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706.1314
|
When Did Cosmic Acceleration Start ?
|
A precise determination, and comparison, of the epoch of the onset of cosmic
acceleration, at redshift z_acc, and of dark energy domination, at z_eq,
provides an interesting measure with which to parameterize dark energy models.
By combining several cosmological datasets we place constraints on the redshift
and age of cosmological acceleration. For a Lambda-CDM model, we find the
constraint z_acc=0.76\pm0.10 at 95% c.l., occurring 6.7\pm0.4 Gyrs ago.
Allowing a constant equation of state but different from -1 changes the
constraints to z_acc=0.81\pm0.12 (6.9\pm0.5 Gyrs ago) and
z_eq=0.48\pm0.14(4.9\pm0.9 Gyrs ago), while dynamical models markedly increase
the error on the constraints with z_acc=0.81\pm0.30 (6.8\pm1.4 Gyrs ago) and
z_eq=0.44\pm0.20 (4.5\pm1.0 Gyrs ago). Unified dark energy models as Silent
Quartessence yield: z_acc=0.80\pm0.16 (6.8\pm0.6 Gyrs ago).
|
astro-ph gr-qc hep-ph
|
a precise determination and comparison of the epoch of the onset of cosmic acceleration at redshift z_acc and of dark energy domination at z_eq provides an interesting measure with which to parameterize dark energy models by combining several cosmological datasets we place constraints on the redshift and age of cosmological acceleration for a lambdacdm model we find the constraint z_acc076pm010 at 95 cl occurring 67pm04 gyrs ago allowing a constant equation of state but different from 1 changes the constraints to z_acc081pm012 69pm05 gyrs ago and z_eq048pm01449pm09 gyrs ago while dynamical models markedly increase the error on the constraints with z_acc081pm030 68pm14 gyrs ago and z_eq044pm020 45pm10 gyrs ago unified dark energy models as silent quartessence yield z_acc080pm016 68pm06 gyrs ago
|
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|
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|
706.1315
|
The Dirac system on the Anti-de Sitter Universe
|
We investigate the global solutions of the Dirac equation on the
Anti-de-Sitter Universe. Since this space is not globally hyperbolic, the
Cauchy problem is not, {\it a priori}, well-posed. Nevertheless we can prove
that there exists unitary dynamics, but its uniqueness crucially depends on the
ratio beween the mass $M$ of the field and the cosmological constant
$\Lambda>0$ : it appears a critical value, $\Lambda/12$, which plays a role
similar to the Breitenlohner-Freedman bound for the scalar fields. When
$M^2\geq \Lambda/12$ there exists a unique unitary dynamics. In opposite, for
the light fermions satisfying $M^2<\Lambda/12$, we construct several asymptotic
conditions at infinity, such that the problem becomes well-posed. In all the
cases, the spectrum of the hamiltonian is discrete. We also prove a result of
equipartition of the energy.
|
math-ph math.AP math.MP
|
we investigate the global solutions of the dirac equation on the antidesitter universe since this space is not globally hyperbolic the cauchy problem is not it a priori wellposed nevertheless we can prove that there exists unitary dynamics but its uniqueness crucially depends on the ratio beween the mass m of the field and the cosmological constant lambda0 it appears a critical value lambda12 which plays a role similar to the breitenlohnerfreedman bound for the scalar fields when m2geq lambda12 there exists a unique unitary dynamics in opposite for the light fermions satisfying m2lambda12 we construct several asymptotic conditions at infinity such that the problem becomes wellposed in all the cases the spectrum of the hamiltonian is discrete we also prove a result of equipartition of the energy
|
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|
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|
706.1316
|
Coupling of Optical Lumped Nanocircuit Elements and Effects of
Substrates
|
We present here a model for the coupling among small nanoparticles excited by
an optical electric field in the framework of our optical lumped nanocircuit
theory [N. Engheta, A. Salandrino, and A. Alu Phys. Rev. Lett. 95, 095504
(2005)]. We derive how this coupling affects the corresponding nanocircuit
model by adding controlled sources that depend on the optical voltages applied
on the coupled particles. With the same technique, we can model also the
presence of a substrate underneath nanocircuit elements, relating its presence
to the coupling with a properly modeled image nanoparticle. These results are
of importance in the understanding and the design of complex optical
nanocircuits at infrared and optical frequencies.
|
cond-mat.mtrl-sci
|
we present here a model for the coupling among small nanoparticles excited by an optical electric field in the framework of our optical lumped nanocircuit theory n engheta a salandrino and a alu phys rev lett 95 095504 2005 we derive how this coupling affects the corresponding nanocircuit model by adding controlled sources that depend on the optical voltages applied on the coupled particles with the same technique we can model also the presence of a substrate underneath nanocircuit elements relating its presence to the coupling with a properly modeled image nanoparticle these results are of importance in the understanding and the design of complex optical nanocircuits at infrared and optical frequencies
|
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|
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|
706.1317
|
A model for learning to segment temporal sequences, utilizing a mixture
of RNN experts together with adaptive variance
|
This paper proposes a novel learning method for a mixture of recurrent neural
network (RNN) experts model, which can acquire the ability to generate desired
sequences by dynamically switching between experts. Our method is based on
maximum likelihood estimation, using a gradient descent algorithm. This
approach is similar to that used in conventional methods; however, we modify
the likelihood function by adding a mechanism to alter the variance for each
expert. The proposed method is demonstrated to successfully learn Markov chain
switching among a set of 9 Lissajous curves, for which the conventional method
fails. The learning performance, analyzed in terms of the generalization
capability, of the proposed method is also shown to be superior to that of the
conventional method. With the addition of a gating network, the proposed method
is successfully applied to the learning of sensory-motor flows for a small
humanoid robot as a realistic problem of time series prediction and generation.
|
nlin.AO
|
this paper proposes a novel learning method for a mixture of recurrent neural network rnn experts model which can acquire the ability to generate desired sequences by dynamically switching between experts our method is based on maximum likelihood estimation using a gradient descent algorithm this approach is similar to that used in conventional methods however we modify the likelihood function by adding a mechanism to alter the variance for each expert the proposed method is demonstrated to successfully learn markov chain switching among a set of 9 lissajous curves for which the conventional method fails the learning performance analyzed in terms of the generalization capability of the proposed method is also shown to be superior to that of the conventional method with the addition of a gating network the proposed method is successfully applied to the learning of sensorymotor flows for a small humanoid robot as a realistic problem of time series prediction and generation
|
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|
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|
706.1318
|
Constructing a maximum utility slate of on-line advertisements
|
We present an algorithm for constructing an optimal slate of sponsored search
advertisements which respects the ordering that is the outcome of a generalized
second price auction, but which must also accommodate complicating factors such
as overall budget constraints. The algorithm is easily fast enough to use on
the fly for typical problem sizes, or as a subroutine in an overall
optimization.
|
cs.DM cs.DS
|
we present an algorithm for constructing an optimal slate of sponsored search advertisements which respects the ordering that is the outcome of a generalized second price auction but which must also accommodate complicating factors such as overall budget constraints the algorithm is easily fast enough to use on the fly for typical problem sizes or as a subroutine in an overall optimization
|
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|
[-0.07965052640159434, 0.05054909288165002, -0.09248114884981225, 0.10120176949403098, -0.15939386050036597, -0.13963463845392388, 0.11440303572829091, 0.40752446661973674, -0.30625990664045655, -0.3642979626273436, 0.153318430452923, -0.21592015158685465, -0.15840933672077354, 0.19856278123071178, -0.0871547237339039, 0.02873634583797426, 0.04249281886093799, 0.04464307691781751, -0.02730474883461401, -0.29055493042594, 0.25656630741169434, 0.14851445460414153, 0.2331944790278231, 0.03003594114805662, 0.097445969049248, 0.02056712992939978, 0.019834680385106513, 0.02564384732695837, -0.08536850516893243, 0.10145672692188752, 0.2708289499034084, 0.2133372464637843, 0.31063769000672525, -0.38604629460361695, -0.12882795139786699, 0.13595901624930481, 0.14374800946848887, 0.08809311525340402, -0.08412034591216774, -0.20856580593352836, 0.06160420245460926, -0.18165191976473696, -0.07013029701286747, -0.0960582731622121, -0.002960584096370205, -0.009394125862708014, -0.3759786590573288, -0.004975269072137082, 0.03157015176369778, -0.037773095874957016, -0.0651639603987156, -0.10397706838745263, 0.03681231259308275, 0.1337061042995042, 0.055751892677958936, 0.015440403754192015, 0.12264153919362973, -0.15084807660370583, -0.18632101949544683, 0.4583804424131109, -0.0033547835154158455, -0.18961240171695187, 0.11438990822963176, -0.02214526246497107, -0.17353663190958962, 0.12839832371701637, 0.23475714869076206, 0.1522137601108801, -0.16831319761507574, 0.036560561104242, -0.07792424425227387, 0.2139067824990038, 0.0310258642590094, 0.009574266473552393, 0.1533245791628536, 0.20434147266731148, 0.19946207917265354, 0.14095334662124515, -0.025623076155992044, -0.09725097412874381, -0.27830038704128274, -0.17778494263127928, -0.1626878577104259, 0.0021540796864897974, -0.10860357326906055, -0.1976167538293427, 0.3500955740004898, 0.14746256820076414, 0.1867370216866895, 0.08509875484366691, 0.33607421812391086, 0.10598418194304911, 0.060845114921610204, 0.11175434055903385, 0.16931912996956416, -0.05603845600759791, 0.09934296204723538, -0.202799735360332, 0.16325976522338967, 0.05456514171354713]
|
706.1319
|
Dealing with delicate issues in waveforms calculations
|
We revisit the calculation of gravitational radiation through the use of Weyl
scalars. We point out several possible problems arising from gauge and tetrad
ambiguities and ways to address them. Our analysis indicates how, relatively
simple corrections can be introduced to remove these ambiguities.
