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707.183
|
Nonlinear transport of Bose-Einstein condensates through mesoscopic
waveguides
|
We study the coherent flow of interacting Bose-condensed atoms in mesoscopic
waveguide geometries. Analytical and numerical methods, based on the mean-field
description of the condensate, are developed to study both stationary as well
as time-dependent propagation processes. We apply these methods to the
propagation of a condensate through an atomic quantum dot in a waveguide,
discuss the nonlinear transmission spectrum and show that resonant transport is
generally suppressed due to an interaction-induced bistability phenomenon.
Finally, we establish a link between the nonlinear features of the transmission
spectrum and the self-consistent quasi-bound states of the quantum dot.
|
cond-mat.other
|
we study the coherent flow of interacting bosecondensed atoms in mesoscopic waveguide geometries analytical and numerical methods based on the meanfield description of the condensate are developed to study both stationary as well as timedependent propagation processes we apply these methods to the propagation of a condensate through an atomic quantum dot in a waveguide discuss the nonlinear transmission spectrum and show that resonant transport is generally suppressed due to an interactioninduced bistability phenomenon finally we establish a link between the nonlinear features of the transmission spectrum and the selfconsistent quasibound states of the quantum dot
|
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|
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|
707.1831
|
On the geometry of the moduli space of spin curves
|
We determine the smooth locus and the locus of canonical singularities in the
Cornalba compactification \bar S_g of the moduli space S_g of spin curves,
i.e., smooth curves of genus g with a theta characteristic. Moreover, the
following lifting result for pluricanonical forms is proved: Every
pluricanonical form on the smooth locus of \bar S_g extends holomorphically to
a desingularisation of \bar S_g.
|
math.AG
|
we determine the smooth locus and the locus of canonical singularities in the cornalba compactification bar s_g of the moduli space s_g of spin curves ie smooth curves of genus g with a theta characteristic moreover the following lifting result for pluricanonical forms is proved every pluricanonical form on the smooth locus of bar s_g extends holomorphically to a desingularisation of bar s_g
|
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|
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|
707.1832
|
Rotational cooling efficiency upon molecular ionization: the case of
Li$_2(a^3\Sigma_u^+)$ and Li$_2^+(X^2\Sigma_g^+)$ interacting with $^4$He
|
The low-temperature (up to about 100K) collisional (de)excitation cross
sections are computed using the full coupled-channel (CC) quantum dynamics for
both Li$_2$ and Li$_2^+$ molecular targets in collision with $^4$He. The
interaction forces are obtained from fairly accurate {\it ab initio}
calculations and the corresponding pseudo-rates are also computed. The results
show surprising similarities between sizes of inelastic flux distributions
within final states in both systems and the findings are connected with the
structural change in the molecular rotor features when the neutral species is
replaced by its ionic counterpart.
|
physics.chem-ph
|
the lowtemperature up to about 100k collisional deexcitation cross sections are computed using the full coupledchannel cc quantum dynamics for both li_2 and li_2 molecular targets in collision with 4he the interaction forces are obtained from fairly accurate it ab initio calculations and the corresponding pseudorates are also computed the results show surprising similarities between sizes of inelastic flux distributions within final states in both systems and the findings are connected with the structural change in the molecular rotor features when the neutral species is replaced by its ionic counterpart
|
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|
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|
707.1833
|
On the girth of random Cayley graphs
|
We prove that random d-regular Cayley graphs of the symmetric group
asymptotically almost surely have girth at least (log_{d-1}|G|)^{1/2}/2 and
that random d-regular Cayley graphs of simple algebraic groups over F_q
asymptotically almost surely have girth at least log_{d-1}|G|/dim(G). For the
symmetric p-groups the girth is between log log |G| and (log|G|)^alpha with
alpha<1. Several conjectures and open questions are presented.
|
math.PR math.GR
|
we prove that random dregular cayley graphs of the symmetric group asymptotically almost surely have girth at least log_d1g122 and that random dregular cayley graphs of simple algebraic groups over f_q asymptotically almost surely have girth at least log_d1gdimg for the symmetric pgroups the girth is between log log g and loggalpha with alpha1 several conjectures and open questions are presented
|
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|
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|
707.1834
|
A Conceptual Analysis of Mass Loss and Frequency Redistribution in
Wolf-Rayet Winds
|
To better understand Wolf-Rayet stars as progenitors of gamma-ray bursts, an
understanding of the effect metallicity has on Wolf-Rayet mass loss is needed.
