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706.3114
|
Polynomial rate convergence to an invariant measure for the continuum
time limit of the Minority Game
|
In this paper we show that the continuum time version of the Minority Game
satisfies the criteria for the application of a theorem on the existence of an
invariant measure. We consider the special case of a game with "sufficiently"
asymmetric initial condition where the number of possible choices for each
individual is S=2 and $\Gamma<+\infty$. An upper bound for the asymptotic
behavior, as the number of agents grows to infinity, of the waiting time for
reaching the stationary state is then obtained.
|
math.PR
|
in this paper we show that the continuum time version of the minority game satisfies the criteria for the application of a theorem on the existence of an invariant measure we consider the special case of a game with sufficiently asymmetric initial condition where the number of possible choices for each individual is s2 and gammainfty an upper bound for the asymptotic behavior as the number of agents grows to infinity of the waiting time for reaching the stationary state is then obtained
|
[['in', 'this', 'paper', 'we', 'show', 'that', 'the', 'continuum', 'time', 'version', 'of', 'the', 'minority', 'game', 'satisfies', 'the', 'criteria', 'for', 'the', 'application', 'of', 'a', 'theorem', 'on', 'the', 'existence', 'of', 'an', 'invariant', 'measure', 'we', 'consider', 'the', 'special', 'case', 'of', 'a', 'game', 'with', 'sufficiently', 'asymmetric', 'initial', 'condition', 'where', 'the', 'number', 'of', 'possible', 'choices', 'for', 'each', 'individual', 'is', 's2', 'and', 'gammainfty', 'an', 'upper', 'bound', 'for', 'the', 'asymptotic', 'behavior', 'as', 'the', 'number', 'of', 'agents', 'grows', 'to', 'infinity', 'of', 'the', 'waiting', 'time', 'for', 'reaching', 'the', 'stationary', 'state', 'is', 'then', 'obtained']]
|
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|
706.3115
|
Finite jet determination of CR mappings
|
We prove the following finite jet determination result for CR mappings: Given
a smooth generic submanifold M of C^N, N >= 2, which is essentially finite and
of finite type at each of its points, for every point p on M there exists an
integer l(p), depending upper-semicontinuously on p, such that for every smooth
generic submanifold M' of C^N of the same dimension as M, if h_1 and h_2:
(M,p)->M' are two germs of smooth finite CR mappings with the same l(p) jet at
p, then necessarily their k-jets agree for all positive integers k. In the
hypersurface case, this result provides several new unique jet determination
properties for holomorphic mappings at the boundary in the real-analytic case;
in particular, it provides the finite jet determination of arbitrary
real-analytic CR mappings between real-analytic hypersurfaces in C^N of
D'Angelo finite type. It also yields a new boundary version of H. Cartan's
uniqueness theorem: if Omega and Omega' are two bounded domains in C^N with
smooth real-analytic boundary, then there exists an integer k, depending only
on the boundary of Omega, such that if H_1 and H_2: Omega -> Omega' are two
proper holomorphic mappings extending smoothly up to the boundary of Omega near
some point boundary point p and agreeing up to order k at p, then necessarily
H_1=H_2.
|
math.CV
|
we prove the following finite jet determination result for cr mappings given a smooth generic submanifold m of cn n 2 which is essentially finite and of finite type at each of its points for every point p on m there exists an integer lp depending uppersemicontinuously on p such that for every smooth generic submanifold m of cn of the same dimension as m if h_1 and h_2 mpm are two germs of smooth finite cr mappings with the same lp jet at p then necessarily their kjets agree for all positive integers k in the hypersurface case this result provides several new unique jet determination properties for holomorphic mappings at the boundary in the realanalytic case in particular it provides the finite jet determination of arbitrary realanalytic cr mappings between realanalytic hypersurfaces in cn of dangelo finite type it also yields a new boundary version of h cartans uniqueness theorem if omega and omega are two bounded domains in cn with smooth realanalytic boundary then there exists an integer k depending only on the boundary of omega such that if h_1 and h_2 omega omega are two proper holomorphic mappings extending smoothly up to the boundary of omega near some point boundary point p and agreeing up to order k at p then necessarily h_1h_2
|
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|
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|
706.3116
|
Series expansion for the density of states of the Ising and Potts models
|
An approximation of the density of states for the Ising and Potts models
based on the high- and low-temperature series are developed.
|
cond-mat.str-el cond-mat.stat-mech
|
an approximation of the density of states for the ising and potts models based on the high and lowtemperature series are developed
|
[['an', 'approximation', 'of', 'the', 'density', 'of', 'states', 'for', 'the', 'ising', 'and', 'potts', 'models', 'based', 'on', 'the', 'high', 'and', 'lowtemperature', 'series', 'are', 'developed']]
|
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|
706.3117
|
How do methanol masers manage to appear in the youngest star vicinities
and isolated molecular clumps?
|
General characteristics of methanol (CH3OH) maser emission are summarized. It
is shown that methanol maser sources are concentrated in the spiral arms. Most
of the methanol maser sources from the Perseus arm are associated with embedded
stellar clusters and a considerable portion is situated close to compact HII
regions. Almost 1/3 of the Perseus Arm sources lie at the edges of optically
identified HII regions which means that massive star formation in the Perseus
Arm is to a great extent triggered by local phenomena. A multiline analysis of
the methanol masers allows us to determine the physical parameters in the
regions of maser formation. Maser modelling shows that class II methanol masers
can be pumped by the radiation of the warm dust as well as by free-free
emission of a hypercompact region hcHII with a turnover frequency exceeding 100
GHz. Methanol masers of both classes can reside in the vicinity of hcHIIs.
Modelling shows that periodic changes of maser fluxes can be reproduced by
variations of the dust temperature by a few percent which may be caused by
variations in the brightness of the central young stellar object reflecting the
character of the accretion process. Sensitive observations have shown that the
masers with low flux densities can still have considerable amplification
factors. The analysis of class I maser surveys allows us to identify four
distinct regimes that differ by the series of their brightest lines.
|
astro-ph
|
general characteristics of methanol ch3oh maser emission are summarized it is shown that methanol maser sources are concentrated in the spiral arms most of the methanol maser sources from the perseus arm are associated with embedded stellar clusters and a considerable portion is situated close to compact hii regions almost 13 of the perseus arm sources lie at the edges of optically identified hii regions which means that massive star formation in the perseus arm is to a great extent triggered by local phenomena a multiline analysis of the methanol masers allows us to determine the physical parameters in the regions of maser formation maser modelling shows that class ii methanol masers can be pumped by the radiation of the warm dust as well as by freefree emission of a hypercompact region hchii with a turnover frequency exceeding 100 ghz methanol masers of both classes can reside in the vicinity of hchiis modelling shows that periodic changes of maser fluxes can be reproduced by variations of the dust temperature by a few percent which may be caused by variations in the brightness of the central young stellar object reflecting the character of the accretion process sensitive observations have shown that the masers with low flux densities can still have considerable amplification factors the analysis of class i maser surveys allows us to identify four distinct regimes that differ by the series of their brightest lines
|
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|
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|
706.3118
|
The structural and magnetic properties of (In1-xFex)2O3 (0.0 <= x <=
0.25) system : prepared by gel combustion method
|
(In1-xFex)2O3 polycrystalline samples with x = (0.0, 0.05, 0.10, 0.15, 0.20
and 0.25) have been synthesized by a gel combustion method. Reitveld refinement
analysis of X raydiffraction data indicated the formation of single phase cubic
bixbyite structure without any parasitic phases. This observation is further
confirmed by high resolution transmission electron microscopy (HRTEM) imaging,
and indexing of the selected-area electron diffraction (SAED) patterns, X-ray
Absorption Spectroscopy (XAS) and Raman Spectroscopy. DC Magnetization studies
as a function of temperature and field indicatethat they are ferromagnetic with
Curie temperature (TC) well above room temperature.
|
cond-mat.mtrl-sci
|
in1xfex2o3 polycrystalline samples with x 00 005 010 015 020 and 025 have been synthesized by a gel combustion method reitveld refinement analysis of x raydiffraction data indicated the formation of single phase cubic bixbyite structure without any parasitic phases this observation is further confirmed by high resolution transmission electron microscopy hrtem imaging and indexing of the selectedarea electron diffraction saed patterns xray absorption spectroscopy xas and raman spectroscopy dc magnetization studies as a function of temperature and field indicatethat they are ferromagnetic with curie temperature tc well above room temperature
|
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|
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|
706.3119
|
G2 Hitchin functionals at one loop
|
We consider the quantization of the effective target space description of
topological M-theory in terms of the Hitchin functional whose critical points
describe seven-manifolds with G2 structure. The one-loop partition function for
this theory is calculated and an extended version of it, that is related to
generalized G2 geometry, is compared with the topological G2 string. We relate
the reduction of the effective action for the extended G2 theory to the Hitchin
functional description of the topological string in six dimensions. The
dependence of the partition functions on the choice of background G2 metric is
also determined.
|
hep-th
|
we consider the quantization of the effective target space description of topological mtheory in terms of the hitchin functional whose critical points describe sevenmanifolds with g2 structure the oneloop partition function for this theory is calculated and an extended version of it that is related to generalized g2 geometry is compared with the topological g2 string we relate the reduction of the effective action for the extended g2 theory to the hitchin functional description of the topological string in six dimensions the dependence of the partition functions on the choice of background g2 metric is also determined
|
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|
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|
706.312
|
Some Thermodynamic Aspects of Pure Glue, Fuzzy Bags and Gauge/String
Duality
|
The thermodynamic properties of a SU(3) gauge theory without quarks are
calculated using a string formulation for 1.2T_c < T < 3T_c. The results are in
good agreement with the lattice data. We also comment on SU(N) gauge theories.
|
hep-ph hep-lat hep-th nucl-th
|
the thermodynamic properties of a su3 gauge theory without quarks are calculated using a string formulation for 12t_c t 3t_c the results are in good agreement with the lattice data we also comment on sun gauge theories
|
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|
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|
706.3121
|
Multi-triangulations as complexes of star polygons
|
Maximal $(k+1)$-crossing-free graphs on a planar point set in convex
position, that is, $k$-triangulations, have received attention in recent
literature, with motivation coming from several interpretations of them.
We introduce a new way of looking at $k$-triangulations, namely as complexes
of star polygons. With this tool we give new, direct, proofs of the fundamental
properties of $k$-triangulations, as well as some new results. This
interpretation also opens-up new avenues of research, that we briefly explore
in the last section.
|
math.CO
|
maximal k1crossingfree graphs on a planar point set in convex position that is ktriangulations have received attention in recent literature with motivation coming from several interpretations of them we introduce a new way of looking at ktriangulations namely as complexes of star polygons with this tool we give new direct proofs of the fundamental properties of ktriangulations as well as some new results this interpretation also opensup new avenues of research that we briefly explore in the last section
|
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|
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|
706.3122
|
Effects of payoff functions and preference distributions in an adaptive
population
|
Adaptive populations such as those in financial markets and distributed
control can be modeled by the Minority Game. We consider how their dynamics
depends on the agents' initial preferences of strategies, when the agents use
linear or quadratic payoff functions to evaluate their strategies. We find that
the fluctuations of the population making certain decisions (the volatility)
depends on the diversity of the distribution of the initial preferences of
strategies. When the diversity decreases, more agents tend to adapt their
strategies together. In systems with linear payoffs, this results in dynamical
transitions from vanishing volatility to a non-vanishing one. For low signal
dimensions, the dynamical transitions for the different signals do not take
place at the same critical diversity. Rather, a cascade of dynamical
transitions takes place when the diversity is reduced. In contrast, no phase
transitions are found in systems with the quadratic payoffs. Instead, a basin
boundary of attraction separates two groups of samples in the space of the
agents' decisions. Initial states inside this boundary converge to small
volatility, while those outside diverge to a large one. Furthermore, when the
preference distribution becomes more polarized, the dynamics becomes more
erratic. All the above results are supported by good agreement between
simulations and theory.
|
q-fin.ST physics.soc-ph
|
adaptive populations such as those in financial markets and distributed control can be modeled by the minority game we consider how their dynamics depends on the agents initial preferences of strategies when the agents use linear or quadratic payoff functions to evaluate their strategies we find that the fluctuations of the population making certain decisions the volatility depends on the diversity of the distribution of the initial preferences of strategies when the diversity decreases more agents tend to adapt their strategies together in systems with linear payoffs this results in dynamical transitions from vanishing volatility to a nonvanishing one for low signal dimensions the dynamical transitions for the different signals do not take place at the same critical diversity rather a cascade of dynamical transitions takes place when the diversity is reduced in contrast no phase transitions are found in systems with the quadratic payoffs instead a basin boundary of attraction separates two groups of samples in the space of the agents decisions initial states inside this boundary converge to small volatility while those outside diverge to a large one furthermore when the preference distribution becomes more polarized the dynamics becomes more erratic all the above results are supported by good agreement between simulations and theory
|
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|
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|
706.3123
|
Comparative study of the inial spikes of SGR giant flares in 1998 and
2004 observed with GEOTAIL: Do magnetospheric instabilities trigger large
scale fracturing of magnetar's crust?
|
We present the unsaturated peak profile of SGR 1900+14 giant flare on 1998
August 27. This was obtained by particle counters of the Low Energy Particle
instrument onboard the GEOTAIL spacecraft. The observed peak profile revealed
four characteristic structures: initial steep rise, intermediate rise to the
peak, exponential decay and small hump in the decay phase. From this light
curve, we found that the isotropic peak luminosity was $2.3\times10^{46}$ erg
s$^{-1}$ and the total energy was $4.3 \times 10^{44}$ erg s$^{-1}$ ($E\gtrsim$
50 keV), assuming that the distance to SGR 1900+14 is 15 kpc and that the
spectrum is optically thin thermal bremsstrahlung with $kT =$ 240 keV. These
are consistent with the previously reported lower limits derived from Ulysses
and Konus-Wind observations. A comparative study of the initial spikes of SGR
1900+14 giant flare in 1998 and SGR 1806-20 in 2004 is also presented. The
timescale of the initial steep rise shows the magnetospheric origin, while the
timescale of the intermediate rise to the peak indicates that it originates
from the crustal fracturing. Finally, we argue that the four structures and
their corresponding timescales provide a clue to identify extragalactic SGR
giant flares among short GRBs.
|
astro-ph
|
we present the unsaturated peak profile of sgr 190014 giant flare on 1998 august 27 this was obtained by particle counters of the low energy particle instrument onboard the geotail spacecraft the observed peak profile revealed four characteristic structures initial steep rise intermediate rise to the peak exponential decay and small hump in the decay phase from this light curve we found that the isotropic peak luminosity was 23times1046 erg s1 and the total energy was 43 times 1044 erg s1 egtrsim 50 kev assuming that the distance to sgr 190014 is 15 kpc and that the spectrum is optically thin thermal bremsstrahlung with kt 240 kev these are consistent with the previously reported lower limits derived from ulysses and konuswind observations a comparative study of the initial spikes of sgr 190014 giant flare in 1998 and sgr 180620 in 2004 is also presented the timescale of the initial steep rise shows the magnetospheric origin while the timescale of the intermediate rise to the peak indicates that it originates from the crustal fracturing finally we argue that the four structures and their corresponding timescales provide a clue to identify extragalactic sgr giant flares among short grbs
|
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|
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|
706.3124
|
The Non-Trapping Degree of Scattering
|
We consider classical potential scattering. If no orbit is trapped at energy
E, the Hamiltonian dynamics defines an integer-valued topological degree. This
can be calculated explicitly and be used for symbolic dynamics of
multi-obstacle scattering.
If the potential is bounded, then in the non-trapping case the boundary of
Hill's Region is empty or homeomorphic to a sphere.
We consider classical potential scattering. If at energy E no orbit is
trapped, the Hamiltonian dynamics defines an integer-valued topological degree
deg(E) < 2. This is calculated explicitly for all potentials, and exactly the
integers < 2 are shown to occur for suitable potentials.
The non-trapping condition is restrictive in the sense that for a bounded
potential it is shown to imply that the boundary of Hill's Region in
configuration space is either empty or homeomorphic to a sphere.
However, in many situations one can decompose a potential into a sum of
non-trapping potentials with non-trivial degree and embed symbolic dynamics of
multi-obstacle scattering. This comprises a large number of earlier results,
obtained by different authors on multi-obstacle scattering.
|
math-ph math.MP
|
we consider classical potential scattering if no orbit is trapped at energy e the hamiltonian dynamics defines an integervalued topological degree this can be calculated explicitly and be used for symbolic dynamics of multiobstacle scattering if the potential is bounded then in the nontrapping case the boundary of hills region is empty or homeomorphic to a sphere we consider classical potential scattering if at energy e no orbit is trapped the hamiltonian dynamics defines an integervalued topological degree dege 2 this is calculated explicitly for all potentials and exactly the integers 2 are shown to occur for suitable potentials the nontrapping condition is restrictive in the sense that for a bounded potential it is shown to imply that the boundary of hills region in configuration space is either empty or homeomorphic to a sphere however in many situations one can decompose a potential into a sum of nontrapping potentials with nontrivial degree and embed symbolic dynamics of multiobstacle scattering this comprises a large number of earlier results obtained by different authors on multiobstacle scattering
|
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|
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|
706.3125
|
Spatial string tension in $N_f=2$ lattice QCD at finite temperature
|
The spatial string tension across a crossover from the low temperature phase
to the high temperature phase is computed in QCD with two flavors of
non-perturbatively improved Wilson fermions at small lattice spacing a \sim
0.12fm. We find that in the low temperature phase spatial string tension agrees
well with zero temperature string tension. Furthermore, it does not show
increasing for temperatures up to T = 1.36 T_{pc}, the highest temperature
considered. Our results agree with some theoretical predictions.
|
hep-lat
|
the spatial string tension across a crossover from the low temperature phase to the high temperature phase is computed in qcd with two flavors of nonperturbatively improved wilson fermions at small lattice spacing a sim 012fm we find that in the low temperature phase spatial string tension agrees well with zero temperature string tension furthermore it does not show increasing for temperatures up to t 136 t_pc the highest temperature considered our results agree with some theoretical predictions
|
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|
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|
706.3126
|
On the structure of relativistic collisionless shocks in electron-ion
plasmas
|
Relativistic collisionless shocks in electron-ion plasma are thought to occur
in the afterglow phase of Gamma-Ray Bursts (GRBs), and in other environments
where relativistic flows interact with the interstellar medium. A particular
regime of shocks in an unmagnetized plasma has generated much interest for GRB
applications. In this paper we present ab-initio particle-in-cell simulations
of unmagnetized relativistic electron-ion shocks. Using long-term
2.5-dimensional simulations with ion-electron mass ratios from 16 to 1000 we
resolve the shock formation and reach a steady-state shock structure beyond the
initial transient. We find that even at high ion-electron mass ratios initially
unmagnetized shocks can be effectively mediated by the ion Weibel instability
with a typical shock thickness of ~50 ion skin-depths. Upstream of the shock
the interaction with merging ion current filaments heats the electron
component, so that the postshock flow achieves near equipartition between the
ions and electrons, with electron temperature reaching 50% of the ion
temperature. This energy exchange helps to explain the large electron energy
fraction inferred from GRB afterglow observations.
|
astro-ph
|
relativistic collisionless shocks in electronion plasma are thought to occur in the afterglow phase of gammaray bursts grbs and in other environments where relativistic flows interact with the interstellar medium a particular regime of shocks in an unmagnetized plasma has generated much interest for grb applications in this paper we present abinitio particleincell simulations of unmagnetized relativistic electronion shocks using longterm 25dimensional simulations with ionelectron mass ratios from 16 to 1000 we resolve the shock formation and reach a steadystate shock structure beyond the initial transient we find that even at high ionelectron mass ratios initially unmagnetized shocks can be effectively mediated by the ion weibel instability with a typical shock thickness of 50 ion skindepths upstream of the shock the interaction with merging ion current filaments heats the electron component so that the postshock flow achieves near equipartition between the ions and electrons with electron temperature reaching 50 of the ion temperature this energy exchange helps to explain the large electron energy fraction inferred from grb afterglow observations
|
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|
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|
706.3127
|
Brane-Worlds Pseudo-Goldstinos
|
We consider a space-time with extra dimensions containing sectors, branes and
bulk, that communicate only through gravitational interactions. In each sector,
if considered separately, supersymmetry could be spontaneously broken, leading
to the appearance of Goldstinos. However, when taken all together, only certain
combinations of the latter states turn out to be true ``would be Goldstinos'',
eaten by the gravitinos. The other (orthogonal) combinations, we call
pseudo-Goldstinos, remain in the low energy spectrum. We discuss explicitly how
this happen in the simplest set-up of five-dimensional space compactified on
S^1/Z_2 . Our results divide into two parts that can be considered separately.