|
gr-qc
|
we revisit the calculation of gravitational radiation through the use of weyl scalars we point out several possible problems arising from gauge and tetrad ambiguities and ways to address them our analysis indicates how relatively simple corrections can be introduced to remove these ambiguities
|
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|
[-0.09597396160560576, 0.11082875022177839, -0.1023640452503142, 0.11581968434620649, -0.1764329848387702, -0.11303248291369528, 0.07903307104821909, 0.3594948551194234, -0.2894048248841004, -0.29423399752175267, 0.045194913358004254, -0.2806964546696029, -0.17501747218722646, 0.1560603161342442, -0.07720992108806968, 0.03333423667672006, 0.05366842220114036, -0.07112168184142899, -0.13918084268251815, -0.22813793513077227, 0.3989632076753134, 0.056472424121404234, 0.16180917375128379, 0.0749833591451699, 0.08092183957342058, -0.018914621979506177, -0.12896131620403717, 0.027177178173918615, -0.09479088950584727, 0.07430695345498282, 0.2583969393956729, 0.09972123937173323, 0.21417643611973539, -0.44552203284745867, -0.2175984427078881, 0.10945822831920603, 0.15044540175321428, 0.19506144125691868, -0.03160378623711453, -0.2967420561577786, 0.06493040458934213, -0.170709160706875, -0.1547977827113672, -0.17114147256043824, -0.07834954153407704, -0.10816176413473758, -0.19560741290280764, 0.05315480493432419, 0.012195368128066713, -0.01858216223560951, -0.0006935253464193506, -0.10440194604664364, 0.023508779572280633, 0.12379751339639453, 0.18003503445916894, 0.002048767256465825, 0.14665697271596978, -0.10161172509701415, -0.15032352253117345, 0.44497138718989765, -0.02237051683054729, -0.22834642714058812, 0.19916040611728517, -0.06628370568664237, -0.17558333946561272, 0.09239366157403724, 0.13460610147078775, 0.11860590159300376, -0.1891812528695234, 0.11648413934480314, 0.03344422221099111, 0.10930088203498269, 0.12440504942258651, 0.015120426171713254, 0.2820252391763709, -0.00417109557681463, -0.021941055967049164, 0.15711142027232033, -0.08122437499762535, -0.058676755099440925, -0.3810080322860317, -0.10313083925707774, -0.09616029757837002, 0.06908787188215436, -0.07847237445093924, -0.12394380933520469, 0.3892386039845984, 0.28738509164064785, 0.17610278549942782, 0.01079323324798183, 0.26860007287574594, 0.10496691580258564, 0.10123501836576244, 0.024495909773659976, 0.26915241045538674, 0.15365066877777941, 0.06430797368838367, -0.24184713590445675, -0.09293309616094286, 0.06470967712812126]
|
706.132
|
Accretion vs colliding wind models for the gamma-ray binary LS I +61
303: an assessment
|
LS I +61 303 is a puzzling Be/X-ray binary with variable gamma-ray emission
at up TeV energies. The nature of the compact object and the origin of the
high-energy emission are unclear. One family of models invokes particle
acceleration in shocks from the collision between the B-star wind and a
relativistic pulsar wind, while another centers on a relativistic jet powered
by accretion. Recent high-resolution radio observations showing a putative
"cometary tail" pointing away from the Be star near periastron have been cited
as support for the pulsar-wind model. We wish here to carry out a quantitative
assessment of these competing models for this extraordinary source. We apply a
3D SPH code for dynamical simulations of both the pulsar-wind-interaction and
accretion-jet models. The former yields a description of the shape of the
wind-wind interaction surface. The latter provides an estimation of the
accretion rate. The results allow critical evaluation of how the two distinct
models confront the data in various wavebands under a range of conditions. When
one accounts for the 3D dynamical wind interaction under realistic constraints
for the relative strength of the B-star and pulsar winds, the resulting form of
the interaction front does not match the putative "cometary tail" claimed from
radio observations. On the other hand, dynamical simulations of the
accretion-jet model indicate that the orbital phase variation of accretion
power includes a secondary broad peak well away from periastron, thus providing
a plausible way to explain the observed TeV gamma ray emission toward apastron.
We conclude that the colliding-wind model is not clearly established for LS I
+61 303, while the accretion-jet model can reproduce many key characteristics
of the observed TeV gamma-ray emission.
|
astro-ph
|
ls i 61 303 is a puzzling bexray binary with variable gammaray emission at up tev energies the nature of the compact object and the origin of the highenergy emission are unclear one family of models invokes particle acceleration in shocks from the collision between the bstar wind and a relativistic pulsar wind while another centers on a relativistic jet powered by accretion recent highresolution radio observations showing a putative cometary tail pointing away from the be star near periastron have been cited as support for the pulsarwind model we wish here to carry out a quantitative assessment of these competing models for this extraordinary source we apply a 3d sph code for dynamical simulations of both the pulsarwindinteraction and accretionjet models the former yields a description of the shape of the windwind interaction surface the latter provides an estimation of the accretion rate the results allow critical evaluation of how the two distinct models confront the data in various wavebands under a range of conditions when one accounts for the 3d dynamical wind interaction under realistic constraints for the relative strength of the bstar and pulsar winds the resulting form of the interaction front does not match the putative cometary tail claimed from radio observations on the other hand dynamical simulations of the accretionjet model indicate that the orbital phase variation of accretion power includes a secondary broad peak well away from periastron thus providing a plausible way to explain the observed tev gamma ray emission toward apastron we conclude that the collidingwind model is not clearly established for ls i 61 303 while the accretionjet model can reproduce many key characteristics of the observed tev gammaray emission
|
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|
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|
706.1321
|
Detailed study of the GRB 030329 radio afterglow deep into the
non-relativistic phase
|
We explore the physics behind one of the brightest radio afterglows ever, GRB
030329, at late times when the jet is non-relativistic. We determine the
physical parameters of the blast wave and its surroundings, in particular the
index of the electron energy distribution, the energy of the blast wave, and
the density (structure) of the circumburst medium. We then compare our results
with those from image size measurements. We observed the GRB 030329 radio
afterglow with the Westerbork Synthesis Radio Telescope and the Giant Metrewave
Radio Telescope at frequencies from 325 MHz to 8.4 GHz, spanning a time range
of 268-1128 days after the burst. We modeled all the available radio data and
derived the physical parameters. The index of the electron energy distribution
is p=2.1, the circumburst medium is homogeneous, and the transition to the
non-relativistic phase happens at t_NR ~ 80 days. The energy of the blast wave
and density of the surrounding medium are comparable to previous findings. Our
findings indicate that the blast wave is roughly spherical at t_NR, and they
agree with the implications from the VLBI studies of image size evolution. It
is not clear from the presented dataset whether we have seen emission from the
counter jet or not. We predict that the Low Frequency Array will be able to
observe the afterglow of GRB 030329 and many other radio afterglows,
constraining the physics of the blast wave during its non-relativistic phase
even further.
|
astro-ph
|
we explore the physics behind one of the brightest radio afterglows ever grb 030329 at late times when the jet is nonrelativistic we determine the physical parameters of the blast wave and its surroundings in particular the index of the electron energy distribution the energy of the blast wave and the density structure of the circumburst medium we then compare our results with those from image size measurements we observed the grb 030329 radio afterglow with the westerbork synthesis radio telescope and the giant metrewave radio telescope at frequencies from 325 mhz to 84 ghz spanning a time range of 2681128 days after the burst we modeled all the available radio data and derived the physical parameters the index of the electron energy distribution is p21 the circumburst medium is homogeneous and the transition to the nonrelativistic phase happens at t_nr 80 days the energy of the blast wave and density of the surrounding medium are comparable to previous findings our findings indicate that the blast wave is roughly spherical at t_nr and they agree with the implications from the vlbi studies of image size evolution it is not clear from the presented dataset whether we have seen emission from the counter jet or not we predict that the low frequency array will be able to observe the afterglow of grb 030329 and many other radio afterglows constraining the physics of the blast wave during its nonrelativistic phase even further
|
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|
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|
706.1322
|
Thermodynamics and the virial expansion for trapped fluids in arbitrary
external potentials
|
We present the full thermodynamics of a fluid confined by an arbitrary
external potential based on the virial expansion of the grand potential. The
fluid may be classical or quantum and it is assumed that interatomic
interactions are pairwise additive. We indicate how the appropriate
"generalized" volume and pressure variables, that replace the usual volume and
hydrostatic pressure, emerge for a given confining potential in the
thermodynamic limit. A discussion of the physical meaning and of the
measurement of these variables is presented. We emphasize that this treatment
yields the correct equation of state of the fluid and we give its virial
expansion. We propose an experiment to measure the heat capacity, so that with
this quantity and the equation of state, the complete thermodynamics of the
system may be extracted. As a corollary, we find that the so-called {\it local
density approximation} for these systems follows in the thermodynamic limit,
although we also point out that it cannot be used indiscriminately for all
local variables. Along the text we discuss the relevance of these findings in
the description of the currently confined ultracold gases.
