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706.4414
|
Decay modes of $^{10}$C nuclei unbound state
|
Unbound states of $^{10}$C nuclei produced as quasi-projectiles in
$^{12}$C+$^{24}$Mg collisions at E/A = 53 and 95 MeV are studied with the Indra
detector array. Multi-particle correlation function analyses provide
experimental evidence of sequential de-excitation mechanisms through the
production of intermediate $^{9}$B, $^{6}$Be and $^{8}$Be unbound nuclei. The
relative contributions of different decay sequences to the total decay width of
the explored states is estimated semi-quantitatively. The obtained results show
that heavy-ion collisions can be used as a tool to access spectroscopic
information about exotic nuclei.
|
nucl-ex
|
unbound states of 10c nuclei produced as quasiprojectiles in 12c24mg collisions at ea 53 and 95 mev are studied with the indra detector array multiparticle correlation function analyses provide experimental evidence of sequential deexcitation mechanisms through the production of intermediate 9b 6be and 8be unbound nuclei the relative contributions of different decay sequences to the total decay width of the explored states is estimated semiquantitatively the obtained results show that heavyion collisions can be used as a tool to access spectroscopic information about exotic nuclei
|
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|
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|
706.4415
|
Labyrinthine pathways towards supercycle attractors in unimodal maps
|
We uncover previously unknown properties of the family of periodic
superstable cycles in unimodal maps characterized each by a Lyapunov exponent
that diverges to minus infinity. Amongst the main novel properties are the
following: i) The basins of attraction for the phases of the cycles develop
fractal boundaries of increasing complexity as the period-doubling structure
advances towards the transition to chaos. ii) The fractal boundaries, formed by
the preimages of the repellor, display hierarchical structures organized
according to exponential clusterings that manifest in the dynamics as
sensitivity to the final state and transient chaos. iii) There is a functional
composition renormalization group (RG) fixed-point map associated to the family
of supercycles. iv) This map is given in closed form by the same kind of
$q$-exponential function found for both the pitchfork and tangent bifurcation
attractors. v) There is a final stage ultra-fast dynamics towards the attractor
with a sensitivity to initial conditions that decreases as an exponential of an
exponential of time.
|
cond-mat.stat-mech nlin.CD
|
we uncover previously unknown properties of the family of periodic superstable cycles in unimodal maps characterized each by a lyapunov exponent that diverges to minus infinity amongst the main novel properties are the following i the basins of attraction for the phases of the cycles develop fractal boundaries of increasing complexity as the perioddoubling structure advances towards the transition to chaos ii the fractal boundaries formed by the preimages of the repellor display hierarchical structures organized according to exponential clusterings that manifest in the dynamics as sensitivity to the final state and transient chaos iii there is a functional composition renormalization group rg fixedpoint map associated to the family of supercycles iv this map is given in closed form by the same kind of qexponential function found for both the pitchfork and tangent bifurcation attractors v there is a final stage ultrafast dynamics towards the attractor with a sensitivity to initial conditions that decreases as an exponential of an exponential of time
|
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|
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|
706.4416
|
Population III star formation in a Lambda CDM universe, II: Effects of a
photodissociating background
|
We examine aspects of primordial star formation in the presence of a
molecular hydrogen-dissociating ultraviolet background. We compare a set of AMR
hydrodynamic cosmological simulations using a single cosmological realization
but with a range of ultraviolet background strengths in the Lyman-Werner band.
This allows us to study the effects of Lyman-Werner radiation on suppressing H2
cooling at low densities as well as the high-density evolution of the
collapsing core in a self-consistent cosmological framework. We find that the
addition of a photodissociating background results in a delay of the collapse
of high density gas at the center of the most massive halo in the simulation
and, as a result, an increase in the virial mass of this halo at the onset of
baryon collapse. We find that, contrary to previous results, Population III
star formation is not suppressed for J$_{21} \geq 0.1$, but occurs even with
backgrounds as high as J$_{21} = 1$. We find that H2 cooling leads to collapse
despite the depressed core molecular hydrogen fractions due to the elevated H2
cooling rates at $T=2-5 \times 10^3$ K. We observe a relationship between the
strength of the photodissociating background and the rate of accretion onto the
evolving protostellar cloud core, with higher LW background fluxes resulting in
higher accretion rates. Finally, we find that the collapsing halo cores in our
simulations do not fragment at densities below $n \sim 10^{10}$ cm$^{-3}$
regardless of the strength of the LW background, suggesting that Population III
stars forming in halos with T$_{vir} \sim 10^4$ K may still form in isolation.
|
astro-ph
|
we examine aspects of primordial star formation in the presence of a molecular hydrogendissociating ultraviolet background we compare a set of amr hydrodynamic cosmological simulations using a single cosmological realization but with a range of ultraviolet background strengths in the lymanwerner band this allows us to study the effects of lymanwerner radiation on suppressing h2 cooling at low densities as well as the highdensity evolution of the collapsing core in a selfconsistent cosmological framework we find that the addition of a photodissociating background results in a delay of the collapse of high density gas at the center of the most massive halo in the simulation and as a result an increase in the virial mass of this halo at the onset of baryon collapse we find that contrary to previous results population iii star formation is not suppressed for j_21 geq 01 but occurs even with backgrounds as high as j_21 1 we find that h2 cooling leads to collapse despite the depressed core molecular hydrogen fractions due to the elevated h2 cooling rates at t25 times 103 k we observe a relationship between the strength of the photodissociating background and the rate of accretion onto the evolving protostellar cloud core with higher lw background fluxes resulting in higher accretion rates finally we find that the collapsing halo cores in our simulations do not fragment at densities below n sim 1010 cm3 regardless of the strength of the lw background suggesting that population iii stars forming in halos with t_vir sim 104 k may still form in isolation
|
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|
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|
706.4417
|
Some Two Color, Four Variable Rado Numbers
|
There exists a minimum integer $N$ such that any 2-coloring of
$\{1,2,...,N\}$ admits a monochromatic solution to $x+y+kz =\ell w$ for $k,\ell
\in \mathbb{Z}^+$, where $N$ depends on $k$ and $\ell$. We determine $N$ when
$\ell-k \in \{0,1,2,3,4,5\}$, for all $k,\ell$ for which
${1/2}((\ell-k)^2-2)(\ell-k+1)\leq k \leq \ell-4$, as well as for arbitrary $k$
when $\ell=2$.
|
math.CO
|
there exists a minimum integer n such that any 2coloring of 12n admits a monochromatic solution to xykz ell w for kell in mathbbz where n depends on k and ell we determine n when ellk in 012345 for all kell for which 12ellk22ellk1leq k leq ell4 as well as for arbitrary k when ell2
|
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|
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|
706.4418
|
Fermi surface pockets in ortho-II YBa$_2$Cu$_3$O$_{6.5}$: the origin of
quantum oscillations?
|
In this paper we explore whether the quantum oscillation signals recently
observed in ortho-II YBa$_2$Cu$_3$O$_{6.5}$ may be explained by conventional
density functional band-structure theory. Our calculations show that the Fermi
surface of YBa$_2$Cu$_3$O$_{6.5}$ is extremely sensitive to small shifts in the
relative positions of the bands. With rigid band shifts of around 30 meV small
tubular pockets of Fermi surface develop around the Y point in the Brillouin
zone. The cross-sectional areas and band masses of the quantum oscillatory
orbits on these pockets are close to those observed. The difference between the
bandstructure of YBa$_2$Cu$_3$O$_{6.5}$ and YBa$_2$Cu$_4$O$_{8}$ are discussed.
|
cond-mat.supr-con cond-mat.str-el
|
in this paper we explore whether the quantum oscillation signals recently observed in orthoii yba_2cu_3o_65 may be explained by conventional density functional bandstructure theory our calculations show that the fermi surface of yba_2cu_3o_65 is extremely sensitive to small shifts in the relative positions of the bands with rigid band shifts of around 30 mev small tubular pockets of fermi surface develop around the y point in the brillouin zone the crosssectional areas and band masses of the quantum oscillatory orbits on these pockets are close to those observed the difference between the bandstructure of yba_2cu_3o_65 and yba_2cu_4o_8 are discussed
|
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|
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|
706.4419
|
Fossil AGN jets as ultra high energy particle accelerators
|
Remnants of AGN jets and their surrounding cocoons leave colossal
magnetohydrodynamic (MHD) fossil structures storing total energies ~10^{60}
erg. The original active galacic nucleus (AGN) may be dead but the fossil will
retain its stable configuration resembling the reversed-field pinch (RFP)
encountered in laboratory MHD experiments.
In an RFP the longitudinal magnetic field changes direction at a critical
distance from the axis, leading to magnetic re-connection there, and to slow
decay of the large-scale RFP field. We show that this field decay induces
large-scale electric fields which can accelerate cosmic rays with an E^{-2}
power-law up to ultra-high energies with a cut-off depending on the fossil
parameters. The cut-off is expected to be rigidity dependent, implying the
observed composition would change from light to heavy close to the cut-off if
one or two nearby AGN fossils dominate. Given that several percent of the
universe's volume may house such slowly decaying structures, these fossils may
even re-energize ultra-high energy cosmic rays from distant/old sources,
offsetting the ``GZK-losses'' due to interactions with photons of the cosmic
microwave background radiation and giving evidence of otherwise undetectable
fossils. In this case the composition would remain light to the highest
energies if distant sources or fossils dominated, but otherwise would be mixed.
It is hoped the new generation of cosmic ray experiments such as the Pierre
Auger Observatory and ultra-high energy neutrino telescopes such as ANITA and
lunar Cherenkov experiments will clarify this.
|
astro-ph
|
remnants of agn jets and their surrounding cocoons leave colossal magnetohydrodynamic mhd fossil structures storing total energies 1060 erg the original active galacic nucleus agn may be dead but the fossil will retain its stable configuration resembling the reversedfield pinch rfp encountered in laboratory mhd experiments in an rfp the longitudinal magnetic field changes direction at a critical distance from the axis leading to magnetic reconnection there and to slow decay of the largescale rfp field we show that this field decay induces largescale electric fields which can accelerate cosmic rays with an e2 powerlaw up to ultrahigh energies with a cutoff depending on the fossil parameters the cutoff is expected to be rigidity dependent implying the observed composition would change from light to heavy close to the cutoff if one or two nearby agn fossils dominate given that several percent of the universes volume may house such slowly decaying structures these fossils may even reenergize ultrahigh energy cosmic rays from distantold sources offsetting the gzklosses due to interactions with photons of the cosmic microwave background radiation and giving evidence of otherwise undetectable fossils in this case the composition would remain light to the highest energies if distant sources or fossils dominated but otherwise would be mixed it is hoped the new generation of cosmic ray experiments such as the pierre auger observatory and ultrahigh energy neutrino telescopes such as anita and lunar cherenkov experiments will clarify this
|
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|
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|
706.442
|
Bounds on Van der Waerden Numbers and Some Related Functions
|
For positive integers $s$ and $k_1, k_2, ..., k_s$, let $w(k_1,k_2,...,k_s)$
be the minimum integer $n$ such that any $s$-coloring $\{1,2,...,n\} \to
\{1,2,...,s\}$ admits a $k_i$-term arithmetic progression of color $i$ for some
$i$, $1 \leq i \leq s$. In the case when $k_1=k_2=...=k_s=k$ we simply write
$w(k;s)$.
That such a minimum integer exists follows from van der Waerden's theorem on
arithmetic progressions.
In the present paper we give a lower bound for $w(k,m)$ for each fixed $m$.
We include a table with values of $w(k,3)$ which match this lower bound closely
for $5 \leq k \leq 16$. We also give an upper bound for $w(k,4)$, an upper
bound for $w(4;s)$, and a lower bound for $w(k;s)$ for an arbitrary fixed $k$.
We discuss a number of other functions that are closely related to the van der
Waerden function.
|
math.CO
|
for positive integers s and k_1 k_2 k_s let wk_1k_2k_s be the minimum integer n such that any scoloring 12n to 12s admits a k_iterm arithmetic progression of color i for some i 1 leq i leq s in the case when k_1k_2k_sk we simply write wks that such a minimum integer exists follows from van der waerdens theorem on arithmetic progressions in the present paper we give a lower bound for wkm for each fixed m we include a table with values of wk3 which match this lower bound closely for 5 leq k leq 16 we also give an upper bound for wk4 an upper bound for w4s and a lower bound for wks for an arbitrary fixed k we discuss a number of other functions that are closely related to the van der waerden function
|
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|
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|
706.4421
|
A presentation for Hilden's subgroup of the braid group
|
Consider the unit ball, B = D x [0,1], containing n unknotted arcs a_1, ...
a_n such that the boundary of each a_i lies in D x {0}. We give a finite
presentation for the mapping class group of B fixing the arcs {a_1, ..., a_n}
setwise and fixing D x {1} pointwise. This presentation is calculated using the
action of this group on a simply-connected complex.
|
math.GR
|
consider the unit ball b d x 01 containing n unknotted arcs a_1 a_n such that the boundary of each a_i lies in d x 0 we give a finite presentation for the mapping class group of b fixing the arcs a_1 a_n setwise and fixing d x 1 pointwise this presentation is calculated using the action of this group on a simplyconnected complex
|
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|
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|
706.4422
|
Dynamics towards the Feigenbaum attractor
|
We expose at a previously unknown level of detail the features of the
dynamics of trajectories that either evolve towards the Feigenbaum attractor or
are captured by its matching repellor. Amongst these features are the
following: i) The set of preimages of the attractor and of the repellor are
embedded (dense) into each other. ii) The preimage layout is obtained as the
limiting form of the rank structure of the fractal boundaries between attractor
and repellor positions for the family of supercycle attractors. iii) The joint
set of preimages for each case form an infinite number of families of
well-defined phase-space gaps in the attractor or in the repellor. iv) The gaps
in each of these families can be ordered with decreasing width in accord to
power laws and are seen to appear sequentially in the dynamics generated by
uniform distributions of initial conditions. v) The power law with log-periodic
modulation associated to the rate of approach of trajectories towards the
attractor (and to the repellor) is explained in terms of the progression of gap
formation. vi) The relationship between the law of rate of convergence to the
attractor and the inexhaustible hierarchy feature of the preimage structure is
elucidated.
|
cond-mat.stat-mech nlin.CD
|
we expose at a previously unknown level of detail the features of the dynamics of trajectories that either evolve towards the feigenbaum attractor or are captured by its matching repellor amongst these features are the following i the set of preimages of the attractor and of the repellor are embedded dense into each other ii the preimage layout is obtained as the limiting form of the rank structure of the fractal boundaries between attractor and repellor positions for the family of supercycle attractors iii the joint set of preimages for each case form an infinite number of families of welldefined phasespace gaps in the attractor or in the repellor iv the gaps in each of these families can be ordered with decreasing width in accord to power laws and are seen to appear sequentially in the dynamics generated by uniform distributions of initial conditions v the power law with logperiodic modulation associated to the rate of approach of trajectories towards the attractor and to the repellor is explained in terms of the progression of gap formation vi the relationship between the law of rate of convergence to the attractor and the inexhaustible hierarchy feature of the preimage structure is elucidated
|
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|
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|
706.4423
|
Tuning Kinetic Magnetism of Strongly Correlated Electrons via Staggered
Flux
|
We explore the kinetic magnetism of the infinite-$U$ repulsive Hubbard models
at low hole densities on various lattices with nearest-neighbor hopping
integrals modulated by a staggered magnetic flux $\pm\phi$. Tuning $\phi$ from
0 to $\pi$ makes the ground state (GS) change from a Nagaoka-type ferromagnetic
state to a Haerter-Shastry-type antiferromagnetic state at a critical $\phi_c$,
with both states being of kinetic origin. Intra-plaquette spin correlation, as
well as the GS energy, signals such a quantum criticality. This tunable kinetic
magnetism is generic, and appears in chains, ladders and two-dimensional
lattices with squares or triangles as elementary constituents.
|
cond-mat.str-el cond-mat.stat-mech
|
we explore the kinetic magnetism of the infiniteu repulsive hubbard models at low hole densities on various lattices with nearestneighbor hopping integrals modulated by a staggered magnetic flux pmphi tuning phi from 0 to pi makes the ground state gs change from a nagaokatype ferromagnetic state to a haertershastrytype antiferromagnetic state at a critical phi_c with both states being of kinetic origin intraplaquette spin correlation as well as the gs energy signals such a quantum criticality this tunable kinetic magnetism is generic and appears in chains ladders and twodimensional lattices with squares or triangles as elementary constituents
|
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|
[-0.20507094597345904, 0.28165861687770016, -0.0016284406969421788, 0.11079541410956728, -0.030479767166176126, -0.18523631926724002, 0.0742364038541717, 0.3787322455428933, -0.2607324430179831, -0.26848955829382726, 0.042743258353469794, -0.35598086463777645, -0.06956538654631003, 0.0941885836201867, 0.12269504236449537, 0.010079389712528178, -0.017794923092189587, 0.019033617428258844, -0.13222269633490788, -0.1651215477993614, 0.2655101310804878, 0.010957478975730114, 0.239401635880533, 0.06411668907262777, 0.07467646050315939, 0.031847040220408844, 0.19195811101909432, -0.0015879009507204357, -0.15018464280782562, 0.02803012490529861, 0.21961007790910356, -0.11760881582373067, 0.17257225769166037, -0.396112300004614, -0.21961786892069013, 0.05649204870293799, 0.136786606478946, 0.14624769519034184, 0.0006815957432416709, -0.296758238011726, -0.026573254393511696, -0.19646974152052088, -0.121052252761652, -0.11916990916223241, -0.005107102082356026, 0.0510292027488743, -0.2788466592564395, 0.11394335016314136, 0.050369370720153184, 0.10341854097419663, -0.05170211550583573, -0.17215380036321126, -0.09461462297599371, 0.05504359132610261, 0.029649804254356576, 0.10782710690247385, 0.11742273436271046, -0.16469196826954813, -0.14474680544257065, 0.34427757192599145, -0.07345995949703808, -0.1526692038181385, 0.22622078097376383, -0.1464419159695114, -0.08505638628021667, 0.15243739765627604, 0.07787741462602035, 0.044123664976244696, -0.11233368130694879, 0.10605389574989922, 0.02747769400011748, 0.1915381589671597, -0.014372155219806653, 0.04955017849386326, 0.3057313927596337, 0.17424481698605968, 0.08908474302764884, 0.1896084185150501, -0.08928791559914029, -0.1357468178005595, -0.22414468990724631, -0.12027987572119424, -0.2742517706889071, 0.11228188452752012, -0.0729236691500869, -0.2166243545735549, 0.39518956629265295, 0.10259905681014062, 0.1918561459518969, -0.01944405773752614, 0.2082622101040263, 0.10684636313786829, 0.022093825632902353, 0.05377326908055693, 0.181784805532937, 0.19656023980902607, 0.11954085914123999, -0.2627341351618892, -0.010217432731664495, 0.08700709148359141]
|
706.4424
|
Steps toward a classifier for the Virtual Observatory. I. Classifying
the SDSS photometric archive
|
Modern photometric multiband digital surveys produce large amounts of data
that, in order to be effectively exploited, need automatic tools capable to
extract from photometric data an objective classification. We present here a
new method for classifying objects in large multi-parametric photometric data
bases, consisting of a combination of a clustering algorithm and a cluster
agglomeration tool. The generalization capabilities and the potentialities of
this approach are tested against the complexity of the Sloan Digital Sky Survey
archive, for which an example of application is reported.
|
astro-ph
|
modern photometric multiband digital surveys produce large amounts of data that in order to be effectively exploited need automatic tools capable to extract from photometric data an objective classification we present here a new method for classifying objects in large multiparametric photometric data bases consisting of a combination of a clustering algorithm and a cluster agglomeration tool the generalization capabilities and the potentialities of this approach are tested against the complexity of the sloan digital sky survey archive for which an example of application is reported
|
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|
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|
706.4425
|
A simple model of Coulomb disorder and screening in graphene
|
We suggest a simple model of disorder in graphene assuming that there are
randomly distributed positive and negative centers with equal concentration
$N/2$ in the bulk of silicon oxide substrate. We show that at zero gate voltage
such disorder creates two-dimensional concentration $n_0 \sim N^{2/3}$ of
electrons and holes in graphene. Electrons and holes reside in alternating in
space puddles of the size $R_0 \sim N^{-1/3}$. A typical puddle has only one or
two carriers in agreement with recent scanning single electron transistor
experiment.
|
cond-mat.mes-hall cond-mat.dis-nn
|
we suggest a simple model of disorder in graphene assuming that there are randomly distributed positive and negative centers with equal concentration n2 in the bulk of silicon oxide substrate we show that at zero gate voltage such disorder creates twodimensional concentration n_0 sim n23 of electrons and holes in graphene electrons and holes reside in alternating in space puddles of the size r_0 sim n13 a typical puddle has only one or two carriers in agreement with recent scanning single electron transistor experiment
|
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|
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|
706.4426
|
Be stars and binaries in the field of the SMC open cluster NGC330 with
VLT-FLAMES
|
Observations of hot stars belonging to the young cluster SMC-NGC330 and its
surrounding region were obtained with the VLT-GIRAFFE facilities in MEDUSA
mode. We investigated the B and Be star properties and proportions in this
environment of low metallicity. We also searched for rapid variability in Be
stars using photometric databases. With spectroscopic measurements we
characterized the emission and properties of Be stars. By cross-correlation
with photometric databases such as MACHO and OGLE, we searched for binaries in
our sample of hot stars, as well as for short-term variability in Be stars. We
report on the global characteristics of the Be star sample (131 objects). We
find that the proportion of early Be stars with a large equivalent width of the
Halpha emission line is higher in the SMC than in the LMC and MW. We find a
slight increase in the proportion of Be stars compared to B-type stars with
decreasing metallicity. We also discovered spectroscopic and photometric
binaries, and for the latter we give their orbital period. We identify 13 Be
stars with short-term variability. We determine their period(s) and find that 9
Be stars are multiperiodic.