First, we build an extension of the bulk five-dimensional supergravity, by a
set of new auxiliary fields, that allows coupling it to branes where
supersymmetry is spontaneously broken. Second, we discuss in details the super
Higgs mechanism in the R_\xi and unitary gauges, in the presence of both of a
bulk Scherk-Schwarz mechanism and brane localized F-terms. This leads us to
compute the gravitino mass and provide explicit formulae for the
pseudo-Goldstinos spectrum.
|
hep-th hep-ph
|
we consider a spacetime with extra dimensions containing sectors branes and bulk that communicate only through gravitational interactions in each sector if considered separately supersymmetry could be spontaneously broken leading to the appearance of goldstinos however when taken all together only certain combinations of the latter states turn out to be true would be goldstinos eaten by the gravitinos the other orthogonal combinations we call pseudogoldstinos remain in the low energy spectrum we discuss explicitly how this happen in the simplest setup of fivedimensional space compactified on s1z_2 our results divide into two parts that can be considered separately first we build an extension of the bulk fivedimensional supergravity by a set of new auxiliary fields that allows coupling it to branes where supersymmetry is spontaneously broken second we discuss in details the super higgs mechanism in the r_xi and unitary gauges in the presence of both of a bulk scherkschwarz mechanism and brane localized fterms this leads us to compute the gravitino mass and provide explicit formulae for the pseudogoldstinos spectrum
|
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|
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|
706.3128
|
Gamma-delayed deuteron emission of the 6Li (0+;T=1) halo state
|
M1 transitions from the $^6$Li($0^+;T=1$) state at 3.563 MeV to the
$^6$Li($1^+$) ground state and to the $\alpha+d$ continuum are studied in a
three-body model. The bound states are described as an $\alpha+n+p$ system in
hyperspherical coordinates on a Lagrange mesh. The ground-state magnetic moment
and the gamma width of the $^6$Li(0$^+$) resonance are well reproduced. The
halo-like structure of the $^6$Li$(0^+)$ resonance is confirmed and is probed
by the M1 transition probability to the $\alpha+d$ continuum. The spectrum is
sensitive to the description of the $\alpha+d$ phase shifts. The corresponding
gamma width is around 1.0 meV, with optimal potentials. Charge symmetry is
analyzed through a comparison with the $\beta$-delayed deuteron spectrum of
$^6$He. In $^6$He, a nearly perfect cancellation effect between short-range and
halo contributions was found. A similar analysis for the $^6$Li($0^+;T=1$)
$\gamma$ decay is performed; it shows that charge-symmetry breaking at large
distances, due to the different binding energies and to different charges,
reduces this effect. The present branching ratio $\Gamma_{\gamma}(0^+\to
\alpha+d)/\Gamma_{\gamma}(0^+\to1^+)\approx 1.3\times 10^{-4}$ should be
observable with current experimental facilities.
|
nucl-th
|
m1 transitions from the 6li0t1 state at 3563 mev to the 6li1 ground state and to the alphad continuum are studied in a threebody model the bound states are described as an alphanp system in hyperspherical coordinates on a lagrange mesh the groundstate magnetic moment and the gamma width of the 6li0 resonance are well reproduced the halolike structure of the 6li0 resonance is confirmed and is probed by the m1 transition probability to the alphad continuum the spectrum is sensitive to the description of the alphad phase shifts the corresponding gamma width is around 10 mev with optimal potentials charge symmetry is analyzed through a comparison with the betadelayed deuteron spectrum of 6he in 6he a nearly perfect cancellation effect between shortrange and halo contributions was found a similar analysis for the 6li0t1 gamma decay is performed it shows that chargesymmetry breaking at large distances due to the different binding energies and to different charges reduces this effect the present branching ratio gamma_gamma0to alphadgamma_gamma0to1approx 13times 104 should be observable with current experimental facilities
|
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|
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|
706.3129
|
Closed-Form Density of States and Localization Length for a
Non-Hermitian Disordered System
|
We calculate the Lyapunov exponent for the non-Hermitian Zakharov-Shabat
eigenvalue problem corresponding to the attractive non-linear Schroedinger
equation with a Gaussian random pulse as initial value function. Using an
extension of the Thouless formula to non-Hermitian random operators, we
calculate the corresponding average density of states. We analyze two cases,
one with circularly symmetric complex Gaussian pulses and the other with real
Gaussian pulses. We discuss the implications in the context of the information
transmission through non-linear optical fibers.
|
cond-mat.dis-nn cond-mat.stat-mech cs.IT math.IT nlin.SI
|
we calculate the lyapunov exponent for the nonhermitian zakharovshabat eigenvalue problem corresponding to the attractive nonlinear schroedinger equation with a gaussian random pulse as initial value function using an extension of the thouless formula to nonhermitian random operators we calculate the corresponding average density of states we analyze two cases one with circularly symmetric complex gaussian pulses and the other with real gaussian pulses we discuss the implications in the context of the information transmission through nonlinear optical fibers
|
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|
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|
706.313
|
Abelian Magnetic Monopoles and Topologically Massive Vector Bosons in
Scalar-Tensor Gravity with Torsion Potential
|
A Lagrangian formulation describing the electromagnetic interaction -
mediated by topologically massive vector bosons - between charged, spin-(1/2)
fermions with an abelian magnetic monopole in a curved spacetime with
non-minimal coupling and torsion potential is presented. The covariant field
equations are obtained. The issue of coexistence of massive photons and
magnetic monopoles is addressed in the present framework. It is found that
despite the topological nature of photon mass generation in curved spacetime
with isotropic dilaton field, the classical field theory describing the
nonrelativistic electromagnetic interaction between a point-like electric
charge and magnetic monopole is inconsistent.
|
gr-qc hep-th
|
a lagrangian formulation describing the electromagnetic interaction mediated by topologically massive vector bosons between charged spin12 fermions with an abelian magnetic monopole in a curved spacetime with nonminimal coupling and torsion potential is presented the covariant field equations are obtained the issue of coexistence of massive photons and magnetic monopoles is addressed in the present framework it is found that despite the topological nature of photon mass generation in curved spacetime with isotropic dilaton field the classical field theory describing the nonrelativistic electromagnetic interaction between a pointlike electric charge and magnetic monopole is inconsistent
|
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|
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|
706.3131
|
A nilpotent quotient algorithm for L-presented groups
|
The main part of this paper contains a description of a nilpotent quotient
algorithm for L-presented groups and a report on applications of its
implementation in the computer algebra system GAP. The appendix introduces two
new infinite series of L-presented groups. Apart from being of interest in
their own right, these new L-presented groups serve as examples for
applications of the nilpotent quotient algorithm.
|
math.GR
|
the main part of this paper contains a description of a nilpotent quotient algorithm for lpresented groups and a report on applications of its implementation in the computer algebra system gap the appendix introduces two new infinite series of lpresented groups apart from being of interest in their own right these new lpresented groups serve as examples for applications of the nilpotent quotient algorithm
|
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|
[-0.16524281821330078, 0.0209401318907112, -0.10463960435299668, 0.009799286859561107, -0.11511744410381652, -0.12274485306988936, 0.010346101395043661, 0.36513945600017905, -0.32054988087475067, -0.26934876205632463, 0.1695536288425501, -0.2481847173476126, -0.16608072716917377, 0.2869786373266834, -0.14669709319423418, -0.05885570510963589, 0.062092637934256345, 0.1200616862734023, -0.05471136346750427, -0.2639761811878998, 0.3368125616834732, -0.011515348654938862, 0.20182516946442774, 0.021062730891571846, 0.11715958763670642, -0.002357985336857382, -0.07686394887514325, -0.051572448668594006, -0.09922872115930659, 0.15891825281141791, 0.2945858638850041, 0.11148089978814824, 0.3119705893477658, -0.3456893569091335, -0.10487558761087712, 0.1095199394840165, 0.19575008921674453, 0.06447901546198409, -0.13983291842487233, -0.2901705372496508, 0.07491119975748006, -0.25101825973251835, -0.13667602486384567, -0.05830235403118422, 0.06417258104193024, 0.006131637070211582, -0.16458859253907576, 0.009580901183653623, 0.0863884708378464, 0.1451726509112632, -0.05491883029208111, -0.1370469525977569, 0.01948117844585795, 0.15840303837467218, 0.002592416654806584, -0.0446437139671616, 0.12496242146153236, -0.07572739545821605, -0.14597699465230107, 0.41538982989732176, -0.009249343838746427, -0.1562031378998654, 0.18166936916531995, -0.10765542081207968, -0.2244216044418863, 0.09996985192992724, 0.1570036215998698, 0.15279054417624138, -0.06408780794299673, 0.18660220249057602, -0.09011210923199542, 0.056091291198754334, 0.02862718164396938, 0.04034010956820566, 0.15892503794748336, 0.18548173288581893, 0.061945111709064804, 0.16260869015968638, 0.09154327364194614, 0.0074558914348017424, -0.41072615719167516, -0.2281450150476303, -0.15831136601627804, 0.042134076928277864, -0.05414798895048989, -0.197456012636394, 0.46687150647630915, 0.14417388386209495, 0.13832059787819162, 0.07081187021685764, 0.2766813659836771, 0.00524002336715057, 0.06799623363986029, 0.05030383109988179, 0.0914657254179474, 0.18593931834038813, 0.010752677022537682, -0.12312760091663222, -0.02994941709039267, 0.16657780967943836]
|
706.3132
|
EasyVoice: Integrating voice synthesis with Skype
|
This paper presents EasyVoice, a system that integrates voice synthesis with
Skype. EasyVoice allows a person with voice disabilities to talk with another
person located anywhere in the world, removing an important obstacle that
affect these people during a phone or VoIP-based conversation.
|
cs.CY cs.HC
|
this paper presents easyvoice a system that integrates voice synthesis with skype easyvoice allows a person with voice disabilities to talk with another person located anywhere in the world removing an important obstacle that affect these people during a phone or voipbased conversation
|
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|
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|
706.3133
|
Tunable photonic band gaps with coherently driven atoms in optical
lattices
|
Optical lattice loaded with cold atoms can exhibit a tunable photonic band
gap for a weak probe field under the conditions of electromagnetically induced
transparency. This system possesses a number of advantageous properties,
including reduced relaxation of Raman coherence and the associated probe
absorption, and simultaneous enhancement of the index modulation and the
resulting reflectivity of the medium. This flexible system has a potential to
serve as a testbed of various designs for the linear and nonlinear photonic
band gap materials at a very low light level and can be employed for realizing
deterministic entanglement between weak quantum fields.
|
quant-ph
|
optical lattice loaded with cold atoms can exhibit a tunable photonic band gap for a weak probe field under the conditions of electromagnetically induced transparency this system possesses a number of advantageous properties including reduced relaxation of raman coherence and the associated probe absorption and simultaneous enhancement of the index modulation and the resulting reflectivity of the medium this flexible system has a potential to serve as a testbed of various designs for the linear and nonlinear photonic band gap materials at a very low light level and can be employed for realizing deterministic entanglement between weak quantum fields
|
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|
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|
706.3134
|
Triadophilia: A Special Corner in the Landscape
|
It is well known that there are a great many apparently consistent vacua of
string theory. We draw attention to the fact that there appear to be very few
Calabi--Yau manifolds with the Hodge numbers h^{11} and h^{21} both small. Of
these, the case (h^{11}, h^{21})=(3,3) corresponds to a manifold on which a
three generation heterotic model has recently been constructed. We point out
also that there is a very close relation between this manifold and several
familiar manifolds including the `three-generation' manifolds with \chi=-6 that
were found by Tian and Yau, and by Schimmrigk, during early investigations. It
is an intriguing possibility that we may live in a naturally defined corner of
the landscape. The location of these three generation models with respect to a
corner of the landscape is so striking that we are led to consider the
possibility of transitions between heterotic vacua. The possibility of these
transitions, that we here refer to as transgressions, is an old idea that goes
back to Witten. Here we apply this idea to connect three generation vacua on
different Calabi-Yau manifolds.
|
hep-th astro-ph hep-ph math.AG
|
it is well known that there are a great many apparently consistent vacua of string theory we draw attention to the fact that there appear to be very few calabiyau manifolds with the hodge numbers h11 and h21 both small of these the case h11 h2133 corresponds to a manifold on which a three generation heterotic model has recently been constructed we point out also that there is a very close relation between this manifold and several familiar manifolds including the threegeneration manifolds with chi6 that were found by tian and yau and by schimmrigk during early investigations it is an intriguing possibility that we may live in a naturally defined corner of the landscape the location of these three generation models with respect to a corner of the landscape is so striking that we are led to consider the possibility of transitions between heterotic vacua the possibility of these transitions that we here refer to as transgressions is an old idea that goes back to witten here we apply this idea to connect three generation vacua on different calabiyau manifolds
|
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|
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|
706.3135
|
Excited $(70,L^+)$ baryon resonances in the relativistic quark model
|
The masses of positive parity $(70,0^+)$ and $(70,2^+)$ nonstrange and
strange baryons are calculated in the relativistic quark model. The
relativistic three-quark equations of the $(70,L^+)$ multiplets are found in
the framework of the dispersion relation technique. The approximate solutions
of these equations using the method based on the extraction of leading
singularities of the amplitude are obtained. The calculated mass values of the
$(70,L^+)$ multiplets are in good agreement with the experimental ones.
|
hep-ph
|
the masses of positive parity 700 and 702 nonstrange and strange baryons are calculated in the relativistic quark model the relativistic threequark equations of the 70l multiplets are found in the framework of the dispersion relation technique the approximate solutions of these equations using the method based on the extraction of leading singularities of the amplitude are obtained the calculated mass values of the 70l multiplets are in good agreement with the experimental ones
|
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|
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|
706.3136
|
Broad distribution of stick-slip events in Slowly Sheared Granular
Media: Table-top production of a Gutenberg-Richter-like distribution
|
We monitor the stick-slip displacements of a very slowly driven moveable
perforated top plate which interacts via shearing with a packing of identical
glass beads confined in a tray. When driven at a constant stress rate, the
distributions of large event displacements and energies triggered by the
stick-slip instabilities exhibit power law responses reminiscent of the
Gutenberg-Richter law for earthquakes. Small events are quasi-size independent,
signaling crossover from single-bead transport to collective behavior.
|
cond-mat.stat-mech cond-mat.soft
|
we monitor the stickslip displacements of a very slowly driven moveable perforated top plate which interacts via shearing with a packing of identical glass beads confined in a tray when driven at a constant stress rate the distributions of large event displacements and energies triggered by the stickslip instabilities exhibit power law responses reminiscent of the gutenbergrichter law for earthquakes small events are quasisize independent signaling crossover from singlebead transport to collective behavior
|
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|
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|
706.3137
|
Asymptotic Enumeration of RNA Structures with Pseudoknots
|
In this paper we present the asymptotic enumeration of RNA structures with
pseudoknots. We develop a general framework for the computation of exponential
growth rate and the sub exponential factors for $k$-noncrossing RNA structures.
Our results are based on the generating function for the number of
$k$-noncrossing RNA pseudoknot structures, ${\sf S}_k(n)$, derived in
\cite{Reidys:07pseu}, where $k-1$ denotes the maximal size of sets of mutually
intersecting bonds. We prove a functional equation for the generating function
$\sum_{n\ge 0}{\sf S}_k(n)z^n$ and obtain for $k=2$ and $k=3$ the analytic
continuation and singular expansions, respectively. It is implicit in our
results that for arbitrary $k$ singular expansions exist and via transfer
theorems of analytic combinatorics we obtain asymptotic expression for the
coefficients. We explicitly derive the asymptotic expressions for 2- and
3-noncrossing RNA structures. Our main result is the derivation of the formula
${\sf S}_3(n) \sim \frac{10.4724\cdot 4!}{n(n-1)...(n-4)}
(\frac{5+\sqrt{21}}{2})^n$.
|
q-bio.BM math.CO
|
in this paper we present the asymptotic enumeration of rna structures with pseudoknots we develop a general framework for the computation of exponential growth rate and the sub exponential factors for knoncrossing rna structures our results are based on the generating function for the number of knoncrossing rna pseudoknot structures sf s_kn derived in citereidys07pseu where k1 denotes the maximal size of sets of mutually intersecting bonds we prove a functional equation for the generating function sum_nge 0sf s_knzn and obtain for k2 and k3 the analytic continuation and singular expansions respectively it is implicit in our results that for arbitrary k singular expansions exist and via transfer theorems of analytic combinatorics we obtain asymptotic expression for the coefficients we explicitly derive the asymptotic expressions for 2 and 3noncrossing rna structures our main result is the derivation of the formula sf s_3n sim frac104724cdot 4nn1n4 frac5sqrt212n
|
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|
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|
706.3138
|
Insights and puzzles in light quark physics
|
Recent work in light flavour hadron physics is reviewed. In particular, I
discuss the significance of the progress achieved with light dynamical quarks
on the lattice for the effective low energy theory of QCD. Also, I draw
attention to some puzzling results from NA48 and KTeV concerning the scalar
form factor relevant for Kmu3 decay -- taken at face value, these indicate
physics beyond the Standard Model.
|
hep-ph
|
recent work in light flavour hadron physics is reviewed in particular i discuss the significance of the progress achieved with light dynamical quarks on the lattice for the effective low energy theory of qcd also i draw attention to some puzzling results from na48 and ktev concerning the scalar form factor relevant for kmu3 decay taken at face value these indicate physics beyond the standard model
|
[['recent', 'work', 'in', 'light', 'flavour', 'hadron', 'physics', 'is', 'reviewed', 'in', 'particular', 'i', 'discuss', 'the', 'significance', 'of', 'the', 'progress', 'achieved', 'with', 'light', 'dynamical', 'quarks', 'on', 'the', 'lattice', 'for', 'the', 'effective', 'low', 'energy', 'theory', 'of', 'qcd', 'also', 'i', 'draw', 'attention', 'to', 'some', 'puzzling', 'results', 'from', 'na48', 'and', 'ktev', 'concerning', 'the', 'scalar', 'form', 'factor', 'relevant', 'for', 'kmu3', 'decay', 'taken', 'at', 'face', 'value', 'these', 'indicate', 'physics', 'beyond', 'the', 'standard', 'model']]
|
[-0.0052919905195294905, 0.17462475175235534, -0.07012479443272407, 0.09514080041095219, -0.06523740040420582, -0.16939942303261804, 0.06429111613772076, 0.3229214801650607, -0.19607518574533364, -0.27202059667218814, 0.05604772270431347, -0.3173055373781333, -0.07716752968333436, 0.18209957851760203, 0.0014568038115447218, 0.09944000144517331, 0.0937258651811686, 0.027501000038517468, -0.06265091577149702, -0.24572426182302562, 0.2960187626692156, 0.051952698289162734, 0.24825105158555688, 0.16777507873308478, 0.025463516118400024, 0.01857012048695293, -0.09862687941076177, -0.030260744093649202, -0.1578603612654137, 0.12044073385186493, 0.2030329042198983, 0.10046041843650694, 0.1721130937732982, -0.41149293035833223, -0.2047830483537506, 0.05996542088122982, 0.08892818675799803, 0.12301657060302343, -0.11597704582064497, -0.30140917954232654, 0.06162857445606002, -0.15258910226508637, -0.1622178665729183, -0.07740911432175022, -0.006701626197547849, -0.0681188449150685, -0.2449493136849593, 0.059741936741347396, -0.01003817283543123, 0.07707055040042508, 0.004910285965624181, -0.2668656705257793, 0.05407487512142821, 0.031614539926081445, 0.15646100927684034, 0.08005721481150073, 0.11188706028924296, -0.22038555804244947, -0.13044007169259147, 0.42835587093775923, -0.04791987689289575, -0.10477603659047886, 0.15494345739540277, -0.2109430271948716, -0.20977320343566438, 0.09423112021194714, 0.207333912169843, 0.007026077163490382, -0.11622162682540489, 0.14138545975341307, -0.03224376582709903, 0.1332099734043533, 0.033735619547466435, 0.09226720840811278, 0.2502684552278934, 0.21160941576288844, -0.0763168444109121, 0.032157081182848546, -0.04149514219765975, -0.14327343134209514, -0.3753774428711922, -0.07795524015796906, -0.10955133569201059, 0.07393858112063202, -0.0775669428983361, -0.04574435236722683, 0.4065463300194648, 0.17324399696239692, 0.2182156629154854, -0.003278888317502358, 0.2511845013183175, 0.07118248453391998, 0.018506202261161172, 0.03355538062610184, 0.33762589316668734, 0.14570612262821558, 0.17073753897354685, -0.24915332436406365, -0.01880298163847659, 0.06690006001118684]
|
706.3139
|
Exclusive Meson Production at NLO
|
We report on numerical studies of the NLO corrections to exclusive meson
electroproduction, both in collider and fixed-target kinematics. Corrections
are found to be huge at small xB and sizeable at intermediate or large xB.
|
hep-ph
|
we report on numerical studies of the nlo corrections to exclusive meson electroproduction both in collider and fixedtarget kinematics corrections are found to be huge at small xb and sizeable at intermediate or large xb
|
[['we', 'report', 'on', 'numerical', 'studies', 'of', 'the', 'nlo', 'corrections', 'to', 'exclusive', 'meson', 'electroproduction', 'both', 'in', 'collider', 'and', 'fixedtarget', 'kinematics', 'corrections', 'are', 'found', 'to', 'be', 'huge', 'at', 'small', 'xb', 'and', 'sizeable', 'at', 'intermediate', 'or', 'large', 'xb']]
|
[-0.09153634038354669, 0.18506885524839162, -0.10244348738342524, 0.17693876592176302, -0.050293669131185326, -0.1322964119325791, 0.04916229571348855, 0.3965187312236854, -0.17349275909364223, -0.22027299723454885, -0.006777339059460376, -0.42175068163446017, 0.07081735041325114, 0.1703244121944798, 0.1349017477993454, 0.12173911601837192, 0.13950794783553908, -0.09255885892946805, -0.0640997011746679, -0.2193348011800221, 0.30898821747728755, 0.06032719521650246, 0.15196897885096924, 0.24225720381364227, 0.056807647818433386, 0.0012531436048448085, -0.08497379390256746, -0.02364712293658938, -0.06438151676307566, 0.02316131040986095, 0.3393560124827283, 0.03097289192623326, 0.12353236845561437, -0.3665603484426226, 0.0006714834698608943, 0.10512552277318069, 0.18708562823677702, 0.11123913835201944, -0.08130767550652049, -0.2611118710466794, 0.15158474169937627, -0.2753760516643524, -0.10010535663792065, -0.16625626241522176, 0.04368935888965747, -0.05629102465297495, -0.3392945903752531, 0.01938418739342264, -0.14671019533915178, 0.04184634789292301, 0.040640507665063656, -0.22153457988585745, -0.043559005350938866, -0.006972747901454568, 0.1316326046096427, 0.07981771153530905, 0.13128236262127757, -0.19969580098986625, -0.1709490818769804, 0.3870077912296568, -0.025927247080419744, -0.11585208305290767, 0.1690705096083028, -0.3810965057462454, -0.2278291775578899, 0.20912881030568053, 0.3651469910783427, 0.12473227822754, -0.11764627961175782, 0.14425654283259065, 0.036045316553541595, 0.16685997407351222, 0.06823764301038214, 0.09549558805967016, 0.1802003697093044, 0.22632414014743907, -0.10921944299313639, 0.009331475647299418, -0.09739010868194913, -0.05807655248790979, -0.43731215064014706, -0.044878070455576693, -0.021092844993940423, 0.0986089393097375, -0.059645588296033177, -0.09253336600959301, 0.21812865829560907, 0.07441000333055854, 0.2978553139737674, -0.03122450624193464, 0.3343935077743871, 0.09866816297705684, 0.12124842413052517, 0.09078762190142048, 0.33929588070937566, 0.12076953048152583, 0.15554774822667242, -0.3026657001248428, 0.05093479717948607, -0.020928317814001014]
|
706.314
|
Saffman-Taylor instability in a non-Brownian suspension: finger
selection and destabilization
|
We study the Saffman-Taylor instability in a non-Brownian suspension by
injection of air. We find that flow structuration in the Hele-Shaw cell can be
described by an effective viscosity depending on the volume fraction. When this
viscosity is used to define the control parameter of the instability, the
classical finger selection for Newtonian fluids is recovered. However, this
picture breaks down when the cell thickness is decreased below approximatively
10 grain sizes. The discrete nature of the grains plays also a determinant role
in the the early destabilization of the fingers observed. The grains produce a
perturbation at the interface proportional to the grain size and can thus be
considered as a "controlled noise". The finite amplitude instability mechanism
proposed earlier by Bensimon et al. allows to link this perturbation to the
actual values of the destabilization threshold.