Using simple analytic models, we study the Mdot - Z relation of a WN star and
compare the results to similar models. We find that Mdot roughly follows a
power law in Z with index 0.88 from -2.5 < log Z/Z_sun < -1 and appears to
flatten by log Z/Z_sun ~ -0.5.
|
astro-ph
|
to better understand wolfrayet stars as progenitors of gammaray bursts an understanding of the effect metallicity has on wolfrayet mass loss is needed using simple analytic models we study the mdot z relation of a wn star and compare the results to similar models we find that mdot roughly follows a power law in z with index 088 from 25 log zz_sun 1 and appears to flatten by log zz_sun 05
|
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|
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|
707.1835
|
Polynomials with PSL(2) monodromy
|
Let K be a field of characteristic p>0, and let q be a power of p. We
determine all polynomials f in K[t]\K[t^p] of degree q(q-1)/2 such that the
Galois group of f(t)-u over K(u) has a transitive normal subgroup isomorphic to
PSL_2(q), subject to a certain ramification hypothesis. As a consequence, we
describe all polynomials f in K[t], of degree not a power of p, such that f is
functionally indecomposable over K but f decomposes over an extension of K.
Moreover, except for one ramification setup (which is treated in the companion
paper arxiv:0707.1837), we describe all indecomposable polynomials f in K[t] of
non-p-power degree which are exceptional, in the sense that x-y is the only
absolutely irreducible factor of f(x)-f(y) which lies in K[x,y]. It is known
that, when K is finite, a polynomial f is exceptional if and only if it induces
a bijection on infinitely many finite extensions of K.
|
math.AG math.NT
|
let k be a field of characteristic p0 and let q be a power of p we determine all polynomials f in ktktp of degree qq12 such that the galois group of ftu over ku has a transitive normal subgroup isomorphic to psl_2q subject to a certain ramification hypothesis as a consequence we describe all polynomials f in kt of degree not a power of p such that f is functionally indecomposable over k but f decomposes over an extension of k moreover except for one ramification setup which is treated in the companion paper arxiv07071837 we describe all indecomposable polynomials f in kt of nonppower degree which are exceptional in the sense that xy is the only absolutely irreducible factor of fxfy which lies in kxy it is known that when k is finite a polynomial f is exceptional if and only if it induces a bijection on infinitely many finite extensions of k
|
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|
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|
707.1836
|
Type-II Matrices and Combinatorial Structures
|
Type-II matrices are a class of matrices used by Jones in his work on spin
models. In this paper we show that type-II matrices arise naturally in
connection with some interesting combinatorial and geometric structures.
|
math.CO
|
typeii matrices are a class of matrices used by jones in his work on spin models in this paper we show that typeii matrices arise naturally in connection with some interesting combinatorial and geometric structures
|
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|
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|
707.1837
|
A new family of exceptional polynomials in characteristic two
|
We produce a new family of polynomials f(x) over fields K of characteristic 2
which are exceptional, in the sense that f(x)-f(y) has no absolutely
irreducible factors in K[x,y] besides the scalar multiples of x-y; when K is
finite, this condition is equivalent to saying there are infinitely many finite
extensions L/K for which the map c --> f(c) is bijective on L. Our polynomials
have degree (2^e-1)*2^(e-1), where e is odd. Combined with our previous paper
arxiv:0707.1835, this completes the classification of indecomposable
exceptional polynomials of degree not a power of the characteristic. The
strategy of our proof is to identify the curves that can arise as the Galois
closure of the branched cover P^1 --> P^1 induced by an exceptional polynomial
f. In this case, the curves turn out to be x^(q+1)+y^(q+1)=a+T(xy), where
T(z)=z^(q/2)+z^(q/4)+...+z. Our proofs rely on new properties of ramification
in Galois covers of curves, as well as the computation of the automorphism
groups of all curves in a certain 2-parameter family.
