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706.2314
|
Hypersurfaces in H^{n+1} and conformally invariant equations: the
generalized Christoffel and Nirenberg problems
|
Our first objective in this paper is to give a natural formulation of the
Christoffel problem for hypersurfaces in $H^{n+1}$, by means of the hyperbolic
Gauss map and the notion of hyperbolic curvature radii for hypersurfaces. Our
second objective is to provide an explicit equivalence of this Christoffel
problem with the famous problem of prescribing scalar curvature on $\S^n$ for
conformal metrics, posed by Nirenberg and Kazdan-Warner. This construction lets
us translate into the hyperbolic setting the known results for the scalar
curvature problem, and also provides a hypersurface theory interpretation of
such an intrinsic problem from conformal geometry. Our third objective is to
place the above result into a more general framework. Specifically, we will
show how the problem of prescribing the hyperbolic Gauss map and a given
function of the hyperbolic curvature radii in $H^{n+1}$ is strongly related to
some important problems on conformally invariant PDEs in terms of the Schouten
tensor. This provides a bridge between the theory of conformal metrics on
$\S^n$ and the theory of hypersurfaces with prescribed hyperbolic Gauss map in
$\H^{n+1}$. The fourth objective is to use the above correspondence to prove
that for a wide family of Weingarten functionals $W(\k_1,..., \k_n)$, the only
compact immersed hypersurfaces in $H^{n+1}$ on which $W$ is constant are round
spheres.
|
math.DG math.AP
|
our first objective in this paper is to give a natural formulation of the christoffel problem for hypersurfaces in hn1 by means of the hyperbolic gauss map and the notion of hyperbolic curvature radii for hypersurfaces our second objective is to provide an explicit equivalence of this christoffel problem with the famous problem of prescribing scalar curvature on sn for conformal metrics posed by nirenberg and kazdanwarner this construction lets us translate into the hyperbolic setting the known results for the scalar curvature problem and also provides a hypersurface theory interpretation of such an intrinsic problem from conformal geometry our third objective is to place the above result into a more general framework specifically we will show how the problem of prescribing the hyperbolic gauss map and a given function of the hyperbolic curvature radii in hn1 is strongly related to some important problems on conformally invariant pdes in terms of the schouten tensor this provides a bridge between the theory of conformal metrics on sn and the theory of hypersurfaces with prescribed hyperbolic gauss map in hn1 the fourth objective is to use the above correspondence to prove that for a wide family of weingarten functionals wk_1 k_n the only compact immersed hypersurfaces in hn1 on which w is constant are round spheres
|
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|
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|
706.2315
|
Spin Polarized Transport Through a Single-Molecule Magnet:
Current-Induced Magnetic Switching
|
Magnetic switching of a single-molecule magnet (SMM) due to spin-polarized
current is investigated theoretically. The charge transfer between the
electrodes takes place via the lowest unoccupied molecular orbital (LUMO) of
the SMM. Generally, the double occupancy of the LUMO level, and a finite
on-site Coulomb repulsion, is taken into account. Owing to the exchange
interaction between electrons in the LUMO level and the SMM's spin, the latter
can be reversed. The perturbation approach (Fermi golden rule) is applied to
calculate current-voltage characteristics. The influence of Coulomb
interactions on the switching process is also analyzed.
|
cond-mat.mes-hall
|
magnetic switching of a singlemolecule magnet smm due to spinpolarized current is investigated theoretically the charge transfer between the electrodes takes place via the lowest unoccupied molecular orbital lumo of the smm generally the double occupancy of the lumo level and a finite onsite coulomb repulsion is taken into account owing to the exchange interaction between electrons in the lumo level and the smms spin the latter can be reversed the perturbation approach fermi golden rule is applied to calculate currentvoltage characteristics the influence of coulomb interactions on the switching process is also analyzed
|
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|
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|
706.2316
|
Stable Border Bases for Ideals of Points
|
Let $X$ be a set of points whose coordinates are known with limited accuracy;
our aim is to give a characterization of the vanishing ideal $I(X)$ independent
of the data uncertainty. We present a method to compute a polynomial basis $B$
of $I(X)$ which exhibits structural stability, that is, if $\widetilde X$ is
any set of points differing only slightly from $X$, there exists a polynomial
set $\widetilde B$ structurally similar to $B$, which is a basis of the
perturbed ideal $ I(\widetilde X)$.
|
math.AC math.NA
|
let x be a set of points whose coordinates are known with limited accuracy our aim is to give a characterization of the vanishing ideal ix independent of the data uncertainty we present a method to compute a polynomial basis b of ix which exhibits structural stability that is if widetilde x is any set of points differing only slightly from x there exists a polynomial set widetilde b structurally similar to b which is a basis of the perturbed ideal iwidetilde x
|
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|
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|
706.2317
|
Study of Di-Pion Transitions Among Upsilon(3S), Upsilon(2S), and
Upsilon(1S) States
|
We present measurements of decay matrix elements for hadronic transitions of
the form Upsilon(nS) -> pi pi Upsilon(mS) where (n, m) = (3, 1), (2, 1), and
(3, 2). We reconstruct charged and neutral pion modes with the final state
Upsilon decaying to either mu+mu- or e+e-. Dalitz plot distributions for the
twelve decay modes are fit individually as well as jointly assuming isospin
symmetry, thereby measuring the matrix elements of the decay amplitude. We
observe and account for the anomaly previously noted in the di-pion invariant
mass distribution for the Upsilon(3S) -> pi pi Upsilon(1S) transition and
obtain good descriptions of the dynamics of the decay using the most general
decay amplitude allowed by partial conservation of the axial-vector current
(PCAC) considerations. The fits further indicate that the Upsilon(2S) -> pi pi
Upsilon(1S) and Upsilon(3S) -> pi pi Upsilon(2S) transitions also show the
presence of terms in the decay amplitude that were previously ignored, although
at a relatively suppressed level.
|
hep-ex
|
we present measurements of decay matrix elements for hadronic transitions of the form upsilonns pi pi upsilonms where n m 3 1 2 1 and 3 2 we reconstruct charged and neutral pion modes with the final state upsilon decaying to either mumu or ee dalitz plot distributions for the twelve decay modes are fit individually as well as jointly assuming isospin symmetry thereby measuring the matrix elements of the decay amplitude we observe and account for the anomaly previously noted in the dipion invariant mass distribution for the upsilon3s pi pi upsilon1s transition and obtain good descriptions of the dynamics of the decay using the most general decay amplitude allowed by partial conservation of the axialvector current pcac considerations the fits further indicate that the upsilon2s pi pi upsilon1s and upsilon3s pi pi upsilon2s transitions also show the presence of terms in the decay amplitude that were previously ignored although at a relatively suppressed level
|
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|
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|
706.2318
|
The Geometry of Regular Shear-Free Null Geodesic Congruences, CR
functions and their Application to the Flat-Space Maxwell Equations
|
We describe here what appears to be a new structure that is hidden in all
asymptotically vanishing Maxwell fields possessing a non-vanishing total
charge. Though we are dealing with real Maxwell fields on real Minkowski space
nevertheless, directly from the asymptotic field one can extract a complex
analytic world-line defined in complex Minkowski space that gives a unified
Lorentz invariant meaning to both the electric and magnetic dipole moments. In
some sense the world-line defines a `complex center of charge' around which
both electric and magnetic dipole moments vanish.
The question of how and where does this complex world-line arise is one of
the two main subjects of this work. The other subject concerns what is known in
the mathematical literature as a CR structure. In GR, CR structures naturally
appear in the physical context of shear-free (or asymptotically shear-free)
null geodesic congruences in space-time. For us, the CR structure is associated
with the embedding of Penrose's real three-dimensional null infinity, I^+, as a
surface in a two complex dimensional space, C^2. It is this embedding, via a
complex function, (a CR function), that is our other area of interest.
Specifically we are interested in the `decomposition' of the CR function into
its real and imaginary parts and the physical information contained in this
decomposition.
|
gr-qc
|
we describe here what appears to be a new structure that is hidden in all asymptotically vanishing maxwell fields possessing a nonvanishing total charge though we are dealing with real maxwell fields on real minkowski space nevertheless directly from the asymptotic field one can extract a complex analytic worldline defined in complex minkowski space that gives a unified lorentz invariant meaning to both the electric and magnetic dipole moments in some sense the worldline defines a complex center of charge around which both electric and magnetic dipole moments vanish the question of how and where does this complex worldline arise is one of the two main subjects of this work the other subject concerns what is known in the mathematical literature as a cr structure in gr cr structures naturally appear in the physical context of shearfree or asymptotically shearfree null geodesic congruences in spacetime for us the cr structure is associated with the embedding of penroses real threedimensional null infinity i as a surface in a two complex dimensional space c2 it is this embedding via a complex function a cr function that is our other area of interest specifically we are interested in the decomposition of the cr function into its real and imaginary parts and the physical information contained in this decomposition
|
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|
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|
706.2319
|
Analysing the elasticity difference tensor of general relativity
|
The elasticity difference tensor, used in [1] to describe elasticity
properties of a continuous medium filling a space-time, is here analysed from
the point of view of the space-time connection. Principal directions associated
with this tensor are compared with eigendirections of the material metric.
Examples concerning spherically symmetric and axially symmetric space-times are
then presented.
|
gr-qc
|
the elasticity difference tensor used in 1 to describe elasticity properties of a continuous medium filling a spacetime is here analysed from the point of view of the spacetime connection principal directions associated with this tensor are compared with eigendirections of the material metric examples concerning spherically symmetric and axially symmetric spacetimes are then presented
|
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|
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|
706.232
|
On large automorphism groups of algebraic curves in positive
characteristic
|
In his investigation on large $K$-automorphism groups of an algebraic curve,
Stichtenoth obtained an upper bound on the order of the first ramification
group of an algebraic curve $\cX$ defined over an algebraically closed field of
characteristic $p$. Stichtenoth's bound has raised the problem of classifying
all $\K$-automorphism groups $G$ of $\cX$ with the following property: There is
a point $P\in \cX$ for which \begin{equation} |G_P^{(1)}|>\frac{p}{p-1}g.
\end{equation} Such a classification is obtained here by proving Theorem 1.3
|
math.AG
|
in his investigation on large kautomorphism groups of an algebraic curve stichtenoth obtained an upper bound on the order of the first ramification group of an algebraic curve cx defined over an algebraically closed field of characteristic p stichtenoths bound has raised the problem of classifying all kautomorphism groups g of cx with the following property there is a point pin cx for which beginequation g_p1fracpp1g endequation such a classification is obtained here by proving theorem 13
|
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|
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|
706.2321
|
Lower bounds for moments of zeta prime rho
|
Assuming the Riemann Hypothesis, we establish lower bounds for moments of the
derivative of the Riemann zeta-function averaged over the non-trivial zeros of
$\zeta(s)$. Our proof is based upon a recent method of Rudnick and
Soundararajan that provides analogous bounds for moments of $L$-functions at
the central point, averaged over families.
|
math.NT
|
assuming the riemann hypothesis we establish lower bounds for moments of the derivative of the riemann zetafunction averaged over the nontrivial zeros of zetas our proof is based upon a recent method of rudnick and soundararajan that provides analogous bounds for moments of lfunctions at the central point averaged over families
|
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|
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|
706.2322
|
Materials with a desired refraction coefficient can be made by embedding
small particles
|
A method is proposed to create materials with a desired refraction
coefficient, possibly negative one. The method consists of embedding into a
given material small particles. Given $n_0(x)$, the refraction coefficient of
the original material in a bounded domain $D \subset \R^3$, and a desired
refraction coefficient $n(x)$, one calculates the number $N(x)$ of small
particles, to be embedded in $D$ around a point $x \in D$ per unit volume of
$D$, in order that the resulting new material has refraction coefficient
$n(x)$.
|
math-ph math.MP
|
a method is proposed to create materials with a desired refraction coefficient possibly negative one the method consists of embedding into a given material small particles given n_0x the refraction coefficient of the original material in a bounded domain d subset r3 and a desired refraction coefficient nx one calculates the number nx of small particles to be embedded in d around a point x in d per unit volume of d in order that the resulting new material has refraction coefficient nx
|
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|
[-0.1734864247917402, 0.14127407608008602, -0.046380462959726775, -0.07703126691389693, -0.07140927019858415, -0.1779297108125941, 0.031028012018196466, 0.3422119561582804, -0.29709174109213965, -0.28124051476351736, 0.035201137720766225, -0.34747627295735406, -0.12322261734161435, 0.13077478791677916, -0.04549385840073228, 0.04258873429512832, -0.018897625958410706, 0.06603891096963752, -0.01185021327706281, -0.22608317816544823, 0.26050178020931325, -0.039432282582288834, 0.18207159671341863, 0.05855132830215663, 0.1611893131687283, -0.009327081374599734, 0.003949299272967548, 0.061070402629855206, -0.11308985885465872, 0.11060826004505521, 0.20065682912358968, 0.022591345330200543, 0.275722855954749, -0.33054061611069413, -0.25292449079953677, 0.09453448968962198, 0.10702841237141955, 0.021944928857520585, -0.08888258356970122, -0.2195854858302216, 0.10869952995420956, -0.10824931954692413, -0.20145957843150672, 0.010380365227053805, 0.10610518595998789, -0.030490992951388584, -0.32923579502214745, 0.04046505091643733, 0.053740107477074715, -0.021292612372568194, -0.04807799390131017, -0.14876792487892798, -0.04470015620449331, 0.08342236698400683, 0.010662585034080577, 0.07568086040342545, 0.1058780790772289, -0.09977103693683337, -0.006233601112531998, 0.4294116014569271, -0.08251887058595014, -0.2591035341185222, 0.09321606863380932, -0.22155526568885983, -0.030389686376310704, 0.24534208793193102, 0.23917809982284358, 0.14051639169409144, -0.06905595792412031, 0.08914235067232966, -0.07406017688250668, 0.20977443259205136, 0.11144599256037575, -0.009379837028795808, 0.18729575777926097, 0.15036868263623768, 0.055554888336124215, 0.14519991891858985, -0.08304606014103118, 0.02440339994684952, -0.31314029185691983, -0.2378061959497267, -0.2641943005856308, 0.05142114286469977, -0.19156534204855077, -0.196869463881296, 0.3747808122780265, 0.04981390301353957, 0.24807962255052676, -0.03202345642039734, 0.2561892398701208, 0.11075712014671142, 0.04391193872235329, 0.06252539089153998, 0.14525449441791308, 0.11111709484603347, 0.11298561219421284, -0.1605596698014202, 0.0963973829937281, 0.10921479817305936]
|
706.2323
|
A sample of mJy radio sources at 1.4 GHz in the Lynx and Hercules fields
- I. Radio imaging, multicolour photometry and spectroscopy
|
With the goal of identifying high redshift radio galaxies with FRI
classification, here are presented high resolution, wide-field radio
observations, near infra-red and optical imaging and multi-object spectroscopy
of two fields of the Leiden-Berkeley Deep Survey. These fields, Hercules.1 and
Lynx.2, contain a complete sample of 81 radio sources with S(1.4 GHz) > 0.5 mJy
within 0.6 square degrees. This sample will form the basis for a study of the
population and cosmic evolution of high redshift, low power, FRI radio sources
which will be presented in Paper II. Currently, the host galaxy identification
fraction is 86% with 11 sources remaining unidentified at a level of r > 25.2
mag (Hercules; 4 sources) or r > 24.4 mag (Lynx; 7 sources) or K > 20 mag.
Spectroscopic redshifts have been determined for 49% of the sample and
photometric redshift estimates are presented for the remainder of the sample.
|
astro-ph
|
with the goal of identifying high redshift radio galaxies with fri classification here are presented high resolution widefield radio observations near infrared and optical imaging and multiobject spectroscopy of two fields of the leidenberkeley deep survey these fields hercules1 and lynx2 contain a complete sample of 81 radio sources with s14 ghz 05 mjy within 06 square degrees this sample will form the basis for a study of the population and cosmic evolution of high redshift low power fri radio sources which will be presented in paper ii currently the host galaxy identification fraction is 86 with 11 sources remaining unidentified at a level of r 252 mag hercules 4 sources or r 244 mag lynx 7 sources or k 20 mag spectroscopic redshifts have been determined for 49 of the sample and photometric redshift estimates are presented for the remainder of the sample
|
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|
[-0.07574964547860073, 0.09863844027178005, -0.022002849883089464, 0.03527565888981236, -0.08490352873716847, -0.08042195188013691, 0.08213419910497197, 0.4552465042640977, -0.11352021090937316, -0.401306413649086, 0.13151142755385029, -0.3441952800787721, 0.018224447024391688, 0.18783433604258912, 0.004487042019724952, -0.026062592588272607, 0.03971679909121747, -0.12723916852087153, -0.011287260906798071, -0.30123881816018555, 0.21376122990689167, 0.1016416708253083, 0.23323552472540013, -0.07372838956739833, 0.11344869423687379, -0.07945833773251477, -0.1622345076530432, -0.021925366906356727, -0.1259792229451292, 0.04072572210810233, 0.31685764485217155, 0.1129662803909246, 0.2468825136468224, -0.24321695828561815, -0.16434532618447345, 0.0735766019388135, 0.19074001460392292, 0.01761880383912659, -0.0429962228204236, -0.2737429260857509, 0.14039262120920756, -0.16602651008688812, -0.1890409915305093, 0.08401997563105526, 0.03721554164860583, 0.07279808210466612, -0.18073353013816348, 0.17551809760695652, -0.04325974457699092, 0.1877144633012936, -0.1351522167100974, -0.15704658752677184, -0.006744306755800408, 0.05843105310481702, -0.09147596341584222, 0.13231954852664837, 0.11799265551942249, -0.1845155671413935, -0.05598134025584589, 0.36417390975658614, -0.01975193069686334, 0.034153080838674625, 0.21530687807669455, -0.2416689799708836, -0.21587019509483948, 0.18391805245286738, 0.19076024029727576, 0.08876939301530942, -0.20716000057043546, 0.02343165620658646, 0.04626276348684485, 0.24551649930629324, 0.032448335215515385, 0.1457051762780348, 0.2700844765871975, 0.10085861701749477, 0.04591575537887501, 0.06361693465761867, -0.32933088859662096, 0.0986044666885088, -0.2829143649548398, -0.07089934263920002, -0.1525849242965486, 0.15396238867431244, -0.1496772346187322, -0.09864510615407457, 0.3720283986098985, 0.08755532428308502, 0.1595385118737711, 0.09785088977086233, 0.2598479142468687, 0.05548251009668415, 0.10108853224004415, 0.10625681727265952, 0.3248121228154934, 0.16091458151671797, 0.06547837575537595, -0.11536316699447467, -0.05389660659596218, -0.05306035147629784]
|
706.2324
|
Special isogenies and tensor product multiplicities
|
We show that any bijection between two root systems that preserves angles
(but not necessarily lengths) gives rise to inequalities relating tensor
product multiplicities for the corresponding complex semisimple Lie groups (or
Lie algebras). We explain the inequalities in two ways: combinatorially, using
Littelmann's Path Model, and geometrically, using isogenies between algebaric
groups defined over an algebraically closed field of positive characteristic.
|
math.RT math.AG
|
we show that any bijection between two root systems that preserves angles but not necessarily lengths gives rise to inequalities relating tensor product multiplicities for the corresponding complex semisimple lie groups or lie algebras we explain the inequalities in two ways combinatorially using littelmanns path model and geometrically using isogenies between algebaric groups defined over an algebraically closed field of positive characteristic
|
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|
[-0.2189877037402062, 0.1377869821906995, -0.09981951589185384, 0.09252631886591835, -0.12155083785464446, -0.1930771021608023, -0.049391160592354176, 0.4140980819901151, -0.3587969118248551, -0.23588449378768284, 0.02639595906422924, -0.2228676634465134, -0.1758918817072446, 0.25840469972688646, -0.09466201896148344, -0.12784865705837165, 0.031730938785439054, 0.10289737258121491, -0.14367458624615065, -0.26986795761472276, 0.40824849823970466, -0.10605779877908889, 0.21383625679018517, 0.040951496591010404, 0.14602082306068512, 0.02572825875493788, 0.0013095933132834972, 0.05239931343033189, -0.16100025242462102, 0.12435626537509022, 0.31959513354776126, 0.08019036888107357, 0.1339626480269456, -0.3897288454275939, -0.056038799079795996, 0.2597657579481752, 0.19380383352719008, -0.0033905943329896656, 0.003337801300785354, -0.23345496274170377, 0.04337821798699518, -0.1803906862774203, -0.14654152775784174, -0.08326843567192554, 0.0484705796547895, -0.013875657932892922, -0.21924977422872138, 0.05359253022188862, 0.07678624597423139, 0.17590937202030252, -0.09210351143678229, -0.1091841833981415, -0.009693787643505682, 0.10906048468689644, -0.012059498640273007, -0.019366108461268124, 0.07327835314396408, -0.03858087229872904, -0.20492292393840128, 0.32484031246314127, 0.019657408170807626, -0.2688247506626912, 0.16918506842827605, -0.17103383245111833, -0.11494340391589268, 0.1517096877759022, 0.0769728013734904, 0.11241565443455212, -0.0638734307623611, 0.12937439638546727, -0.1257177727867759, 0.05004264752290422, 0.11671488475234758, -0.010677584206625339, 0.17264022563563963, -0.025950994808226824, 0.08228402019989106, 0.10561594238594896, 0.0788973176010674, -0.07525612703043848, -0.36639411639302005, -0.1831216507501179, -0.09993342344739264, 0.1314087165859922, -0.15208727505875774, -0.18221191840336448, 0.37845315585934347, 0.05894989177824989, 0.21743716185465606, 0.18355305789678353, 0.17276444398016938, 0.05199130980538264, 0.14620400676006196, 0.07209965440955374, 0.09065905691409905, 0.30238717951391253, -0.0642688428596293, -0.1258922164448567, 0.007173753441161205, 0.2113147343493878]
|
706.2325
|
The Monitor project: JW 380 -- a 0.26, 0.15 Msol pre main sequence
eclipsing binary in the Orion Nebula Cluster
|
We report the discovery of a low-mass (0.26 +/- 0.02, 0.15 +/- 0.01 Msol)
pre-main-sequence eclipsing binary with a 5.3 day orbital period. JW 380 was
detected as part of a high-cadence time-resolved photometric survey (the
Monitor project) using the 2.5m Isaac Newton Telescope and Wide Field Camera
for a survey of a single field in the Orion Nebula Cluster (ONC) region in V
and i bands. The star is assigned a 99 per cent membership probability from
proper motion measurements, and radial velocity observations indicate a
systemic velocity within 1 sigma of that of the ONC. Modelling of the combined
light and radial velocity curves of the system gave stellar radii of 1.19 +0.04
-0.18 Rsol and 0.90 +0.17 -0.03 Rsol for the primary and secondary, with a
significant third light contribution which is also visible as a third peak in
the cross-correlation functions used to derive radial velocities. The masses
and radii appear to be consistent with stellar models for 2-3 Myr age from
several authors, within the present observational errors. These observations
probe an important region of mass-radius parameter space, where there are
currently only a handful of known pre-main-sequence eclipsing binary systems
with precise measurements available in the literature.