|
cond-mat.soft
|
we study the saffmantaylor instability in a nonbrownian suspension by injection of air we find that flow structuration in the heleshaw cell can be described by an effective viscosity depending on the volume fraction when this viscosity is used to define the control parameter of the instability the classical finger selection for newtonian fluids is recovered however this picture breaks down when the cell thickness is decreased below approximatively 10 grain sizes the discrete nature of the grains plays also a determinant role in the the early destabilization of the fingers observed the grains produce a perturbation at the interface proportional to the grain size and can thus be considered as a controlled noise the finite amplitude instability mechanism proposed earlier by bensimon et al allows to link this perturbation to the actual values of the destabilization threshold
|
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|
[-0.12475940974150533, 0.19628684416875994, -0.08598461204011293, 0.028657020963592468, -0.04243950118874981, -0.07962981135971899, 0.04541992711542297, 0.28287463284430714, -0.29435188956150826, -0.3040039515714195, 0.09653176649908678, -0.20848304565401535, -0.12250208152784374, 0.1358488864319766, -0.0797062247420532, 0.008624279649905269, -0.006466317909980451, -0.03042775081100119, 0.003552398115845166, -0.20745925209315044, 0.27772334312007213, 0.105216781975851, 0.3000022954491042, 0.06054473061277701, 0.05415733488460146, -0.03731840556949703, 0.009956485251930073, 0.06314358857535098, -0.20347265106054188, 0.01413617495542569, 0.2088913710101297, -0.012596920591500336, 0.2523915607407417, -0.44059571273026676, -0.2568498573259172, 0.06624106441821603, 0.16087123683405646, 0.1302795276644021, -0.010441543779974926, -0.2157144492651832, 0.08954356447963492, -0.14489905655585453, -0.180087549085083, 0.014612905042123621, 0.05050162622623526, -0.009412132474648203, -0.28061430596739706, 0.1358185851675404, 0.07884116171702851, 0.03353337906504961, -0.07219124990421939, -0.06352566812105857, -0.06513952062444857, 0.11385517900709376, 0.07346848589895008, 0.02632115953805836, 0.22837139532160367, -0.14592917320100984, -0.02895200211745109, 0.3945341155775925, -0.059829292945516206, -0.2030983789939515, 0.18653051300232645, -0.13961496226571118, -0.030444758407173367, 0.19847019361569987, 0.1515045708154131, 0.07425125284174824, -0.09507449707598425, 0.02830111296524771, -0.031157041532769256, 0.1941564671481096, 0.1147978027269625, -0.061231308813839064, 0.20629724947885222, 0.20307399525585837, 0.03391678597995617, 0.17201105340462122, -0.11221819755920365, -0.09006659670972544, -0.2857759494375247, -0.14698301522863388, -0.15968085226201773, 0.04065050687521941, -0.12807579250846068, -0.16860689479436208, 0.3395120418786894, 0.13079216960183665, 0.2085448418859474, 0.019643669484020042, 0.27224382753212034, 0.11612891499462952, 0.0742309722831867, 0.06090365354155265, 0.2899371481799677, 0.12464114267593182, 0.13014462631940163, -0.2963373006311293, 0.11237196715116964, 0.09216583933235982]
|
706.3141
|
Higher-Order Calculus of Variations on Time Scales
|
We prove a version of the Euler-Lagrange equations for certain problems of
the calculus of variations on time scales with higher-order delta derivatives.
|
math.OC math.CA math.FA
|
we prove a version of the eulerlagrange equations for certain problems of the calculus of variations on time scales with higherorder delta derivatives
|
[['we', 'prove', 'a', 'version', 'of', 'the', 'eulerlagrange', 'equations', 'for', 'certain', 'problems', 'of', 'the', 'calculus', 'of', 'variations', 'on', 'time', 'scales', 'with', 'higherorder', 'delta', 'derivatives']]
|
[-0.19470541835155175, 0.03600323366244202, -0.10044738974260248, 0.10789539669032978, -0.11492909806901994, -0.05817824035235073, -0.0519455187022686, 0.25217662362948706, -0.36572217325801437, -0.3099445456881886, 0.14007510965609032, -0.2531996298095454, -0.11573240322911221, 0.18199949096078458, -0.08638244953370937, 0.06750923144104688, 0.07327522272649019, 0.05047224753576776, -0.14437523698839155, -0.2110889647156, 0.34415319699632085, -0.0960812267401944, 0.1144044887598442, 0.08773835343511208, 0.2188529701417555, -0.02737593614374814, -0.01382598693927993, 0.042030681734499725, -0.15525959270155948, 0.11530895798426608, 0.19795437213843284, 0.041129022867054395, 0.331969976020248, -0.4503811571909034, -0.19359436501627383, 0.08313293297491643, 0.05764994426104038, 0.08039310149362554, 0.06086938213253313, -0.325333788505067, 0.06345425655498453, -0.05238345888969691, -0.19833653857526573, -0.05563779924388813, 0.042690555220874754, 0.11460555433903051, -0.2666662009027989, 0.13264532516831937, 0.0422887179352667, 0.06539467572356047, -0.13485835650530847, -0.100900630041471, 0.00442359831346118, -0.029965280777896227, 0.04481982357759515, -0.06788475896515277, 0.042291642632335424, -0.1056492385332999, -0.14474617155349773, 0.40533300910307013, -0.1276607054245213, -0.30644818962268205, 0.04876994001476661, -0.11591238447505495, -0.24628966548682554, 0.06150842729308035, 0.15366598575011545, 0.25908729563588684, -0.07805413056326949, 0.16020800063953453, 0.020824105843253757, 0.2130202999257523, 0.1336932785242148, 0.07186979087798492, 0.04370336926987638, 0.11817143448507009, 0.15603904494934756, 0.10827433374588905, -0.048741477045595, -0.171328358028246, -0.416013119985228, -0.16977688779487557, -0.06550129246897995, 0.01964909753397755, -0.17800603898080147, -0.22089624769337798, 0.3926341332009305, 0.1267547633741861, 0.10951657334099645, 0.21941722836345434, 0.2247994010863097, 0.2677304604212227, 0.08809042175340911, 0.04929456726202498, 0.12163052505449108, 0.18461287369870621, 0.1735060213579108, -0.2239091291051844, 0.06189987996755087, 0.18074474888651268]
|
706.3142
|
Three-point correlations for quantum star graphs
|
We compute the three point correlation function for the eigenvalues of the
Laplacian on quantum star graphs in the limit where the number of edges tends
to infinity. This extends a work by Berkolaiko and Keating, where they get the
2-point correlation function and show that it follows neither Poisson, nor
random matrix statistics. It makes use of the trace formula and combinatorial
analysis.
|
math-ph math.MP
|
we compute the three point correlation function for the eigenvalues of the laplacian on quantum star graphs in the limit where the number of edges tends to infinity this extends a work by berkolaiko and keating where they get the 2point correlation function and show that it follows neither poisson nor random matrix statistics it makes use of the trace formula and combinatorial analysis
|
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|
[-0.07827475394879002, 0.07001641782699153, -0.11835434450767934, 0.10775207217920979, -0.07281836417678278, -0.09634574175288435, 0.052042388917470817, 0.3160628766345326, -0.2509143842107733, -0.26789962594921235, 0.08554067345721705, -0.327132100937888, -0.21797846064146142, 0.119856803357834, -0.023954828102432657, 0.046700910810614005, 0.04108237054970232, 0.07088567041500937, -0.058814075290570145, -0.22775465305312537, 0.3405101031967206, 0.030514205142026185, 0.2501404268805345, 0.09058868847205304, 0.06677711513930262, 0.08409065671003191, -0.07532599876140011, -0.0046549913658964215, -0.13271777691682018, 0.04602435720516951, 0.20940724917454645, 0.11158780691766879, 0.24066816536651459, -0.39537478852435015, -0.158690295094857, 0.14462469030695502, 0.15267809620127082, 0.05988979747053236, 0.029937090423118207, -0.2130608807783574, 0.09891694196335266, -0.14424697064532666, -0.12993117338555749, -0.046504230795108015, 0.03182155257491104, 0.03829276893520728, -0.28157538546292926, 0.07428443921526195, 0.11217799831501907, 0.012030963189317845, 0.019253702161222463, -0.12907132171676494, -0.0010696844619815238, 0.11653292074333876, 0.02668588513188297, 0.03323615056433482, 0.11015056992619066, -0.11155470876474283, -0.06916336755784869, 0.32825668930308893, -0.051362280260946136, -0.23261689554419718, 0.14537279261276126, -0.19768302414013306, -0.158922922128113, 0.052986707276431844, 0.0816865567539935, 0.13736233340023318, -0.0980863775475882, 0.1470934931830925, -0.058455840655369684, 0.11484555359720616, 0.08428969910892192, -0.0011563835214474238, 0.14571277732829913, 0.03118788388383109, 0.12221867209882475, 0.16042040770116728, -0.07736342027419596, -0.11488932019710774, -0.29370894870953634, -0.1764395443824469, -0.31566914945142344, 0.1209052250349032, -0.15361891628640478, -0.23675407844712026, 0.3798774261958897, 0.1397828314511571, 0.253536000585882, 0.14672505597991403, 0.24033404112560675, 0.17506194706220413, 0.05216847648262046, 0.10652300275978632, 0.15821900561422808, 0.2157722890660807, 0.08955819191032788, -0.18197899267397588, 0.044415872973331716, 0.11797481092071394]
|
706.3143
|
First Order Superfluid to Bose Metal Transition in Systems with Resonant
Pairing
|
Systems showing resonant superfluidity, driven by an exchange coupling of
strength $g$ between uncorrelated pairs of itinerant fermions and tightly bound
ones, undergo a first order phase transition as $g$ increases beyond some
critical value $g_c$. The superfluid phase for $g \leq g_c$ is characterized by
a gap in the fermionic single particle spectrum and an acoustic sound-wave like
collective mode of the bosonic resonating fermion pairs inside this gap. For
$g>g_c$ this state gives way to a phase uncorrelated bosonic liquid with a
$q^2$ spectrum.
|
cond-mat.supr-con cond-mat.str-el
|
systems showing resonant superfluidity driven by an exchange coupling of strength g between uncorrelated pairs of itinerant fermions and tightly bound ones undergo a first order phase transition as g increases beyond some critical value g_c the superfluid phase for g leq g_c is characterized by a gap in the fermionic single particle spectrum and an acoustic soundwave like collective mode of the bosonic resonating fermion pairs inside this gap for gg_c this state gives way to a phase uncorrelated bosonic liquid with a q2 spectrum
|
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|
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|
706.3144
|
Comment on the paper "Weyssenhoff fluid dynamics in a 1+3 covariant
approach" (arXiv:0706.2367)
|
Few comments are given to clarify some issues of Weyssenhoff fluid in the
Einstein-Cartan gravity.
|
astro-ph gr-qc
|
few comments are given to clarify some issues of weyssenhoff fluid in the einsteincartan gravity
|
[['few', 'comments', 'are', 'given', 'to', 'clarify', 'some', 'issues', 'of', 'weyssenhoff', 'fluid', 'in', 'the', 'einsteincartan', 'gravity']]
|
[-0.2593390095978975, 0.13865451862414677, -0.038383806496858595, 0.11908253853519758, -0.23261945694684982, -0.2143740553408861, -0.10052803568542004, 0.25494282618165015, -0.233952305590113, -0.3763389671842257, 0.07343196424189954, -0.3562878593802452, -0.09374934807419777, 0.057937026023864746, -0.21116775584717593, 0.0030828534935911497, -0.02142258094002803, 0.09150980338454247, -0.13524870996673902, -0.33286654700835544, 0.3671458395818869, 0.08602178854246935, 0.11886018322159847, 0.12147448708613713, 0.06814454309642315, -0.17627632043634853, -0.10154986226310332, 0.03719179270168146, -0.2133462203045686, 0.01417847660680612, 0.2604699338786304, 0.09516549309094748, 0.3339413814091434, -0.528146892786026, -0.30191341216365497, -0.0483106109003226, 0.050546531782795986, 0.1876369214616716, -0.05217847094560663, -0.32134897777189814, 0.019216877097884815, -0.1859371021389961, -0.12239706016456088, -0.08365969384709994, 0.02717135672767957, -0.015082014724612236, -0.05944410289327304, 0.08853320591151714, 0.018080961952606837, 0.031176866342624027, -0.06087133695061008, -0.12844237641741832, 0.040672860791285834, 0.03674340423506995, 0.2363024113078912, 0.020251970551908017, 0.16567136980593206, -0.2167814875021577, -0.06121482625603676, 0.4854932318131129, -0.032156893114248915, -0.30045610101272663, 0.11817933712154627, -0.15281357591350872, -0.17853391837949553, 0.010800974443554878, 0.0650667256054779, 0.06895942632108927, -0.17601640646656355, 0.06889470765988032, -0.01859740565220515, 0.056496248890956245, 0.13833958075071376, 0.0426680584748586, 0.32305171713232994, 0.10822950278719266, -0.09663782427087426, 0.07829262434194485, 0.06187064958115419, -0.16416681359211605, -0.44503032267093656, -0.1479788785179456, -0.05600807794059316, 0.011460670456290244, -0.09245955968896548, -0.16466825877626737, 0.29937916845083234, 0.2499408286064863, 0.08491515815258026, -0.03418186983714501, 0.15409120184679825, -0.030220922579367957, -0.07495445224146048, 0.12590320309003195, 0.28628491769583586, 0.26794197745621207, 0.14288789733933907, -0.2016165403028329, -0.10996152792746822, 0.08429249695812663]
|
706.3145
|
Revisiting Signature of Minimal Gauge Mediation
|
We revisit phenomenology of the minimal gauge-mediated model. This model is
motivated from the SUSY CP and flavor problems. A specific feature of this
model is that \tan\beta is naturally large, since the B term in the Higgs
potential is zero at the messenger scale. This leads to significant SUSY
contributions to various low-energy observables. We evaluate the anomalous
magnetic moment of the muon and the branching ratio of \bar{B}\to X_s\gamma
taking account of recent theoretical and experimental developments. We find
that the current experimental data prefer a low messenger scale (\sim 100 TeV)
and gluino mass around 1 TeV. We also calculate the branching ratios of
\bar{B}\to X_s l^+l^-, B_s\to \mu^+\mu^-, and B^-\to \tau^- \bar{\nu}, and show
that these observables are strongly correlated with each other in this model.
|
hep-ph
|
we revisit phenomenology of the minimal gaugemediated model this model is motivated from the susy cp and flavor problems a specific feature of this model is that tanbeta is naturally large since the b term in the higgs potential is zero at the messenger scale this leads to significant susy contributions to various lowenergy observables we evaluate the anomalous magnetic moment of the muon and the branching ratio of barbto x_sgamma taking account of recent theoretical and experimental developments we find that the current experimental data prefer a low messenger scale sim 100 tev and gluino mass around 1 tev we also calculate the branching ratios of barbto x_s ll b_sto mumu and bto tau barnu and show that these observables are strongly correlated with each other in this model
|
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|
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|
706.3146
|
WiFi Epidemiology: Can Your Neighbors' Router Make Yours Sick?
|
In densely populated urban areas WiFi routers form a tightly interconnected
proximity network that can be exploited as a substrate for the spreading of
malware able to launch massive fraudulent attack and affect entire urban areas
WiFi networks. In this paper we consider several scenarios for the deployment
of malware that spreads solely over the wireless channel of major urban areas
in the US. We develop an epidemiological model that takes into consideration
prevalent security flaws on these routers. The spread of such a contagion is
simulated on real-world data for geo-referenced wireless routers. We uncover a
major weakness of WiFi networks in that most of the simulated scenarios show
tens of thousands of routers infected in as little time as two weeks, with the
majority of the infections occurring in the first 24 to 48 hours. We indicate
possible containment and prevention measure to limit the eventual harm of such
an attack.
|
cs.CR physics.soc-ph
|
in densely populated urban areas wifi routers form a tightly interconnected proximity network that can be exploited as a substrate for the spreading of malware able to launch massive fraudulent attack and affect entire urban areas wifi networks in this paper we consider several scenarios for the deployment of malware that spreads solely over the wireless channel of major urban areas in the us we develop an epidemiological model that takes into consideration prevalent security flaws on these routers the spread of such a contagion is simulated on realworld data for georeferenced wireless routers we uncover a major weakness of wifi networks in that most of the simulated scenarios show tens of thousands of routers infected in as little time as two weeks with the majority of the infections occurring in the first 24 to 48 hours we indicate possible containment and prevention measure to limit the eventual harm of such an attack
|
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|
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|
706.3147
|
Half-Supersymmetric Solutions in Five-Dimensional Supergravity
|
We present a systematic classification of half-supersymmetric solutions of
gauged N=2, D=5 supergravity coupled to an arbitrary number of abelian vector
multiplets for which at least one of the Killing spinors generate a time-like
Killing vector.
|
hep-th
|
we present a systematic classification of halfsupersymmetric solutions of gauged n2 d5 supergravity coupled to an arbitrary number of abelian vector multiplets for which at least one of the killing spinors generate a timelike killing vector
|
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|
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|
706.3148
|
Finite size effects on surface excess quantities: application to crystal
growth and surface melting of epitaxial layers
|
From a macroscopic point of view phase transitions as surface melting or two
dimensional (2D) towards three dimensional (3D) growth mode (Stranski-Krastanov
transition) can be described in terms of Gibbs excess quantity duly amended by
size effects (since usual Gibbs excess quantities are only well defined for
semi-infinite systems). The aim of this study is to consider such amended
quantities to describe surface melting and Stranski-Krastanov transition of
epitaxial layers. the so-introduced size effects allows us to predict the
equilibrium thickness of the wetting layer of the Stranski-Krastanov growth
mode and to describe and classify two different melting cases: the incomplete
melting relayed by a first order transition and the continuous premelting
relayed by continuous overheating
|
cond-mat.mtrl-sci
|
from a macroscopic point of view phase transitions as surface melting or two dimensional 2d towards three dimensional 3d growth mode stranskikrastanov transition can be described in terms of gibbs excess quantity duly amended by size effects since usual gibbs excess quantities are only well defined for semiinfinite systems the aim of this study is to consider such amended quantities to describe surface melting and stranskikrastanov transition of epitaxial layers the sointroduced size effects allows us to predict the equilibrium thickness of the wetting layer of the stranskikrastanov growth mode and to describe and classify two different melting cases the incomplete melting relayed by a first order transition and the continuous premelting relayed by continuous overheating
|
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|
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|
706.3149
|
Probing the truncation of galaxy dark matter halos in high density
environments from hydrodynamical N-body simulations
|
We analyze high resolution, N-body hydrodynamical simulations of fiducial
galaxy clusters to probe tidal stripping of the dark matter subhalos. These
simulations include a prescription for star formation allowing us to track the
fate of the stellar component as well. We investigate the effect of tidal
stripping on cluster galaxies hosted in these dark matter subhalos as a
function of cluster-centric radius. To quantify the extent of the dark matter
halos of cluster galaxies, we introduce the half mass radius r_half as a
diagnostic, and study its evolution with projected cluster-centric distance R
as a function of redshift. We find a well defined trend for (r_half,R): the
closer the galaxies are to the center of the cluster, the smaller the half mass
radius. Interestingly, this trend is inferred in all redshift frames examined
in this work ranging from z=0 to z=0.7. At z=0, galaxy halos in the central
regions of clusters are found to be highly truncated, with the most compact
half mass radius of 10 kpc. We also find that r_half depends on luminosity and
we present scaling relations of r_half with galaxy luminosity. The
corresponding total mass of the cluster galaxies is also found to increase with
projected cluster-centric distance and luminosity, but with more scatter than
the (r_half,R) trend. Comparing the distribution of stellar mass to total mass
for cluster galaxies, we find that the dark matter component is preferentially
stripped, whereas the stellar component remains protected by the halo and is
much less affected by tidal forces. We compare these results with galaxy-galaxy
lensing probes of r_half and find qualitative agreement. (Abridged)
|
astro-ph
|
we analyze high resolution nbody hydrodynamical simulations of fiducial galaxy clusters to probe tidal stripping of the dark matter subhalos these simulations include a prescription for star formation allowing us to track the fate of the stellar component as well we investigate the effect of tidal stripping on cluster galaxies hosted in these dark matter subhalos as a function of clustercentric radius to quantify the extent of the dark matter halos of cluster galaxies we introduce the half mass radius r_half as a diagnostic and study its evolution with projected clustercentric distance r as a function of redshift we find a well defined trend for r_halfr the closer the galaxies are to the center of the cluster the smaller the half mass radius interestingly this trend is inferred in all redshift frames examined in this work ranging from z0 to z07 at z0 galaxy halos in the central regions of clusters are found to be highly truncated with the most compact half mass radius of 10 kpc we also find that r_half depends on luminosity and we present scaling relations of r_half with galaxy luminosity the corresponding total mass of the cluster galaxies is also found to increase with projected clustercentric distance and luminosity but with more scatter than the r_halfr trend comparing the distribution of stellar mass to total mass for cluster galaxies we find that the dark matter component is preferentially stripped whereas the stellar component remains protected by the halo and is much less affected by tidal forces we compare these results with galaxygalaxy lensing probes of r_half and find qualitative agreement abridged
|
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|
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|
706.315
|
Measurement of the Cross Section for open b-Quark Production in
Two-Photon Interactions at LEP
|
Inclusive beauty-quark production in two-photon collisions has been measured
at LEP using an integrated luminosity of 698 pb-1 collected by the ALEPH
detector with sqrt(s) between 130 and 209 GeV. The b quarks were identified
using lifetime information. The cross section is found to be sigma(e+ e- --> e+
e- b \bar{b} X) = (5.4 +/- 0.8 (stat) +/- 0.8 (syst)) pb which is consistent
with Next-to-Leading Order QCD.
