon Identification at ATLAS and CMS
|
Muonic final states will provide clean signatures formany physics processes
at the LHC. The two LHC experiments ATLAS and CMS will be able to identify
muons with a high reconstruction efficiency above 96% and a high transverse
momentum resolution better than 2% for transverse momenta below 400 GeV/c and
about 10% at 1 TeV/c. The two experiments follow complentary concepts of muon
detection. ATLAS has an instrumented air-toroid mangetic system serving as a
stand-alone muon spectrometer. CMS relies on high bending power and momentum
resolution in the inner detector, and uses an iron yoke to increase its
magnetic field. The iron yoke is instrumented with chambers used for muon
identification. Therefore, muon momenta can only be reconstructed with high
precision by combining inner-detector information with the data from the muon
chambers.
|
hep-ex
|
muonic final states will provide clean signatures formany physics processes at the lhc the two lhc experiments atlas and cms will be able to identify muons with a high reconstruction efficiency above 96 and a high transverse momentum resolution better than 2 for transverse momenta below 400 gevc and about 10 at 1 tevc the two experiments follow complentary concepts of muon detection atlas has an instrumented airtoroid mangetic system serving as a standalone muon spectrometer cms relies on high bending power and momentum resolution in the inner detector and uses an iron yoke to increase its magnetic field the iron yoke is instrumented with chambers used for muon identification therefore muon momenta can only be reconstructed with high precision by combining innerdetector information with the data from the muon chambers
|
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|
[-0.025505369378796477, 0.2514181122695752, -0.037965866077075326, 0.07298797667191517, -0.061138275211427624, -0.15454716455396705, -0.046991477379443376, 0.3472980402087367, -0.1704980259665882, -0.41795289674847147, 0.057564177092505754, -0.39489075993224393, 0.13275727566595621, 0.223183849520292, -0.006152957681507811, 0.08315795087979695, 0.12861089267140974, -0.0019624865406255173, -0.11276023613846325, -0.19400853917780003, 0.18275879255649963, 0.2021788422542617, 0.2768470015996466, 0.10546207013283307, 0.18834366202152766, 0.0015187216244315304, -0.016931451177160353, -0.010484914992033965, -0.08136595787084479, 0.04808153393339205, 0.3015819683132004, 0.08771349047127319, 0.11981109679698593, -0.40650038940348027, -0.07206183919448435, 0.06587928246090731, 0.13370897872446794, 0.0014709730515271191, -0.08561221489272132, -0.2874107229831357, 0.1502676429593657, -0.19735560460588125, -0.13794315803070062, -0.05526792916183279, -0.0713517074647367, -0.0308584675245999, -0.26532161393474174, 0.02896331807994467, -0.006286016100738931, 0.12835729934685813, -0.045236478531256494, -0.18967830940006727, -0.010377242831205289, 0.06014695792554284, 0.038248890341721534, 0.10085746499904116, 0.20755801957071296, -0.14539384535389152, -0.191660424195758, 0.257671958997875, -0.02228296054474456, -0.17773563362746023, 0.2100136829026806, -0.2567162468780096, -0.054238641619916976, 0.236620755455508, 0.22012965992005087, 0.04557908465719129, -0.18006980633289796, 0.03243765972809514, 0.023900583525752927, 0.21762013727227064, 0.07488592650638673, 0.02627457948364904, 0.23831800419807903, 0.2595096079735305, 0.10492523057811608, 0.07396466406080579, -0.23939093595047986, 0.04201413226115892, -0.3430448039874845, -0.16853192395816638, -0.12781680752999905, 0.03586378332418133, -0.021397501475330788, -0.04200243112433145, 0.3848090413187843, 0.0876155909862164, 0.2672043300002784, -0.04114300779279644, 0.3683155501100022, 0.009759772172029035, 0.12324682496466094, 0.03113079326608636, 0.278087843473502, 0.1310777888086984, 0.2225092102876153, -0.21442660846835457, 0.013428886281693076, 0.037987888029842515]
|
707.0906
|
A spectral sequence to compute L2-Betti numbers of groups and groupoids
|
We construct a spectral sequence for L2-type cohomology groups of discrete
measured groupoids. Based on the spectral sequence, we prove the Hopf-Singer
conjecture for aspherical manifolds with poly-surface fundamental groups. More
generally, we obtain a permanence result for the Hopf-Singer conjecture under
taking fiber bundles whose base space is an aspherical manifold with
poly-surface fundamental group. As further sample applications of the spectral
sequence, we obtain new vanishing theorems and explicit computations of
L2-Betti numbers of groups and manifolds and obstructions to the existence of
normal subrelations in measured equivalence relations.
|
math.DS math.AT
|
we construct a spectral sequence for l2type cohomology groups of discrete measured groupoids based on the spectral sequence we prove the hopfsinger conjecture for aspherical manifolds with polysurface fundamental groups more generally we obtain a permanence result for the hopfsinger conjecture under taking fiber bundles whose base space is an aspherical manifold with polysurface fundamental group as further sample applications of the spectral sequence we obtain new vanishing theorems and explicit computations of l2betti numbers of groups and manifolds and obstructions to the existence of normal subrelations in measured equivalence relations
|
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|
[-0.18652338490034615, 0.06834624311435117, -0.13747050494340987, 0.12435888816554357, -0.08271039013975653, -0.11202553253963418, 0.04349334664835498, 0.39664134462417544, -0.2809365878802264, -0.2760298339671445, 0.129036991079552, -0.1797377715829289, -0.13685325782574798, 0.2410938368639213, -0.15071445992537613, -0.016166517437414277, 0.08732822375243594, 0.06386843492844324, -0.10615283694525046, -0.2429196849551009, 0.45803372968716183, -0.04420538307114066, 0.2455919529900126, 0.044534209740332106, 0.1087425156742677, 0.0017933652457920298, -0.04580619713912407, -0.021933375231870826, -0.18517078020363703, 0.17225132151453318, 0.27192010841835507, 0.06391354532773211, 0.1820866371312275, -0.358070219288451, -0.16452239149239387, 0.20745326038557052, 0.11064918424891329, 0.027251773085659264, -0.058435497689897184, -0.3004168137993621, 0.14626556413847652, -0.1174647221141013, -0.18722198700168352, -0.10061583672810731, 0.044107058042681765, 0.050922479801650704, -0.20965910749844457, 0.020371962279809273, 0.10860855676148129, 0.11858047494643378, -0.10653775085791431, -0.0805937438486037, -0.04598354884883624, 0.16938971320766655, 0.02743923673719026, -0.04349436989889063, 0.0706048668746906, -0.04271047386801106, -0.12551870681987753, 0.3657986320041377, -0.07680227253157859, -0.17962494244713378, 0.1348533674568773, -0.13755637415866742, -0.24258775906316166, 0.13800759441165747, 0.10310636929653842, 0.1703855531161715, -0.01093182979344294, 0.09256539452920036, -0.10577909514607711, 0.09045975648894392, 0.08650823012422557, 0.04154888797422935, 0.10544496737741704, 0.11584626147041804, 0.12366162562186177, 0.11451661763123996, -0.0055919364830693125, -0.02037153695442382, -0.3316613022537752, -0.23165061628852768, -0.1180460677246681, 0.1674564377747305, -0.14630420228694538, -0.1823286386206746, 0.3499773638162377, 0.014152935673964435, 0.17185179566985917, 0.20663234572215328, 0.21517433226643795, 0.08143981163598725, 0.04242613023125577, 0.04189784578101217, 0.13483267639303345, 0.3170442969334879, -0.028040614187845897, -0.09641713259912942, -0.07236050832588439, 0.2166208903861885]
|
707.0907
|
The concrete theory of numbers : Problem of simplicity of Fermat
number-twins
|
The problem of simplicity of Fermat number-twins $f_{n}^{\pm}=2^{2^n}\pm3$ is
studied. The question for what $n$ numbers $f_{n}^{\pm}$ are composite is
investigated. The factor-identities for numbers of a kind $x^2 \pm k $ are
found.