|
math.NT math.AG
|
we produce a new family of polynomials fx over fields k of characteristic 2 which are exceptional in the sense that fxfy has no absolutely irreducible factors in kxy besides the scalar multiples of xy when k is finite this condition is equivalent to saying there are infinitely many finite extensions lk for which the map c fc is bijective on l our polynomials have degree 2e12e1 where e is odd combined with our previous paper arxiv07071835 this completes the classification of indecomposable exceptional polynomials of degree not a power of the characteristic the strategy of our proof is to identify the curves that can arise as the galois closure of the branched cover p1 p1 induced by an exceptional polynomial f in this case the curves turn out to be xq1yq1atxy where tzzq2zq4z our proofs rely on new properties of ramification in galois covers of curves as well as the computation of the automorphism groups of all curves in a certain 2parameter family
|
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|
[-0.20381763048171705, 0.09186926803458846, -0.1116760260076262, 0.01891729745984776, -0.08402591018821112, -0.14566797691222746, -0.007721949226834113, 0.33434507736819796, -0.3208514610538259, -0.22126565967919304, 0.08591731828273623, -0.2562159583569155, -0.1365416800854291, 0.24365919978008604, -0.1139760570395083, -0.008129545036354102, 0.009575043569202534, 0.11420362431090325, -0.05509351979999337, -0.3363974515872542, 0.3459163555147825, -0.06905732767627341, 0.17234794613614213, 0.031231663207290695, 0.09132768117124215, 0.009009568483452312, 0.004392958825337701, -0.033349800715222956, -0.12857355155765618, 0.09609786978617194, 0.3270708727533929, 0.09122095072525553, 0.2101800031028688, -0.3078033500249148, -0.17207290681399173, 0.2584139735379722, 0.1627559509521234, 0.002998882586689433, 0.007932782678108197, -0.191997808339147, 0.12660166044584004, -0.11468668684701697, -0.1627711438544793, -0.0753210997354472, 0.06802170917580952, 0.07797360306140036, -0.2532917221687967, -0.0005662495357682928, 0.14871149563550717, 0.17864543070318178, -0.006177759487763978, -0.1472908989089774, -0.038533416319114625, 0.06857603510088665, 0.015279401796578895, 0.06584062926121988, 0.04981200296097086, -0.10463603752868948, -0.1009989775440772, 0.3726210604443622, -0.06694879785354715, -0.1874810363748111, 0.12998444886907237, -0.1704740974630113, -0.1725891331443563, 0.17971595965209416, 0.08573509697453119, 0.1534194416817627, -0.0429789106456667, 0.19278165987925605, -0.14252931542705483, 0.10286398296011612, 0.09286552375706378, -0.006037840499629965, 0.1572865083871875, 0.05067124661945854, 0.0931680132063775, 0.1296199050899304, -0.00016823442128952593, -0.03255802947387565, -0.3857127001218032, -0.16993517584051004, -0.13427386376497452, 0.1088223483312504, -0.09049013668263797, -0.18349060265900335, 0.43441165771801027, 0.07329531682771631, 0.20035193523508496, 0.10205141258920776, 0.2083345026592724, 0.07917329281699495, 0.0795996070963156, 0.0502100324989442, 0.15444548419618515, 0.17482201304082992, -0.042343561162851984, -0.15735597852035427, 0.014153457382053602, 0.11420909400767414]
|
707.1838
|
Computing the complete CS decomposition
|
An algorithm is developed to compute the complete CS decomposition (CSD) of a
partitioned unitary matrix. Although the existence of the CSD has been
recognized since 1977, prior algorithms compute only a reduced version (the
2-by-1 CSD) that is equivalent to two simultaneous singular value
decompositions. The algorithm presented here computes the complete 2-by-2 CSD,
which requires the simultaneous diagonalization of all four blocks of a unitary
matrix partitioned into a 2-by-2 block structure. The algorithm appears to be
the only fully specified algorithm available. The computation occurs in two
phases. In the first phase, the unitary matrix is reduced to bidiagonal block
form, as described by Sutton and Edelman. In the second phase, the blocks are
simultaneously diagonalized using techniques from bidiagonal SVD algorithms of
Golub, Kahan, and Demmel. The algorithm has a number of desirable numerical
features.