|
cond-mat.stat-mech
|
we present the full thermodynamics of a fluid confined by an arbitrary external potential based on the virial expansion of the grand potential the fluid may be classical or quantum and it is assumed that interatomic interactions are pairwise additive we indicate how the appropriate generalized volume and pressure variables that replace the usual volume and hydrostatic pressure emerge for a given confining potential in the thermodynamic limit a discussion of the physical meaning and of the measurement of these variables is presented we emphasize that this treatment yields the correct equation of state of the fluid and we give its virial expansion we propose an experiment to measure the heat capacity so that with this quantity and the equation of state the complete thermodynamics of the system may be extracted as a corollary we find that the socalled it local density approximation for these systems follows in the thermodynamic limit although we also point out that it cannot be used indiscriminately for all local variables along the text we discuss the relevance of these findings in the description of the currently confined ultracold gases
|
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|
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|
706.1323
|
GRB 030329: 3 years of radio afterglow monitoring
|
Radio observations of gamma-ray burst (GRB) afterglows are essential for our
understanding of the physics of relativistic blast waves, as they enable us to
follow the evolution of GRB explosions much longer than the afterglows in any
other wave band. We have performed a three-year monitoring campaign of GRB
030329 with the Westerbork Synthesis Radio Telescopes (WSRT) and the Giant
Metrewave Radio Telescope (GMRT). Our observations, combined with observations
at other wavelengths, have allowed us to determine the GRB blast wave physical
parameters, such as the total burst energy and the ambient medium density, as
well as investigate the jet nature of the relativistic outflow. Further, by
modeling the late-time radio light curve of GRB 030329, we predict that the
Low-Frequency Array (LOFAR, 30-240 MHz) will be able to observe afterglows of
similar GRBs, and constrain the physics of the blast wave during its
non-relativistic phase.
|
astro-ph
|
radio observations of gammaray burst grb afterglows are essential for our understanding of the physics of relativistic blast waves as they enable us to follow the evolution of grb explosions much longer than the afterglows in any other wave band we have performed a threeyear monitoring campaign of grb 030329 with the westerbork synthesis radio telescopes wsrt and the giant metrewave radio telescope gmrt our observations combined with observations at other wavelengths have allowed us to determine the grb blast wave physical parameters such as the total burst energy and the ambient medium density as well as investigate the jet nature of the relativistic outflow further by modeling the latetime radio light curve of grb 030329 we predict that the lowfrequency array lofar 30240 mhz will be able to observe afterglows of similar grbs and constrain the physics of the blast wave during its nonrelativistic phase
|
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|
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|
706.1324
|
GRB 030329: three years of radio afterglow monitoring
|
Radio observations of gamma-ray burst (GRB) afterglows are essential for our
understanding of the physics of relativistic blast waves, as they enable us to
follow the evolution of GRB explosions much longer than the afterglows in any
other wave band. We have performed a three-year monitoring campaign of GRB
030329 with the Westerbork Synthesis Radio Telescopes (WSRT) and the Giant
Metrewave Radio Telescope (GMRT). Our observations, combined with observations
at other wavelengths, have allowed us to determine the GRB blast wave physical
parameters, such as the total burst energy and the ambient medium density, as
well as investigate the jet nature of the relativistic outflow. Further, by
modeling the late-time radio light curve of GRB 030329, we predict that the Low
Frequency Array (LOFAR, 30-240 MHz) will be able to observe afterglows of
similar GRBs, and constrain the physics of the blast wave during its
non-relativistic phase.
|
astro-ph
|
radio observations of gammaray burst grb afterglows are essential for our understanding of the physics of relativistic blast waves as they enable us to follow the evolution of grb explosions much longer than the afterglows in any other wave band we have performed a threeyear monitoring campaign of grb 030329 with the westerbork synthesis radio telescopes wsrt and the giant metrewave radio telescope gmrt our observations combined with observations at other wavelengths have allowed us to determine the grb blast wave physical parameters such as the total burst energy and the ambient medium density as well as investigate the jet nature of the relativistic outflow further by modeling the latetime radio light curve of grb 030329 we predict that the low frequency array lofar 30240 mhz will be able to observe afterglows of similar grbs and constrain the physics of the blast wave during its nonrelativistic phase
|
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|
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|
706.1325
|
Possible astronomical references in the planning of the Great Hopewell
Road
|
The possible existence of astronomical references in the planning of the
so-called Great Hopewell Road, a 90 Kilometres straight road composed of two
parallel earthen embankments which, according to recent surveys, likely
connected the Hopewell ceremonial centres of Newark and Chillicothe, Ohio, are
investigated. It turns out that a very peculiar, although simple, set of
astronomical alignments took place in connection with the road during possible
periods of its construction. The possibility of a non-fortuitous connection is
thus proposed and analysed.
|
physics.hist-ph
|
the possible existence of astronomical references in the planning of the socalled great hopewell road a 90 kilometres straight road composed of two parallel earthen embankments which according to recent surveys likely connected the hopewell ceremonial centres of newark and chillicothe ohio are investigated it turns out that a very peculiar although simple set of astronomical alignments took place in connection with the road during possible periods of its construction the possibility of a nonfortuitous connection is thus proposed and analysed
|
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|
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|
706.1326
|
The oscillation stability problem for the Urysohn sphere: A
combinatorial approach
|
We study the oscillation stability problem for the Urysohn sphere, an analog
of the distortion problem for $\ell_2$ in the context of the Urysohn space
$\Ur$. In particular, we show that this problem reduces to a purely
combinatorial problem involving a family of countable ultrahomogeneous metric
spaces with finitely many distances.
|
math.MG math.CO
|
we study the oscillation stability problem for the urysohn sphere an analog of the distortion problem for ell_2 in the context of the urysohn space ur in particular we show that this problem reduces to a purely combinatorial problem involving a family of countable ultrahomogeneous metric spaces with finitely many distances
|
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|
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|
706.1327
|
Hopf Algebras of Heap Ordered Trees and Permutations
|
It is known that there is a Hopf algebra structure on the vector space with
basis all heap-ordered trees. We give a new bialgebra structure on the space
with basis all permutations and show that there is a direct bialgebra
isomorphism between the Hopf algebra of heap-ordered trees and the bialgebra of
permutations.
|
math.RA
|
it is known that there is a hopf algebra structure on the vector space with basis all heapordered trees we give a new bialgebra structure on the space with basis all permutations and show that there is a direct bialgebra isomorphism between the hopf algebra of heapordered trees and the bialgebra of permutations
|
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|
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|
706.1328
|
N = 4 Superfiel Phase Space Coordinates and Hamiltonian Quantization
|
The N = 4 superfield phase space coordinates are given in the harmonic
superspace. The expressions of the N = 4 classical equations of motion are
determined in terms of the spinorial and harmonic supercharges. Furthermore,
the N = 4 supersymmetric actions are obtained by means of the fermionic and
harmonic functionals. On the other hand, the Hamiltonian quantization is
studied by performing the N = 4 supersymmetric action in harmonic subspace in
terms of analytic N = 4 superfield phase space coordinates.
|
hep-th
|
the n 4 superfield phase space coordinates are given in the harmonic superspace the expressions of the n 4 classical equations of motion are determined in terms of the spinorial and harmonic supercharges furthermore the n 4 supersymmetric actions are obtained by means of the fermionic and harmonic functionals on the other hand the hamiltonian quantization is studied by performing the n 4 supersymmetric action in harmonic subspace in terms of analytic n 4 superfield phase space coordinates
|
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|
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|
706.1329
|
Solidity of viscous liquids. V. Long-wavelength dominance of the
dynamics
|
This paper is the fifth in a series exploring the physical consequences of
the solidity of glass-forming liquids. Paper IV proposed a model where the
density field is described by a time-dependent Ginzburg-Landau equation of the
nonconserved type with rates in $k$ space of the form $\Gamma_0+Dk^2$. The
model assumes that $D\gg\Gamma_0a^2$ where $a$ is the average intermolecular
distance; this inequality expresses a long-wavelength dominance of the dynamics
which implies that the Hamiltonian (free energy) to a good approximation may be
taken to be ultralocal. In the present paper we argue that this is the simplest
model consistent with the following three experimental facts: 1) Viscous
liquids approaching the glass transition do not develop long-range order; 2)
The glass has lower compressibility than the liquid; 3) The alpha process
involves several decades of relaxation times shorter than the mean relaxation
time. The paper proceeds to list six further experimental facts characterizing
equilibrium viscous liquid dynamics and shows that these are readily understood
in terms of the model; some are direct consequences, others are quite natural
when viewed in light of the model.
|
cond-mat.soft
|
this paper is the fifth in a series exploring the physical consequences of the solidity of glassforming liquids paper iv proposed a model where the density field is described by a timedependent ginzburglandau equation of the nonconserved type with rates in k space of the form gamma_0dk2 the model assumes that dgggamma_0a2 where a is the average intermolecular distance this inequality expresses a longwavelength dominance of the dynamics which implies that the hamiltonian free energy to a good approximation may be taken to be ultralocal in the present paper we argue that this is the simplest model consistent with the following three experimental facts 1 viscous liquids approaching the glass transition do not develop longrange order 2 the glass has lower compressibility than the liquid 3 the alpha process involves several decades of relaxation times shorter than the mean relaxation time the paper proceeds to list six further experimental facts characterizing equilibrium viscous liquid dynamics and shows that these are readily understood in terms of the model some are direct consequences others are quite natural when viewed in light of the model
|
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|
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|
706.133
|
Note on: Considering the Case for Biodiversity Cycles: Reexamining the
Evidence for Periodicity in the Fossil Record, by Lieberman and Melott, arXiv
preprint 0704.2896
|
Lieberman and Melott built their recent arXiv preprint 0704.2896 on my
published paper and (a preprint of) a subsequent comment by Liebermans
associate Cornette. But had this group waited for the Cornette comment to
actually appear in print together with the expected Reply, they would have
learned that his comment exposes Cornettes confusion that likely was due to
journal misprint of my figure. Thus 0704.2896 is baseless. Despite receiving
the extended Reply with Errata, these authors still fail to recognize that
detrending of paleontological records-which they erroneously promote as a
must-is an arbitrary rather than a universal operation.
|
q-bio.PE astro-ph physics.geo-ph
|
lieberman and melott built their recent arxiv preprint 07042896 on my published paper and a preprint of a subsequent comment by liebermans associate cornette but had this group waited for the cornette comment to actually appear in print together with the expected reply they would have learned that his comment exposes cornettes confusion that likely was due to journal misprint of my figure thus 07042896 is baseless despite receiving the extended reply with errata these authors still fail to recognize that detrending of paleontological recordswhich they erroneously promote as a mustis an arbitrary rather than a universal operation
|
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|
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|
706.1331
|
On a Smale Theorem and Nonhomogeneous Equilibria in Cooperative Systems
|
A standard result by Smale states that n dimensional strongly cooperative
dynamical systems can have arbitrary dynamics when restricted to unordered
invariant hyperspaces. In this paper this result is extended to the case when
all solutions of the strongly cooperative system are bounded and converge
towards one of only two equilibria outside of the hyperplane.