|
math.GM
|
the problem of simplicity of fermat numbertwins f_npm22npm3 is studied the question for what n numbers f_npm are composite is investigated the factoridentities for numbers of a kind x2 pm k are found
|
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|
[-0.25137334670229206, 0.13598651747251378, -0.03697117563770634, 0.11230383110874943, -0.03925206464040896, -0.14467886981457986, -0.006238151036588283, 0.3119934160133888, -0.27949951935944883, -0.3453655146576207, 0.08058518315825997, -0.3076746382204623, -0.09945566657577352, 0.23669772559841132, -0.01678480930497934, 0.04427609457794962, -0.02375177318101813, 0.14290746918012356, -0.026708942789841313, -0.31294598404703466, 0.3102815828189768, -0.0557667878135268, 0.18634804379965725, 0.0076443922930750354, 0.055720682603162555, -0.046276633097822296, 0.030735469423234463, -0.003235403175369419, -0.13831198047685983, 0.09801431866924695, 0.2351514524619641, 0.12403954340723054, 0.2830895421833828, -0.2919206378082263, -0.16101337301320043, 0.11384748712438962, 0.1380946116265038, -0.01962177028301461, -0.017727927529606325, -0.16338203532685494, 0.17891609626982746, -0.07763422473237433, -0.21100605343436374, -0.015952847384173293, 0.1229116704700322, 0.031990830433265914, -0.2695055266778017, 0.052709795663069034, 0.04596303236381761, 0.11389694061001827, 0.02799531290757245, -0.23143180395508633, -0.0006098946363761507, 0.05376339047055306, 0.04296107749165646, -0.012014856610190252, 0.0138212778958781, -0.13441997605921893, -0.07499392363162519, 0.45907365402271005, 0.04755568947514583, -0.18966782780299926, 0.06466239700415011, -0.14011487461112695, -0.15834429278841305, 0.14882083725312661, 0.08502952960030787, 0.17719848396192336, -0.09660043201312937, 0.15250193244167443, -0.14122568176866607, 0.15445772372186184, 0.12193055759216177, 0.0249453099637196, 0.18008855884445124, 0.12628772212513562, -0.05000286713114072, 0.15973742322289738, -0.051341387635931886, -0.062262888323387194, -0.26105782877782296, -0.181075730842763, -0.23206521568273933, 0.12467914453611292, -0.025391326863960974, -0.09679703226569912, 0.29037045009819595, 0.044448724080776346, 0.18747914786418451, 0.03816988421925183, 0.19212511920466505, 0.12438153135108537, -0.04137109173461795, 0.0011537482897783149, 0.2068494988669609, 0.2034664207362923, 0.06703360430125532, -0.189479927596604, 0.05261569418783846, 0.10075672735171072]
|
707.0908
|
Reheating and Cosmic String Production
|
We compute the string production rate at the end of inflation, using the
string spectrum obtained in \lss in a near-de Sitter space. Our result shows
that highly excited strings are hardly produced, thus the simple slow-roll
inflation alone does not offer a cosmic string production mechanism.
|
hep-th
|
we compute the string production rate at the end of inflation using the string spectrum obtained in lss in a nearde sitter space our result shows that highly excited strings are hardly produced thus the simple slowroll inflation alone does not offer a cosmic string production mechanism
|
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|
[-0.16172859630488018, 0.21228666383614567, -0.14169869802773316, 0.18539444092621513, -0.07719661840336754, -0.11203705435222451, 0.011927684016050176, 0.31005488819581395, -0.23962996355158853, -0.22876657006588388, 0.03243526816863487, -0.21951024909999142, -0.06068583191471531, 0.1945611484982866, -0.006775063601263026, -0.029259500509880958, 0.07133914576595689, 0.03845686349581848, 0.03430989341552746, -0.30281386504623486, 0.2914229992856371, 0.16959901490902646, 0.2992135553442417, 0.02682063362977289, 0.038970636352500386, -0.06510558722917228, -0.02954979013760594, -0.038143929104603076, -0.1549668916796168, 0.11159141468221044, 0.187918270001822, 0.19238119548622598, 0.09943945202580158, -0.4455340845470733, -0.24568066579547335, 0.16446084052601712, 0.21645132613744825, 0.2011068072962634, -0.08501378043574538, -0.2075172808972445, 0.10548965309429517, -0.18573798975867636, -0.08558166624502615, -0.07134288749558494, -0.03983633070342005, -0.11419847663095657, -0.25094610897507125, 0.08814632499768854, -0.023850320913937895, -0.04924090770370466, -0.04506688094400662, 0.004668997779012995, -0.057407320046084044, 0.009637186125396414, 0.09573235438066593, 0.10890521619350035, 0.16964770018301428, -0.15991057945970208, -0.12336589929033467, 0.37648643426438594, -0.17491135437120783, -0.12089104577898979, 0.10824103837713916, -0.18504915201164623, -0.19767856684097268, 0.1238108574353317, 0.07636813157574927, 0.12230762573791311, -0.12667365504943945, 0.19077607230382396, 0.10102106609996012, 0.17496631947405478, 0.14635030470511062, 0.059782837586913336, 0.32986129431965505, 0.12407621201325922, -0.016175737406345123, 0.10749154306076308, -0.033357761086935694, -0.0866795107672744, -0.4141711579992416, -0.04300331696867943, -0.1570249177129107, 0.07630862685278346, -0.1221940678722681, -0.24167944827770932, 0.35027007044273173, 0.06447850128120565, 0.23967281417881556, 0.08480858707681616, 0.23733865846186242, 0.06477600034138069, 0.0033323354672323514, 0.11352989874146086, 0.32772725701649136, 0.04423819418917311, 0.16130638116613982, -0.20879603408405834, -0.0063437189252928215, 0.09882684087658182]
|
707.0909
|
Spectrum Sensing in Cognitive Radios Based on Multiple Cyclic
Frequencies
|
Cognitive radios sense the radio spectrum in order to find unused frequency
bands and use them in an agile manner. Transmission by the primary user must be
detected reliably even in the low signal-to-noise ratio (SNR) regime and in the
face of shadowing and fading. Communication signals are typically
cyclostationary, and have many periodic statistical properties related to the
symbol rate, the coding and modulation schemes as well as the guard periods,
for example. These properties can be exploited in designing a detector, and for
distinguishing between the primary and secondary users' signals. In this paper,
a generalized likelihood ratio test (GLRT) for detecting the presence of
cyclostationarity using multiple cyclic frequencies is proposed. Distributed
decision making is employed by combining the quantized local test statistics
from many secondary users. User cooperation allows for mitigating the effects
of shadowing and provides a larger footprint for the cognitive radio system.