|
astro-ph
|
observations of hot stars belonging to the young cluster smcngc330 and its surrounding region were obtained with the vltgiraffe facilities in medusa mode we investigated the b and be star properties and proportions in this environment of low metallicity we also searched for rapid variability in be stars using photometric databases with spectroscopic measurements we characterized the emission and properties of be stars by crosscorrelation with photometric databases such as macho and ogle we searched for binaries in our sample of hot stars as well as for shortterm variability in be stars we report on the global characteristics of the be star sample 131 objects we find that the proportion of early be stars with a large equivalent width of the halpha emission line is higher in the smc than in the lmc and mw we find a slight increase in the proportion of be stars compared to btype stars with decreasing metallicity we also discovered spectroscopic and photometric binaries and for the latter we give their orbital period we identify 13 be stars with shortterm variability we determine their periods and find that 9 be stars are multiperiodic
|
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|
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|
706.4427
|
Growing neutrinos and cosmological selection
|
The time evolution of a cosmological scalar field can be stopped by an
increasing mass of the neutrinos. This leads to a transition from a
cosmological scaling solution with dynamical dark energy at early time to a
cosmological constant dominated universe at late time. The trigger for the
transition is set at the time when the neutrinos become non-relativistic. The
characteristic mass scale for dark energy is thus related to the neutrino mass,
the only known particle physics scale in its vicinity. This explains the ``why
now problem'' for dark energy. We present a particle physics realization of
this ``growing matter'' scenario. It is based on the very slowly varying mass
of a superheavy scalar triplet field whose expectation value dominates the
light neutrino masses.
|
hep-ph
|
the time evolution of a cosmological scalar field can be stopped by an increasing mass of the neutrinos this leads to a transition from a cosmological scaling solution with dynamical dark energy at early time to a cosmological constant dominated universe at late time the trigger for the transition is set at the time when the neutrinos become nonrelativistic the characteristic mass scale for dark energy is thus related to the neutrino mass the only known particle physics scale in its vicinity this explains the why now problem for dark energy we present a particle physics realization of this growing matter scenario it is based on the very slowly varying mass of a superheavy scalar triplet field whose expectation value dominates the light neutrino masses
|
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|
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|
706.4428
|
Semi-analytical approach to magnetized temperature autocorrelations
|
The cosmic microwave background (CMB) temperature autocorrelations, induced
by a magnetized adiabatic mode of curvature inhomogeneities, are computed with
semi-analytical methods. As suggested by the latest CMB data, a nearly
scale-invariant spectrum for the adiabatic mode is consistently assumed. In
this situation, the effects of a fully inhomogeneous magnetic field are
scrutinized and constrained with particular attention to harmonics which are
relevant for the region of Doppler oscillations. Depending on the parameters of
the stochastic magnetic field a hump may replace the second peak of the angular
power spectrum. Detectable effects on the Doppler region are then expected only
if the magnetic power spectra have quasi-flat slopes and typical amplitude
(smoothed over a comoving scale of Mpc size and redshifted to the epoch of
gravitational collapse of the protogalaxy) exceeding 0.1 nG. If the magnetic
energy spectra are bluer (i.e. steeper in frequency) the allowed value of the
smoothed amplitude becomes, comparatively, larger (in the range of 20 nG). The
implications of this investigation for the origin of large-scale magnetic
fields in the Universe are discussed. Connections with forthcoming experimental
observations of CMB temperature fluctuations are also suggested and partially
explored.
|
astro-ph gr-qc hep-ph hep-th
|
the cosmic microwave background cmb temperature autocorrelations induced by a magnetized adiabatic mode of curvature inhomogeneities are computed with semianalytical methods as suggested by the latest cmb data a nearly scaleinvariant spectrum for the adiabatic mode is consistently assumed in this situation the effects of a fully inhomogeneous magnetic field are scrutinized and constrained with particular attention to harmonics which are relevant for the region of doppler oscillations depending on the parameters of the stochastic magnetic field a hump may replace the second peak of the angular power spectrum detectable effects on the doppler region are then expected only if the magnetic power spectra have quasiflat slopes and typical amplitude smoothed over a comoving scale of mpc size and redshifted to the epoch of gravitational collapse of the protogalaxy exceeding 01 ng if the magnetic energy spectra are bluer ie steeper in frequency the allowed value of the smoothed amplitude becomes comparatively larger in the range of 20 ng the implications of this investigation for the origin of largescale magnetic fields in the universe are discussed connections with forthcoming experimental observations of cmb temperature fluctuations are also suggested and partially explored
|
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|
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|
706.4429
|
Observation of B^0 \to D^{*-} \tau^+ \nu_{\tau} decay at Belle
|
We report an observation of the decay $B^0\to D^{*-} \tau^+ \nu_{\tau}$ in a
data sample containing $535\times10^6$ $B\bar{B}$ pairs collected with the
Belle detector at the KEKB asymmetric-energy $e^+e^-$ collider. We find a
signal with a significance of 5.2 standard deviations and measure the branching
fraction $\mathcal{B}(B^0\to D^{*-} \tau ^+ \nu_{\tau})=(2.02 ^{+0.40}_{-0.37}
(stat) \pm 0.37 (syst)) % $. This is the first observation of an exclusive $B$
decay with a $b \to c \tau \nu_{\tau}$ transition.
|
hep-ex
|
we report an observation of the decay b0to d tau nu_tau in a data sample containing 535times106 bbarb pairs collected with the belle detector at the kekb asymmetricenergy ee collider we find a signal with a significance of 52 standard deviations and measure the branching fraction mathcalbb0to d tau nu_tau202 040_037 stat pm 037 syst this is the first observation of an exclusive b decay with a b to c tau nu_tau transition
|
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|
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|
706.443
|
Investigating the extended geometric scaling region at LHC with
polarized and unpolarized final states
|
We present predictions for charged hadron production and Lambda polarization
in p-p and p-Pb collisions at the LHC using the saturation inspired DHJ model
for the dipole cross section in the extended geometric scaling region.
|
hep-ph
|
we present predictions for charged hadron production and lambda polarization in pp and ppb collisions at the lhc using the saturation inspired dhj model for the dipole cross section in the extended geometric scaling region
|
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|
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|
706.4431
|
The Einstein static universe in Loop Quantum Cosmology
|
Loop Quantum Cosmology strongly modifies the high-energy dynamics of
Friedman-Robertson-Walker models and removes the big-bang singularity. We
investigate how LQC corrections affect the stability properties of the Einstein
static universe. In General Relativity, the Einstein static model with positive
cosmological constant Lambda is unstable to homogeneous perturbations. We show
that LQC modifications can lead to a centre of stability for a large enough
positive value of Lambda.
|
gr-qc astro-ph hep-th
|
loop quantum cosmology strongly modifies the highenergy dynamics of friedmanrobertsonwalker models and removes the bigbang singularity we investigate how lqc corrections affect the stability properties of the einstein static universe in general relativity the einstein static model with positive cosmological constant lambda is unstable to homogeneous perturbations we show that lqc modifications can lead to a centre of stability for a large enough positive value of lambda
|
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|
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|
706.4432
|
The minority game: An economics perspective
|
This paper gives a critical account of the minority game literature. The
minority game is a simple congestion game: players need to choose between two
options, and those who have selected the option chosen by the minority win. The
learning model proposed in this literature seems to differ markedly from the
learning models commonly used in economics. We relate the learning model from
the minority game literature to standard game-theoretic learning models, and
show that in fact it shares many features with these models. However, the
predictions of the learning model differ considerably from the predictions of
most other learning models. We discuss the main predictions of the learning
model proposed in the minority game literature, and compare these to
experimental findings on congestion games.
|
q-fin.GN physics.soc-ph
|
this paper gives a critical account of the minority game literature the minority game is a simple congestion game players need to choose between two options and those who have selected the option chosen by the minority win the learning model proposed in this literature seems to differ markedly from the learning models commonly used in economics we relate the learning model from the minority game literature to standard gametheoretic learning models and show that in fact it shares many features with these models however the predictions of the learning model differ considerably from the predictions of most other learning models we discuss the main predictions of the learning model proposed in the minority game literature and compare these to experimental findings on congestion games
|
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|
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|
706.4433
|
Relaxation dynamics of a quantum Brownian particle in an ideal gas
|
We show how the quantum analog of the Fokker-Planck equation for describing
Brownian motion can be obtained as the diffusive limit of the quantum linear
Boltzmann equation. The latter describes the quantum dynamics of a tracer
particle in a dilute, ideal gas by means of a translation-covariant master
equation. We discuss the type of approximations required to obtain the
generalized form of the Caldeira-Leggett master equation, along with their
physical justification. Microscopic expressions for the diffusion and
relaxation coefficients are obtained by analyzing the limiting form of the
equation in both the Schroedinger and the Heisenberg picture.
|
quant-ph
|
we show how the quantum analog of the fokkerplanck equation for describing brownian motion can be obtained as the diffusive limit of the quantum linear boltzmann equation the latter describes the quantum dynamics of a tracer particle in a dilute ideal gas by means of a translationcovariant master equation we discuss the type of approximations required to obtain the generalized form of the caldeiraleggett master equation along with their physical justification microscopic expressions for the diffusion and relaxation coefficients are obtained by analyzing the limiting form of the equation in both the schroedinger and the heisenberg picture
|
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|
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|
706.4434
|
Pairing of 1D Bose-Fermi mixtures with unequal masses
|
We have considered one-dimensional Bose-Fermi mixture with equal densities
and unequal masses using numerical density matrix renormalization group (DMRG).
For the mass ratio of K-Rb mixture and attraction between bosons and fermions,
we determined the phase diagram. For weak boson-boson interactions, there is a
direct transition between two-component Luttinger liquid and collapsed phases
as the boson-fermion attraction is increased. For strong enough boson-boson
interactions, we find an intermediate "paired" phase, which is a
single-component Luttinger liquid of composite particles. We investigated
correlation functions of such a "paired" phase, studied the stability of
"paired" phase to density imbalance, and discussed various experimental
techniques which can be used to detect it.
|
cond-mat.str-el cond-mat.other
|
we have considered onedimensional bosefermi mixture with equal densities and unequal masses using numerical density matrix renormalization group dmrg for the mass ratio of krb mixture and attraction between bosons and fermions we determined the phase diagram for weak bosonboson interactions there is a direct transition between twocomponent luttinger liquid and collapsed phases as the bosonfermion attraction is increased for strong enough bosonboson interactions we find an intermediate paired phase which is a singlecomponent luttinger liquid of composite particles we investigated correlation functions of such a paired phase studied the stability of paired phase to density imbalance and discussed various experimental techniques which can be used to detect it
|
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|
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|
706.4435
|
Discovery of Very High Energy gamma-rays from 1ES 1011+496 at z=0.212
|
We report on the discovery of Very High Energy (VHE) gamma-ray emission from
the BL Lacertae object 1ES1011+496. The observation was triggered by an optical
outburst in March 2007 and the source was observed with the MAGIC telescope
from March to May 2007. Observing for 18.7 hr we find an excess of 6.2 sigma
with an integrated flux above 200 GeV of (1.58$\pm0.32) 10^{-11}$ photons
cm$^{-2}$ s$^{-1}$. The VHE gamma-ray flux is >40% higher than in March-April
2006 (reported elsewhere), indicating that the VHE emission state may be
related to the optical emission state. We have also determined the redshift of
1ES1011+496 based on an optical spectrum that reveals the absorption lines of
the host galaxy. The redshift of z=0.212 makes 1ES1011+496 the most distant
source observed to emit VHE gamma-rays up to date.
|
astro-ph
|
we report on the discovery of very high energy vhe gammaray emission from the bl lacertae object 1es1011496 the observation was triggered by an optical outburst in march 2007 and the source was observed with the magic telescope from march to may 2007 observing for 187 hr we find an excess of 62 sigma with an integrated flux above 200 gev of 158pm032 1011 photons cm2 s1 the vhe gammaray flux is 40 higher than in marchapril 2006 reported elsewhere indicating that the vhe emission state may be related to the optical emission state we have also determined the redshift of 1es1011496 based on an optical spectrum that reveals the absorption lines of the host galaxy the redshift of z0212 makes 1es1011496 the most distant source observed to emit vhe gammarays up to date
|
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|
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|
706.4436
|
On the moment limit of quantum observables, with an application to the
balanced homodyne detection
|
We consider the moment operators of the observable (i.e. a semispectral
measure or POM) associated with the balanced homodyne detection statistics,
with paying attention to the correct domains of these unbounded operators. We
show that the high amplitude limit, when performed on the moment operators,
actually determines uniquely the entire statistics of a rotated quadrature
amplitude of the signal field, thereby verifying the usual assumption that the
homodyne detection achieves a measurement of that observable. We also consider,
in a general setting, the possibility of constructing a measurement of a single
quantum observable from a sequence of observables by taking the limit on the
level of moment operators of these observables. In this context, we show that
under some natural conditions (each of which is satisfied by the homodyne
detector example), the existence of the moment limits ensures that the
underlying probability measures converge weakly to the probability measure of
the limiting observable. The moment approach naturally requires that the
observables be determined by their moment operator sequences (which does not
automatically happen), and it turns out, in particular, that this is the case
for the balanced homodyne detector.
|
quant-ph
|
we consider the moment operators of the observable ie a semispectral measure or pom associated with the balanced homodyne detection statistics with paying attention to the correct domains of these unbounded operators we show that the high amplitude limit when performed on the moment operators actually determines uniquely the entire statistics of a rotated quadrature amplitude of the signal field thereby verifying the usual assumption that the homodyne detection achieves a measurement of that observable we also consider in a general setting the possibility of constructing a measurement of a single quantum observable from a sequence of observables by taking the limit on the level of moment operators of these observables in this context we show that under some natural conditions each of which is satisfied by the homodyne detector example the existence of the moment limits ensures that the underlying probability measures converge weakly to the probability measure of the limiting observable the moment approach naturally requires that the observables be determined by their moment operator sequences which does not automatically happen and it turns out in particular that this is the case for the balanced homodyne detector
|
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|
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|
706.4437
|
Gravitational waves from inspiralling compact binaries: hexagonal
template placement and its efficiency in detecting physical signals
|
Matched filtering is used to search for gravitational waves emitted by
inspiralling compact binaries in data from the ground-based interferometers.
One of the key aspects of the detection process is the design of a template
bank that covers the astrophysically pertinent parameter space. In an earlier
paper, we described a template bank that is based on a square lattice. Although
robust, we showed that the square placement is over-efficient, with the
implication that it is computationally more demanding than required. In this
paper, we present a template bank based on an hexagonal lattice, which size is
reduced by 40% with respect to the proposed square placement. We describe the
practical aspects of the hexagonal template bank implementation, its size, and
computational cost. We have also performed exhaustive simulations to
characterize its efficiency and safeness. We show that the bank is adequate to
search for a wide variety of binary systems (primordial black holes, neutron
stars and stellar mass black holes) and in data from both current detectors
(initial LIGO, Virgo and GEO600) as well as future detectors (advanced LIGO and
EGO). Remarkably, although our template bank placement uses a metric arising
from a particular template family, namely stationary phase approximation, we
show that it can be used successfully with other template families (e.g., Pade
resummation and effective one-body approximation). This quality of being
effective for different template families makes the proposed bank suitable for
a search that would use several of them in parallel (e.g., in a binary black
hole search). The hexagonal template bank described in this paper is currently
used to search for non-spinning inspiralling compact binaries in data from the
Laser Interferometer Gravitational-Wave Observatory (LIGO).
|
gr-qc
|
matched filtering is used to search for gravitational waves emitted by inspiralling compact binaries in data from the groundbased interferometers one of the key aspects of the detection process is the design of a template bank that covers the astrophysically pertinent parameter space in an earlier paper we described a template bank that is based on a square lattice although robust we showed that the square placement is overefficient with the implication that it is computationally more demanding than required in this paper we present a template bank based on an hexagonal lattice which size is reduced by 40 with respect to the proposed square placement we describe the practical aspects of the hexagonal template bank implementation its size and computational cost we have also performed exhaustive simulations to characterize its efficiency and safeness we show that the bank is adequate to search for a wide variety of binary systems primordial black holes neutron stars and stellar mass black holes and in data from both current detectors initial ligo virgo and geo600 as well as future detectors advanced ligo and ego remarkably although our template bank placement uses a metric arising from a particular template family namely stationary phase approximation we show that it can be used successfully with other template families eg pade resummation and effective onebody approximation this quality of being effective for different template families makes the proposed bank suitable for a search that would use several of them in parallel eg in a binary black hole search the hexagonal template bank described in this paper is currently used to search for nonspinning inspiralling compact binaries in data from the laser interferometer gravitationalwave observatory ligo
|
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|
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|
706.4438
|
Non-Markovian quantum jumps
|
Open quantum systems that interact with structured reservoirs exhibit
non-Markovian dynamics. We present a quantum jump method for treating the
dynamics of such systems. This approach is a generalization of the standard
Monte Carlo Wave Function (MCWF) method for Markovian dynamics. The MCWF method
identifies decay rates with jump probabilities and fails for non-Markovian
systems where the time-dependent rates become temporarily negative. Our
non-Markovian quantum jump (NMQJ) approach circumvents this problem and
provides an efficient unravelling of the ensemble dynamics.
|
quant-ph
|
open quantum systems that interact with structured reservoirs exhibit nonmarkovian dynamics we present a quantum jump method for treating the dynamics of such systems this approach is a generalization of the standard monte carlo wave function mcwf method for markovian dynamics the mcwf method identifies decay rates with jump probabilities and fails for nonmarkovian systems where the timedependent rates become temporarily negative our nonmarkovian quantum jump nmqj approach circumvents this problem and provides an efficient unravelling of the ensemble dynamics
|
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|
[-0.11682292956393212, 0.13901931092423184, -0.12065728795714677, 0.10703639816929353, 0.016253004624741153, -0.21014794126385822, 0.04764911303063855, 0.36123046088032423, -0.29901332248700785, -0.20656279856339096, 0.02718606318521779, -0.25207594151142987, -0.17273301706882194, 0.2482708182069473, 0.012929448700742797, 0.09284071137662978, 0.1185687743127346, -0.031088905851356687, -0.020566015131771566, -0.20325725944712758, 0.2736441063112579, 0.05386053497350076, 0.2672164115938358, 0.009270332672167569, 0.1564246602472849, 0.025360537951928563, 0.026826844876632096, -0.036969249123649205, -0.11120210260496606, 0.08071257572009927, 0.23275842799339444, 0.08324894085526466, 0.3368734983261675, -0.4192521464312449, -0.2699408919317648, 0.07709665461443364, 0.1250522560418176, 0.22928728541592136, -0.0507698435569182, -0.33748272618395275, -0.0240078660834115, -0.18672761452035047, -0.1564446796895936, -0.11686505903489888, -0.02738234223506879, -0.0013117219146806746, -0.28035615272819997, 0.1618692116229795, 0.06409034067764878, 0.0026608819500324897, -4.119869990972802e-05, -0.040802023524884136, 0.08578783422417473, 0.124587981950026, -0.04405594993586419, -0.02292367651243694, 0.1780569949944038, -0.09970764235476963, -0.15641495580784975, 0.31617972254171034, -0.10180565521586686, -0.2487215072091203, 0.22821314886386973, -0.09924707385434886, -0.13491191164357588, 0.17302949560107664, 0.16172232280950993, 0.16022004335973178, -0.2136241824948229, 0.10087219727429328, 0.04213709078048851, 0.12382021315133898, -0.0504053963079059, 0.03903912483365275, 0.1692091395627358, 0.1932481355033815, 0.054514525074046104, 0.16761002682615073, -0.05012175645970274, -0.28910858505405485, -0.26778183369897307, -0.1752465885132551, -0.17341916605946608, 0.09708872278624767, -0.06788116364587041, -0.23034716332913377, 0.3305456951726228, 0.22472180232871325, 0.15479098659707233, 0.08922705957957078, 0.2595390287868213, 0.2053345035368693, -0.013923898083157837, 0.10670122953015379, 0.10978062226204202, 0.14854556852078532, 0.08009159545181319, -0.3420470021039364, 0.11474096779129468, 0.053096821991493924]
|
706.4439
|
AGN Observations in the GeV/TeV Energy Range with the MAGIC Telescope
|
MAGIC currently is the largest imaging atmospheric Cerenkov telescope
world-wide. Since 2004, gamma-ray emission from several active galactic nuclei
in the GeV/TeV energy range has been detected, some of which were newly
discovered as very-high energy gamma-ray sources. The gamma-rays are assumed to
originate from particle acceleration processes in the AGN jets. We give an
overview of the AGN observed and detected by MAGIC, discuss spectral and
temporal properties of these and show physics implications of some selected
observations.
|
astro-ph
|
magic currently is the largest imaging atmospheric cerenkov telescope worldwide since 2004 gammaray emission from several active galactic nuclei in the gevtev energy range has been detected some of which were newly discovered as veryhigh energy gammaray sources the gammarays are assumed to originate from particle acceleration processes in the agn jets we give an overview of the agn observed and detected by magic discuss spectral and temporal properties of these and show physics implications of some selected observations
|
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|
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|
706.444
|
2-State 3-Symbol Universal Turing Machines Do Not Exist
|
In this brief note, we give a simple information-theoretic proof that 2-state
3-symbol universal Turing machines cannot possibly exist, unless one loosens
the definition of "universal".
|
cs.OH
|
in this brief note we give a simple informationtheoretic proof that 2state 3symbol universal turing machines cannot possibly exist unless one loosens the definition of universal
|
[['in', 'this', 'brief', 'note', 'we', 'give', 'a', 'simple', 'informationtheoretic', 'proof', 'that', '2state', '3symbol', 'universal', 'turing', 'machines', 'can', 'not', 'possibly', 'exist', 'unless', 'one', 'loosens', 'the', 'definition', 'of', 'universal']]
|
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|
706.4441
|
Free $n$-distributions: holonomy, sub-Riemannian structures, Fefferman
constructions and dual distributions
|
This paper analyses the parabolic geometries generated by a free
$n$-distribution in the tangent space of a manifold. It shows that certain
holonomy reductions of the associated normal Tractor connections, imply
preferred connections with special properties, along with Riemannian or
sub-Riemannian structures on the manifold. It constructs examples of these
holonomy reductions in the simplest cases. The main results, however, lie in
the free 3-distributions. In these cases, there are normal Fefferman
constructions over CR and Lagrangian contact structures corresponding to
holonomy reductions to SO(4,2) and SO(3,3), respectively. There is also a
fascinating construction of a `dual' distribution when the holonomy reduces to
$G_2'$.