|
hep-ex
|
inclusive beautyquark production in twophoton collisions has been measured at lep using an integrated luminosity of 698 pb1 collected by the aleph detector with sqrts between 130 and 209 gev the b quarks were identified using lifetime information the cross section is found to be sigmae e e e b barb x 54 08 stat 08 syst pb which is consistent with nexttoleading order qcd
|
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|
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|
706.3151
|
Meta-stable A_n quiver gauge theories
|
We study metastable dynamical breaking of supersymmetry in A_n quiver gauge
theories. We present a general analysis and criteria for the perturbative
existence of metastable vacua in quivers of any length. Different mechanisms of
gauge mediation can be realized.
|
hep-th
|
we study metastable dynamical breaking of supersymmetry in a_n quiver gauge theories we present a general analysis and criteria for the perturbative existence of metastable vacua in quivers of any length different mechanisms of gauge mediation can be realized
|
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|
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|
706.3152
|
Remarks on the calculus of variations on time scales
|
The calculus of variations is a classical subject which has gain throughout
the last three hundred years a level of rigor and elegance that only time can
give. In this note we show that, contrary to the classical field, available
formulations and results on the recent calculus of variations on time scales
are still at the heuristic level.
|
math.OC math.CA
|
the calculus of variations is a classical subject which has gain throughout the last three hundred years a level of rigor and elegance that only time can give in this note we show that contrary to the classical field available formulations and results on the recent calculus of variations on time scales are still at the heuristic level
|
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|
[-0.09377034869173477, 0.07421637397933879, -0.12940257828650548, 0.053808137292748894, -0.05779842778654962, -0.07869739046095517, 0.03763448212552687, 0.3714436335681841, -0.2754078296751812, -0.3261585121267828, 0.15630420669311143, -0.2521123664276996, -0.13763093819905972, 0.20648037146873258, -0.12408199082610422, -0.015610014730743292, 0.0959971210887206, 0.09017922266803939, -0.09022416591901204, -0.3124773531895259, 0.2912897666081272, 0.04234294285837176, 0.23160546155774903, 0.10277416462335608, 0.12707280269663396, -0.060091339541470695, -0.042434957279855835, 0.033887260633617126, -0.09188306467745108, 0.13825276754656005, 0.2133861880364089, 0.12034133943761217, 0.33621145327222246, -0.47605945263057947, -0.22238176508710303, 0.053553553330230305, 0.10038491116900897, 0.10933833788269488, -0.022281529947890545, -0.21892574538701567, 0.07982287893738148, -0.11475102828237517, -0.07899001927179253, -0.046772620706931396, 0.07262348630345138, -0.008056135928450987, -0.1702928864878827, 0.07792266029543404, 0.07041580710110479, 0.0872796196651099, -0.03552053013720132, -0.13774842158730688, 0.051978024935092904, 0.09434819319446025, 0.09305050793697993, 0.034607475315389255, 0.08289499258108694, -0.08904703523048424, -0.16426721037012235, 0.3667802943944417, -0.06130962632596493, -0.17378422633969579, 0.22842666617562546, -0.17135069016688342, -0.1702671032960944, 0.11803940612951229, 0.14033414628196123, 0.12130649174274556, -0.11747024494126954, 0.11861925705231662, -0.057314430459819994, 0.22066497870174975, 0.08854588446335802, 0.05875493500156906, 0.16020112425281569, 0.16279132379989686, 0.04192657606547762, 0.06312093678620997, -0.08615922230167379, -0.16552642003857884, -0.32795452920655754, -0.1191708810370544, -0.118006859271755, 0.02538406095820768, -0.033833921308416455, -0.11888946037225682, 0.4343714760295276, 0.2076065373619023, 0.1466217440520895, 0.11158200472408648, 0.3144316354702259, 0.15489639375551506, 0.08485717607806598, 0.05009379158406679, 0.2756056814968329, 0.10572889122855046, 0.14450823982920627, -0.12640991243373217, 0.08017654642502874, 0.01905343301016195]
|
706.3153
|
Connections between Romanovski and other polynomials
|
A connection between Romanovski polynomials and those polynomials that solve
the one-dimensional Schr\"odinger equation with the trigonometric Rosen-Morse
and hyperbolic Scarf potential is established. The map is constructed by
reworking the Rodrigues formula in an elementary and natural way. The
generating function is summed in closed form from which recursion relations and
addition theorems follow. Relations to some classical polynomials are also
given.
|
math.CA
|
a connection between romanovski polynomials and those polynomials that solve the onedimensional schrodinger equation with the trigonometric rosenmorse and hyperbolic scarf potential is established the map is constructed by reworking the rodrigues formula in an elementary and natural way the generating function is summed in closed form from which recursion relations and addition theorems follow relations to some classical polynomials are also given
|
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|
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|
706.3154
|
M31 and Local Group QSO's
|
Previous analyses have shown companion galaxies aligned along the minor axis
of M31. The alignment includes some galaxies of higher redshift than
conventionally accepted for Local Group members. Here we look at the
distribution of all high redshift objects listed in a 10 x 10 deg. area around
M31. We find not only galaxies of higher redshift but also quasars along the
minor axis of this brightest Local Group galaxy, Some are an unusual class of
low z, quasar-galaxy.
Previously observers had noted radio sources aligned along the minor axis of
M31. The ejection directions of quasars from active galaxy nuclei is also along
the minor axis within a cone of about 20 deg. opening angle. It is shown here
that the quasar-like and higher redshift objects associated with M31 are
relatively concentrated along this axis.
M33 also falls closely along the minor axis of M31 and the famous 3C48 and
similar redshift galaxy/quasars are seen along a line coming from this Local
Group companion of M31. What appears to be dusty nebulosity has also been shown
to exist along this extended line in the sky.
|
astro-ph
|
previous analyses have shown companion galaxies aligned along the minor axis of m31 the alignment includes some galaxies of higher redshift than conventionally accepted for local group members here we look at the distribution of all high redshift objects listed in a 10 x 10 deg area around m31 we find not only galaxies of higher redshift but also quasars along the minor axis of this brightest local group galaxy some are an unusual class of low z quasargalaxy previously observers had noted radio sources aligned along the minor axis of m31 the ejection directions of quasars from active galaxy nuclei is also along the minor axis within a cone of about 20 deg opening angle it is shown here that the quasarlike and higher redshift objects associated with m31 are relatively concentrated along this axis m33 also falls closely along the minor axis of m31 and the famous 3c48 and similar redshift galaxyquasars are seen along a line coming from this local group companion of m31 what appears to be dusty nebulosity has also been shown to exist along this extended line in the sky
|
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|
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|
706.3155
|
Collider Phenomenology of Unparticle Physics
|
Low energy phenomenology of the unparticle physics associated with an exact
scale invariant sector possessing a non-trivial infrared fixed point at a
higher energy scale is explored for both electron-positron and hadronic
colliders. Feynman rules for a spin 0, 1 or 2 unparticle coupled to a variety
of standard model gauge invariant operators that are relevant to many low
energy processes involving either real emissions of unparticles or their
virtual propagator effects are presented. Missing energy and/or recoil mass
distributions of the unparticle in the associated production of unparticle
together with a photon or $Z$ boson at LEP2 and ILC as well as in $Z$ decay
into an unparticle plus a fermion-antifermion pair are studied. Monojet
production at hadronic collisions is explored. The complex phase in the
unparticle propagator that can give rise to interesting interference effects
between an unparticle exchange diagram and the standard model amplitudes are
studied in details for the Drell-Yan process as well as muon pair and diphoton
production in electron-positron annihilation. These energy and/or recoil mass
distributions (with the exception in hadron colliders) and interference effects
are found sensitively depending not only on the scale dimension but also on the
spin of the unparticle. For the spin-2 unparticle, its physical effects is
found to resemble that of a tower of Kaluza-Klein gravitons, which strongly
indicates that the underlying unparticle physics may have root in a higher
dimensional theory. A connection between unparticle physics and theories of
large extra dimension is speculated. Experimental constraints on the unparticle
scale are deduced from the LEP2 data on mono-photon production and from the
4-fermion contact interactions.
|
hep-ph hep-th
|
low energy phenomenology of the unparticle physics associated with an exact scale invariant sector possessing a nontrivial infrared fixed point at a higher energy scale is explored for both electronpositron and hadronic colliders feynman rules for a spin 0 1 or 2 unparticle coupled to a variety of standard model gauge invariant operators that are relevant to many low energy processes involving either real emissions of unparticles or their virtual propagator effects are presented missing energy andor recoil mass distributions of the unparticle in the associated production of unparticle together with a photon or z boson at lep2 and ilc as well as in z decay into an unparticle plus a fermionantifermion pair are studied monojet production at hadronic collisions is explored the complex phase in the unparticle propagator that can give rise to interesting interference effects between an unparticle exchange diagram and the standard model amplitudes are studied in details for the drellyan process as well as muon pair and diphoton production in electronpositron annihilation these energy andor recoil mass distributions with the exception in hadron colliders and interference effects are found sensitively depending not only on the scale dimension but also on the spin of the unparticle for the spin2 unparticle its physical effects is found to resemble that of a tower of kaluzaklein gravitons which strongly indicates that the underlying unparticle physics may have root in a higher dimensional theory a connection between unparticle physics and theories of large extra dimension is speculated experimental constraints on the unparticle scale are deduced from the lep2 data on monophoton production and from the 4fermion contact interactions
|
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|
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|
706.3156
|
Interfaces and the edge percolation map of random directed networks
|
The traditional node percolation map of directed networks is reanalyzed in
terms of edges. In the percolated phase, edges can mainly organize into five
distinct giant connected components, interfaces bridging the communication of
nodes in the strongly connected component and those in the in- and
out-components. Formal equations for the relative sizes in number of edges of
these giant structures are derived for arbitrary joint degree distributions in
the presence of local and two-point correlations. The uncorrelated null model
is fully solved analytically and compared against simulations, finding an
excellent agreement between the theoretical predictions and the edge
percolation map of synthetically generated networks with exponential or
scale-free in-degree distribution and exponential out-degree distribution.
Interfaces, and their internal organization giving place from "hairy ball"
percolation landscapes to bottleneck straits, could bring new light to the
discussion of how structure is interwoven with functionality, in particular in
flow networks.
|
cond-mat.dis-nn physics.soc-ph
|
the traditional node percolation map of directed networks is reanalyzed in terms of edges in the percolated phase edges can mainly organize into five distinct giant connected components interfaces bridging the communication of nodes in the strongly connected component and those in the in and outcomponents formal equations for the relative sizes in number of edges of these giant structures are derived for arbitrary joint degree distributions in the presence of local and twopoint correlations the uncorrelated null model is fully solved analytically and compared against simulations finding an excellent agreement between the theoretical predictions and the edge percolation map of synthetically generated networks with exponential or scalefree indegree distribution and exponential outdegree distribution interfaces and their internal organization giving place from hairy ball percolation landscapes to bottleneck straits could bring new light to the discussion of how structure is interwoven with functionality in particular in flow networks
|
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|
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|
706.3157
|
Power corrections for jets at hadron colliders
|
We discuss non-perturbative QCD corrections to jet distributions in hadron
collisions, focussing on hadronisation and underlying event contributions.
Using soft gluon resummation and Monte-Carlo modelling we show that
hadronisation dominates at small values of the jet radius R, behaving as 1/R,
while underlying event corrections grow with the jet area. This provides a
handle to disentangle them and parametrize them in terms of measurable QCD
parameters, which might enjoy a degree of universality.
|
hep-ph
|
we discuss nonperturbative qcd corrections to jet distributions in hadron collisions focussing on hadronisation and underlying event contributions using soft gluon resummation and montecarlo modelling we show that hadronisation dominates at small values of the jet radius r behaving as 1r while underlying event corrections grow with the jet area this provides a handle to disentangle them and parametrize them in terms of measurable qcd parameters which might enjoy a degree of universality
|
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|
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|
706.3158
|
On contact tops and integrable tops
|
In this paper, we introduce a geometric structure called top, which is a
trivialized bundle of plane pencils over a Riemannian 3-manifold, defined as
the set of kernels of a circle of 1-forms (e.g. of contact and integrable
forms) with particular properties with respect to the metric. We classify the
manifolds which admit tops and we describe the associated metrics.
|
math.DG math.GT
|
in this paper we introduce a geometric structure called top which is a trivialized bundle of plane pencils over a riemannian 3manifold defined as the set of kernels of a circle of 1forms eg of contact and integrable forms with particular properties with respect to the metric we classify the manifolds which admit tops and we describe the associated metrics
|
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|
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|
706.3159
|
Une s\'emantique observationnelle du mod\`ele des bo\^ites pour la
r\'esolution de programmes logiques (version \'etendue)
|
This report specifies an observational semantics and gives an original
presentation of the Byrd's box model. The approach accounts for the semantics
of Prolog tracers independently of a particular implementation. Traces are, in
general, considered as rather obscure and difficult to use. The proposed formal
presentation of a trace constitutes a simple and pedagogical approach for
teaching Prolog or for implementing Prolog tracers. It constitutes a form of
declarative specification for the tracers. Our approach highlights qualities of
the box model which made its success, but also its drawbacks and limits. As a
matter of fact, the presented semantics is only one example to illustrate
general problems relating to tracers and observing processes. Observing
processes know, from observed processes, only their traces. The issue is then
to be able to reconstitute by the sole analysis of the trace the main part of
the observed process, and if possible, without any loss of information.
|
cs.PL cs.SE
|
this report specifies an observational semantics and gives an original presentation of the byrds box model the approach accounts for the semantics of prolog tracers independently of a particular implementation traces are in general considered as rather obscure and difficult to use the proposed formal presentation of a trace constitutes a simple and pedagogical approach for teaching prolog or for implementing prolog tracers it constitutes a form of declarative specification for the tracers our approach highlights qualities of the box model which made its success but also its drawbacks and limits as a matter of fact the presented semantics is only one example to illustrate general problems relating to tracers and observing processes observing processes know from observed processes only their traces the issue is then to be able to reconstitute by the sole analysis of the trace the main part of the observed process and if possible without any loss of information
|
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|
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|
706.316
|
Spin pumping by a field-driven domain wall
|
We calculate the charge current in a metallic ferromagnet to first order in
the time derivative of the magnetization direction. Irrespective of the
microscopic details, the result can be expressed in terms of the conductivities
of the majority and minority electrons and the non-adiabatic spin transfer
torque parameter $\beta$. The general expression is evaluated for the specific
case of a field-driven domain wall and for that case depends strongly on the
ratio of $\beta$ and the Gilbert damping constant. These results may provide an
experimental method to determine this ratio, which plays a crucial role for
current-driven domain-wall motion.
|
cond-mat.mes-hall
|
we calculate the charge current in a metallic ferromagnet to first order in the time derivative of the magnetization direction irrespective of the microscopic details the result can be expressed in terms of the conductivities of the majority and minority electrons and the nonadiabatic spin transfer torque parameter beta the general expression is evaluated for the specific case of a fielddriven domain wall and for that case depends strongly on the ratio of beta and the gilbert damping constant these results may provide an experimental method to determine this ratio which plays a crucial role for currentdriven domainwall motion
|
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|
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|
706.3161
|
Euler Walk on a Cayley Tree
|
We show that the Euler walk on a Cayley tree exhibits two regimes (dynamic
phases): a condensed phase and a low-density phase. In the condensed phase the
self-organized area grows as a compact domain. In the low-density phase the
proportion of self-organized (visited) nodes decreases rapidly from one
generation of the tree to the next. We describe in detail returns of the Euler
walk to the root and growth of the self-organized domain in the condensed
phase. We also investigate the critical behaviour of the Euler walk at the
point separating the two regimes.
|
cond-mat.stat-mech math.PR
|
we show that the euler walk on a cayley tree exhibits two regimes dynamic phases a condensed phase and a lowdensity phase in the condensed phase the selforganized area grows as a compact domain in the lowdensity phase the proportion of selforganized visited nodes decreases rapidly from one generation of the tree to the next we describe in detail returns of the euler walk to the root and growth of the selforganized domain in the condensed phase we also investigate the critical behaviour of the euler walk at the point separating the two regimes
|
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|
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|
706.3162
|
Remarks on the density of the law of the occupation time for Bessel
bridges and stable excursions
|
Smoothness and asymptotic behaviors are studied for the densities of the law
of the occupation time on the positive line for Bessel bridges and the
normalized excursion of strictly stable processes. The key role is played by
these properties for functions defined by Riemann--Liouville fractional
integrals.
|
math.PR
|
smoothness and asymptotic behaviors are studied for the densities of the law of the occupation time on the positive line for bessel bridges and the normalized excursion of strictly stable processes the key role is played by these properties for functions defined by riemannliouville fractional integrals
|
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|
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|
706.3163
|
Verhulst's logistic curve
|
We observe that the elementary logistic differential equation dP/dt=(1-P/M)kP
may be solved by first changing the variable to R=(M-P)/P. This reduces the
logistic differential equation to the simple linear differential equation
dR/dt=-kR, which can be solved without using the customary but slightly more
elaborate methods applied to the original logistic DE. The resulting solution
in terms of R can be converted by simple algebra to the familiar sigmoid
expression involving P. A biological argument is given for introducing logistic
growth via the simpler DE for R. It is also shown that the sigmoid P may be
written in terms of the hyperbolic tangent by a simple translation that is also
motivated by a biological argument.
|
math.HO math.CA
|
we observe that the elementary logistic differential equation dpdt1pmkp may be solved by first changing the variable to rmpp this reduces the logistic differential equation to the simple linear differential equation drdtkr which can be solved without using the customary but slightly more elaborate methods applied to the original logistic de the resulting solution in terms of r can be converted by simple algebra to the familiar sigmoid expression involving p a biological argument is given for introducing logistic growth via the simpler de for r it is also shown that the sigmoid p may be written in terms of the hyperbolic tangent by a simple translation that is also motivated by a biological argument
|
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|
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|
706.3164
|
Poisson sigma model on the sphere
|
We evaluate the path integral of the Poisson sigma model on sphere and study
the correlators of quantum observables. We argue that for the path integral to
be well-defined the corresponding
Poisson structure should be unimodular. The construction of the finite
dimensional BV theory is presented and we argue that it is responsible for the
leading semiclassical contribution. For a (twisted) generalized Kahler manifold
we discuss the gauge fixed action for the Poisson sigma model. Using the
localization we prove that for the holomorphic Poisson structure the
semiclassical result for the correlators is indeed the full quantum result.
|
hep-th math.SG
|
we evaluate the path integral of the poisson sigma model on sphere and study the correlators of quantum observables we argue that for the path integral to be welldefined the corresponding poisson structure should be unimodular the construction of the finite dimensional bv theory is presented and we argue that it is responsible for the leading semiclassical contribution for a twisted generalized kahler manifold we discuss the gauge fixed action for the poisson sigma model using the localization we prove that for the holomorphic poisson structure the semiclassical result for the correlators is indeed the full quantum result
|
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|
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|
706.3165
|
A solution for actors' viewpoints representation with collaborative
product development
|
As product complexity and marketing competition increase, a collaborative
product development is necessary for companies which develop high quality
products in short lead-times. To support product actors from different fields,
disciplines, and locations, wishing to exchange and share information, the
representation of the actors' viewpoints is the underlying requirement of the
collaborative product development. The actors' viewpoints approach was designed
to provide an organisational framework following the actors' perspectives in
the collaboration, and their relationships, could be explicitly gathered and
formatted. The approach acknowledges the inevitability of multiple integration
of product information as different views, promotes gathering of actors'
interests, and encourages retrieved adequate information while providing
support for integration through PLM and/or SCM collaboration. In this paper, a
solution for neutral viewpoints representation is proposed. The product,
process, and organisation information models are seriatim discussed. A series
of issues referring to the viewpoints representation are discussed in detail.
Based on XML standard, taking cyclone vessel as an example, an application case
of part of product information modelling is stated.
|
cs.HC
|
as product complexity and marketing competition increase a collaborative product development is necessary for companies which develop high quality products in short leadtimes to support product actors from different fields disciplines and locations wishing to exchange and share information the representation of the actors viewpoints is the underlying requirement of the collaborative product development the actors viewpoints approach was designed to provide an organisational framework following the actors perspectives in the collaboration and their relationships could be explicitly gathered and formatted the approach acknowledges the inevitability of multiple integration of product information as different views promotes gathering of actors interests and encourages retrieved adequate information while providing support for integration through plm andor scm collaboration in this paper a solution for neutral viewpoints representation is proposed the product process and organisation information models are seriatim discussed a series of issues referring to the viewpoints representation are discussed in detail based on xml standard taking cyclone vessel as an example an application case of part of product information modelling is stated
|
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|
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|
706.3166
|
The Equations of Motion of a Charged Particle in the Five-Dimensional
Model of the General Relativity Theory with the Four-Dimensional Nonholonomic
Velocity Space
|
We consider the four-dimensional nonholonomic distribution defined by the
4-potential of the electromagnetic field on the manifold. This distribution has
a metric tensor with the Lorentzian signature $(+,-,-,-)$, therefore, the
causal structure appears as in the general relativity theory. By means of the
Pontryagin's maximum principle we proved that the equations of the horizontal
geodesics for this distribution are the same as the equations of motion of a
charged particle in the general relativity theory. This is a Kaluza -- Klein
problem of classical and quantum physics solved by methods of sub-Lorentzian
geometry. We study the geodesics sphere which appears in a constant magnetic
field and its singular points. Sufficiently long geodesics are not optimal
solutions of the variational problem and define the nonholonomic wavefront.