|
astro-ph
|
we report the discovery of a lowmass 026 002 015 001 msol premainsequence eclipsing binary with a 53 day orbital period jw 380 was detected as part of a highcadence timeresolved photometric survey the monitor project using the 25m isaac newton telescope and wide field camera for a survey of a single field in the orion nebula cluster onc region in v and i bands the star is assigned a 99 per cent membership probability from proper motion measurements and radial velocity observations indicate a systemic velocity within 1 sigma of that of the onc modelling of the combined light and radial velocity curves of the system gave stellar radii of 119 004 018 rsol and 090 017 003 rsol for the primary and secondary with a significant third light contribution which is also visible as a third peak in the crosscorrelation functions used to derive radial velocities the masses and radii appear to be consistent with stellar models for 23 myr age from several authors within the present observational errors these observations probe an important region of massradius parameter space where there are currently only a handful of known premainsequence eclipsing binary systems with precise measurements available in the literature
|
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|
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|
706.2326
|
The Cosmic Horseshoe: Discovery of an Einstein Ring around a Giant
Luminous Red Galaxy
|
We report the discovery of an almost complete Einstein ring of diameter 10"
in Sloan Digital Sky Survey (SDSS) Data Release 5 (DR5). Spectroscopic data
from the 6m telescope of the Special Astrophysical Observatory reveals that the
deflecting galaxy has a line-of-sight velocity dispersion in excess of 400 km/s
and a redshift of 0.444, whilst the source is a star-forming galaxy with a
redshift of 2.379. From its color and luminosity, we conclude that the lens is
an exceptionally massive Luminous Red Galaxy (LRG) with a mass within the
Einstein radius of 5 x 10^12 solar masses. This remarkable system provides a
laboratory for probing the dark matter distribution in LRGs at distances out to
3 effective radii, and studying the properties of high redshift star-forming
galaxies.
|
astro-ph
|
we report the discovery of an almost complete einstein ring of diameter 10 in sloan digital sky survey sdss data release 5 dr5 spectroscopic data from the 6m telescope of the special astrophysical observatory reveals that the deflecting galaxy has a lineofsight velocity dispersion in excess of 400 kms and a redshift of 0444 whilst the source is a starforming galaxy with a redshift of 2379 from its color and luminosity we conclude that the lens is an exceptionally massive luminous red galaxy lrg with a mass within the einstein radius of 5 x 1012 solar masses this remarkable system provides a laboratory for probing the dark matter distribution in lrgs at distances out to 3 effective radii and studying the properties of high redshift starforming galaxies
|
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|
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|
706.2327
|
A Robust Atom-Photon Entanglement Source for Quantum Repeaters
|
We demonstrate a novel way to efficiently and very robust create an
entanglement between an atomic and a photonic qubit. A single laser beam is
used to excite one atomic ensemble and two different spatial modes of scattered
Raman fields are collected to generate the atom-photon entanglement. With the
help of build-in quantum memory, the entanglement still exists after 20.5
$\mu$s storage time which is further proved by the violation of CHSH type
Bell's inequality. Our entanglement procedure is the building block for a novel
robust quantum repeater architecture [Zhao et al, Phys. Rev. Lett. 98, 240502
(2007)]. Our approach can be easily extended to generate high dimensional
atom-photon entanglements.
|
quant-ph
|
we demonstrate a novel way to efficiently and very robust create an entanglement between an atomic and a photonic qubit a single laser beam is used to excite one atomic ensemble and two different spatial modes of scattered raman fields are collected to generate the atomphoton entanglement with the help of buildin quantum memory the entanglement still exists after 205 mus storage time which is further proved by the violation of chsh type bells inequality our entanglement procedure is the building block for a novel robust quantum repeater architecture zhao et al phys rev lett 98 240502 2007 our approach can be easily extended to generate high dimensional atomphoton entanglements
|
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|
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|
706.2328
|
Unique mechanisms from finite two-state trajectories
|
Single molecule data made of on and off events are ubiquitous. Famous
examples include enzyme turnover, probed via fluorescence, and opening and
closing of ion-channel, probed via the flux of ions. The data reflects the
dynamics in the underlying multi-substate on-off kinetic scheme (KS) of the
process, but the determination of the underlying KS is difficult, and sometimes
even impossible, due to the loss of information in the mapping of the
mutli-dimensional KS onto two dimensions. A way to deal with this problem
considers canonical (unique) forms. (Unique canonical form is constructed from
an infinitely long trajectory, but many KSs.) Here we introduce canonical forms
of reduced dimensions that can handle any KS (i.e. also KSs with symmetry and
irreversible transitions). We give the mapping of KSs into reduced dimensions
forms, which is based on topology of KSs, and the tools for extracting the
reduced dimensions form from finite data. The canonical forms of reduced
dimensions constitute a powerful tool in discriminating between KSs.
|
q-bio.QM cond-mat.other q-bio.OT
|
single molecule data made of on and off events are ubiquitous famous examples include enzyme turnover probed via fluorescence and opening and closing of ionchannel probed via the flux of ions the data reflects the dynamics in the underlying multisubstate onoff kinetic scheme ks of the process but the determination of the underlying ks is difficult and sometimes even impossible due to the loss of information in the mapping of the mutlidimensional ks onto two dimensions a way to deal with this problem considers canonical unique forms unique canonical form is constructed from an infinitely long trajectory but many kss here we introduce canonical forms of reduced dimensions that can handle any ks ie also kss with symmetry and irreversible transitions we give the mapping of kss into reduced dimensions forms which is based on topology of kss and the tools for extracting the reduced dimensions form from finite data the canonical forms of reduced dimensions constitute a powerful tool in discriminating between kss
|
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|
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|
706.2329
|
Numerical Kaehler-Ricci soliton on the second del Pezzo
|
The second del Pezzo surface is known by work of Tian-Zhu and Wang-Zhu to
admit a unique Kaehler-Ricci soliton. Applying a method described in
hep-th/0703057, we use Ricci flow to numerically compute that soliton metric.
We numerically compute the value of its Perelman entropy (or Gaussian density).
|
math.DG gr-qc hep-th
|
the second del pezzo surface is known by work of tianzhu and wangzhu to admit a unique kaehlerricci soliton applying a method described in hepth0703057 we use ricci flow to numerically compute that soliton metric we numerically compute the value of its perelman entropy or gaussian density
|
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|
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|
706.233
|
Three body resonances in two meson-one baryon systems
|
We report four $\Sigma$'s and three $\Lambda$'s, in the 1500 - 1800 MeV
region, as two meson - one baryon S-wave $(1/2)^+$ resonances. We solve Faddeev
equations in the coupled channel approach. The invariant mass of one of the
meson-baryon pairs and that of the three particles have been varied and peaks
in the squared three body $T$-matrix have been found very close to the existing
$S$ = -1, $J^P= 1/2^+$ low lying baryon resonances. The input two-body
$t$-matrices for meson-meson and meson-baryon interaction have been calculated
by solving the Bethe-Salpeter equation with the potentials obtained in the
chiral unitary approach.
|
nucl-th
|
we report four sigmas and three lambdas in the 1500 1800 mev region as two meson one baryon swave 12 resonances we solve faddeev equations in the coupled channel approach the invariant mass of one of the mesonbaryon pairs and that of the three particles have been varied and peaks in the squared three body tmatrix have been found very close to the existing s 1 jp 12 low lying baryon resonances the input twobody tmatrices for mesonmeson and mesonbaryon interaction have been calculated by solving the bethesalpeter equation with the potentials obtained in the chiral unitary approach
|
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|
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|
706.2331
|
Pricing American Options for Jump Diffusions by Iterating Optimal
Stopping Problems for Diffusions
|
We approximate the price of the American put for jump diffusions by a
sequence of functions, which are computed iteratively. This sequence converges
to the price function uniformly and exponentially fast. Each element of the
approximating sequence solves an optimal stopping problem for geometric
Brownian motion, and can be numerically computed using the classical finite
difference methods. We prove the convergence of this numerical scheme and
present examples to illustrate its performance.
|
cs.CE
|
we approximate the price of the american put for jump diffusions by a sequence of functions which are computed iteratively this sequence converges to the price function uniformly and exponentially fast each element of the approximating sequence solves an optimal stopping problem for geometric brownian motion and can be numerically computed using the classical finite difference methods we prove the convergence of this numerical scheme and present examples to illustrate its performance
|
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|
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|
706.2332
|
Predictions from non trivial Quark-Lepton complementarity
|
The complementarity between the quark and lepton mixing matrices is shown to
provide robust predictions. We obtain these predictions by first showing that
the matrix V_M, product of the quark (CKM) and lepton (PMNS) mixing matrices,
may have a zero (1,3) entry which is favored by experimental data.
We obtain that any theoretical model with a vanishing (1,3) entry of V_M that
is in agreement with quark data, solar, and atmospheric mixing angle leads to
$\theta_{13}^{PMNS}=(9{^{+1}_{-2}})^\circ$. This value is consistent with the
present 90% CL experimental upper limit. We also investigate the prediction on
the lepton phases. We show that the actual evidence, under the only assumption
that the correlation matrix V_M product of CKM and PMNS has a zero in the entry
(1,3), gives us a prediction for the three CP-violating invariants J, S_1, and
S_2. A better determination of the lepton mixing angles will give stronger
prediction for the CP-violating invariants in the lepton sector. These will be
tested in the next generation experiments. Finally we compute the effect of non
diagonal neutrino mass in "l_i -> l_j gamma" in SUSY theories with non trivial
Quark-Lepton complementarity and a flavor symmetry. The Quark-Lepton
complementarity and the flavor symmetry strongly constrain the theory and we
obtain a clear prediction for the contribution to "mu -> e gamma" and the "tau"
decays "tau -> e gamma" and "tau -> mu gamma". If the Dirac neutrino Yukawa
couplings are degenerate but the low energy neutrino masses are not degenerate,
then the lepton decays are related among them by the V_M entries. On the other
hand, if the Dirac neutrino Yukawa couplings are hierarchical or the low energy
neutrino masses are degenerate, then the prediction for the lepton decays comes
from the CKM hierarchy.
|
hep-ph
|
the complementarity between the quark and lepton mixing matrices is shown to provide robust predictions we obtain these predictions by first showing that the matrix v_m product of the quark ckm and lepton pmns mixing matrices may have a zero 13 entry which is favored by experimental data we obtain that any theoretical model with a vanishing 13 entry of v_m that is in agreement with quark data solar and atmospheric mixing angle leads to theta_13pmns91_2circ this value is consistent with the present 90 cl experimental upper limit we also investigate the prediction on the lepton phases we show that the actual evidence under the only assumption that the correlation matrix v_m product of ckm and pmns has a zero in the entry 13 gives us a prediction for the three cpviolating invariants j s_1 and s_2 a better determination of the lepton mixing angles will give stronger prediction for the cpviolating invariants in the lepton sector these will be tested in the next generation experiments finally we compute the effect of non diagonal neutrino mass in l_i l_j gamma in susy theories with non trivial quarklepton complementarity and a flavor symmetry the quarklepton complementarity and the flavor symmetry strongly constrain the theory and we obtain a clear prediction for the contribution to mu e gamma and the tau decays tau e gamma and tau mu gamma if the dirac neutrino yukawa couplings are degenerate but the low energy neutrino masses are not degenerate then the lepton decays are related among them by the v_m entries on the other hand if the dirac neutrino yukawa couplings are hierarchical or the low energy neutrino masses are degenerate then the prediction for the lepton decays comes from the ckm hierarchy
|
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|
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|
706.2333
|
Loschmidt echo and stochastic-like quantum dynamics of nano-particles
|
We investigate time evolution of prepared vibrational state (system) coupled
to a reservoir with dense spectrum of its vibrational states. We assume that
the reservoir has an equidistant spectrum, and the system - reservoir coupling
matrix elements are independent of the reservoir states. The analytical
solution manifests three regimes of the evolution for the system: (I) weakly
damped oscillations; (II) multicomponent Loschmidt echo in recurrence cycles;
(III) overlapping recurrence cycles. We find the characteristic critical values
of the system - reservoir coupling constant for the transitions between these
regimes. Stochastic dynamics occurs in the regime (III) due to inevoidably in
any real system coarse graining of time or energy measurements, or initial
condition uncertainty. Even though a specific toy model is investigated here,
when properly interpreted it yields quite reasonable description for a variety
of physically relevant phenomena.
|
cond-mat.stat-mech cond-mat.mes-hall
|
we investigate time evolution of prepared vibrational state system coupled to a reservoir with dense spectrum of its vibrational states we assume that the reservoir has an equidistant spectrum and the system reservoir coupling matrix elements are independent of the reservoir states the analytical solution manifests three regimes of the evolution for the system i weakly damped oscillations ii multicomponent loschmidt echo in recurrence cycles iii overlapping recurrence cycles we find the characteristic critical values of the system reservoir coupling constant for the transitions between these regimes stochastic dynamics occurs in the regime iii due to inevoidably in any real system coarse graining of time or energy measurements or initial condition uncertainty even though a specific toy model is investigated here when properly interpreted it yields quite reasonable description for a variety of physically relevant phenomena
|
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|
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|
706.2334
|
MadGraph/MadEvent v4: The New Web Generation
|
We present the latest developments of the MadGraph/MadEvent Monte Carlo event
generator and several applications to hadron collider physics. In the current
version events at the parton, hadron and detector level can be generated
directly from a web interface, for arbitrary processes in the Standard Model
and in several physics scenarios beyond it (HEFT, MSSM, 2HDM). The most
important additions are: a new framework for implementing user-defined new
physics models; a standalone running mode for creating and testing matrix
elements; generation of events corresponding to different processes, such as
signal(s) and backgrounds, in the same run; two platforms for data analysis,
where events are accessible at the parton, hadron and detector level; and the
generation of inclusive multi-jet samples by combining parton-level events with
parton showers. To illustrate the new capabilities of the package some
applications to hadron collider physics are presented:
1) Higgs search in pp \to H \to W^+W^-: signal and backgrounds.
2) Higgs CP properties: pp \to H jj$in the HEFT.
3) Spin of a new resonance from lepton angular distributions.
4) Single-top and Higgs associated production in a generic 2HDM.
5) Comparison of strong SUSY pair production at the SPS points.
6) Inclusive W+jets matched samples: comparison with the Tevatron data.
|
hep-ph
|
we present the latest developments of the madgraphmadevent monte carlo event generator and several applications to hadron collider physics in the current version events at the parton hadron and detector level can be generated directly from a web interface for arbitrary processes in the standard model and in several physics scenarios beyond it heft mssm 2hdm the most important additions are a new framework for implementing userdefined new physics models a standalone running mode for creating and testing matrix elements generation of events corresponding to different processes such as signals and backgrounds in the same run two platforms for data analysis where events are accessible at the parton hadron and detector level and the generation of inclusive multijet samples by combining partonlevel events with parton showers to illustrate the new capabilities of the package some applications to hadron collider physics are presented 1 higgs search in pp to h to ww signal and backgrounds 2 higgs cp properties pp to h jjin the heft 3 spin of a new resonance from lepton angular distributions 4 singletop and higgs associated production in a generic 2hdm 5 comparison of strong susy pair production at the sps points 6 inclusive wjets matched samples comparison with the tevatron data
|
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|
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|
706.2335
|
Lateral Effects in Fermion Antibunching
|
Lateral effects are analyzed in the antibunching of a beam of free
non-interacting fermions. The emission of particles from a source is
dynamically described in a 3D full quantum field-theoretical framework. The
size of the source and the detectors, as well as the temperature of the source
are taken into account and the behavior of the visibility is scrutinized as a
function of these parameters.
|
quant-ph
|
lateral effects are analyzed in the antibunching of a beam of free noninteracting fermions the emission of particles from a source is dynamically described in a 3d full quantum fieldtheoretical framework the size of the source and the detectors as well as the temperature of the source are taken into account and the behavior of the visibility is scrutinized as a function of these parameters
|
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|
[-0.10102327635081915, 0.18281513690375364, -0.10724913619028834, 0.07547868477682082, 0.010530985254221237, -0.09672970564032976, 0.007025941414758563, 0.36747278404923583, -0.2416222419159917, -0.3132652434851759, 0.05620080615537098, -0.30273647411511495, -0.047854166477918625, 0.18732577408305728, 0.025514758507219643, 0.0721559127076314, 0.018947376095904755, 0.0325447171066816, -0.044746470651947534, -0.1589640250429511, 0.29565618264202315, 0.07444314624791822, 0.257331675864183, 0.08812711824877904, 0.09849405088103734, 0.016498027835041285, -0.019031728066217442, 0.063585890055849, -0.05224832370877266, 0.030742708765543424, 0.1984918862151412, 0.0793091858808811, 0.2108362092421605, -0.40729894351500734, -0.2654251679778099, 0.024770724006856863, 0.14077482588875753, 0.12019650503419912, -0.04038894495998437, -0.34087222647280074, 0.007981883662824447, -0.149184291709501, -0.15189453664307412, 0.021393856291587535, -0.021311225856725985, 0.03785865876035621, -0.2362375957174943, 0.07481745443879985, 0.05595035667961033, 0.03437029556013071, -0.04505237230601219, -0.09463049753640707, -0.04461158416233957, 0.18436703260701437, 0.036064819984424575, -0.00018955191883903284, 0.14266038823944444, -0.17213997893895094, -0.08759207452933948, 0.44453088325949813, -0.06380037404596806, -0.19484886879531238, 0.14509187163068699, -0.13566781100458825, -0.03849982278994643, 0.14343462781264232, 0.16728836992898813, 0.10511645927595405, -0.180578513436306, 0.0763502625588444, -0.01833082533513124, 0.15744353911051384, 0.009235751055754148, 0.08860819522434703, 0.25192236089362546, 0.17830699218007234, -0.024722493511552993, 0.2151213119075132, -0.14782249477620307, -0.08214730369643523, -0.34859525048388884, -0.15616319361501016, -0.22160539088340905, 0.038827584841503546, -0.064512119527745, -0.18672942623782615, 0.42711083616774814, 0.12173299319469012, 0.21692821450818042, -0.00039872438714015656, 0.30411137004311267, 0.1385467595868529, 0.10369550506942547, 0.009690574914790117, 0.2460688802556923, 0.11959244837411322, 0.06380885034226454, -0.2491973126701151, 0.02047169809632648, 0.009097682541379562]
|
706.2336
|
Testing AdS/CFT Deviations from pQCD Heavy Quark Energy Loss with Pb+Pb
at LHC
|
Heavy quark jet quenching in nuclear collisions at LHC is predicted and
compared using the classical gravity AdS/CFT correspondence and Standard Model
perturbative QCD. The momentum independence and inverse quark mass dependence
of the drag coefficient in AdS/CFT differs substantially from the
characteristic log(pT/M)/pT variation of the drag in QCD. We propose that the
measurement of the momentum dependence of the double ratio of the nuclear
modification factors of charm and bottom jets is a robust observable that can
be used to search for strong coupling deviations from perturbative QCD
predictions.
|
nucl-th
|
heavy quark jet quenching in nuclear collisions at lhc is predicted and compared using the classical gravity adscft correspondence and standard model perturbative qcd the momentum independence and inverse quark mass dependence of the drag coefficient in adscft differs substantially from the characteristic logptmpt variation of the drag in qcd we propose that the measurement of the momentum dependence of the double ratio of the nuclear modification factors of charm and bottom jets is a robust observable that can be used to search for strong coupling deviations from perturbative qcd predictions
|
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|
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|
706.2337
|
The extended structure of the remote cluster B514 in M31. Detection of
extra-tidal stars
|
We present a study of the density profile of the remote M31 globular cluster
B514, obtained from HST/ACS observations. Coupling the analysis of the
distribution of the integrated light with star counts we can reliably follow
the profile of the cluster out to r~35", corresponding to ~130pc. The profile
is well fitted, out to ~15 core radii, by a King Model having C=1.65. With an
estimated core radius r_c=0.38", this corresponds to a tidal radius of r_t~17"
(~65pc). We find that both the light and the star counts profiles show a
departure from the best fit King model for r>~8" - as a surface brightness
excess at large radii, and the star counts profile shows a clear break in
correspondence of the estimated tidal radius. Both features are interpreted as
the signature of the presence of extratidal stars around the cluster. We also
show that B514 has a half-light radius significantly larger than ordinary
globular clusters of the same luminosity. In the M_V vs. log r_h plane, B514
lies in a region inhabited by peculiar clusters, like Omega Cen, G1, NGC2419
and others, as well as by the nuclei of dwarf elliptical galaxies.
|
astro-ph
|
we present a study of the density profile of the remote m31 globular cluster b514 obtained from hstacs observations coupling the analysis of the distribution of the integrated light with star counts we can reliably follow the profile of the cluster out to r35 corresponding to 130pc the profile is well fitted out to 15 core radii by a king model having c165 with an estimated core radius r_c038 this corresponds to a tidal radius of r_t17 65pc we find that both the light and the star counts profiles show a departure from the best fit king model for r8 as a surface brightness excess at large radii and the star counts profile shows a clear break in correspondence of the estimated tidal radius both features are interpreted as the signature of the presence of extratidal stars around the cluster we also show that b514 has a halflight radius significantly larger than ordinary globular clusters of the same luminosity in the m_v vs log r_h plane b514 lies in a region inhabited by peculiar clusters like omega cen g1 ngc2419 and others as well as by the nuclei of dwarf elliptical galaxies
|
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|
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|
706.2338
|
The light variability of the helium strong star HD 37776 as a result of
its inhomogeneous elemental surface distribution
|
We simulate light curves of the helium strong chemically peculiar star HD
37776 assuming that the observed periodic light variations originate as a
result of inhomogeneous horizontal distribution of chemical elements on the
surface of a rotating star. We show that chemical peculiarity influences the
monochromatic radiative flux, mainly due to bound-free processes. Using the
model of the distribution of silicon and helium on HD 37776 surface, derived
from spectroscopy, we calculate a photometric map of the surface and
consequently the uvby light curves of this star. Basically, the predicted light
curves agree in shape and amplitude with the observed ones. We conclude that
the basic properties of variability of this helium strong chemically peculiar
star can be understood in terms of the model of spots with peculiar chemical
composition.
|
astro-ph
|
we simulate light curves of the helium strong chemically peculiar star hd 37776 assuming that the observed periodic light variations originate as a result of inhomogeneous horizontal distribution of chemical elements on the surface of a rotating star we show that chemical peculiarity influences the monochromatic radiative flux mainly due to boundfree processes using the model of the distribution of silicon and helium on hd 37776 surface derived from spectroscopy we calculate a photometric map of the surface and consequently the uvby light curves of this star basically the predicted light curves agree in shape and amplitude with the observed ones we conclude that the basic properties of variability of this helium strong chemically peculiar star can be understood in terms of the model of spots with peculiar chemical composition
|
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|
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|
706.2339
|
Low-Scale Technicolor at the Tevatron and LHC
|
The Tevatron experiments CDF and DO are close to making definitive statements
about the technicolor discovery mode rho_T -> W pi_T for M(rho_T) <~ 230 GeV
and M(pi_T) <~ 125 GeV. We propose new incisive tests for this mode and
searches for others that may be feasible at the Tevatron and certainly are at
the LHC. The other searches include two long discussed, namely, omega_T ->
gamma pi_T and l+l-, and a new one -- for the I^G J^{PC} = 1^- 1^{++} partner,
a_T, of the rho_T. Adopting the argument that the technicolor contribution to S
is reduced if M(a_T) is near M(rho_T), we enumerate important a_T decays and
estimate production rates at the colliders.
|
hep-ph hep-ex
|
the tevatron experiments cdf and do are close to making definitive statements about the technicolor discovery mode rho_t w pi_t for mrho_t 230 gev and mpi_t 125 gev we propose new incisive tests for this mode and searches for others that may be feasible at the tevatron and certainly are at the lhc the other searches include two long discussed namely omega_t gamma pi_t and ll and a new one for the ig jpc 1 1 partner a_t of the rho_t adopting the argument that the technicolor contribution to s is reduced if ma_t is near mrho_t we enumerate important a_t decays and estimate production rates at the colliders
|
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|
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|
706.234
|
Hodge-Stickelberger polygons for L-functions of exponential sums of
P(x^s)
|
Let P(x) be a one-variable Laurent polynomial of degree (d_1,d_2) over a
finite field of characteristic p. For any fixed positive integer s not
divisible by p, we prove that the (normalized) p-adic Newton polygon of the
L-functions of exponential sums of P(x^s) has a tight lower bound which we call
`Hodge-Stickelberger polygon', depending only on d_1,d_2,s, and (p mod s). This
Hodge-Stickelberger polygon is a weighted convolution of a `Hodge polygon' for
L-function of exponential sum of P(x) and the `Newton polygon' for L-function
of exponential sum of x^s (given by the classical Stickelberger theory). We
prove an analogous Hodge-Stickelberger lower bound for multivariable Laurent
polynomials as well.