Simulation examples demonstrate the resulting performance gains in the low SNR
regime and the benefits of cooperative detection.
|
cs.IT math.IT
|
cognitive radios sense the radio spectrum in order to find unused frequency bands and use them in an agile manner transmission by the primary user must be detected reliably even in the low signaltonoise ratio snr regime and in the face of shadowing and fading communication signals are typically cyclostationary and have many periodic statistical properties related to the symbol rate the coding and modulation schemes as well as the guard periods for example these properties can be exploited in designing a detector and for distinguishing between the primary and secondary users signals in this paper a generalized likelihood ratio test glrt for detecting the presence of cyclostationarity using multiple cyclic frequencies is proposed distributed decision making is employed by combining the quantized local test statistics from many secondary users user cooperation allows for mitigating the effects of shadowing and provides a larger footprint for the cognitive radio system simulation examples demonstrate the resulting performance gains in the low snr regime and the benefits of cooperative detection
|
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|
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|
707.091
|
Cosmic-Ray Heating of Molecular Gas in the Nuclear Disk: Low Star
Formation Efficiency
|
Understanding the processes occurring in the nuclear disk of our Galaxy is
interesting in its own right, as part of the Milky Way Galaxy, but also because
it is the closest galactic nucleus. It has been more than two decades since it
was recognized that the general phenomenon of higher gas temperature in the
inner few hundred parsecs by comparison with local clouds in the disk of the
Galaxy. This is one of the least understood characteristics of giant molecular
clouds having a much higher gas temperature than dust temperature in the inner
few degrees of the Galactic center. We propose that an enhanced flux of
cosmic-ray electrons, as evidenced recently by a number of studies, are
responsible for directly heating the gas clouds in the nuclear disk, elevating
the temperature of molecular gas ($\sim$ 75K) above the dust temperature
($\sim$ 20K). In addition we report the detection of nonthermal radio emission
from Sgr B2-F based on low-frequency GMRT and VLA observations. The higher
ionization fraction and thermal energy due to the impact of nonthermal
electrons in star forming sites have important implications in slowing down
star formation in the nuclear disk of our galaxy and nuclei of galaxies.
|
astro-ph
|
understanding the processes occurring in the nuclear disk of our galaxy is interesting in its own right as part of the milky way galaxy but also because it is the closest galactic nucleus it has been more than two decades since it was recognized that the general phenomenon of higher gas temperature in the inner few hundred parsecs by comparison with local clouds in the disk of the galaxy this is one of the least understood characteristics of giant molecular clouds having a much higher gas temperature than dust temperature in the inner few degrees of the galactic center we propose that an enhanced flux of cosmicray electrons as evidenced recently by a number of studies are responsible for directly heating the gas clouds in the nuclear disk elevating the temperature of molecular gas sim 75k above the dust temperature sim 20k in addition we report the detection of nonthermal radio emission from sgr b2f based on lowfrequency gmrt and vla observations the higher ionization fraction and thermal energy due to the impact of nonthermal electrons in star forming sites have important implications in slowing down star formation in the nuclear disk of our galaxy and nuclei of galaxies
|
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|
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|
707.0911
|
A Complete Survey of the Central Molecular Zone in NH3
|
We present a map of the major part of the central molecular zone (CMZ) of
simultaneous observations in the NH3 (J,K) = (1,1) and (2,2) lines using the
Kagoshima 6-m telescope. The mapped area is -1.000 < l < 1.625 deg, -0.375 < b
< +0.250 deg. The kinetic temperatures derived from the (2,2) to (1,1)
intensity ratios are 20--80 K or exceed 80 K. The gases corresponding to
temperature of 20--80 K and > 80 K contain 75% and 25% of the total NH3 flux,
respectively. These temperatures indicate that the dense molecular gas in the
CMZ is dominated by gas that is warmer than the majority of the dust present
there. A comparison with the CO survey by Sawada et al. (2001) shows that the
NH3 emitting region is surrounded by a high pressure region on the l-v plane.
Although NH3 emission traces dense gas, it is not extended into a high pressure
region. Therefore, the high pressure region is less dense and has to be hotter.
This indicates that the molecular cloud complex in the Galactic center region
has a ``core'' of dense and warm clouds which are traced by the NH3 emission,
and an ``envelope'' of less dense and hotter gas clouds. Besides heating by
ambipolar diffusion, the hot plasma gas emitting the X-ray emission may heat
the hot ``envelope''.
|
astro-ph
|
we present a map of the major part of the central molecular zone cmz of simultaneous observations in the nh3 jk 11 and 22 lines using the kagoshima 6m telescope the mapped area is 1000 l 1625 deg 0375 b 0250 deg the kinetic temperatures derived from the 22 to 11 intensity ratios are 2080 k or exceed 80 k the gases corresponding to temperature of 2080 k and 80 k contain 75 and 25 of the total nh3 flux respectively these temperatures indicate that the dense molecular gas in the cmz is dominated by gas that is warmer than the majority of the dust present there a comparison with the co survey by sawada et al 2001 shows that the nh3 emitting region is surrounded by a high pressure region on the lv plane although nh3 emission traces dense gas it is not extended into a high pressure region therefore the high pressure region is less dense and has to be hotter this indicates that the molecular cloud complex in the galactic center region has a core of dense and warm clouds which are traced by the nh3 emission and an envelope of less dense and hotter gas clouds besides heating by ambipolar diffusion the hot plasma gas emitting the xray emission may heat the hot envelope
|
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|
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|
707.0912
|
An SU(3) symmetry for light neutrinos
|
It is proposed that light neutrinos form a triplet in a global SU(3) symmetry
in mass eigenstate basis. Assuming that the SU(3)symmetry is broken in the
direction (-alambda_{3}+frac{b}/{sqrt{3}}lambda_{8}), and after going to the
flavor basis we predict atmospheric mixing angle, sin ^{2}theta_{23}=0.5 and
sin theta_{13}=0 if nu_{mu}-nu_{tau} symmetry is assumed. In the flavor basis
the diagonal part of matrix coefficient of b (dominant part) is found to
transform like (lambda_{3}+frac{1}/{sqrt{3}}lambda_{8}). Imposing the same on
matrix coefficient of $a$ fixes solar mixing angle,sin ^{2}theta
_{12}=frac{1}{3}. Implications for neutrinoless double beta-decay are
discussed.
|
hep-ph
|
it is proposed that light neutrinos form a triplet in a global su3 symmetry in mass eigenstate basis assuming that the su3symmetry is broken in the direction alambda_3fracbsqrt3lambda_8 and after going to the flavor basis we predict atmospheric mixing angle sin 2theta_2305 and sin theta_130 if nu_munu_tau symmetry is assumed in the flavor basis the diagonal part of matrix coefficient of b dominant part is found to transform like lambda_3frac1sqrt3lambda_8 imposing the same on matrix coefficient of a fixes solar mixing anglesin 2theta _12frac13 implications for neutrinoless double betadecay are discussed
|
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|
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|
707.0913
|
A vanishing theorem for sheaves of small differential operators in
positive characteristic
|
Let $X$ be a smooth variety over an algebraically closed field $k$ of
positive characteristic, ${\rm D}_X$ the sheaf of PD-differential operators,
and ${\bar D}_X$ its central reduction, the sheaf of small differential
operators. In this paper we show that if $X$ is a line-hyperplane incidence
variety (a partial flag variety of type $(1,n,n+1)$) or a quadric of arbitrary
dimension (in this case the characteristic is supposed to be odd) then ${\rm
H}^{i}(X,{\bar D}_X)=0$ for $i>0$. Using this vanishing result and the derived
localization theorem for crystalline differential operators (\cite{BMR}) we
show that the Frobenius pushforward of the structure sheaf is a tilting bundle
on these varieties, provided that $p>h$, the Coxeter number of the
corresponding group.