|
math.NA
|
an algorithm is developed to compute the complete cs decomposition csd of a partitioned unitary matrix although the existence of the csd has been recognized since 1977 prior algorithms compute only a reduced version the 2by1 csd that is equivalent to two simultaneous singular value decompositions the algorithm presented here computes the complete 2by2 csd which requires the simultaneous diagonalization of all four blocks of a unitary matrix partitioned into a 2by2 block structure the algorithm appears to be the only fully specified algorithm available the computation occurs in two phases in the first phase the unitary matrix is reduced to bidiagonal block form as described by sutton and edelman in the second phase the blocks are simultaneously diagonalized using techniques from bidiagonal svd algorithms of golub kahan and demmel the algorithm has a number of desirable numerical features
|
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|
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|
707.1839
|
Water Waves and Integrability
|
The Euler's equations describe the motion of inviscid fluid. In the case of
shallow water, when a perturbative asymtotic expansion of the Euler's equations
is taken (to a certain order of smallness of the scale parameters), relations
to certain integrable equations emerge. Some recent results concerning the use
of integrable equation in modeling the motion of shallow water waves are
reviewed in this contribution.
|
nlin.SI math-ph math.MP
|
the eulers equations describe the motion of inviscid fluid in the case of shallow water when a perturbative asymtotic expansion of the eulers equations is taken to a certain order of smallness of the scale parameters relations to certain integrable equations emerge some recent results concerning the use of integrable equation in modeling the motion of shallow water waves are reviewed in this contribution
|
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|
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|
707.184
|
Domain Formation in v=2/3 Fractional Quantum Hall Systems
|
We study the domain formation in the v=2/3 fractional quantum Hall systems
basing on the density matrix renormalization group (DMRG) analysis. The
ground-state energy and the pair correlation functions are calculated for
various spin polarizations. The results confirm the domain formation in
partially spin polarized states, but the presence of the domain wall increases
the energy of partially spin polarized states and the ground state is either
spin unpolarized state or fully spin polarized state depending on the Zeeman
energy. We expect coupling with external degrees of freedom such as nuclear
spins is important to reduce the energy of partially spin polarized state.
|
cond-mat.mes-hall cond-mat.str-el
|
we study the domain formation in the v23 fractional quantum hall systems basing on the density matrix renormalization group dmrg analysis the groundstate energy and the pair correlation functions are calculated for various spin polarizations the results confirm the domain formation in partially spin polarized states but the presence of the domain wall increases the energy of partially spin polarized states and the ground state is either spin unpolarized state or fully spin polarized state depending on the zeeman energy we expect coupling with external degrees of freedom such as nuclear spins is important to reduce the energy of partially spin polarized state
|
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|
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|
707.1841
|
A Review of H2CO 6cm Masers in the Galaxy
|
We present a review of the field of formaldehyde (H2CO) 6cm masers in the
Galaxy. Previous to our ongoing work, H2CO 6cm masers had been detected in the
Galaxy only toward three regions: NGC7538 IRS1, Sgr B2, and G29.96-0.02.
Current efforts by our group using the Very Large Array, Arecibo, and the Green
Bank Telescope have resulted in the detection of four new H2CO 6cm maser
regions. We discuss the characteristics of the known H2CO masers and the
association of H2CO 6cm masers with very young regions of massive star
formation. We also review the current ideas on the pumping mechanism for H2CO
6cm masers.
|
astro-ph
|
we present a review of the field of formaldehyde h2co 6cm masers in the galaxy previous to our ongoing work h2co 6cm masers had been detected in the galaxy only toward three regions ngc7538 irs1 sgr b2 and g2996002 current efforts by our group using the very large array arecibo and the green bank telescope have resulted in the detection of four new h2co 6cm maser regions we discuss the characteristics of the known h2co masers and the association of h2co 6cm masers with very young regions of massive star formation we also review the current ideas on the pumping mechanism for h2co 6cm masers
|
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|
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|
707.1842
|
Foundations of the calculus of variations in generalized function
algebras
|
We propose the use of algebras of generalized functions for the analysis of
certain highly singular problems in the calculus of variations. After a general
study of extremal problems on open subsets of Euclidean space in this setting
we introduce the first and second variation of a variational problem. We then
derive necessary (Euler-Lagrange equations) and sufficient conditions for
extremals. The concept of association is used to obtain connections to a
distributional description of singular variational problems. We study
variational symmetries and derive an appropriate version of N\"other's theorem.