This wavefront is limited by a convex elliptic cone. We also study variational
principle approach to the problem. The Euler -- Lagrange equations are the same
as those obtained by the Pontryagin's maximum principle if the restriction of
the metric tensor on the distribution is the same.
|
math.DG gr-qc math.MG math.OC physics.class-ph
|
we consider the fourdimensional nonholonomic distribution defined by the 4potential of the electromagnetic field on the manifold this distribution has a metric tensor with the lorentzian signature therefore the causal structure appears as in the general relativity theory by means of the pontryagins maximum principle we proved that the equations of the horizontal geodesics for this distribution are the same as the equations of motion of a charged particle in the general relativity theory this is a kaluza klein problem of classical and quantum physics solved by methods of sublorentzian geometry we study the geodesics sphere which appears in a constant magnetic field and its singular points sufficiently long geodesics are not optimal solutions of the variational problem and define the nonholonomic wavefront this wavefront is limited by a convex elliptic cone we also study variational principle approach to the problem the euler lagrange equations are the same as those obtained by the pontryagins maximum principle if the restriction of the metric tensor on the distribution is the same
|
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|
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|
706.3167
|
Production of a sterile species via active-sterile mixing: an exactly
solvable model
|
The production of a sterile species via active-sterile mixing in a thermal
medium is studied in an exactly solvable model. The \emph{exact} time evolution
of the sterile distribution function is determined by the dispersion relations
and damping rates $\Gamma_{1,2}$ for the quasiparticle modes. These depend on
$\wtg = \Gamma_{aa}/2\Delta E$, with $\Gamma_{aa}$ the interaction rate of the
active species in absence of mixing and $\Delta E$ the oscillation frequency in
the medium without damping. $\wtg \ll1,\wtg \gg 1$ describe the weak and strong
damping limits respectively. For $\wtg\ll1$, $\Gamma_1 = \Gamma_{aa}\cos^2\tm ;
\Gamma_{2}=\Gamma_{aa}\sin^2\tm$ where $\tm$ is the mixing angle in the medium
and the sterile distribution function \emph{does not} obey a simple rate
equation. For $\wtg \gg 1$, $\Gamma_1= \Gamma_{aa}$ and $\Gamma_2 = \Gamma_{aa}
\sin^22\tm/4\wtg^2$, is the sterile production rate. In this regime sterile
production is suppressed and the oscillation frequency \emph{vanishes} at an
MSW resonance, with a breakdown of adiabaticity. These are consequences of
quantum Zeno suppression. For active neutrinos with standard model interactions
the strong damping limit is \emph{only} available near an MSW resonance
\emph{if} $\sin\theta \lesssim \alpha_w$ with $\theta$ the vacuum mixing angle.
The full set of quantum kinetic equations for sterile production for arbitrary
$\wtg$ are obtained from the quantum master equation. Cosmological resonant
sterile neutrino production is quantum Zeno suppressed relieving potential
uncertainties associated with the QCD phase transition.
|
hep-ph
|
the production of a sterile species via activesterile mixing in a thermal medium is studied in an exactly solvable model the emphexact time evolution of the sterile distribution function is determined by the dispersion relations and damping rates gamma_12 for the quasiparticle modes these depend on wtg gamma_aa2delta e with gamma_aa the interaction rate of the active species in absence of mixing and delta e the oscillation frequency in the medium without damping wtg ll1wtg gg 1 describe the weak and strong damping limits respectively for wtgll1 gamma_1 gamma_aacos2tm gamma_2gamma_aasin2tm where tm is the mixing angle in the medium and the sterile distribution function emphdoes not obey a simple rate equation for wtg gg 1 gamma_1 gamma_aa and gamma_2 gamma_aa sin22tm4wtg2 is the sterile production rate in this regime sterile production is suppressed and the oscillation frequency emphvanishes at an msw resonance with a breakdown of adiabaticity these are consequences of quantum zeno suppression for active neutrinos with standard model interactions the strong damping limit is emphonly available near an msw resonance emphif sintheta lesssim alpha_w with theta the vacuum mixing angle the full set of quantum kinetic equations for sterile production for arbitrary wtg are obtained from the quantum master equation cosmological resonant sterile neutrino production is quantum zeno suppressed relieving potential uncertainties associated with the qcd phase transition
|
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|
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|
706.3168
|
Fluctuations and the clustering of color sources
|
We present our results on multiplicity and $p_T$ fluctuations at LHC energies
in the framework of the clustering of color sources. In this approach,
elementary color sources -strings- overlap forming clusters, so the number of
effective sources is modified. We find that the fluctuations are proportional
to the number of those clusters.
|
hep-ph
|
we present our results on multiplicity and p_t fluctuations at lhc energies in the framework of the clustering of color sources in this approach elementary color sources strings overlap forming clusters so the number of effective sources is modified we find that the fluctuations are proportional to the number of those clusters
|
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|
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|
706.3169
|
N=1* model superpotential revisited (IR behaviour of N=4 limit)
|
The one-loop contribution to the superpotential, in particular the
Veneziano-Yankielowicz potential in N=1 supersymmetric Yang-Mills model is
discussed from an elementary field theory method and the matrix model point of
view. Both approaches are based on the Renormalization Group variation of the
superconformal N=4 supersymmetric Yang-Mills model.
|
hep-th
|
the oneloop contribution to the superpotential in particular the venezianoyankielowicz potential in n1 supersymmetric yangmills model is discussed from an elementary field theory method and the matrix model point of view both approaches are based on the renormalization group variation of the superconformal n4 supersymmetric yangmills model
|
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|
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|
706.317
|
Asymptotic Analysis of General Multiuser Detectors in MIMO DS-CDMA
Channels
|
We analyze a MIMO DS-CDMA channel with a general multiuser detector including
a nonlinear multiuser detector, using the replica method. In the many-user,
limit the MIMO DS-CDMA channel with the multiuser detector is decoupled into a
bank of single-user SIMO Gaussian channels if a spatial spreading scheme is
employed. On the other hand, it is decoupled into a bank of single-user MIMO
Gaussian channels if a spatial spreading scheme is not employed. The spectral
efficiency of the MIMO DS-CDMA channel with the spatial spreading scheme is
comparable with that of the MIMO DS-CDMA channel using an optimal space-time
block code without the spatial spreading scheme. In the case of the QPSK data
modulation scheme the spectral efficiency of the MIMO DS-CDMA channel with the
MMSE detector shows {\it waterfall} behavior and is very close to the
corresponding sum capacity when the system load is just below the transition
point of the {\it waterfall} behavior. Our result implies that the performance
of a multiuser detector taking the data modulation scheme into consideration
can be far superior to that of linear multiuser detectors.
|
cs.IT math.IT
|
we analyze a mimo dscdma channel with a general multiuser detector including a nonlinear multiuser detector using the replica method in the manyuser limit the mimo dscdma channel with the multiuser detector is decoupled into a bank of singleuser simo gaussian channels if a spatial spreading scheme is employed on the other hand it is decoupled into a bank of singleuser mimo gaussian channels if a spatial spreading scheme is not employed the spectral efficiency of the mimo dscdma channel with the spatial spreading scheme is comparable with that of the mimo dscdma channel using an optimal spacetime block code without the spatial spreading scheme in the case of the qpsk data modulation scheme the spectral efficiency of the mimo dscdma channel with the mmse detector shows it waterfall behavior and is very close to the corresponding sum capacity when the system load is just below the transition point of the it waterfall behavior our result implies that the performance of a multiuser detector taking the data modulation scheme into consideration can be far superior to that of linear multiuser detectors
|
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|
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|
706.3171
|
Comment to the article "Possible Systematic Effects in Fomblin Coated
Storage Cell Neutron Lifetime Measurements", Steve K. Lamoreaux [1]
|
The author of article discusses the possible systematic effects in our
experiment using reference and picture from allegedly our publication. First of
all this publication does not exist. The assumption of author about the
probability of lower energy upscattering is in a rough contradiction (300
times) with our experimental limit which is extremely lower, about 6x10-9 per
neutron collision. The second assumption of author concerning quasi-stable
orbits of UCN with higher energy due to specular neutron reflection from trap
wall is also in a rough contradiction with our experimental data clear
demonstrated in our previous articles as well in the last very detailed article
recently presented in the arXiv.
We are very surprised that author discusses well known questions studied in
our experiment in details.
|
nucl-ex
|
the author of article discusses the possible systematic effects in our experiment using reference and picture from allegedly our publication first of all this publication does not exist the assumption of author about the probability of lower energy upscattering is in a rough contradiction 300 times with our experimental limit which is extremely lower about 6x109 per neutron collision the second assumption of author concerning quasistable orbits of ucn with higher energy due to specular neutron reflection from trap wall is also in a rough contradiction with our experimental data clear demonstrated in our previous articles as well in the last very detailed article recently presented in the arxiv we are very surprised that author discusses well known questions studied in our experiment in details
|
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|
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|
706.3172
|
Switching of the vortex polarity in a magnetic nanodisk by a DC current
|
We study the dynamics of a vortex state nanodisk due to a dc spin current,
perpendicular to the disk plane. The irreversible switching of the vortex
polarity takes place above some threshold current. The detailed description of
these processes is obtained by spin-lattice simulations.
|
cond-mat.str-el
|
we study the dynamics of a vortex state nanodisk due to a dc spin current perpendicular to the disk plane the irreversible switching of the vortex polarity takes place above some threshold current the detailed description of these processes is obtained by spinlattice simulations
|
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|
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|
706.3173
|
Sine-Gordon solitons, auxiliary fields, and singular limit of a double
pendulums chain
|
We consider the continuum version of an elastic chain supporting topological
and non-topological degrees of freedom; this generalizes a model for the
dynamics of DNA recently proposed and investigated by ourselves. In a certain
limit, the non-topological degrees of freedom are frozen, and the model reduces
to the sine-Gordon equations and thus supports well-known topological soliton
solutions. We consider a (singular) perturbative expansion around this limit
and study in particular how the non-topological field assume the role of an
auxiliary field. This provides a more general framework for the slaving of this
degree of freedom on the topological one, already observed elsewhere in the
context of the mentioned DNA model; in this framework one expects such
phenomenon to arise in a quite large class of field-theoretical models.
|
math-ph math.MP nlin.PS
|
we consider the continuum version of an elastic chain supporting topological and nontopological degrees of freedom this generalizes a model for the dynamics of dna recently proposed and investigated by ourselves in a certain limit the nontopological degrees of freedom are frozen and the model reduces to the sinegordon equations and thus supports wellknown topological soliton solutions we consider a singular perturbative expansion around this limit and study in particular how the nontopological field assume the role of an auxiliary field this provides a more general framework for the slaving of this degree of freedom on the topological one already observed elsewhere in the context of the mentioned dna model in this framework one expects such phenomenon to arise in a quite large class of fieldtheoretical models
|
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|
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|
706.3174
|
NGC4438 and its environment at radio wavelengths
|
We present multi-frequency, radio-continuum and HI observations of NGC4438,
the highly-disturbed, active galaxy in the Virgo cluster, with the VLA and the
GMRT. High-resolution observations with the VLA at 4860 and 8460 MHz show the
presence of an inverted-spectrum radio nucleus located between the highly
asymmetric lobes of radio emission. This demonstrates that these lobes arise
due to an AGN rather than a compact nuclear starburst. The low-frequency radio
continuum observations made with the GMRT detect the extended emission on the
western side of the galaxy whose spectral index is flatter at higher
frequencies and suggests that it is a mixture of thermal and non-thermal
emission.
The HI observations show an elongated structure which is displaced by ~4.1
kpc on the western side of NGC4438 and has a size of ~9.8 kpc and a mass of
1.8*10^8 M_sun. The velocity field suggests systematic rotation. We also detect
HI emission from the disk of the galaxy with a mass of 1.2*10^8 M_sun. We
detect a faint HI tail towards the north of NGC4438 close to a stellar tail
seen in deep optical observations. This HI tail has a total extent of ~50 kpc
and a mass of 1.4*10^8 M_sun if it is at the distance of NGC4438. The velocity
of the HI tail is ~-10 km/s similar to that of HI emission from IC 3355, but
the possibility that the tail could be foreground Galactic emission cannot be
ruled out. We discuss the different structures in the light of different
models.
|
astro-ph
|
we present multifrequency radiocontinuum and hi observations of ngc4438 the highlydisturbed active galaxy in the virgo cluster with the vla and the gmrt highresolution observations with the vla at 4860 and 8460 mhz show the presence of an invertedspectrum radio nucleus located between the highly asymmetric lobes of radio emission this demonstrates that these lobes arise due to an agn rather than a compact nuclear starburst the lowfrequency radio continuum observations made with the gmrt detect the extended emission on the western side of the galaxy whose spectral index is flatter at higher frequencies and suggests that it is a mixture of thermal and nonthermal emission the hi observations show an elongated structure which is displaced by 41 kpc on the western side of ngc4438 and has a size of 98 kpc and a mass of 18108 m_sun the velocity field suggests systematic rotation we also detect hi emission from the disk of the galaxy with a mass of 12108 m_sun we detect a faint hi tail towards the north of ngc4438 close to a stellar tail seen in deep optical observations this hi tail has a total extent of 50 kpc and a mass of 14108 m_sun if it is at the distance of ngc4438 the velocity of the hi tail is 10 kms similar to that of hi emission from ic 3355 but the possibility that the tail could be foreground galactic emission cannot be ruled out we discuss the different structures in the light of different models
|
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|
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|
706.3175
|
Unveiling new systematics in the self-assembly of atomic chains on
Si(111)
|
Self-assembled arrays of atomic chains on Si(111) represent a fascinating
family of nanostructures with quasi-one-dimensional electronic properties.
These surface reconstructions are stabilized by a variety of adsorbates ranging
from alkali and alkaline earth metals to noble and rare earth metals. Combining
the complementary strength of dynamical low-energy electron diffraction,
scanning tunneling microscopy and angle-resolved photoemission spectroscopy, we
recently showed that besides monovalent and divalent adsorbates, trivalent
adsorbates are also able to stabilize silicon honeycomb chains. Consequently
silicon honeycomb chains emerge as a most stable, universal building block
shared by many atomic chain structures. We here present the systematics behind
the self-assembly mechanism of these chain systems and relate the valence state
of the adsorbate to the accessible symmetries of the chains.
|
cond-mat.other
|
selfassembled arrays of atomic chains on si111 represent a fascinating family of nanostructures with quasionedimensional electronic properties these surface reconstructions are stabilized by a variety of adsorbates ranging from alkali and alkaline earth metals to noble and rare earth metals combining the complementary strength of dynamical lowenergy electron diffraction scanning tunneling microscopy and angleresolved photoemission spectroscopy we recently showed that besides monovalent and divalent adsorbates trivalent adsorbates are also able to stabilize silicon honeycomb chains consequently silicon honeycomb chains emerge as a most stable universal building block shared by many atomic chain structures we here present the systematics behind the selfassembly mechanism of these chain systems and relate the valence state of the adsorbate to the accessible symmetries of the chains
|
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|
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|
706.3176
|
Properties of noncommutative axionic electrodynamics
|
Using the gauge-invariant but path-dependent variables formalism, we compute
the static quantum potential for noncommutative axionic electrodynamics, and
find a radically different result than the corresponding commutative case. We
explicitly show that the static potential profile is analogous to that
encountered in both non-Abelian axionic electrodynamics and in Yang-Mills
theory with spontaneous symmetry breaking of scale symmetry.
|
hep-th
|
using the gaugeinvariant but pathdependent variables formalism we compute the static quantum potential for noncommutative axionic electrodynamics and find a radically different result than the corresponding commutative case we explicitly show that the static potential profile is analogous to that encountered in both nonabelian axionic electrodynamics and in yangmills theory with spontaneous symmetry breaking of scale symmetry
|
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|
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|
706.3177
|
Role of homeostasis in learning sparse representations
|
Neurons in the input layer of primary visual cortex in primates develop
edge-like receptive fields. One approach to understanding the emergence of this
response is to state that neural activity has to efficiently represent sensory
data with respect to the statistics of natural scenes. Furthermore, it is
believed that such an efficient coding is achieved using a competition across
neurons so as to generate a sparse representation, that is, where a relatively
small number of neurons are simultaneously active. Indeed, different models of
sparse coding, coupled with Hebbian learning and homeostasis, have been
proposed that successfully match the observed emergent response. However, the
specific role of homeostasis in learning such sparse representations is still
largely unknown. By quantitatively assessing the efficiency of the neural
representation during learning, we derive a cooperative homeostasis mechanism
that optimally tunes the competition between neurons within the sparse coding
algorithm. We apply this homeostasis while learning small patches taken from
natural images and compare its efficiency with state-of-the-art algorithms.
Results show that while different sparse coding algorithms give similar coding
results, the homeostasis provides an optimal balance for the representation of
natural images within the population of neurons. Competition in sparse coding
is optimized when it is fair. By contributing to optimizing statistical
competition across neurons, homeostasis is crucial in providing a more
efficient solution to the emergence of independent components.
|
q-bio.NC
|
neurons in the input layer of primary visual cortex in primates develop edgelike receptive fields one approach to understanding the emergence of this response is to state that neural activity has to efficiently represent sensory data with respect to the statistics of natural scenes furthermore it is believed that such an efficient coding is achieved using a competition across neurons so as to generate a sparse representation that is where a relatively small number of neurons are simultaneously active indeed different models of sparse coding coupled with hebbian learning and homeostasis have been proposed that successfully match the observed emergent response however the specific role of homeostasis in learning such sparse representations is still largely unknown by quantitatively assessing the efficiency of the neural representation during learning we derive a cooperative homeostasis mechanism that optimally tunes the competition between neurons within the sparse coding algorithm we apply this homeostasis while learning small patches taken from natural images and compare its efficiency with stateoftheart algorithms results show that while different sparse coding algorithms give similar coding results the homeostasis provides an optimal balance for the representation of natural images within the population of neurons competition in sparse coding is optimized when it is fair by contributing to optimizing statistical competition across neurons homeostasis is crucial in providing a more efficient solution to the emergence of independent components
|
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|
[-0.06938039924098442, 0.10723098003281284, -0.06404840800317779, 0.06803485414371785, -0.06257569281779955, -0.18538501183090286, 0.03721441804076982, 0.4197193516904604, -0.2937591244555202, -0.3055310224616113, 0.05051710789938729, -0.22480850018338358, -0.2710721564759393, 0.141502625314082, -0.14233330064618022, 0.026026025765000602, 0.05205131328532851, 0.06326491605960229, 0.023185172926972464, -0.25028269497710653, 0.24710430314793227, 0.09138269875346955, 0.35520059617949173, -0.030610227166155798, 0.14704324711841507, -0.0526466113206131, 9.509137279428212e-06, -0.026542184659613676, -0.022160182332975967, 0.180380184696091, 0.37329879269978783, 0.19000033994611076, 0.3332265411715839, -0.4558934895074473, -0.2577173303734445, 0.08194405235045185, 0.17199244666885816, 0.10753029149511945, -0.04881421695711901, -0.2457155269875595, 0.10161569590095133, -0.13295070848848045, 0.008723485608074188, -0.12012200372961176, 0.008822934286858458, 0.028529080721720706, -0.32720306311116915, 0.0661848006085946, 0.06942321795432424, 0.07434034035582326, -0.08681477667131271, -0.07042344390176158, -0.001916973899011459, 0.20991320264965102, 0.03663228445406179, 0.05974178298055071, 0.15168755552685095, -0.18865753328031037, -0.11704102357843298, 0.329380199833942, -0.014966534246923402, -0.194010027383961, 0.21450306320319826, -0.07134701828142645, -0.12850082684225872, 0.13732965389241886, 0.20634567846164964, 0.05974315008791411, -0.1675803043060669, -0.0007286938654250606, -0.05065738433349746, 0.21066250818507515, 0.03621405691930414, 0.031109154207912167, 0.1707797727523891, 0.2603150703830941, 0.04698573096123585, 0.14844774572792735, -0.07085713954329227, -0.11023926827438439, -0.2055311190310569, -0.05368586304284369, -0.1842625635836801, -0.025769536096017513, -0.13782130501609588, -0.1384866547057883, 0.42406574219663057, 0.1760950450460551, 0.19976671445799418, 0.0881855477693808, 0.29670038192112624, 0.051944518638506895, 0.12258970032784, 0.09283438767615573, 0.21237091580199788, 0.12671166139065526, 0.08926400932302056, -0.2347052296102294, 0.13547937729935763, 0.027268628918450423]
|
706.3178
|
Representing a product system representation as a contractive semigroup
and applications to regular isometric dilations
|
In this paper we propose a new technical tool for analyzing representations
of Hilbert $C^*$-product systems. Using this tool, we give a new proof that
every doubly commuting representation over $\mathbb{N}^k$ has a regular
isometric dilation, and we also prove sufficient conditions for the existence
of a regular isometric dilation of representations over more general
subsemigroups of $\mathbb{R}_+^k$.
|
math.OA
|
in this paper we propose a new technical tool for analyzing representations of hilbert cproduct systems using this tool we give a new proof that every doubly commuting representation over mathbbnk has a regular isometric dilation and we also prove sufficient conditions for the existence of a regular isometric dilation of representations over more general subsemigroups of mathbbr_k
|
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|
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|
706.3179
|
Supernova remnants with magnetars: clues to magnetar formation
|
I discuss the lack of observational evidence that magnetars are formed as
rapidly rotating neutron stars. Supernova remnants containing magnetars do not
show the excess of kinetic energy expected for such a formation scenario, nor
is there any evidence for a relic pulsar wind nebula. However, it could be that
magnetars are formed with somewhat slower rotation periods, or that not all
excess rotational energy was used to boost the explosion energy, for example as
a result of gravitational radiation. Another observational tests for the rapid
initial period hypothesis is to look for statistical evidence that about 1% of
the observed supernovae have an additional 1E40-1E44 erg/s excess energy during
the first year, caused by the spin down luminosity of a magnetar. An
alternative scenario for the high magnetic fields of magnetars is the fossil
field hypothesis, in which the magnetic field is inherited from the progenitor
star. Direct observational tests for this hypothesis are harder to formulate,
unless the neutron star formed in the SN1987A explosion emerges as a slowly
rotating magnetar. Finally, I point out the possible connection between the
jets in Cas A and its X-ray point source: the jets in Cas A may indicate that
the explosion was accompanied by an X-ray flash, probably powered by a rapidly
rotating compact object. However, the point source in Cas A does not seem to be
a rapidly rotating neutron star, suggesting that the neutron star has slowed
down considerably in 330 yr, requiring a magnetar-like field.