An application is given in the context of strongly cooperative systems of
reaction diffusion equations. It is shown that such a system can have a
continuum of spatially inhomogeneous steady states, even when all solutions of
the underlying reaction system converge to one of only three equilibria.
|
math.DS math.AP
|
a standard result by smale states that n dimensional strongly cooperative dynamical systems can have arbitrary dynamics when restricted to unordered invariant hyperspaces in this paper this result is extended to the case when all solutions of the strongly cooperative system are bounded and converge towards one of only two equilibria outside of the hyperplane an application is given in the context of strongly cooperative systems of reaction diffusion equations it is shown that such a system can have a continuum of spatially inhomogeneous steady states even when all solutions of the underlying reaction system converge to one of only three equilibria
|
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|
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|
706.1332
|
Constraints on Galaxy Structure and Evolution from the Light of Nearby
Systems
|
We review knowledge of galaxy structures obtained by their emitted light and
in the local universe where they can be studied in great detail. We discuss the
shapes of, and stellar motions within, galaxies, compositional clues derived
from their spectra, and what luminous matter implies about their dark matter
content. Implications on the current theory of hierarchical galaxy formation
are explored.
|
astro-ph
|
we review knowledge of galaxy structures obtained by their emitted light and in the local universe where they can be studied in great detail we discuss the shapes of and stellar motions within galaxies compositional clues derived from their spectra and what luminous matter implies about their dark matter content implications on the current theory of hierarchical galaxy formation are explored
|
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|
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|
706.1333
|
An explicit construction of the Quillen homotopical category of dg Lie
algebras
|
Let $\g_1$ and $\g_2$ be two dg Lie algebras, then it is well-known that the
$L_\infty$ morphisms from $\g_1$ to $\g_2$ are in 1-1 correspondence to the
solutions of the Maurer-Cartan equation in some dg Lie algebra
$\Bbbk(\g_1,\g_2)$. Then the gauge action by exponents of the zero degree
component $\Bbbk(\g_1,\g_2)^0$ on $MC\subset\Bbbk(\g_1,\g_2)^1$ gives an
explicit "homotopy relation" between two $L_\infty$ morphisms. We prove that
the quotient category by this relation (that is, the category whose objects are
$L_\infty$ algebras and morphisms are $L_\infty$ morphisms modulo the gauge
relation) is well-defined, and is a localization of the category of dg Lie
algebras and dg Lie maps by quasi-isomorphisms. As localization is unique up to
an equivalence, it is equivalent to the Quillen-Hinich homotopical category of
dg Lie algebras [Q1,2], [H1,2]. Moreover, we prove that the Quillen's concept
of a homotopy coincides with ours. The last result was conjectured by
V.Dolgushev [D].
|
math.KT math.QA
|
let g_1 and g_2 be two dg lie algebras then it is wellknown that the l_infty morphisms from g_1 to g_2 are in 11 correspondence to the solutions of the maurercartan equation in some dg lie algebra bbbkg_1g_2 then the gauge action by exponents of the zero degree component bbbkg_1g_20 on mcsubsetbbbkg_1g_21 gives an explicit homotopy relation between two l_infty morphisms we prove that the quotient category by this relation that is the category whose objects are l_infty algebras and morphisms are l_infty morphisms modulo the gauge relation is welldefined and is a localization of the category of dg lie algebras and dg lie maps by quasiisomorphisms as localization is unique up to an equivalence it is equivalent to the quillenhinich homotopical category of dg lie algebras q12 h12 moreover we prove that the quillens concept of a homotopy coincides with ours the last result was conjectured by vdolgushev d
|
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|
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|
706.1334
|
Transients from initial conditions based on Lagrangian perturbation
theory in N-body simulations
|
We explore the initial conditions for cosmological N-body simulations
suitable for calculating the skewness and kurtosis of the density field. In
general, the initial conditions based on the perturbation theory (PT) provide
incorrect second-order and higher-order growth. These errors implied by the use
of the perturbation theory to set up the initial conditions in N-body
simulations are called transients. Unless these transients are completely
suppressed compared with the dominant growing mode, we can not reproduce the
correct evolution of cumulants with orders higher than two, even though there
is no problem with the numerical scheme. We investigate the impact of
transients on the observable statistical quantities by performing $N$-body
simulations with initial conditions based on Lagrangian perturbation theory
(LPT). We show that the effects of transients on the kurtosis from the initial
conditions, based on second-order Lagrangian perturbation theory (2LPT) have
almost disappeared by $z\sim5$, as long as the initial conditions are set at $z
> 30$. This means that for practical purposes, the initial conditions based on
2LPT are accurate enough for numerical calculations of skewness and kurtosis.
|
astro-ph
|
we explore the initial conditions for cosmological nbody simulations suitable for calculating the skewness and kurtosis of the density field in general the initial conditions based on the perturbation theory pt provide incorrect secondorder and higherorder growth these errors implied by the use of the perturbation theory to set up the initial conditions in nbody simulations are called transients unless these transients are completely suppressed compared with the dominant growing mode we can not reproduce the correct evolution of cumulants with orders higher than two even though there is no problem with the numerical scheme we investigate the impact of transients on the observable statistical quantities by performing nbody simulations with initial conditions based on lagrangian perturbation theory lpt we show that the effects of transients on the kurtosis from the initial conditions based on secondorder lagrangian perturbation theory 2lpt have almost disappeared by zsim5 as long as the initial conditions are set at z 30 this means that for practical purposes the initial conditions based on 2lpt are accurate enough for numerical calculations of skewness and kurtosis
|
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|
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|
706.1335
|
Geometric mesoscopic correlations in quasi-one dimension
|
We study analytically and numerically field/intensity correlations in wave
transport through volume-disordered waveguide. The obtained channel and spacial
correlations deviate from those found in framework of
Dorokhov-Mello-Pereyra-Kumar (DMPK) formalism, that we relate to
inapplicability of equivalent channel approximation in DMPK. We show that this
can be remedied by introducing boundary correction -- an escape function which
depends on the waveguide geometry -- that describes wave transport near a
boundary between random medium and free space. We obtain the expressions for
field/intensity channel and spacial correlation functions which agree with the
numerics and are consistent with the perturbative expressions in slab geometry
as well as experiments conducted in Q1D.
|
cond-mat.mes-hall cond-mat.dis-nn
|
we study analytically and numerically fieldintensity correlations in wave transport through volumedisordered waveguide the obtained channel and spacial correlations deviate from those found in framework of dorokhovmellopereyrakumar dmpk formalism that we relate to inapplicability of equivalent channel approximation in dmpk we show that this can be remedied by introducing boundary correction an escape function which depends on the waveguide geometry that describes wave transport near a boundary between random medium and free space we obtain the expressions for fieldintensity channel and spacial correlation functions which agree with the numerics and are consistent with the perturbative expressions in slab geometry as well as experiments conducted in q1d
|
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|
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|
706.1336
|
Can aerosols be trapped in open flows?
|
The fate of aerosols in open flows is relevant in a variety of physical
contexts. Previous results are consistent with the assumption that such
finite-size particles always escape in open chaotic advection. Here we show
that a different behavior is possible. We analyze the dynamics of aerosols both
in the absence and presence of gravitational effects, and both when the
dynamics of the fluid particles is hyperbolic and nonhyperbolic. Permanent
trapping of aerosols much heavier than the advecting fluid is shown to occur in
all these cases. This phenomenon is determined by the occurrence of multiple
vortices in the flow and is predicted to happen for realistic particle-fluid
density ratios.
|
nlin.CD astro-ph physics.flu-dyn
|
the fate of aerosols in open flows is relevant in a variety of physical contexts previous results are consistent with the assumption that such finitesize particles always escape in open chaotic advection here we show that a different behavior is possible we analyze the dynamics of aerosols both in the absence and presence of gravitational effects and both when the dynamics of the fluid particles is hyperbolic and nonhyperbolic permanent trapping of aerosols much heavier than the advecting fluid is shown to occur in all these cases this phenomenon is determined by the occurrence of multiple vortices in the flow and is predicted to happen for realistic particlefluid density ratios
|
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|
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|
706.1337
|
A note on Poisson homogeneous spaces
|
We identify the cotangent bundle Lie algebroid of a Poisson homogeneous space
G/H of a Poisson Lie group G as a quotient of a transformation Lie algebroid
over G. As applications, we describe the modular vector fields of G/H, and we
identify the Poisson cohomology of G/H with coefficients in powers of its
canonical line bundle with relative Lie algebra cohomology of the Drinfeld Lie
algebra associated to G/H. We also construct a Poisson groupoid over G/H which
is symplectic near the identity section. This note serves as preparation for
forthcoming papers, in which we will compute explicitly the Poisson cohomology
and study their symplectic groupoids for certain examples of Poisson
homogeneous spaces related to semi-simple Lie groups.
|
math.DG math.SG
|
we identify the cotangent bundle lie algebroid of a poisson homogeneous space gh of a poisson lie group g as a quotient of a transformation lie algebroid over g as applications we describe the modular vector fields of gh and we identify the poisson cohomology of gh with coefficients in powers of its canonical line bundle with relative lie algebra cohomology of the drinfeld lie algebra associated to gh we also construct a poisson groupoid over gh which is symplectic near the identity section this note serves as preparation for forthcoming papers in which we will compute explicitly the poisson cohomology and study their symplectic groupoids for certain examples of poisson homogeneous spaces related to semisimple lie groups
|
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|
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|
706.1338
|
Supersymmetric Hamiltonian Approach to Edge Excitations in $\nu = 5/2$
Fractional Quantum Hall Effect
|
A supersymmetric Hamiltonian is constructed for the edge excitations of the
Moore-Read (Pfaffian) like state, which is a realization of the N=2
supersymmetric CS model. Fermionic generators and their conjugates are
introduced to deal with the fermion pairing, whose condensation form a BCS like
state. After Bogoliubov transformation, a N=2 supersymmetric and
nonrelativistic Hamiltonian is found to take a known form, which is integrable.