Finally, a number of applications to geometry, mechanics, elastostatics and
elastodynamics are presented.
|
math.FA math.OC
|
we propose the use of algebras of generalized functions for the analysis of certain highly singular problems in the calculus of variations after a general study of extremal problems on open subsets of euclidean space in this setting we introduce the first and second variation of a variational problem we then derive necessary eulerlagrange equations and sufficient conditions for extremals the concept of association is used to obtain connections to a distributional description of singular variational problems we study variational symmetries and derive an appropriate version of nothers theorem finally a number of applications to geometry mechanics elastostatics and elastodynamics are presented
|
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|
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|
707.1843
|
Determinantal transition kernels for some interacting particles on the
line
|
We find the transition kernels for four Markovian interacting particle
systems on the line, by proving that each of these kernels is intertwined with
a Karlin-McGregor type kernel. The resulting kernels all inherit the
determinantal structure from the Karlin-McGregor formula, and have a similar
form to Schutz's kernel for the totally asymmetric simple exclusion process.
|
math.PR math-ph math.MP
|
we find the transition kernels for four markovian interacting particle systems on the line by proving that each of these kernels is intertwined with a karlinmcgregor type kernel the resulting kernels all inherit the determinantal structure from the karlinmcgregor formula and have a similar form to schutzs kernel for the totally asymmetric simple exclusion process
|
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|
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|
707.1844
|
Gamma-ray absorption in the microquasar SS433
|
We discuss the gamma-ray absorption in the inner region of the microquasar
SS433. Our investigation includes several contributions to the opacity of this
system. They result from the ambient fields generated by the primary star,
possibly an A-type supergiant, and a very extended disk around the black hole.
Besides the sharp and dramatic absorption effect that occurs every time the
star crosses the emission zone, we find in the UV photon field from the
extended disk an important source of absorption for very high energy
gamma-rays. This results in periodic gamma-ray observational signatures.
|
astro-ph
|
we discuss the gammaray absorption in the inner region of the microquasar ss433 our investigation includes several contributions to the opacity of this system they result from the ambient fields generated by the primary star possibly an atype supergiant and a very extended disk around the black hole besides the sharp and dramatic absorption effect that occurs every time the star crosses the emission zone we find in the uv photon field from the extended disk an important source of absorption for very high energy gammarays this results in periodic gammaray observational signatures
|
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|
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|
707.1845
|
On a theorem in multi-parameter potential theory
|
We prove a theorem on additive Levy processes and give applications
|
math.PR
|
we prove a theorem on additive levy processes and give applications
|
[['we', 'prove', 'a', 'theorem', 'on', 'additive', 'levy', 'processes', 'and', 'give', 'applications']]
|
[-0.1054180579429323, 0.09753167891705578, -0.1742841603065079, 0.17983343249017542, -0.04976513033563441, -0.16020853880962188, 0.10573942823843523, 0.384679185395891, -0.28061367300423706, -0.11196852526204153, 0.15381727465005082, -0.21710652316158469, -0.24740114554085516, 0.3078893724490296, -0.23792230735786937, 0.012409542771902952, 0.07576574351299893, -0.026435963640158825, 0.08072309280661019, -0.24995556236668068, 0.2995267754251307, -0.13439797254448588, 0.17213844203136183, 0.1638719176196239, 0.26237884163856506, 0.08980564925480973, -0.18205039643428542, -0.1516961589116942, -0.291728843934834, 0.08530113608999686, 0.2858640043572946, -0.02112059919586913, 0.3159338113936511, -0.38818921555172314, -0.22462640596892347, 0.1948853460225192, -0.031006005296314306, 0.04741606040095741, -0.09374320886986838, -0.3203805820508437, 0.12203101957724853, -0.15600453825159508, -0.16996750912883066, -0.15075056966055522, 0.06421211531216447, 0.09250555983321233, -0.3982979678972201, 0.05001044358042153, 0.30222000588070264, 0.04607505308972164, -0.03382371171292933, -0.16734739528460937, 0.13042921098795804, -0.013021054296669636, -0.01136085137047551, -0.13943959341850132, 0.2246184737252241, -0.0064772706140171395, -0.28304123251952906, 0.27776759185574273, -0.10497142175551165, -0.24310267615047368, 0.1734080451794646, -0.08605406213213097, -0.21830934675579722, 0.004719388078559528, 0.23792021399871868, 0.09631550312042236, -0.09914866081354293, 0.2966629879665561, -0.018757103180343456, 0.052866992286660454, 0.1307593011720614, 0.10704236274415796, 0.058390206953679975, 0.08075868626209823, 0.24584719115360218, 0.23953638395125215, 0.04237841520543126, -0.09162426248870113, -0.32759668271649967, -0.19083837453614583, -0.12168471608310938, 0.23386270315809685, -0.13753831416066864, -0.29365667226639663, 0.2822837175547399, 0.11698630964383483, 0.1491458057002588, 0.21737318460575558, 0.20087867704304782, 0.23253167733888735, -0.16469033900648355, 0.06668754751709374, 0.010838218371976505, 0.28212291798131034, 0.08096045124429194, 0.04650136388160966, 0.07541815470904112, 0.14041518318382176]