|
astro-ph
|
i discuss the lack of observational evidence that magnetars are formed as rapidly rotating neutron stars supernova remnants containing magnetars do not show the excess of kinetic energy expected for such a formation scenario nor is there any evidence for a relic pulsar wind nebula however it could be that magnetars are formed with somewhat slower rotation periods or that not all excess rotational energy was used to boost the explosion energy for example as a result of gravitational radiation another observational tests for the rapid initial period hypothesis is to look for statistical evidence that about 1 of the observed supernovae have an additional 1e401e44 ergs excess energy during the first year caused by the spin down luminosity of a magnetar an alternative scenario for the high magnetic fields of magnetars is the fossil field hypothesis in which the magnetic field is inherited from the progenitor star direct observational tests for this hypothesis are harder to formulate unless the neutron star formed in the sn1987a explosion emerges as a slowly rotating magnetar finally i point out the possible connection between the jets in cas a and its xray point source the jets in cas a may indicate that the explosion was accompanied by an xray flash probably powered by a rapidly rotating compact object however the point source in cas a does not seem to be a rapidly rotating neutron star suggesting that the neutron star has slowed down considerably in 330 yr requiring a magnetarlike field
|
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|
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|
706.318
|
The Emerging Features of Bipolar Magnetic Regions during Solar Minima
|
Solar magnetic synoptic charts obtained by NSO/Kitt Peak and SOHO/MDI are
analyzed for studying the appearance of bipolar magnetic regions (BMRs) during
solar minima. As a result, we find the emergence of long-lived BMRs has three
typical features. (1) BMRs' emerging rates of the new cycles increase about 3
times faster than those of the old cycles decrease. (2) Two consecutive solar
cycles have an overlapping period of near 10 Carrington rotations. During this
very short overlapping time interval, BMRs of two cycles tend to concentrate in
the same longitudes. (3) About 53% BMRs distribute with a longitudinal distance
of 1/8 solar rotation. Such phenomenon suggests a longitudinal mode of m=8
existing during solar minima.
|
astro-ph
|
solar magnetic synoptic charts obtained by nsokitt peak and sohomdi are analyzed for studying the appearance of bipolar magnetic regions bmrs during solar minima as a result we find the emergence of longlived bmrs has three typical features 1 bmrs emerging rates of the new cycles increase about 3 times faster than those of the old cycles decrease 2 two consecutive solar cycles have an overlapping period of near 10 carrington rotations during this very short overlapping time interval bmrs of two cycles tend to concentrate in the same longitudes 3 about 53 bmrs distribute with a longitudinal distance of 18 solar rotation such phenomenon suggests a longitudinal mode of m8 existing during solar minima
|
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|
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|
706.3181
|
Simulation of the Single- and Double-Slit Experiments with Quantum
Walkers
|
We employ the broken-link model to create a barrier with slits in a
two-dimensional lattice. The diffraction and interference patterns of the
probability distribution of quantum walkers passing through the slits are
analyzed. Simulations were performed using the main types of coins, and display
diffraction and interference patterns that depend on the choice of coins.
|
quant-ph
|
we employ the brokenlink model to create a barrier with slits in a twodimensional lattice the diffraction and interference patterns of the probability distribution of quantum walkers passing through the slits are analyzed simulations were performed using the main types of coins and display diffraction and interference patterns that depend on the choice of coins
|
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|
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|
706.3182
|
Flux Densities and Radio Polarization Characteristics of Two Vela-like
Pulsars
|
We report on dual-frequency radio polarimetry observations of two young,
energetic pulsars, PSRs J0940-5428 and J1301-6305. These were among the first
Vela-like pulsars discovered in the Parkes Multibeam survey. We conducted
observations of these pulsars with the Australia Telescope Compact Array (ATCA)
at center frequencies of 1384 and 2496 MHz using pulsar gating while preserving
full Stokes parameters. After correcting for bandwidth depolarization, we have
measured polarization characteristics, flux densities, and rotation measures
for these pulsars. The spectral indices derived from the ATCA data are shallow
but still consistent with values seen for pulsars of this type. The rotation
measures for both pulsars are consistent with those reported recently using
data from the Parkes telescope, and both pulsars have highly linearly polarized
pulse profiles at both 1384 and 2496 MHz. Our results support a previously
noted correlation between high degree of linear polarization, shallow spectral
index, and large spin-down luminosity.
|
astro-ph
|
we report on dualfrequency radio polarimetry observations of two young energetic pulsars psrs j09405428 and j13016305 these were among the first velalike pulsars discovered in the parkes multibeam survey we conducted observations of these pulsars with the australia telescope compact array atca at center frequencies of 1384 and 2496 mhz using pulsar gating while preserving full stokes parameters after correcting for bandwidth depolarization we have measured polarization characteristics flux densities and rotation measures for these pulsars the spectral indices derived from the atca data are shallow but still consistent with values seen for pulsars of this type the rotation measures for both pulsars are consistent with those reported recently using data from the parkes telescope and both pulsars have highly linearly polarized pulse profiles at both 1384 and 2496 mhz our results support a previously noted correlation between high degree of linear polarization shallow spectral index and large spindown luminosity
|
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|
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|
706.3183
|
Entanglement Production in Non-Equilibrium Thermodynamics
|
We define and analyse the concept of entanglement production during the
evolution of a general quantum mechanical dissipative system. While it is
important to minimise entropy production in order to achieve thermodynamical
efficiency, maximising the rate of change of entanglement is important in
quantum information processing. Quantitative relations are obtained between
entropy and entanglement productions, under specific assumptions detailed in
the text. We apply these to the processes of dephasing and decay of
correlations between two initially entangled qubits. Both the Master equation
treatment as well as the higher Hilbert space analysis are presented. Our
formalism is very general and contains as special cases many reported
individual instance of entanglement dynamics, such as, for example, the
recently discovered notion of the sudden death of entanglement.
|
quant-ph
|
we define and analyse the concept of entanglement production during the evolution of a general quantum mechanical dissipative system while it is important to minimise entropy production in order to achieve thermodynamical efficiency maximising the rate of change of entanglement is important in quantum information processing quantitative relations are obtained between entropy and entanglement productions under specific assumptions detailed in the text we apply these to the processes of dephasing and decay of correlations between two initially entangled qubits both the master equation treatment as well as the higher hilbert space analysis are presented our formalism is very general and contains as special cases many reported individual instance of entanglement dynamics such as for example the recently discovered notion of the sudden death of entanglement
|
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|
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|
706.3184
|
Late-time behaviour of the tilted Bianchi type VI$_{-1/9}$ models
|
We study tilted perfect fluid cosmological models with a constant equation of
state parameter in spatially homogeneous models of Bianchi type VI$_{-1/9}$
using dynamical systems methods and numerical simulations. We study models with
and without vorticity, with an emphasis on their future asymptotic evolution.
We show that for models with vorticity there exists, in a small region of
parameter space, a closed curve acting as the attractor.
|
gr-qc astro-ph math-ph math.MP
|
we study tilted perfect fluid cosmological models with a constant equation of state parameter in spatially homogeneous models of bianchi type vi_19 using dynamical systems methods and numerical simulations we study models with and without vorticity with an emphasis on their future asymptotic evolution we show that for models with vorticity there exists in a small region of parameter space a closed curve acting as the attractor
|
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|
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|
706.3185
|
Resistivity effects in surface superconductivity of thin films in strong
magnetic fields
|
Phase slips creation in the thin film in perpendicular magnetic filed with
edge superconductivity is studied. These centers are due to thermal activation
of the order parameter below superconducting temperature transition leading to
the suppression of the superconductivity. The corresponding resistance is
calculated. The Alsamazov- Larkin correction to the conductivity above the
critical magnetic field destroying the surface superconductivity is studied.
Such structures could be applied as a new system for the study of the phase
slip phenomenon in one- dimensional superconducting wires.
|
cond-mat.supr-con
|
phase slips creation in the thin film in perpendicular magnetic filed with edge superconductivity is studied these centers are due to thermal activation of the order parameter below superconducting temperature transition leading to the suppression of the superconductivity the corresponding resistance is calculated the alsamazov larkin correction to the conductivity above the critical magnetic field destroying the surface superconductivity is studied such structures could be applied as a new system for the study of the phase slip phenomenon in one dimensional superconducting wires
|
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|
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|
706.3186
|
Precision spectroscopy with two correlated atoms
|
We discuss techniques that allow for long coherence times in laser
spectroscopy experiments with two trapped ions. We show that for this purpose
not only entangled ions prepared in decoherence-free subspaces can be used but
also a pair of ions that are not entangled but subject to the same kind of
phase noise. We apply this technique to a measurement of the electric
quadrupole moment of the 3d D5/2 state of 40Ca+ and to a measurement of the
linewidth of an ultrastable laser exciting a pair of 40Ca+ ions.
|
quant-ph physics.atom-ph
|
we discuss techniques that allow for long coherence times in laser spectroscopy experiments with two trapped ions we show that for this purpose not only entangled ions prepared in decoherencefree subspaces can be used but also a pair of ions that are not entangled but subject to the same kind of phase noise we apply this technique to a measurement of the electric quadrupole moment of the 3d d52 state of 40ca and to a measurement of the linewidth of an ultrastable laser exciting a pair of 40ca ions
|
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|
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|
706.3187
|
Simulations of the Poynting--Robertson Cosmic Battery in Resistive
Accretion Disks
|
We describe the results of numerical "2.5--dimensional" MHD simulations of an
initially unmagnetized disk model orbiting a central point--mass and responding
to the continual generation of poloidal magnetic field due to a secular source
that emulates the Poynting--Robertson (PR) drag on electrons in the vicinity of
a luminous stellar or compact accreting object. The fluid in the disk and in
the surrounding hotter atmosphere has finite electrical conductivity and allows
for the magnetic field to diffuse freely out of the areas where it is
generated, while at the same time, the differential rotation of the disk twists
the poloidal field and quickly induces a substantial toroidal--field component.
The secular PR term has dual purpose in these simulations as the source of the
magnetic field and the trigger of a magnetorotational instability (MRI) in the
disk. The MRI is especially mild and does not destroy the disk because a small
amount of resistivity dampens the instability efficiently. In simulations with
moderate resistivities (diffusion timescales up to $\sim$16 local dynamical
times) and after $\sim$100 orbits, the MRI has managed to transfer outward
substantial amounts of angular momentum and the inner edge of the disk, along
with azimuthal magnetic flux, has flowed toward the central point--mass where a
new, magnetized, nuclear disk has formed. The toroidal field in this nuclear
disk is amplified by differential rotation and it cannot be contained; when it
approaches equipartition, it unwinds vertically and produces episodic jet--like
outflows. The poloidal field in the inner region cannot diffuse back out if the
characteristic diffusion time is of the order of or larger than the dynamical
time; it continues to grow linearly in time undisturbed and without saturation,
as the outer sections of many poloidal loops are being drawn radially outward.
|
astro-ph
|
we describe the results of numerical 25dimensional mhd simulations of an initially unmagnetized disk model orbiting a central pointmass and responding to the continual generation of poloidal magnetic field due to a secular source that emulates the poyntingrobertson pr drag on electrons in the vicinity of a luminous stellar or compact accreting object the fluid in the disk and in the surrounding hotter atmosphere has finite electrical conductivity and allows for the magnetic field to diffuse freely out of the areas where it is generated while at the same time the differential rotation of the disk twists the poloidal field and quickly induces a substantial toroidalfield component the secular pr term has dual purpose in these simulations as the source of the magnetic field and the trigger of a magnetorotational instability mri in the disk the mri is especially mild and does not destroy the disk because a small amount of resistivity dampens the instability efficiently in simulations with moderate resistivities diffusion timescales up to sim16 local dynamical times and after sim100 orbits the mri has managed to transfer outward substantial amounts of angular momentum and the inner edge of the disk along with azimuthal magnetic flux has flowed toward the central pointmass where a new magnetized nuclear disk has formed the toroidal field in this nuclear disk is amplified by differential rotation and it cannot be contained when it approaches equipartition it unwinds vertically and produces episodic jetlike outflows the poloidal field in the inner region cannot diffuse back out if the characteristic diffusion time is of the order of or larger than the dynamical time it continues to grow linearly in time undisturbed and without saturation as the outer sections of many poloidal loops are being drawn radially outward
|
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|
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|
706.3188
|
A tutorial on conformal prediction
|
Conformal prediction uses past experience to determine precise levels of
confidence in new predictions. Given an error probability $\epsilon$, together
with a method that makes a prediction $\hat{y}$ of a label $y$, it produces a
set of labels, typically containing $\hat{y}$, that also contains $y$ with
probability $1-\epsilon$. Conformal prediction can be applied to any method for
producing $\hat{y}$: a nearest-neighbor method, a support-vector machine, ridge
regression, etc.
Conformal prediction is designed for an on-line setting in which labels are
predicted successively, each one being revealed before the next is predicted.
The most novel and valuable feature of conformal prediction is that if the
successive examples are sampled independently from the same distribution, then
the successive predictions will be right $1-\epsilon$ of the time, even though
they are based on an accumulating dataset rather than on independent datasets.
In addition to the model under which successive examples are sampled
independently, other on-line compression models can also use conformal
prediction. The widely used Gaussian linear model is one of these.
This tutorial presents a self-contained account of the theory of conformal
prediction and works through several numerical examples. A more comprehensive
treatment of the topic is provided in "Algorithmic Learning in a Random World",
by Vladimir Vovk, Alex Gammerman, and Glenn Shafer (Springer, 2005).
|
cs.LG stat.ML
|
conformal prediction uses past experience to determine precise levels of confidence in new predictions given an error probability epsilon together with a method that makes a prediction haty of a label y it produces a set of labels typically containing haty that also contains y with probability 1epsilon conformal prediction can be applied to any method for producing haty a nearestneighbor method a supportvector machine ridge regression etc conformal prediction is designed for an online setting in which labels are predicted successively each one being revealed before the next is predicted the most novel and valuable feature of conformal prediction is that if the successive examples are sampled independently from the same distribution then the successive predictions will be right 1epsilon of the time even though they are based on an accumulating dataset rather than on independent datasets in addition to the model under which successive examples are sampled independently other online compression models can also use conformal prediction the widely used gaussian linear model is one of these this tutorial presents a selfcontained account of the theory of conformal prediction and works through several numerical examples a more comprehensive treatment of the topic is provided in algorithmic learning in a random world by vladimir vovk alex gammerman and glenn shafer springer 2005
|
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|
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|
706.3189
|
Exponentially Expanding Radiation Dominated and Dust Dominated Universes
in Brans-Dicke Theory
|
The Brans-Dicke Theory of Gravity is one of the most promising alternatives
to the Einstein's Theory of General Relativity. We have examined an action term
with wrong signs for both the kinetic and mass terms for the scalar field and
have found solutions for both the scale factor of the universe and the
Brans-Dicke scalar field which vary exponentially in time.
|
gr-qc
|
the bransdicke theory of gravity is one of the most promising alternatives to the einsteins theory of general relativity we have examined an action term with wrong signs for both the kinetic and mass terms for the scalar field and have found solutions for both the scale factor of the universe and the bransdicke scalar field which vary exponentially in time
|
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|
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|
706.319
|
Equilibrium nano-shape changes induced by epitaxial stress (generalised
Wulf-Kaishew theorem)
|
A generalised Wulf-Kaishew theorem is given describing the equilibrium shape
(ES) of an isolated 3D crystal A deposited coherently onto a lattice mismatched
planar substrate. For this purpose a free polyhedral crystal is formed then
homogeneously strained to be accommodated onto the lattice mismatched
substrate. During its elastic inhomogeneous relaxation the epitaxial contact
remains coherent so that the 3D crystal drags the atoms of the contact area and
produces a strain field in the substrate. The ES of the deposit is obtained by
minimising at constant volume the total energy (bulk and surface energies)
taking into account the bulk elastic relaxation. Our main results are: (1)
Epitaxial strain acts against wetting (adhesion) so that globally it leads to a
thickening of the ES. (2) Owing to strain the ES changes with size. More
precisely the various facets extension changes, some facets decreasing, some
others increasing. (3) Each dislocation entrance, necessary for relaxing
plastically too large crystals abruptly modifies the ES and thus the different
facets extension in a jerky way. (4) In all cases the usual self-similarity
with size is lost when misfit is considered. We illustrate these points in case
of box shaped and truncated pyramidal crystals. Some experimental evidences are
discussed.
|
cond-mat.mtrl-sci
|
a generalised wulfkaishew theorem is given describing the equilibrium shape es of an isolated 3d crystal a deposited coherently onto a lattice mismatched planar substrate for this purpose a free polyhedral crystal is formed then homogeneously strained to be accommodated onto the lattice mismatched substrate during its elastic inhomogeneous relaxation the epitaxial contact remains coherent so that the 3d crystal drags the atoms of the contact area and produces a strain field in the substrate the es of the deposit is obtained by minimising at constant volume the total energy bulk and surface energies taking into account the bulk elastic relaxation our main results are 1 epitaxial strain acts against wetting adhesion so that globally it leads to a thickening of the es 2 owing to strain the es changes with size more precisely the various facets extension changes some facets decreasing some others increasing 3 each dislocation entrance necessary for relaxing plastically too large crystals abruptly modifies the es and thus the different facets extension in a jerky way 4 in all cases the usual selfsimilarity with size is lost when misfit is considered we illustrate these points in case of box shaped and truncated pyramidal crystals some experimental evidences are discussed
|
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|
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|
706.3191
|
Spinar Paradigm and Gamma Ray Bursts Central Engine
|
A spinar is a quasi-equilibrium collapsing object whose equilibrium is
maintained by the balance of centrifugal and gravitational forces and whose
evolution is determined by its magnetic field. The spinar quasi equilibrium
model recently discussed as the course for extralong X-ray plateu in GRB
(Lipunov & Gorbovskoy, 2007). We propose a simple non stationary
three-parameter collapse model with the determining role of rotation and
magnetic field in this paper. The input parameters of the theory are the mass,
angular momentum, and magnetic field of the collapsar. The model includes
approximate description of the following effects: centrifugal force,
relativistic effects of the Kerr metrics, pressure of nuclear matter,
dissipation of angular momentum due to magnetic field, decrease of the dipole
magnetic moment due to compression and general-relativity effects (the black
hole has no hare), neutrino cooling, time dilatation, and gravitational
redshift. The model describes the temporal behavior of the central engine and
demonstrates the qualitative variety of the types of such behavior in nature.
We apply our approach to explain the observed features of gamma-ray bursts of
all types. In particular, the model allows the phenomena of precursors, x-ray
and optical bursts, and the appearance of a plateau on time scales of several
thousand seconds to be unified.
|
astro-ph
|
a spinar is a quasiequilibrium collapsing object whose equilibrium is maintained by the balance of centrifugal and gravitational forces and whose evolution is determined by its magnetic field the spinar quasi equilibrium model recently discussed as the course for extralong xray plateu in grb lipunov gorbovskoy 2007 we propose a simple non stationary threeparameter collapse model with the determining role of rotation and magnetic field in this paper the input parameters of the theory are the mass angular momentum and magnetic field of the collapsar the model includes approximate description of the following effects centrifugal force relativistic effects of the kerr metrics pressure of nuclear matter dissipation of angular momentum due to magnetic field decrease of the dipole magnetic moment due to compression and generalrelativity effects the black hole has no hare neutrino cooling time dilatation and gravitational redshift the model describes the temporal behavior of the central engine and demonstrates the qualitative variety of the types of such behavior in nature we apply our approach to explain the observed features of gammaray bursts of all types in particular the model allows the phenomena of precursors xray and optical bursts and the appearance of a plateau on time scales of several thousand seconds to be unified
|
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|
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|
706.3192
|
Hankel determinant and orthogonal polynomials for the Gaussian weight
with a jump
|
We obtain asymptotics in n for the n-dimensional Hankel determinant whose
symbol is the Gaussian multiplied by a step-like function. We use
Riemann-Hilbert analysis of the related system of orthogonal polynomials to
obtain our results.
|
math.FA math-ph math.MP
|
we obtain asymptotics in n for the ndimensional hankel determinant whose symbol is the gaussian multiplied by a steplike function we use riemannhilbert analysis of the related system of orthogonal polynomials to obtain our results
|
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|
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|
706.3193
|
Crossing the Wall: Branes vs. Bundles
|
We test a recently proposed wall-crossing formula for the change of the
Hilbert space of BPS states in d=4,N=2 theories. We study decays of D4D2D0
systems into pairs of D4D2D0 systems and we show how the wall-crossing formula
reproduces results of Goettsche and Yoshioka on wall-crossing behavior of the
moduli of slope-stable holomorphic bundles over holomorphic surfaces. Our
comparison shows very clearly that the moduli space of the D4D2D0 system on a
rigid surface in a Calabi-Yau is not the same as the moduli space of torsion
free sheaves, even when worldhseet instantons are neglected. Moreover, we argue
that the physical formula should make some new mathematical predictions for a
future theory of the moduli of stable objects in the derived category.
|
hep-th
|
we test a recently proposed wallcrossing formula for the change of the hilbert space of bps states in d4n2 theories we study decays of d4d2d0 systems into pairs of d4d2d0 systems and we show how the wallcrossing formula reproduces results of goettsche and yoshioka on wallcrossing behavior of the moduli of slopestable holomorphic bundles over holomorphic surfaces our comparison shows very clearly that the moduli space of the d4d2d0 system on a rigid surface in a calabiyau is not the same as the moduli space of torsion free sheaves even when worldhseet instantons are neglected moreover we argue that the physical formula should make some new mathematical predictions for a future theory of the moduli of stable objects in the derived category
|
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|
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|
706.3194
|
Phase resolved spectroscopy of the Vela pulsar with XMM-Newton
|
The ~10^4 y old Vela Pulsar represents the bridge between the young Crab-like
and the middle-aged rotation powered pulsars. Its multiwavelength behaviour is
due to the superposition of different spectral components. We take advantage of
the unprecedented harvest of photons collected by XMM-Newton to assess the Vela
Pulsar spectral shape and to study the pulsar spectrum as a function of its
rotational phase. As for the middle-aged pulsars Geminga, PSR B0656+14 and PSR
B1055-52 (the "Three Musketeers"), the phase-integrated spectrum of Vela is
well described by a three-component model, consisting of two blackbodies
(T_bb1=(1.06+/-0.03)x10^6 K, R_bb1=5.1+/-0.3 km, T_bb2=(2.16+/-0.06)x10^6 K,
R_bb2=0.73+/-0.08 km) plus a power-law (gamma=2.2+/-0.3). The relative
contributions of the three components are seen to vary as a function of the
pulsar rotational phase. The two blackbodies have a shallow 7-9% modulation.