We prove this Hodge-Stickelberger polygon is the limit of generic Newton
polygons of P(x^s) in a sense that was made explicit in the paper.
|
math.NT math.AG
|
let px be a onevariable laurent polynomial of degree d_1d_2 over a finite field of characteristic p for any fixed positive integer s not divisible by p we prove that the normalized padic newton polygon of the lfunctions of exponential sums of pxs has a tight lower bound which we call hodgestickelberger polygon depending only on d_1d_2s and p mod s this hodgestickelberger polygon is a weighted convolution of a hodge polygon for lfunction of exponential sum of px and the newton polygon for lfunction of exponential sum of xs given by the classical stickelberger theory we prove an analogous hodgestickelberger lower bound for multivariable laurent polynomials as well we prove this hodgestickelberger polygon is the limit of generic newton polygons of pxs in a sense that was made explicit in the paper
|
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|
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|
706.2341
|
Tri-Bimaximal Neutrino Mixing and the Family Symmetry Z_7 x Z_3
|
The Non-Abelian finite group PSL_2(7) is the only simple subgroup of SU(3)
with a complex three-dimensional irreducible representation. It has two maximal
subgroups, S_4 which, along with its own A_4 subgroup, has been successfully
applied in numerous models of flavor, as well as the 21 element Frobenius group
Z_7 x Z_3, which has gained much less attention. We show that it can also be
used to generate tri-bimaximal mixing in the neutrino sector, while allowing
for quark and charged lepton hierarchies.
|
hep-ph hep-th
|
the nonabelian finite group psl_27 is the only simple subgroup of su3 with a complex threedimensional irreducible representation it has two maximal subgroups s_4 which along with its own a_4 subgroup has been successfully applied in numerous models of flavor as well as the 21 element frobenius group z_7 x z_3 which has gained much less attention we show that it can also be used to generate tribimaximal mixing in the neutrino sector while allowing for quark and charged lepton hierarchies
|
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|
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|
706.2342
|
Gravitational Wilson Loop and Large Scale Curvature
|
In a quantum theory of gravity the gravitational Wilson loop, defined as a
suitable quantum average of a parallel transport operator around a large
near-planar loop, provides important information about the large-scale
curvature properties of the geometry. Here we shows that such properties can be
systematically computed in the strong coupling limit of lattice regularized
quantum gravity, by performing a local average over rotations, using an assumed
near-uniform measure in group space. We then relate the resulting quantum
averages to an expected semi-classical form valid for macroscopic observers,
which leads to an identification of the gravitational correlation length
appearing in the Wilson loop with an observed large-scale curvature. Our
results suggest that strongly coupled gravity leads to a positively curved (De
Sitter-like) quantum ground state, implying a positive effective cosmological
constant at large distances.
|
hep-th gr-qc
|
in a quantum theory of gravity the gravitational wilson loop defined as a suitable quantum average of a parallel transport operator around a large nearplanar loop provides important information about the largescale curvature properties of the geometry here we shows that such properties can be systematically computed in the strong coupling limit of lattice regularized quantum gravity by performing a local average over rotations using an assumed nearuniform measure in group space we then relate the resulting quantum averages to an expected semiclassical form valid for macroscopic observers which leads to an identification of the gravitational correlation length appearing in the wilson loop with an observed largescale curvature our results suggest that strongly coupled gravity leads to a positively curved de sitterlike quantum ground state implying a positive effective cosmological constant at large distances
|
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|
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|
706.2343
|
Nonlinear perturbations of Fuchsian systems: corrections and
linearization, normal forms
|
Nonlinear perturbation of Fuchsian systems are studied in a region including
two singularities. It is proved that such systems are generally not
analytically equivalent to their linear part (they are not linearizable) and
the obstructions are found constructively, as a countable set of numbers.
Furthermore, assuming a polynomial character of the nonlinear part, it is shown
that there exists a unique formal "correction" of the nonlinear part so that
the "corrected" system is formally linearizable.
Normal forms of these systems are found, providing also their classification.
|
math.CA
|
nonlinear perturbation of fuchsian systems are studied in a region including two singularities it is proved that such systems are generally not analytically equivalent to their linear part they are not linearizable and the obstructions are found constructively as a countable set of numbers furthermore assuming a polynomial character of the nonlinear part it is shown that there exists a unique formal correction of the nonlinear part so that the corrected system is formally linearizable normal forms of these systems are found providing also their classification
|
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|
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|
706.2344
|
Detectors for the James Webb Space Telescope Near-Infrared Spectrograph
I: Readout Mode, Noise Model, and Calibration Considerations
|
We describe how the James Webb Space Telescope (JWST) Near-Infrared
Spectrograph's (NIRSpec's) detectors will be read out, and present a model of
how noise scales with the number of multiple non-destructive reads
sampling-up-the-ramp. We believe that this noise model, which is validated
using real and simulated test data, is applicable to most astronomical
near-infrared instruments. We describe some non-ideal behaviors that have been
observed in engineering grade NIRSpec detectors, and demonstrate that they are
unlikely to affect NIRSpec sensitivity, operations, or calibration. These
include a HAWAII-2RG reset anomaly and random telegraph noise (RTN). Using real
test data, we show that the reset anomaly is: (1) very nearly noiseless and (2)
can be easily calibrated out. Likewise, we show that large-amplitude RTN
affects only a small and fixed population of pixels. It can therefore be
tracked using standard pixel operability maps.
|
astro-ph
|
we describe how the james webb space telescope jwst nearinfrared spectrographs nirspecs detectors will be read out and present a model of how noise scales with the number of multiple nondestructive reads samplinguptheramp we believe that this noise model which is validated using real and simulated test data is applicable to most astronomical nearinfrared instruments we describe some nonideal behaviors that have been observed in engineering grade nirspec detectors and demonstrate that they are unlikely to affect nirspec sensitivity operations or calibration these include a hawaii2rg reset anomaly and random telegraph noise rtn using real test data we show that the reset anomaly is 1 very nearly noiseless and 2 can be easily calibrated out likewise we show that largeamplitude rtn affects only a small and fixed population of pixels it can therefore be tracked using standard pixel operability maps
|
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|
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|
706.2345
|
Phenomenology from a U(1) gauged hidden sector
|
We consider the phenomenological consequences of a hidden Higgs sector
extending the Standard Model (SM), in which the matter content are uncharged
under the SM gauge groups. We consider a simple case where the hidden sector is
gauged under a U(1) with one Higgs singlet. The only couplings between SM and
the hidden sector are through mixings between the neutral gauge bosons of the
two respective sectors, and between the Higgs bosons. We find signals testable
at the LHC that can reveal the existence and shed light on the nature of such a
hidden sector.
|
hep-ph
|
we consider the phenomenological consequences of a hidden higgs sector extending the standard model sm in which the matter content are uncharged under the sm gauge groups we consider a simple case where the hidden sector is gauged under a u1 with one higgs singlet the only couplings between sm and the hidden sector are through mixings between the neutral gauge bosons of the two respective sectors and between the higgs bosons we find signals testable at the lhc that can reveal the existence and shed light on the nature of such a hidden sector
|
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|
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|
706.2346
|
Non-Gaussianity analysis on local morphological measures of WMAP data
|
The decomposition of a signal on the sphere with the steerable wavelet
constructed from the second Gaussian derivative gives access to the
orientation, signed-intensity, and elongation of the signal's local features.
In the present work, the non-Gaussianity of the WMAP temperature data of the
cosmic microwave background (CMB) is analyzed in terms of the first four
moments of the statistically isotropic random fields associated with these
local morphological measures, at wavelet scales corresponding to angular sizes
between 27.5 arcminutes and 30 degrees on the celestial sphere. While no
detection is made neither in the orientation analysis nor in the elongation
analysis, a strong detection is made in the excess kurtosis of the
signed-intensity of the WMAP data. The non-Gaussianity is observed with a
significance level below 0.5% at a wavelet scale corresponding to an angular
size around 10 degrees, and confirmed at neighbour scales. This supports a
previous detection of an excess of kurtosis in the wavelet coefficient of the
WMAP data with the axisymmetric Mexican hat wavelet (Vielva et al. 2004).
Instrumental noise and foreground emissions are not likely to be at the origin
of the excess of kurtosis. Large-scale modulations of the CMB related to some
unknown systematics are rejected as possible origins of the detection. The
observed non-Gaussianity may therefore probably be imputed to the CMB itself,
thereby questioning the basic inflationary scenario upon which the present
concordance cosmological model relies. Taking the CMB temperature angular power
spectrum of the concordance cosmological model at face value, further analysis
also suggests that this non-Gaussianity is not confined to the directions on
the celestial sphere with an anomalous signed-intensity.
|
astro-ph
|
the decomposition of a signal on the sphere with the steerable wavelet constructed from the second gaussian derivative gives access to the orientation signedintensity and elongation of the signals local features in the present work the nongaussianity of the wmap temperature data of the cosmic microwave background cmb is analyzed in terms of the first four moments of the statistically isotropic random fields associated with these local morphological measures at wavelet scales corresponding to angular sizes between 275 arcminutes and 30 degrees on the celestial sphere while no detection is made neither in the orientation analysis nor in the elongation analysis a strong detection is made in the excess kurtosis of the signedintensity of the wmap data the nongaussianity is observed with a significance level below 05 at a wavelet scale corresponding to an angular size around 10 degrees and confirmed at neighbour scales this supports a previous detection of an excess of kurtosis in the wavelet coefficient of the wmap data with the axisymmetric mexican hat wavelet vielva et al 2004 instrumental noise and foreground emissions are not likely to be at the origin of the excess of kurtosis largescale modulations of the cmb related to some unknown systematics are rejected as possible origins of the detection the observed nongaussianity may therefore probably be imputed to the cmb itself thereby questioning the basic inflationary scenario upon which the present concordance cosmological model relies taking the cmb temperature angular power spectrum of the concordance cosmological model at face value further analysis also suggests that this nongaussianity is not confined to the directions on the celestial sphere with an anomalous signedintensity
|
[['the', 'decomposition', 'of', 'a', 'signal', 'on', 'the', 'sphere', 'with', 'the', 'steerable', 'wavelet', 'constructed', 'from', 'the', 'second', 'gaussian', 'derivative', 'gives', 'access', 'to', 'the', 'orientation', 'signedintensity', 'and', 'elongation', 'of', 'the', 'signals', 'local', 'features', 'in', 'the', 'present', 'work', 'the', 'nongaussianity', 'of', 'the', 'wmap', 'temperature', 'data', 'of', 'the', 'cosmic', 'microwave', 'background', 'cmb', 'is', 'analyzed', 'in', 'terms', 'of', 'the', 'first', 'four', 'moments', 'of', 'the', 'statistically', 'isotropic', 'random', 'fields', 'associated', 'with', 'these', 'local', 'morphological', 'measures', 'at', 'wavelet', 'scales', 'corresponding', 'to', 'angular', 'sizes', 'between', '275', 'arcminutes', 'and', '30', 'degrees', 'on', 'the', 'celestial', 'sphere', 'while', 'no', 'detection', 'is', 'made', 'neither', 'in', 'the', 'orientation', 'analysis', 'nor', 'in', 'the', 'elongation', 'analysis', 'a', 'strong', 'detection', 'is', 'made', 'in', 'the', 'excess', 'kurtosis', 'of', 'the', 'signedintensity', 'of', 'the', 'wmap', 'data', 'the', 'nongaussianity', 'is', 'observed', 'with', 'a', 'significance', 'level', 'below', '05', 'at', 'a', 'wavelet', 'scale', 'corresponding', 'to', 'an', 'angular', 'size', 'around', '10', 'degrees', 'and', 'confirmed', 'at', 'neighbour', 'scales', 'this', 'supports', 'a', 'previous', 'detection', 'of', 'an', 'excess', 'of', 'kurtosis', 'in', 'the', 'wavelet', 'coefficient', 'of', 'the', 'wmap', 'data', 'with', 'the', 'axisymmetric', 'mexican', 'hat', 'wavelet', 'vielva', 'et', 'al', '2004', 'instrumental', 'noise', 'and', 'foreground', 'emissions', 'are', 'not', 'likely', 'to', 'be', 'at', 'the', 'origin', 'of', 'the', 'excess', 'of', 'kurtosis', 'largescale', 'modulations', 'of', 'the', 'cmb', 'related', 'to', 'some', 'unknown', 'systematics', 'are', 'rejected', 'as', 'possible', 'origins', 'of', 'the', 'detection', 'the', 'observed', 'nongaussianity', 'may', 'therefore', 'probably', 'be', 'imputed', 'to', 'the', 'cmb', 'itself', 'thereby', 'questioning', 'the', 'basic', 'inflationary', 'scenario', 'upon', 'which', 'the', 'present', 'concordance', 'cosmological', 'model', 'relies', 'taking', 'the', 'cmb', 'temperature', 'angular', 'power', 'spectrum', 'of', 'the', 'concordance', 'cosmological', 'model', 'at', 'face', 'value', 'further', 'analysis', 'also', 'suggests', 'that', 'this', 'nongaussianity', 'is', 'not', 'confined', 'to', 'the', 'directions', 'on', 'the', 'celestial', 'sphere', 'with', 'an', 'anomalous', 'signedintensity']]
|
[-0.11278795193777316, 0.09798082104443219, -0.09775620028333462, 0.06446924701427903, -0.08322335516050872, -0.04713224495881824, -0.009094701233078484, 0.3417412813373462, -0.2469484240454794, -0.3016716801457935, 0.09206389136164, -0.3198510643804049, -0.05768026846150557, 0.18026616414405267, -0.005778491647948546, 0.012780176380356015, -0.018867109567616825, 0.0158747993176803, -0.03367341866013939, -0.2507687823726209, 0.2599860496482708, 0.18056733187857188, 0.2809298341507437, -0.001924470865547105, 0.08187454253116071, -0.0521321675007197, -0.11389575419792285, 0.0018786638423248573, -0.11497638299815999, 0.08595959766923139, 0.19228167404696622, 0.11386631568807556, 0.1917874191749703, -0.3398522590149056, -0.22027467320483454, 0.13553864335537785, 0.10109459885775492, 0.08083809286741868, 0.0002981358522514778, -0.3103514206086941, 0.03888015506996049, -0.10896446088208231, -0.13274584883496304, -0.03149752739592697, 0.013172304963141129, -0.02240714426691368, -0.2555631977678449, 0.17699231941638843, 0.05503030567542063, 0.0908758050787987, -0.05750434516446182, -0.1345665714186099, -0.05337396348930067, 0.041534706545321064, 0.062903245250453, 0.04949069908239094, 0.1534918881331881, -0.10266806816087208, -0.1005752383791669, 0.3753925109144162, -0.0931051378586778, -0.15267630378129304, 0.1411994671584883, -0.21487098274821484, -0.17467458836596322, 0.14056360395142192, 0.1549854762679725, 0.01575832950960224, -0.13230358985839066, 0.07860667297047459, 0.01829346511081827, 0.22117923454174565, 0.10457368000427744, 0.0258917878877751, 0.29291462747000707, 0.09060075482422555, 0.08391319916462871, 0.10943489049440595, -0.21632865878292015, -0.016866001673042773, -0.30752374362480756, -0.04674073637083725, -0.21495802798825833, 0.016389620179338468, -0.15857002911140658, -0.16861425049169662, 0.42353422324932005, 0.15450557688708175, 0.2250448462022986, 0.0397698862465202, 0.32196968696252615, 0.055876737272073686, 0.0635484159104871, 0.05338970414207627, 0.3029157726444451, 0.12157699771018492, 0.0946331543761685, -0.20009514695169248, 0.05239511978191634, -0.021229102309034378]
|
706.2347
|
On the cyclicity of weight-homogeneous centers
|
Let W be a weight-homogeneous planar polynomial differential system with a
center. We find an upper bound of the number of limit cycles which bifurcate
from the period annulus of W under a generic polynomial perturbation. We apply
this result to a particular family of planar polynomial systems having a
nilpotent center without meromorphic first integral.
|
math.DS
|
let w be a weighthomogeneous planar polynomial differential system with a center we find an upper bound of the number of limit cycles which bifurcate from the period annulus of w under a generic polynomial perturbation we apply this result to a particular family of planar polynomial systems having a nilpotent center without meromorphic first integral
|
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|
[-0.23202735345278466, 0.06965694429553489, -0.10292451505249899, -0.03326702117296269, -0.08989896731717247, -0.1393986092131984, 0.03665544644796422, 0.25905930284144624, -0.3098133520023631, -0.256561042325172, 0.11508756574143522, -0.2345938241175775, -0.13478883119699145, 0.22806095820851624, -0.0658487358180407, 0.036912632773497274, 0.10241831727658532, 0.11598636165477469, -0.07320738360119451, -0.2580297788081225, 0.339061755088291, -0.0752989302854985, 0.14991582013733154, -0.01809442183522541, 0.10174295721974756, 0.035386377916438505, 0.06785573741477233, -0.021388875258188427, -0.1763564233634887, 0.1200783044498946, 0.2354419063111501, 0.04094520874787122, 0.2200419679949326, -0.3814164837822318, -0.13243654260544904, 0.22749248250121518, 0.16712161685739244, 0.08957978325322204, -0.023656214753698026, -0.22354854267489696, 0.09796097265955593, -0.1880007278440254, -0.24868440910774683, 0.023425851865405484, 0.09943426076123225, 0.0022008462443149517, -0.2983719026087783, -0.0016675351154325263, 0.12124308724222439, 0.09584114841449523, -0.035453488426615616, -0.07372458467190361, -0.0663899323636932, 0.04289854382763484, -0.06185146717221609, 0.06756411050446332, 0.0818448439489917, -0.04257820236879135, -0.1270651924257566, 0.32000943498132983, -0.15579741772048042, -0.21706406752179777, 0.12568087968975306, -0.19526170653158, -0.17668169711084505, 0.15771534305531532, 0.17713330602938576, 0.16585608132715737, -0.09591444554306301, 0.19275382162803517, -0.13543693970755807, 0.13548558409924485, 0.16002006206794508, -0.029832150487761413, 0.19954995842584008, 0.09324409071788457, 0.14772295498239277, 0.18665078446792904, -0.020356251575451876, -0.022226584917266985, -0.3506162357849202, -0.12690842805750435, -0.13346351041192456, 0.13420343715032296, -0.1271815882022825, -0.2110030005486416, 0.36492960569116156, 0.022044142841228416, 0.21589488845451602, 0.13784077864797187, 0.1826710983711694, 0.18826002659209604, 0.040984414799822844, 0.10840794375898051, 0.16238509798755071, 0.18554519584202872, 0.020124200615100563, -0.16260352635539935, -0.02760674776176789, 0.15620574660715647]
|
706.2348
|
Analytic linearization of nonlinear perturbations of Fuchsian systems
|
Nonlinear perturbation of Fuchsian systems are studied in regions including
two singularities. Such systems are not necessarily analytically equivalent to
their linear part (they are not linearizable). Nevertheless, it is shown that
in the case when the linear part has commuting monodromy, and the eigenvalues
have positive real parts, there exists a unique correction function of the
nonlinear part so that the corrected system becomes analytically linearizable.
|
math.CA
|
nonlinear perturbation of fuchsian systems are studied in regions including two singularities such systems are not necessarily analytically equivalent to their linear part they are not linearizable nevertheless it is shown that in the case when the linear part has commuting monodromy and the eigenvalues have positive real parts there exists a unique correction function of the nonlinear part so that the corrected system becomes analytically linearizable
|
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|
[-0.18176186368140435, 0.06393949594348669, -0.0533297996022808, 0.08581625627277335, -0.06760529726187685, -0.18349304702827957, -0.09197661072821982, 0.3683603819348474, -0.2991644563848403, -0.1793492041986936, 0.16944819268572436, -0.3373973814513423, -0.2423673402518034, 0.1971828729581477, -0.052778638906276494, 0.09050809521116872, 0.05783152725345997, 0.07647093183555599, -0.06143766340848281, -0.2874900895229944, 0.3907686210334746, -0.05489723911203111, 0.16922982960397295, 0.031205196121234947, 0.10909310936121576, -0.051037072374332526, -0.007850826154949505, 0.052818536063406, -0.05545539741943861, -0.0033471347041316886, 0.3184516323876303, 0.06825995033801492, 0.26177789529424106, -0.3991507265383183, -0.16131315816805433, 0.18068059657547456, 0.17572999701821315, 0.09309879248377992, -0.027881878370822254, -0.23532637092979874, 0.10296108461082426, -0.13483391495755137, -0.14879255123269647, -0.11059069494480517, 0.0921767463268184, 6.599398329854012e-05, -0.21532877627760172, 0.06729194198026141, 0.09902696142584752, 0.031453206162176915, -0.049144060469107395, -0.07394017809967218, -0.06559742999666218, 0.1353190624239375, 0.003059934352419457, -0.053056830514236285, 0.07830950280707051, -0.09497360476473374, -0.02127843494735547, 0.3859231232929586, -0.024414626551347216, -0.3021780920367855, 0.18244088889766874, -0.1574047188510868, -0.14577467170710773, 0.15862895735998206, 0.12193544571802242, 0.12475108964118495, -0.12375466504465239, 0.1652850432368343, -0.05880336873511325, 0.16424322303440145, 0.048062197175988954, 0.012316251840831629, 0.18512101354661273, 0.03570913811172567, 0.09227020644110197, 0.10824963633916271, 0.05869373688196291, -0.1118605568198793, -0.33457094236318746, -0.09939944890758662, -0.17784385084271875, 0.03264842470873272, -0.02562286010435122, -0.22534693407247525, 0.36496087480614436, 0.0652845043501358, 0.16018913850646965, 0.05798121604290026, 0.2784637085478336, 0.23502205818919325, 0.1208654496742329, 0.10308146011779334, 0.29625372578209236, 0.12637558210738448, 0.07574982010001845, -0.20474706100188753, 0.0467876485034601, 0.07977171784350232]
|
706.2349
|
The $^{15}$O($\alpha$,$\gamma$)$^{19}$Ne Breakout Reaction and Impact on
X-Ray Bursts
|
The breakout reaction $^{15}$O($\alpha,\gamma$)$^{19}$Ne, which regulates the
flow between the hot CNO cycle and the rp-process, is critical for the
explanation of the burst amplitude and periodicity of X-ray bursters. We report
on the first successful measurement of the critical $\alpha$-decay branching
ratios of relevant states in $^{19}$Ne populated via
$^{19}$F($^3$He,t)$^{19}$Ne. Based on the experimental results and our previous
lifetime measurements of these states, we derive the first experimental rate of
$^{15}$O($\alpha,\gamma$)$^{19}$Ne. The impact of our experimental results on
the burst pattern and periodicity for a range of accretion rates is analyzed.
|
nucl-ex astro-ph
|
the breakout reaction 15oalphagamma19ne which regulates the flow between the hot cno cycle and the rpprocess is critical for the explanation of the burst amplitude and periodicity of xray bursters we report on the first successful measurement of the critical alphadecay branching ratios of relevant states in 19ne populated via 19f3het19ne based on the experimental results and our previous lifetime measurements of these states we derive the first experimental rate of 15oalphagamma19ne the impact of our experimental results on the burst pattern and periodicity for a range of accretion rates is analyzed
|
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|
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|
706.235
|
Kummer subfields of tame division algebras over Henselian valued fields
|
By generalizing the method used by Tignol and Amitsur in [TA85], we determine
necessary and sufficient conditions for an arbitrary tame central division
algebra D over a Henselian valued field E to have Kummer subfields [Corollary
2.11 and Corollary 2.12]. We prove also that if D is a tame semiramified
division algebra of prime power degree p^n over E such that p\neq char(\bar E)
and rk(\Gamma_D/\Gamma_E)\geq 3 [resp., such that p\neq char(\bar E) and p^3
divides exp(\Gamma_D/\Gamma_E)], then D is non-cyclic [Proposition 3.1] [resp.,
D is not an elementary abelian crossed product [Proposition 3.2]].
|
math.RA
|
by generalizing the method used by tignol and amitsur in ta85 we determine necessary and sufficient conditions for an arbitrary tame central division algebra d over a henselian valued field e to have kummer subfields corollary 211 and corollary 212 we prove also that if d is a tame semiramified division algebra of prime power degree pn over e such that pneq charbar e and rkgamma_dgamma_egeq 3 resp such that pneq charbar e and p3 divides expgamma_dgamma_e then d is noncyclic proposition 31 resp d is not an elementary abelian crossed product proposition 32
|
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|
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|
706.2351
|
Probing the Relation Between X-ray-Derived and Weak-Lensing-Derived
Masses for Shear-Selected Galaxy Clusters: I. A781
|
We compare X-ray and weak-lensing masses for four galaxy clusters that
comprise the top-ranked shear-selected cluster system in the Deep Lens Survey.