|
math.DG math.AP math.MG
|
this paper analyses the parabolic geometries generated by a free ndistribution in the tangent space of a manifold it shows that certain holonomy reductions of the associated normal tractor connections imply preferred connections with special properties along with riemannian or subriemannian structures on the manifold it constructs examples of these holonomy reductions in the simplest cases the main results however lie in the free 3distributions in these cases there are normal fefferman constructions over cr and lagrangian contact structures corresponding to holonomy reductions to so42 and so33 respectively there is also a fascinating construction of a dual distribution when the holonomy reduces to g_2
|
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|
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|
706.4442
|
A First Synoptic Blazar Study Comprising Thirteen Blazars Visible in
E>100 GeV Gamma-Rays
|
Since 2002, the number of detected blazars at E_\gamma > 100 GeV has more
than doubled. I study all currently known BL Lac-type objects with published
energy spectra. Their intrinsic energy spectra are reconstructed by removing
extragalactic background light attenuation effects. The emission properties are
then compared and correlated among each other, with X-ray data, and with the
individual black hole masses. In addition, I consider temporal properties of
the very high energy gamma-ray flux. Key findings concern the flux--black hole
mass and variability scale--black hole mass connections and the correlation of
the spectral slope and the luminosity. As a specific application, the study
allows to constrain the still undetermined redshift of the blazar PG 1553+113.
|
astro-ph
|
since 2002 the number of detected blazars at e_gamma 100 gev has more than doubled i study all currently known bl lactype objects with published energy spectra their intrinsic energy spectra are reconstructed by removing extragalactic background light attenuation effects the emission properties are then compared and correlated among each other with xray data and with the individual black hole masses in addition i consider temporal properties of the very high energy gammaray flux key findings concern the fluxblack hole mass and variability scaleblack hole mass connections and the correlation of the spectral slope and the luminosity as a specific application the study allows to constrain the still undetermined redshift of the blazar pg 1553113
|
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|
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|
706.4443
|
Thermal Dileptons at LHC
|
We predict dilepton invariant-mass spectra for central 5.5 ATeV Pb-Pb
collisions at LHC. Hadronic emission in the low-mass region is calculated using
in-medium spectral functions of light vector mesons within hadronic many-body
theory. In the intermediate-mass region thermal radiation from the Quark-Gluon
Plasma, evaluated perturbatively with hard-thermal loop corrections, takes
over. An important source over the entire mass range are decays of correlated
open-charm hadrons, rendering the nuclear modification of charm and bottom
spectra a critical ingredient.
|
hep-ph nucl-ex nucl-th
|
we predict dilepton invariantmass spectra for central 55 atev pbpb collisions at lhc hadronic emission in the lowmass region is calculated using inmedium spectral functions of light vector mesons within hadronic manybody theory in the intermediatemass region thermal radiation from the quarkgluon plasma evaluated perturbatively with hardthermal loop corrections takes over an important source over the entire mass range are decays of correlated opencharm hadrons rendering the nuclear modification of charm and bottom spectra a critical ingredient
|
[['we', 'predict', 'dilepton', 'invariantmass', 'spectra', 'for', 'central', '55', 'atev', 'pbpb', 'collisions', 'at', 'lhc', 'hadronic', 'emission', 'in', 'the', 'lowmass', 'region', 'is', 'calculated', 'using', 'inmedium', 'spectral', 'functions', 'of', 'light', 'vector', 'mesons', 'within', 'hadronic', 'manybody', 'theory', 'in', 'the', 'intermediatemass', 'region', 'thermal', 'radiation', 'from', 'the', 'quarkgluon', 'plasma', 'evaluated', 'perturbatively', 'with', 'hardthermal', 'loop', 'corrections', 'takes', 'over', 'an', 'important', 'source', 'over', 'the', 'entire', 'mass', 'range', 'are', 'decays', 'of', 'correlated', 'opencharm', 'hadrons', 'rendering', 'the', 'nuclear', 'modification', 'of', 'charm', 'and', 'bottom', 'spectra', 'a', 'critical', 'ingredient']]
|
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|
706.4444
|
Automatic Active-Region Identification and Azimuth Disambiguation of the
SOLIS/VSM Full-Disk Vector Magnetograms
|
The Vector Spectromagnetograph (VSM) of the NSO's Synoptic Optical Long-Term
Investigations of the Sun (SOLIS) facility is now operational and obtains the
first-ever vector magnetic field measurements of the entire visible solar
hemisphere. To fully exploit the unprecedented SOLIS/VSM data, however, one
must first address two critical problems: first, the study of solar active
regions requires an automatic, physically intuitive, technique for
active-region identification in the solar disk. Second, use of active-region
vector magnetograms requires removal of the azimuthal $180^o$-ambiguity in the
orientation of the transverse magnetic field component. Here we report on an
effort to address both problems simultaneously and efficiently. To identify
solar active regions we apply an algorithm designed to locate complex,
flux-balanced, magnetic structures with a dominant E-W orientation on the disk.
Each of the disk portions corresponding to active regions is thereafter
extracted and subjected to the Nonpotential Magnetic Field Calculation (NPFC)
method that provides a physically-intuitive solution of the 180-degree
ambiguity. Both algorithms have been integrated into the VSM data pipeline and
operate in real time, without human intervention. We conclude that this
combined approach can contribute meaningfully to our emerging capability for
full-disk vector magnetography as pioneered by SOLIS today and will be carried
out by ground-based and space-borne magnetographs in the future.
|
astro-ph
|
the vector spectromagnetograph vsm of the nsos synoptic optical longterm investigations of the sun solis facility is now operational and obtains the firstever vector magnetic field measurements of the entire visible solar hemisphere to fully exploit the unprecedented solisvsm data however one must first address two critical problems first the study of solar active regions requires an automatic physically intuitive technique for activeregion identification in the solar disk second use of activeregion vector magnetograms requires removal of the azimuthal 180oambiguity in the orientation of the transverse magnetic field component here we report on an effort to address both problems simultaneously and efficiently to identify solar active regions we apply an algorithm designed to locate complex fluxbalanced magnetic structures with a dominant ew orientation on the disk each of the disk portions corresponding to active regions is thereafter extracted and subjected to the nonpotential magnetic field calculation npfc method that provides a physicallyintuitive solution of the 180degree ambiguity both algorithms have been integrated into the vsm data pipeline and operate in real time without human intervention we conclude that this combined approach can contribute meaningfully to our emerging capability for fulldisk vector magnetography as pioneered by solis today and will be carried out by groundbased and spaceborne magnetographs in the future
|
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|
[-0.09636126119647906, 0.12056438068537048, -0.034394825087722646, 0.06256985064856618, -0.12665390047026379, -0.056666201797122374, 0.012760874899950895, 0.43045061156064557, -0.2271688129779611, -0.339737222291547, 0.1098035170460503, -0.23792786178352873, -0.1148332703761694, 0.22742202630574018, -0.029999233575361786, 0.048848647261639996, 0.07829058251976433, 0.009013248770163533, -0.016547578246038603, -0.20268779524610908, 0.2575078236215423, 0.08954657505558242, 0.25629750298977827, -0.008127638557703015, 0.09584788626291607, -0.019077790010682615, -0.08128894655296855, 0.01362248043514093, -0.08699355046753604, 0.12829329845295068, 0.23894605176015335, 0.15377280562469942, 0.26050518261509364, -0.45928187925439845, -0.21774971622831085, 0.04919525707234143, 0.16281815321055468, 0.02877729247729673, -0.0279457340714339, -0.2790860971569587, 0.07378443547816385, -0.08645990469524165, -0.13055201989997392, -0.08657477302120277, -0.006979139687707336, -0.024289666264235493, -0.2963940593172823, -0.003345637112682124, -0.0028159274749177104, 0.12675057229937978, -0.1459031885213544, -0.07033648897122824, -0.03625696958276626, 0.17681081753455852, 0.05033601859014071, 0.10008114601572325, 0.15259818795847854, -0.11865521520019719, -0.1263052826439828, 0.3453592208869149, -0.06404817751363705, -0.11143977388418748, 0.14375617866110252, -0.17016063964787567, -0.139518464345075, 0.14901543595676608, 0.21663839306178811, 0.10726922545103026, -0.1515818162924002, 0.053304480712941034, -0.03311538966773657, 0.17501635079463704, 0.004815495630913374, -0.012562164225789348, 0.256977992978963, 0.14168858380640664, 0.058604518668202495, 0.1316728483908921, -0.2231083440585463, -0.05921391186050393, -0.24782667755100288, -0.14707144312493717, -0.0981791492943701, 0.0071133734896761235, -0.0414696732146329, -0.15111307116029293, 0.4095369450119658, 0.2001300763481399, 0.1775488741250272, -0.03507780749462189, 0.36275975166655117, 0.039467753296045134, 0.11659023213382971, 0.08117577898467593, 0.313516066787301, 0.1362880969645108, 0.19680267553018968, -0.2309781992865078, 0.02182557420475346, 0.042564496205246265]
|
706.4445
|
Random Fiber Laser
|
We investigate the effects of two dimensional confinement on the lasing
properties of a classical random laser system operating in the incoherent
feedback (diffusive) regime. A suspension of 250nm rutile (TiO2) particles in a
Rhodamine 6G solution was inserted into the hollow core of a photonic crystal
fiber (PCF) generating the first random fiber laser and a novel
quasi-one-dimensional RL geometry. Comparison with similar systems in bulk
format shows that the random fiber laser presents an efficiency that is at
least two orders of magnitude higher.
|
physics.optics
|
we investigate the effects of two dimensional confinement on the lasing properties of a classical random laser system operating in the incoherent feedback diffusive regime a suspension of 250nm rutile tio2 particles in a rhodamine 6g solution was inserted into the hollow core of a photonic crystal fiber pcf generating the first random fiber laser and a novel quasionedimensional rl geometry comparison with similar systems in bulk format shows that the random fiber laser presents an efficiency that is at least two orders of magnitude higher
|
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|
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|
706.4446
|
An optimization problem with volume constrain in Orlicz spaces
|
We consider the optimization problem of minimizing $\int_{\Omega}G(|\nabla
u|) dx$ in the class of functions $W^{1,G}(\Omega)$, with a constrain on the
volume of $\{u>0\}$. The conditions on the function $G$ allow for a different
behavior at
0 and at $\infty$. We consider a penalization problem, and we prove that for
small values of the penalization parameter, the constrained volume is attained.
In this way we prove that every solution $u$ is locally Lipschitz continuous
and that the free boundary, $\partial\{u>0\}\cap \Omega$, is smooth.
|
math.AP
|
we consider the optimization problem of minimizing int_omegagnabla u dx in the class of functions w1gomega with a constrain on the volume of u0 the conditions on the function g allow for a different behavior at 0 and at infty we consider a penalization problem and we prove that for small values of the penalization parameter the constrained volume is attained in this way we prove that every solution u is locally lipschitz continuous and that the free boundary partialu0cap omega is smooth
|
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|
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|
706.4447
|
Pure motives, mixed motives and extensions of motives associated to
singular surfaces
|
We first recall the construction of the Chow motive modelling intersection
cohomology of a proper surface and study its fundamental properties. Using
Voevodsky's category of effective geometrical motives, we then study the motive
of the exceptional divisor in a non-singular blow-up. If all geometric
irreducible components of the divisor are of genus zero, then Voevodsky's
formalism allows us to construct certain one-extensions of Chow motives, as
canonical sub-quotients of the motive with compact support of the smooth part
of the surface. Specializing to Hilbert--Blumenthal surfaces, we recover a
motivic interpretation of a recent construction of A. Caspar.
|
math.KT math.AG
|
we first recall the construction of the chow motive modelling intersection cohomology of a proper surface and study its fundamental properties using voevodskys category of effective geometrical motives we then study the motive of the exceptional divisor in a nonsingular blowup if all geometric irreducible components of the divisor are of genus zero then voevodskys formalism allows us to construct certain oneextensions of chow motives as canonical subquotients of the motive with compact support of the smooth part of the surface specializing to hilbertblumenthal surfaces we recover a motivic interpretation of a recent construction of a caspar
|
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|
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|
706.4448
|
Search for Anomalous Production of Multilepton Events in p-pbar
Collisions at sqrt(s) = 1.96 TeV
|
We report a search for the anomalous production of events with multiple
charged leptons in p-pbar collisions at sqrt{s} = 1.96 TeV using a data sample
corresponding to an integrated luminosity of 346 pb^{-1} collected by the CDF
II detector at the Fermilab Tevatron. The search is divided into three-lepton
and four-or-more-lepton data samples. We observe six events in the three-lepton
sample and zero events in the >=4-lepton sample. Both numbers of events are
consistent with standard model background expectations. Within the framework of
an R-parity violating supergravity model, the results are interpreted as mass
limits on the lightest neutralino and chargino particles. For one particular
choice of model parameters, the limits are M_neutralino > 110 GeV/c^{2} and
M_chargino > 203 GeV/c^{2} at 95% confidence level; the variation of these mass
limits with model parameters is presented.
|
hep-ex
|
we report a search for the anomalous production of events with multiple charged leptons in ppbar collisions at sqrts 196 tev using a data sample corresponding to an integrated luminosity of 346 pb1 collected by the cdf ii detector at the fermilab tevatron the search is divided into threelepton and fourormorelepton data samples we observe six events in the threelepton sample and zero events in the 4lepton sample both numbers of events are consistent with standard model background expectations within the framework of an rparity violating supergravity model the results are interpreted as mass limits on the lightest neutralino and chargino particles for one particular choice of model parameters the limits are m_neutralino 110 gevc2 and m_chargino 203 gevc2 at 95 confidence level the variation of these mass limits with model parameters is presented
|
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|
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|
706.4449
|
Cheeger constants of surfaces and isoperimetric inequalities
|
We show that the Cheeger constant of compact surfaces is bounded by a
function of the area. We apply this to isoperimetric profiles of bounded genus
non-compact surfaces, to show that if their isoperimetric profile grows faster
than $\sqrt t$, then it grows at least as fast as a linear function. This
generalizes a result of Gromov for simply connected surfaces.
We study the isoperimetric problem in dimension 3. We show that if the
filling volume function in dimension 2 is Euclidean, while in dimension 3 is
sub-Euclidean and there is a $g$ such that minimizers in dimension 3 have genus
at most $g$, then the filling function in dimension 3 is `almost' linear.
|
math.DG math.GR math.GT math.MG
|
we show that the cheeger constant of compact surfaces is bounded by a function of the area we apply this to isoperimetric profiles of bounded genus noncompact surfaces to show that if their isoperimetric profile grows faster than sqrt t then it grows at least as fast as a linear function this generalizes a result of gromov for simply connected surfaces we study the isoperimetric problem in dimension 3 we show that if the filling volume function in dimension 2 is euclidean while in dimension 3 is subeuclidean and there is a g such that minimizers in dimension 3 have genus at most g then the filling function in dimension 3 is almost linear
|
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|
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|
706.445
|
Quadratic optimal functional quantization of stochastic processes and
numerical applications
|
In this paper, we present an overview of the recent developments of
functional quantization of stochastic processes, with an emphasis on the
quadratic case. Functional quantization is a way to approximate a process,
viewed as a Hilbert-valued random variable, using a nearest neighbour
projection on a finite codebook. A special emphasis is made on the
computational aspects and the numerical applications, in particular the pricing
of some path-dependent European options.
|
math.PR
|
in this paper we present an overview of the recent developments of functional quantization of stochastic processes with an emphasis on the quadratic case functional quantization is a way to approximate a process viewed as a hilbertvalued random variable using a nearest neighbour projection on a finite codebook a special emphasis is made on the computational aspects and the numerical applications in particular the pricing of some pathdependent european options
|
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|
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|
706.4451
|
Turbulence models generator
|
In this paper we explore a possibility that all transport turbulent models
are contained in a coarse-grained kinetic equation. Building on a recent work
by H.Chen et al (2004), we account for fluctuations of a single -point
probability density in turbulence, by introducing a``two-level'' (${\bf
c,v}$)-phase-space, separating microscopic (${\bf c'\equiv c_{micro}= c-v}$)
and hydrodynamic (${\bf v'=v-V}$) modes. Unlike traditional kinetic theories,
with hydrodynamic approximations derived in terms of small deviations from
thermodynamic equilibrium, the theory developed in this work, is based on a
far- from -equilibrium isotropic and homogeneous turbulence as an unperturbed
state. The expansion in dimensionless rate of strain leads to a new class of
turbulent models, including the well-known ${\cal K}-{\cal E}$, Reynolds stress
and all possible nonlinear models. The role of interaction of the fluxes in
physical space with the energy flux across the scales, not present in standard
modeling, is demonstrated on example of turbulent channel flow. To close the
system, neither equation for turbulent kinetic energy nor information on
pressure-velocity correlations, contained in the derived coarse-grained kinetic
equation, are needed.
|
nlin.CG physics.flu-dyn
|
in this paper we explore a possibility that all transport turbulent models are contained in a coarsegrained kinetic equation building on a recent work by hchen et al 2004 we account for fluctuations of a single point probability density in turbulence by introducing atwolevel bf cvphasespace separating microscopic bf cequiv c_micro cv and hydrodynamic bf vvv modes unlike traditional kinetic theories with hydrodynamic approximations derived in terms of small deviations from thermodynamic equilibrium the theory developed in this work is based on a far from equilibrium isotropic and homogeneous turbulence as an unperturbed state the expansion in dimensionless rate of strain leads to a new class of turbulent models including the wellknown cal kcal e reynolds stress and all possible nonlinear models the role of interaction of the fluxes in physical space with the energy flux across the scales not present in standard modeling is demonstrated on example of turbulent channel flow to close the system neither equation for turbulent kinetic energy nor information on pressurevelocity correlations contained in the derived coarsegrained kinetic equation are needed
|
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|
[-0.13468640072671914, 0.1455543170322503, -0.06857868718784736, 0.03442495155316063, -0.02105028764209385, -0.07075130650069737, -0.003617893346736944, 0.27365050789748513, -0.26249698933950344, -0.2964488618823072, 0.005578840016739356, -0.24854007227411276, -0.10299624046743956, 0.17576691818553522, -0.01354751898907125, 0.05627308818403372, 0.025434024401853772, -0.01788350004773197, -0.042409979842188986, -0.16624172922388955, 0.30627835151836885, 0.08499962572268276, 0.27679443777387225, 0.018130437514289867, 0.11056724112199316, -0.04998305999284047, -0.035722024172955995, 0.04498939994478268, -0.22211904006795774, 0.06820330938302674, 0.199150765407234, 0.0428401853044539, 0.24271867977628528, -0.4519961756859841, -0.297567602696417, 0.0747626002361527, 0.14098220495209315, 0.11399125060618877, 0.0029720088959736533, -0.23157682152854842, 0.030848465594571342, -0.1870082675270888, -0.08779698243191422, -0.07470659160076878, 0.048338328352804445, 0.04193949016612456, -0.2881469209759691, 0.18031335194313594, 0.0588871649125331, 0.0721996767002396, -0.08018058915839119, -0.09436754827309118, -0.07141173042378626, 0.05049746688780223, 0.02826757636598073, 0.03741660266559636, 0.1287826509079571, -0.16637643552615394, -0.06161212277068042, 0.38587521560230226, -0.0763207309646532, -0.22350492466513208, 0.20025017353344632, -0.12677130770198133, -0.11319534927823169, 0.14361977750208055, 0.16889497304476017, 0.10634933091256074, -0.1648694841295405, 0.11912231381913528, -0.04304483373359057, 0.14287600114343954, 0.019716771997695486, 0.003725350003954846, 0.21066977318814892, 0.1581794441336506, -0.002584445387731458, 0.08662434475128214, -0.0926006717924137, -0.1552785171316341, -0.34476916015156284, -0.12622621064318, -0.19959921872671044, 0.09736939458424215, -0.05847228327420876, -0.16425893467385322, 0.35577754863418726, 0.1762753730791426, 0.16715958168957556, 0.028448000670577192, 0.2639147135602354, 0.12101954661870137, -0.002552981378759669, 0.14437816826475047, 0.27332346652753564, 0.164787171814634, 0.1273788810832166, -0.20532106176332765, 0.03276491447468288, 0.08761448952299002]
|
706.4452
|
What is the Mathematical Structure of Quantum Spacetime?
|
We survey indications from different branches of Physics that the fine scale
structure of spacetime is not adequately described by a manifold. Based on the
hints we accumulate, we propose a new structure, which we call a quantum topos.
In the process of constructing a quantum topos for quantum gravity, we propose
a new, operational approach to the problem of the obervables in quantum
gravity, which leads to a new mathematical point of view on the state sum
models.
|
gr-qc
|
we survey indications from different branches of physics that the fine scale structure of spacetime is not adequately described by a manifold based on the hints we accumulate we propose a new structure which we call a quantum topos in the process of constructing a quantum topos for quantum gravity we propose a new operational approach to the problem of the obervables in quantum gravity which leads to a new mathematical point of view on the state sum models
|
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|
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|
706.4453
|
Systematic search for VHE gamma-ray emission from X-ray bright
high-frequency BL Lac objects
|
All but three (M87, BL Lac and 3C 279) extragalactic sources detected so far
at very high energy (VHE) gamma-rays belong to the class of high-frequency
peaked BL Lac (HBL) objects. This suggested to us a systematic scan of
candidate sources with the MAGIC telescope, based on the compilation of X-ray
blazars by Donato et al. (2001). The observations took place from December 2004
to March 2006 and cover sources on the northern sky visible under small zenith
distances zd < 30 degrees at culmination. The sensitivity of the search was
planned for detecting X-ray bright F(1 keV) > 2 uJy) sources emitting at least
the same energy flux at 200 GeV as at 1 keV. In order to avoid strong gamma-ray
attenuation close to the energy threshold, the redshift of the sources was
constrained to values z<0.3. Of the fourteen sources observed, 1ES 1218+304 and
1ES 2344+514 have been detected in addition to the known bright TeV blazars Mrk
421 and Mrk 501. A marginal excess of 3.5 sigma from the position of 1ES
1011+496 was observed and has been confirmed as a source of VHE gamma-rays by a
second MAGIC observation triggered by a high optical state (Albert et al.