|
707.1846
|
Dust formation by bubble-burst phenomenon at the surface of a liquid
steel bath
|
We have developed an experimental device for studying the main mechanism of
dust formation in electric arc furnace steelmaking: the burst of gas bubbles at
the liquid steel surface. As in the case of the air-water system, the
bubble-burst process takes place in three steps: breaking of the film cap,
projection of film drops, and projection of jet drops. The film break and the
jet drop formation are observed with a high-speed video camera. The film drop
aerosol enters a particle counter, which characterizes the drops in size and
number. Results are presented and discussed. The quantification of both types
of projections leads to the conclusion that the film drop projections represent
the major source of dust. The amount of film drops greatly decreases with the
parent bubble size. Bubbles with diameter under 4mm theoretically do not
produce film drops. Decreasing the CO-bubble size enough would therefore
represent an effective solution for reducing drastically the electric arc
furnace dust emission.
|
cond-mat.mtrl-sci
|
we have developed an experimental device for studying the main mechanism of dust formation in electric arc furnace steelmaking the burst of gas bubbles at the liquid steel surface as in the case of the airwater system the bubbleburst process takes place in three steps breaking of the film cap projection of film drops and projection of jet drops the film break and the jet drop formation are observed with a highspeed video camera the film drop aerosol enters a particle counter which characterizes the drops in size and number results are presented and discussed the quantification of both types of projections leads to the conclusion that the film drop projections represent the major source of dust the amount of film drops greatly decreases with the parent bubble size bubbles with diameter under 4mm theoretically do not produce film drops decreasing the cobubble size enough would therefore represent an effective solution for reducing drastically the electric arc furnace dust emission
|
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|
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|
707.1847
|
On a general theorem for additive Levy processes
|
We prove a new theorem on additive Levy processes and show that this theorem
implies several proved theorems and a hard conjectured theorem.
|
math.PR
|
we prove a new theorem on additive levy processes and show that this theorem implies several proved theorems and a hard conjectured theorem
|
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|
[-0.11193202371182649, 0.08888244989287594, -0.23842505110508722, 0.21444242185933274, 0.0026942908601916356, -0.17800315603127945, 0.1078611372605614, 0.30078003425960953, -0.29207156015479047, -0.17775642879955147, 0.1001790801225149, -0.16525240137201289, -0.22619721844144489, 0.31663556380764296, -0.2207879839141084, 0.04048771694626497, 0.090463955603216, -0.011515609272148298, 0.02554774005978328, -0.24472691960956738, 0.27543428183897684, -0.1580839864099803, 0.23411322996506226, 0.2527413129725534, 0.21538180829552206, 0.09027311882085126, -0.17216591140174348, -0.060746107331436615, -0.21528087840978632, 0.08592995709699133, 0.2665680382886659, 0.029120298193605697, 0.33246088675830676, -0.33653409357952035, -0.17984566602693952, 0.19697618597875471, 0.002963447457422381, 0.03648488681115534, -0.027062491792173165, -0.2932597610127667, 0.18277120446462347, -0.15228632821337038, -0.26994781386431144, -0.09941282058539598, 0.0013264368247726688, 0.005925326243690823, -0.32735256008479907, 0.04844114615622422, 0.40498382630555524, -0.02654378274050744, -0.048033681779128055, -0.09860171227837386, 0.01908710609068689, -0.049169839278835316, 0.08198349720434002, -0.037309286918531616, 0.08103165473869961, -0.008389776481477462, -0.2500399651977679, 0.23339959136817767, -0.048883792276129774, -0.1335018325759017, 0.16358256801638915, -0.11553639712055093, -0.32525074862591596, 0.04112781713838163, 0.06979249782212403, 0.1566213609083839, -0.132716859974291, 0.20714569735118066, -0.15726348757743835, 0.1391342797357103, 0.2069118764737378, 0.041280690600852606, 0.07186411477058478, 0.024381893322519634, 0.16756883858824553, 0.22436726320049036, 0.033428552084723895, -0.06953500332715719, -0.2843560310404586, -0.16214058216175306, -0.21781676076352596, 0.2027268489093884, -0.1508929720945636, -0.20947760432634666, 0.20515213993823397, 0.0857200906611979, 0.09154325108165326, 0.2260269720674209, 0.1724609147919261, 0.17306921116845764, -0.0681595730635783, 0.14325117024228626, 0.16743592124270357, 0.30716308586947294, 0.07962541219413928, 0.026488934765043465, -0.00405604044056457, 0.22335689686967627]
|
707.1848
|
Jones Pairs
|
Motivated by Jones' braid group representations constructed from spin models,
we define {\sl a Jones pair} to be a pair of $\nbyn$ matrices $(A,B)$ such that
the endomorphisms $X_A$ and $\D_B$ form a representation of a braid group. When
$A$ and $B$ are type-II matrices, we call $(A,B)$ {\sl an invertible Jones
pair}. We develop the theory of Jones pairs in this thesis.