|
math.AG math.RT
|
let x be a smooth variety over an algebraically closed field k of positive characteristic rm d_x the sheaf of pddifferential operators and bar d_x its central reduction the sheaf of small differential operators in this paper we show that if x is a linehyperplane incidence variety a partial flag variety of type 1nn1 or a quadric of arbitrary dimension in this case the characteristic is supposed to be odd then rm hixbar d_x0 for i0 using this vanishing result and the derived localization theorem for crystalline differential operators citebmr we show that the frobenius pushforward of the structure sheaf is a tilting bundle on these varieties provided that ph the coxeter number of the corresponding group
|
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|
[-0.2327982724361521, 0.0644110818311674, -0.06674328701670415, 0.03239085260013651, -0.07119260049616319, -0.12525234785529651, -0.04486335116234841, 0.3187873243753399, -0.36665476085285525, -0.16413510120141186, 0.0804347596401515, -0.21463420834541985, -0.138581284249085, 0.20333491056849848, -0.12630272632564551, -0.05131704311653656, 0.006116222197306342, 0.13144267438162519, -0.10166479718048192, -0.2833303115403396, 0.45262947101478596, -0.08802755018197266, 0.2149533887131838, 0.07004007438081317, 0.12835378255528798, 0.023216026236436198, 0.04400977909764541, 0.01987115237404526, -0.13417230593345916, 0.1279392787359289, 0.3294715504556994, 0.06739139513644789, 0.18631578225384665, -0.344061621543785, -0.1198039435049785, 0.21808059109025635, 0.13058453198963044, 0.018789040964163308, -0.014808296570013877, -0.273517446956248, 0.16654706459459184, -0.19385343868218893, -0.17334584941272624, -0.06376473372802138, 0.11431872196616107, 0.007958487378865746, -0.29140706448743003, -0.019085885256312655, 0.09119136059390646, 0.16489586971874814, -0.06455491861041603, -0.10594768851712745, -0.10602846339627701, 0.01688410722688007, -0.0245012292330752, 0.09867263872937267, 0.13779158684857457, -0.09203377999074291, -0.08368687576564428, 0.3295830466377083, -0.10789903197603833, -0.24913719056972436, 0.09107837713963818, -0.2151594093551726, -0.09358798358880449, 0.17448457192430006, 0.09975954305679936, 0.19069049581386416, 0.007292854973327069, 0.18832348948074337, -0.14803014555945992, 0.0999507752297047, 0.05754115368472412, 0.005397489007529137, 0.09485802325408647, 0.08807874654303305, 0.08961272539246627, 0.06740710726964087, -0.0488707251435179, 0.006356500105799309, -0.39697936128816635, -0.23025743711540209, -0.08923068282586298, 0.2212828628502653, -0.12073235495128236, -0.15009335825119965, 0.37319722116600523, 0.05000331248655649, 0.2395503599898023, 0.0946868632870194, 0.22201863085917597, 0.11106287942467523, 0.04682002509694679, 0.014104043824253105, 0.09589842545808226, 0.2431195304961875, -0.018439817043794653, -0.186267279090576, 0.0056953667704614675, 0.14474005121571412]
|
707.0914
|
Method of characteristics and solution of DGLAP evolution equation in
leading order (LO) and next to leading order (NLO) at small-x
|
In this paper the singlet and non-singlet structure functions have been
obtained by solving Dokshitzer, Gribove, Lipatov, Alterelli, Parisi (DGLAP)
evolution equations in leading order (LO) and next to leading order (NLO) at
the small x limit. Here we have used a Taylor Series expansion and then the
method of characteristics to solve the evolution equations. We have also
calculated t and x-evolutions of deuteron structure function and the results
are compared with the New Muon Collaboration (NMC) data.
|
hep-ph
|
in this paper the singlet and nonsinglet structure functions have been obtained by solving dokshitzer gribove lipatov alterelli parisi dglap evolution equations in leading order lo and next to leading order nlo at the small x limit here we have used a taylor series expansion and then the method of characteristics to solve the evolution equations we have also calculated t and xevolutions of deuteron structure function and the results are compared with the new muon collaboration nmc data
|
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|
[-0.051479949869892815, 0.0944609680067893, -0.13582349948996267, 0.089991043822223, -0.05754254060470826, -0.02050061748278412, -0.017420661144333518, 0.3425128322892955, -0.21315697663427366, -0.2884157544921164, 0.06618422577339043, -0.3108913195258998, -0.088987455812174, 0.10811558939734256, 0.08329564734519303, 0.13677820167806629, 0.031039248359716172, -0.009573894111415395, -0.1155098606046144, -0.2863609167723009, 0.3529358677469291, 0.038638950579545715, 0.24091288845913558, 0.09587498252316341, 0.12278617601750975, -0.024168402851595508, -0.035689984103543806, -0.020645104445420302, -0.15746818634064555, 0.07286611599726724, 0.24560860537186072, 0.024616194317455996, 0.1934349964487717, -0.42467356436922177, -0.12170787555673583, 0.04320057020704081, 0.13936633012838082, 0.11232454661134776, -0.008585790619737917, -0.26395279333575977, 0.09854432944111623, -0.24992506662020822, -0.16676159905172983, -0.16358107803752284, -0.024922644646910876, 0.027354524658339752, -0.31324542502044134, 0.0675776252222955, -0.040134756983100595, -0.014243321284627566, -0.05317276401154987, -0.1899768090867377, -0.03131089441768535, 0.0846914537553373, 0.08453395423462748, 0.11511422479646159, 0.0073896201520964695, -0.13988392647089704, -0.1558932203061685, 0.3525930333084294, -0.10617357900354092, -0.17645412843142236, 0.08956356155277871, -0.2132397050146836, -0.15191387071262125, 0.12939621081164518, 0.1918400187565425, 0.1370882832901794, -0.2092413210700109, 0.1527761430804642, 0.006862048126224961, 0.10944628415254319, 0.10546767546541312, -0.0012165442431895908, 0.06694359553663375, 0.16458900870344081, -0.03148809495357821, 0.06865361811254513, -0.060893100659913296, -0.10449839072519695, -0.29935108986380815, -0.09946575346584251, -0.11375599996150508, 0.032450014864421124, -0.0840905374571811, -0.09759187206093754, 0.3902807598086921, 0.13394953032302392, 0.186052487969592, 0.045960774572638724, 0.255243256688118, 0.1875821358566596, 0.09102878765302844, 0.09201113967672474, 0.21087683047857378, 0.18515246806896063, 0.15290164891872313, -0.26916698668176287, 0.05557462037238595, 0.13462030825314003]
|
707.0915
|
D-affinity and Frobenius morphism on quadrics
|
We compute decomposition of Frobenius push-forwards of line bundles on
quadrics into a direct sum of line bundles and spinor bundles. As an
application we show when the Frobenius push-forward gives a tilting bundle and
we apply it to study D-modules on quadrics.
|
math.AG math.RT
|
we compute decomposition of frobenius pushforwards of line bundles on quadrics into a direct sum of line bundles and spinor bundles as an application we show when the frobenius pushforward gives a tilting bundle and we apply it to study dmodules on quadrics
|
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|
[-0.23049740397999452, -0.07951670894392517, -0.06906513895752818, 0.0634288020258726, -0.13609528931420903, -0.10589589042112578, -0.02421177694097508, 0.43336925300401313, -0.33243088892032935, -0.11333997362444914, 0.06836400691116619, -0.19086293419173292, -0.2036921924933098, 0.1918355134250813, -0.15352992351751688, -0.05704942120369091, 0.07961116701927642, 0.07323746288974964, -0.14654028329045274, -0.2902127807597132, 0.5250230913245401, -0.04775969507605877, 0.3033727730927599, 0.12105866483694246, 0.16661155099309113, 0.07154275427117597, 0.008772792013058828, -0.044842470025773656, -0.14184901876331762, 0.1544708217017699, 0.2898239466513312, 0.10996336821293415, 0.1305266574544962, -0.3915356801996051, -0.05444946246178344, 0.22161481988637946, 0.1443787065529546, 0.01804853915128597, 0.04881309760669463, -0.26997824948887494, 0.06603385494253057, -0.12926981546158015, -0.1149186886153942, -0.18453057801220998, 0.054238649301750715, 0.03524511857066563, -0.22378044392437088, -0.11659962809536346, 0.06337443810649389, 0.19855077798629917, -0.13141955154254858, -0.09303897913805274, -0.11987725125495778, 0.00863983991980921, 0.012787287426722605, -0.01007954511509905, 0.20009487147204752, -0.056272414664542955, -0.16188578368272893, 0.38778009746483594, -0.1356769079494095, -0.23355290061945833, 0.06550267011706912, -0.11062674195137481, -0.10990354193504466, 0.17650357358764077, 0.11529767851150313, 0.23938026239142515, 0.13868038024215926, 0.09665800151036143, -0.1767359205716571, 0.03523213217078253, 0.08992427126179602, -0.08545341000480708, 0.16387296506463614, 0.0811905514741273, 0.0787537086289376, 0.1627138577791494, -0.06907629943994242, -0.07298963438979415, -0.40009559309759807, -0.3705342962125013, -0.037239799839119576, 0.26739166366196304, -0.06619034100697528, -0.16330984719422495, 0.41905716711893504, 0.050329142098509985, 0.3392521359004773, 0.1712368905414329, 0.30026028686484624, 0.04807515743156072, 0.0803863434716626, -0.04773619563080544, 0.1758565468507884, 0.3580006812374259, -0.06642846973223049, -0.08456724864798923, -0.16623585026841178, 0.2704375199973583]
|
707.0916
|
Local Tunneling Spectroscopy across a Metamagnetic Critical Point in the
Bi-layer Ruthenate Sr3Ru2O7
|
The local spectroscopic signatures of metamagnetic criticality in Sr3Ru2O7
were explored using scanning tunneling microscopy (STM). Singular features in
the tunneling spectrum were found close to the Fermi level, as would be
expected in a Stoner picture of itinerant electron metamagnetism. These
features showed a pronounced magnetic field dependence across the metamagnetic
critical point, which cannot be understood in terms of a naive Stoner theory.