The cooler blackbody, possibly related to the bulk of the neutron star surface,
has a complex modulation, with two peaks per period, separated by ~0.35 in
phase, the radio pulse occurring exactly in between. The hotter blackbody,
possibly originating from a hot polar region, has a nearly sinusoidal
modulation, with a single, broad maximum aligned with the second peak of the
cooler blackbody, trailing the radio pulse by ~0.15 in phase. The non thermal
component, magnetospheric in origin, is present only during 20% of the pulsar
phase and appears to be opposite to the radio pulse. XMM-Newton phase-resolved
spectroscopy unveils the link between the thermally emitting surface of the
neutron star and its charge-filled magnetosphere, probing emission geometry as
a function of the pulsar rotation. This is a fundamental piece of information
for future 3-dimensional modeling of the pulsar magnetosphere.
|
astro-ph
|
the 104 y old vela pulsar represents the bridge between the young crablike and the middleaged rotation powered pulsars its multiwavelength behaviour is due to the superposition of different spectral components we take advantage of the unprecedented harvest of photons collected by xmmnewton to assess the vela pulsar spectral shape and to study the pulsar spectrum as a function of its rotational phase as for the middleaged pulsars geminga psr b065614 and psr b105552 the three musketeers the phaseintegrated spectrum of vela is well described by a threecomponent model consisting of two blackbodies t_bb1106003x106 k r_bb15103 km t_bb2216006x106 k r_bb2073008 km plus a powerlaw gamma2203 the relative contributions of the three components are seen to vary as a function of the pulsar rotational phase the two blackbodies have a shallow 79 modulation the cooler blackbody possibly related to the bulk of the neutron star surface has a complex modulation with two peaks per period separated by 035 in phase the radio pulse occurring exactly in between the hotter blackbody possibly originating from a hot polar region has a nearly sinusoidal modulation with a single broad maximum aligned with the second peak of the cooler blackbody trailing the radio pulse by 015 in phase the non thermal component magnetospheric in origin is present only during 20 of the pulsar phase and appears to be opposite to the radio pulse xmmnewton phaseresolved spectroscopy unveils the link between the thermally emitting surface of the neutron star and its chargefilled magnetosphere probing emission geometry as a function of the pulsar rotation this is a fundamental piece of information for future 3dimensional modeling of the pulsar magnetosphere
|
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|
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|
706.3195
|
Genetic Transferability of Anomalous Irradiation Alterations of
Antibiotic Activity
|
It previously has been discovered that visible light irradiation of
crystalline substrates can lead to enhancement of subsequent enzymatic reaction
rates as sharply peaked oscillatory functions of irradiation time. The
particular activating irradiation times can vary with source of a given enzyme
and thus, presumably, its molecular structure. The experiments reported here
demonstrate that the potential for this anomalous enzyme reaction rate
enhancement can be transferred from one bacterial species to another coincident
with transfer of the genetic determinant for the relevant enzyme. In
particular, the effect of crystal-irradiated chloramphenicol on growth of
bacterial strains in which a transferable R-factor DNA plasmid coding for
chloramphenicol resistance was or was not present (S. panama R+, E. coli R+,
and E. coli R-) was determined. Chloramphenicol samples irradiated 10, 35 and
60 sec produced increased growth rates (diminished inhibition) for the
resistant S. panama and E. coli strains, while having no such effect on growth
rate of the sensitive E. coli strain. Consistent with past findings,
chloramphenicol samples irradiated 5, 30 and 55 sec produced decreased growth
rates (increased inhibition) for all three strains.
|
q-bio.BM
|
it previously has been discovered that visible light irradiation of crystalline substrates can lead to enhancement of subsequent enzymatic reaction rates as sharply peaked oscillatory functions of irradiation time the particular activating irradiation times can vary with source of a given enzyme and thus presumably its molecular structure the experiments reported here demonstrate that the potential for this anomalous enzyme reaction rate enhancement can be transferred from one bacterial species to another coincident with transfer of the genetic determinant for the relevant enzyme in particular the effect of crystalirradiated chloramphenicol on growth of bacterial strains in which a transferable rfactor dna plasmid coding for chloramphenicol resistance was or was not present s panama r e coli r and e coli r was determined chloramphenicol samples irradiated 10 35 and 60 sec produced increased growth rates diminished inhibition for the resistant s panama and e coli strains while having no such effect on growth rate of the sensitive e coli strain consistent with past findings chloramphenicol samples irradiated 5 30 and 55 sec produced decreased growth rates increased inhibition for all three strains
|
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|
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|
706.3196
|
Super Heavy Dark Matter and UHECR Anisotropy at Low Energy
|
Super Heavy quasi-stable particles are naturally produced in the early
universe and could represent a substantial fraction of the Dark Matter: the
so-called Super Heavy Dark Matter (SHDM). The decay of SHDM represents also a
possible source of Ultra High Energy Cosmic Rays (UHECR), with a reliably
calculated spectrum of the particles produced in the decay $(\propto
E^{-1.9})$. The SHDM model for the production of UHECR can explain
quantitatively only the excess of UHE events observed by AGASA. In the case of
an observed spectrum not showing the AGASA excess the SHDM model can provide
only a {\it subdominant} contribution to the UHECR flux. We discuss here the
basic features of SHDM for the production of a {\it subdominant} UHECR flux, we
refer our study to the possible signatures of the model at the Auger
observatory discussing in particular the expected chemical composition and
anisotropy.
|
astro-ph
|
super heavy quasistable particles are naturally produced in the early universe and could represent a substantial fraction of the dark matter the socalled super heavy dark matter shdm the decay of shdm represents also a possible source of ultra high energy cosmic rays uhecr with a reliably calculated spectrum of the particles produced in the decay propto e19 the shdm model for the production of uhecr can explain quantitatively only the excess of uhe events observed by agasa in the case of an observed spectrum not showing the agasa excess the shdm model can provide only a it subdominant contribution to the uhecr flux we discuss here the basic features of shdm for the production of a it subdominant uhecr flux we refer our study to the possible signatures of the model at the auger observatory discussing in particular the expected chemical composition and anisotropy
|
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|
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|
706.3197
|
An HI study of three long-tailed irregular galaxies in the cluster
Abell1367
|
We present the results on the distribution and kinematics of H$\sc{i}$ gas
with higher sensitivity and in one case of higher spectral resolution as well
than reported earlier, of three irregular galaxies CGCG 097073, 097079 and
097087 (UGC 06697) in the cluster Abell 1367. These galaxies are known to
exhibit long (50$-$75 kpc) tails of radio continuum and optical emission lines
(H$\alpha$) pointing away from the cluster centre and arcs of starformation on
the opposite sides of the tails. These features as well as the H{\sc i}
properties, with two of the galaxies (CGCG 097073 and 097079) exhibiting
sharper gradients in H{\sc i} intensity on the side of the tails, are
consistent with the H{\sc i} gas being affected by the ram pressure of the
intracluster medium. However the H{\sc i} emission in all the three galaxies
extends to much smaller distances than the radio-continuum and H$\alpha$ tails,
and are possibly still bound to the parent galaxies. Approximately 20$-$30 per
cent of the H{\sc i} mass is seen to accumulate on the downstream side due to
the effects of ram pressure.
|
astro-ph
|
we present the results on the distribution and kinematics of hsci gas with higher sensitivity and in one case of higher spectral resolution as well than reported earlier of three irregular galaxies cgcg 097073 097079 and 097087 ugc 06697 in the cluster abell 1367 these galaxies are known to exhibit long 5075 kpc tails of radio continuum and optical emission lines halpha pointing away from the cluster centre and arcs of starformation on the opposite sides of the tails these features as well as the hsc i properties with two of the galaxies cgcg 097073 and 097079 exhibiting sharper gradients in hsc i intensity on the side of the tails are consistent with the hsc i gas being affected by the ram pressure of the intracluster medium however the hsc i emission in all the three galaxies extends to much smaller distances than the radiocontinuum and halpha tails and are possibly still bound to the parent galaxies approximately 2030 per cent of the hsc i mass is seen to accumulate on the downstream side due to the effects of ram pressure
|
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|
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|
706.3198
|
Overspinning a nearly extreme charged black hole via a quantum tunneling
process
|
We examine a nearly extreme macroscopic Reissner-Nordstrom black hole in the
context of semi-classical gravity. The absorption rate associated with the
quantum tunneling process of scalar particles whereby this black hole can
acquire enough angular momentum to violate the weak cosmic censorship
conjecture is shown to be nonzero.
|
gr-qc hep-th
|
we examine a nearly extreme macroscopic reissnernordstrom black hole in the context of semiclassical gravity the absorption rate associated with the quantum tunneling process of scalar particles whereby this black hole can acquire enough angular momentum to violate the weak cosmic censorship conjecture is shown to be nonzero
|
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|
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|
706.3199
|
Scattering of twist fields from D-branes and orientifolds
|
We compute the two-point function for Z_N orbifold twist fields on the disk
and RP2. We apply this to a computation of the O(g_s) correction to the Kahler
potential for (the symmetric combination of) blow-up modes in type I string
theory on T^6/Z_3. This is related by supersymmetry to the one-loop field
dependent correction to the Fayet-Iliopoulos D-term for the anomalous U(1)
factor. We find this correction to be non-vanishing away from the orbifold
point.
|
hep-th
|
we compute the twopoint function for z_n orbifold twist fields on the disk and rp2 we apply this to a computation of the og_s correction to the kahler potential for the symmetric combination of blowup modes in type i string theory on t6z_3 this is related by supersymmetry to the oneloop field dependent correction to the fayetiliopoulos dterm for the anomalous u1 factor we find this correction to be nonvanishing away from the orbifold point
|
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|
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|
706.32
|
Vortex generation in protoplanetary disks with an embedded giant planet
|
Vortices in protoplanetary disks can capture solid particles and form
planetary cores within shorter timescales than those involved in the standard
core-accretion model. We investigate vortex generation in thin unmagnetized
protoplanetary disks with an embedded giant planet with planet to star mass
ratio $10^{-4}$ and $10^{-3}$. Two-dimensional hydrodynamical simulations of a
protoplanetary disk with a planet are performed using two different numerical
methods. The results of the non-linear simulations are compared with a
time-resolved modal analysis of the azimuthally averaged surface density
profiles using linear perturbation theory. Finite-difference methods
implemented in polar coordinates generate vortices moving along the gap created
by Neptune-mass to Jupiter-mass planets. The modal analysis shows that unstable
modes are generated with growth rate of order $0.3 \Omega_K$ for azimuthal
numbers m=4,5,6, where $\Omega_K$ is the local Keplerian frequency.
Shock-capturing Cartesian-grid codes do not generate very much vorticity around
a giant planet in a standard protoplanetary disk. Modal calculations confirm
that the obtained radial profiles of density are less susceptible to the growth
of linear modes on timescales of several hundreds of orbital periods.
Navier-Stokes viscosity of the order $\nu=10^{-5}$ (in units of $a^2 \Omega_p$)
is found to have a stabilizing effect and prevents the formation of vortices.
This result holds at high resolution runs and using different types of boundary
conditions. Giant protoplanets of Neptune-mass to Jupiter-mass can excite the
Rossby wave instability and generate vortices in thin disks. The presence of
vortices in protoplanetary disks has implications for planet formation, orbital
migration, and angular momentum transport in disks.
|
astro-ph
|
vortices in protoplanetary disks can capture solid particles and form planetary cores within shorter timescales than those involved in the standard coreaccretion model we investigate vortex generation in thin unmagnetized protoplanetary disks with an embedded giant planet with planet to star mass ratio 104 and 103 twodimensional hydrodynamical simulations of a protoplanetary disk with a planet are performed using two different numerical methods the results of the nonlinear simulations are compared with a timeresolved modal analysis of the azimuthally averaged surface density profiles using linear perturbation theory finitedifference methods implemented in polar coordinates generate vortices moving along the gap created by neptunemass to jupitermass planets the modal analysis shows that unstable modes are generated with growth rate of order 03 omega_k for azimuthal numbers m456 where omega_k is the local keplerian frequency shockcapturing cartesiangrid codes do not generate very much vorticity around a giant planet in a standard protoplanetary disk modal calculations confirm that the obtained radial profiles of density are less susceptible to the growth of linear modes on timescales of several hundreds of orbital periods navierstokes viscosity of the order nu105 in units of a2 omega_p is found to have a stabilizing effect and prevents the formation of vortices this result holds at high resolution runs and using different types of boundary conditions giant protoplanets of neptunemass to jupitermass can excite the rossby wave instability and generate vortices in thin disks the presence of vortices in protoplanetary disks has implications for planet formation orbital migration and angular momentum transport in disks
|
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|
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|
706.3201
|
Volume Weighted Measures of Eternal Inflation in the Bousso-Polchinski
Landscape
|
We consider the cosmological dynamics associated with volume weighted
measures of eternal inflation, in the Bousso-Polchinski model of the string
theory landscape. We find that this measure predicts that observers are most
likely to find themselves in low energy vacua with one flux considerably larger
than the rest. Furthermore, it allows for a satisfactory anthropic explanation
of the cosmological constant problem by producing a smooth, and approximately
constant, distribution of potentially observable values of Lambda. The low
energy vacua selected by this measure are often short lived. If we require
anthropically acceptable vacua to have a minimum life-time of 10 billion years,
then for reasonable parameters a typical observer should expect their vacuum to
have a life-time of approximately 12 billion years. This prediction is model
dependent, but may point toward a solution to the coincidence problem of
cosmology.
|
hep-th astro-ph gr-qc
|
we consider the cosmological dynamics associated with volume weighted measures of eternal inflation in the boussopolchinski model of the string theory landscape we find that this measure predicts that observers are most likely to find themselves in low energy vacua with one flux considerably larger than the rest furthermore it allows for a satisfactory anthropic explanation of the cosmological constant problem by producing a smooth and approximately constant distribution of potentially observable values of lambda the low energy vacua selected by this measure are often short lived if we require anthropically acceptable vacua to have a minimum lifetime of 10 billion years then for reasonable parameters a typical observer should expect their vacuum to have a lifetime of approximately 12 billion years this prediction is model dependent but may point toward a solution to the coincidence problem of cosmology
|
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|
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|
706.3202
|
Source Matching in the SDSS and RASS: Which Galaxies are Really X-ray
Sources?
|
The current view of galaxy formation holds that all massive galaxies harbor a
massive black hole at their center, but that these black holes are not always
in an actively accreting phase. X-ray emission is often used to identify
accreting sources, but for galaxies that are not harboring quasars
(low-luminosity active galaxies), the X-ray flux may be weak, or obscured by
dust. To aid in the understanding of weakly accreting black holes in the local
universe, a large sample of galaxies with X-ray detections is needed. We
cross-match the ROSAT All Sky Survey (RASS) with galaxies from the Sloan
Digital Sky Survey Data Release 4 (SDSS DR4) to create such a sample. Because
of the high SDSS source density and large RASS positional errors, the
cross-matched catalog is highly contaminated by random associations. We
investigate the overlap of these surveys and provide a statistical test of the
validity of RASS-SDSS galaxy cross-matches. SDSS quasars provide a test of our
cross-match validation scheme, as they have a very high fraction of true RASS
matches. We find that the number of true matches between the SDSS main galaxy
sample and the RASS is highly dependent on the optical spectral classification
of the galaxy; essentially no star-forming galaxies are detected, while more
than 0.6% of narrow-line Seyferts are detected in the RASS. Also, galaxies with
ambiguous optical classification have a surprisingly high RASS detection
fraction. This allows us to further constrain the SEDs of low-luminosity active
galaxies. Our technique is quite general, and can be applied to any
cross-matching between surveys with well-understood positional errors.
|
astro-ph
|
the current view of galaxy formation holds that all massive galaxies harbor a massive black hole at their center but that these black holes are not always in an actively accreting phase xray emission is often used to identify accreting sources but for galaxies that are not harboring quasars lowluminosity active galaxies the xray flux may be weak or obscured by dust to aid in the understanding of weakly accreting black holes in the local universe a large sample of galaxies with xray detections is needed we crossmatch the rosat all sky survey rass with galaxies from the sloan digital sky survey data release 4 sdss dr4 to create such a sample because of the high sdss source density and large rass positional errors the crossmatched catalog is highly contaminated by random associations we investigate the overlap of these surveys and provide a statistical test of the validity of rasssdss galaxy crossmatches sdss quasars provide a test of our crossmatch validation scheme as they have a very high fraction of true rass matches we find that the number of true matches between the sdss main galaxy sample and the rass is highly dependent on the optical spectral classification of the galaxy essentially no starforming galaxies are detected while more than 06 of narrowline seyferts are detected in the rass also galaxies with ambiguous optical classification have a surprisingly high rass detection fraction this allows us to further constrain the seds of lowluminosity active galaxies our technique is quite general and can be applied to any crossmatching between surveys with wellunderstood positional errors
|
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|
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|
706.3203
|
Detecting Axion-Like Particles With Gamma Ray Telescopes
|
We propose that axion-like particles (ALPs) with a two-photon vertex,
consistent with all astrophysical and laboratory bounds, may lead to a
detectable signature in the spectra of high-energy gamma ray sources. This
occurs as a result of gamma rays being converted into ALPs in the magnetic
fields of efficient astrophysical accelerators according to the "Hillas
criterion", such as jets of active galactic nuclei or hot spots of radio
galaxies. The discovery of such an effect is possible by GLAST in the 1-100 GeV
range and by ground based gamma ray telescopes in the TeV range.
|
hep-ph astro-ph
|
we propose that axionlike particles alps with a twophoton vertex consistent with all astrophysical and laboratory bounds may lead to a detectable signature in the spectra of highenergy gamma ray sources this occurs as a result of gamma rays being converted into alps in the magnetic fields of efficient astrophysical accelerators according to the hillas criterion such as jets of active galactic nuclei or hot spots of radio galaxies the discovery of such an effect is possible by glast in the 1100 gev range and by ground based gamma ray telescopes in the tev range
|
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|
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|
706.3204
|
Optimal purifications and fidelity for displaced thermal states
|
We evaluate the Uhlmann fidelity between two one-mode displaced thermal
states as the maximal probability transition between appropriate purifications
of the given states. The optimal purifications defining the fidelity are proved
to be two-mode displaced Gaussian states.
|
quant-ph
|
we evaluate the uhlmann fidelity between two onemode displaced thermal states as the maximal probability transition between appropriate purifications of the given states the optimal purifications defining the fidelity are proved to be twomode displaced gaussian states
|
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|
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|
706.3205
|
Exact Solutions of the Isothermal Lane--Emden Equation with Rotation and
Implications for the Formation of Planets and Satellites
|
We have derived exact solutions of the isothermal Lane--Emden equation with
and without rotation in a cylindrical geometry. The corresponding hydrostatic
equilibria are most relevant to the dynamics of the protosolar nebula before
and during the stages of planet and satellite formation. The nonrotating
solution for the mass density is analytic, nonsingular, monotonically
decreasing with radius, and it satisfies easily the usual physical boundary
conditions at the center. When differential rotation is added to the
Lane--Emden equation, an entire class of exact solutions for the mass density
appears. We have determined all of these solutions analytically as well. Within
this class, solutions that are power laws or combinations of power laws are not
capable of satisfying the associated boundary--value problem, but they are
nonetheless of profound importance because they constitute "baselines" to which
the actual solutions approach when the central boundary conditions are imposed.
Numerical integrations that enforce such physical boundary conditions show that
the actual radial equilibrium density profiles emerge from the center close to
the nonrotating solution, but once they cross below the corresponding
baselines, they cease to be monotonic. The actual solutions are forced to
oscillate permanently about the baseline solutions without ever settling onto
them because the central boundary conditions strictly prohibit such settling,
even in the asymptotic regime of large radii. Based on our results, we expect
that quasistatically--evolving protoplanetary disks should develop oscillatory
density profiles in their midplanes during their isothermal phase. The peaks in
these profiles correspond to local potential minima and their locations are
ideal sites for the formation of protoplanets ...
|
astro-ph
|
we have derived exact solutions of the isothermal laneemden equation with and without rotation in a cylindrical geometry the corresponding hydrostatic equilibria are most relevant to the dynamics of the protosolar nebula before and during the stages of planet and satellite formation the nonrotating solution for the mass density is analytic nonsingular monotonically decreasing with radius and it satisfies easily the usual physical boundary conditions at the center when differential rotation is added to the laneemden equation an entire class of exact solutions for the mass density appears we have determined all of these solutions analytically as well within this class solutions that are power laws or combinations of power laws are not capable of satisfying the associated boundaryvalue problem but they are nonetheless of profound importance because they constitute baselines to which the actual solutions approach when the central boundary conditions are imposed numerical integrations that enforce such physical boundary conditions show that the actual radial equilibrium density profiles emerge from the center close to the nonrotating solution but once they cross below the corresponding baselines they cease to be monotonic the actual solutions are forced to oscillate permanently about the baseline solutions without ever settling onto them because the central boundary conditions strictly prohibit such settling even in the asymptotic regime of large radii based on our results we expect that quasistaticallyevolving protoplanetary disks should develop oscillatory density profiles in their midplanes during their isothermal phase the peaks in these profiles correspond to local potential minima and their locations are ideal sites for the formation of protoplanets
|
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|
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|
706.3206
|
A Spectroscopic Study of Mass Outflows in the Interacting Binary RY
Scuti
|
The massive interacting binary RY Scuti is an important representative of an
active mass-transferring system that is changing before our eyes and which may
be an example of the formation of a Wolf-Rayet star through tidal stripping.