Our aim is to study the connections among association schemes, spin models
and four-weight spin models using the viewpoint of Jones pairs. We use Nomura's
method to construct a pair of algebras from the matrices $(A,B)$, which we call
the Nomura algebras of $(A,B)$. These algebras become the central tool in this
thesis. We explore their properties in Chapters \ref{Nomura} and \ref{IINom}.
In Chapter \ref{JP}, we introduce Jones pairs. We prove the equivalence of
four-weight spin models and invertible Jones pairs. We extend some existing
concepts for four-weight spin models to Jones pairs. In Chapter
\ref{SpinModels}, we provide new proofs for some well-known results on the
Bose-Mesner algebras associated with spin models.
We document the main results of the thesis in Chapter \ref{InvJP}. We prove
that every four-weight spin model comes from a symmetric spin model (up to
odd-gauge equivalence). We present four Bose-Mesner algebras associated to each
four-weight spin model. We study the relations among these algebras. In
particular, we provide a strategy to search for four-weight spin models. This
strategy is analogous to the method given by Bannai, Bannai and Jaeger for
finding spin models.
|
math.CO
|
motivated by jones braid group representations constructed from spin models we define sl a jones pair to be a pair of nbyn matrices ab such that the endomorphisms x_a and d_b form a representation of a braid group when a and b are typeii matrices we call ab sl an invertible jones pair we develop the theory of jones pairs in this thesis our aim is to study the connections among association schemes spin models and fourweight spin models using the viewpoint of jones pairs we use nomuras method to construct a pair of algebras from the matrices ab which we call the nomura algebras of ab these algebras become the central tool in this thesis we explore their properties in chapters refnomura and refiinom in chapter refjp we introduce jones pairs we prove the equivalence of fourweight spin models and invertible jones pairs we extend some existing concepts for fourweight spin models to jones pairs in chapter refspinmodels we provide new proofs for some wellknown results on the bosemesner algebras associated with spin models we document the main results of the thesis in chapter refinvjp we prove that every fourweight spin model comes from a symmetric spin model up to oddgauge equivalence we present four bosemesner algebras associated to each fourweight spin model we study the relations among these algebras in particular we provide a strategy to search for fourweight spin models this strategy is analogous to the method given by bannai bannai and jaeger for finding spin models
|
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|
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|
707.1849
|
Hausdorrf dimension for level sets and k-multiple times
|
We compute the Hausdorff dimension of the zero set of an additive Levy
process.