2007). For the remaining sources, we present here the 99% confidence level
upper limits on the integral flux above ~200 GeV. We characterize the sample of
HBLs (including all HBLs detected at VHE so far) by looking for correlations
between their multi-frequency spectral indices determined from simultaneous
optical, archival X-ray, and radio luminosities, finding that the VHE emitting
HBLs do not seem to constitute a unique subclass. The absorption corrected
gamma-ray luminosities at 200 GeV of the HBLs are generally not higher than
their X-ray luminosities at 1 keV.
|
astro-ph
|
all but three m87 bl lac and 3c 279 extragalactic sources detected so far at very high energy vhe gammarays belong to the class of highfrequency peaked bl lac hbl objects this suggested to us a systematic scan of candidate sources with the magic telescope based on the compilation of xray blazars by donato et al 2001 the observations took place from december 2004 to march 2006 and cover sources on the northern sky visible under small zenith distances zd 30 degrees at culmination the sensitivity of the search was planned for detecting xray bright f1 kev 2 ujy sources emitting at least the same energy flux at 200 gev as at 1 kev in order to avoid strong gammaray attenuation close to the energy threshold the redshift of the sources was constrained to values z03 of the fourteen sources observed 1es 1218304 and 1es 2344514 have been detected in addition to the known bright tev blazars mrk 421 and mrk 501 a marginal excess of 35 sigma from the position of 1es 1011496 was observed and has been confirmed as a source of vhe gammarays by a second magic observation triggered by a high optical state albert et al 2007 for the remaining sources we present here the 99 confidence level upper limits on the integral flux above 200 gev we characterize the sample of hbls including all hbls detected at vhe so far by looking for correlations between their multifrequency spectral indices determined from simultaneous optical archival xray and radio luminosities finding that the vhe emitting hbls do not seem to constitute a unique subclass the absorption corrected gammaray luminosities at 200 gev of the hbls are generally not higher than their xray luminosities at 1 kev
|
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|
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|
706.4454
|
Synchronization in networks of networks: the onset of coherent
collective behavior in systems of interacting populations of heterogeneous
oscillators
|
The onset of synchronization in networks of networks is investigated.
Specifically, we consider networks of interacting phase oscillators in which
the set of oscillators is composed of several distinct populations. The
oscillators in a given population are heterogeneous in that their natural
frequencies are drawn from a given distribution, and each population has its
own such distribution. The coupling among the oscillators is global, however,
we permit the coupling strengths between the members of different populations
to be separately specified. We determine the critical condition for the onset
of coherent collective behavior, and develop the illustrative case in which the
oscillator frequencies are drawn from a set of (possibly different)
Cauchy-Lorentz distributions. One motivation is drawn from neurobiology, in
which the collective dynamics of several interacting populations of oscillators
(such as excitatory and inhibitory neurons and glia) are of interest.
|
math.DS
|
the onset of synchronization in networks of networks is investigated specifically we consider networks of interacting phase oscillators in which the set of oscillators is composed of several distinct populations the oscillators in a given population are heterogeneous in that their natural frequencies are drawn from a given distribution and each population has its own such distribution the coupling among the oscillators is global however we permit the coupling strengths between the members of different populations to be separately specified we determine the critical condition for the onset of coherent collective behavior and develop the illustrative case in which the oscillator frequencies are drawn from a set of possibly different cauchylorentz distributions one motivation is drawn from neurobiology in which the collective dynamics of several interacting populations of oscillators such as excitatory and inhibitory neurons and glia are of interest
|
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|
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|
706.4455
|
Anomalous metallic state of Cu$_{0.07}$TiSe$_2$: an optical spectroscopy
study
|
We report an optical spectroscopy study on the newly discovered
superconductor Cu$_{0.07}$TiSe$_2$. Consistent with the development from a
semimetal or semiconductor with a very small indirect energy gap upon doping
TiSe$_2$, it is found that the compound has a low carrier density. Most
remarkably, the study reveals a substantial shift of the "screened" plasma edge
in reflectance towards high energy with decreasing temperature. This
phenomenon, rarely seen in metals, indicates either a sizeable increase of the
conducting carrier concentration or/and a decrease of the effective mass of
carriers with reducing temperature. We attribute the shift primarily to the
later effect.
|
cond-mat.supr-con cond-mat.str-el
|
we report an optical spectroscopy study on the newly discovered superconductor cu_007tise_2 consistent with the development from a semimetal or semiconductor with a very small indirect energy gap upon doping tise_2 it is found that the compound has a low carrier density most remarkably the study reveals a substantial shift of the screened plasma edge in reflectance towards high energy with decreasing temperature this phenomenon rarely seen in metals indicates either a sizeable increase of the conducting carrier concentration orand a decrease of the effective mass of carriers with reducing temperature we attribute the shift primarily to the later effect
|
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|
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|
706.4456
|
Heavy-Quark Kinetics in the QGP at LHC
|
We present predictions for the nuclear modification factor and elliptic flow
of D and B mesons, as well as of their decay electrons, in semicentral Pb-Pb
collisions at the LHC. Heavy quarks are propagated in a Quark-Gluon Plasma
using a relativistic Langevin simulation with drag and diffusion coefficients
from elastic interactions with light anti-/quarks and gluons, including
non-perturbative resonance scattering. Hadronization at T_c is performed within
a combined coalescence-fragmentation scheme.
|
hep-ph nucl-ex nucl-th
|
we present predictions for the nuclear modification factor and elliptic flow of d and b mesons as well as of their decay electrons in semicentral pbpb collisions at the lhc heavy quarks are propagated in a quarkgluon plasma using a relativistic langevin simulation with drag and diffusion coefficients from elastic interactions with light antiquarks and gluons including nonperturbative resonance scattering hadronization at t_c is performed within a combined coalescencefragmentation scheme
|
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|
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|
706.4457
|
Dissipation Scale Fluctuations and Chemical Reaction Rates in Turbulent
Flows
|
Small separation between reactants, not exceeding $10^{-8}-10^{-7}cm$, is the
necessary condition for various chemical reactions. It is shown that random
advection and stretching by turbulence leads to formation of scalar-enriched
sheets of {\it strongly fluctuating thickness} $\eta_{c}$. The molecular-level
mixing is achieved by diffusion across these sheets (interfaces) separating the
reactants. Since diffusion time scale is $\tau_{d}\propto \eta_{c}^{2}$, the
knowledge of probability density $Q(\eta_{c},Re)$ is crucial for evaluation of
chemical reaction rates. In this paper we derive the probability density
$Q(\eta_{c},Re,Sc)$ and predict a transition in the reaction rate behavior from
${\cal R}\propto \sqrt{Re}$ ($Re\leq 10^{4}$) to the high-Re asymptotics ${\cal
R}\propto Re^{0}$. The theory leads to an approximate universality of
transitional Reynolds number $Re_{tr}\approx 10^{4}$. It is also shown that if
chemical reaction involves short-lived reactants, very strong anomalous
fluctuations of the length-scale $\eta_{c}$ may lead to non-negligibly small
reaction rates.
|
nlin.CD astro-ph physics.flu-dyn
|
small separation between reactants not exceeding 108107cm is the necessary condition for various chemical reactions it is shown that random advection and stretching by turbulence leads to formation of scalarenriched sheets of it strongly fluctuating thickness eta_c the molecularlevel mixing is achieved by diffusion across these sheets interfaces separating the reactants since diffusion time scale is tau_dpropto eta_c2 the knowledge of probability density qeta_cre is crucial for evaluation of chemical reaction rates in this paper we derive the probability density qeta_cresc and predict a transition in the reaction rate behavior from cal rpropto sqrtre releq 104 to the highre asymptotics cal rpropto re0 the theory leads to an approximate universality of transitional reynolds number re_trapprox 104 it is also shown that if chemical reaction involves shortlived reactants very strong anomalous fluctuations of the lengthscale eta_c may lead to nonnegligibly small reaction rates
|
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|
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|
706.4458
|
The Popescu-Gabriel theorem for triangulated categories
|
The Popescu-Gabriel theorem states that each Grothendieck abelian category is
a localization of a module category. In this paper, we prove an analogue where
Grothendieck abelian categories are replaced by triangulated categories which
are well generated (in the sense of Neeman) and algebraic (in the sense of
Keller). The role of module categories is played by derived categories of small
differential graded categories. An analogous result for topological
triangulated categories has recently been obtained by A. Heider.
|
math.KT
|
the popescugabriel theorem states that each grothendieck abelian category is a localization of a module category in this paper we prove an analogue where grothendieck abelian categories are replaced by triangulated categories which are well generated in the sense of neeman and algebraic in the sense of keller the role of module categories is played by derived categories of small differential graded categories an analogous result for topological triangulated categories has recently been obtained by a heider
|
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|
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|
706.4459
|
A note on the stability for Kawahara-KdV type equations
|
In this paper we establish the nonlinear stability of solitary traveling-wave
solutions for the Kawahara-KdV equation $$u_t+uu_x+u_{xxx}-\gamma_1
u_{xxxxx}=0,$$ and the modified Kawahara-KdV equation
$$u_t+3u^2u_x+u_{xxx}-\gamma_2 u_{xxxxx}=0,$$ where $\gamma_i\in\mathbb{R}$ is
a positive number when $i=1,2$. The main approach used to determine the
stability of solitary traveling-waves will be the theory developed by Albert
|
math.AP
|
in this paper we establish the nonlinear stability of solitary travelingwave solutions for the kawaharakdv equation u_tuu_xu_xxxgamma_1 u_xxxxx0 and the modified kawaharakdv equation u_t3u2u_xu_xxxgamma_2 u_xxxxx0 where gamma_iinmathbbr is a positive number when i12 the main approach used to determine the stability of solitary travelingwaves will be the theory developed by albert
|
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|
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|
706.446
|
Counterterms in Dimensionally Continued AdS Gravity
|
We revise two regularization mechanisms for Lovelock gravity with AdS
asymptotics. The first one corresponds to the Dirichlet counterterm method,
where local functionals of the boundary metric are added to the bulk action on
top of a Gibbons-Hawking-Myers term that defines the Dirichlet problem in
gravity. The generalized Gibbons-Hawking term can be found in any Lovelock
theory following the Myers' procedure to achieve a well-posed action principle
for a Dirichlet boundary condition on the metric, which is proved to be
equivalent to the Hamiltonian formulation for a radial foliation of spacetime.
In turn, a closed expression for the Dirichlet counterterms does not exist for
a generic Lovelock gravity. The second method supplements the bulk action with
boundary terms which depend on the extrinsic curvature (Kounterterms), and
whose explicit form is independent of the particular theory considered.
In this paper, we use Dimensionally Continued AdS Gravity (Chern-Simons-AdS
in odd and Born-Infeld-AdS in even dimensions) as a toy model to perform the
first explicit comparison between both regularization prescriptions. This can
be done thanks to the fact that, in this theory, the Dirichlet counterterms can
be readily integrated out from the divergent part of the Dirichlet variation of
the action.
The agreement between both procedures at the level of the boundary terms
suggests the existence of a general property of any Lovelock-AdS gravity:
intrinsic counterterms are generated as the difference between the Kounterterm
series and the corresponding Gibbons-Hawking-Myers term.
|
hep-th gr-qc
|
we revise two regularization mechanisms for lovelock gravity with ads asymptotics the first one corresponds to the dirichlet counterterm method where local functionals of the boundary metric are added to the bulk action on top of a gibbonshawkingmyers term that defines the dirichlet problem in gravity the generalized gibbonshawking term can be found in any lovelock theory following the myers procedure to achieve a wellposed action principle for a dirichlet boundary condition on the metric which is proved to be equivalent to the hamiltonian formulation for a radial foliation of spacetime in turn a closed expression for the dirichlet counterterms does not exist for a generic lovelock gravity the second method supplements the bulk action with boundary terms which depend on the extrinsic curvature kounterterms and whose explicit form is independent of the particular theory considered in this paper we use dimensionally continued ads gravity chernsimonsads in odd and borninfeldads in even dimensions as a toy model to perform the first explicit comparison between both regularization prescriptions this can be done thanks to the fact that in this theory the dirichlet counterterms can be readily integrated out from the divergent part of the dirichlet variation of the action the agreement between both procedures at the level of the boundary terms suggests the existence of a general property of any lovelockads gravity intrinsic counterterms are generated as the difference between the kounterterm series and the corresponding gibbonshawkingmyers term
|
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|
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|
706.4461
|
The Infrared Properties of Hickson Compact Groups
|
Compact groups of galaxies provide a unique environment to study the
mechanisms by which star formation occurs amid continuous gravitational
encounters. We present 2MASS (JHK), Spitzer IRAC (3.5-8 micron) and MIPS (24
micron) observations of a sample of twelve Hickson Compact Groups (HCGs 2, 7,
16, 19, 22, 31, 42, 48, 59, 61, 62, and 90) that includes a total of 45
galaxies. The near-infrared colors of the sample galaxies are largely
consistent with being dominated by slightly reddened normal stellar
populations. Galaxies that have the most significant PAH and/or hot dust
emission (as inferred from excess 8 micron flux) also tend to have larger
amounts of extinction and/or K-band excess and stronger 24 micron emission, all
of which suggest ongoing star formation activity. We separate the twelve HCGs
in our sample into three types based on the ratio of the group HI mass to
dynamical mass. We find evidence that galaxies in the most gas-rich groups tend
to be the most actively star forming. Galaxies in the most gas-poor groups tend
to be tightly clustered around a narrow range in colors consistent with the
integrated light from a normal stellar population. We interpret these trends as
indicating that galaxies in gas-rich groups experience star formation and/or
nuclear actively until their neutral gas consumed, stripped, or ionized. The
galaxies in this sample exhibit a ``gap'' between gas-rich and gas-poor groups
in infrared color space that is sparsely populated and not seen in the Spitzer
First Look Survey sample. This gap may suggest a rapid evolution of galaxy
properties in response to dynamical effects. These results suggest that the
global properties of the groups and the local properties of the galaxies are
connected.
|
astro-ph
|
compact groups of galaxies provide a unique environment to study the mechanisms by which star formation occurs amid continuous gravitational encounters we present 2mass jhk spitzer irac 358 micron and mips 24 micron observations of a sample of twelve hickson compact groups hcgs 2 7 16 19 22 31 42 48 59 61 62 and 90 that includes a total of 45 galaxies the nearinfrared colors of the sample galaxies are largely consistent with being dominated by slightly reddened normal stellar populations galaxies that have the most significant pah andor hot dust emission as inferred from excess 8 micron flux also tend to have larger amounts of extinction andor kband excess and stronger 24 micron emission all of which suggest ongoing star formation activity we separate the twelve hcgs in our sample into three types based on the ratio of the group hi mass to dynamical mass we find evidence that galaxies in the most gasrich groups tend to be the most actively star forming galaxies in the most gaspoor groups tend to be tightly clustered around a narrow range in colors consistent with the integrated light from a normal stellar population we interpret these trends as indicating that galaxies in gasrich groups experience star formation andor nuclear actively until their neutral gas consumed stripped or ionized the galaxies in this sample exhibit a gap between gasrich and gaspoor groups in infrared color space that is sparsely populated and not seen in the spitzer first look survey sample this gap may suggest a rapid evolution of galaxy properties in response to dynamical effects these results suggest that the global properties of the groups and the local properties of the galaxies are connected
|
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|
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|
706.4462
|
Disorder induced transition into a one-dimensional Wigner glass
|
The destruction of quasi-long range crystalline order as a consequence of
strong disorder effects is shown to accompany the strict localization of all
classical plasma modes of one-dimensional Wigner crystals at T=0. We construct
a phase diagram that relates the structural phase properties of Wigner crystals
to a plasmon delocalization transition recently reported. Deep inside the
strictly localized phase of the strong disorder regime, we observe
``glass-like'' behavior. However, well into the critical phase with a plasmon
mobility edge, the system retains its crystalline composition. We predict that
a transition between the two phases occurs at a critical value of the relative
disorder strength. This transition has an experimental signature in the AC
conductivity as a local maximum of the largest spectral amplitude as a function
of the relative disorder strength.
|
cond-mat.dis-nn cond-mat.str-el
|
the destruction of quasilong range crystalline order as a consequence of strong disorder effects is shown to accompany the strict localization of all classical plasma modes of onedimensional wigner crystals at t0 we construct a phase diagram that relates the structural phase properties of wigner crystals to a plasmon delocalization transition recently reported deep inside the strictly localized phase of the strong disorder regime we observe glasslike behavior however well into the critical phase with a plasmon mobility edge the system retains its crystalline composition we predict that a transition between the two phases occurs at a critical value of the relative disorder strength this transition has an experimental signature in the ac conductivity as a local maximum of the largest spectral amplitude as a function of the relative disorder strength
|
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|
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|
706.4463
|
The Nonlinear Evolution of Instabilities Driven by Magnetic Buoyancy: A
New Mechanism for the Formation of Coherent Magnetic Structures
|
Motivated by the problem of the formation of active regions from a
deep-seated solar magnetic field, we consider the nonlinear three-dimensional
evolution of magnetic buoyancy instabilities resulting from a smoothly
stratified horizontal magnetic field. By exploring the case for which the
instability is continuously driven we have identified a new mechanism for the
formation of concentrations of magnetic flux.
|
astro-ph
|
motivated by the problem of the formation of active regions from a deepseated solar magnetic field we consider the nonlinear threedimensional evolution of magnetic buoyancy instabilities resulting from a smoothly stratified horizontal magnetic field by exploring the case for which the instability is continuously driven we have identified a new mechanism for the formation of concentrations of magnetic flux
|
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|
[-0.1726655152042286, 0.23627810227542612, 0.00828525683668963, 0.05118407646659762, -0.050588640652723234, -0.00972678283450462, 0.004831453753729998, 0.3099192107506728, -0.28767872390226795, -0.34569492011125813, 0.07607715035457227, -0.1661058634014453, -0.12675159117522633, 0.21759647209102573, 0.03200932094922005, -0.04591220030087536, -0.03203047114282341, -0.013019702128939709, -0.013842525110595812, -0.13771557281093705, 0.38460272866285455, 0.050181095014815616, 0.24068509061205184, -0.01946513293216289, 0.05860598296937296, -0.08406590043677617, 0.002115681199199062, 0.10054747264642837, -0.17426954158897495, 0.051182427299524644, 0.13421786746988862, 0.034742090503795675, 0.29030425669783255, -0.473777995050206, -0.306601266108327, 0.046872936757439275, 0.16840383311796744, 0.09639463848947405, -0.14894903170229015, -0.25792677300761185, 0.044450102220052634, -0.1062297711259354, -0.1416462759282124, 0.00485439193277162, -0.010998575241794274, 0.05915433881899058, -0.3287305650695906, 0.10759239576725384, 0.07306287671297283, 0.10879696493621095, -0.16713494087679912, -0.00699407639676484, -0.10420279264828916, 0.09140522021137304, 0.10399595069130725, 0.08571692248332803, 0.18796224089465657, -0.18732459183340355, -0.07264023345216351, 0.33018806605142054, -0.040174881690892124, -0.12170763007538804, 0.17671750526938398, -0.1808155706404882, -0.0979813351374814, 0.19864805126404864, 0.19441014321489355, 0.15148655893438953, -0.11637377814721253, 0.0642407714562901, -0.03266879506567019, 0.099447160095008, 0.022783888472338854, -0.052695525731196846, 0.3329717196461003, 0.2361500788109093, 0.060393912705861155, 0.17894631062271232, -0.153223619772658, -0.0760639451317868, -0.2416908326479843, -0.12448934362254153, -0.0888074677816387, 0.05774668701214053, -0.04092133848659568, -0.21615269196898504, 0.41629562981553, 0.13914026174362812, 0.18327948918281975, -0.07550835440337847, 0.2762598926990719, 0.10694973495338995, 0.0665527839624023, 0.10676837067703827, 0.3045717623653048, 0.20865320213044347, 0.15107473431123516, -0.2832808159291744, 0.0210133491131335, 0.07771355104711601]
|
706.4464
|
The Persistence of High-Frequency Spin Fluctuations in Overdoped
La$_{2-x}$Sr$_{x}$CuO$_{4}$ ($x$=0.22)
|
We report a detailed inelastic neutron scattering study of the collective
magnetic excitations of overdoped superconducting La1.78Sr0.22CuO4 for the
energy range 0-160 meV. Our measurements show that overdoping suppresses the
strong response present for optimally doped La2-xSrxCuO4 which is peaked near
50 meV. The remaining response is peaked at incommensurate wavevectors for all
energies investigated. We observe a strong high-frequency magnetic response for
E >= 80 meV suggesting that significant antiferromagnetic exchange couplings
persist well into the overdoped part of the cuprate phase diagram.
|
cond-mat.supr-con cond-mat.str-el
|
we report a detailed inelastic neutron scattering study of the collective magnetic excitations of overdoped superconducting la178sr022cuo4 for the energy range 0160 mev our measurements show that overdoping suppresses the strong response present for optimally doped la2xsrxcuo4 which is peaked near 50 mev the remaining response is peaked at incommensurate wavevectors for all energies investigated we observe a strong highfrequency magnetic response for e 80 mev suggesting that significant antiferromagnetic exchange couplings persist well into the overdoped part of the cuprate phase diagram
|
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|
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|
706.4465
|
Electric Flux Tube in Magnetic Plasma
|
In this paper we study a methodical problem related to the magnetic scenario
recently suggested and initiated by the authors \cite{Liao_ES_mono} to
understand the strongly coupled quark-gluon plasma (sQGP): the electric flux
tube in monopole plasma. A macroscopic approach, interpolating between Bose
condensed (dual superconductor) and classical gas medium is developed first.