The main difference between the Moore-Read state and our BCS like state is that
the number of fermion pairs in our formalism is not fixed. However, we have
also found that the excited states in our model looks similar but not exactly
the same as Moore and Read's.
|
hep-th cond-mat.mes-hall
|
a supersymmetric hamiltonian is constructed for the edge excitations of the mooreread pfaffian like state which is a realization of the n2 supersymmetric cs model fermionic generators and their conjugates are introduced to deal with the fermion pairing whose condensation form a bcs like state after bogoliubov transformation a n2 supersymmetric and nonrelativistic hamiltonian is found to take a known form which is integrable the main difference between the mooreread state and our bcs like state is that the number of fermion pairs in our formalism is not fixed however we have also found that the excited states in our model looks similar but not exactly the same as moore and reads
|
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|
[-0.11344086237243443, 0.22675093465451418, -0.09428649430628866, 0.10812781666131091, -0.04461829559087554, -0.19376335663504765, 0.014021451922807111, 0.28818915606409845, -0.18379797089645372, -0.2726804301367208, 0.03264120626928551, -0.30920809070604655, -0.12811596305774792, 0.09790107604931109, 0.006740605177973131, 0.0509083987230302, 0.022916962251266732, 0.11102975004385891, -0.1161716985142058, -0.24574346272441158, 0.3135756568933305, -0.02633570203657395, 0.26873878830312087, 0.012861559963701958, 0.04135851875928763, -0.0028011534970054136, 0.09028109271145825, -0.04668027592872802, -0.0593085521381259, 0.06723676190085826, 0.2498085163866303, 0.04637307873261826, 0.16344199289700814, -0.3989077790673556, -0.19558806402242876, 0.10400892358094486, 0.1668819412214881, 0.16847913055140193, -0.023770122198454504, -0.31375603032730787, 0.03044725748726965, -0.20567915804817208, -0.13627415812308236, -0.0849488868012226, 0.015806229843292385, -0.06674632137063392, -0.23981123425203674, 0.06523649071443417, 0.0714328845414067, -0.014318558181652665, -0.04353970905348043, -0.14399387688484108, -0.11095277830567543, 0.06472081010412824, 0.02356596892475084, 0.058929489854823, 0.08027226627122477, -0.18391888335983303, -0.11007037922640198, 0.4066146291775762, -0.04957350906001271, -0.22303085195432817, 0.18173241603030224, -0.09957016137403636, -0.1298231701907103, 0.11070122556286931, 0.027408770422750552, 0.10001766689362869, -0.11769988921670509, 0.1407526915739124, -0.11386340106504836, 0.14759946621156164, 0.031361564426333643, 0.06366805185098201, 0.20545291554714953, 0.10502995862459232, 0.04184713094894375, 0.15474185599928855, -0.03849813564115071, -0.18015051593621528, -0.33753162370495765, -0.19550931449940176, -0.23542282705394818, 0.06608542204178645, 0.02144535766949827, -0.1955526504399521, 0.4100965471297968, 0.11344954516971484, 0.2000775860381379, 0.049876169187232984, 0.20969669669076602, 0.1571314912019131, 0.07969192090968136, 0.0705255962613072, 0.2144578776392986, 0.1383882884401828, 0.04543551873315924, -0.2658542181104297, -0.041668193449108264, 0.12286012710371454]
|
706.1339
|
Verification theorem and construction of $\epsilon$-optimal controls for
control of abstract evolution equations
|
We study several aspects of the dynamic programming approach to optimal
control of abstract evolution equations, including a class of semilinear
partial differential equations. We introduce and prove a verification theorem
which provides a sufficient condition for optimality. Moreover we prove sub-
and superoptimality principles of dynamic programming and give an explicit
construction of $\epsilon$-optimal controls.
|
math.OC
|
we study several aspects of the dynamic programming approach to optimal control of abstract evolution equations including a class of semilinear partial differential equations we introduce and prove a verification theorem which provides a sufficient condition for optimality moreover we prove sub and superoptimality principles of dynamic programming and give an explicit construction of epsilonoptimal controls
|
[['we', 'study', 'several', 'aspects', 'of', 'the', 'dynamic', 'programming', 'approach', 'to', 'optimal', 'control', 'of', 'abstract', 'evolution', 'equations', 'including', 'a', 'class', 'of', 'semilinear', 'partial', 'differential', 'equations', 'we', 'introduce', 'and', 'prove', 'a', 'verification', 'theorem', 'which', 'provides', 'a', 'sufficient', 'condition', 'for', 'optimality', 'moreover', 'we', 'prove', 'sub', 'and', 'superoptimality', 'principles', 'of', 'dynamic', 'programming', 'and', 'give', 'an', 'explicit', 'construction', 'of', 'epsilonoptimal', 'controls']]
|
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|
706.134
|
Cluster abundances and S-Z power spectra: effects of non-Gaussianity and
early dark energy
|
In the standard Lambda CDM cosmological model with a Gaussian primordial
density fluctuation field, the relatively low value of the mass variance
parameter (sigma_8=0.74{+0.05}{-0.06}, obtained from the WMAP 3-year data)
results in a reduced likelihood that the measured level of CMB anisotropy on
the scales of clusters is due to the Sunyaev-Zeldovich (S-Z) effect. To assess
the feasibility of producing higher levels of S-Z power, we explore two
alternative models which predict higher cluster abundance. In the first model
the primordial density field has a chi^2_1 distribution, whereas in the second
an early dark energy component gives rise to the desired higher cluster
abundance. We carry out the necessary detailed calculations of the levels of
S-Z power spectra, cluster number counts, and angular 2-point correlation
function of clusters, and compare (in a self-consistent way) their predicted
redshift distributions. Our results provide a sufficient basis upon which the
viability of the three models may be tested by future high quality
measurements.
|
astro-ph
|
in the standard lambda cdm cosmological model with a gaussian primordial density fluctuation field the relatively low value of the mass variance parameter sigma_8074005006 obtained from the wmap 3year data results in a reduced likelihood that the measured level of cmb anisotropy on the scales of clusters is due to the sunyaevzeldovich sz effect to assess the feasibility of producing higher levels of sz power we explore two alternative models which predict higher cluster abundance in the first model the primordial density field has a chi2_1 distribution whereas in the second an early dark energy component gives rise to the desired higher cluster abundance we carry out the necessary detailed calculations of the levels of sz power spectra cluster number counts and angular 2point correlation function of clusters and compare in a selfconsistent way their predicted redshift distributions our results provide a sufficient basis upon which the viability of the three models may be tested by future high quality measurements
|
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|
[-0.09604855603977756, 0.09971456913178298, -0.1235026642973037, 0.11739451396967278, -0.05680548469389572, -0.04083587205822363, 0.026938473141705326, 0.31823936940621844, -0.19904658583771884, -0.3573990672059451, 0.029099225707252586, -0.2768045060172583, -0.02527164461958052, 0.1817842873601161, 0.042750631002182106, 0.025939058334531508, 0.03120495448088121, 0.009133874706860995, -0.04529945966236677, -0.28173212758294724, 0.29561175633977466, 0.18943313575999918, 0.293966851601342, -0.0029744525592328994, 0.06486002564116868, -0.07366592032622923, -0.09583940660235407, 0.042089354738874256, -0.1526120159637828, 0.08356199201610841, 0.1853772787860563, 0.12794784660913847, 0.23218623144440823, -0.38565506338604594, -0.22561143704619752, 0.12524486304430654, 0.12599933826885884, 0.10831674768109133, -0.05726517014770693, -0.25125763151478375, 0.08007214033394852, -0.2055907974088471, -0.12706619736580355, -0.051699802273614974, -0.03246760253981927, 0.018811301527392563, -0.2603928455409342, 0.19030692990658418, -0.0188684508280606, 0.02679802009753653, -0.09825278786098901, -0.16963873827118287, -0.07587329265017226, 0.07933823431625306, 0.022067885425632948, 0.02397246655671998, 0.15045949411959206, -0.16888958961796602, -0.06627347145585413, 0.38580387739359207, -0.12020132434115095, -0.11518059679125466, 0.14251165046450337, -0.20258486943624024, -0.18241267327992422, 0.09265555353518927, 0.16292850762706707, 0.04039189480127966, -0.14068862737841764, 0.06787157351676076, 0.03196414578457088, 0.23047837409346053, 0.04761539341050124, 0.009664981852398318, 0.2959757712376802, 0.10969196034100422, 0.06917297181749493, 0.12575276760214577, -0.17126063448259807, -0.01981636569849889, -0.2665033816709915, -0.09836687621478953, -0.17614859711589678, 0.04347888299750176, -0.15475201811740297, -0.15038732072022162, 0.3995940858240491, 0.17680069413138613, 0.24991336898034755, 0.0882208052826401, 0.33572068916188563, 0.13923856897284012, 0.05747366832633673, -0.010864016244117662, 0.2613241323855641, 0.1875529146223159, 0.06104845939930411, -0.23630840693612923, 0.03781541094547079, -0.025196135719160333]
|
706.1341
|
A Study in Depth of f0(1370)
|
Claims have been made that f0(1370) does not exist. The five primary sets of
data requiring its existence are refitted. Major dispersive effects due to the
opening of the 4pi threshold are included for the first time; the sigma -> 4pi
amplitude plays a strong role. Crystal Barrel data on pbar-p -> 3pizero at rest
require f0(1370) signals of at least 32 and 33 standard deviations in 1S0 and
3P1 annihilation respectively. Furthermore, they agree within 5 MeV for mass
and width. Data on pbar-p -> eta-eta-pizero agree and require at least a 19
standard deviation contribution. This alone is sufficient to demonstrate the
existence of f0(1370). BES II data for J/Psi -> phi-pi-pi contain a visible
f0(1370) signal > 8 standard devations. In all cases, a resonant phase
variation is required. The possibility of a second pole in the sigma amplitude
due to the opening of the 4pi channel is excluded. Cern-Munich data for pi-pi
elastic scattering are fitted well with the inclusion of some mixing between
sigma, f0(1370) and f0(1500). The pi-pi widths for f2(1565), rho3(1690),
rho3(1990) and f4(2040) are determined.