The weak-lensing observations of this system, which is associated with A781,
are from the Kitt Peak Mayall 4-m telescope, and the X-ray observations are
from both Chandra and XMM-Newton. For a faithful comparison of masses, we adopt
the same matter density profile for each method, which we choose to be an NFW
profile. Since neither the X-ray nor weak-lensing data are deep enough to well
constrain both the NFW scale radius and central density, we estimate the scale
radius using a fitting function for the concentration derived from cosmological
hydrodynamic simulations and an X-ray estimate of the mass assuming
isothermality. We keep this scale radius in common for both X-ray and
weak-lensing profiles, and fit for the central density, which scales linearly
with mass. We find that for three of these clusters, there is agreement between
X-ray and weak-lensing NFW central densities, and thus masses. For the other
cluster, the X-ray central density is higher than that from weak-lensing by 2
sigma. X-ray images suggest that this cluster may be undergoing a merger with a
smaller cluster. This work serves as an additional step towards understanding
the possible biases in X-ray and weak-lensing cluster mass estimation methods.
Such understanding is vital to efforts to constrain cosmology using X-ray or
weak-lensing cluster surveys to trace the growth of structure over cosmic time.
|
astro-ph
|
we compare xray and weaklensing masses for four galaxy clusters that comprise the topranked shearselected cluster system in the deep lens survey the weaklensing observations of this system which is associated with a781 are from the kitt peak mayall 4m telescope and the xray observations are from both chandra and xmmnewton for a faithful comparison of masses we adopt the same matter density profile for each method which we choose to be an nfw profile since neither the xray nor weaklensing data are deep enough to well constrain both the nfw scale radius and central density we estimate the scale radius using a fitting function for the concentration derived from cosmological hydrodynamic simulations and an xray estimate of the mass assuming isothermality we keep this scale radius in common for both xray and weaklensing profiles and fit for the central density which scales linearly with mass we find that for three of these clusters there is agreement between xray and weaklensing nfw central densities and thus masses for the other cluster the xray central density is higher than that from weaklensing by 2 sigma xray images suggest that this cluster may be undergoing a merger with a smaller cluster this work serves as an additional step towards understanding the possible biases in xray and weaklensing cluster mass estimation methods such understanding is vital to efforts to constrain cosmology using xray or weaklensing cluster surveys to trace the growth of structure over cosmic time
|
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|
[-0.03088108910086714, 0.0686145447191103, -0.12444799759429055, 0.12304367225783888, -0.09555790052507762, -0.060624433726401916, 0.007466265705601914, 0.43185344498811495, -0.1813758417960149, -0.3597032731195812, 0.10302393616190555, -0.3196679952098325, -0.03802625274471556, 0.22387704140805628, 0.013442385403046021, 0.026300642323208813, 0.058193288663969424, -0.03426782407035185, -0.08160358587248297, -0.2572294512759787, 0.32143315090175045, 0.1150641082438694, 0.2080556834116578, -0.016841446296714337, 0.06544574722324291, -0.011503388080698028, -0.09225790837871624, 0.03054318548689899, -0.15994103888776479, 0.08045341981404343, 0.22505325079251678, 0.12923929753517846, 0.206952292649382, -0.35763191238597586, -0.20979250843996955, 0.06432827122685779, 0.18155529075436325, 0.04733181410515106, -0.06756572074005562, -0.2601563917672254, 0.08615454506711583, -0.21392417882201203, -0.160463213785494, 0.013942264327051217, -0.008106430949846382, 0.05851686805886228, -0.24282306559894565, 0.19090182724750865, -0.04759106625191515, 0.008995090877644933, -0.16028478657472264, -0.0979910279756389, -0.01850897883910134, 0.11030862355794481, 0.011418148926018503, 0.08457097327317506, 0.17838188188932377, -0.17103209460744398, -0.009174726692645394, 0.37669770097658956, -0.044840486288377765, -0.02649476170279239, 0.1746539671995405, -0.2010782400908815, -0.22258653945898937, 0.07040318514751231, 0.1493880897377131, 0.051974052365930605, -0.16121833426173615, 0.023487660947156142, -0.04646636032137192, 0.2943927366765592, 0.05592783328352703, -0.0023385587547138744, 0.33734744124367466, 0.1242113735779752, 0.10572384747986992, 0.06911095606432384, -0.2440397456969104, 0.004029487595757385, -0.24502847299608307, -0.08213546403028348, -0.15370898105495384, 0.05482072367038484, -0.13181012884726645, -0.14885082728815852, 0.30962420724439643, 0.12884541172313851, 0.2373258099659373, 0.11444313359425744, 0.3257505526582216, 0.08759121220403661, 0.11864936047563245, 0.0762631123667054, 0.26763717152576877, 0.17330388150105078, 0.059990971126409685, -0.2240074869291282, 0.01317315813107991, 0.0002624548074823839]
|
706.2352
|
Electron-acoustic-phonon scattering and electron relaxation in
two-coupled quantum rings
|
Electron relaxation, induced by acoustic phonons, is studied for coupled
quantum rings in the presence of external fields, both electric and magnetic.
We address the problem of a single electron in vertically coupled GaAs quantum
rings. Electron-phonon interaction is accounted for both deformation potential
and piezoelectric field coupling mechanisms. Depending on the external fields,
the ring radii and the separation between the rings, we show that the two
different couplings have different weights and importance. Significant
oscillations are found in the scattering rates from electron excited states to
the ground state, as a function of either the geometry of the system or the
external fields.
|
cond-mat.other cond-mat.mtrl-sci
|
electron relaxation induced by acoustic phonons is studied for coupled quantum rings in the presence of external fields both electric and magnetic we address the problem of a single electron in vertically coupled gaas quantum rings electronphonon interaction is accounted for both deformation potential and piezoelectric field coupling mechanisms depending on the external fields the ring radii and the separation between the rings we show that the two different couplings have different weights and importance significant oscillations are found in the scattering rates from electron excited states to the ground state as a function of either the geometry of the system or the external fields
|
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|
[-0.21704691833860817, 0.2074298341359411, -0.0012579387319939478, 0.053222053810688, 0.007612992219981693, -0.13804918525829202, -0.021301530128610986, 0.38233943590450853, -0.2987310005795388, -0.28534253397513004, 0.02678599835351287, -0.28433475363999605, -0.08969666615261564, 0.19191418160418314, 0.07827419010656221, 9.718043286175955e-05, -0.002843204318057923, 0.015469144788082867, -0.03485628610166411, -0.192145362021845, 0.34702495933466015, 0.026923795507866003, 0.3031035181401031, 0.08759049604247723, 0.06467150270556365, 0.045640819477626965, 0.07382848894312269, 0.04637360772494936, -0.08762850286376696, 0.06816764154659939, 0.19841172782138788, -0.04089059391990304, 0.22104850258855593, -0.4993156818761712, -0.2080497048263039, 0.05556968375153485, 0.12374116501194381, 0.1621378312508265, -0.08832163682562255, -0.2679868962460508, 0.0016773761117032597, -0.14245436300656625, -0.09709961743404467, -0.053629771988129335, 0.02967539343739017, 0.059147121668571515, -0.28157638107382116, 0.09738118199720269, 0.06111690979561813, 0.06112214117532685, -0.14120337210063424, -0.08370268953675848, -0.03395199730460133, 0.1071652303161543, 0.056018628193331615, 0.021553452809651694, 0.20306611643838032, -0.1598788003304175, -0.12801076626139027, 0.3417490991009843, -0.08956609339719372, -0.1826735378376075, 0.2018632356343525, -0.16444921571583976, 0.00130806912645875, 0.1267326143104583, 0.17601836680745084, 0.1164342935241404, -0.14040099401913939, 0.10910153514705598, 0.018632189392866122, 0.14332177743670485, 0.07306602018486176, 0.0736999084419083, 0.27185033813473725, 0.10596496210034405, 0.011321108236387815, 0.13822341908789462, -0.12317920722555192, -0.06314888747320288, -0.2526540706555049, -0.11440318117938227, -0.1722021491133741, 0.06998674724738868, -0.05465732415905222, -0.14780789682907716, 0.418014990152525, 0.12179398258560381, 0.16461380356479258, -0.07827305807066816, 0.28033111243553105, 0.1134978256310292, 0.09831639001412051, 0.03605563526950954, 0.30849222012218974, 0.216044755173581, 0.051377759054524914, -0.31830730634031906, 0.007494554030043738, -0.0016840405629149505]
|
706.2353
|
Modeling partitioning of Min proteins between daughter cells after
septation in Escherichia coli
|
Ongoing sub-cellular oscillation of Min proteins is required to block
minicelling in E. coli. Experimentally, Min oscillations are seen in newly
divided cells and no minicells are produced. In model Min systems many daughter
cells do not oscillate following septation because of unequal partitioning of
Min proteins between the daughter cells. Using the 3D model of Huang et al., we
investigate the septation process in detail to determine the cause of the
asymmetric partitioning of Min proteins between daughter cells. We find that
this partitioning problem arises at certain phases of the MinD and MinE
oscillations with respect to septal closure and it persists independently of
parameter variation. At most 85% of the daughter cells exhibit Min oscillation
following septation. Enhanced MinD binding at the static polar and dynamic
septal regions, consistent with cardiolipin domains, does not substantially
increase this fraction of oscillating daughters. We believe that this problem
will be shared among all existing Min models and discuss possible biological
mechanisms that may minimize partitioning errors of Min proteins following
septation.
|
q-bio.SC
|
ongoing subcellular oscillation of min proteins is required to block minicelling in e coli experimentally min oscillations are seen in newly divided cells and no minicells are produced in model min systems many daughter cells do not oscillate following septation because of unequal partitioning of min proteins between the daughter cells using the 3d model of huang et al we investigate the septation process in detail to determine the cause of the asymmetric partitioning of min proteins between daughter cells we find that this partitioning problem arises at certain phases of the mind and mine oscillations with respect to septal closure and it persists independently of parameter variation at most 85 of the daughter cells exhibit min oscillation following septation enhanced mind binding at the static polar and dynamic septal regions consistent with cardiolipin domains does not substantially increase this fraction of oscillating daughters we believe that this problem will be shared among all existing min models and discuss possible biological mechanisms that may minimize partitioning errors of min proteins following septation
|
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|
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|
706.2354
|
FPTAS for optimizing polynomials over the mixed-integer points of
polytopes in fixed dimension
|
We show the existence of a fully polynomial-time approximation scheme (FPTAS)
for the problem of maximizing a non-negative polynomial over mixed-integer sets
in convex polytopes, when the number of variables is fixed. Moreover, using a
weaker notion of approximation, we show the existence of a fully
polynomial-time approximation scheme for the problem of maximizing or
minimizing an arbitrary polynomial over mixed-integer sets in convex polytopes,
when the number of variables is fixed.
|
math.OC
|
we show the existence of a fully polynomialtime approximation scheme fptas for the problem of maximizing a nonnegative polynomial over mixedinteger sets in convex polytopes when the number of variables is fixed moreover using a weaker notion of approximation we show the existence of a fully polynomialtime approximation scheme for the problem of maximizing or minimizing an arbitrary polynomial over mixedinteger sets in convex polytopes when the number of variables is fixed
|
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|
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|
706.2355
|
Supergravity origin of the MSSM inflation
|
We consider the supergravity origin of the recently proposed MSSM
inflationary model, which relies on the existence of a saddle point along a
dimension six flat direction. We derive the conditions that the Kahler
potential has to satisfy for the saddle point to exist irrespective of the
hidden sector vevs. We show that these conditions are satisfied by a simple
class of Kahler potentials, which we find to have a similar form as in various
string theory compactifications. For these potentials, slow roll MSSM inflation
requires no fine tuning of the soft supersymmetry breaking parameters.
|
hep-th astro-ph hep-ph
|
we consider the supergravity origin of the recently proposed mssm inflationary model which relies on the existence of a saddle point along a dimension six flat direction we derive the conditions that the kahler potential has to satisfy for the saddle point to exist irrespective of the hidden sector vevs we show that these conditions are satisfied by a simple class of kahler potentials which we find to have a similar form as in various string theory compactifications for these potentials slow roll mssm inflation requires no fine tuning of the soft supersymmetry breaking parameters
|
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|
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|
706.2356
|
Anonymous quantum communication
|
We present the first protocol for the anonymous transmission of a quantum
state that is information-theoretically secure against an active adversary,
without any assumption on the number of corrupt participants. The anonymity of
the sender and receiver is perfectly preserved, and the privacy of the quantum
state is protected except with exponentially small probability. Even though a
single corrupt participant can cause the protocol to abort, the quantum state
can only be destroyed with exponentially small probability: if the protocol
succeeds, the state is transferred to the receiver and otherwise it remains in
the hands of the sender (provided the receiver is honest).
|
quant-ph
|
we present the first protocol for the anonymous transmission of a quantum state that is informationtheoretically secure against an active adversary without any assumption on the number of corrupt participants the anonymity of the sender and receiver is perfectly preserved and the privacy of the quantum state is protected except with exponentially small probability even though a single corrupt participant can cause the protocol to abort the quantum state can only be destroyed with exponentially small probability if the protocol succeeds the state is transferred to the receiver and otherwise it remains in the hands of the sender provided the receiver is honest
|
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|
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|
706.2357
|
Charm-quark fragmentation with an effective coupling constant
|
We use a recently proposed non-perturbative model, based on an effective
strong coupling constant and free from tunable parameters, to study c-flavoured
hadron production in e+e- annihilation. Charm-quark production is described in
the framework of perturbative fragmentation functions, with NLO coefficient
functions, NLL non-singlet DGLAP evolution and NNLL large-x resummation. We
model hadronization effects by means of the effective coupling constant in the
NNLO approximation and compare our results with experimental data taken at the
Z0 pole and at the Upsilon(4S) resonance. We find that, within the experimental
and theoretical uncertainties, our model is able to give a reasonable
description of D*+-meson spectra from ALEPH for x<1-Lambda/m_c. More serious
discrepancies are instead present when comparing with D and D^* data from BELLE
and CLEO in x-space. Within the errors, our model is nonetheless capable of
reproducing the first ten Mellin moments of all considered data sets. However,
the fairly large theoretical uncertainties call for a full NNLO/NNLL analysis.
|
hep-ph
|
we use a recently proposed nonperturbative model based on an effective strong coupling constant and free from tunable parameters to study cflavoured hadron production in ee annihilation charmquark production is described in the framework of perturbative fragmentation functions with nlo coefficient functions nll nonsinglet dglap evolution and nnll largex resummation we model hadronization effects by means of the effective coupling constant in the nnlo approximation and compare our results with experimental data taken at the z0 pole and at the upsilon4s resonance we find that within the experimental and theoretical uncertainties our model is able to give a reasonable description of dmeson spectra from aleph for x1lambdam_c more serious discrepancies are instead present when comparing with d and d data from belle and cleo in xspace within the errors our model is nonetheless capable of reproducing the first ten mellin moments of all considered data sets however the fairly large theoretical uncertainties call for a full nnlonnll analysis
|
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|
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|
706.2358
|
Measurement of the Lambda_b lifetime using semileptonic decays
|
We report a measurement of the Lambda_b lifetime using a sample corresponding
to 1.3 fb$^{-1}$ of data collected by the D0 experiment in 2002--2006 during
Run II of the Fermilab Tevatron collider. The Lambda_b baryon is reconstructed
via the decay Lambda_b -> mu nu Lambda_c X. Using $4437 \pm 329$ signal
candidates, we measure the Lambda_b lifetime to be $\tau(Lambda_b)$ =
1.290^{+0.119}_{-0.110}(stat) ^{+0.087}_{-0.091} (syst) ps, which is among the
most precise measurements in semileptonic Lambda_b decays. This result is in
good agreement with the world average value.
|
hep-ex
|
we report a measurement of the lambda_b lifetime using a sample corresponding to 13 fb1 of data collected by the d0 experiment in 20022006 during run ii of the fermilab tevatron collider the lambda_b baryon is reconstructed via the decay lambda_b mu nu lambda_c x using 4437 pm 329 signal candidates we measure the lambda_b lifetime to be taulambda_b 12900119_0110stat 0087_0091 syst ps which is among the most precise measurements in semileptonic lambda_b decays this result is in good agreement with the world average value
|
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|
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|
706.2359
|
Electronic compressibility of a graphene bilayer
|
We calculate the electronic compressibility arising from electron-electron
interactions for a graphene bilayer within the Hartree-Fock approximation. We
show that, due to the chiral nature of the particles in this system, the
compressibility is rather different from those of either the two-dimensional
electron gas or ordinary semiconductors. We find that an inherent competition
between the contributions coming from intra-band exchange interactions
(dominant at low densities) and inter-band interactions (dominant at moderate
densities) leads to a non-monotonic behavior of the compressibility as a
function of carrier density.
|
cond-mat.str-el
|
we calculate the electronic compressibility arising from electronelectron interactions for a graphene bilayer within the hartreefock approximation we show that due to the chiral nature of the particles in this system the compressibility is rather different from those of either the twodimensional electron gas or ordinary semiconductors we find that an inherent competition between the contributions coming from intraband exchange interactions dominant at low densities and interband interactions dominant at moderate densities leads to a nonmonotonic behavior of the compressibility as a function of carrier density
|
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|
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|
706.236
|
Magnetorotational collapse of very massive stars to black holes in full
general relativity
|
We perform axisymmetric simulations of the magnetorotational collapse of very
massive stars in full general relativity. Our simulations are applicable to the
collapse of supermassive stars (M > 10^3M_sun) and to very massive Pop III
stars. We model our initial configurations by n=3 polytropes. The ratio of
magnetic to rotational kinetic energy in these configurations is chosen to be
small (1% and 10%). We find that such magnetic fields do not affect the initial
collapse significantly. The core collapses to a black hole, after which black
hole excision is employed to continue the evolution long enough for the hole to
reach a quasi-stationary state. We find that the black hole mass is M_h = 0.95M
and its spin parameter is J_h/M_h^2 = 0.7, with the remaining matter forming a
torus around the black hole. We freeze the spacetime metric ("Cowling
approximation") and continue to follow the evolution of the torus after the
black hole has relaxed to quasi-stationary equilibrium. In the absence of
magnetic fields, the torus settles down following ejection of a small amount of
matter due to shock heating. When magnetic fields are present, the field lines
gradually collimate along the hole's rotation axis. MHD shocks and the MRI
generate MHD turbulence in the torus and stochastic accretion onto the central
black hole. When the magnetic field is strong, a wind is generated in the
torus, and the torus undergoes radial oscillations that drive episodic
accretion onto the hole. These oscillations produce long-wavelength
gravitational waves potentially detectable by LISA. The final state of the
magnetorotational collapse always consists of a central black hole surrounded
by a collimated magnetic field and a hot, thick accretion torus. This system is
a viable candidate for the central engine of a long-soft gamma-ray burst.
|
astro-ph gr-qc
|
we perform axisymmetric simulations of the magnetorotational collapse of very massive stars in full general relativity our simulations are applicable to the collapse of supermassive stars m 103m_sun and to very massive pop iii stars we model our initial configurations by n3 polytropes the ratio of magnetic to rotational kinetic energy in these configurations is chosen to be small 1 and 10 we find that such magnetic fields do not affect the initial collapse significantly the core collapses to a black hole after which black hole excision is employed to continue the evolution long enough for the hole to reach a quasistationary state we find that the black hole mass is m_h 095m and its spin parameter is j_hm_h2 07 with the remaining matter forming a torus around the black hole we freeze the spacetime metric cowling approximation and continue to follow the evolution of the torus after the black hole has relaxed to quasistationary equilibrium in the absence of magnetic fields the torus settles down following ejection of a small amount of matter due to shock heating when magnetic fields are present the field lines gradually collimate along the holes rotation axis mhd shocks and the mri generate mhd turbulence in the torus and stochastic accretion onto the central black hole when the magnetic field is strong a wind is generated in the torus and the torus undergoes radial oscillations that drive episodic accretion onto the hole these oscillations produce longwavelength gravitational waves potentially detectable by lisa the final state of the magnetorotational collapse always consists of a central black hole surrounded by a collimated magnetic field and a hot thick accretion torus this system is a viable candidate for the central engine of a longsoft gammaray burst
|
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|
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|
706.2361
|
A Parallactic Distance of 389 +24/-21 parsecs to the Orion Nebula
Cluster from Very Long Baseline Array Observations
|
We determine the parallax and proper motion of the flaring, non-thermal radio
star GMR A, a member of the Orion Nebula Cluster, using Very Long Baseline
Array observations. Based on the parallax, we measure a distance of 389 +24/-21
parsecs to the source. Our measurement places the Orion Nebula Cluster
considerably closer than the canonical distance of 480 +/- 80 parsecs
determined by Genzel et al. (1981). A change of this magnitude in distance
lowers the luminosities of the stars in the cluster by a factor of ~ 1.5. We
briefly discuss two effects of this change--an increase in the age spread of
the pre-main sequence stars and better agreement between the zero-age
main-sequence and the temperatures and luminosities of massive stars.