Utilizing new and previously published spectra, we present examples of how a
number of illustrative absorption and emission features vary during the binary
orbit. We identify spectral features associated with each component, calculate
a new, double-lined spectroscopic binary orbit, and find masses of 7.1 +/- 1.2
M_sun for the bright supergiant and 30.0 +/- 2.1 M_sun for the hidden massive
companion. Through tomographic reconstruction of the component spectra from the
composite spectra, we confirm the O9.7 Ibpe spectral class of the bright
supergiant and discover a B0.5 I spectrum associated with the hidden massive
companion; however, we suggest that the latter is actually the spectrum of the
photosphere of the accretion torus immediately surrounding the massive
companion. We describe the complex nature of the mass loss flows from the
system in the context of recent hydrodynamical models for beta Lyr, leading us
to conclude RY Scuti has matter leaving the system in two ways: 1) a bipolar
outflow from winds generated by the hidden massive companion, and 2) mass from
the bright O9.7 Ibpe supergiant flowing from the region near the L2 point to
fill out a large, dense circumbinary disk. This circumbinary disk (radius ~ 1
AU) may feed the surrounding double-toroidal nebula (radius ~ 2000 AU).
|
astro-ph
|
the massive interacting binary ry scuti is an important representative of an active masstransferring system that is changing before our eyes and which may be an example of the formation of a wolfrayet star through tidal stripping utilizing new and previously published spectra we present examples of how a number of illustrative absorption and emission features vary during the binary orbit we identify spectral features associated with each component calculate a new doublelined spectroscopic binary orbit and find masses of 71 12 m_sun for the bright supergiant and 300 21 m_sun for the hidden massive companion through tomographic reconstruction of the component spectra from the composite spectra we confirm the o97 ibpe spectral class of the bright supergiant and discover a b05 i spectrum associated with the hidden massive companion however we suggest that the latter is actually the spectrum of the photosphere of the accretion torus immediately surrounding the massive companion we describe the complex nature of the mass loss flows from the system in the context of recent hydrodynamical models for beta lyr leading us to conclude ry scuti has matter leaving the system in two ways 1 a bipolar outflow from winds generated by the hidden massive companion and 2 mass from the bright o97 ibpe supergiant flowing from the region near the l2 point to fill out a large dense circumbinary disk this circumbinary disk radius 1 au may feed the surrounding doubletoroidal nebula radius 2000 au
|
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|
[-0.09882100860533469, 0.09810179603615524, -0.04444201655114586, 0.05768878736920623, -0.1108417311612861, -0.09979456616369929, 0.03503832148931952, 0.3673974575510076, -0.20679801751804702, -0.32512863114194457, 0.08232227338775366, -0.307884837647493, -0.08163560691931356, 0.1679338601363056, -0.048746113848462586, -0.032683598836336064, 0.12025326558294855, -0.02054174218479419, -0.06786666578342238, -0.209452000084654, 0.3450867938456916, 0.04617175869761082, 0.06104220946890717, -0.05748340382315062, 0.026539041865675735, -0.06898119979823682, -0.04213484169664879, -0.09271576418737028, -0.13714365475692936, 0.04864800760146825, 0.16585464734152, 0.13692773219996265, 0.21241364342223132, -0.33154275348633055, -0.23658652208792438, 0.0326437979570723, 0.21850679220657154, 0.016433038627004893, -0.07665194587551151, -0.2729036680284786, 0.09636248941137064, -0.24763577325199143, -0.1958519053907611, 0.04625408038567407, 0.061597472262674424, 0.017287361045747587, -0.2531474855720621, 0.10658269752591785, 0.055660584142740756, 0.0640673066113739, -0.11730359845008201, -0.08607762438115985, -0.07382162586402367, 0.07955906297150656, 0.043359153270584476, 0.05802917584557744, 0.1559469651610849, -0.13276970818317926, -0.025344153034633825, 0.36951493777866873, -0.06984666233858829, -0.014461527821146139, 0.26902382808665065, -0.19397472883692057, -0.16299825830252043, 0.19979104500639588, 0.16228092069729788, 0.16325914075900408, -0.16056143542059048, -0.012057634618107872, -0.047771409308506534, 0.2184016395106123, 0.0399896551007718, 0.04568497781219164, 0.3796950984088814, 0.1345881685583281, -0.019892168507183425, 0.1450784324067684, -0.24105787952088148, -0.04885461188837135, -0.2331840737229761, -0.12358253883851394, -0.13729144968464188, 0.08407443233945665, -0.13094303649689995, -0.12590951388193092, 0.3690838795507468, 0.09950985010818993, 0.23671204457842127, -0.040609383403481095, 0.28847919300809, 0.08552442039822877, 0.09047576723023361, 0.15065832845788418, 0.31641628456247206, 0.19076264375809016, 0.1062127258178598, -0.2420784333307969, -0.005765308396589449, 0.016629466110010857]
|
706.3207
|
Mirror symmetry and T-duality in the complement of an anticanonical
divisor
|
We study the geometry of complexified moduli spaces of special Lagrangian
submanifolds in the complement of an anticanonical divisor in a compact Kahler
manifold. In particular, we explore the connections between T-duality and
mirror symmetry in concrete examples, and show how quantum corrections arise in
this context.
|
math.SG math.AG math.DG
|
we study the geometry of complexified moduli spaces of special lagrangian submanifolds in the complement of an anticanonical divisor in a compact kahler manifold in particular we explore the connections between tduality and mirror symmetry in concrete examples and show how quantum corrections arise in this context
|
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|
[-0.216124245025059, 0.05892764819826822, -0.05844275316500917, 0.15179455763551386, -0.12246879709369325, -0.12049130285951368, -0.026093945387711235, 0.37040859730319775, -0.26869406878076335, -0.19789712535257034, 0.059690264288950315, -0.23688391065522235, -0.274955652337125, 0.1592606415456914, -0.22938254441907432, -0.018990897910392032, 0.034676592638517946, 0.016365056897097444, -0.1838877374662998, -0.26147061921259823, 0.5060320334865692, -0.024426442504107478, 0.21356414020695585, 0.09479766246906675, 0.09492194775412692, -0.01790523101536042, 0.015482261955262498, -0.018948661464395278, -0.15903532526832312, 0.13896341728878783, 0.30235944548621774, 0.051423690975346464, 0.1293226094876832, -0.45706896135147584, -0.17038435942711347, 0.20012802258133888, 0.10741401214073314, 0.06755940188118752, -0.03419735904862272, -0.3020167294493381, 0.002912651876265064, -0.11790800062899894, -0.22689025332789592, -0.14131362037237813, -0.0053924714076392195, -0.02351577895534958, -0.10777975539577768, -0.07727252000427627, 0.061279490391941784, 0.12273653146830645, -0.026386059345083035, -0.01674369613620195, -0.08692951787738724, 0.033723128850551995, 0.09285888147163898, 0.03406164795655678, 0.09988627313547074, -0.1501104897829367, -0.11833887593820691, 0.3926821729128665, -0.08276785678289672, -0.29676682723963516, 0.08127808364781927, -0.11613003291348194, -0.22725064279709725, 0.0635133398860257, 0.19462493236394637, 0.2080710979743286, -0.02092096114412267, 0.251029913529179, -0.06387648391636445, 0.02956928143357026, 0.09866943355015617, 0.029293822156800393, 0.1493372729994317, 0.12440932305787314, 0.08054416818900946, 0.18009217425269333, -0.019142239929196683, -0.14661539948738597, -0.4652355861790637, -0.2506453524680531, -0.09471869353759796, 0.1457339009230441, -0.16403587005891282, -0.13594211415050828, 0.39504150489464085, 0.04022862076600815, 0.24930181551447256, 0.044503445697433135, 0.20038096539359143, -0.029715364407549832, 0.01864390162394402, 0.03552612230340217, 0.25756912308923424, 0.22868981899971025, -0.010939499452472367, -0.19153875916046983, -0.1834214633191995, 0.15049808121662825]
|
706.3208
|
The chiral condensate in a constant electromagnetic field
|
We study the shift of the chiral condensate in a constant electromagnetic
field in the context of chiral perturbation theory. Using the Schwinger
proper-time formalism, we derive a one-loop expression correct to all orders in
$m_{\pi}^2 / eH$. Our result correctly reproduces a previously derived
``low-energy theorem'' for $m_\pi = 0$. We show that it is essential to include
corrections due to non-vanishing $m_\pi$ in order for a low energy theorem to
have any approximate regime of validity in the physical universe. We generalize
these results to systems containing electric fields, and discuss the regime of
validity for the results. In particular, we discuss the circumstances in which
the method formally breaks down due to pair creation in an electric field.
|
hep-ph
|
we study the shift of the chiral condensate in a constant electromagnetic field in the context of chiral perturbation theory using the schwinger propertime formalism we derive a oneloop expression correct to all orders in m_pi2 eh our result correctly reproduces a previously derived lowenergy theorem for m_pi 0 we show that it is essential to include corrections due to nonvanishing m_pi in order for a low energy theorem to have any approximate regime of validity in the physical universe we generalize these results to systems containing electric fields and discuss the regime of validity for the results in particular we discuss the circumstances in which the method formally breaks down due to pair creation in an electric field
|
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|
[-0.13884280379978986, 0.1306354251716867, -0.09530998134453382, 0.11135487727226079, -0.034498315889529195, -0.061524220836200134, 0.04421525217980115, 0.3325267667185609, -0.17537862156956074, -0.27848066088250456, 0.01192693751962746, -0.24207585084275537, -0.1263256994263903, 0.17101174345075645, -0.01113235646811854, 0.01463921254641619, -0.026403107654945066, 0.06418649470355331, -0.058213560840021036, -0.21111478263653127, 0.32521734125677404, 0.00199105022396861, 0.2688934216432336, 0.13757713531347446, 0.0733893562358718, 0.0340431892731767, 0.02454811055995837, -0.0090566819314571, -0.15899813203210797, 0.04847192186314393, 0.22725684587655887, 0.02659692253502665, 0.2085631939292956, -0.39131013286777405, -0.19459514001466552, 0.08509393547810301, 0.13105484655424327, 0.20466725734950772, -0.014071701477993937, -0.25268874018445237, 0.13104003263801775, -0.19745977819083305, -0.22177894452602423, -0.14420057640669226, 0.011854411883498816, -0.032466930992697846, -0.30137116111376705, 0.1050224457554394, 0.05426659451958042, 0.0010506919968654128, -0.09104383781849712, -0.07733457444329597, 0.03504739833815696, 0.10142355659945297, 0.10182488542010992, 0.054686174847326484, 0.10687921123438272, -0.16486778327052584, -0.10216834188728523, 0.4023920423468622, -0.11553212424873241, -0.16335828247002693, 0.12719960236225372, -0.16667499200405725, -0.15360005260171258, 0.11329154875872954, 0.14460779037796148, 0.11390116715318516, -0.15470489195915832, 0.16095553979276633, -0.008279698603481305, 0.12327824352786508, 0.09849590376144697, 0.04969483705926217, 0.1927762596687975, 0.09366080820356973, 0.005032128750291818, 0.12767900047166383, -0.041834462946672146, -0.11289685188221331, -0.3766442364504357, -0.13751174073191014, -0.16054730066939593, 0.060507818626067716, -0.0799709244348997, -0.1545810323353356, 0.37369514953251143, 0.23591458885891348, 0.18016333125253842, 0.04699239933749802, 0.281913515462094, 0.1665929659483015, 0.08255076284144669, 0.05826235882069195, 0.2752091418443044, 0.20309297981214153, 0.10035913067032434, -0.24403764883901516, -0.07189565060362846, 0.09496008098407202]
|
706.3209
|
GRB060218 and GRBs associated with Supernovae Ib/c
|
We plan to fit the complete gamma- and X-ray light curves of the long
duration GRB060218, including the prompt emission, in order to clarify the
nature of the progenitors and the astrophysical scenario of the class of GRBs
associated to SNe Ib/c. The initial total energy of the electron-positron
plasma E_{e^\pm}^{tot}=2.32\times 10^{50} erg has a particularly low value
similarly to the other GRBs associated with SNe. For the first time we observe
a baryon loading B=10^{-2} which coincides with the upper limit for the
dynamical stability of the fireshell. The effective CircumBurst Medium (CBM)
density shows a radial dependence n_{cbm} \propto r^{-\alpha} with
1.0<\alpha<1.7 and monotonically decreases from 1 to 10^{-6} particles/cm^3.
Such a behavior is interpreted as due to a fragmentation in the fireshell.
Analogies with the fragmented density and filling factor characterizing Novae
are outlined. The fit presented is particularly significant in view of the
complete data set available for GRB060218 and of the fact that it fulfills the
Amati relation. We fit GRB060218, usually considered as an X-Ray Flash (XRF),
as a "canonical GRB" within our theoretical model. The smallest possible black
hole, formed by the gravitational collapse of a neutron star in a binary
system, is consistent with the especially low energetics of the class of GRBs
associated with SNe Ib/c. We give the first evidence for a fragmentation in the
fireshell. Such a fragmentation is crucial in explaining both the unusually
large T_{90} and the consequently inferred abnormal low value of the CBM
effective density.
|
astro-ph
|
we plan to fit the complete gamma and xray light curves of the long duration grb060218 including the prompt emission in order to clarify the nature of the progenitors and the astrophysical scenario of the class of grbs associated to sne ibc the initial total energy of the electronpositron plasma e_epmtot232times 1050 erg has a particularly low value similarly to the other grbs associated with sne for the first time we observe a baryon loading b102 which coincides with the upper limit for the dynamical stability of the fireshell the effective circumburst medium cbm density shows a radial dependence n_cbm propto ralpha with 10alpha17 and monotonically decreases from 1 to 106 particlescm3 such a behavior is interpreted as due to a fragmentation in the fireshell analogies with the fragmented density and filling factor characterizing novae are outlined the fit presented is particularly significant in view of the complete data set available for grb060218 and of the fact that it fulfills the amati relation we fit grb060218 usually considered as an xray flash xrf as a canonical grb within our theoretical model the smallest possible black hole formed by the gravitational collapse of a neutron star in a binary system is consistent with the especially low energetics of the class of grbs associated with sne ibc we give the first evidence for a fragmentation in the fireshell such a fragmentation is crucial in explaining both the unusually large t_90 and the consequently inferred abnormal low value of the cbm effective density
|
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|
[-0.0843622751075865, 0.1429514626615708, -0.06082417137981185, 0.16787231212334805, -0.07649185241912661, -0.07216012420044149, 0.05960091233709714, 0.3657742523011348, -0.1860820822038797, -0.3071116983974428, 0.048636127554581535, -0.30968979136596025, -0.02850958676292346, 0.19866997264005123, -0.009323920408897252, 0.01437880787508268, 0.05782105255002903, -0.005656127411653457, -0.09436986881222478, -0.19839592647610557, 0.3012440018921427, 0.10912050181992261, 0.22796636430849698, 0.02323837636739981, 0.0659177738527823, -0.04334770107683292, -0.03222462347885858, -0.007192475218344706, -0.14915692553838863, 0.040241018944393525, 0.22377835332815674, 0.12997939310466441, 0.20822126573109095, -0.3767176518887885, -0.24727823455376843, 0.11085008642018107, 0.12600344646889866, 0.03553374243008448, -0.046697041317669725, -0.2270264532610299, 0.0619714520371454, -0.22710079504252384, -0.17767833065213767, 0.04623173762335318, 0.06900909015162271, 0.06599345524146821, -0.2404697616153344, 0.14013081903664606, 0.022194929904401535, -0.012465101976993, -0.10661392230050344, -0.049334207698627404, -0.02876799850939558, 0.031719683190649335, 0.0890263954888245, 0.06947017574460371, 0.10000926137407902, -0.16957524573092955, -0.02969299673445915, 0.444139366743234, -0.0561773801422282, -0.013737855876912834, 0.18560608766731704, -0.1732353875470095, -0.14343899044845448, 0.16155011890840676, 0.12584409332949187, 0.08018197780116819, -0.12269271296205805, 0.004966927549367213, -0.013150338516646038, 0.16209616221728837, 0.020578942305940064, 0.06370196934140887, 0.25307601023472936, 0.1965861277738897, -0.0051366643761454325, 0.10762988235909861, -0.15405847381155652, -0.021620553120949987, -0.3500402260134336, -0.11760989978517357, -0.15850126794218897, 0.11533236439124896, -0.12081522570306959, -0.15585951898708894, 0.36784869325271835, 0.07813495380694598, 0.24720166136533295, 0.04552573473654642, 0.2516908570360543, 0.1244145515639366, 0.053680209422235184, 0.11621011005948309, 0.29245778518966453, 0.1494532852567476, 0.10655690249228127, -0.25568319102683246, 0.09706062432058035, 0.010030925830049433]
|
706.321
|
Self-interaction correction with Wannier functions
|
We describe the behavior of the Perdew-Zunger self-interaction-corrected
local density approximation (SIC-LDA) functional when implemented in a
plane-wave pseudopotential formalism with Wannier functions. Prototypical
semiconductors and wide-bandgap oxides show a large overcorrection of the LDA
bandgap. Application to transition-metal oxides and elements with d electrons
is hindered by a serious breaking of the spherical symmetry, which appears even
in a closed shell free atom. Our results indicate that, when all spherical
approximations are lifted, the general applicability of orbital-dependent
potentials is very limited and should be reconsidered in favor of rotationally
invariant functionals.
|
cond-mat.other
|
we describe the behavior of the perdewzunger selfinteractioncorrected local density approximation siclda functional when implemented in a planewave pseudopotential formalism with wannier functions prototypical semiconductors and widebandgap oxides show a large overcorrection of the lda bandgap application to transitionmetal oxides and elements with d electrons is hindered by a serious breaking of the spherical symmetry which appears even in a closed shell free atom our results indicate that when all spherical approximations are lifted the general applicability of orbitaldependent potentials is very limited and should be reconsidered in favor of rotationally invariant functionals
|
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|
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|
706.3211
|
Path probability density functions for semi-Markovian random walks
|
In random walks, the path representation of the Green's function is an
infinite sum over the length of path probability density functions (PDFs). Here
we derive and solve, in Laplace space, the recursion relation for the n order
path PDF for any arbitrarily inhomogeneous semi-Markovian random walk in a
one-dimensional (1D) chain of L states. The recursion relation relates the n
order path PDF to L/2 (round towards zero for an odd L) shorter path PDFs, and
has n independent coefficients that obey a universal formula. The z transform
of the recursion relation straightforwardly gives the generating function for
path PDFs, from which we obtain the Green's function of the random walk, and
derive an explicit expression for any path PDF of the random walk. These
expressions give the most detailed description of arbitrarily inhomogeneous
semi-Markovian random walks in 1D.
|
math-ph math.MP physics.bio-ph q-bio.OT
|
in random walks the path representation of the greens function is an infinite sum over the length of path probability density functions pdfs here we derive and solve in laplace space the recursion relation for the n order path pdf for any arbitrarily inhomogeneous semimarkovian random walk in a onedimensional 1d chain of l states the recursion relation relates the n order path pdf to l2 round towards zero for an odd l shorter path pdfs and has n independent coefficients that obey a universal formula the z transform of the recursion relation straightforwardly gives the generating function for path pdfs from which we obtain the greens function of the random walk and derive an explicit expression for any path pdf of the random walk these expressions give the most detailed description of arbitrarily inhomogeneous semimarkovian random walks in 1d
|
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|
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|
706.3212
|
Linear Stability of Closed Timelike Geodesics
|
The linear stability of closed timelike geodesics (CTGs) is analyzed in two
spacetimes with cylindrical sources, an infinite rotating dust cylinder, and a
cylindrical cloud of static cosmic strings with a central spinning string. We
also study the existence and linear stability of closed timelike curves in
spacetimes that share some common features with the G\"odel universe
(G\"odel-type spacetimes). In this case the existence of CTGs depends on the
`background' metric. The CTGs in a subclass of inhomogeneous stationary
cosmological solutions of the Einstein-Maxwell equations with topology $
S^3\times \mathbb R$ are also examined.
|
gr-qc
|
the linear stability of closed timelike geodesics ctgs is analyzed in two spacetimes with cylindrical sources an infinite rotating dust cylinder and a cylindrical cloud of static cosmic strings with a central spinning string we also study the existence and linear stability of closed timelike curves in spacetimes that share some common features with the godel universe godeltype spacetimes in this case the existence of ctgs depends on the background metric the ctgs in a subclass of inhomogeneous stationary cosmological solutions of the einsteinmaxwell equations with topology s3times mathbb r are also examined
|
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|
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|
706.3213
|
A Spitzer IRAC Census of the Asymptotic Giant Branch Populations in
Local Group Dwarfs. II. IC 1613
|
We present Spitzer Space Telescope IRAC photometry of the Local Group dwarf
irregular galaxy IC 1613. We compare our 3.6, 4.5, 5.8, and 8.0 micron
photometry with broadband optical photometry and find that the optical data do
not detect 43% and misidentify an additional 11% of the total AGB population,
likely because of extinction caused by circumstellar material. Further, we find
that a narrowband optical carbon star study of IC 1613 detects 50% of the total
AGB population and only considers 18% of this population in calculating the
carbon to M-type AGB ratio. We derive an integrated mass-loss rate from the AGB
stars of 0.2-1.0 x 10^(-3) solar masses per year and find that the distribution
of bolometric luminosities and mass-loss rates are consistent with those for
other nearby metal-poor galaxies. Both the optical completeness fractions and
mass-loss rates in IC 1613 are very similar to those in the Local Group dwarf
irregular, WLM, which is expected given their similar characteristics and
evolutionary histories.
|
astro-ph
|
we present spitzer space telescope irac photometry of the local group dwarf irregular galaxy ic 1613 we compare our 36 45 58 and 80 micron photometry with broadband optical photometry and find that the optical data do not detect 43 and misidentify an additional 11 of the total agb population likely because of extinction caused by circumstellar material further we find that a narrowband optical carbon star study of ic 1613 detects 50 of the total agb population and only considers 18 of this population in calculating the carbon to mtype agb ratio we derive an integrated massloss rate from the agb stars of 0210 x 103 solar masses per year and find that the distribution of bolometric luminosities and massloss rates are consistent with those for other nearby metalpoor galaxies both the optical completeness fractions and massloss rates in ic 1613 are very similar to those in the local group dwarf irregular wlm which is expected given their similar characteristics and evolutionary histories
|
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|
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|
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