In addition, a pseudo-gap structure was observed over several tens of meV,
accompanied by a c(2x2) superstructure in STM images. This result represents a
new electronic ordering at the surface in the absence of any measurable surface
reconstruction.
|
cond-mat.str-el
|
the local spectroscopic signatures of metamagnetic criticality in sr3ru2o7 were explored using scanning tunneling microscopy stm singular features in the tunneling spectrum were found close to the fermi level as would be expected in a stoner picture of itinerant electron metamagnetism these features showed a pronounced magnetic field dependence across the metamagnetic critical point which cannot be understood in terms of a naive stoner theory in addition a pseudogap structure was observed over several tens of mev accompanied by a c2x2 superstructure in stm images this result represents a new electronic ordering at the surface in the absence of any measurable surface reconstruction
|
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|
[-0.17640226100159523, 0.17708112851071817, -0.09670545008982746, 0.11159307180451623, -0.025188371614394082, -0.1300316258611229, 0.09198570624273718, 0.3556283437826026, -0.279967164235691, -0.3193554393678474, -0.04299074557694929, -0.32996098639873356, -0.161392913128321, 0.18367375136473968, 0.004020230289405355, 0.001337111412654989, -0.019908138846333783, 0.009344352306260798, -0.12832277304886913, -0.22148198578641035, 0.25755823679187767, 0.0574048303354245, 0.2916334440770487, 0.10756106616799326, -0.007512534301405629, -0.020553449715057816, 0.11836897109885915, 0.07573525915191007, -0.12147767747340438, 0.02301543214931511, 0.3223331745852752, -0.0721102117632444, 0.20892228803852328, -0.42024911993827957, -0.2509798926923675, -0.0188339670914082, 0.15535509392234068, 0.11739774122990919, -0.04535404387010763, -0.3102377036299843, 0.06592149642081215, -0.09366839953089276, -0.129749824956749, -0.10533431822505708, -0.09247210628773946, -0.04038571961259899, -0.2056577574140437, 0.14349012303864583, 0.033556794944720775, 0.1873752707078193, -0.1141537022715336, -0.053233786566684455, -0.060388507975193746, 0.023319678604961015, 0.023516527766612574, 0.12476059724716694, 0.16401917660662618, -0.1150971882587048, -0.14996204745078173, 0.32800464352924164, -0.06794610222837386, -0.03591167712091611, 0.16128609181704143, -0.2628196373474426, -0.09129009857917061, 0.23037088888052565, 0.04498617044793299, 0.06766079721721606, -0.1678416051676882, 0.07731804696735568, -0.03142742242646189, 0.17720302241062968, 0.08925522420591173, 0.06129185368683046, 0.2971244438085705, 0.18743719881884038, 0.027684599841729954, 0.10584478909619904, -0.1961716331022147, -0.02297793825318177, -0.2513478619691271, -0.13973412481853023, -0.21329778100614652, 0.09537785155085797, -0.03106538510361973, -0.20806886119624743, 0.40582744956862793, 0.15123121025792968, 0.2493236994912597, -0.1182317675100841, 0.2207385180077276, 0.10689647916968589, 0.10170026613363567, -0.005414962683481952, 0.22853070870489597, 0.11165353329180597, 0.12667397147407217, -0.25262028911730827, 0.11571587008186796, 0.024171796819875732]
|
707.0917
|
Toroidal embeddings and polyhedral divisors
|
Given an effective action of an (n-1)-dimensional torus on an n-dimensional
normal affine variety, Mumford constructs a toroidal embedding, while Altmann
and Hausen give a description in terms of a polyhedral divisor on a curve. We
compare the fan of the toroidal embedding with this polyhedral divisor.
|
math.AG
|
given an effective action of an n1dimensional torus on an ndimensional normal affine variety mumford constructs a toroidal embedding while altmann and hausen give a description in terms of a polyhedral divisor on a curve we compare the fan of the toroidal embedding with this polyhedral divisor
|
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|
[-0.17873470962760932, -0.007549497399521259, -0.10983304637781482, 0.020952250003477835, -0.14781880426280042, -0.0966035793040027, -0.014616024858774022, 0.3051350266533963, -0.27955051996012, -0.18840107706157452, 0.05776042634611355, -0.22325985188140196, -0.17520964958090732, 0.21418835593268593, -0.23592023139304302, -0.07403176384878919, 0.02146550363048594, 0.08601278978142332, -0.1091795723211575, -0.2922259312360845, 0.38719602309642953, -0.04477898206839219, 0.26903045916573165, 0.05565154893284149, 0.1589440952471279, 0.0287340560710018, 0.021065456971050577, 0.03599273324250541, -0.18126666141634293, 0.235108789864016, 0.2736233198975629, 0.11582439212485197, 0.13361121501099874, -0.4114672613746308, -0.17087069394418652, 0.15085172267789218, 0.12378446348605955, 0.006091852687259621, -0.024192866022163566, -0.21614815661327003, 0.016081634165838042, -0.14692729307298966, -0.21319580333743324, -0.08803024446155797, 0.09538911905218946, -0.03652323350592695, -0.23178544490935005, -0.13789337138618105, 0.1508106059256069, 0.2004134608828958, -0.0763294264634556, -0.09088579252203728, -0.04600341247513573, -0.011666010074475978, -0.04351382286466183, 0.16490752178620785, 0.0625188128169418, -0.13419464583746454, -0.13544618144155818, 0.38196182163788917, -0.07215571161755856, -0.3021876867662402, 0.10627832558957186, -0.07230981562207354, -0.07097798926716155, 0.18599771274293356, 0.14540210336526024, 0.18747565187910137, -0.017386347095065927, 0.2129064282152227, -0.17059144942941976, 0.042843562253612154, 0.09876286870542358, -0.08347505701586921, 0.1660235034688277, 0.1401300357179122, 0.07928732272356431, 0.1635512530090327, -0.032976442502137826, -0.05665228393751177, -0.3768781244834053, -0.19661902941446355, -0.11000911264303834, 0.20372022078075308, -0.21949858457175767, -0.2639750658257052, 0.42331731349150553, -0.08037347261338158, 0.25332637522320084, 0.09059540260065485, 0.2529654228722954, 0.032358363389651826, -0.034163132626959615, 0.09283386207522547, 0.10777067701193563, 0.17930563929629453, -0.08627325028399045, -0.17957345832218516, -0.03294444056425957, 0.2587992188897222]
|
707.0918
|
Improved VLBI astrometry of OH maser stars
|
Aims: Accurate distances to evolved stars with high mass loss rates are
needed for studies of many of their fundamental properties. However, as these
stars are heavily obscured and variable, optical and infrared astrometry is
unable to provide enough accuracy.