|
astro-ph
|
we determine the parallax and proper motion of the flaring nonthermal radio star gmr a a member of the orion nebula cluster using very long baseline array observations based on the parallax we measure a distance of 389 2421 parsecs to the source our measurement places the orion nebula cluster considerably closer than the canonical distance of 480 80 parsecs determined by genzel et al 1981 a change of this magnitude in distance lowers the luminosities of the stars in the cluster by a factor of 15 we briefly discuss two effects of this changean increase in the age spread of the premain sequence stars and better agreement between the zeroage mainsequence and the temperatures and luminosities of massive stars
|
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|
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|
706.2362
|
Magnetization plateaus and sublattice ordering in easy axis Kagome
lattice antiferromagnets
|
We study kagome lattice antiferromagnets where the effects of easy axis
single-ion anisotropy ($D$) dominates over the Heisenberg exchange $J$. For $S
\ge 3/2$, virtual quantum fluctuations help lift the extensive classical
degeneracy. We demonstrate the presence of a one-third magnetization plateau
for a broad range of magnetic fields $J^3/D^2 \lesssim B \lesssim JS$ along the
easy axis. The fully equilibriated system at low temperature on this plateau
develops an unusual {\em nematic} order that breaks sublattice rotation
symmetry but not translation symmetry--however, extremely slow dynamics
associated with this ordering is expected to lead to glassy freezing of the
system on intermediate time-scales.
|
cond-mat.str-el
|
we study kagome lattice antiferromagnets where the effects of easy axis singleion anisotropy d dominates over the heisenberg exchange j for s ge 32 virtual quantum fluctuations help lift the extensive classical degeneracy we demonstrate the presence of a onethird magnetization plateau for a broad range of magnetic fields j3d2 lesssim b lesssim js along the easy axis the fully equilibriated system at low temperature on this plateau develops an unusual em nematic order that breaks sublattice rotation symmetry but not translation symmetryhowever extremely slow dynamics associated with this ordering is expected to lead to glassy freezing of the system on intermediate timescales
|
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|
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|
706.2363
|
Dying Dyons Don't Count
|
The dyonic 1/4-BPS states in 4D string theory with N=4 spacetime
supersymmetry are counted by a Siegel modular form. The pole structure of the
modular form leads to a contour dependence in the counting formula obscuring
its duality invariance. We exhibit the relation between this ambiguity and the
(dis-)appearance of bound states of 1/2-BPS configurations. Using this insight
we propose a precise moduli-dependent contour prescription for the counting
formula. We then show that the degeneracies are duality-invariant and are
correctly adjusted at the walls of marginal stability to account for the
(dis-)appearance of the two-centered bound states. Especially, for large black
holes none of these bound states exists at the attractor point and none of
these ambiguous poles contributes to the counting formula. Using this fact we
also propose a second, moduli-independent contour which counts the "immortal
dyons" that are stable everywhere.
|
hep-th
|
the dyonic 14bps states in 4d string theory with n4 spacetime supersymmetry are counted by a siegel modular form the pole structure of the modular form leads to a contour dependence in the counting formula obscuring its duality invariance we exhibit the relation between this ambiguity and the disappearance of bound states of 12bps configurations using this insight we propose a precise modulidependent contour prescription for the counting formula we then show that the degeneracies are dualityinvariant and are correctly adjusted at the walls of marginal stability to account for the disappearance of the twocentered bound states especially for large black holes none of these bound states exists at the attractor point and none of these ambiguous poles contributes to the counting formula using this fact we also propose a second moduliindependent contour which counts the immortal dyons that are stable everywhere
|
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|
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|
706.2364
|
Super Star Cluster NGC1705-1: A Local Analogue to the Birthsite of
Long-duration Gamma-ray Bursts
|
Recent observations suggest that global properties of the host galaxies for
long-duration gamma-ray bursts (GRBs) are particularly well-suited for creating
the massive star progenitors of these GRBs. Motivated by the hypothesis that
massive young star clusters located in metal-poor, low-metallicity galaxies are
a natural birthsite for GRB progenitors, we present a comparison study of the
ISM properties along the sightline toward the super star cluster, NGC1705-1,
and those in distant GRB hosts. Using the same set of metal transitions in the
UV and applying known ISM structures in NGC1705, we find that NGC1705-1
resembles distant GRB host galaxies in its high neutral gas column, low
molecular gas fraction, low metallicity, alpha-element enhancement,and low dust
depletion. The lack of molecular gas is due to the enhanced UV radiation field
in the starburst environment, consistent with the expectations for GRB
progenitors. In addition, the known presence of dense neutral gas clouds at
r<500 pc from NGC1705-1 provides a natural reservoir of C^+, Si^+, and Fe^+
ions that may be subsequently excited by the afterglow UV radiation field to
produce excited lines commonly seen in GRB host ISM. We further argue that the
apparent offset in the velocity profiles of low- and high-ionization
transitions from absorption-line observations alone already offers important
clues for related starburst episodes in GRB host galaxies. Our study shows that
a statistical comparison between the ISM around star clusters and high-redshift
GRB progenitors is important for identifying the key physical parameters that
facilitate the formation of GRBs.
|
astro-ph
|
recent observations suggest that global properties of the host galaxies for longduration gammaray bursts grbs are particularly wellsuited for creating the massive star progenitors of these grbs motivated by the hypothesis that massive young star clusters located in metalpoor lowmetallicity galaxies are a natural birthsite for grb progenitors we present a comparison study of the ism properties along the sightline toward the super star cluster ngc17051 and those in distant grb hosts using the same set of metal transitions in the uv and applying known ism structures in ngc1705 we find that ngc17051 resembles distant grb host galaxies in its high neutral gas column low molecular gas fraction low metallicity alphaelement enhancementand low dust depletion the lack of molecular gas is due to the enhanced uv radiation field in the starburst environment consistent with the expectations for grb progenitors in addition the known presence of dense neutral gas clouds at r500 pc from ngc17051 provides a natural reservoir of c si and fe ions that may be subsequently excited by the afterglow uv radiation field to produce excited lines commonly seen in grb host ism we further argue that the apparent offset in the velocity profiles of low and highionization transitions from absorptionline observations alone already offers important clues for related starburst episodes in grb host galaxies our study shows that a statistical comparison between the ism around star clusters and highredshift grb progenitors is important for identifying the key physical parameters that facilitate the formation of grbs
|
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|
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|
706.2365
|
Chain motifs: The tails and handles of complex networks
|
Great part of the interest in complex networks has been motivated by the
presence of structured, frequently non-uniform, connectivity. Because diverse
connectivity patterns tend to result in distinct network dynamics, and also
because they provide the means to identify and classify several types of
complex networks, it becomes important to obtain meaningful measurements of the
local network topology. In addition to traditional features such as the node
degree, clustering coefficient and shortest path, motifs have been introduced
in the literature in order to provide complementary description of the networks
connectivity. The current work proposes a new type of motifs, namely chains of
nodes, namely sequences of connected nodes with degree two. These chains have
been subdivided into cords, tails, rings and handles, depending on the type of
their extremities (e.g. open or connected). A theoretical analysis of the
density of such motifs in random and scale free networks is described, and an
algorithm for identifying those motifs in general networks is presented. The
potential of considering chains for network characterization has been
illustrated with respect to five categories of real-world networks including 16
cases. Several interesting findings were obtained, including the fact that
several chains were observed in the real-world networks, especially the WWW,
books, and power-grid. The possibility of chains resulting from incompletely
sampled networks is also investigated.
|
cond-mat.dis-nn cond-mat.stat-mech
|
great part of the interest in complex networks has been motivated by the presence of structured frequently nonuniform connectivity because diverse connectivity patterns tend to result in distinct network dynamics and also because they provide the means to identify and classify several types of complex networks it becomes important to obtain meaningful measurements of the local network topology in addition to traditional features such as the node degree clustering coefficient and shortest path motifs have been introduced in the literature in order to provide complementary description of the networks connectivity the current work proposes a new type of motifs namely chains of nodes namely sequences of connected nodes with degree two these chains have been subdivided into cords tails rings and handles depending on the type of their extremities eg open or connected a theoretical analysis of the density of such motifs in random and scale free networks is described and an algorithm for identifying those motifs in general networks is presented the potential of considering chains for network characterization has been illustrated with respect to five categories of realworld networks including 16 cases several interesting findings were obtained including the fact that several chains were observed in the realworld networks especially the www books and powergrid the possibility of chains resulting from incompletely sampled networks is also investigated
|
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|
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|
706.2366
|
Theoretical study of ferroelectric potassium nitrate
|
We present a detailed study of the structural behavior and polarization
reversal mechanism in phase III of KNO$_3$, an unusual ferroelectric material
in which the nitrate groups rotate during polarization reversal. This material
was one of several studied in a previous work [O. Di\'eguez and D. Vanderbilt,
Phys. Rev. Lett. {\bf 96}, 056401 (2006)] where methods were described for
computing curves of energy versus electric polarization. In the present work we
extend and systematize the previous first-principles calculations on KNO$_3$,
and analyze in detail a two-parameter model in which the energy of the system
is written as a low-order expansion in the polarization and the nitrate group
orientation. We confirm that this model reproduces the first-principles results
for KNO$_3$ very well and construct its parameter-space phase diagram,
describing regions where unusual triple-well potentials appear. We also present
first-principles calculations of KNO$_3$ under pressure, finding that its
energy-versus-polarization curves change character by developing a
first-derivative discontinuity at zero polarization.
|
cond-mat.mtrl-sci
|
we present a detailed study of the structural behavior and polarization reversal mechanism in phase iii of kno_3 an unusual ferroelectric material in which the nitrate groups rotate during polarization reversal this material was one of several studied in a previous work o dieguez and d vanderbilt phys rev lett bf 96 056401 2006 where methods were described for computing curves of energy versus electric polarization in the present work we extend and systematize the previous firstprinciples calculations on kno_3 and analyze in detail a twoparameter model in which the energy of the system is written as a loworder expansion in the polarization and the nitrate group orientation we confirm that this model reproduces the firstprinciples results for kno_3 very well and construct its parameterspace phase diagram describing regions where unusual triplewell potentials appear we also present firstprinciples calculations of kno_3 under pressure finding that its energyversuspolarization curves change character by developing a firstderivative discontinuity at zero polarization
|
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|
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|
706.2367
|
Weyssenhoff fluid dynamics in general relativity using a 1+3 covariant
approach
|
The Weyssenhoff fluid is a perfect fluid with spin where the spin of the
matter fields is the source of torsion in an Einstein-Cartan framework. Obukhov
and Korotky showed that this fluid can be described as an effective fluid with
spin in general relativity. A dynamical analysis of such a fluid is performed
in a gauge invariant manner using the 1+3 covariant approach. This yields the
propagation and constraint equations for the set of dynamical variables. A
verification of these equations is performed for the special case of
irrotational flow with zero peculiar acceleration by evolving the constraints.
|
gr-qc astro-ph
|
the weyssenhoff fluid is a perfect fluid with spin where the spin of the matter fields is the source of torsion in an einsteincartan framework obukhov and korotky showed that this fluid can be described as an effective fluid with spin in general relativity a dynamical analysis of such a fluid is performed in a gauge invariant manner using the 13 covariant approach this yields the propagation and constraint equations for the set of dynamical variables a verification of these equations is performed for the special case of irrotational flow with zero peculiar acceleration by evolving the constraints
|
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|
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|
706.2368
|
A Note on Carleman's Inequality
|
We study a weighted version of Carleman's inequality via Carleman's original
approach. As an application of our result, we prove a conjecture of Bennett.
|
math.CA
|
we study a weighted version of carlemans inequality via carlemans original approach as an application of our result we prove a conjecture of bennett
|
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|
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|
706.2369
|
Surface Operators and Knot Homologies
|
Topological gauge theories in four dimensions which admit surface operators
provide a natural framework for realizing homological knot invariants. Every
such theory leads to an action of the braid group on branes on the
corresponding moduli space. This action plays a key role in the construction of
homological knot invariants. We illustrate the general construction with
examples based on surface operators in N=2 and N=4 twisted gauge theories which
lead to a categorification of the Alexander polynomial, the equivariant knot
signature, and certain analogs of the Casson invariant.
This paper is based on a lecture delivered at the International Congress on
Mathematical Physics 2006, Rio de Janeiro, and at the RTN Workshop 2006,
Napoli.
|
hep-th math.GT math.QA
|
topological gauge theories in four dimensions which admit surface operators provide a natural framework for realizing homological knot invariants every such theory leads to an action of the braid group on branes on the corresponding moduli space this action plays a key role in the construction of homological knot invariants we illustrate the general construction with examples based on surface operators in n2 and n4 twisted gauge theories which lead to a categorification of the alexander polynomial the equivariant knot signature and certain analogs of the casson invariant this paper is based on a lecture delivered at the international congress on mathematical physics 2006 rio de janeiro and at the rtn workshop 2006 napoli
|
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|
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|
706.237
|
Strange attractors in periodically-kicked degenerate Hopf bifurcations
|
We prove that spiral sinks (stable foci of vector fields) can be transformed
into strange attractors exhibiting sustained, observable chaos if subjected to
periodic pulsatile forcing. We show that this phenomenon occurs in the context
of periodically-kicked degenerate supercritical Hopf bifurcations. The results
and their proofs make use of a new multi-parameter version of the theory of
rank one maps developed by Wang and Young.
|
math.DS math-ph math.MP
|
we prove that spiral sinks stable foci of vector fields can be transformed into strange attractors exhibiting sustained observable chaos if subjected to periodic pulsatile forcing we show that this phenomenon occurs in the context of periodicallykicked degenerate supercritical hopf bifurcations the results and their proofs make use of a new multiparameter version of the theory of rank one maps developed by wang and young
|
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|
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|
706.2371
|
The rotating Morse potential model for diatomic molecules in the
tridiagonal J-matrix representation: I. Bound states
|
This is the first in a series of articles in which we study the rotating
Morse potential model for diatomic molecules in the tridiagonal J-matrix
representation. Here, we compute the bound states energy spectrum by
diagonalizing the finite dimensional Hamiltonian matrix of H2, LiH, HCl and CO
molecules for arbitrary angular momentum. The calculation was performed using
the J-matrix basis that supports a tridiagonal matrix representation for the
reference Hamiltonian. Our results for these diatomic molecules have been
compared with available numerical data satisfactorily. The proposed method is
handy, very efficient, and it enhances accuracy by combining analytic power
with a convergent and stable numerical technique.
|
physics.chem-ph physics.atom-ph
|
this is the first in a series of articles in which we study the rotating morse potential model for diatomic molecules in the tridiagonal jmatrix representation here we compute the bound states energy spectrum by diagonalizing the finite dimensional hamiltonian matrix of h2 lih hcl and co molecules for arbitrary angular momentum the calculation was performed using the jmatrix basis that supports a tridiagonal matrix representation for the reference hamiltonian our results for these diatomic molecules have been compared with available numerical data satisfactorily the proposed method is handy very efficient and it enhances accuracy by combining analytic power with a convergent and stable numerical technique
|
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|
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|
706.2372
|
Prym varieties and applications
|
The classical definition of Prym varieties deals with the unramified covers
of curves. The aim of the present paper is to give explicit algebraic
descriptions of the Prym varieties associated to ramified double covers of
algebraic curves. We make a careful study of the connection with the concept of
algebraic completely integrable systems and we apply the methods to some
problems of Mathematical Physics.
|
math.AG math-ph math.MP
|
the classical definition of prym varieties deals with the unramified covers of curves the aim of the present paper is to give explicit algebraic descriptions of the prym varieties associated to ramified double covers of algebraic curves we make a careful study of the connection with the concept of algebraic completely integrable systems and we apply the methods to some problems of mathematical physics
|
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|
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|
706.2373
|
A widely tunable parametric amplifier based on a SQUID array resonator
|
We create a Josephson parametric amplifier from a transmission line resonator
whose inner conductor is made from a series SQUID array. By changing the
magnetic flux through the SQUID loops, we are able to adjust the circuit's
resonance frequency and, consenquently, the center of the amplified band,
between 4 and 7.8 GHz. We observe that the amplifier has gains as large as 28
dB and infer that it adds less than twice the input vacuum noise.
|
cond-mat.supr-con cond-mat.mes-hall
|
we create a josephson parametric amplifier from a transmission line resonator whose inner conductor is made from a series squid array by changing the magnetic flux through the squid loops we are able to adjust the circuits resonance frequency and consenquently the center of the amplified band between 4 and 78 ghz we observe that the amplifier has gains as large as 28 db and infer that it adds less than twice the input vacuum noise
|
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|
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|
706.2374
|
Line and Mean Opacities for Ultracool Dwarfs and Extrasolar Planets
|
Opacities and chemical abundance data are crucial ingredients of ultracool
dwarf and extrasolar giant planet atmosphere models. We report here on the
detailed sources of molecular opacity data employed by our group for this
application. We also present tables of Rosseland and Planck mean opacities
which are of use in some studies of the atmospheres, interiors, and evolution
of planets and brown dwarfs. For the tables presented here we have included the
opacities of important atomic and molecular species, including the alkali
elements, pressure induced absorption by hydrogen, and other significant
opacity sources but neglect opacity from condensates. We report for each
species how we have assembled molecular line data from a combination of public
databases, laboratory data that is not yet in the public databases, and our own
numerical calculations. We combine these opacities with abundances computed
from a chemical equilibrium model using recently revised solar abundances to
compute mean opacities. The chemical equilibrium calculation accounts for the
settling of condensates in a gravitational field, and is applicable to
ultracool dwarf and extrasolar planetary atmospheres, but not circumstellar
disks. We find that the inclusion of alkali atomic opacity substantially
increases the mean opacities over those currently in the literature at
densities relevant to the atmospheres and interiors of giant planets and brown
dwarfs. We provide our opacity tables for public use and discuss their
limitations.
|
astro-ph
|
opacities and chemical abundance data are crucial ingredients of ultracool dwarf and extrasolar giant planet atmosphere models we report here on the detailed sources of molecular opacity data employed by our group for this application we also present tables of rosseland and planck mean opacities which are of use in some studies of the atmospheres interiors and evolution of planets and brown dwarfs for the tables presented here we have included the opacities of important atomic and molecular species including the alkali elements pressure induced absorption by hydrogen and other significant opacity sources but neglect opacity from condensates we report for each species how we have assembled molecular line data from a combination of public databases laboratory data that is not yet in the public databases and our own numerical calculations we combine these opacities with abundances computed from a chemical equilibrium model using recently revised solar abundances to compute mean opacities the chemical equilibrium calculation accounts for the settling of condensates in a gravitational field and is applicable to ultracool dwarf and extrasolar planetary atmospheres but not circumstellar disks we find that the inclusion of alkali atomic opacity substantially increases the mean opacities over those currently in the literature at densities relevant to the atmospheres and interiors of giant planets and brown dwarfs we provide our opacity tables for public use and discuss their limitations
|
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|
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|
706.2375
|
Connecting LHC, ILC, and Quintessence
|
If the cold dark matter consists of weakly interacting massive particles
(WIMPs), anticipated measurements of the WIMP properties at the Large Hadron
Collider (LHC) and the International Linear Collider (ILC) will provide an
unprecedented experimental probe of cosmology at temperatures of order 1 GeV.
It is worth emphasizing that the expected outcome of these tests may or may not
be consistent with the picture of standard cosmology. For example, in
kination-dominated quintessence models of dark energy, the dark matter relic
abundance can be significantly enhanced compared to that obtained from freeze
out in a radiation-dominated universe. Collider measurements then will
simultaneously probe both dark matter and dark energy. In this article, we
investigate the precision to which the LHC and ILC can determine the dark
matter and dark energy parameters under those circumstances. We use an
illustrative set of four benchmark points in minimal supergravity in analogy
with the four LCC benchmark points. The precision achievable together at the
LHC and ILC is sufficient to discover kination-dominated quintessence, under
the assumption that the WIMPs are the only dark matter component. The LHC and
ILC can thus play important roles as alternative probes of both dark matter and
dark energy.
|
hep-ph astro-ph hep-th
|
if the cold dark matter consists of weakly interacting massive particles wimps anticipated measurements of the wimp properties at the large hadron collider lhc and the international linear collider ilc will provide an unprecedented experimental probe of cosmology at temperatures of order 1 gev it is worth emphasizing that the expected outcome of these tests may or may not be consistent with the picture of standard cosmology for example in kinationdominated quintessence models of dark energy the dark matter relic abundance can be significantly enhanced compared to that obtained from freeze out in a radiationdominated universe collider measurements then will simultaneously probe both dark matter and dark energy in this article we investigate the precision to which the lhc and ilc can determine the dark matter and dark energy parameters under those circumstances we use an illustrative set of four benchmark points in minimal supergravity in analogy with the four lcc benchmark points the precision achievable together at the lhc and ilc is sufficient to discover kinationdominated quintessence under the assumption that the wimps are the only dark matter component the lhc and ilc can thus play important roles as alternative probes of both dark matter and dark energy
|
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|
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|
706.2376
|
Dynamical Masses for Pre-Main Sequence Stars: A Preliminary Physical
Orbit for V773 Tau A
|
We report on interferometric and radial-velocity observations of the
double-lined 51-d period binary (A) component of the quadruple pre-main
sequence (PMS) system V773 Tau. With these observations we have estimated
preliminary visual and physical orbits of the V773 Tau A subsystem. Among other
parameters, our orbit model includes an inclination of 66.0 $\pm$ 2.4 deg, and
allows us to infer the component dynamical masses and system distance. In
particular we find component masses of 1.54 $\pm$ 0.14 and 1.332 $\pm$ 0.097
M$_{\sun}$ for the Aa (primary) and Ab (secondary) components respectively.