|
hep-ex
|
claims have been made that f01370 does not exist the five primary sets of data requiring its existence are refitted major dispersive effects due to the opening of the 4pi threshold are included for the first time the sigma 4pi amplitude plays a strong role crystal barrel data on pbarp 3pizero at rest require f01370 signals of at least 32 and 33 standard deviations in 1s0 and 3p1 annihilation respectively furthermore they agree within 5 mev for mass and width data on pbarp etaetapizero agree and require at least a 19 standard deviation contribution this alone is sufficient to demonstrate the existence of f01370 bes ii data for jpsi phipipi contain a visible f01370 signal 8 standard devations in all cases a resonant phase variation is required the possibility of a second pole in the sigma amplitude due to the opening of the 4pi channel is excluded cernmunich data for pipi elastic scattering are fitted well with the inclusion of some mixing between sigma f01370 and f01500 the pipi widths for f21565 rho31690 rho31990 and f42040 are determined
|
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|
[-0.12891002837969953, 0.16542420324055884, -0.041910015972566675, 0.10804336805608467, -0.05774351139502712, -0.12586774827709057, 0.05171635142399062, 0.33970050489658427, -0.1739323998710419, -0.295365835944105, 0.06125576023933017, -0.35936316919523753, 0.004582241811821687, 0.17392803107163515, 0.05871624586937799, 0.0699302891517545, 0.09017838850542474, 0.03382741375130483, -0.03858297690013209, -0.16145692810539328, 0.270443737726316, 0.009327756107153222, 0.22030929767061025, 0.12036205542905407, 0.024445218094303434, 0.016858851740500707, -0.04286108122223282, -0.07125030321546139, -0.135934195646037, 0.027129405659848248, 0.23181435052069954, 0.07085809188001072, 0.1514718015253378, -0.3473381166956548, -0.10640956081407166, 0.1380777834518545, 0.1367680150849093, 0.07347206119983189, -0.006834561118973826, -0.2820503956681096, 0.1355553612637537, -0.11182743407941113, -0.13029114608706413, -0.027323095815727252, 0.027434344619550025, -0.04742889726084882, -0.3007852589241871, 0.1470437691665399, 0.00029354278418374646, 0.06775118988114355, -0.03981165043225555, -0.22018870068767546, -0.05012536132387046, 0.06271984892758145, 0.06218104939319022, 0.06910765084341683, 0.11693078975846198, -0.10270813590413409, -0.1110795740594809, 0.379871043444199, -0.06876707003162853, -0.14747995838316175, 0.13755963901465962, -0.171186445648889, -0.12074420352509224, 0.24784204256774364, 0.14390348057475358, 0.0072365674516721365, -0.15703274921952992, 0.09157238829541074, -0.01748969000677214, 0.2322160883073363, 0.13731016170891835, 0.07451218068225031, 0.17926522366429581, 0.16934284404851496, -0.018652375612873584, 0.03274396686525694, -0.15593708799777276, -0.03981852263544054, -0.38797915108794956, -0.0775966383998507, -0.08044836974245143, 0.03380441685127236, -0.018605630351906245, -0.1057225599612013, 0.32055456425470097, 0.04007990469610126, 0.23894523059408684, 0.03170403913359276, 0.24919920149205746, 0.083436720334154, 0.0925933337615182, 0.06867189339800985, 0.35327516601975584, 0.15809874255852452, 0.12551011756897487, -0.23423296698197138, 0.04319003716060335, -0.0502469473329089]
|
706.1342
|
Low-temperature electron dephasing time in AuPd revisited
|
Ever since the first discoveries of the quantum-interference transport in
mesoscopic systems, the electron dephasing times, $\tau_\phi$, in the
concentrated AuPd alloys have been extensively measured. The samples were made
from different sources with different compositions, prepared by different
deposition methods, and various geometries (1D narrow wires, 2D thin films, and
3D thickfilms) were studied. Surprisingly, the low-temperature behavior of
$\tau_\phi$ inferred by different groups over two decades reveals a systematic
correlation with the level of disorder of the sample. At low temperatures,
where $\tau_\phi$ is (nearly) independent of temperature, a scaling
$\tau_\phi^{\rm max} \propto D^{-\alpha}$ is found, where $tau_\phi^{\rm max}$
is the maximum value of $\tau_\phi$ measured in the experiment, $D$ is the
electron diffusion constant, and the exponent $\alpha$ is close to or slightly
larger than 1. We address this nontrivial scaling behavior and suggest that the
most possible origin for this unusual dephasing is due to dynamical structure
defects, while other theoretical explanations may not be totally ruled out.
|
cond-mat.mes-hall cond-mat.dis-nn
|
ever since the first discoveries of the quantuminterference transport in mesoscopic systems the electron dephasing times tau_phi in the concentrated aupd alloys have been extensively measured the samples were made from different sources with different compositions prepared by different deposition methods and various geometries 1d narrow wires 2d thin films and 3d thickfilms were studied surprisingly the lowtemperature behavior of tau_phi inferred by different groups over two decades reveals a systematic correlation with the level of disorder of the sample at low temperatures where tau_phi is nearly independent of temperature a scaling tau_phirm max propto dalpha is found where tau_phirm max is the maximum value of tau_phi measured in the experiment d is the electron diffusion constant and the exponent alpha is close to or slightly larger than 1 we address this nontrivial scaling behavior and suggest that the most possible origin for this unusual dephasing is due to dynamical structure defects while other theoretical explanations may not be totally ruled out
|
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|
[-0.11221767778915819, 0.21949388787616045, -0.06095125029969495, 0.0376623510645004, 0.01302882738491462, -0.18675636455081984, 0.02245876572560519, 0.38144483740907165, -0.24000444435878307, -0.310036566411145, 0.0540897875551309, -0.334632760938257, -0.07056904862329247, 0.21402402693493058, 0.016634543662075885, 0.054800545369653265, -0.03138866049994249, -0.035752612156284155, -0.1106218899385567, -0.23402605043520452, 0.27916559781006073, 0.059374463686253875, 0.3074747549311724, 0.05059503623633645, 0.03304448597045848, -0.06086207487242064, 0.024031517685216386, 0.05556312897242606, -0.17743590410414073, 0.006860583779052831, 0.2352165728341788, -0.033152737290629376, 0.20614186039674678, -0.41389018121967636, -0.23520939185254974, 0.0656036003500958, 0.1541421475885727, 0.08551534334692405, -0.01911212495469954, -0.21633569466939662, 0.06896540329726122, -0.10582671568990917, -0.1003763219108805, -0.013265201251488178, 0.08748749859223608, -0.004160899855560274, -0.21457112833086284, 0.12862164721009323, 0.03478043465347582, 0.10386724642994523, -0.059691913753340486, -0.17097890964505497, -0.014833002899831627, 0.08944165524374056, 0.07480804301740136, 0.024178380041303172, 0.15668198222701904, -0.09860811673023591, -0.08034767391836795, 0.3632005505322013, -0.024585891360493405, -0.08889788574888371, 0.20016730076895328, -0.23966841499750444, -0.10362892284756527, 0.16552105351292995, 0.08841584016918205, 0.1248002407810418, -0.17167841158261582, 0.0529323873024623, -0.0044687593966955316, 0.1892901520448504, 0.0716312576449127, 0.04295200988999568, 0.20676524464615795, 0.18181104387476807, 0.012772508447233122, 0.11642662194026343, -0.11391618792113149, -0.06266800576595415, -0.19674095928203314, -0.12026861200283748, -0.20196290669264272, 0.11553843247975237, -0.09355461894847394, -0.12896474052504345, 0.363424135556852, 0.12675751960232445, 0.22011597968812566, 0.008088609577680473, 0.22639343923001434, 0.1207950447802432, 0.07700534240866545, 0.05471155557606835, 0.2562884507191484, 0.12194041836773976, 0.09215154924249873, -0.23153888080560137, 0.12756544484873303, -0.03692462508333847]
|
706.1343
|
Interacting like charges in Landau levels: Planar geometry, symmetries,
and effective quasiparticles
|
We consider a system of two interacting particles with like but unequal
charges in a magnetic field in the planar geometry. We construct a complete
basis of states compatible with both the axial symmetry and magnetic
translations. The basis is obtained using a canonical transformation that
generates effective quasiparticles with modified interactions. We establish a
connection of this transformation with the SU(2) algebra and make use of the
SU(2) Baker-Campbell-Hausdorff formulas for evaluating the interaction matrix
elements. We calculate analytically the eigenenergies of the problem (Haldane
pseudopotentials) in the first few Landau levels for a relatively wide class of
interaction potentials.
|
cond-mat.mes-hall
|
we consider a system of two interacting particles with like but unequal charges in a magnetic field in the planar geometry we construct a complete basis of states compatible with both the axial symmetry and magnetic translations the basis is obtained using a canonical transformation that generates effective quasiparticles with modified interactions we establish a connection of this transformation with the su2 algebra and make use of the su2 bakercampbellhausdorff formulas for evaluating the interaction matrix elements we calculate analytically the eigenenergies of the problem haldane pseudopotentials in the first few landau levels for a relatively wide class of interaction potentials
|
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|
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|
706.1344
|
A Class of Partially Solvable Two-Dimensional Quantum Models with
Periodic Potentials
|
The supersymmetrical approach is used to analyse a class of two-dimensional
quantum systems with periodic potentials. In particular, the method of
SUSY-separation of variables allowed us to find a part of the energy spectra
and the corresponding wave functions (partial solvability) for several models.