Methods: Astrometry using masers in the circumstellar envelopes can be used
to overcome this problem. We have observed the OH masers of a number of
Asymptotic Giant Branch (AGB) stars for approximately 1 year with the Very Long
Baseline Array (VLBA). We have used the technique of phase referencing with
in-beam calibrators to test the improvements this technique can provide to Very
Long Baseline Interferometry (VLBI) OH maser astrometric observations.
Results: We have significantly improved the parallax and proper motion
measurements of the Mira variable stars U Her, S CrB and RR Aql.
Conclusions: It is shown that both in-beam phase-referencing and a decrease
in solar activity during the observations significantly improves the accuracy
of the astrometric observations. The improved distances to S CrB (418 +21 -18
pc) and RR Aql (633 +214 -128 pc) are fully consistent with published P-L
relations, but the distance to U Her (266 +32 -28 pc) is significantly smaller.
We conclude that for sources that are bright and have a nearby in-beam
calibrator, VLBI OH maser astrometry can be used to determine distances to OH
masing stars of up to ~2 kpc.
|
astro-ph
|
aims accurate distances to evolved stars with high mass loss rates are needed for studies of many of their fundamental properties however as these stars are heavily obscured and variable optical and infrared astrometry is unable to provide enough accuracy methods astrometry using masers in the circumstellar envelopes can be used to overcome this problem we have observed the oh masers of a number of asymptotic giant branch agb stars for approximately 1 year with the very long baseline array vlba we have used the technique of phase referencing with inbeam calibrators to test the improvements this technique can provide to very long baseline interferometry vlbi oh maser astrometric observations results we have significantly improved the parallax and proper motion measurements of the mira variable stars u her s crb and rr aql conclusions it is shown that both inbeam phasereferencing and a decrease in solar activity during the observations significantly improves the accuracy of the astrometric observations the improved distances to s crb 418 21 18 pc and rr aql 633 214 128 pc are fully consistent with published pl relations but the distance to u her 266 32 28 pc is significantly smaller we conclude that for sources that are bright and have a nearby inbeam calibrator vlbi oh maser astrometry can be used to determine distances to oh masing stars of up to 2 kpc
|
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|
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|
707.0919
|
Effects of hadronic loops on the direct CP violation of $B_{c}$
|
It is well known that the final state interaction plays an important role in
the decays of $B$-meson. The contribution of the final state interaction which
is supposed to be long-distance effects, to the concerned processes can
interfere with that of the short-distance effects produced via the tree and/or
loop diagrams at quark-gluon level. The interference may provide a source for
the direct CP violation $\mathcal{A}_{CP}$ in the process $B_{c}^{+}\to
D^{0}\pi^{+}$. We find that a typical value of $\mathcal{A}_{CP}$ when the
final state interaction effect is taken into account can be about -22% which is
different from that without the final state interaction effect. Therefore, when
we extract information on CP violation from the data which will be available at
LHCb and the new experiments in $B$-factories, the contribution from the final
state interaction must be included. This study may be crucial for searching new
physics in the future.
|
hep-ph
|
it is well known that the final state interaction plays an important role in the decays of bmeson the contribution of the final state interaction which is supposed to be longdistance effects to the concerned processes can interfere with that of the shortdistance effects produced via the tree andor loop diagrams at quarkgluon level the interference may provide a source for the direct cp violation mathcala_cp in the process b_cto d0pi we find that a typical value of mathcala_cp when the final state interaction effect is taken into account can be about 22 which is different from that without the final state interaction effect therefore when we extract information on cp violation from the data which will be available at lhcb and the new experiments in bfactories the contribution from the final state interaction must be included this study may be crucial for searching new physics in the future
|
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|
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|
707.092
|
Spatial Topology and its Structural Analysis based on the Concept of
Simplicial Complex
|
This paper introduces a model that identifies spatial relationships for a
structural analysis based on the concept of simplicial complex. The spatial
relationships are identified through overlapping two map layers, namely a
primary layer and a contextual layer. The identified spatial relationships are
represented as a simplical complex, in which simplices and vertices
respectively represent two layers of objects. The model relies on the simplical
complex for structural representation and analysis. To quantify structural
properties of individual primary objects (or equivalently simplices), and the
simplicial complex as a whole, we define a set of centrality measures by
considering multidimensional chains of connectivity, i.e. the number of
contextual objects shared by a pair of primary objects. With the model, the
interaction and relationships with a geographic system are modeled from both
local and global perspectives. The structural properties and modeling
capabilities are illustrated with a simple example and a case study applied to
the structural analysis of an urban system.
|
physics.data-an physics.space-ph
|
this paper introduces a model that identifies spatial relationships for a structural analysis based on the concept of simplicial complex the spatial relationships are identified through overlapping two map layers namely a primary layer and a contextual layer the identified spatial relationships are represented as a simplical complex in which simplices and vertices respectively represent two layers of objects the model relies on the simplical complex for structural representation and analysis to quantify structural properties of individual primary objects or equivalently simplices and the simplicial complex as a whole we define a set of centrality measures by considering multidimensional chains of connectivity ie the number of contextual objects shared by a pair of primary objects with the model the interaction and relationships with a geographic system are modeled from both local and global perspectives the structural properties and modeling capabilities are illustrated with a simple example and a case study applied to the structural analysis of an urban system
|
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|
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|
707.0921
|
Astrophysics in Southern Africa
|
The government of South Africa has identified astronomy as a field in which
their country has a strategic advantage and is consequently investing very
significantly in astronomical infrastructure. South Africa now operates a 10-m
class optical telescope, the Southern African Large Telescope (SALT), and is
one of two countries short listed to host the Square Kilometre Array (SKA), an
ambitious international project to construct a radio telescope with a
sensitivity one hundred times that of any existing telescope. The challenge now
is to produce an indigenous community of users for these facilities,
particularly from among the black population which was severely disadvantaged
under the apartheid regime. In this paper I briefly describe the observing
facilities in Southern Africa before going on to discuss the various
collaborations that are allowing us to use astronomy as a tool for development,
and at the same time to train a new generation of astronomers who will be well
grounded in the science and linked to their colleagues internationally.