Then we work out a microscopic approach based on detailed quantum mechanical
calculation of the monopole scattering on electric flux tube, evaluating
induced currents for all partial waves. As expected, the flux tube looses its
stability when particles can penetrate it: we make this condition precise by
calculating the critical value for the product of the flux tube size times the
particle momentum, above which the flux tube dissolves. Lattice static
potentials indicate that flux tubes seem to dissolve at $T>T_{dissolution}
\approx 1.3 T_c$. Using our criterion one gets an estimate of the magnetic
density $n\approx 4.4 \sim 6.6 fm^{-3}$ at this temperature.
|
hep-ph
|
in this paper we study a methodical problem related to the magnetic scenario recently suggested and initiated by the authors citeliao_es_mono to understand the strongly coupled quarkgluon plasma sqgp the electric flux tube in monopole plasma a macroscopic approach interpolating between bose condensed dual superconductor and classical gas medium is developed first then we work out a microscopic approach based on detailed quantum mechanical calculation of the monopole scattering on electric flux tube evaluating induced currents for all partial waves as expected the flux tube looses its stability when particles can penetrate it we make this condition precise by calculating the critical value for the product of the flux tube size times the particle momentum above which the flux tube dissolves lattice static potentials indicate that flux tubes seem to dissolve at tt_dissolution approx 13 t_c using our criterion one gets an estimate of the magnetic density napprox 44 sim 66 fm3 at this temperature
|
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|
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|
706.4466
|
Flux enhancement and multistability induced by time delays in a feedback
controlled flashing ratchet
|
Feedback controlled ratchets are thermal rectifiers that use information on
the state of the system to operate. We study the effects of time delays in the
feedback for a protocol that performs an instantaneous maximization of the
center-of-mass velocity in the many particle case. For small delays the
center-of-mass velocity decreases for increasing delays (although not as fast
as in the few particle case). However, for large delays we find the surprising
result that the presence of a delay can improve the flux performance of the
ratchet. In fact, the maximum flux obtained with the optimal periodic protocol
is attained. This implies that the delayed feedback protocol considered can
perform better than its non-delayed counterpart. The improvement of the flux
observed in the presence of large delays is the result of the emergence of a
new dynamical regime where the presence of the delayed feedback stabilizes
quasiperiodic solutions that resemble the solutions obtained in a certain
closed-loop protocol with thresholds. In addition, in this new regime the
system presents multistability, i.e. several quasiperiodic solutions can be
stable for a fixed time delay.
|
cond-mat.stat-mech
|
feedback controlled ratchets are thermal rectifiers that use information on the state of the system to operate we study the effects of time delays in the feedback for a protocol that performs an instantaneous maximization of the centerofmass velocity in the many particle case for small delays the centerofmass velocity decreases for increasing delays although not as fast as in the few particle case however for large delays we find the surprising result that the presence of a delay can improve the flux performance of the ratchet in fact the maximum flux obtained with the optimal periodic protocol is attained this implies that the delayed feedback protocol considered can perform better than its nondelayed counterpart the improvement of the flux observed in the presence of large delays is the result of the emergence of a new dynamical regime where the presence of the delayed feedback stabilizes quasiperiodic solutions that resemble the solutions obtained in a certain closedloop protocol with thresholds in addition in this new regime the system presents multistability ie several quasiperiodic solutions can be stable for a fixed time delay
|
[['feedback', 'controlled', 'ratchets', 'are', 'thermal', 'rectifiers', 'that', 'use', 'information', 'on', 'the', 'state', 'of', 'the', 'system', 'to', 'operate', 'we', 'study', 'the', 'effects', 'of', 'time', 'delays', 'in', 'the', 'feedback', 'for', 'a', 'protocol', 'that', 'performs', 'an', 'instantaneous', 'maximization', 'of', 'the', 'centerofmass', 'velocity', 'in', 'the', 'many', 'particle', 'case', 'for', 'small', 'delays', 'the', 'centerofmass', 'velocity', 'decreases', 'for', 'increasing', 'delays', 'although', 'not', 'as', 'fast', 'as', 'in', 'the', 'few', 'particle', 'case', 'however', 'for', 'large', 'delays', 'we', 'find', 'the', 'surprising', 'result', 'that', 'the', 'presence', 'of', 'a', 'delay', 'can', 'improve', 'the', 'flux', 'performance', 'of', 'the', 'ratchet', 'in', 'fact', 'the', 'maximum', 'flux', 'obtained', 'with', 'the', 'optimal', 'periodic', 'protocol', 'is', 'attained', 'this', 'implies', 'that', 'the', 'delayed', 'feedback', 'protocol', 'considered', 'can', 'perform', 'better', 'than', 'its', 'nondelayed', 'counterpart', 'the', 'improvement', 'of', 'the', 'flux', 'observed', 'in', 'the', 'presence', 'of', 'large', 'delays', 'is', 'the', 'result', 'of', 'the', 'emergence', 'of', 'a', 'new', 'dynamical', 'regime', 'where', 'the', 'presence', 'of', 'the', 'delayed', 'feedback', 'stabilizes', 'quasiperiodic', 'solutions', 'that', 'resemble', 'the', 'solutions', 'obtained', 'in', 'a', 'certain', 'closedloop', 'protocol', 'with', 'thresholds', 'in', 'addition', 'in', 'this', 'new', 'regime', 'the', 'system', 'presents', 'multistability', 'ie', 'several', 'quasiperiodic', 'solutions', 'can', 'be', 'stable', 'for', 'a', 'fixed', 'time', 'delay']]
|
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|
706.4467
|
Surface Brightness Fluctuations from archival ACS images: a stellar
population and distance study
|
We derive Surface Brightness Fluctuations (SBF) and integrated magnitudes in
the V- and I-bands using Advanced Camera for Surveys (ACS) archival data. The
sample includes 14 galaxies covering a wide range of physical properties:
morphology, total absolute magnitude, integrated color. We take advantage of
the latter characteristic of the sample to check existing empirical
calibrations of absolute SBF magnitudes both in the I- and V-passbands.
Additionally, by comparing our SBF and color data with the Teramo-SPoT simple
stellar population models, and other recent sets of population synthesis
models, we discuss the feasibility of stellar population studies based on
fluctuation magnitudes analysis. The main result of this study is that
multiband optical SBF data and integrated colors can be used to significantly
constrain the chemical composition of the dominant stellar system in the
galaxy, but not the age in the case of systems older than 3 Gyr.
SBF color gradients are also detected and analyzed. These SBF gradient data,
together with other available data, point to the existence of mass dependent
metallicity gradients in galaxies, with the more massive objects showing a
non--negligible SBF versus color gradient. The comparison with models suggests
that such gradients imply more metal rich stellar populations in the galaxies'
inner regions with respect to the outer ones.
|
astro-ph
|
we derive surface brightness fluctuations sbf and integrated magnitudes in the v and ibands using advanced camera for surveys acs archival data the sample includes 14 galaxies covering a wide range of physical properties morphology total absolute magnitude integrated color we take advantage of the latter characteristic of the sample to check existing empirical calibrations of absolute sbf magnitudes both in the i and vpassbands additionally by comparing our sbf and color data with the teramospot simple stellar population models and other recent sets of population synthesis models we discuss the feasibility of stellar population studies based on fluctuation magnitudes analysis the main result of this study is that multiband optical sbf data and integrated colors can be used to significantly constrain the chemical composition of the dominant stellar system in the galaxy but not the age in the case of systems older than 3 gyr sbf color gradients are also detected and analyzed these sbf gradient data together with other available data point to the existence of mass dependent metallicity gradients in galaxies with the more massive objects showing a nonnegligible sbf versus color gradient the comparison with models suggests that such gradients imply more metal rich stellar populations in the galaxies inner regions with respect to the outer ones
|
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|
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|
706.4468
|
Experimental Results on |Vcb| and b -> c l nu Transitions
|
A review of recent analyses on semileptonic decays of B mesons into charmed
final states is given. |Vcb| is extracted both by the Babar and the Belle
collaboration from their datasets using inclusively and exclusively
reconstructed final states.
In addition there are recent results on the determination of exclusive
branching fractions to the ground states D and D*, as well as to excited D**
states. Those play an important role in understanding the composition of the
total decay width. They represent also a sizable fraction of the backgrounds
for exclusive analyses and are presented here as well.
|
hep-ex
|
a review of recent analyses on semileptonic decays of b mesons into charmed final states is given vcb is extracted both by the babar and the belle collaboration from their datasets using inclusively and exclusively reconstructed final states in addition there are recent results on the determination of exclusive branching fractions to the ground states d and d as well as to excited d states those play an important role in understanding the composition of the total decay width they represent also a sizable fraction of the backgrounds for exclusive analyses and are presented here as well
|
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|
[-0.05409918155955611, 0.21678372532187495, -0.056150817701151386, 0.0855898302475701, -0.0029910190712622146, -0.08668723094670736, 0.07636681126704267, 0.3097923792821845, -0.17742094265047423, -0.27845438145408313, 0.027715608573605104, -0.38715434152652156, -0.022887894677324702, 0.15329157348395778, 0.08019769985286385, 0.11421481890186246, 0.15776616630634083, 0.026393207812624185, -0.021215572464759892, -0.20014783366554484, 0.2937245707930133, 0.028921539559192265, 0.22659979073196343, 0.116769233411274, -0.04621674892847839, 0.012767428297011815, -0.10444609840285302, -0.01899463316598504, -0.12850056473914648, 0.08894984622620353, 0.2345603336796126, 0.17516083763336243, 0.14649176190501637, -0.3712638562890826, -0.07294394394152404, 0.1067182649570258, 0.18877491259889811, 0.10229792316896077, -0.04465799038682479, -0.38270500417529923, 0.09588789997487954, -0.1540110940305689, -0.06183659020792117, -0.11969528112982966, 0.0811329164839897, -0.042634221729966476, -0.27136059938785956, 0.09231644608386427, -0.020211496474413376, 0.03283466340628328, -0.059797680946355014, -0.29473701689737974, -0.06423442434884377, 0.1349692721995189, 0.08168984650509413, 0.08987147289990764, 0.16330503207660213, -0.17153453532385535, -0.1982110440923074, 0.3600000789408217, -0.048353171465707195, -0.18664060138434785, 0.1844129046003968, -0.18418240111762868, -0.14702267966895682, 0.10180628466775123, 0.25380851660576675, 0.07579574159816983, -0.14054130651440816, 0.0698379796243167, -0.062360246512155555, 0.134153906001527, 0.055999777250990423, 0.12777527571972652, 0.17659621998744526, 0.18512861532418384, -0.06078876153153089, 0.07347376749025102, -0.0483078649987649, -0.06293370644321915, -0.3781717258167079, -0.13204359890144204, -0.11819326289036532, 0.07860947174251742, 0.026819171677415557, -0.10822738456952664, 0.38752302168340413, -0.0030736619529804004, 0.34550661104011166, -0.03334037698421281, 0.27516775756843925, 0.043345756833585575, 0.04855251391766324, 0.045907120639218264, 0.30359194035997095, 0.20541299787858866, 0.1081899944584836, -0.2344408048504061, 0.11464881842485485, 0.014469223267389173]
|
706.4469
|
Density Matrix Renormalization Group Study of Incompressible Fractional
Quantum Hall States
|
We develop the Density Matrix Renormalization Group (DMRG) technique for
numerically studying incompressible fractional quantum Hall (FQH) states on the
sphere. We calculate accurate estimates for ground state energies and
excitationgaps at FQH filling fractions \nu=1/3 and \nu=5/2 for systems that
are almost twice as large as the largest ever studied by exact diagonalization.
We establish, by carefully comparing with existing numerical results on smaller
systems, that DMRG is a highly effective numerical tool for studying
incompressible FQH states.
|
cond-mat.mes-hall cond-mat.str-el
|
we develop the density matrix renormalization group dmrg technique for numerically studying incompressible fractional quantum hall fqh states on the sphere we calculate accurate estimates for ground state energies and excitationgaps at fqh filling fractions nu13 and nu52 for systems that are almost twice as large as the largest ever studied by exact diagonalization we establish by carefully comparing with existing numerical results on smaller systems that dmrg is a highly effective numerical tool for studying incompressible fqh states
|
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|
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|
706.447
|
Two flavor QCD and confinement - II
|
This paper is part of a program of investigation of the chiral transition in
Nf=2 QCD, started in Phys.Rev.D72:114510,2005. Progress is reported on the
understanding of some possible systematic errors. A direct test of first order
scaling is presented.
|
hep-lat
|
this paper is part of a program of investigation of the chiral transition in nf2 qcd started in physrevd721145102005 progress is reported on the understanding of some possible systematic errors a direct test of first order scaling is presented
|
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|
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|
706.4471
|
Notes on D-branes and dualities in (p,q) minimal superstring theory
|
We study boundary states in (p,q) minimal superstring theory, combining the
explicit form of matter wave functions. Within the modular bootstrap framework,
Cardy states of (p,q) minimal superconformal field theory are completely
determined in both cases of the different supercharge combinations, and the
remaining consistency checks in the super-Liouville case are also performed.
Using these boundary states, we determine the explicit form of FZZT- and
ZZ-brane boundary states both in type 0A and 0B GSO projections. Annulus
mplitudes of FZZT branes are evaluated and principal FZZT branes are
identified. In particular, we found that these principal FZZT branes do not
satisfy Cardy's consistency conditions for each other and play a role of
order/disorder parameters of the Kramers-Wannier duality in spacetime of this
superstring theory.
|
hep-th
|
we study boundary states in pq minimal superstring theory combining the explicit form of matter wave functions within the modular bootstrap framework cardy states of pq minimal superconformal field theory are completely determined in both cases of the different supercharge combinations and the remaining consistency checks in the superliouville case are also performed using these boundary states we determine the explicit form of fzzt and zzbrane boundary states both in type 0a and 0b gso projections annulus mplitudes of fzzt branes are evaluated and principal fzzt branes are identified in particular we found that these principal fzzt branes do not satisfy cardys consistency conditions for each other and play a role of orderdisorder parameters of the kramerswannier duality in spacetime of this superstring theory
|
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|
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|
706.4472
|
Chaos at the border of criticality
|
The present paper points out to a novel scenario for formation of chaotic
attractors in a class of models of excitable cell membranes near an
Andronov-Hopf bifurcation (AHB). The mechanism underlying chaotic dynamics
admits a simple and visual description in terms of the families of
one-dimensional first-return maps, which are constructed using the combination
of asymptotic and numerical techniques. The bifurcation structure of the
continuous system (specifically, the proximity to a degenerate AHB) endows the
Poincare map with distinct qualitative features such as unimodality and the
presence of the boundary layer, where the map is strongly expanding. This
structure of the map in turn explains the bifurcation scenarios in the
continuous system including chaotic mixed-mode oscillations near the border
between the regions of sub- and supercritical AHB. The proposed mechanism
yields the statistical properties of the mixed-mode oscillations in this
regime. The statistics predicted by the analysis of the Poincare map and those
observed in the numerical experiments of the continuous system show a very good
agreement.
|
nlin.CD
|
the present paper points out to a novel scenario for formation of chaotic attractors in a class of models of excitable cell membranes near an andronovhopf bifurcation ahb the mechanism underlying chaotic dynamics admits a simple and visual description in terms of the families of onedimensional firstreturn maps which are constructed using the combination of asymptotic and numerical techniques the bifurcation structure of the continuous system specifically the proximity to a degenerate ahb endows the poincare map with distinct qualitative features such as unimodality and the presence of the boundary layer where the map is strongly expanding this structure of the map in turn explains the bifurcation scenarios in the continuous system including chaotic mixedmode oscillations near the border between the regions of sub and supercritical ahb the proposed mechanism yields the statistical properties of the mixedmode oscillations in this regime the statistics predicted by the analysis of the poincare map and those observed in the numerical experiments of the continuous system show a very good agreement
|
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|
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|
706.4473
|
HyperKahler and quaternionic Kahler manifolds with S^1-symmetries
|
We study relations between quaternionic Riemannian manifolds admitting
different types of symmetries. We show that any hyperKahler manifold admitting
hyperKahler potential and triholomorphic action of S^1 can be constructed from
another hyperKahler manifold (of lower dimention) with an action of S^1 which
fixes one complex structure and rotates the other two and vice versa. We also
study corresponding quaternionic Kahler manifolds equipped with a quaternionic
Kahler action of the circle. In particular we show that any positive
quaternionic Kahler manifold with S^1 symmetry admits a Kahler metric on an
open everywhere dense subset.
|
math.DG math-ph math.MP
|
we study relations between quaternionic riemannian manifolds admitting different types of symmetries we show that any hyperkahler manifold admitting hyperkahler potential and triholomorphic action of s1 can be constructed from another hyperkahler manifold of lower dimention with an action of s1 which fixes one complex structure and rotates the other two and vice versa we also study corresponding quaternionic kahler manifolds equipped with a quaternionic kahler action of the circle in particular we show that any positive quaternionic kahler manifold with s1 symmetry admits a kahler metric on an open everywhere dense subset
|
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|
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|
706.4474
|
F(R) gravity in purely affine formulation
|
The purely affine, metric-affine and purely metric formulation of general
relativity are dynamically equivalent and the relation between them is
analogous to the Legendre relation between the Lagrangian and Hamiltonian
dynamics. We show that one cannot construct a dynamically equivalent, purely
affine Lagrangian from a metric-affine or metric F(R) Lagrangian, nonlinear in
the curvature scalar. Thus the equivalence between the purely affine picture
and the two other formulations does not hold for metric-affine and metric
theories of gravity with a nonlinear dependence on the curvature, i.e. F(R)
gravity does not have a purely affine formulation. We also show that this
equivalence is restored if the metric tensor is conformally transformed from
the Jordan to the Einstein frame, in which F(R) gravity turns into general
relativity with a scalar field. This peculiar behavior of general relativity,
among relativistic theories of gravitation, with respect to purely affine,
metric-affine and purely metric variation could indicate the physicality of the
Einstein frame. On the other hand, it could explain why this theory cannot
interpolate among phenomenological behaviors at different scales.
|
gr-qc math-ph math.MP
|
the purely affine metricaffine and purely metric formulation of general relativity are dynamically equivalent and the relation between them is analogous to the legendre relation between the lagrangian and hamiltonian dynamics we show that one cannot construct a dynamically equivalent purely affine lagrangian from a metricaffine or metric fr lagrangian nonlinear in the curvature scalar thus the equivalence between the purely affine picture and the two other formulations does not hold for metricaffine and metric theories of gravity with a nonlinear dependence on the curvature ie fr gravity does not have a purely affine formulation we also show that this equivalence is restored if the metric tensor is conformally transformed from the jordan to the einstein frame in which fr gravity turns into general relativity with a scalar field this peculiar behavior of general relativity among relativistic theories of gravitation with respect to purely affine metricaffine and purely metric variation could indicate the physicality of the einstein frame on the other hand it could explain why this theory cannot interpolate among phenomenological behaviors at different scales
|
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|
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|
706.4475
|
Black chain of pearls in 5D de Sitter spacetime
|
We analyze some exact chain-shaped black hole solutions in 5-dimensional
spacetime. Unlike usual black string and black ring solutions, the topology of
the horizons of the new solutions are neither $\mathbb{R}\times R^{2}$ nor
$S^1\times S^2$ but rather like several topological spheres concatenating each
other at single points. The shape of the horizon suggests the name \emph{black
chain of pearls} on which each \emph{pearl} is a topological 3-sphere on the
chain. In addition to the usual black hole hairs, the number of pearls can be
viewed as a new hair of the black chain of pearls.
|
hep-th
|
we analyze some exact chainshaped black hole solutions in 5dimensional spacetime unlike usual black string and black ring solutions the topology of the horizons of the new solutions are neither mathbbrtimes r2 nor s1times s2 but rather like several topological spheres concatenating each other at single points the shape of the horizon suggests the name emphblack chain of pearls on which each emphpearl is a topological 3sphere on the chain in addition to the usual black hole hairs the number of pearls can be viewed as a new hair of the black chain of pearls
|
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|
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|
706.4476
|
Perturbative Quantum Corrections to the Supersymmetric CP^1 Kink with
Twisted Mass
|
We present an explicit calculation of the one-loop quantum corrections to the
mass and the two central charges of the kink solution of an N=(2,2)
supersymmetric CP^1 model with twisted mass, using supersymmetry preserving
dimensional regularization adapted to solitons. We find that the quantum
corrections of the mass and one of the central charges are nontrivial (but
saturate the BPS bound), while the other central charge receives no
corrections. The nontrivial central charge correction corresponds to a quantum
anomaly, which in our scheme appears as parity violation in the regulating
extra dimension, and its magnitude is in agreement with exact results obtained
by Dorey on the basis of a massive analog of mirror symmetry from a dual U(1)
gauge theory, confirming also the recent work by Shifman, Vainshtein, and
Zwicky.
|
hep-th
|
we present an explicit calculation of the oneloop quantum corrections to the mass and the two central charges of the kink solution of an n22 supersymmetric cp1 model with twisted mass using supersymmetry preserving dimensional regularization adapted to solitons we find that the quantum corrections of the mass and one of the central charges are nontrivial but saturate the bps bound while the other central charge receives no corrections the nontrivial central charge correction corresponds to a quantum anomaly which in our scheme appears as parity violation in the regulating extra dimension and its magnitude is in agreement with exact results obtained by dorey on the basis of a massive analog of mirror symmetry from a dual u1 gauge theory confirming also the recent work by shifman vainshtein and zwicky
|
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|
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|
706.4477
|
On a Teichmueller functor between the categories of complex tori and the
Effros-Shen algebras
|
A covariant functor from the category of the complex tori to the category of
the Effros-Shen algebras is constructed. The functor maps isomorphic complex
tori to the stably isomorphic Effros-Shen algebras. Our construction is based
on the Teichmueller theory of the Riemann surfaces.
|
math.AG math.OA
|
a covariant functor from the category of the complex tori to the category of the effrosshen algebras is constructed the functor maps isomorphic complex tori to the stably isomorphic effrosshen algebras our construction is based on the teichmueller theory of the riemann surfaces
|
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|
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|
706.4478
|
The Optimal Single Copy Measurement for the Hidden Subgroup Problem
|
The optimization of measurements for the state distinction problem has
recently been applied to the theory of quantum algorithms with considerable
successes, including efficient new quantum algorithms for the non-abelian
hidden subgroup problem. Previous work has identified the optimal single copy
measurement for the hidden subgroup problem over abelian groups as well as for
the non-abelian problem in the setting where the subgroups are restricted to be
all conjugate to each other. Here we describe the optimal single copy
measurement for the hidden subgroup problem when all of the subgroups of the
group are given with equal a priori probability. The optimal measurement is
seen to be a hybrid of the two previously discovered single copy optimal
measurements for the hidden subgroup problem.
|
quant-ph
|
the optimization of measurements for the state distinction problem has recently been applied to the theory of quantum algorithms with considerable successes including efficient new quantum algorithms for the nonabelian hidden subgroup problem previous work has identified the optimal single copy measurement for the hidden subgroup problem over abelian groups as well as for the nonabelian problem in the setting where the subgroups are restricted to be all conjugate to each other here we describe the optimal single copy measurement for the hidden subgroup problem when all of the subgroups of the group are given with equal a priori probability the optimal measurement is seen to be a hybrid of the two previously discovered single copy optimal measurements for the hidden subgroup problem
|
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|
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|
706.4479
|
Experimental characterization of frequency dependent squeezed light
|
We report on the demonstration of broadband squeezed laser beams that show a
frequency dependent orientation of the squeezing ellipse. Carrier frequency as
well as quadrature angle were stably locked to a reference laser beam at
1064nm. This frequency dependent squeezing was characterized in terms of noise
power spectra and contour plots of Wigner functions. The later were measured by
quantum state tomography. Our tomograph allowed a stable lock to a local
oscillator beam for arbitrary quadrature angles with one degree precision.