These models are not amenable to conventional separation of variables, and they
can be considered as two-dimensional generalizations of Lame, associated Lame,
and trigonometric Razavy potentials. All these models have the symmetry
operators of fourth order in momenta, and one of them (the Lame potential)
obeys the property of self-isospectrality.
|
hep-th cond-mat.mes-hall math-ph math.MP quant-ph
|
the supersymmetrical approach is used to analyse a class of twodimensional quantum systems with periodic potentials in particular the method of susyseparation of variables allowed us to find a part of the energy spectra and the corresponding wave functions partial solvability for several models these models are not amenable to conventional separation of variables and they can be considered as twodimensional generalizations of lame associated lame and trigonometric razavy potentials all these models have the symmetry operators of fourth order in momenta and one of them the lame potential obeys the property of selfisospectrality
|
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|
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|
706.1345
|
Spectroscopy and multiband photometry of the afterglow of intermediate
duration gamma-ray burst 040924 and its host galaxy
|
We present optical photometry and spectroscopy of the afterglow and host
galaxy of gamma-ray burst 040924. This GRB had a rather short duration of T90
~2.4s, and a well sampled optical afterglow light curve. We aim to use this
dataset to find further evidence that this burst is consistent with a massive
star core-collapse progenitor. We combine the afterglow data reported here with
data taken from the literature and compare the host properties with survey
data. We find that the global behaviour of the optical afterglow is well fit by
a broken power-law, with a break at ~0.03 days. We determine the redshift z =
0.858 +/- 0.001 from the detected emission lines in our spectrum. Using the
spectrum and photometry we derive global properties of the host, showing it to
have similar properties to long GRB hosts. We detect the [Ne III] emission line
in the spectrum, and compare the fluxes of this line of a sample of 15 long GRB
host galaxies with survey data, showing the long GRB hosts to be comparable to
local metal-poor emission line galaxies in their [Ne III] emission. We fit the
supernova bump accompanying this burst, and find that it is similar to other
long GRB supernova bumps, but fainter. All properties of GRB 040924 are
consistent with an origin in the core-collapse of a massive star: the
supernova, the spectrum and SED of the host and the afterglow.
|
astro-ph
|
we present optical photometry and spectroscopy of the afterglow and host galaxy of gammaray burst 040924 this grb had a rather short duration of t90 24s and a well sampled optical afterglow light curve we aim to use this dataset to find further evidence that this burst is consistent with a massive star corecollapse progenitor we combine the afterglow data reported here with data taken from the literature and compare the host properties with survey data we find that the global behaviour of the optical afterglow is well fit by a broken powerlaw with a break at 003 days we determine the redshift z 0858 0001 from the detected emission lines in our spectrum using the spectrum and photometry we derive global properties of the host showing it to have similar properties to long grb hosts we detect the ne iii emission line in the spectrum and compare the fluxes of this line of a sample of 15 long grb host galaxies with survey data showing the long grb hosts to be comparable to local metalpoor emission line galaxies in their ne iii emission we fit the supernova bump accompanying this burst and find that it is similar to other long grb supernova bumps but fainter all properties of grb 040924 are consistent with an origin in the corecollapse of a massive star the supernova the spectrum and sed of the host and the afterglow
|
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|
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|
706.1346
|
Southern wide very low-mass stars and brown dwarfs in resolved binary
and multiple systems
|
The results of the Koenigstuhl survey in the Southern Hemisphere are
presented. I have searched for common-proper motion companions to 173 field
very low-mass stars and brown dwarfs with spectral types > M5.0V and magnitudes
J <= 14.5 mag. I have measured for the first time the common-proper motion of
two new wide systems containing very low-mass components, Koenigstuhl 2 AB and
3 A-BC. Together with Koenigstuhl 1 AB and 2M0126-50AB, they are among the
widest systems in their respective classes (r = 450-11900 AU). Koenigstuhl 3
A-BC contains a well-known F8V star and a M8.0+L3.0V tight binary. I have
determined the minimum frequency of field wide multiples (r > 100 AU) with
late-type components at 5.0+/-1.8 % and the frequency of field wide late-type
binaries with mass ratios q > 0.5 at 1.2+/-0.9 %. These values represent a key
diagnostic of evolution history and low-mass star and brown-dwarf formation
scenarios. Additionally, the proper motions of 76 field very low-mass dwarfs
are measured here for the first time.
|
astro-ph
|
the results of the koenigstuhl survey in the southern hemisphere are presented i have searched for commonproper motion companions to 173 field very lowmass stars and brown dwarfs with spectral types m50v and magnitudes j 145 mag i have measured for the first time the commonproper motion of two new wide systems containing very lowmass components koenigstuhl 2 ab and 3 abc together with koenigstuhl 1 ab and 2m012650ab they are among the widest systems in their respective classes r 45011900 au koenigstuhl 3 abc contains a wellknown f8v star and a m80l30v tight binary i have determined the minimum frequency of field wide multiples r 100 au with latetype components at 5018 and the frequency of field wide latetype binaries with mass ratios q 05 at 1209 these values represent a key diagnostic of evolution history and lowmass star and browndwarf formation scenarios additionally the proper motions of 76 field very lowmass dwarfs are measured here for the first time
|
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|
[-0.12493654417722852, 0.13624166350780775, -0.026538359673245797, 0.04949777038426056, -0.07533165850069468, -0.11389631870249876, 0.042324907267230406, 0.40066495469824376, -0.15099105896734738, -0.3907804889250783, 0.05626383624879549, -0.28149743921630366, -0.019395476230714893, 0.19923941607740295, -0.02646608200643353, -0.03235206695314411, 0.1096351200750074, -0.039889137676174316, -0.031280783362409595, -0.25963962557313, 0.2759347220977085, -0.023714261707154256, 0.06503052192189748, -0.06101932633031584, 0.04360347213901438, -0.052746587477129285, -0.0626171404360263, -0.02971878446214184, -0.21316083553116372, 0.009427207569249823, 0.2674785337021834, 0.10223595484431032, 0.2220224866855748, -0.27148557614031854, -0.11528809825872083, 0.05229944942071091, 0.14544891044379601, -0.02510055045514733, -0.05125013716324362, -0.2527683187413171, 0.147054193718241, -0.17618160490742354, -0.121651457156986, 0.035655224271401574, 0.15480894672896572, 0.09016595416572652, -0.24442650892925036, 0.10256894830911997, 0.05899178534687226, 0.15611953439804005, -0.12709962383031997, -0.23235113590018516, -0.02589999591118267, 0.08346776471361282, -0.026191790856397414, 0.0915820073893388, 0.10916800725662822, -0.11421888202257142, -0.053333241763654386, 0.3890822844556238, -0.0870059198269597, -0.023690497765540074, 0.278518785027009, -0.21581176062456414, -0.16996717880645035, 0.137853934235806, 0.13414611452542058, 0.17287348999783303, -0.18074202419500326, 0.01612405288121604, 0.044417745713181384, 0.17547526782013098, 0.078284395602237, 0.07357288803021082, 0.34087806705479756, 0.10603315720302967, -0.005686963677846184, 0.015085445671295158, -0.27154456793413134, -0.04289680701397548, -0.20218881141597736, -0.12249981391809503, -0.12249086004434319, 0.04655846285993304, -0.1445876734848488, -0.11039666089677264, 0.35648732173810654, 0.07844569500759715, 0.19988991058567138, 0.05384805298386778, 0.226469867479622, 0.07317241343604755, 0.11667795611259563, 0.11568400010914553, 0.2990909566206834, 0.20206653625598248, 0.10477863094486485, -0.17535345284032483, -0.013255108771197309, -0.03291471769054762]
|
706.1347
|
The Two-State Vector Formalism
|
The two-state vector formalism (TSVF), the time-symmetric description of the
standard quantum mechanics originated by Aharonov, Bergmann and Lebowitz is
reviewed. The TSVF describes a quantum system at a particular time by two
quantum states: the usual one, evolving forward in time, defined by the results
of a complete measurement at the earlier time, and by the quantum state
evolving backward in time, defined by the results of a complete measurement at
a later time.