|
astro-ph
|
the government of south africa has identified astronomy as a field in which their country has a strategic advantage and is consequently investing very significantly in astronomical infrastructure south africa now operates a 10m class optical telescope the southern african large telescope salt and is one of two countries short listed to host the square kilometre array ska an ambitious international project to construct a radio telescope with a sensitivity one hundred times that of any existing telescope the challenge now is to produce an indigenous community of users for these facilities particularly from among the black population which was severely disadvantaged under the apartheid regime in this paper i briefly describe the observing facilities in southern africa before going on to discuss the various collaborations that are allowing us to use astronomy as a tool for development and at the same time to train a new generation of astronomers who will be well grounded in the science and linked to their colleagues internationally
|
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|
[-0.0728997669875531, 0.1300711216244963, -0.05159087776399513, 0.08396278974094723, -0.16763368366490594, -0.12165426731211837, 0.04317095388002444, 0.38027683698867515, -0.20495667621470626, -0.3369800470394605, 0.20296039254824835, -0.30373126563968184, -0.12586627450591328, 0.23370031856863602, -0.05262843439378208, -0.07709268958977901, 0.09028098041975371, -0.04631143012765523, 0.035423211398443614, -0.2991675418324587, 0.22001900207024158, 0.18967120037818747, 0.2877542390488088, 0.015421070677736523, 0.09721263769505441, -0.07169703807590938, -0.08485290589855939, -0.017013871676015962, -0.074899051154317, 0.11916267496204322, 0.3822187281827011, 0.1941171220827439, 0.35827095814548976, -0.40617359969083494, -0.1319522018453515, 0.09875397748461492, 0.10197523125680164, 0.05021430269059748, -0.0032836335161757634, -0.3313714744148367, -0.006877980552750026, -0.24287878845182315, -0.22676123884256658, 0.03954451912219023, 0.03230606153303553, 0.0375197223932823, -0.19778040330360144, -0.04768284590256105, -0.08101180534761558, 0.08975371368734802, -0.0331046506868982, -0.1371794716687873, 0.020349198172192613, 0.21114651258841793, 0.04165685361197286, 0.057384749979530345, 0.07503528278512687, -0.1585219847279737, -0.07960483791851779, 0.382603612364974, -0.045681242305762704, -0.02084306596278599, 0.18711471184662248, -0.2254669435702764, -0.1924531772255716, 0.07578805086299459, 0.22260369294005014, 0.06046517836157142, -0.20408253518796368, 0.07140332645319243, -0.024627539482558282, 0.17053407206620294, 0.09846408176945703, 0.027984827637626993, 0.30436860608141414, 0.1957887457435235, 0.12169600603818076, 0.11737953118409211, -0.17980815106775702, -0.07291747413848232, -0.20003007486087793, -0.12723896239753585, -0.140837154576907, 0.03405218550838848, 0.005326661670640134, -0.11653652226427434, 0.3833442521508692, 0.1350345722734701, 0.06382975949928528, 0.025486640879180192, 0.2883869061394163, -0.046721894000145814, 0.16258361467824703, 0.04157912015642335, 0.2687171607039778, 0.03176945742651275, 0.19709599543882467, -0.12296220348017835, 0.05314910627912912, -0.025772800646358875]
|
707.0922
|
B-type defects in Landau-Ginzburg models
|
We consider Landau-Ginzburg models with possibly different superpotentials
glued together along one-dimensional defect lines. Defects preserving B-type
supersymmetry can be represented by matrix factorisations of the difference of
the superpotentials. The composition of these defects and their action on
B-type boundary conditions is described in this framework. The cases of
Landau-Ginzburg models with superpotential W=X^d and W=X^d+Z^2 are analysed in
detail, and the results are compared to the CFT treatment of defects in N=2
superconformal minimal models to which these Landau-Ginzburg models flow in the
IR.
|
hep-th
|
we consider landauginzburg models with possibly different superpotentials glued together along onedimensional defect lines defects preserving btype supersymmetry can be represented by matrix factorisations of the difference of the superpotentials the composition of these defects and their action on btype boundary conditions is described in this framework the cases of landauginzburg models with superpotential wxd and wxdz2 are analysed in detail and the results are compared to the cft treatment of defects in n2 superconformal minimal models to which these landauginzburg models flow in the ir
|
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|
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|
707.0923
|
Quark-gluon plasma paradox
|
Based on simple physics arguments it is shown that the concept of quark-gluon
plasma, a state of matter consisting of uncorrelated quarks, antiquarks, and
gluons, has a fundamental problem.
|
hep-ph
|
based on simple physics arguments it is shown that the concept of quarkgluon plasma a state of matter consisting of uncorrelated quarks antiquarks and gluons has a fundamental problem
|
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|
[-0.05808700968366887, 0.3327435164166422, -0.23141557164490223, 0.08421003382155222, -0.06849233382220926, -0.12164148158425915, 0.026224250808872026, 0.30668072942002067, -0.16569654405887785, -0.20011046348974623, -0.04000450009158973, -0.28703892423674976, -0.04508623416567671, 0.11614089895939005, 0.02661142228492375, 0.08009466991342347, 0.08519278055634992, 0.03987234194987807, -0.011050780074458151, -0.22698419284203958, 0.3483972665050934, -0.045146985172197736, 0.28562609774285347, 0.1806220031536088, 0.1924658840971774, 0.02424382129362945, -0.034603795036673546, -0.019083144849744337, -0.03891741918226311, 0.03759599062373284, 0.15390502629352026, 0.09047590624059326, 0.24090496604812556, -0.41918770628499574, -0.2364850794928598, 0.0702402060530309, 0.12353034458797553, 0.07828686039509444, -0.054237010202306354, -0.23080115784601918, 0.037994128266542124, -0.2247279630010498, -0.15619873733998374, -0.0479479104095813, 0.02570104695342738, -0.06388355200660639, -0.2852325924383155, 0.06620797508492551, 0.043724168453301335, -0.02811760847167722, 0.044736206637904175, -0.16119138790487214, -0.020317920451534206, -0.0049388712304162564, 0.06760945346945062, 0.08209616024496741, 0.15669548941840386, -0.22993225173960471, -0.16167097024876495, 0.4556880140343906, -0.0026913982783925944, -0.20443495138195053, 0.24590606673556412, -0.08308787855865626, -0.11941397061635708, 0.09958258481969222, 0.18687472502090807, 0.11118662395867808, -0.22084994283344211, 0.12606970622035643, -0.16989451068742523, 0.19756471307884002, 0.06320774792854128, 0.07631156559840872, 0.31522836613244026, 0.2651996187351901, 0.0004065405529249331, 0.11684829292112384, 0.048817350432790556, -0.08946446990915413, -0.32802355957442314, -0.07930182726604157, -0.2205796945711662, 0.049946630373597145, -0.050514719882028596, -0.21491375687865316, 0.4229941774031212, 0.065986393469161, 0.1117702673414144, -0.09107898150024743, 0.3233121404873914, 0.08473114826684368, -0.036072772381634546, 0.12998874149895434, 0.26380032660632297, 0.2604890061092788, 0.13681161488759622, -0.2267975234426558, 0.003432924811053893, 0.1512391228100349]
|
707.0924
|
How to define the boundaries of a convective zone and how extended is
overshooting?
|
Under nonlocal convection theory, convection extends without limit therefore
no apparent boundary can be defined clearly as in the local theory. From the
requirement of a similar structure for both local and non-local models having
the same depth of convection zone, and taking into account the driving
mechanism of turbulent convection, we argue that a proper definition of the
boundary of a convective zone should be the place where the convective energy
flux (i.e. the correlation of turbulent velocity and temperature) changes its
sign. Therefore, it is convectively unstable region when the flux is positive,
and it is convective overshooting zone when the flux becomes negative. The
physical picture of the overshooting zone drawn by the usual non-local
mixing-length theory is not correct. In fact, convection is already
sub-adiabatic ($\nabla<\nabla_{ad}$) far before reaching the unstable boundary;
while in the overshooting zone below the convective zone, convection is
sub-adiabatic and super-radiative ($\nabla_{rad}<\nabla<\nabla_{ad}$). The
transition between the adiabatic temperature gradient and the radiative one is
continuous and smooth instead of a sudden switch. In the unstable zone the
temperature gradient is approaching radiative rather than going to adiabatic.
We would like to claim again that, the overshooting distance is different for
different physical quantities......
|
astro-ph
|
under nonlocal convection theory convection extends without limit therefore no apparent boundary can be defined clearly as in the local theory from the requirement of a similar structure for both local and nonlocal models having the same depth of convection zone and taking into account the driving mechanism of turbulent convection we argue that a proper definition of the boundary of a convective zone should be the place where the convective energy flux ie the correlation of turbulent velocity and temperature changes its sign therefore it is convectively unstable region when the flux is positive and it is convective overshooting zone when the flux becomes negative the physical picture of the overshooting zone drawn by the usual nonlocal mixinglength theory is not correct in fact convection is already subadiabatic nablanabla_ad far before reaching the unstable boundary while in the overshooting zone below the convective zone convection is subadiabatic and superradiative nabla_radnablanabla_ad the transition between the adiabatic temperature gradient and the radiative one is continuous and smooth instead of a sudden switch in the unstable zone the temperature gradient is approaching radiative rather than going to adiabatic we would like to claim again that the overshooting distance is different for different physical quantities
|
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|
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|
707.0925
|
The braid groups of the projective plane and the Fadell-Neuwirth short
exact sequence
|
We study the pure braid groups $P_n(RP^2)$ of the real projective plane
$RP^2$, and in particular the possible splitting of the Fadell-Neuwirth short
exact sequence $1 \to P_m(RP^2 {x_1,...,x_n} \to P_{n+m}(RP^2)
\stackrel{p_{\ast}}{\to} P_n(RP^2) \to 1$, where $n\geq 2$ and $m\geq 1$, and
$p_{\ast}$ is the homomorphism which corresponds geometrically to forgetting
the last $m$ strings. This problem is equivalent to that of the existence of a
section for the associated fibration $p: F_{n+m}(RP^2) \to F_n(RP^2)$ of
configuration spaces. Van Buskirk proved in 1966 that $p$ and $p_{\ast}$ admit
a section if $n=2$ and $m=1$. Our main result in this paper is to prove that
there is no section if $n\geq 3$. As a corollary, it follows that $n=2$ and
$m=1$ are the only values for which a section exists. As part of the proof, we
derive a presentation of $P_n(RP^2)$: this appears to be the first time that
such a presentation has been given in the literature.