Frequency dependent orientations of the squeezing ellipse are necessary for
squeezed states of light to provide a broadband sensitivity improvement in
third generation gravitational wave interferometers. We consider the
application of our system to long baseline interferometers such as a future
squeezed light upgraded GEO600 detector.
|
quant-ph
|
we report on the demonstration of broadband squeezed laser beams that show a frequency dependent orientation of the squeezing ellipse carrier frequency as well as quadrature angle were stably locked to a reference laser beam at 1064nm this frequency dependent squeezing was characterized in terms of noise power spectra and contour plots of wigner functions the later were measured by quantum state tomography our tomograph allowed a stable lock to a local oscillator beam for arbitrary quadrature angles with one degree precision frequency dependent orientations of the squeezing ellipse are necessary for squeezed states of light to provide a broadband sensitivity improvement in third generation gravitational wave interferometers we consider the application of our system to long baseline interferometers such as a future squeezed light upgraded geo600 detector
|
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|
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|
706.448
|
Quantum Projection in an Ising Spin Liquid
|
A transverse magnetic field is used to scan the diagonal and off-diagonal
susceptibility of the uniaxial quantum magnet,
$\text{LiHo}_{0.045}\text{Y}_{0.955}\text{F}_4$. Clusters of strongly-coupled
spins act as the primary source for the response functions, which result from a
field-induced quantum projection of the system into a classically forbidden
(meaning non-Ising) regime. Calculations based on spin pairs reproduce only
some features of the data and fail to predict the measured off-diagonal
response, providing evidence of a multi-spin collective state.
|
cond-mat.other cond-mat.dis-nn
|
a transverse magnetic field is used to scan the diagonal and offdiagonal susceptibility of the uniaxial quantum magnet textliho_0045texty_0955textf_4 clusters of stronglycoupled spins act as the primary source for the response functions which result from a fieldinduced quantum projection of the system into a classically forbidden meaning nonising regime calculations based on spin pairs reproduce only some features of the data and fail to predict the measured offdiagonal response providing evidence of a multispin collective state
|
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|
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|
706.4481
|
Isogravity: Toward an Electroweak and Gravitational Unification
|
We present a model that unites the electroweak interaction with general
relativity without specifying a space-time metric. This is made possible by
embedding the kinetic terms for gravity and electroweak theory using one $\SL$
connection variable. The gauge theory is specified without relying on a
space-time metric. We show that once a symmetry breaking mechanism is
implemented that selects a global time-like direction, the electroweak theory
and general relativity emerges with their associated massless degrees of
freedom; the spin 1 vector boson and the spin 2 graviton.
|
hep-th
|
we present a model that unites the electroweak interaction with general relativity without specifying a spacetime metric this is made possible by embedding the kinetic terms for gravity and electroweak theory using one sl connection variable the gauge theory is specified without relying on a spacetime metric we show that once a symmetry breaking mechanism is implemented that selects a global timelike direction the electroweak theory and general relativity emerges with their associated massless degrees of freedom the spin 1 vector boson and the spin 2 graviton
|
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|
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|
706.4482
|
The Evolution of the Cosmic Microwave Background
|
We discuss the time dependence and future of the Cosmic Microwave Background
(CMB) in the context of the standard cosmological model, in which we are now
entering a state of endless accelerated expansion. The mean temperature will
simply decrease until it reaches the effective temperature of the de Sitter
vacuum, while the dipole will oscillate as the Sun orbits the Galaxy. However,
the higher CMB multipoles have a richer phenomenology. The CMB anisotropy power
spectrum will for the most part simply project to smaller scales, as the
comoving distance to last scattering increases, and we derive a scaling
relation that describes this behaviour. However, there will also be a dramatic
increase in the integrated Sachs-Wolfe contribution at low multipoles. We also
discuss the effects of tensor modes and optical depth due to Thomson
scattering. We introduce a correlation function relating the sky maps at two
times and the closely related power spectrum of the difference map. We compute
the evolution both analytically and numerically, and present simulated future
sky maps.
|
astro-ph
|
we discuss the time dependence and future of the cosmic microwave background cmb in the context of the standard cosmological model in which we are now entering a state of endless accelerated expansion the mean temperature will simply decrease until it reaches the effective temperature of the de sitter vacuum while the dipole will oscillate as the sun orbits the galaxy however the higher cmb multipoles have a richer phenomenology the cmb anisotropy power spectrum will for the most part simply project to smaller scales as the comoving distance to last scattering increases and we derive a scaling relation that describes this behaviour however there will also be a dramatic increase in the integrated sachswolfe contribution at low multipoles we also discuss the effects of tensor modes and optical depth due to thomson scattering we introduce a correlation function relating the sky maps at two times and the closely related power spectrum of the difference map we compute the evolution both analytically and numerically and present simulated future sky maps
|
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|
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|
706.4483
|
Epicyclic Oscillations of Fluid Bodies: Newtonian Nonslender Torus
|
We study epicyclic oscillations of fluid tori around black holes (in the
Paczynski-Wiita potential) and derive exact analytic expressions for their
radial and vertical eigenfrequencies nu_r and nu_z to second-order accuracy in
the width of the torus. We prove that pressure effects make the
eigenfrequencies smaller than those for free particles. However, the particular
ratio nu_z/nu_r=3/2, which is important for the theory of high-frequency
quasi-periodic oscillations (QPOs), occurs when the fluid tori epicyclic
frequencies nu_r and nu_z are about 15% higher than the ones corresponding to
free particles. Our results therefore suggest that previous estimates of black
hole spins from QPOs have produced values that are too high.
|
astro-ph
|
we study epicyclic oscillations of fluid tori around black holes in the paczynskiwiita potential and derive exact analytic expressions for their radial and vertical eigenfrequencies nu_r and nu_z to secondorder accuracy in the width of the torus we prove that pressure effects make the eigenfrequencies smaller than those for free particles however the particular ratio nu_znu_r32 which is important for the theory of highfrequency quasiperiodic oscillations qpos occurs when the fluid tori epicyclic frequencies nu_r and nu_z are about 15 higher than the ones corresponding to free particles our results therefore suggest that previous estimates of black hole spins from qpos have produced values that are too high
|
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|
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|
706.4484
|
Spectroscopic Surveys: Present
|
I summarize the current spectroscopic sky surveys and some of the scientific
results, emphasizing the largest sky survey to-date, the Sloan Digital Sky
Survey (SDSS). Techniques used commonly in spectral analyses are discussed,
followed by the present needs and challenges for solving some of the unknown
problems. I discuss how the Virtual Observatory (VO) can help astronomers in
carrying out related research.
|
astro-ph
|
i summarize the current spectroscopic sky surveys and some of the scientific results emphasizing the largest sky survey todate the sloan digital sky survey sdss techniques used commonly in spectral analyses are discussed followed by the present needs and challenges for solving some of the unknown problems i discuss how the virtual observatory vo can help astronomers in carrying out related research
|
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|
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|
707.0001
|
Constants of Geodesic Motion in Higher-Dimensional Black-Hole Spacetimes
|
In [arXiv:hep-th/0611083] we announced the complete integrability of geodesic
motion in the general higher-dimensional rotating black-hole spacetimes. In the
present paper we prove all the necessary steps leading to this conclusion. In
particular, we demonstrate the independence of the constants of motion and the
fact that they Poisson commute. The relation to a different set of constants of
motion constructed in [arXiv:hep-th/0612029] is also briefly discussed.
|
hep-th gr-qc
|
in arxivhepth0611083 we announced the complete integrability of geodesic motion in the general higherdimensional rotating blackhole spacetimes in the present paper we prove all the necessary steps leading to this conclusion in particular we demonstrate the independence of the constants of motion and the fact that they poisson commute the relation to a different set of constants of motion constructed in arxivhepth0612029 is also briefly discussed
|
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|
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|
707.0002
|
Electromagnetic Field in Higher-Dimensional Black-Hole Spacetimes
|
A special test electromagnetic field in the spacetime of the
higher-dimensional generally rotating NUT-(A)dS black hole is found. It is
adjusted to the hidden symmetries of the background represented by the
principal Killing-Yano tensor. Such electromagnetic field generalizes the field
of charged black hole in four dimensions. In higher dimensions, however, the
gravitational back reaction of such a field cannot be consistently solved.
|
hep-th gr-qc
|
a special test electromagnetic field in the spacetime of the higherdimensional generally rotating nutads black hole is found it is adjusted to the hidden symmetries of the background represented by the principal killingyano tensor such electromagnetic field generalizes the field of charged black hole in four dimensions in higher dimensions however the gravitational back reaction of such a field cannot be consistently solved
|
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|
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|
707.0003
|
The Spatial Structure of An Accretion Disk
|
Based on the microlensing variability of the two-image gravitational lens
HE1104-1805 observed between 0.4 and 8 microns, we have measured the size and
wavelength-dependent structure of the quasar accretion disk. Modeled as a power
law in temperature, T proportional to R^-beta, we measure a B-band (0.13
microns in the rest frame) half-light radius of R_{1/2,B} = 6.7 (+6.2 -3.2) x
10^15 cm (68% CL) and a logarithmic slope of beta=0.61 (+0.21 -0.17) for our
standard model with a logarithmic prior on the disk size. Both the scale and
the slope are consistent with simple thin disk models where beta=3/4 and
R_{1/2,B} = 5.9 x 10^15 cm for a Shakura-Sunyaev disk radiating at the
Eddington limit with 10% efficiency. The observed fluxes favor a slightly
shallower slope, beta=0.55 (+0.03 -0.02), and a significantly smaller size for
beta=3/4.
|
astro-ph
|
based on the microlensing variability of the twoimage gravitational lens he11041805 observed between 04 and 8 microns we have measured the size and wavelengthdependent structure of the quasar accretion disk modeled as a power law in temperature t proportional to rbeta we measure a bband 013 microns in the rest frame halflight radius of r_12b 67 62 32 x 1015 cm 68 cl and a logarithmic slope of beta061 021 017 for our standard model with a logarithmic prior on the disk size both the scale and the slope are consistent with simple thin disk models where beta34 and r_12b 59 x 1015 cm for a shakurasunyaev disk radiating at the eddington limit with 10 efficiency the observed fluxes favor a slightly shallower slope beta055 003 002 and a significantly smaller size for beta34
|
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|
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|
707.0004
|
An Algorithm to Construct A Basis for the Module of Logarithmic Vector
Fields
|
We consider logarithmic vector fields parametrized by finite collections of
weighted hyperplanes. For a finite collection of weighted hyperplanes in a
two-dimensional vector space, it is known that the set of such vector fields is
a free module of rank two whose basis elements are homogeneous. We give an
algorithm to construct a homogeneous basis for the module.
|
math.CO
|
we consider logarithmic vector fields parametrized by finite collections of weighted hyperplanes for a finite collection of weighted hyperplanes in a twodimensional vector space it is known that the set of such vector fields is a free module of rank two whose basis elements are homogeneous we give an algorithm to construct a homogeneous basis for the module
|
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|
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|
707.0005
|
Higgs Physics as a Window Beyond the MSSM (BMSSM)
|
We interpret the current experimental limit on the lightest Higgs boson mass
to suggest that if nature is supersymmetric, there are additional interactions
beyond those of the MSSM coming from new degrees of freedom around the TeV
scale. Within an effective field theory analysis, the leading order corrections
to the MSSM are described in terms of only two operators. This provides a
highly constrained description of Beyond MSSM (BMSSM) physics. The scalar Higgs
spectrum as well as the chargino and neutralino spectrum and couplings are
modified in a distinctive way. These operators can be generated by a variety of
microscopic mechanisms.
|
hep-ph
|
we interpret the current experimental limit on the lightest higgs boson mass to suggest that if nature is supersymmetric there are additional interactions beyond those of the mssm coming from new degrees of freedom around the tev scale within an effective field theory analysis the leading order corrections to the mssm are described in terms of only two operators this provides a highly constrained description of beyond mssm bmssm physics the scalar higgs spectrum as well as the chargino and neutralino spectrum and couplings are modified in a distinctive way these operators can be generated by a variety of microscopic mechanisms
|
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|
[-0.10502988145234857, 0.2245712436536514, -0.04452276027284212, 0.17208890395589393, -0.091698723637711, -0.14649761183934268, -0.0037507038634952785, 0.2953196268201354, -0.24384157533416212, -0.3366816710717607, 0.044315821454297785, -0.28305180978011524, -0.06288513842748829, 0.16792763433635863, 0.01727832335803547, 0.03399095817994658, 0.03525308871844617, 0.025611723819286517, -0.039462151480746444, -0.21496379381912475, 0.297499017554824, 0.04419770753610473, 0.14134319296272674, 0.10128129715109152, 0.018153419598273123, 0.0017846234714483271, 0.0007642568042962858, -0.04540185683803393, -0.0906100557212364, 0.13012498210525453, 0.204603640749903, 0.0693365656909081, 0.1309321850612022, -0.3488944374442119, -0.206381230956257, 0.13018320783013754, 0.19600913133403047, 0.1136577872992816, -0.04162268538493663, -0.31842047547792446, 0.0863282889638345, -0.23492132271132846, -0.12392633311487365, -0.12042214944013532, -0.08460074298355802, -0.10619236352752046, -0.2863298861475864, 0.09526625335634926, -0.04566120310100994, 0.02326258261328434, -0.0035204083548102637, -0.1501483887429395, -0.09737402272853299, 0.02902253477898712, 0.1545960117352776, -0.014760871436262485, 0.19163886793787674, -0.2237139329922819, -0.16832867383929245, 0.4392521545881092, -0.10568599649451414, -0.18151015905884677, 0.18940081356996946, -0.1499304662753671, -0.12660849595553067, 0.12372602034581474, 0.1882461620273419, 0.09610304974496715, -0.1852321194595482, 0.22629963371352035, -0.040527025223847955, 0.1727300652551769, 0.022984260654003167, 0.11099812175875695, 0.2945327779075297, 0.18146844197060027, 0.059631010586635606, 0.056303096214761164, -0.022835258823256977, -0.14159720501687267, -0.4540975697264813, -0.08523480428179891, -0.0734918703426524, 0.03617529905894495, -0.08459709359115072, -0.11616597958554578, 0.4442180696192502, 0.16314135305007163, 0.2530124889004349, 0.0007368257674987954, 0.2770692576645034, 0.09674727016515883, 0.11334989694786249, 0.0173391155289984, 0.32893963623791933, 0.1313866092708183, 0.08103239841962068, -0.17725573536146913, -0.04305376458710226, 0.0948006882110961]
|
707.0006
|
Spectroscopic Analysis of H I Absorption Line Systems in 40 HIRES
Quasars
|
We list and analyze H I absorption lines at redshifts 2 < z < 4 with column
density (12 < log(N_HI) < 19) in 40 high-resolutional (FWHM = 8.0 km/s) quasar
spectra obtained with the Keck+HIRES. We de-blend and fit all H I lines within
1,000 km/s of 86 strong H I lines whose column densities are log(N_HI/[cm^-2])
> 15. Unlike most prior studies, we use not only Lya but also all visible
higher Lyman series lines to improve the fitting accuracy. This reveals
components near to higher column density systems that can not be seen in Lya.
We list the Voigt profile fits to the 1339 H I components that we found. We
examined physical properties of H I lines after separating them into several
sub-samples according to their velocity separation from the quasars, their
redshift, column density and the S/N ratio of the spectrum. We found two
interesting trends for lines with 12 < log(N_HI) < 15 which are within 200-1000
km/s of systems with log(N_HI) > 15. First, their column density distribution
becomes steeper, meaning relatively fewer high column density lines, at z <
2.9. Second, their column density distribution also becomes steeper and their
line width becomes broader by about 2-3 km/s when they are within 5,000 km/s of
their quasar.
|
astro-ph
|
we list and analyze h i absorption lines at redshifts 2 z 4 with column density 12 logn_hi 19 in 40 highresolutional fwhm 80 kms quasar spectra obtained with the keckhires we deblend and fit all h i lines within 1000 kms of 86 strong h i lines whose column densities are logn_hicm2 15 unlike most prior studies we use not only lya but also all visible higher lyman series lines to improve the fitting accuracy this reveals components near to higher column density systems that can not be seen in lya we list the voigt profile fits to the 1339 h i components that we found we examined physical properties of h i lines after separating them into several subsamples according to their velocity separation from the quasars their redshift column density and the sn ratio of the spectrum we found two interesting trends for lines with 12 logn_hi 15 which are within 2001000 kms of systems with logn_hi 15 first their column density distribution becomes steeper meaning relatively fewer high column density lines at z 29 second their column density distribution also becomes steeper and their line width becomes broader by about 23 kms when they are within 5000 kms of their quasar
|
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|
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|
707.0007
|
Meta-Stable Dynamical Supersymmetry Breaking Near Points of Enhanced
Symmetry
|
We show that metastable supersymmetry breaking is generic near certain
enhanced symmetry points of gauge theory moduli spaces. Our model consists of
two sectors coupled by a singlet and combines dynamical supersymmetry breaking
with an O'Raifeartaigh mechanism in terms of confined variables. All relevant
mass parameters, including the supersymmetry breaking scale, are generated
dynamically. The metastable vacua appear as a result of a balance between
non-perturbative and perturbative quantum effects along a pseudo-runaway
direction.
|
hep-th hep-ph
|
we show that metastable supersymmetry breaking is generic near certain enhanced symmetry points of gauge theory moduli spaces our model consists of two sectors coupled by a singlet and combines dynamical supersymmetry breaking with an oraifeartaigh mechanism in terms of confined variables all relevant mass parameters including the supersymmetry breaking scale are generated dynamically the metastable vacua appear as a result of a balance between nonperturbative and perturbative quantum effects along a pseudorunaway direction
|
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|
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|
707.0008
|
Reliable Final Computational Results from Faulty Quantum Computation
|
In this paper we extend both standard fault tolerance theory and Kitaev's
model for quantum computation, combining them so as to yield quantitative
results that reveal the interplay between the two. Our analysis establishes a
methodology that allows us to quantitatively determine design parameters for a
quantum computer, the values of which ensure that an overall computation of
interest yields a correct *final result* with some prescribed probability of
success, as opposed to merely ensuring that the desired *final quantum state*
is obtained. As a specific example of the practical application of our
approach, we explicitly calculate the number of levels of error correction
concatenation needed to achieve a correct final result for the overall
computation with some prescribed success probability. Since our methodology
allows one to determine parameters required in order to achieve the correct
final result for the overall quantum computation, as opposed to merely ensuring
that the desired final quantum state is produced, our method enables the
determination of complete quantum computational resource requirements
associated to the actual solution of practical problems.
|
quant-ph
|
in this paper we extend both standard fault tolerance theory and kitaevs model for quantum computation combining them so as to yield quantitative results that reveal the interplay between the two our analysis establishes a methodology that allows us to quantitatively determine design parameters for a quantum computer the values of which ensure that an overall computation of interest yields a correct final result with some prescribed probability of success as opposed to merely ensuring that the desired final quantum state is obtained as a specific example of the practical application of our approach we explicitly calculate the number of levels of error correction concatenation needed to achieve a correct final result for the overall computation with some prescribed success probability since our methodology allows one to determine parameters required in order to achieve the correct final result for the overall quantum computation as opposed to merely ensuring that the desired final quantum state is produced our method enables the determination of complete quantum computational resource requirements associated to the actual solution of practical problems
|
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|
[-0.07204845425007599, 0.03934669259478272, -0.09097260665148496, 0.0511216551284971, -0.04663770725950599, -0.1393048300913402, 0.10171187836410744, 0.31734378754028253, -0.23971049053328378, -0.37282590661730086, 0.06568362986203283, -0.19691399139235727, -0.1423182933085731, 0.22964888095456576, -0.09532562016309905, 0.1377281601960671, 0.10028764137923385, 0.06632676124173616, -0.07988355417602828, -0.2751304292633514, 0.26765174485476956, 0.09093493774666318, 0.30617570025048085, 0.0706274238122361, 0.09690886981519205, 0.012674075585756717, -0.025038366083587917, -0.009264234275157962, -0.1353876095860947, 0.15503243822537896, 0.2749101391807198, 0.15737761850867954, 0.2838253309790577, -0.40309843993080513, -0.18036853705399802, 0.07879388224998755, 0.12184538885518642, 0.1828869643933805, -0.019759621247649194, -0.24466383293271066, 0.12938276839575596, -0.1871440112617399, -0.1506697405608637, -0.12956096519316945, -0.03909933989069291, -0.020936654691717453, -0.2976338901583638, 0.034939573649317025, 0.06794617979288367, -0.013195174336433411, -0.03411990279398326, -0.0942570417933166, 0.0057623702380806205, 0.21716926252735513, 0.015042730951016502, 0.046400050447721566, 0.12072265289723873, -0.1348033320092197, -0.14893431234073692, 0.3841001529166741, -0.021068016015924514, -0.21069589599967004, 0.1710297757054546, -0.07735874047502875, -0.1358555977312582, 0.11661375923880508, 0.14721855914220214, 0.06863181168479579, -0.10350712170225701, 0.0326408302913686, 0.01600151454497661, 0.1886279397351401, 0.02542351012650345, 0.08111126246329929, 0.15461783939839474, 0.14628500573070985, 0.09200564544115748, 0.15255503109656274, -0.04660449665488808, -0.14737855431357666, -0.35338593101395027, -0.20069154523845228, -0.19149305231603128, 0.043251396124916415, -0.078255329146632, -0.17288741910031863, 0.4097340920248202, 0.20240386351286102, 0.20949701696102108, 0.10492720212055637, 0.3206335880394493, 0.11053780741989612, 0.012121160333710057, 0.03389939102211169, 0.23110903616628742, 0.1266417346349252, 0.05181760791689158, -0.23195148834559534, 0.11351630085813148, 0.04471944418336664]
|
707.0009
|
Invariant weighted algebras $L_p^w(G)$
|
The paper deals with weighted spaces $L_p^w(G)$ on a locally compact group G.