Our modeling of the subsystem component spectral energy distributions finds
temperatures and luminosities consistent with previous studies, and coupled
with the component mass estimates allows for comparison with PMS stellar models
in the intermediate-mass range. We compare V773 Tau A component properties with
several popular solar-composition models for intermediate-mass PMS stars. All
models predict masses consistent to within 2-sigma of the dynamically
determined values, though some models predict values that are more consistent
than others.
|
astro-ph
|
we report on interferometric and radialvelocity observations of the doublelined 51d period binary a component of the quadruple premain sequence pms system v773 tau with these observations we have estimated preliminary visual and physical orbits of the v773 tau a subsystem among other parameters our orbit model includes an inclination of 660 pm 24 deg and allows us to infer the component dynamical masses and system distance in particular we find component masses of 154 pm 014 and 1332 pm 0097 m_sun for the aa primary and ab secondary components respectively our modeling of the subsystem component spectral energy distributions finds temperatures and luminosities consistent with previous studies and coupled with the component mass estimates allows for comparison with pms stellar models in the intermediatemass range we compare v773 tau a component properties with several popular solarcomposition models for intermediatemass pms stars all models predict masses consistent to within 2sigma of the dynamically determined values though some models predict values that are more consistent than others
|
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|
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|
706.2377
|
Collisional parton energy loss in a finite size QCD medium revisited:
Off mass-shell effects
|
We study the collisional energy loss mechanism for particles produced off
mass-shell in a finite size QCD medium. The off mass-shell effects introduced
are to consider particles produced in wave packets instead of plane waves and
the length scale associated to an in-medium particles' life-time. We show that
these effects reduce the energy loss as compared to the case when the particles
are described as freely propagating from the source. The reduction of the
energy loss is stronger as this scale becomes of the order or smaller than the
medium size. We discuss possible consequences of the result on the description
of the energy loss process in the parton recombination scenario.
|
hep-ph
|
we study the collisional energy loss mechanism for particles produced off massshell in a finite size qcd medium the off massshell effects introduced are to consider particles produced in wave packets instead of plane waves and the length scale associated to an inmedium particles lifetime we show that these effects reduce the energy loss as compared to the case when the particles are described as freely propagating from the source the reduction of the energy loss is stronger as this scale becomes of the order or smaller than the medium size we discuss possible consequences of the result on the description of the energy loss process in the parton recombination scenario
|
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|
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|
706.2378
|
Geysers in the Lagoon: new Herbig-Haro objects in M8
|
Aims: We search for direct evidence of ongoing star formation by accretion in
the Lagoon Nebula (M8), using optical wide-field narrow-band imaging obtained
at La Silla Observatory.
Methods: We examine [SII] and Halpha images for line-emission features that
could be interpreted as signatures of outflow activity of the exciting sources.
Results: We discover five new Herbig-Haro objects, study in detail their
morphology and attempt to identify their potential driving sources among the
population of T Tauri stars and embedded sources in the surroundings.
Conclusions: The results reported here conclusively demonstrate the existence
of very young stars going through the accreting phase in the M8 region.
|
astro-ph
|
aims we search for direct evidence of ongoing star formation by accretion in the lagoon nebula m8 using optical widefield narrowband imaging obtained at la silla observatory methods we examine sii and halpha images for lineemission features that could be interpreted as signatures of outflow activity of the exciting sources results we discover five new herbigharo objects study in detail their morphology and attempt to identify their potential driving sources among the population of t tauri stars and embedded sources in the surroundings conclusions the results reported here conclusively demonstrate the existence of very young stars going through the accreting phase in the m8 region
|
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|
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|
706.2379
|
The Derivative Expansion of the Effective Action and the Renormalization
Group Equation
|
The perturbative evaluation of the effective action can be expanded in powers
of derivatives of the external field. We apply the renormalization group
equation to the term in the effective action that is second order in the
derivatives of the external field and all orders in a constant external field,
considering both massless scalar $\phi_4^4$ model and massless scalar
electrodynamics. A so-called ``on shell'' renormalization scheme permits one to
express this ``kinetic term'' for the scalar field entirely in terms of the
renormalization group functions appropriate for this scheme. These
renormalization group functions can be related to those associated with minimal
subtraction.
|
hep-th
|
the perturbative evaluation of the effective action can be expanded in powers of derivatives of the external field we apply the renormalization group equation to the term in the effective action that is second order in the derivatives of the external field and all orders in a constant external field considering both massless scalar phi_44 model and massless scalar electrodynamics a socalled on shell renormalization scheme permits one to express this kinetic term for the scalar field entirely in terms of the renormalization group functions appropriate for this scheme these renormalization group functions can be related to those associated with minimal subtraction
|
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|
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|
706.238
|
Tightening of knots in proteins
|
We perform theoretical studies of stretching of 20 proteins with knots within
a coarse grained model. The knot's ends are found to jump to well defined
sequential locations that are associated with sharp turns whereas in
homopolymers they diffuse around and eventually slide off. The waiting times of
the jumps are increasingly stochastic as the temperature is raised. Larger
knots do not return to their native locations when a protein is released after
stretching.
|
q-bio.BM cond-mat.soft
|
we perform theoretical studies of stretching of 20 proteins with knots within a coarse grained model the knots ends are found to jump to well defined sequential locations that are associated with sharp turns whereas in homopolymers they diffuse around and eventually slide off the waiting times of the jumps are increasingly stochastic as the temperature is raised larger knots do not return to their native locations when a protein is released after stretching
|
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|
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|
706.2381
|
Koszul duality in deformation quantization, I
|
Let $\alpha$ be a polynomial Poisson bivector on a finite-dimensional vector
space $V$ over $\mathbb{C}$. Then Kontsevich [K97] gives a formula for a
quantization $f\star g$ of the algebra $S(V)^*$. We give a construction of an
algebra with the PBW property defined from $\alpha$ by generators and
relations. Namely, we define an algebra as the quotient of the free tensor
algebra $T(V^*)$ by relations $x_i\otimes x_j-x_j\otimes x_i=R_{ij}(\hbar)$
where $R_{ij}(\hbar)\in T(V^*)\otimes\hbar \mathbb{C}[[\hbar]]$, $R_{ij}=\hbar
\Sym(\alpha_{ij})+\mathcal{O}(\hbar^2)$, with one relation for each pair of
$i,j=1...\dim V$. We prove that the constructed algebra obeys the PBW property,
and this is a generalization of the Poincar\'{e}-Birkhoff-Witt theorem. In the
case of a linear Poisson structure we get the PBW theorem itself, and for a
quadratic Poisson structure we get an object closely related to a quantum
$R$-matrix on $V$. At the same time we get a free resolution of the deformed
algebra (for an arbitrary $\alpha$).
The construction of this PBW algebra is rather simple, as well as the proof
of the PBW property. The major efforts should be undertaken to prove the
conjecture that in this way we get an algebra isomorphic to the Kontsevich
star-algebra.
|
math.QA
|
let alpha be a polynomial poisson bivector on a finitedimensional vector space v over mathbbc then kontsevich k97 gives a formula for a quantization fstar g of the algebra sv we give a construction of an algebra with the pbw property defined from alpha by generators and relations namely we define an algebra as the quotient of the free tensor algebra tv by relations x_iotimes x_jx_jotimes x_ir_ijhbar where r_ijhbarin tvotimeshbar mathbbchbar r_ijhbar symalpha_ijmathcalohbar2 with one relation for each pair of ij1dim v we prove that the constructed algebra obeys the pbw property and this is a generalization of the poincarebirkhoffwitt theorem in the case of a linear poisson structure we get the pbw theorem itself and for a quadratic poisson structure we get an object closely related to a quantum rmatrix on v at the same time we get a free resolution of the deformed algebra for an arbitrary alpha the construction of this pbw algebra is rather simple as well as the proof of the pbw property the major efforts should be undertaken to prove the conjecture that in this way we get an algebra isomorphic to the kontsevich staralgebra
|
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|
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|
706.2382
|
A characteristic observable signature of preferred frame effects in
relativistic binary pulsars
|
In this paper we develop a consistent, phenomenological methodology to
measure preferred-frame effects (PFEs) in binary pulsars that exhibit a high
rate of periastron advance. We show that in these systems the existence of a
preferred frame for gravity leads to an observable characteristic `signature'
in the timing data, which uniquely identifies this effect. We expand the
standard Damour-Deruelle timing formula to incorporate this `signature' and
show how this new PFE timing model can be used to either measure or constrain
the parameters related to a violation of the local Lorentz invariance of
gravity in the strong internal fields of neutron stars. In particular, we
demonstrate that in the presence of PFEs we expect a set of the new timing
parameters to have a unique relationship that can be measured and tested
incontrovertibly. This new methodology is applied to the Double Pulsar, which
turns out to be the ideal test system for this kind of experiments.The
currently available dataset allows us only to study the impact of PFEs on the
orbital precession rate, d omega/dt, providing limits that are, at the moment,
clearly less stringent than existing limits on PFE strong-field parameters.
However, simulations show that the constraints improve fast in the coming
years, allowing us to study all new PFE timing parameters and to check for the
unique relationship between them. Finally, we show how a combination of several
suitable systems in a "PFE antenna array", expected to be availabe for instance
with the Square-Kilometre-Array (SKA), provides full sensitivity to possible
violations of local Lorentz invariance in strong gravitational fields in all
directions of the sky. This PFE antenna array may eventually allow us to
determine the direction of a preferred frame should it exist.
|
astro-ph
|
in this paper we develop a consistent phenomenological methodology to measure preferredframe effects pfes in binary pulsars that exhibit a high rate of periastron advance we show that in these systems the existence of a preferred frame for gravity leads to an observable characteristic signature in the timing data which uniquely identifies this effect we expand the standard damourderuelle timing formula to incorporate this signature and show how this new pfe timing model can be used to either measure or constrain the parameters related to a violation of the local lorentz invariance of gravity in the strong internal fields of neutron stars in particular we demonstrate that in the presence of pfes we expect a set of the new timing parameters to have a unique relationship that can be measured and tested incontrovertibly this new methodology is applied to the double pulsar which turns out to be the ideal test system for this kind of experimentsthe currently available dataset allows us only to study the impact of pfes on the orbital precession rate d omegadt providing limits that are at the moment clearly less stringent than existing limits on pfe strongfield parameters however simulations show that the constraints improve fast in the coming years allowing us to study all new pfe timing parameters and to check for the unique relationship between them finally we show how a combination of several suitable systems in a pfe antenna array expected to be availabe for instance with the squarekilometrearray ska provides full sensitivity to possible violations of local lorentz invariance in strong gravitational fields in all directions of the sky this pfe antenna array may eventually allow us to determine the direction of a preferred frame should it exist
|
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|
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|
706.2383
|
Allovalency revisited: an analysis of multisite phosphorylation and
substrate rebinding
|
The utilization of multiple phosphorylation sites in regulating a biological
response is ubiquitous in cell signaling. If each site contributes an
additional, equivalent binding site, then one consequence of an increase in the
number of phosphorylations may be to increase the probability that, upon
disassociation, a ligand immediately rebinds to its receptor. How such effects
may influence cell signaling systems has been less studied. Here, a
self-consistent integral equation formalism for ligand rebinding, in
conjunction with Monte Carlo simulations, is employed to further investigate
the effects of multiple, equivalent binding sites on shaping biological
responses. Multiple regimes that characterize qualitatively different physics
due to the differential prevalence of rebinding effects are predicted.
Calculations suggest that when ligand rebinding contributes significantly to
the dose response, a purely allovalent model can influence the binding curves
nonlinearly. The model also predicts that ligand rebinding in itself appears
insufficient to generative a highly cooperative biological response.
|
q-bio.SC q-bio.MN
|
the utilization of multiple phosphorylation sites in regulating a biological response is ubiquitous in cell signaling if each site contributes an additional equivalent binding site then one consequence of an increase in the number of phosphorylations may be to increase the probability that upon disassociation a ligand immediately rebinds to its receptor how such effects may influence cell signaling systems has been less studied here a selfconsistent integral equation formalism for ligand rebinding in conjunction with monte carlo simulations is employed to further investigate the effects of multiple equivalent binding sites on shaping biological responses multiple regimes that characterize qualitatively different physics due to the differential prevalence of rebinding effects are predicted calculations suggest that when ligand rebinding contributes significantly to the dose response a purely allovalent model can influence the binding curves nonlinearly the model also predicts that ligand rebinding in itself appears insufficient to generative a highly cooperative biological response
|
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|
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|
706.2384
|
Galois theory of iterated endomorphisms
|
Given an abelian algebraic group $A$ over a global field $F$, $\alpha \in
A(F)$, and a prime $\ell$, the set of all preimages of $\alpha$ under some
iterate of $[\ell]$ generates an extension of $F$ that contains all
$\ell$-power torsion points as well as a Kummer-type extension. We analyze the
Galois group of this extension, and for several classes of $A$ we give a simple
characterization of when the Galois group is as large as possible up to
constraints imposed by the endomorphism ring or the Weil pairing. This Galois
group encodes information about the density of primes $\p$ in the ring of
integers of $F$ such that the order of $(\alpha \bmod{\p})$ is prime to $\ell$.
We compute this density in the general case for several classes of $A$,
including elliptic curves and one-dimensional tori. For example, if $F$ is a
number field, $A/F$ is an elliptic curve with surjective 2-adic representation
and $\alpha \in A(F)$ with $\alpha \not\in 2A(F(A[4]))$, then the density of
$\mathfrak{p}$ with ($\alpha \bmod{\p}$) having odd order is 11/21.
|
math.NT
|
given an abelian algebraic group a over a global field f alpha in af and a prime ell the set of all preimages of alpha under some iterate of ell generates an extension of f that contains all ellpower torsion points as well as a kummertype extension we analyze the galois group of this extension and for several classes of a we give a simple characterization of when the galois group is as large as possible up to constraints imposed by the endomorphism ring or the weil pairing this galois group encodes information about the density of primes p in the ring of integers of f such that the order of alpha bmodp is prime to ell we compute this density in the general case for several classes of a including elliptic curves and onedimensional tori for example if f is a number field af is an elliptic curve with surjective 2adic representation and alpha in af with alpha notin 2afa4 then the density of mathfrakp with alpha bmodp having odd order is 1121
|
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|
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|
706.2385
|
Dynamical ultrafast all-optical switching of planar GaAs/AlAs photonic
microcavities
|
The authors study the ultrafast switching-on and -off of planar GaAs/AlAs
microcavities. Up to 0.8% refractive index changes are achieved by optically
exciting free carriers at 1720 nm and a pulse energy of 1.8 micro Joules. The
cavity resonance is dynamically tracked by measuring reflectivity versus time
delay with tunable laser pulses, and is found to shift by as much as 3.3
linewidths within a few picoseconds. The switching-off occurs with a decay time
of around 50 ps. The authors derive the dynamic behavior of the carrier density
and of the complex refractive index. They propose that the inferred 10 GHz
switching rate may be tenfold improved by optimized sample growth.
|
physics.optics
|
the authors study the ultrafast switchingon and off of planar gaasalas microcavities up to 08 refractive index changes are achieved by optically exciting free carriers at 1720 nm and a pulse energy of 18 micro joules the cavity resonance is dynamically tracked by measuring reflectivity versus time delay with tunable laser pulses and is found to shift by as much as 33 linewidths within a few picoseconds the switchingoff occurs with a decay time of around 50 ps the authors derive the dynamic behavior of the carrier density and of the complex refractive index they propose that the inferred 10 ghz switching rate may be tenfold improved by optimized sample growth
|
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|
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|
706.2386
|
The Scattering Polarization of the Sr I 4607 \AA Line at the Diffraction
Limit Resolution of a 1-m Telescope
|
One of the greatest challenges in solar and stellar physics in coming years
will be to observe the Second Solar Spectrum with a spatial resolution
significantly better than 1 arcsec. This type of scattering polarization
observations would probably allow us to discover hitherto unknown aspects of
the Sun's hidden magnetism. Here we report on some theoretical predictions for
the photospheric line of Sr I at 4607 \AA, which we have obtained by solving
the three-dimensional (3D) radiative transfer problem of scattering line
polarization in a realistic hydrodynamical model of the solar photosphere. We
have taken into account not only the anisotropy of the radiation field in the
3D medium and the Hanle effect of a tangled magnetic field, but also the
symmetry breaking effects caused by the horizontal atmospheric inhomogeneities
produced by the solar surface convection. Interestingly, the Q/I and U/I linear
polarization signals of the emergent spectral line radiation have sizable
values and fluctuations, even at the very center of the solar disk where we
meet the forward scattering case. The ensuing small-scale patterns in Q/I and
U/I turn out to be sensitive to the assumed magnetic field model, and are of
great diagnostic value. We argue that it should be possible to observe them
with the help of a 1-m telescope equipped with adaptive optics and a suitable
polarimeter.
|
astro-ph
|
one of the greatest challenges in solar and stellar physics in coming years will be to observe the second solar spectrum with a spatial resolution significantly better than 1 arcsec this type of scattering polarization observations would probably allow us to discover hitherto unknown aspects of the suns hidden magnetism here we report on some theoretical predictions for the photospheric line of sr i at 4607 aa which we have obtained by solving the threedimensional 3d radiative transfer problem of scattering line polarization in a realistic hydrodynamical model of the solar photosphere we have taken into account not only the anisotropy of the radiation field in the 3d medium and the hanle effect of a tangled magnetic field but also the symmetry breaking effects caused by the horizontal atmospheric inhomogeneities produced by the solar surface convection interestingly the qi and ui linear polarization signals of the emergent spectral line radiation have sizable values and fluctuations even at the very center of the solar disk where we meet the forward scattering case the ensuing smallscale patterns in qi and ui turn out to be sensitive to the assumed magnetic field model and are of great diagnostic value we argue that it should be possible to observe them with the help of a 1m telescope equipped with adaptive optics and a suitable polarimeter
|
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|
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|
706.2387
|
Fermi surface of CeIn3 above the Neel critical field
|
We report measurements of the de Haas-van Alphen effect in CeIn3 in magnetic
fields extending to ~90 T, well above the Ne'el critical field of Hc ~61 T. The
unreconstructed Fermi surface a-sheet is observed in the high magnetic field
polarized paramagnetic limit, but with its effective mass and Fermi surface
volume strongly reduced in size compared to that observed in the low magnetic
field paramagnetic regime under pressure. The spheroidal topology of this sheet
provides an ideal realization of the transformation from a `large Fermi
surface' accommodating f-electrons to a `small Fermi surface' when the
f-electron moments become polarized.
|
cond-mat.str-el cond-mat.mtrl-sci
|
we report measurements of the de haasvan alphen effect in cein3 in magnetic fields extending to 90 t well above the neel critical field of hc 61 t the unreconstructed fermi surface asheet is observed in the high magnetic field polarized paramagnetic limit but with its effective mass and fermi surface volume strongly reduced in size compared to that observed in the low magnetic field paramagnetic regime under pressure the spheroidal topology of this sheet provides an ideal realization of the transformation from a large fermi surface accommodating felectrons to a small fermi surface when the felectron moments become polarized
|
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|
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|
706.2388
|
Longitudinal Spin Measurements with Inclusive Hadrons in Polarized p+p
Collisions at 200 GeV
|
We present measurements of the double longitudinal spin asymmetries for
inclusive pi0 and pi+(-) production in polarized p+p collisions at sqrt(s) =
200 GeV at mid-rapidity with the STAR detector from the 2005 RHIC run. These
measurements are used to access Delta G/G, the gluon polarization in the
proton. The observed unpolarized inclusive cross sections show good agreement
with NLO pQCD calculations. The double longitudinal spin asymmetries are
compared to NLO pQCD calculations based on different assumptions for the gluon
polarization in the nucleon to provide constraints on Delta G/G. At the present
level of statistics the measured asymmetries disfavor a large positive gluon
polarization, but cannot yet distinguish between other scenarios.
|
hep-ex
|
we present measurements of the double longitudinal spin asymmetries for inclusive pi0 and pi production in polarized pp collisions at sqrts 200 gev at midrapidity with the star detector from the 2005 rhic run these measurements are used to access delta gg the gluon polarization in the proton the observed unpolarized inclusive cross sections show good agreement with nlo pqcd calculations the double longitudinal spin asymmetries are compared to nlo pqcd calculations based on different assumptions for the gluon polarization in the nucleon to provide constraints on delta gg at the present level of statistics the measured asymmetries disfavor a large positive gluon polarization but cannot yet distinguish between other scenarios
|
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|
[-0.03473224331433552, 0.22649933566987915, -0.15123712039452844, 0.1500939166372908, -0.014268808016952659, -0.117749141069258, -0.019355822874266387, 0.37376216245840105, -0.17470576216666295, -0.23400021916521446, -0.10747393921961443, -0.3851462675125471, 0.11967081252285945, 0.16877526254601044, 0.12797006893171264, 0.09351906149199099, 0.141232345402906, -0.037812071858362675, -0.06088742361420633, -0.20276326085409632, 0.27797840510486693, 0.06667562777874991, 0.24307339181957235, 0.20469579055705772, 0.038220423196824935, 0.09284014674735122, -0.08268665966534172, -0.05900796070324889, -0.15320807763678854, 0.00932116570584185, 0.32051000028981697, -0.007831668269708254, 0.02228204087753381, -0.3875199520760881, -0.038245397019116875, 0.09018932444658796, 0.12307770729863218, 0.0858567649993347, -0.01430939396751845, -0.25103654014778193, 0.10287550364487938, -0.2327623595067832, -0.10381296449174572, -0.09114908609106871, -0.012759931273259488, -0.027032415033318102, -0.3805539864323301, 0.11703034601773002, -0.09024957208228963, 0.04266889022138847, 0.0395454567208487, -0.26247943332626683, -0.10631070284372461, -0.018016294488916174, 0.09940920348578532, 0.1554146871372463, 0.17609873046915578, -0.16802387809626193, -0.23324867595718907, 0.340931279268781, -0.02144850115915428, -0.1485846048703284, 0.12607483921913495, -0.32579267815786545, -0.1690239743724565, 0.16261222429706582, 0.2506083260689463, 0.08725829749268346, -0.16936554046696983, 0.07165688939806257, -0.0038959934359549414, 0.1897281554847723, 0.11506848797684402, 0.07861625092839729, 0.19547612394464003, 0.18117223678252362, -0.05040338520692395, 0.0011949602869987888, -0.1806301503882943, -0.06014019953935141, -0.41548410181089174, -0.03412889513336787, -0.056085969762144874, 0.09625177228229274, -0.08329134206191416, -0.03181151853641495, 0.3438902525896473, 0.09082230520769892, 0.2831837625562912, 0.016393673770445667, 0.354791642973266, 0.10499618559801352, 0.06486700561695866, 0.0967406223395041, 0.33834949383162893, 0.20964311968003, 0.19252924792402024, -0.2700810365640791, 0.09043134294773024, -0.04095576276969431]
|
706.2389
|
Models for microquasars
|
I review current models used to interpret the spectra and variability of
microquasars. Among other things, I discuss the structure of the accretion flow
and its dependence on mass accretion rate, the intrinsic connection between hot
comptonizing corona and compact radio jet in the hard state, as well as
possible models for the spectral hysteresis observed during outbursts of
transient sources. Finally I comment on several models for the non-poissonian
X-ray noise in black hole binaries which, at least in some instances, is
suspected to be associated with some form of coupling between disc and jet
activity.