|
math.GT math.GR
|
we study the pure braid groups p_nrp2 of the real projective plane rp2 and in particular the possible splitting of the fadellneuwirth short exact sequence 1 to p_mrp2 x_1x_n to p_nmrp2 stackrelp_astto p_nrp2 to 1 where ngeq 2 and mgeq 1 and p_ast is the homomorphism which corresponds geometrically to forgetting the last m strings this problem is equivalent to that of the existence of a section for the associated fibration p f_nmrp2 to f_nrp2 of configuration spaces van buskirk proved in 1966 that p and p_ast admit a section if n2 and m1 our main result in this paper is to prove that there is no section if ngeq 3 as a corollary it follows that n2 and m1 are the only values for which a section exists as part of the proof we derive a presentation of p_nrp2 this appears to be the first time that such a presentation has been given in the literature
|
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|
[-0.1511270915839396, 0.08673871329504272, -0.07250371566604848, 0.052085250844997696, -0.039177186040195246, -0.12711034623918518, -0.00798299177018488, 0.3444258588797494, -0.26670403153660566, -0.25688320847428187, 0.11720851162486029, -0.26667418711562485, -0.14458424457030108, 0.17357104146640573, -0.09120886940696596, -0.03443731813238005, 0.030581782659478234, 0.10463079660130828, -0.057677725192093784, -0.27969924457239975, 0.3544883276960944, -0.04806861035594554, 0.16813050392052573, 0.05808235061723714, 0.10662233787932551, 0.005998397505398365, 0.024969811035607685, -0.006628459644497641, -0.1739356441798033, 0.08896141685154789, 0.30210156014951683, 0.11256631811605704, 0.21450904010476282, -0.33723749462890146, -0.13375561093699012, 0.19602929748557257, 0.14840845110194895, 0.06889066437490585, -0.02340643447136269, -0.21170498060465684, 0.17999448259001685, -0.14846748244501776, -0.13455783510143124, 0.003240438619133979, 0.14663846903299324, -0.018206458251736588, -0.2655057919792981, 0.012343304100502658, 0.16407387473014176, 0.03059953201762182, -0.038193718184898265, -0.11156906471931494, -0.04160514473133789, 0.1214898581172796, 0.05325997728016853, 0.10689259448476236, 0.030234730464950104, -0.07487141680528704, -0.10714195664322017, 0.37916189015861723, -0.04024077935656845, -0.18786673733633286, 0.1393797380643453, -0.15640399913966105, -0.17053322323704226, 0.13367680034556445, 0.08512445508764944, 0.14881338173017256, -0.046606892791745444, 0.15024587072060136, -0.12644102415632483, 0.17130478162118454, 0.12409569173363731, -0.04848460921933312, 0.08771681626196076, 0.11681398164774698, 0.10456276541082, 0.12180757753772899, -0.036710454467074605, -0.02435765007742049, -0.3873264091526902, -0.2143388098916789, -0.1642498294908816, 0.14214316344876218, -0.03788421779027953, -0.14228008797973543, 0.33431287114852226, 0.07828126691638074, 0.21523566240282266, 0.08881384460621743, 0.24902286996280512, 0.09937753700791864, 0.019389661191493872, 0.05951507355363089, 0.18316103586139496, 0.16790288694252903, 0.03031936978558766, -0.1221591021073357, -0.008988067392109824, 0.12186644126929892]
|
707.0926
|
Theorem proving support in programming language semantics
|
We describe several views of the semantics of a simple programming language
as formal documents in the calculus of inductive constructions that can be
verified by the Coq proof system. Covered aspects are natural semantics,
denotational semantics, axiomatic semantics, and abstract interpretation.
Descriptions as recursive functions are also provided whenever suitable, thus
yielding a a verification condition generator and a static analyser that can be
run inside the theorem prover for use in reflective proofs. Extraction of an
interpreter from the denotational semantics is also described. All different
aspects are formally proved sound with respect to the natural semantics
specification.
|
cs.LO cs.PL
|
we describe several views of the semantics of a simple programming language as formal documents in the calculus of inductive constructions that can be verified by the coq proof system covered aspects are natural semantics denotational semantics axiomatic semantics and abstract interpretation descriptions as recursive functions are also provided whenever suitable thus yielding a a verification condition generator and a static analyser that can be run inside the theorem prover for use in reflective proofs extraction of an interpreter from the denotational semantics is also described all different aspects are formally proved sound with respect to the natural semantics specification
|
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|
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|
707.0927
|
Huge Transverse Magnetization in the Field-Induced Phase of the
Antiferromagnetic Molecular Wheel CsFe8
|
The 1H-NMR spectrum and nuclear relaxation rate 1/T_1 in the
antiferromagnetic wheel CsFe8 were measured to characterize the previously
observed magnetic field-induced low-temperature phase around the level crossing
at 8 T. The data show that the phase is characterized by a huge staggered
transverse polarization of the electronic Fe spins, and the opening of a gap,
providing microscopic evidence for the interpretation of the phase as a
field-induced magneto-elastic instability.
|
cond-mat.str-el
|
the 1hnmr spectrum and nuclear relaxation rate 1t_1 in the antiferromagnetic wheel csfe8 were measured to characterize the previously observed magnetic fieldinduced lowtemperature phase around the level crossing at 8 t the data show that the phase is characterized by a huge staggered transverse polarization of the electronic fe spins and the opening of a gap providing microscopic evidence for the interpretation of the phase as a fieldinduced magnetoelastic instability
|
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|
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|
707.0928
|
Tau tagging at Atlas and CMS
|
The tau identification and reconstruction algorithms developed for the LHC
experiments Atlas and CMS are presented. Reconstruction methods suitable for
use at High Level Trigger and off-line are described in detail
|
hep-ex
|
the tau identification and reconstruction algorithms developed for the lhc experiments atlas and cms are presented reconstruction methods suitable for use at high level trigger and offline are described in detail
|
[['the', 'tau', 'identification', 'and', 'reconstruction', 'algorithms', 'developed', 'for', 'the', 'lhc', 'experiments', 'atlas', 'and', 'cms', 'are', 'presented', 'reconstruction', 'methods', 'suitable', 'for', 'use', 'at', 'high', 'level', 'trigger', 'and', 'offline', 'are', 'described', 'in', 'detail']]
|
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|
707.0929
|
Phase Structure of Thermal QCD/QED:A Gauge Invariant Solution of the HTL
Resummed Improved Ladder Dyson-Schwinger Equation
|
Based on the hard-thermal-loop resummed improved ladder Dyson-Schwinger
quation for the fermion mass function, we propose a procedure how we can get
the gauge invariant solution in the sense it satisfies the Ward-Takahashi
identity. Results of the numerical analysis are shown and properties of the
``gauge-invariant'' solutions are discussed.
|
hep-ph
|
based on the hardthermalloop resummed improved ladder dysonschwinger quation for the fermion mass function we propose a procedure how we can get the gauge invariant solution in the sense it satisfies the wardtakahashi identity results of the numerical analysis are shown and properties of the gaugeinvariant solutions are discussed
|
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|
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|
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