If w is a positive measurable function on G then we define the space
$L_p^w(G)$, $p\ge1$, as $L_p^w(G)=\{f:fw\in L_p(G)\}$. We consider weights such
that these weighted spaces are algebras with respect to usual convolution. It
is shown that for p>1 such weights exists on any sigma-compact group. We prove
also a criterion known earlier in special cases: $L_1^w(G)$ is an algebra if
and only if w is submultiplicative. It is proved that invariant algebras
$L_p^w(G)$, $p>1$, have approximate units of standard form, but this may not be
true for a non-invariant algebra.
|
math.FA
|
the paper deals with weighted spaces l_pwg on a locally compact group g if w is a positive measurable function on g then we define the space l_pwg pge1 as l_pwgffwin l_pg we consider weights such that these weighted spaces are algebras with respect to usual convolution it is shown that for p1 such weights exists on any sigmacompact group we prove also a criterion known earlier in special cases l_1wg is an algebra if and only if w is submultiplicative it is proved that invariant algebras l_pwg p1 have approximate units of standard form but this may not be true for a noninvariant algebra
|
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|
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|
707.001
|
Equation-of-state model for shock compression of hot dense matter
|
A quantum equation-of-state model is presented and applied to the calculation
of high-pressure shock Hugoniot curves beyond the asymptotic fourfold density,
close to the maximum compression where quantum effects play a role. An
analytical estimate for the maximum attainable compression is proposed. It
gives a good agreement with the equation-of-state model.
|
physics.plasm-ph
|
a quantum equationofstate model is presented and applied to the calculation of highpressure shock hugoniot curves beyond the asymptotic fourfold density close to the maximum compression where quantum effects play a role an analytical estimate for the maximum attainable compression is proposed it gives a good agreement with the equationofstate model
|
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|
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|
707.0011
|
Calculating the probability of detecting radio signals from alien
civilizations
|
Although it might not be self-evident, it is in fact entirely possible to
calculate the probability of detecting alien radio signals by understanding
what types of extraterrestrial radio emissions can be expected and what
properties these emissions can have. Using the Drake equation as the obvious
starting point, and logically identifying and enumerating constraints of
interstellar radio communications can yield the probability of detecting a
genuine alien radio signal.
|
physics.pop-ph astro-ph
|
although it might not be selfevident it is in fact entirely possible to calculate the probability of detecting alien radio signals by understanding what types of extraterrestrial radio emissions can be expected and what properties these emissions can have using the drake equation as the obvious starting point and logically identifying and enumerating constraints of interstellar radio communications can yield the probability of detecting a genuine alien radio signal
|
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|
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|
707.0012
|
Electron operator at the edge of the 1/3 fractional quantum Hall liquid
|
This study builds upon the work of Palacios and MacDonald (Phys. Rev. Lett.
{\bf 76}, 118 (1996)), wherein they identify the bosonic excitations of Wen's
approach for the edge of the 1/3 fractional quantum Hall state with certain
operators introduced by Stone. Using a quantum Monte Carlo method, we extend to
larger systems containing up to 40 electrons and obtain more accurate
thermodynamic limits for various matrix elements for a short range interaction.
The results are in agreement with those of Palacios and MacDonald for small
systems, but offer further insight into the detailed approach to the
thermodynamic limit. For the short range interaction, the results are
consistent with the chiral Luttinger liquid predictions.We also study
excitations using the Coulomb ground state for up to nine electrons to
ascertain the effect of interactions on the results; in this case our tests of
the chiral Luttinger liquid approach are inconclusive.
|
cond-mat.mes-hall
|
this study builds upon the work of palacios and macdonald phys rev lett bf 76 118 1996 wherein they identify the bosonic excitations of wens approach for the edge of the 13 fractional quantum hall state with certain operators introduced by stone using a quantum monte carlo method we extend to larger systems containing up to 40 electrons and obtain more accurate thermodynamic limits for various matrix elements for a short range interaction the results are in agreement with those of palacios and macdonald for small systems but offer further insight into the detailed approach to the thermodynamic limit for the short range interaction the results are consistent with the chiral luttinger liquid predictionswe also study excitations using the coulomb ground state for up to nine electrons to ascertain the effect of interactions on the results in this case our tests of the chiral luttinger liquid approach are inconclusive
|
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|
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|
707.0013
|
Shell-structure effects on high-pressure Rankine-Hugoniot shock adiabats
|
Rankine-Hugoniot shock adiabats are calculated in the pressure range 1
Mbar-10 Gbar with two atomic-structure models: the atom in a spherical cell and
the atom in a jellium of charges. These quantum self-consistent-field models
include shell effects, which have a strong impact on pressure and shock
velocity along the shock adiabat. Comparisons with experimental data are
presented and quantum effects are interpreted in terms of electronic specific
heat. A simple analytical estimate for the maximum compression is proposed,
depending on initial density, atomic weight and atomic number.
|
physics.plasm-ph physics.atom-ph
|
rankinehugoniot shock adiabats are calculated in the pressure range 1 mbar10 gbar with two atomicstructure models the atom in a spherical cell and the atom in a jellium of charges these quantum selfconsistentfield models include shell effects which have a strong impact on pressure and shock velocity along the shock adiabat comparisons with experimental data are presented and quantum effects are interpreted in terms of electronic specific heat a simple analytical estimate for the maximum compression is proposed depending on initial density atomic weight and atomic number
|
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|
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|
707.0014
|
Testing Gluino Spin with Three-Body Decays
|
We examine the possibility of distinguishing a supersymmetric gluino from a
Kaluza-Klein gluon of universal extra dimensions (UED) at the Large Hadron
Collider (LHC). We focus on the case when all kinematically allowed tree-level
decays of this particle are 3-body decays into two jets and a massive daughter
(typically weak gaugino or Kaluza-Klein weak gauge boson). We show that the
shapes of the dijet invariant mass distributions differ significantly in the
two models, as long as the mass of the decaying particle mA is substantially
larger than the mass of the massive daughter mB. We present a simple analysis
estimating the number of events needed to distinguish between the two models
under idealized conditions. For example, for mA/mB=10, we find the required
number of events to be of order several thousand, which should be available at
the LHC within a few years. This conclusion is confirmed by a parton level
Monte Carlo study which includes the effects of experimental cuts and the
combinatoric background.
|
hep-ph
|
we examine the possibility of distinguishing a supersymmetric gluino from a kaluzaklein gluon of universal extra dimensions ued at the large hadron collider lhc we focus on the case when all kinematically allowed treelevel decays of this particle are 3body decays into two jets and a massive daughter typically weak gaugino or kaluzaklein weak gauge boson we show that the shapes of the dijet invariant mass distributions differ significantly in the two models as long as the mass of the decaying particle ma is substantially larger than the mass of the massive daughter mb we present a simple analysis estimating the number of events needed to distinguish between the two models under idealized conditions for example for mamb10 we find the required number of events to be of order several thousand which should be available at the lhc within a few years this conclusion is confirmed by a parton level monte carlo study which includes the effects of experimental cuts and the combinatoric background
|
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|
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|
707.0015
|
Investigations in Two-Dimensional Quantum Field Theory by the Bootstrap
and TCSA Methods
|
This thesis contains three main parts, which are largely independent. In the
first part we deal with the boundary bootstrap in supersymmetric factorized
scattering theory. We give a description of supersymmetry in the case when the
space is a half-line and present rules for the determination of the
representations in which higher level boundary bound states transform, and for
the determination of the supersymmetric one-particle reflection matrix factors
for the higher level boundary bound states. These rules apply under the
condition that the bulk particles transform in the kink or in the boson-fermion
representation. Examples for the application of these rules to specific models
are also given. In the second part we investigate the problem whether the TCSA
spectrum can be approximated by the spectrum of the original Hamiltonian
operator in which the coefficients of the terms are suitably changed. The
investigation is done in the case of the critical Ising model on a strip with
an external magnetic field on one of the boundaries. Another truncation method
that preserves the solvability of the model is also considered. The results of
perturbative and numerical calculations show that the above approximation is
possible and that the qualitative behaviour of the truncated spectrum as a
function of the coupling constant depends on the truncation method. In the
third part we investigate the phase structure of the two- and three-frequency
sine-Gordon models using the TCSA. In the case of the three-frequency model the
tricritical point, several points of the critical line and a few points of the
line of first order transition are found.
|
hep-th
|
this thesis contains three main parts which are largely independent in the first part we deal with the boundary bootstrap in supersymmetric factorized scattering theory we give a description of supersymmetry in the case when the space is a halfline and present rules for the determination of the representations in which higher level boundary bound states transform and for the determination of the supersymmetric oneparticle reflection matrix factors for the higher level boundary bound states these rules apply under the condition that the bulk particles transform in the kink or in the bosonfermion representation examples for the application of these rules to specific models are also given in the second part we investigate the problem whether the tcsa spectrum can be approximated by the spectrum of the original hamiltonian operator in which the coefficients of the terms are suitably changed the investigation is done in the case of the critical ising model on a strip with an external magnetic field on one of the boundaries another truncation method that preserves the solvability of the model is also considered the results of perturbative and numerical calculations show that the above approximation is possible and that the qualitative behaviour of the truncated spectrum as a function of the coupling constant depends on the truncation method in the third part we investigate the phase structure of the two and threefrequency sinegordon models using the tcsa in the case of the threefrequency model the tricritical point several points of the critical line and a few points of the line of first order transition are found
|
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|
[-0.12127655196820754, 0.10574949144278037, -0.07986027669247198, 0.05680949519204611, -0.028238078477610458, -0.08771663000521704, 0.03842606166086848, 0.32578532321028897, -0.2415494583243811, -0.2574203152680534, 0.12445796620844725, -0.27443213847918985, -0.15248696407895548, 0.15694121288410406, 0.0020926279618879388, 0.04870202103308562, 0.03385412513449702, 0.08048319601778554, -0.08619993982209478, -0.22806846842765666, 0.3772960482664777, 0.015024536059120264, 0.25334707181722327, 0.08003029862924575, 0.05249323171538468, -0.0008599079228309608, 0.0012940415921638866, -0.020157722611862532, -0.11229529100975603, 0.11481529859276453, 0.19087823684153016, 0.05534002110109485, 0.2176223802969031, -0.40248226473586085, -0.19092223240719158, 0.07785641970924705, 0.1438337717054972, 0.11109314798297168, 0.0024507590747970044, -0.26897983937845404, 0.07161537779966133, -0.14037336994647637, -0.15878467424683473, -0.05343908825942754, -0.024232452179990368, -0.013107447082112575, -0.25657460902540113, 0.0759631943711886, 0.07192552360970085, 0.03393699762197207, -0.10431999426292277, -0.10100136138141955, -0.030154032024315835, 0.12437219565283325, 0.06135325934568427, 0.005648623367591308, 0.085111563352661, -0.16812016431791296, -0.102970839122139, 0.3856441379592565, -0.06096105819248676, -0.22609048982336405, 0.150643364358622, -0.17407529548852493, -0.1432298143801076, 0.11045382177043292, 0.12867321534853043, 0.1370574486927197, -0.12202254005301238, 0.13398783173371048, -0.05045747193748709, 0.14942020109162837, 0.037061737811057274, -0.0104071370743472, 0.17137965932577648, 0.13613379090980687, 0.05125680225241173, 0.17083165038892664, -0.06689568392404309, -0.12257394163938011, -0.38061749253607574, -0.1402988832437708, -0.18608531359336927, -0.005831669015146193, -0.09949411017344319, -0.20341602633653702, 0.43885825449686455, 0.1479032107574131, 0.22213409218071403, 0.03094510036972048, 0.26063445234542776, 0.19548455636254317, 0.05130336796699834, 0.03811777997191039, 0.25102624870565543, 0.1300910059701637, 0.06285236971417149, -0.2283222863319735, 0.008091180695941622, 0.12885717800604288]
|
707.0016
|
Abstract polymer models with general pair interactions
|
A convergence criterion of cluster expansion is presented in the case of an
abstract polymer system with general pair interactions (i.e. not necessarily
hard core or repulsive). As a concrete example, the low temperature disordered
phase of the BEG model with infinite range interactions, decaying polynomially
as $1/r^{d+\lambda}$ with $\lambda>0$, is studied.
|
math-ph math.CO math.MP
|
a convergence criterion of cluster expansion is presented in the case of an abstract polymer system with general pair interactions ie not necessarily hard core or repulsive as a concrete example the low temperature disordered phase of the beg model with infinite range interactions decaying polynomially as 1rdlambda with lambda0 is studied
|
[['a', 'convergence', 'criterion', 'of', 'cluster', 'expansion', 'is', 'presented', 'in', 'the', 'case', 'of', 'an', 'abstract', 'polymer', 'system', 'with', 'general', 'pair', 'interactions', 'ie', 'not', 'necessarily', 'hard', 'core', 'or', 'repulsive', 'as', 'a', 'concrete', 'example', 'the', 'low', 'temperature', 'disordered', 'phase', 'of', 'the', 'beg', 'model', 'with', 'infinite', 'range', 'interactions', 'decaying', 'polynomially', 'as', '1rdlambda', 'with', 'lambda0', 'is', 'studied']]
|
[-0.13071060778719246, 0.2016320083699504, -0.05547399470336078, 0.07879392399598717, -0.04241818353058953, -0.2253563753055299, -0.025939122645878325, 0.3638464108876446, -0.2592144601923578, -0.2602968642889869, 0.09448386331353628, -0.28085690720335527, -0.07360279429064807, 0.11876852270763587, 0.06812462245579809, 0.0211759765504622, 0.03871873002864566, 0.10498386373579063, -0.04614543098518077, -0.22449008231142573, 0.2903917954467675, 0.03450106250523936, 0.20621614698685853, 0.08537694831908334, 0.06321505679935559, 0.04741031475200811, 0.08139892267611097, 0.05466175678313947, -0.14100338504010557, 0.008316088869583373, 0.215267142664422, 0.01451987849877161, 0.2574381335985427, -0.36697692161097245, -0.20249764635866763, 0.15963244200775437, 0.20335993199956184, 0.1030617085988542, -0.06201600557987524, -0.26550441603724134, 0.04450655842711236, -0.23788486980358323, -0.18675164907586342, -0.048098295577801764, 0.03595310738127606, 0.04787610230200431, -0.2815207382755391, 0.12713924505035668, 0.12239410509081448, 0.05799901894494599, -0.07683609741484272, -0.05363411891420244, -0.017233492916121203, 0.047884222398530324, 0.01172014887161626, 0.04866631859548244, 0.12072180235283632, -0.13224753051740573, -0.08079250189977899, 0.4092163420190998, -0.05537242293996992, -0.18020338813463846, 0.2625774018028203, -0.11179417322444565, -0.08650670408764306, 0.15366200613332728, 0.14576642627955652, 0.1094099029296023, -0.1207242831953016, 0.11956319531172459, -0.031175407927994635, 0.1950063322689019, 0.003515790107057375, 0.012139643794701746, 0.17451883324732384, 0.21176087766812712, 0.030912907447154615, 0.223618917751546, 0.007095993752134782, -0.1465434648060039, -0.33784296301503974, -0.10296317202714729, -0.20098427872118704, 0.02107513123037814, -0.12281391313116924, -0.26433324534446, 0.2993028161170728, 0.04040333094970122, 0.2099671860170715, 0.0732988453671044, 0.2501704629291506, 0.10776872821060904, 0.01456084843798011, 0.02393602022864655, 0.2017521540469983, 0.15604417950061023, 0.10602393919857693, -0.1546968637289954, 0.044579114682753294, 0.07529626895363133]
|
707.0017
|
A Morse type uniqueness theorem for non-parametric minimizing
hypersurfaces
|
A classical result about minimal geodesics on R^2 with Z^2 periodic metric
that goes back to H.M. Morse asserts that a minimal geodesic that is asymptotic
to a periodic minimal geodesic cannot intersect any periodic minimal geodesic
of the same period. This paper treats a similar theorem for nonparametric
minimizing hypersurfaces without selfintersections -- as were studied by J.
Moser, V. Bangert, P.H. Rabinowitz, E. Stredulinsky and others.
|
math.AP math.DS
|
a classical result about minimal geodesics on r2 with z2 periodic metric that goes back to hm morse asserts that a minimal geodesic that is asymptotic to a periodic minimal geodesic cannot intersect any periodic minimal geodesic of the same period this paper treats a similar theorem for nonparametric minimizing hypersurfaces without selfintersections as were studied by j moser v bangert ph rabinowitz e stredulinsky and others
|
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|
[-0.2161891420802741, 0.10033735412923592, -0.10765119357062365, 0.12263674236166833, -0.11757685930760049, -0.2123043147791455, 0.055413966816015986, 0.302686350281114, -0.2524693680009735, -0.21832527592778206, 0.06938472317371851, -0.3107059015405934, -0.13056767780556164, 0.18138954221312678, -0.22406709170552777, 0.07450499747004082, 0.09137598373718671, 0.0740074041341223, -0.06020253652414835, -0.24770156673934143, 0.2756701557160313, -0.04917513009216359, 0.17607277433549526, 0.04850756114265367, 0.09946836409881822, 0.08265788306885247, 0.0018769035914238653, 0.030530208137942785, -0.2053946778507262, 0.08246215945804741, 0.2022114015226044, 0.05736674486534364, 0.23854950014779816, -0.38636154100410086, -0.2642703374236155, 0.21586574067069747, 0.1316360751472747, 0.029155517080381735, 0.01977245564357058, -0.24375258444516518, 0.14269729060774197, -0.0405714612579279, -0.24469797833780968, -0.004088831175841502, 0.08545797703259472, 0.036318610408412874, -0.17977331801831944, 0.047707337816593365, 0.1833370649047307, 0.10718737037699502, -0.05419364680688995, -0.048232209264064456, -0.11016697820220421, 0.050940651335378194, 0.10229139339609711, 0.14235268474848412, 0.08388160960053775, 0.04790145609486125, -0.10563786933198571, 0.3484349961378681, -0.1568957091962446, -0.25028529462974464, 0.166501191444695, -0.11321533520692098, -0.11743831682477647, 0.1391103264959112, 0.0775893290819072, 0.15435695431348104, -0.15590983840511807, 0.22980595545394958, -0.10529082731661776, 0.07353382018297466, 0.2220724273000413, -0.08561850548374342, 0.14434770683396553, 0.006203980609051772, 0.15336813292910914, 0.08743274936786116, -0.018466260155607293, -0.06078011140143916, -0.3407073918340811, -0.1937684749127991, -0.21044859809995586, 0.1701661344904734, -0.12893496412039324, -0.21350267806104314, 0.3705252147793992, -0.005425350181932158, 0.19579787659389314, 0.13497147711476923, 0.21994349481051426, 0.030735485379083723, -0.016789643900814718, 0.1499383096972397, 0.18754119814873965, 0.10633111703070576, 0.01607434685800725, -0.1477442256647593, -0.02315420973628982, 0.20682421726271955]
|
707.0018
|
AC susceptibility and $^{51}$V NMR study of MnV$_2$O$_4$
|
We report $^{51}$V zero-field NMR of manganese vanadate spinel of
MnV$_2$O$_4$, together with both ac and dc magnetization measurements. The
field and temperature dependence of ac susceptibilities show a
reentrant-spin-glass-like behavior below the ferrimagnetic(FEM) ordering
temperature. The zero-field NMR spectrum consists of multiple lines ranging
from 240 MHz to 320 MHz. Its temperature dependence reveals that the ground
state is given by the simultaneous formation of a long-range FEM order and a
short-range order component. We attribute the spin-glass-like anomalies to
freezing and fluctuations of the short-range ordered state caused by the
competition between spin and orbital ordering of the V site.
|
cond-mat.str-el
|
we report 51v zerofield nmr of manganese vanadate spinel of mnv_2o_4 together with both ac and dc magnetization measurements the field and temperature dependence of ac susceptibilities show a reentrantspinglasslike behavior below the ferrimagneticfem ordering temperature the zerofield nmr spectrum consists of multiple lines ranging from 240 mhz to 320 mhz its temperature dependence reveals that the ground state is given by the simultaneous formation of a longrange fem order and a shortrange order component we attribute the spinglasslike anomalies to freezing and fluctuations of the shortrange ordered state caused by the competition between spin and orbital ordering of the v site
|
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|
[-0.2093687982764095, 0.24176934541668743, 0.0008937177434563637, -0.04428830181830563, -0.05917916200705804, -0.08938571565784514, 0.11748512359336019, 0.3800166891189292, -0.26007237285375595, -0.31490631960332394, 0.04260309624485672, -0.36801538076251744, -0.04024885765014915, 0.14377520587295295, 0.14006314914673568, -0.017497601411887446, -0.061762289060279724, 0.03753681057132781, -0.12294300404493697, -0.1459357826935593, 0.25414941176772116, 0.015220446598250418, 0.3129850749834441, 0.11844914723187686, 0.09475198714528232, 0.010669517605565488, 0.13671206585131584, 0.032633021995425227, -0.12235016671744234, 0.024364494075998663, 0.24815879584755748, -0.05501555004506372, 0.13551070707850157, -0.37008281900547446, -0.18735976852709427, 0.047374554416164755, 0.06876601514726645, 0.13124468498397618, -0.03265439028153196, -0.2861444958532229, 0.04590943134971894, -0.1327270473539829, -0.09660774781601504, -0.12641625680029392, -0.01871635714895092, 0.04699416761053726, -0.2764289228618145, 0.18900533579289913, 0.10428086539701326, 0.21692324396921323, -0.1577845863730181, -0.17591888433787972, -0.04734378726221621, 0.05671567928511649, 0.04001672131242231, 0.07925418564191204, 0.16567073677666486, -0.06507619669195265, -0.14534390287008137, 0.31884388349950316, -0.09292261316906661, 0.03362207642756403, 0.14991035998333246, -0.2301659698598087, -0.0583944244729355, 0.19713027554331347, 0.07795235591940582, 0.06540841162670404, -0.14469436305575073, 0.05299004838510882, 0.048099643778987226, 0.28122127706184985, 0.024028204148635268, 0.02859283575322479, 0.2419573411345482, 0.15251576668582856, 0.04394769387319684, 0.17669469223648776, -0.19387518660762, -0.061738288160413504, -0.19508847236225846, -0.08911783264949918, -0.20248096249066294, 0.057060928037390116, -0.07891696152670193, -0.1520124552771449, 0.43238810639828446, 0.15892247553914784, 0.21051938962191344, -0.05496118410956115, 0.23819781320169567, 0.07725900492514484, 0.03632537473458797, 0.025451893712161108, 0.18599230636842548, 0.25441114165820183, 0.17233470525126904, -0.40054630471626296, 0.08045876652933658, -0.03448314755689353]
|
707.0019
|
Probing the Dust and Gas in the Transitional Disk of CS Cha with Spitzer
|
Here we present the Spitzer IRS spectrum of CS Cha, a member of the ~2 Myr
old Chamaeleon star-forming region, which reveals an optically thick
circumstellar disk truncated at ~43 AU, the largest hole modeled in a
transitional disk to date. Within this inner hole, ~5x10^-5 lunar masses of
dust are located in a small optically thin inner region which extends from 0.1
to 1 AU. In addition, the disk of CS Cha has bigger grain sizes and more
settling than the previously modeled transitional disks DM Tau, GM Aur, and
CoKu Tau/4, suggesting that CS Cha is in a more advanced state of dust
evolution. The Spitzer IRS spectrum also shows [Ne II] 12.81 micron
fine-structure emission with a luminosity of 1.3x10^29 ergs s^-1, indicating
that optically thin gas is present in this ~43 AU hole, in agreement with
H_alpha measurements and a UV excess which indicate that CS Cha is still
accreting 1.2x10^-8 M_sun yr^-1. We do not find a correlation of the [Ne II]
flux with L_X, however, there is a possible correlation with mass accretion
rate, which if confirmed would suggest that EUV fluxes due to accretion are the
main agent for formation of the [Ne II] line.