|
quant-ph
|
the twostate vector formalism tsvf the timesymmetric description of the standard quantum mechanics originated by aharonov bergmann and lebowitz is reviewed the tsvf describes a quantum system at a particular time by two quantum states the usual one evolving forward in time defined by the results of a complete measurement at the earlier time and by the quantum state evolving backward in time defined by the results of a complete measurement at a later time
|
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|
[-0.13012417171150445, 0.21603723692397275, -0.12738236819083493, 0.045905707511119546, 0.02580189565817515, -0.1503308530834814, 0.04306890801837047, 0.2521462833881378, -0.23131328789517283, -0.26383082032824556, 0.042486306463057795, -0.2405848994354407, -0.08598034419119358, 0.18209326927860578, -0.017631075357397396, 0.0905809985101223, 0.06579493265599012, 0.057351437568043666, -0.07286065151294073, -0.21364400457590818, 0.31105194583535195, 0.07711548320328196, 0.2502036945832272, -0.0010449457603196302, 0.1282018555700779, 0.09312631948230167, -0.07055371870597203, 0.02616466333468755, -0.12188319346557061, 0.05084410072226698, 0.22877450625101725, 0.10210602628688017, 0.29149980017915367, -0.4494189082831144, -0.2161573610516886, 0.02217261535425981, 0.04746508965889613, 0.15502809807347753, -0.025469516447434823, -0.3775423768659433, 0.017231680241723855, -0.1278978020697832, -0.14812609345341723, -1.7288774251937866e-05, 0.04076741128539046, -0.06212472543120384, -0.1517866256988297, 0.09985568468769392, 0.11370816329494118, 0.02358186977605025, -0.016213345130284627, -0.02153014954645187, 0.012875298094004393, 0.05759859242166082, -0.05590924388729036, 0.07334348435203235, 0.09174094187716643, -0.07928614359349012, -0.2280329006165266, 0.34517588576922814, -0.10980282167283197, -0.17776189401745796, 0.1266246296465397, -0.1317594074519972, -0.09183132746567328, 0.08406574777017037, 0.0791346159329017, 0.11158770898977916, -0.16968134543548027, 0.12941954682115464, -0.00888498722265164, 0.0849693330625693, 0.04532293230295181, 0.00865591964373986, 0.17732253635923068, 0.12191359146808585, -0.02959956863274177, 0.09512406090274453, -0.00880696455637614, -0.22188030583163101, -0.35080047195156416, -0.19955061410209357, -0.21735014155507087, 0.10869054393221934, -0.0462535566832715, -0.09230428293347359, 0.44043476566672324, 0.07093550809969505, 0.21523253424093128, 0.04730061315620939, 0.29538957272966704, 0.17565979075928528, 0.00799394831682245, 0.055393118603775895, 0.238769627759854, 0.16156002898079655, 0.18226866823931534, -0.22553259440387288, 0.0644508941968282, 0.10503707160552343]
|
706.1348
|
Weak Value and Weak Measurements
|
The weak value of a variable O is a description of an effective interaction
with that variable in the limit of weak coupling. It is particularly important
for a pre- and post-selected quantum system.
|
quant-ph
|
the weak value of a variable o is a description of an effective interaction with that variable in the limit of weak coupling it is particularly important for a pre and postselected quantum system
|
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|
[-0.17351990417741678, 0.1489316644596436, -0.08739263446563307, 0.06356728885678903, -0.007899383466471644, -0.18094543341602035, 0.07427323414423667, 0.3308717522989301, -0.22518576031057713, -0.2754276844618075, 0.07710766813868437, -0.2206464069758487, -0.09175409672453123, 0.20045206871102839, 0.0021191124448224027, 0.018514015355750042, 0.08988799045191091, 0.07928812346996411, -0.034616948454640806, -0.1827008389210438, 0.3475650058073156, 0.06912075492265798, 0.24802759728010962, 0.026749433086746755, 0.10524563187295023, 0.06453570796806804, 0.05489815281265799, 0.07390217510435511, -0.028616255732391866, 0.11284755389480029, 0.21927624631515594, 0.06868602412150186, 0.3127325476859422, -0.2988309215562528, -0.16770298080518842, 0.052431342548088115, 0.07525967598399695, 0.1436860528500641, -0.03177882898051072, -0.28648946428781047, 0.027747469803537515, -0.14488024974707514, -0.11033193947856917, -0.05602032398147618, 0.14211450769182513, 0.014535688904716688, -0.3709594149224679, 0.06474490876922466, 0.10284585905644823, 0.03150954830241116, -0.03353621150531313, -0.008969034078558358, 0.02269453653956161, 0.13302015747381923, -0.001061686930958839, 0.06933183256564114, 0.087352001135621, -0.2348054155214306, -0.024701793691800797, 0.3830698275209322, -0.14767034570275642, -0.1569293124929947, 0.2102227517787148, -0.08377294697086601, -0.12757486559669762, 0.09455347521340146, 0.10235451271428782, 0.15804005896343903, -0.14743107524426544, 0.13339003254762194, -0.030510628623340058, 0.19939792443833806, -0.02220113989075317, 0.10176826247890644, 0.20321651293403087, 0.1674338137073552, 0.06335375896271538, 0.1006346108556232, -0.07239583174369353, -0.1126889985821703, -0.36769864949233394, -0.23321760764263352, -0.17781339162577162, 0.11741399717078928, -0.1365124177566887, -0.21943106090047343, 0.33257779983036656, 0.15170347293400588, 0.2181350759449689, -0.04255156495663173, 0.24276512083323562, 0.19909670805175075, 0.007787569371216437, 0.001199628007324303, 0.336672734523959, 0.20926092077484904, 0.0969531381612315, -0.24274018617785154, 0.09457879372434143, 0.040959515978636986]
|
706.1349
|
Improved quark mass density- dependent model with quark-sigma meson and
quark-omega meson couplings
|
An improved quark mass density- dependent model with the non-linear scalar
sigma field and the $\omega$-meson field is presented. We show that the present
model can describe saturation properties, the equation of state, the
compressibility and the effective nuclear mass of nuclear matter under mean
field approximation successfully. The comparison of the present model and the
quark-meson coupling model is addressed.
|
nucl-th
|
an improved quark mass density dependent model with the nonlinear scalar sigma field and the omegameson field is presented we show that the present model can describe saturation properties the equation of state the compressibility and the effective nuclear mass of nuclear matter under mean field approximation successfully the comparison of the present model and the quarkmeson coupling model is addressed
|
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|
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|
706.135
|
The Anisotropic Distribution of Satellite Galaxies
|
We identify satellites of isolated galaxies in SDSS and examine their angular
distribution. Using mock catalogues generated from cosmological N-body
simulations, we demonstrate that the selection criteria used to select isolated
galaxies and their satellites must be very strict in order to correctly
identify systems in which the primary galaxy dominates its environment. The
criteria used in many previous studies instead select predominantly group
members. We refine a set of selection criteria for which the group
contamination is estimated to be less than 7% and present a catalogue of the
resulting sample. The angular distribution of satellites about their host is
biased towards the major axes for spheroidal galaxies and probably also for red
disc galaxies, but is isotropic for blue disc galaxies, i.e. it is the colour
of the host that determines the distribution of its satellites rather than its
morphology. The similar anisotropy measured in this study as in studies that
were dominated by groups implies that group-specific processes are not
responsible for the angular distribution. Satellites that are most likely to
have been recently accreted show a tendancy to lie along the same axis as the
surrounding large scale structure. The orientations of isolated early and
intermediate-type galaxies also align with the surrounding large scale
structures. We discuss the origin of the anisotropic satellite distribution and
consider the implications of our results, critically assessing the respective
roles played by the orientation of the visible galaxy within its dark matter
halo; anisotropic accretion of satellites from the larger scale environment;
and the biased nature of satellites as tracers of the underlying dark matter
subhalo population. (Abridged)
|
astro-ph
|
we identify satellites of isolated galaxies in sdss and examine their angular distribution using mock catalogues generated from cosmological nbody simulations we demonstrate that the selection criteria used to select isolated galaxies and their satellites must be very strict in order to correctly identify systems in which the primary galaxy dominates its environment the criteria used in many previous studies instead select predominantly group members we refine a set of selection criteria for which the group contamination is estimated to be less than 7 and present a catalogue of the resulting sample the angular distribution of satellites about their host is biased towards the major axes for spheroidal galaxies and probably also for red disc galaxies but is isotropic for blue disc galaxies ie it is the colour of the host that determines the distribution of its satellites rather than its morphology the similar anisotropy measured in this study as in studies that were dominated by groups implies that groupspecific processes are not responsible for the angular distribution satellites that are most likely to have been recently accreted show a tendancy to lie along the same axis as the surrounding large scale structure the orientations of isolated early and intermediatetype galaxies also align with the surrounding large scale structures we discuss the origin of the anisotropic satellite distribution and consider the implications of our results critically assessing the respective roles played by the orientation of the visible galaxy within its dark matter halo anisotropic accretion of satellites from the larger scale environment and the biased nature of satellites as tracers of the underlying dark matter subhalo population abridged
|
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|
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706.1351
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Scattering of charge carriers by point defects in bilayer graphene
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Theory of scattering of massive chiral fermions in bilayer graphene by radial
symmetric potential is developed. It is shown that in the case when the
electron wavelength is much larger than the radius of the potential the
scattering cross-section is proportional to the electron wavelength. This leads
to the mobility independent on the electron concentration. In contrast with the
case of single-layer, neutral and charged defects are, in general, equally
relevant for the resistivity of the bilayer graphene.
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cond-mat.mes-hall cond-mat.mtrl-sci
|
theory of scattering of massive chiral fermions in bilayer graphene by radial symmetric potential is developed it is shown that in the case when the electron wavelength is much larger than the radius of the potential the scattering crosssection is proportional to the electron wavelength this leads to the mobility independent on the electron concentration in contrast with the case of singlelayer neutral and charged defects are in general equally relevant for the resistivity of the bilayer graphene
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