|
astro-ph
|
i review current models used to interpret the spectra and variability of microquasars among other things i discuss the structure of the accretion flow and its dependence on mass accretion rate the intrinsic connection between hot comptonizing corona and compact radio jet in the hard state as well as possible models for the spectral hysteresis observed during outbursts of transient sources finally i comment on several models for the nonpoissonian xray noise in black hole binaries which at least in some instances is suspected to be associated with some form of coupling between disc and jet activity
|
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|
[-0.07465533896819833, 0.10393491125732814, -0.02737440096848097, 0.1619585480639404, -0.11103643291658655, -0.12316012973465103, 0.037846997706699616, 0.44208779587343183, -0.2241867753417836, -0.3248990585225798, 0.12403200944218323, -0.3071144575291534, -0.06674245216874118, 0.24332003678031958, -0.04599946366920683, -0.004045731700673585, 0.01989415143232447, -0.030795481675256465, -0.04037572426262993, -0.18747165817623362, 0.3468799169376953, 0.07182385208632451, 0.15566452556366542, 0.02038689468478419, 0.06127266044315604, -0.08990928258977293, -0.0483938541849019, -0.009345326467042732, -0.11450799296312418, 0.032458460558513084, 0.22448338980131066, 0.12877065219829992, 0.17550974465263336, -0.39717725848721475, -0.24936626195792377, 0.04888596666074291, 0.137465281743249, -0.0012820981042075557, -0.0268657010399074, -0.20087987203727065, 0.041452189249745044, -0.24078370386869022, -0.1042256743524742, 0.007991928444003937, 0.08088185554658323, 0.048529752018890274, -0.17265695169599266, 0.12120614893081569, 0.08273558678062268, 0.008658713987577208, -0.13789188010814918, -0.05128533566207385, -0.0562880643014556, 0.09945193179835056, 0.16070314713624143, 0.02108254347515014, 0.16896975615071422, -0.1787724325831826, -0.1414572926737445, 0.3535882984192024, -0.04938688101643005, -0.04424430332962692, 0.25666625010444943, -0.22464560470591807, -0.18946524391661293, 0.11869570397839103, 0.19330070352124185, 0.10517945500167529, -0.11511132461990989, -0.02371414087607151, 0.011885709244489055, 0.17513273365449966, 0.03644292691204044, 0.1034547363014258, 0.33662609678222655, 0.13149285353912213, -0.0025274456363440175, 0.14226837524815375, -0.18534550035537997, -0.03984754716019751, -0.29211261088854257, -0.07387844692032362, -0.13142889964192644, 0.10602489825741378, -0.12405723891612239, -0.14810417807053716, 0.38680213514340983, 0.10811365867206424, 0.2619777932935922, -0.01740231579193634, 0.28672287133090274, 0.08364788645916839, 0.027998187190363396, 0.1652083742605119, 0.28699237525225474, 0.18498642438273763, 0.14543798885586642, -0.27236331383380846, 0.08810091398886799, 0.021840301611143902]
|
706.239
|
Stochastic Parabolic Equations of Full Second Order
|
A procedure is described for defining a generalized solution for stochastic
differential equations using the Cameron-Martin version of the Wiener Chaos
expansion. Existence and uniqueness of this Wiener Chaos solution is
established for parabolic stochastic PDEs such that both the drift and the
diffusion operators are of the second order.
|
math.PR math.AP
|
a procedure is described for defining a generalized solution for stochastic differential equations using the cameronmartin version of the wiener chaos expansion existence and uniqueness of this wiener chaos solution is established for parabolic stochastic pdes such that both the drift and the diffusion operators are of the second order
|
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|
[-0.14785265860147775, 0.04276595055125654, -0.0956593712978065, 0.09339739720104262, -0.10539456412661821, -0.08051608392968773, -0.04663014555349946, 0.23689208345487714, -0.37327690437436106, -0.1686203695833683, 0.20977405942045152, -0.264320422206074, -0.1909644104540348, 0.18730736574158072, -0.05529087743721903, 0.11693925185129046, 0.03344739140942693, 0.015944567173719407, -0.04644096768926829, -0.2044128930196166, 0.35653581165708603, -0.007838924073148519, 0.17718899928964674, -0.057447412982583046, 0.21088754820637404, -0.023209790280088783, -0.07424805677495896, 0.02973609265871346, -0.1423547108990897, 0.10970970708876848, 0.2266012755362317, 0.04666633386630565, 0.3342053146660328, -0.34316065020859243, -0.21209324914962052, 0.09266390925273299, 0.12364578478853218, 0.08850268743932248, -0.06324871871620416, -0.3301370780542493, 0.06022351345978677, -0.13461476925760507, -0.21423930060118437, -0.09140295241028071, 0.005536569776013494, 0.0939443611446768, -0.366857877895236, 0.15466141403652728, 0.13685853354632854, 0.023433102732524275, -0.09145658070221543, -0.04094800112769008, -0.014806704446673393, 0.03325562322512269, -0.02703211551066488, -0.04024507252499461, 0.049866600073873994, -0.06972856871318073, -0.17941852383315562, 0.33854360247030857, -0.14585180287482216, -0.3103766543418169, 0.12776848712936043, -0.13878790196031332, -0.10534919447265566, 0.14065053213387727, 0.13682455638423563, 0.14450567208230494, -0.2265035292133689, 0.14817685952191822, -0.007412472218275071, 0.07010354271158575, 0.1259046923648566, -0.01691027401946485, 0.029422359261661767, 0.17931445617228747, 0.19205471374094485, 0.0881325663998723, -0.023793171122670174, -0.20875159215182065, -0.3771234601736069, -0.20792112048249692, -0.15042445716913788, 0.07126235742121935, -0.18331146127486136, -0.2633360743522644, 0.37277586441487076, 0.13732082705944776, 0.10167898612096905, 0.07944850325584411, 0.21557446119375526, 0.30509671254083515, -0.05341045600362122, 0.07121054082352202, 0.1955728952214122, 0.24876682105474174, 0.18693186047952623, -0.20346522752719465, 0.09886565626598895, 0.251283894572407]
|
706.2391
|
From Random Processes to Generalized Fields: A Unified Approach to
Stochastic Integration
|
The paper studies stochastic integration with respect to Gaussian processes
and fields. It is more convenient to work with a field than a process: by
definition, a field is a collection of stochastic integrals for a class of
deterministic integrands. The problem is then to extend the definition to
random integrands. An orthogonal decomposition of chaos space of the random
field leads to two such extensions, corresponding to the \Ito-Skorokhod and the
Stratononovich integrals, and provides an efficient tool to study these
integrals, both analytically and numerically. For a Gaussian process, a natural
definition of the integral follows from a canonical correspondence between
random processes and a special class of random fields.
|
math.PR
|
the paper studies stochastic integration with respect to gaussian processes and fields it is more convenient to work with a field than a process by definition a field is a collection of stochastic integrals for a class of deterministic integrands the problem is then to extend the definition to random integrands an orthogonal decomposition of chaos space of the random field leads to two such extensions corresponding to the itoskorokhod and the stratononovich integrals and provides an efficient tool to study these integrals both analytically and numerically for a gaussian process a natural definition of the integral follows from a canonical correspondence between random processes and a special class of random fields
|
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|
[-0.1142211555207551, 0.11202096836017403, -0.11572749245920227, 0.07723883351092546, -0.10949039210456314, -0.06946265266637679, 0.04400821266955956, 0.3610510106559272, -0.29309190644857447, -0.21864571210745773, 0.10369635784478339, -0.22473811371742772, -0.19819627145120688, 0.22756918049878902, -0.06209087063482887, 0.06192306733295858, 0.03765093344934956, 0.022262009049488884, -0.0701918093391132, -0.2113387284733288, 0.3449565073022166, 0.03393817760956448, 0.24038955022429898, -0.026841866813163768, 0.14180971805828516, 0.04921439224602403, -0.05872649479204336, 0.017575039148387324, -0.0947086806010522, 0.15359574848228041, 0.2168475774427255, 0.10178984515368938, 0.29835041896817655, -0.36918152903986945, -0.19990952307912144, 0.1350760023940254, 0.11949794970165419, 0.1051741968504749, 0.007425307205365342, -0.25161896686296203, 0.05643227117685161, -0.13174872951968028, -0.15843021189101744, -0.09900313567554762, 0.03153084453010747, 0.008894866311436033, -0.37448161877356134, 0.011860046393095373, 0.08519953220184925, 0.049254637589124406, -0.01836783710137211, -0.05828436300460551, 0.0410611899695485, 0.06787407614693448, 0.03824668932927805, 0.07734719737063724, 0.08867923220669902, -0.12862934799747425, -0.16593015326925362, 0.36621256231389065, -0.08775225247905133, -0.2711758673325315, 0.19459490096280435, -0.11200494793671611, -0.12008332854203947, 0.1442328708567279, 0.15923379146837974, 0.15598749423080738, -0.21472985751356358, 0.11456637407248202, -0.008657593070319644, 0.058701229436943926, 0.04643277921252423, 0.014194304270350986, 0.15646456909441464, 0.1067818347448567, 0.10461541209034286, 0.18715295883583594, -0.0253506211169601, -0.1884206449696878, -0.31038706048249126, -0.21217243732498572, -0.15335909805789188, 0.06613402097351714, -0.12002748069245901, -0.24646270996681205, 0.400729788437922, 0.13164344075899403, 0.19818940003998242, 0.11236417277607026, 0.27288871881057014, 0.1847850132381191, 0.030935988769874915, 0.028782398133698078, 0.11045366575939346, 0.23833168221864146, 0.07875925426681836, -0.12110149505053151, 0.007537872115200436, 0.0752144493162632]
|
706.2392
|
New interpretation for energy gap $\Delta$ of the cut-off approximation
in the BCS theory of superconductivity
|
This paper concerns the solution of the self-consistency equation for energy
gap parameter $\Delta_{\bf k}$ in the BCS theory of superconductivity. We show
that there exists a well-defined relation between the solution for energy gap
parameter amplitude $|\Delta_{\bf k}|$ for a general interaction $V_{{\bf
k},{\bf k}'}$ and energy gap $\Delta$ obtained by using the cut-off
approximation. The relation between $|\Delta_{\bf k}|$ and $\Delta$ indicates
that $\Delta$ is a weighted average over $|\Delta_{\bf k}|$ of electronic
states within cut-off energy $\xi_c$ around the Fermi surface. In this
interpretation for $\Delta$, $\xi_c$ is not a property of $V_{{\bf k},{\bf
k}'}$, but a parameter specifying the energy range within which the weighted
average over $|\Delta_{\bf k}|$ is taken. We show that the proper choice for
the value of $\xi_c$ is only a few $k_BT_c$ (i.e., $\xi_c/k_BT_c$ is about 3 or
4). We also show that the cut-off approximation, even with
$\xi_c/k_BT_c=\infty$, is a good approximation when it is used to calculate
quantities such as the condensation energy and the specific heat, but it leads
to significant overestimation for the Josephson critical current density of a
Josephson junction if $\xi_c/k_BT_c \gg 1$ is assumed.
|
cond-mat.supr-con
|
this paper concerns the solution of the selfconsistency equation for energy gap parameter delta_bf k in the bcs theory of superconductivity we show that there exists a welldefined relation between the solution for energy gap parameter amplitude delta_bf k for a general interaction v_bf kbf k and energy gap delta obtained by using the cutoff approximation the relation between delta_bf k and delta indicates that delta is a weighted average over delta_bf k of electronic states within cutoff energy xi_c around the fermi surface in this interpretation for delta xi_c is not a property of v_bf kbf k but a parameter specifying the energy range within which the weighted average over delta_bf k is taken we show that the proper choice for the value of xi_c is only a few k_bt_c ie xi_ck_bt_c is about 3 or 4 we also show that the cutoff approximation even with xi_ck_bt_cinfty is a good approximation when it is used to calculate quantities such as the condensation energy and the specific heat but it leads to significant overestimation for the josephson critical current density of a josephson junction if xi_ck_bt_c gg 1 is assumed
|
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|
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|
706.2393
|
Consequences Of Fully Dressing Quark-Gluon Vertex Function With
Two-Point Gluon Lines
|
We extend recent studies of the effects of quark-gluon vertex dressing upon
the solutions of the Dyson-Schwinger equation for the quark propagator. A
momentum delta function is used to represent the dominant infrared strength of
the effective gluon propagator so that the resulting integral equations become
algebraic. The quark-gluon vertex is constructed from the complete set of
diagrams involving only 2-point gluon lines. The additional diagrams, including
those with crossed gluon lines, are shown to make an important contribution to
the DSE solutions for the quark propagator, because of their large color
factors and the rapid growth in their number.
|
nucl-th
|
we extend recent studies of the effects of quarkgluon vertex dressing upon the solutions of the dysonschwinger equation for the quark propagator a momentum delta function is used to represent the dominant infrared strength of the effective gluon propagator so that the resulting integral equations become algebraic the quarkgluon vertex is constructed from the complete set of diagrams involving only 2point gluon lines the additional diagrams including those with crossed gluon lines are shown to make an important contribution to the dse solutions for the quark propagator because of their large color factors and the rapid growth in their number
|
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|
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|
706.2394
|
Theory for superconductivity in a magnetic field: A local approximation
approach
|
We present a microscopic theory for superconductivity in a magnetic field
based on a local approximation approach. We derive an expression for free
energy density $F$ as a function of temperature $T$ and vector potential {\bf
a}, and two basic equations of the theory: the first is an implicit solution
for energy gap parameter amplitude $|\Delta_{\bf k}|$ as a function of wave
vector {\bf k}, temperature $T$ and vector potential {\bf a}; and the second is
a London-like relation between electrical current density {\bf j} and vector
potential {\bf a}, with an ``effective superconducting electron density'' $n_s$
that is both $T$- and {\bf a}-dependent. The two equations allow determination
of spatial variations of {\bf a} and $|\Delta_{\bf k}|$ in a superconductor for
given temperature $T$, applied magnetic field ${\bf H}_a$ and sample geometry.
The theory shows the existence of a ``partly-paired state,'' in which paired
electrons (having $|\Delta_{\bf k}|>0$) and de-paired electrons (having
$|\Delta_{\bf k}|=0$) co-exist. Such a ``partly-paired state'' exists even at
T=0 when $H_a$ is above a threshold for a given sample, giving rise to a
non-vanishing Knight shift at T=0 for $H_a$ above the threshold. We expect the
theory to be valid for highly-local superconductors for all temperatures and
magnetic fields below the superconducting transition. In the low-field limit,
the theory reduces to the local-limit result of BCS. As examples, we apply the
theory to the case of a semi-infinite superconductor in an applied magnetic
field ${\bf H}_a$ parallel to the surface of the superconductor and the case of
an isolated vortex in an infinite superconductor, and determine, in each case,
spatial variations of quantities such as {\bf a} and $|\Delta_{\bf k}|$. We
also calculate...
|
cond-mat.supr-con
|
we present a microscopic theory for superconductivity in a magnetic field based on a local approximation approach we derive an expression for free energy density f as a function of temperature t and vector potential bf a and two basic equations of the theory the first is an implicit solution for energy gap parameter amplitude delta_bf k as a function of wave vector bf k temperature t and vector potential bf a and the second is a londonlike relation between electrical current density bf j and vector potential bf a with an effective superconducting electron density n_s that is both t and bf adependent the two equations allow determination of spatial variations of bf a and delta_bf k in a superconductor for given temperature t applied magnetic field bf h_a and sample geometry the theory shows the existence of a partlypaired state in which paired electrons having delta_bf k0 and depaired electrons having delta_bf k0 coexist such a partlypaired state exists even at t0 when h_a is above a threshold for a given sample giving rise to a nonvanishing knight shift at t0 for h_a above the threshold we expect the theory to be valid for highlylocal superconductors for all temperatures and magnetic fields below the superconducting transition in the lowfield limit the theory reduces to the locallimit result of bcs as examples we apply the theory to the case of a semiinfinite superconductor in an applied magnetic field bf h_a parallel to the surface of the superconductor and the case of an isolated vortex in an infinite superconductor and determine in each case spatial variations of quantities such as bf a and delta_bf k we also calculate
|
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|
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|
706.2395
|
Combining Weak Lensing Tomography with Halo Clustering to Probe Dark
Energy
|
Two methods of constraining the properties of dark energy are weak lensing
tomography and cluster counting. Uncertainties in mass calibration of clusters
can be reduced by using the properties of halo clustering (the clustering of
clusters). However, within a single survey, weak lensing and halo clustering
probe the same density fluctuations. We explore the question of whether this
information can be used twice -- once in weak lensing and then again in halo
clustering to calibrate cluster masses -- or whether the combined dark energy
constraints are weaker than the sum of the individual constraints. For a survey
like the Dark Energy Survey (DES), we find that the cosmic shearing of source
galaxies at high redshifts is indeed highly correlated with halo clustering at
lower redshifts. Surprisingly, this correlation does not degrade cosmological
constraints for a DES-like survey, and in fact, constraints are marginally
improved since the correlations themselves act as additional observables. This
considerably simplifies the analysis for a DES-like survey: when weak lensing
and halo clustering are treated as independent experiments, the combined dark
energy constraints (cluster counts included) are accurate if not slightly
conservative. Our findings mirror those of Takada and Bridle, who investigated
correlations between the cosmic shear and cluster counts.
|
astro-ph
|
two methods of constraining the properties of dark energy are weak lensing tomography and cluster counting uncertainties in mass calibration of clusters can be reduced by using the properties of halo clustering the clustering of clusters however within a single survey weak lensing and halo clustering probe the same density fluctuations we explore the question of whether this information can be used twice once in weak lensing and then again in halo clustering to calibrate cluster masses or whether the combined dark energy constraints are weaker than the sum of the individual constraints for a survey like the dark energy survey des we find that the cosmic shearing of source galaxies at high redshifts is indeed highly correlated with halo clustering at lower redshifts surprisingly this correlation does not degrade cosmological constraints for a deslike survey and in fact constraints are marginally improved since the correlations themselves act as additional observables this considerably simplifies the analysis for a deslike survey when weak lensing and halo clustering are treated as independent experiments the combined dark energy constraints cluster counts included are accurate if not slightly conservative our findings mirror those of takada and bridle who investigated correlations between the cosmic shear and cluster counts
|
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|
[-0.09261642829308589, 0.09902002791566729, -0.1296903190875123, 0.18714850625651774, -0.10931616493505357, -0.07544018476834438, 0.008171835635545585, 0.35357948944312084, -0.22795428971076392, -0.39557353318141303, 0.05898248745410088, -0.2989782450417873, -0.007854304784505165, 0.19588044544411226, 0.028686605045214076, -0.0003335999366207957, 0.06360605983533828, -0.03458289813085143, -0.06341611480929893, -0.32716560159842, 0.30675995574227255, 0.1361826182448585, 0.2524174851241517, -0.003296711284832414, 0.058778107583779715, 0.002132263651640691, -0.11796321127829808, 0.07759198085966937, -0.1648543579345113, 0.05504158449879953, 0.2240539321623137, 0.14030811703775228, 0.2219820143287919, -0.3617039232978166, -0.19749810529661738, 0.14269730407432676, 0.21275354126982135, 0.10761628656882077, -0.057913392949665854, -0.290878651911402, 0.0751122419190194, -0.15710745858982791, -0.09872333090660607, -0.018772172539728908, -0.04144719580940792, 0.09812713333886126, -0.2237542718098375, 0.20806327390397344, 0.01247633352595854, 0.0011051275533408367, -0.05925319136895717, -0.10864715273102075, -0.052941589736668716, 0.08928498766328245, 0.008415932534262538, 0.023209207760642645, 0.19725281281025134, -0.19500902938206904, -0.007067678529216353, 0.4034114859521095, -0.07100384835238907, -0.11813041571472666, 0.16468575554142886, -0.15335589153130122, -0.24230565949402785, 0.07883689150367887, 0.147129893156108, 0.05872127799239248, -0.17712655267484653, 0.04687725331231704, 0.00014632804665641098, 0.23342569556839654, 0.04983004241530311, 0.06102945266023113, 0.2962480675617779, 0.08760553919205562, 0.1296565001532252, 0.06218187351656041, -0.14150393295693647, 0.0031953383216478406, -0.2568344070158642, -0.04382225814362325, -0.16713552130386233, 0.034098437724186546, -0.10775766385212515, -0.13120520776229466, 0.3178094636759001, 0.12706442872920243, 0.20821978396958593, 0.08319270711511446, 0.3328251833912774, 0.06756426261111709, 0.07470403700663245, 0.029227947710303296, 0.33300759175017, 0.14684727210367987, 0.03729618301963791, -0.21221197044403461, 0.03493225887610481, -0.02103182351735095]
|
706.2396
|
Model of embedded spaces: the field equations
|
A study of the Model of Embedded Spaces (MES) with a relativistic version of
Finslerian geometry is continued. The field equations of the MES (Einstein and
Maxwell types) are derived, and this formally completes geometrization of
classical electrodynamics. The minimal action principle leads to geometrization
of the field sources (the right-hand sides of the equations) and, as a
consequence, to a field hypothesis of matter, a direct confirmation of W.
Clifford's ideas.
|
gr-qc
|
a study of the model of embedded spaces mes with a relativistic version of finslerian geometry is continued the field equations of the mes einstein and maxwell types are derived and this formally completes geometrization of classical electrodynamics the minimal action principle leads to geometrization of the field sources the righthand sides of the equations and as a consequence to a field hypothesis of matter a direct confirmation of w cliffords ideas
|
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|
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|
706.2397
|
Inversely Unstable Solutions of Two-Dimensional Systems on Genus-p
Surfaces and the Topology of Knotted Attractors
|
In this paper, we will show that a periodic nonlinear, time-varying
dissipative system that is defined on a genus-p surface contains one or more
invariant sets which act as attractors. Moreover, we shall generalize a result
in [Martins, 2004] and give conditions under which these invariant sets are not
homeomorphic to a circle individually, which implies the existence of chaotic
behaviour. This is achieved by studying the appearance of inversely unstable
solutions within each invariant set.
|
math.DS
|
in this paper we will show that a periodic nonlinear timevarying dissipative system that is defined on a genusp surface contains one or more invariant sets which act as attractors moreover we shall generalize a result in martins 2004 and give conditions under which these invariant sets are not homeomorphic to a circle individually which implies the existence of chaotic behaviour this is achieved by studying the appearance of inversely unstable solutions within each invariant set
|
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|
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|
706.2398
|
Toy models of a non-associative quantum mechanics
|
Toy models of a non-associative quantum mechanics are presented. The
Heisenberg equation of motion is modified using a non-associative commutator.