|
astro-ph
|
here we present the spitzer irs spectrum of cs cha a member of the 2 myr old chamaeleon starforming region which reveals an optically thick circumstellar disk truncated at 43 au the largest hole modeled in a transitional disk to date within this inner hole 5x105 lunar masses of dust are located in a small optically thin inner region which extends from 01 to 1 au in addition the disk of cs cha has bigger grain sizes and more settling than the previously modeled transitional disks dm tau gm aur and coku tau4 suggesting that cs cha is in a more advanced state of dust evolution the spitzer irs spectrum also shows ne ii 1281 micron finestructure emission with a luminosity of 13x1029 ergs s1 indicating that optically thin gas is present in this 43 au hole in agreement with h_alpha measurements and a uv excess which indicate that cs cha is still accreting 12x108 m_sun yr1 we do not find a correlation of the ne ii flux with l_x however there is a possible correlation with mass accretion rate which if confirmed would suggest that euv fluxes due to accretion are the main agent for formation of the ne ii line
|
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|
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|
707.002
|
Minimal Seesaw as an Ultraviolet Insensitive Cure for the Problems of
Anomaly Mediation
|
We show that an intermediate scale supersymmetric left-right seesaw scenario
with automatic R-parity conservation can cure the problem of tachyonic slepton
masses that arises when supersymmetry is broken by anomaly mediation, while
preserving ultraviolet insensitivity. The reason for this is the existence of
light B - L = 2 higgses with yukawa couplings to the charged leptons. We find
these theories to have distinct predictions compared to the usual mSUGRA and
gauge mediated models as well as the minimal AMSB models. Such predictions
include a condensed gaugino mass spectrum and possibly a correspondingly
condensed sfermion spectrum.
|
hep-ph hep-th
|
we show that an intermediate scale supersymmetric leftright seesaw scenario with automatic rparity conservation can cure the problem of tachyonic slepton masses that arises when supersymmetry is broken by anomaly mediation while preserving ultraviolet insensitivity the reason for this is the existence of light b l 2 higgses with yukawa couplings to the charged leptons we find these theories to have distinct predictions compared to the usual msugra and gauge mediated models as well as the minimal amsb models such predictions include a condensed gaugino mass spectrum and possibly a correspondingly condensed sfermion spectrum
|
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|
[-0.11011708268222023, 0.2852512076808241, 0.013291999990581237, 0.22449749756351786, -0.1106431250202846, -0.255977129982289, -0.02180654128777802, 0.3276868510168997, -0.20559665711319192, -0.3451989548914927, 0.05574306057260788, -0.2781984679935936, -0.062640858348459, 0.04233880280616119, -0.02833581902705965, 0.04852016441563659, -0.002470687918483894, -0.03508642244529217, -0.08215093168311138, -0.19697033463818756, 0.3164076013292404, -0.004819177170383169, 0.1897376644464725, 0.08810247464026226, 0.04231000939220626, -0.06619212171558211, 0.022390569228322266, -0.1134709295484812, -0.06158610092345353, 0.06813130797502495, 0.20709278892598454, 0.07249579910545591, 0.08178909656968206, -0.341898755546897, -0.2196697212849803, 0.21751285939814247, 0.19080774649541746, 0.11847929172762768, -0.09948167189995342, -0.29755661462215666, 0.0873082394023089, -0.24140965267817707, -0.11198312465839604, -0.08191461768001318, -0.07509189056470356, -0.19661080066493633, -0.3507774556055665, 0.1384210743114075, -0.03474119578938971, 0.00033569502386640994, -0.003260741352123466, -0.1168737064308903, -0.1308203021180816, -0.00238956623565792, 0.29036205394213344, -0.04776957143157562, 0.16491787153930265, -0.23875532187075613, -0.1799278235845664, 0.46449455646599863, -0.0939668119994012, -0.16943900922729455, 0.21249299755745985, -0.08873129139178769, -0.17060015030128464, 0.099567791650151, 0.13002099729380867, 0.10378617278121888, -0.1515231356205867, 0.24155601178310773, -0.07838322940540124, 0.16084542751629302, 0.06125928891049896, 0.06139010538723558, 0.3223814067846917, 0.17779796208041979, 0.06368683345189834, 0.02815828840941825, -0.01668890611209134, -0.07575549626168102, -0.4376810671008648, -0.07047322799669618, -0.05165691732210999, 0.06015983889959356, -0.09325072381297433, -0.1161154711698281, 0.3833498669431565, 0.1471763122058969, 0.2623807879169769, 0.11156999300347958, 0.2715926906292109, 0.08179719296056143, 0.15419161353728417, 0.006931323300492257, 0.29332343548873163, 0.10240044979690673, 0.10038748838532557, -0.27270207705689553, -0.0859187457789766, 0.0932647907670508]
|
707.0021
|
Towards Fault Tolerant Adiabatic Quantum Computation
|
I show how to protect adiabatic quantum computation (AQC) against decoherence
and certain control errors, using a hybrid methodology involving dynamical
decoupling, subsystem and stabilizer codes, and energy gaps. Corresponding
error bounds are derived. As an example I show how to perform
decoherence-protected AQC against local noise using at most two-body
interactions.
|
quant-ph
|
i show how to protect adiabatic quantum computation aqc against decoherence and certain control errors using a hybrid methodology involving dynamical decoupling subsystem and stabilizer codes and energy gaps corresponding error bounds are derived as an example i show how to perform decoherenceprotected aqc against local noise using at most twobody interactions
|
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|
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|
707.0022
|
Lagrangian Mechanics and Variational Integrators on Two-Spheres
|
Euler-Lagrange equations and variational integrators are developed for
Lagrangian mechanical systems evolving on a product of two-spheres. The
geometric structure of a product of two-spheres is carefully considered in
order to obtain global equations of motion. Both continuous equations of motion
and variational integrators completely avoid the singularities and complexities
introduced by local parameterizations or explicit constraints. We derive global
expressions for the Euler-Lagrange equations on two-spheres which are more
compact than existing equations written in terms of angles. Since the
variational integrators are derived from Hamilton's principle, they preserve
the geometric features of the dynamics such as symplecticity, momentum maps, or
total energy, as well as the structure of the configuration manifold.
Computational properties of the variational integrators are illustrated for
several mechanical systems.
|
math.NA
|
eulerlagrange equations and variational integrators are developed for lagrangian mechanical systems evolving on a product of twospheres the geometric structure of a product of twospheres is carefully considered in order to obtain global equations of motion both continuous equations of motion and variational integrators completely avoid the singularities and complexities introduced by local parameterizations or explicit constraints we derive global expressions for the eulerlagrange equations on twospheres which are more compact than existing equations written in terms of angles since the variational integrators are derived from hamiltons principle they preserve the geometric features of the dynamics such as symplecticity momentum maps or total energy as well as the structure of the configuration manifold computational properties of the variational integrators are illustrated for several mechanical systems
|
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|
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|
707.0023
|
pi N to Multi-pi N Scattering in the 1/N_c Expansion
|
We extend the 1/N_c meson-baryon scattering formalism to pi N to multi-pi N
case. We first show that the leading-order large N_c processes proceed through
resonant intermediate states (e.g., rho N or pi Delta). We find that the pole
structure of baryon resonances can be uniquely identified by their
(non)appearance in eta N or mixed partial-wave pi Delta final states.
|
hep-ph
|
we extend the 1n_c mesonbaryon scattering formalism to pi n to multipi n case we first show that the leadingorder large n_c processes proceed through resonant intermediate states eg rho n or pi delta we find that the pole structure of baryon resonances can be uniquely identified by their nonappearance in eta n or mixed partialwave pi delta final states
|
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|
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|
707.0024
|
An Extensive Collection of Stellar Wind X-ray Source Region Emission
Line Parameters,Temperatures, Velocities, and Their Radial Distributions as
Obtained from Chandra Observations of 17 OB Stars
|
Chandra high energy resolution observations have now been obtained from
numerous non-peculiar O and early B stars. The observed X-ray emission line
properties differ from pre-launch predictions, and the interpretations are
still problematic. We present a straightforward analysis of a broad collection
of OB stellar line profile data to search for morphological trends. X-ray line
emission parameters and the spatial distributions of derived quantities are
examined with respect to luminosity class. The X-ray source locations and their
corresponding temperatures are extracted by using the He-like f/i line ratios
and the H-like to He-like line ratios respectively. Our luminosity class study
reveals line widths increasing with luminosity. Although the majority of the OB
emission lines are found to be symmetric, with little central line
displacement, there is evidence for small, but finite, blue-ward line-shifts
that also increase with luminosity. The spatial X-ray temperature distributions
indicate that the highest temperatures occur near the star and steadily
decrease outward. This trend is most pronounced in the OB supergiants. For the
lower density wind stars, both high and low X-ray source temperatures exist
near the star. However, we find no evidence of any high temperature X-ray
emission in the outer wind regions for any OB star. Since the temperature
distributions are counter to basic shock model predictions, we call this the
"near-star high-ion problem" for OB stars. By invoking the traditional OB
stellar mass loss rates, we find a good correlation between the fir-inferred
radii and their associated X-ray continuum optical depth unity radii. We
conclude by presenting some possible explanations to the X-ray source problems
that have been revealed by this study.
|
astro-ph
|
chandra high energy resolution observations have now been obtained from numerous nonpeculiar o and early b stars the observed xray emission line properties differ from prelaunch predictions and the interpretations are still problematic we present a straightforward analysis of a broad collection of ob stellar line profile data to search for morphological trends xray line emission parameters and the spatial distributions of derived quantities are examined with respect to luminosity class the xray source locations and their corresponding temperatures are extracted by using the helike fi line ratios and the hlike to helike line ratios respectively our luminosity class study reveals line widths increasing with luminosity although the majority of the ob emission lines are found to be symmetric with little central line displacement there is evidence for small but finite blueward lineshifts that also increase with luminosity the spatial xray temperature distributions indicate that the highest temperatures occur near the star and steadily decrease outward this trend is most pronounced in the ob supergiants for the lower density wind stars both high and low xray source temperatures exist near the star however we find no evidence of any high temperature xray emission in the outer wind regions for any ob star since the temperature distributions are counter to basic shock model predictions we call this the nearstar highion problem for ob stars by invoking the traditional ob stellar mass loss rates we find a good correlation between the firinferred radii and their associated xray continuum optical depth unity radii we conclude by presenting some possible explanations to the xray source problems that have been revealed by this study
|
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|
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|
707.0025
|
On quantization of massive non-Abelian gauge fields
|
A simpler method of quantization is given for massive gauge theories. This
method gives the same results as those of the conventional massive gauge theory
with ghost and Higgs fields under the Higgs mass. Besides, we point out
physical importance of helicity zero states in non-Abelian gauge theories even
in massless case. Furthermore, forms of mass terms that were impossible before,
e.g. symmetric mass, are possible now. Applying our method to SU(2)xU(1)
symmetry has no particular difficulty, and gives a variant of the standard
model without the Higgs boson.
|
hep-ph
|
a simpler method of quantization is given for massive gauge theories this method gives the same results as those of the conventional massive gauge theory with ghost and higgs fields under the higgs mass besides we point out physical importance of helicity zero states in nonabelian gauge theories even in massless case furthermore forms of mass terms that were impossible before eg symmetric mass are possible now applying our method to su2xu1 symmetry has no particular difficulty and gives a variant of the standard model without the higgs boson
|
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|
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|
707.0026
|
Introducing a Probabilistic Structure on Sequential Dynamical Systems,
Simulation and Reduction of Probabilistic Sequential Networks
|
A probabilistic structure on sequential dynamical systems is introduced here,
the new model will be called Probabilistic Sequential Network, PSN. The
morphisms of Probabilistic Sequential Networks are defined using two algebraic
conditions. It is proved here that two homomorphic Probabilistic Sequential
Networks have the same equilibrium or steady state probabilities if the
morphism is either an epimorphism or a monomorphism. Additionally, the proof of
the set of PSN with its morphisms form the category PSN, having the category of
sequential dynamical systems SDS, as a full subcategory is given. Several
examples of morphisms, subsystems and simulations are given.
|
q-bio.GN math.PR q-bio.MN
|
a probabilistic structure on sequential dynamical systems is introduced here the new model will be called probabilistic sequential network psn the morphisms of probabilistic sequential networks are defined using two algebraic conditions it is proved here that two homomorphic probabilistic sequential networks have the same equilibrium or steady state probabilities if the morphism is either an epimorphism or a monomorphism additionally the proof of the set of psn with its morphisms form the category psn having the category of sequential dynamical systems sds as a full subcategory is given several examples of morphisms subsystems and simulations are given
|
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|
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|
707.0027
|
The Boltzmann-Hamel Equations for Optimal Control
|
We extend the Boltzmann-Hamel equations to the optimal control setting,
producing a set of equations for both kinematic and dynamic nonholonomic
optimal control problems. In particular, we will show the dynamic optimal
control problem can be written as a minimal set of 4n-2m first order
differential equations of motion.
|
math.OC
|
we extend the boltzmannhamel equations to the optimal control setting producing a set of equations for both kinematic and dynamic nonholonomic optimal control problems in particular we will show the dynamic optimal control problem can be written as a minimal set of 4n2m first order differential equations of motion
|
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|
[-0.17549528393577388, 0.032343242674114855, -0.05185700285228643, 0.05463401733481504, -0.14852141168840388, -0.08877425726027564, 0.006855954198127097, 0.30671377263051713, -0.3619974353846083, -0.3221332866777765, 0.15453279641347917, -0.2235364695475932, -0.14791249919762003, 0.2323362888332377, -0.1274547407284696, 0.18784273336542415, 0.04063762252793667, 0.006850159033498866, -0.08095662420655185, -0.22037334363669792, 0.30176146202621623, -0.060652323582387986, 0.20173146296292543, -0.017488011337341146, 0.24114645673754684, 0.02372335980428343, 0.017814621725615036, 0.1186635984266375, -0.14154146391244488, 0.12276756166767805, 0.3196219650513314, 0.10916648173031021, 0.3022163055361585, -0.4122261103797466, -0.18019121938801191, 0.09721953344551172, 0.15523968876755617, 0.16039872835291194, -0.001292756421768919, -0.23564539350410726, 0.11115617353588025, -0.14324420806704127, -0.1420280803391274, -0.09930402650795084, -0.027400832048597487, 0.05873024225869077, -0.35223700613417525, 0.02277630163317031, 0.03366168386283073, -0.0062317781229602525, -0.1739255070607079, -0.053082527236101476, 0.0018778376063292332, 0.15112831390046694, -0.03442535150617836, -0.03149227812846608, 0.11984487668551663, -0.11164455611179484, -0.1870650714857781, 0.4172084440893315, -0.04957421192592208, -0.31281297943217956, 0.10559260433024549, -0.10231973627146254, -0.12036174147370014, 0.09598380345058569, 0.29572841548113193, 0.1970388902390891, -0.2263154193679703, 0.10364867909192206, -0.06441406905651093, 0.13489379838574678, 0.05805236562848725, -0.005537825616750311, 0.10315154827734892, 0.16931976755942277, 0.18970828400330342, 0.15828756219955123, 0.007661839352643236, -0.1443078004299326, -0.35376907488767134, -0.12109370355276351, -0.0381363358824177, 0.05151110594259932, -0.0971017604730305, -0.13422141965240875, 0.3587426356178649, 0.17116783131588933, 0.1398421703897258, 0.08081078147416577, 0.26045894258199853, 0.19636325093612889, -0.03962934726571783, 0.09342701176300328, 0.2096910157756127, 0.10231484833391423, 0.12343908537258493, -0.2673213602975011, 0.04497599017192075, 0.0785525465344495]
|
707.0028
|
The spectral energy distribution of quiescent black hole X-ray binaries:
new constraints from Spitzer
|
(Abridged) Among the various issues that remain open in the field of
accretion onto black hole X-ray binaries (BHBs) is the way the gas accretes at
very low Eddington ratios, in the so-called quiescent regime. While there is
general agreement that the X-rays are produced by a population of high-energy
electrons near to the BH, the controversy comes about in modeling the
contribution from inflowing vs. outflowing particles, and their relative energy
budget. Recent Spitzer observations of three quiescent BHBs have shown evidence
for excess emission with respect to the tail of the companion star between 8-24
micron. We suggest that synchrotron emission from a partially self-absorbed
outflow might be responsible for the observed mid-IR excess, in place of, or in
addition to, thermal emission from circumbinary material. If so, then the jet
synchrotron luminosity exceeds the measured 2-10 keV luminosity by a factor of
a few in these systems. In turn, the mechanical power stored in the jet exceeds
the bolometric X-ray luminosity at least by 4 orders of magnitude. We then
compile the broadband spectral energy distribution (SED) of A0620-00, the
lowest Eddington-ratio stellar mass BH with a known radio counterpart, by means
of simultaneous radio, optical and X-ray observations, and the archival Spitzer
data. We are able to fit the SED of A0620-00 with a `maximally jet-dominated'
model in which the radio through the soft X-rays are dominated by synchrotron
emission, while the hard X-rays are dominated by inverse Compton at the jet
base. The fitted parameters land in a range of values that is reminiscent of
the Galactic Center super-massive BH Sgr A*. Most notably, the inferred ratio
of the jet acceleration rate to local cooling rates is two orders of magnitude
weaker with respect to higher luminosity, hard state sources.
|
astro-ph
|
abridged among the various issues that remain open in the field of accretion onto black hole xray binaries bhbs is the way the gas accretes at very low eddington ratios in the socalled quiescent regime while there is general agreement that the xrays are produced by a population of highenergy electrons near to the bh the controversy comes about in modeling the contribution from inflowing vs outflowing particles and their relative energy budget recent spitzer observations of three quiescent bhbs have shown evidence for excess emission with respect to the tail of the companion star between 824 micron we suggest that synchrotron emission from a partially selfabsorbed outflow might be responsible for the observed midir excess in place of or in addition to thermal emission from circumbinary material if so then the jet synchrotron luminosity exceeds the measured 210 kev luminosity by a factor of a few in these systems in turn the mechanical power stored in the jet exceeds the bolometric xray luminosity at least by 4 orders of magnitude we then compile the broadband spectral energy distribution sed of a062000 the lowest eddingtonratio stellar mass bh with a known radio counterpart by means of simultaneous radio optical and xray observations and the archival spitzer data we are able to fit the sed of a062000 with a maximally jetdominated model in which the radio through the soft xrays are dominated by synchrotron emission while the hard xrays are dominated by inverse compton at the jet base the fitted parameters land in a range of values that is reminiscent of the galactic center supermassive bh sgr a most notably the inferred ratio of the jet acceleration rate to local cooling rates is two orders of magnitude weaker with respect to higher luminosity hard state sources
|
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|
[-0.035699141867975785, 0.14679972850480827, -0.037130775830661086, 0.12949054790029335, -0.08312922618509729, -0.07307113531219252, 0.048778852984561756, 0.4638226417666775, -0.19494652367252224, -0.3410602314133292, 0.06689027712238416, -0.3328118849964023, 0.044336663657736225, 0.22840955096328536, -0.012813391867961923, -0.007317017281568072, 0.028356810069595607, -0.09018788916390326, -0.040853295615732164, -0.18839637307387036, 0.3106892262585461, 0.11695051877680471, 0.17640687350649387, 0.0060950539169548935, 0.0684156203610424, -0.07675860224733666, -0.04834808923019949, -0.029418728959951866, -0.09421536892512418, 0.06263144257383706, 0.24914321932483907, 0.0985162263710478, 0.18502973750770343, -0.3564704492830245, -0.22308883789484785, 0.07177558438304883, 0.16283760943481604, -0.030783370402799444, -0.03227135988210833, -0.18619974570396214, 0.05526915316418666, -0.24430975075811148, -0.15551239452877288, 0.07986440247840296, 0.039031052856579804, 0.010400975434409486, -0.19933782131411135, 0.14371773310921201, 0.03315317200724197, 0.018248268168309104, -0.15655387217036876, -0.061096011198883464, -0.07136183720973904, 0.025744742840938903, 0.0980025265701273, 0.07781433229792421, 0.20883779636726288, -0.16818680234758532, -0.08907557301759972, 0.37919186832288565, -0.05372392289553595, 0.02760764101788528, 0.22077176112531668, -0.2480667286962902, -0.14694780786600659, 0.2300756735948183, 0.12509283348286557, 0.09593023226154432, -0.15840021226144696, 0.003920681326614567, -0.0149001225529207, 0.24066149352268332, 0.05102857058015415, 0.08297102280211205, 0.3600212655188042, 0.09394482479083462, 0.002604831961946467, 0.16657683273177532, -0.2183390725530305, -0.019256737479403364, -0.24655100071834304, -0.0439717473462224, -0.1555033037624464, 0.13238986459900073, -0.1276169353364513, -0.08330980957400891, 0.33689307772270327, 0.08203092598814075, 0.23792956012569494, 0.03382806470499263, 0.34094544994344905, 0.1347774363689172, 0.07538925371334051, 0.18098950444136636, 0.37449419736009787, 0.14381427655067547, 0.10841897829056922, -0.24737579177481012, 0.07564196995404249, -0.0002578062178977465]
|
707.0029
|
Zooming into the coexisting regime of ferromagnetism and
superconductivity in ErRh4B4 single crystals
|
High resolution measurements of the dynamic magnetic susceptibility are
reported for ferromagnetic re-entrant superconductor, ErRh$_{4}$B$_{4}$.
Detailed investigation of the coexisting regime reveals unusual
temperature-asymmetric and magnetically anisotropic behavior. The
superconducting phase appears via a series of discontinuous steps upon warming
from the ferromagnetic normal phase, whereas the ferromagnetic phase develops
via a gradual transition. A model based on local field inhomogeneity is
proposed to explain the observations.
|
cond-mat.str-el cond-mat.supr-con
|
high resolution measurements of the dynamic magnetic susceptibility are reported for ferromagnetic reentrant superconductor errh_4b_4 detailed investigation of the coexisting regime reveals unusual temperatureasymmetric and magnetically anisotropic behavior the superconducting phase appears via a series of discontinuous steps upon warming from the ferromagnetic normal phase whereas the ferromagnetic phase develops via a gradual transition a model based on local field inhomogeneity is proposed to explain the observations
|
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|
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|
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