Possible physical applications of a non-associative quantum mechanics are
considered. The idea is discussed that a non-associative algebra could be the
operator language for the non-perturbative quantum theory. In such approach the
non-perturbative quantum theory has observables and unobservables quantities.
|
quant-ph hep-ph hep-th math.RA
|
toy models of a nonassociative quantum mechanics are presented the heisenberg equation of motion is modified using a nonassociative commutator possible physical applications of a nonassociative quantum mechanics are considered the idea is discussed that a nonassociative algebra could be the operator language for the nonperturbative quantum theory in such approach the nonperturbative quantum theory has observables and unobservables quantities
|
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|
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|
706.2399
|
Cosmological Constraints on f(R) Acceleration Models
|
Models which accelerate the expansion of the universe through the addition of
a function of the Ricci scalar f(R) leave a characteristic signature in the
large-scale structure of the universe at the Compton wavelength scale of the
extra scalar degree of freedom. We search for such a signature in current
cosmological data sets: the WMAP cosmic microwave background (CMB) power
spectrum, SNLS supernovae distance measures, the SDSS luminous red galaxy power
spectrum, and galaxy-CMB angular correlations. Due to theoretical uncertainties
in the nonlinear evolution of f(R) models, the galaxy power spectrum
conservatively yields only weak constraints on the models despite the strong
predicted signature in the linear matter power spectrum. Currently the tightest
constraints involve the modification to the integrated Sachs-Wolfe effect from
growth of gravitational potentials during the acceleration epoch. This effect
is manifest for large Compton wavelengths in enhanced low multipole power in
the CMB and anti-correlation between the CMB and tracers of the potential. They
place a bound on the Compton wavelength of the field be less than of order the
Hubble scale.
|
astro-ph gr-qc
|
models which accelerate the expansion of the universe through the addition of a function of the ricci scalar fr leave a characteristic signature in the largescale structure of the universe at the compton wavelength scale of the extra scalar degree of freedom we search for such a signature in current cosmological data sets the wmap cosmic microwave background cmb power spectrum snls supernovae distance measures the sdss luminous red galaxy power spectrum and galaxycmb angular correlations due to theoretical uncertainties in the nonlinear evolution of fr models the galaxy power spectrum conservatively yields only weak constraints on the models despite the strong predicted signature in the linear matter power spectrum currently the tightest constraints involve the modification to the integrated sachswolfe effect from growth of gravitational potentials during the acceleration epoch this effect is manifest for large compton wavelengths in enhanced low multipole power in the cmb and anticorrelation between the cmb and tracers of the potential they place a bound on the compton wavelength of the field be less than of order the hubble scale
|
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|
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|
706.24
|
Causality and Unitarity Are Not Violated in Space-Times with an
Additional Compact Time-like Dimension
|
The hypothesis that the causal properties of space-time, as well as other
properties of physical systems like unitarity, charge conservation, etc., might
be decided by the higher dimensional structure (in particular,
higher-dimensional physical laws), rather than by the four-dimensional one, is
explored in order to evade the most awkward problems of higher-dimensional
theories with compact extra time-like dimensions: violation of causality and of
unitarity.
|
hep-ph gr-qc
|
the hypothesis that the causal properties of spacetime as well as other properties of physical systems like unitarity charge conservation etc might be decided by the higher dimensional structure in particular higherdimensional physical laws rather than by the fourdimensional one is explored in order to evade the most awkward problems of higherdimensional theories with compact extra timelike dimensions violation of causality and of unitarity
|
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|
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|
706.2401
|
Leptogenesis and dark matter unified in a non-SUSY model for neutrino
masses
|
We propose a unified explanation for the origin of dark matter and baryon
number asymmetry on the basis of a non-supersymmetric model for neutrino
masses. Neutrino masses are generated in two distinct ways, that is, a
tree-level seesaw mechanism with a single right-handed neutrino, and one-loop
radiative effects by a new additional doublet scalar. A spontaneously broken
U(1)$^\prime$ brings a $Z_2$ symmetry which restricts couplings of this new
scalar and controls the neutrino masses. It also guarantees the stability of a
CDM candidate. We examine two possible candidate for the CDM. We also show that
the decay of a heavy right-handed neutrino related to the seesaw mechanism can
generate baryon number asymmetry through leptogenesis.
|
hep-ph
|
we propose a unified explanation for the origin of dark matter and baryon number asymmetry on the basis of a nonsupersymmetric model for neutrino masses neutrino masses are generated in two distinct ways that is a treelevel seesaw mechanism with a single righthanded neutrino and oneloop radiative effects by a new additional doublet scalar a spontaneously broken u1prime brings a z_2 symmetry which restricts couplings of this new scalar and controls the neutrino masses it also guarantees the stability of a cdm candidate we examine two possible candidate for the cdm we also show that the decay of a heavy righthanded neutrino related to the seesaw mechanism can generate baryon number asymmetry through leptogenesis
|
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|
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|
706.2402
|
Realizable spin models and entanglement dynamics in superconducting flux
qubit systems
|
Realizable spin models are investigated in a two superconducting flux qubit
system. It is shown that a specific adjustment of system parameters in the two
flux qubit system makes it possible to realize an artificial two-spin system
that cannot be found naturally. For the artificial two-spin systems, time
evolution of a prepared quantum state is discussed to quantify quantum
entanglement dynamics. The concurrence and fidelity as a function of time are
shown to reveal a characteristic entanglement dynamics of the artificial spin
systems. It is found that the unentangled input state can evolute to be a
maximally entangled output state periodically due to the exchange interactions
induced by two-qubit flipping tunneling processes while single-qubit flipping
tunneling processes plays a role of magnetic fields for the artificial spins.
|
cond-mat.mes-hall
|
realizable spin models are investigated in a two superconducting flux qubit system it is shown that a specific adjustment of system parameters in the two flux qubit system makes it possible to realize an artificial twospin system that cannot be found naturally for the artificial twospin systems time evolution of a prepared quantum state is discussed to quantify quantum entanglement dynamics the concurrence and fidelity as a function of time are shown to reveal a characteristic entanglement dynamics of the artificial spin systems it is found that the unentangled input state can evolute to be a maximally entangled output state periodically due to the exchange interactions induced by twoqubit flipping tunneling processes while singlequbit flipping tunneling processes plays a role of magnetic fields for the artificial spins
|
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|
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|
706.2403
|
Existence and non-existence results for quasilinear elliptic exterior
problems with nonlinear boundary conditions
|
Existence and non-existence results are established for quasilinear elliptic
problems with nonlinear boundary conditions and lack of compactness. The proofs
combine variational methods with the geometrical feature, due to the
competition between the different growths of the non-linearities.
|
math.AP
|
existence and nonexistence results are established for quasilinear elliptic problems with nonlinear boundary conditions and lack of compactness the proofs combine variational methods with the geometrical feature due to the competition between the different growths of the nonlinearities
|
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|
[-0.10984991183718912, 0.027903266275595678, -0.08021378639693323, 0.08455225995031039, -0.1338926218878968, -0.13047515885218194, -0.07476224524802283, 0.2977720460315284, -0.3117675100404181, -0.3150152135150213, 0.17077758501430876, -0.28759748714142724, -0.10385063190723916, 0.21653711094864106, -0.07169355819381676, 0.11586746852844954, 0.08108070894683662, -0.0768103507396422, -0.1357356762194908, -0.2218003865012801, 0.4391680008878833, -0.08686021084309016, 0.25920236228328003, 0.13614815091224095, 0.08912318827290285, -0.040112272971064636, -0.0021243645858607793, 0.013369447086006403, -0.17784142935354458, 0.18789365262675442, 0.27594753942991557, 0.04268094171818934, 0.32343670961103943, -0.4474513903260231, -0.23128707839274093, 0.07530868335283901, 0.04202946676186433, 0.09611930196345049, -0.04913535350198416, -0.310547144201241, 0.08478284427454989, -0.007405183743685484, -0.165299940253853, -0.097564630228781, -0.037044953652902654, 0.1316312292933856, -0.2871829618111645, 0.1594094731109707, 0.135286233363379, 0.09109614171872013, -0.15467604173126778, -0.08176503600062508, -0.04909390554530546, 0.07567897517430155, 0.11166113986339617, -0.06388947258605376, -0.012355896742328218, -0.14975811827829794, -0.14020131228148544, 0.33236761055396574, -0.01531558322083009, -0.23568332058034444, 0.3020593991601153, -0.08447561000081662, -0.09625288538977896, 0.10930095262531388, 0.15833543949319343, 0.13009675044419342, -0.10478642818174864, 0.06714783310867221, 0.008913986375677939, 0.1404462664780256, 0.10041763107782524, 0.055127923327841256, 0.07257907391574822, 0.13320808769448808, 0.13568696749739742, 0.13883640901430658, -0.0038269420191155454, -0.13567014624315657, -0.3454750165049183, -0.060499638024913635, -0.11103951408968944, 0.014601133935349552, -0.1400096754560333, -0.1953095780489476, 0.3566339559068805, 0.11971095315866957, 0.18490269907603138, 0.06832065266606055, 0.21609600343569918, 0.12475661466535377, 0.02716122425504421, 0.029671095924353914, 0.27429774393768686, 0.21771278822990625, 0.12897000491226973, -0.25940353169081437, 0.07195633519931059, 0.14508595842083818]
|
706.2404
|
Commuting linear operators and algebraic decompositions
|
For commuting linear operators $P_0,P_1,..., P_\ell$ we describe a range of
conditions which are weaker than invertibility. When any of these conditions
hold we may study the composition $P=P_0P_1... P_\ell$ in terms of the
component operators or combinations thereof. In particular the general
inhomogeneous problem $Pu=f$ reduces to a system of simpler problems. These
problems capture the structure of the solution and range spaces and, if the
operators involved are differential, then this gives an effective way of
lowering the differential order of the problem to be studied. Suitable systems
of operators may be treated analogously. For a class of decompositions the
higher symmetries of a composition $P$ may be derived from generalised
symmmetries of the component operators $P_i$ in the system.
|
math.OA math.AP
|
for commuting linear operators p_0p_1 p_ell we describe a range of conditions which are weaker than invertibility when any of these conditions hold we may study the composition pp_0p_1 p_ell in terms of the component operators or combinations thereof in particular the general inhomogeneous problem puf reduces to a system of simpler problems these problems capture the structure of the solution and range spaces and if the operators involved are differential then this gives an effective way of lowering the differential order of the problem to be studied suitable systems of operators may be treated analogously for a class of decompositions the higher symmetries of a composition p may be derived from generalised symmmetries of the component operators p_i in the system
|
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|
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|
706.2405
|
Dispersion Relation for Alfven Waves in a Viscous, Diffusive Plasma
|
Propagation of Alfven waves in the solar plasma has been a topic of
scientific interest for a long time. We have derived a dispersion relation for
shear Alfven waves in a viscous and diffusive plasma.
|
astro-ph
|
propagation of alfven waves in the solar plasma has been a topic of scientific interest for a long time we have derived a dispersion relation for shear alfven waves in a viscous and diffusive plasma
|
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|
[-0.2160170650508787, 0.27194783235234876, -0.08854903030608381, 0.0787739383322852, -0.1033638492758785, -0.01393350213766098, -0.06895887018846614, 0.36246185818953175, -0.2400735661919628, -0.23950710424355098, 0.03682562289094286, -0.2502731204032898, -0.06475322438137872, 0.2722690261368241, 0.06597043169396265, 0.13807325389768396, 0.05013997809894915, -0.01935590635985136, 0.0277060916647315, -0.08658652875040258, 0.18664765996592386, 0.08495603129267693, 0.26777144691773824, 0.048314931243658064, 0.12637438603809903, -0.1207143799934004, -0.03491773333932672, 0.05980764089950493, -0.17061811599331642, 0.01106270221727235, 0.26493808520691736, 0.07218912233864623, 0.3545738523293819, -0.5075203946658543, -0.40599670662943804, -0.053400842685784614, 0.22622198519696082, 0.11966212945325035, -0.08057846312544176, -0.21132512912154197, -0.03091737473649638, -0.19748360589146613, -0.0894084412072386, 0.10160674921103886, 0.1681344640640808, 0.08626615736367448, -0.24907878035945552, 0.15825123708761696, 0.06575874122125762, 0.06406770824853864, -0.06405857354402542, -0.0034094179315226417, -0.039955008814909626, 0.060412708350590295, 0.181321430472391, 0.03569729388026255, 0.10072198559397033, -0.1480898804696543, -0.018853354241166798, 0.44594420407499585, -0.1216877100190946, -0.19568079092672894, 0.1938583608384111, -0.20373497102659063, -0.09036276810137289, 0.18596636091492005, 0.267294996311622, 0.04792033920862845, -0.11895649063267878, 0.034339764180393625, -0.0876668891204255, 0.07510906915579524, 0.15501302805330072, 0.0008012634036796434, 0.3132010006478855, 0.24447192597602094, -0.014934072956176742, 0.0614425574928256, -0.1358696848956502, 0.05854479351214, -0.23540404800857817, -0.16707580910463418, -0.14106857425400188, 0.02360568339271205, -0.05873826346983801, -0.22185846040291446, 0.46558593768360357, 0.15404863650245326, 0.06080621022930635, 0.020603365264832973, 0.2786419752453055, 0.1615785856332098, -0.007370718887874058, 0.182157047146133, 0.39559884199074336, 0.25592911834163323, 0.21442782660680157, -0.2049504119902849, 0.050898828064756735, 0.07566741848630565]
|
706.2406
|
Collective motion in quantum diffusive environment
|
The general problem of dissipation in macroscopic large-amplitude collective
motion and its relation to energy diffusion of intrinsic degrees of freedom of
a nucleus is studied. By applying the cranking approach to the nuclear
many-body system, a set of coupled dynamical equations for the collective
classical variable and the quantum mechanical occupancies of the intrinsic
nuclear states is derived. Different dynamical regimes of the intrinsic nuclear
motion and its consequences on time properties of collective dissipation are
discussed.
|
nucl-th
|
the general problem of dissipation in macroscopic largeamplitude collective motion and its relation to energy diffusion of intrinsic degrees of freedom of a nucleus is studied by applying the cranking approach to the nuclear manybody system a set of coupled dynamical equations for the collective classical variable and the quantum mechanical occupancies of the intrinsic nuclear states is derived different dynamical regimes of the intrinsic nuclear motion and its consequences on time properties of collective dissipation are discussed
|
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|
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|
706.2407
|
Parity violation in hydrogen revisited
|
We reconsider parity violation experiments in atomic hydrogen and deuterium
in the light of existing tests of the Electroweak interactions, and assess
whether new experiments, using improved experimental techniques, could make
useful contributions to testing the Standard Model (SM). We find that, if
parity experiments in hydrogen can be done, they remain highly desirable
because there is negligible atomic-physics uncertainty and low energy tests of
weak neutral current interactions are needed to probe for new physics beyond
the SM. Of particular interest would be a measurement of the nuclear spin
independent coupling C_{1D} for the deuteron at a combined error (theory +
experiment) of 0.3%. This would provide a factor of three improvement to the
precision on sin^2 theta_W at very low momentum transfer provided by heavy atom
Atomic Parity Violation (APV) experiments. Also, experiments in H and D could
provide precise measurements of three other electron-nucleon,
weak-neutral-current coupling constants: C_{1p}, C_{2p},and C_{2D}, which have
not been accurately determined to date. Analysis of a generic APV experiment in
deuterium indicates that a 0.3% measurement of C_{1D} requires development of a
slow (77K) metastable beam of ~ 5x10^14 D(2S) s^-1 per hyperfine component. The
advent of UV radiation from free electron laser (FEL) technology could allow
production of such a beam.
|
hep-ph
|
we reconsider parity violation experiments in atomic hydrogen and deuterium in the light of existing tests of the electroweak interactions and assess whether new experiments using improved experimental techniques could make useful contributions to testing the standard model sm we find that if parity experiments in hydrogen can be done they remain highly desirable because there is negligible atomicphysics uncertainty and low energy tests of weak neutral current interactions are needed to probe for new physics beyond the sm of particular interest would be a measurement of the nuclear spin independent coupling c_1d for the deuteron at a combined error theory experiment of 03 this would provide a factor of three improvement to the precision on sin2 theta_w at very low momentum transfer provided by heavy atom atomic parity violation apv experiments also experiments in h and d could provide precise measurements of three other electronnucleon weakneutralcurrent coupling constants c_1p c_2pand c_2d which have not been accurately determined to date analysis of a generic apv experiment in deuterium indicates that a 03 measurement of c_1d requires development of a slow 77k metastable beam of 5x1014 d2s s1 per hyperfine component the advent of uv radiation from free electron laser fel technology could allow production of such a beam
|
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|
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|
706.2408
|
A New Type of Two-photon Forward Radiation in Pure Liquids
|
Unexpected spectral features are observed in the two photon spectrum of the
pure water in the forward direction when an 80 femtosecond laser pulse is
focused at 10^10Wcm-2 or less. Such intensity is much lower than the breakdown
or stimulated threshold of the liquid water. The two broad features are about
2700cm-1 and 5000cm-1 red shifted from the hyper-Rayleigh wavelength,
respectively, and they are quadratic with the laser intensity. They do not
match the known Raman or hyper-Raman frequencies of water, and they are both
centered at a narrow angle in the forward direction. Several other liquids also
exhibited similar but molecular specific spectral features.
|
physics.chem-ph physics.optics
|
unexpected spectral features are observed in the two photon spectrum of the pure water in the forward direction when an 80 femtosecond laser pulse is focused at 1010wcm2 or less such intensity is much lower than the breakdown or stimulated threshold of the liquid water the two broad features are about 2700cm1 and 5000cm1 red shifted from the hyperrayleigh wavelength respectively and they are quadratic with the laser intensity they do not match the known raman or hyperraman frequencies of water and they are both centered at a narrow angle in the forward direction several other liquids also exhibited similar but molecular specific spectral features
|
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|
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|
706.2409
|
On the Number of Nodal Domains of Random Spherical Harmonics
|
Let N(f) be a number of nodal domains of a random Gaussian spherical harmonic
f of degree n. We prove that as n grows to infinity, the mean of N(f)/n^2 tends
to a positive constant, and that N(f)/n^2 exponentially concentrates around
that constant.
This result is consistent with predictions made by Bogomolny and Schmit using
a percolation-like model for nodal domains of random Gaussian plane waves.
|
math-ph math.MP math.PR
|
let nf be a number of nodal domains of a random gaussian spherical harmonic f of degree n we prove that as n grows to infinity the mean of nfn2 tends to a positive constant and that nfn2 exponentially concentrates around that constant this result is consistent with predictions made by bogomolny and schmit using a percolationlike model for nodal domains of random gaussian plane waves
|
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|
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|
706.241
|
On the Supergravity Description of Wilson Loop in Non-commutative Dipole
Field Theory
|
The Wilson loop in the non-commutative dipole field theory is re-examined
within the framework of dual gravity description. In contrast to the previous
investigations, we let the dual string be moving along the deformed $S^5$ and
find the exact expression of the interquark potential. The potential shows a
Coulomb behavior at all distance and does not have a minimum distance between
quarks, which exhibits in the static configuration. After comparing the
potential of the static and moving configurations we find that while the dual
string is static at long distance it will transit to a moving configuration at
short distance. We also analyze an electric dipole system and find that it
shows a similar transition property. Finally, we mention the unsuitable
approximation made in the previous paper [hep-th/0701069] and find that the
interquark potential in a gauge theory with a non-constant non-commutativity
has a Coulomb behavior at all distance.
|
hep-th
|
the wilson loop in the noncommutative dipole field theory is reexamined within the framework of dual gravity description in contrast to the previous investigations we let the dual string be moving along the deformed s5 and find the exact expression of the interquark potential the potential shows a coulomb behavior at all distance and does not have a minimum distance between quarks which exhibits in the static configuration after comparing the potential of the static and moving configurations we find that while the dual string is static at long distance it will transit to a moving configuration at short distance we also analyze an electric dipole system and find that it shows a similar transition property finally we mention the unsuitable approximation made in the previous paper hepth0701069 and find that the interquark potential in a gauge theory with a nonconstant noncommutativity has a coulomb behavior at all distance
|
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|
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|
706.2411
|
Violation of the London Law and Onsager-Feynman quantization in
multicomponent superconductors
|
Non-classical response to rotation is a hallmark of quantum ordered states
such as superconductors and superfluids. The rotational responses of all
currently known single-component "super" states of matter (superconductors,
superfluids and supersolids) are largely described by two fundamental
principles and fall into two categories according to whether the systems are
composed of charged or neutral particles: the London law relating the angular
velocity to a subsequently established magnetic field and the Onsager-Feynman
quantization of superfluid velocity. These laws are theoretically shown to be
violated in a two-component superconductor such as the projected liquid
metallic states of hydrogen and deuterium at high pressures. The rotational
responses of liquid metallic hydrogen or deuterium identify them as a new class
of dissipationless states; they also directly point to a particular
experimental route for verification of their existence.
|
cond-mat.supr-con astro-ph hep-ph
|
nonclassical response to rotation is a hallmark of quantum ordered states such as superconductors and superfluids the rotational responses of all currently known singlecomponent super states of matter superconductors superfluids and supersolids are largely described by two fundamental principles and fall into two categories according to whether the systems are composed of charged or neutral particles the london law relating the angular velocity to a subsequently established magnetic field and the onsagerfeynman quantization of superfluid velocity these laws are theoretically shown to be violated in a twocomponent superconductor such as the projected liquid metallic states of hydrogen and deuterium at high pressures the rotational responses of liquid metallic hydrogen or deuterium identify them as a new class of dissipationless states they also directly point to a particular experimental route for verification of their existence
|
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|
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|
706.2412
|
Generalized gauge-invariance for gravitational waves
|
The aim of this paper is to show the gauge-invariance on the response of
interferometers to gravitational waves (GWs). In this process, after a review
of results on the Tranverse-Traceless (TT) gauge, where, in general, the
theoretical computations on GWs are performed, which is due for completness, we
analyse the gauge of the local observer, which represents the gauge of a
laboratory environment on Earth. The gauge-invariance between the two gauges is
shown in its full angular and frequency dependences. In previous works in the
literature this gauge-invariance was shown only in the low frequencies
approximation or in the simplest geometry of the interferometer in respect to
the propagating GW (i.e. both of the arms of the interferometer are
perpendicular to the propagating GW). As far as the computation of the response
functions in the gauge of the local observer is concerned, a common
misconception about interferometers is also clarifed.
|
gr-qc
|
the aim of this paper is to show the gaugeinvariance on the response of interferometers to gravitational waves gws in this process after a review of results on the tranversetraceless tt gauge where in general the theoretical computations on gws are performed which is due for completness we analyse the gauge of the local observer which represents the gauge of a laboratory environment on earth the gaugeinvariance between the two gauges is shown in its full angular and frequency dependences in previous works in the literature this gaugeinvariance was shown only in the low frequencies approximation or in the simplest geometry of the interferometer in respect to the propagating gw ie both of the arms of the interferometer are perpendicular to the propagating gw as far as the computation of the response functions in the gauge of the local observer is concerned a common misconception about interferometers is also clarifed
|
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|
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|
706.2413
|
Comparison of Theory and Direct Numerical Simulations of Drag Reduction
by Rodlike Polymers in Turbulent Channel Flows
|
Numerical simulations of turbulent channel flows, with or without additives,
are limited in the extent of the Reynolds number \Re and Deborah number \De.
The comparison of such simulations to theories of drag reduction, which are
usually derived for asymptotically high \Re and \De, calls for some care. In
this paper we present a study of drag reduction by rodlike polymers in a
turbulent channel flow using direct numerical simulation and illustrate how
these numerical results should be related to the recently developed theory.
|
nlin.CD
|
numerical simulations of turbulent channel flows with or without additives are limited in the extent of the reynolds number re and deborah number de the comparison of such simulations to theories of drag reduction which are usually derived for asymptotically high re and de calls for some care in this paper we present a study of drag reduction by rodlike polymers in a turbulent channel flow using direct numerical simulation and illustrate how these numerical results should be related to the recently developed theory
|
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|
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|
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