|
math.PR
|
we compute the hausdorff dimension of the zero set of an additive levy process
|
[['we', 'compute', 'the', 'hausdorff', 'dimension', 'of', 'the', 'zero', 'set', 'of', 'an', 'additive', 'levy', 'process']]
|
[-0.1191965432039329, 0.14480822484412265, -0.07944466492959432, 0.09316568684114047, -0.03305854817985424, -0.0743377897888422, 0.08183804739798818, 0.3153397683054209, -0.35947627467768534, -0.07904184756002255, 0.07429650884919933, -0.3231770859232971, -0.12729465003524507, 0.16028181037732533, -0.155151315299528, 0.11367078976971763, -0.0712480367760041, 0.10659738603447165, 0.03659668990543911, -0.33662607840129305, 0.43409344873258043, -0.0050654612215501925, 0.22380469340298856, -0.004283501101391656, 0.21565341736589158, -0.0438471962697804, -0.1271051506378821, -0.01810550782829523, -0.22810553167281405, 0.12694442405232362, 0.18381209086094583, 0.04105442730776433, 0.280553475022316, -0.3052200725568192, -0.13089190889149904, 0.25517891719937325, 0.07848951007638659, 0.019285706537110463, 0.09090101945080928, -0.2990268067722874, 0.15658989947821414, -0.23959422829960073, -0.23604262683407537, -0.10429515835962125, 0.11663969819034849, -0.09354396164417267, -0.324935667615916, -0.028708290308713913, 0.1579056696168014, 0.07837042791236724, -0.07191683957353234, -0.15598254624222005, -0.003908948224437024, 0.16549214487063832, 0.010015810105999532, -0.026591359379900887, 0.17596988822333515, -0.053245452897889275, -0.1966393556379314, 0.2692429933231324, -0.1379313401744834, -0.27934933081269264, 0.1920690495254738, -0.2376141601375171, -0.052993210697812695, 0.18135089533669607, 0.17719969592456306, 0.08736863386418138, -0.14212390554270574, 0.2693221638245242, -0.03824880486354232, 0.10735451696174485, 0.08206070680171251, 0.036767389359218736, 0.04501214171094554, 0.13985924422740936, 0.24080382806382009, 0.21390772264982974, -0.1058760310656258, -0.04849647517715182, -0.36726451611944605, -0.17546242927866323, -0.2840239186771214, 0.16497721597884915, -0.2106784065919263, -0.3469259478151798, 0.3292196367734245, 0.1295209215687854, 0.21902209972696646, 0.17721372290647455, 0.22348543416176522, 0.23252089447279495, -0.1510500679058688, 0.09383840240272028, 0.008591153525880404, 0.1662633836801563, -0.04193747243178742, -0.1584293141162821, 0.025106113869696856, 0.14615365909412503]
|
707.185
|
New insights on the dense molecular gas in NGC253 as traced by HCN and
HCO+
|
We have imaged the central ~1kpc of the circumnuclear starburst disk in the
galaxy NGC253 in the HCN(1-0), HCO+(1-0), and CO(1-0) transitions at 60pc
resolution using the Owens Valley Radio Observatory Millimeter-Wavelength Array
(OVRO). We have also obtained Atacama Pathfinder Experiment (APEX) observations
of the HCN(4-3) and the HCO+(4-3) lines of the starburst disk. We find that the
emission from the HCN(1-0) and HCO+(1-0) transitions, both indicators of dense
molecular gas, trace regions which are non-distinguishable within the
uncertainties of our observations. Even though the continuum flux varies by
more than a factor 10 across the starburst disk, the HCN/HCO+ ratio is constant
throughout the disk, and we derive an average ratio of 1.1+/-0.2. From an
excitation analysis we find that all lines from both molecules are subthermally
excited and that they are optically thick. This subthermal excitation implies
that the observed HCN/HCO+ line ratio is sensitive to the underlying chemistry.
The constant line ratio thus implies that there are no strong abundance
gradients across the starburst disk of NGC253. This finding may also explain
the variations in L'(HCN)/L'(HCO+) between different star forming galaxies both
nearby and at high redshifts.
|
astro-ph
|
we have imaged the central 1kpc of the circumnuclear starburst disk in the galaxy ngc253 in the hcn10 hco10 and co10 transitions at 60pc resolution using the owens valley radio observatory millimeterwavelength array ovro we have also obtained atacama pathfinder experiment apex observations of the hcn43 and the hco43 lines of the starburst disk we find that the emission from the hcn10 and hco10 transitions both indicators of dense molecular gas trace regions which are nondistinguishable within the uncertainties of our observations even though the continuum flux varies by more than a factor 10 across the starburst disk the hcnhco ratio is constant throughout the disk and we derive an average ratio of 1102 from an excitation analysis we find that all lines from both molecules are subthermally excited and that they are optically thick this subthermal excitation implies that the observed hcnhco line ratio is sensitive to the underlying chemistry the constant line ratio thus implies that there are no strong abundance gradients across the starburst disk of ngc253 this finding may also explain the variations in lhcnlhco between different star forming galaxies both nearby and at high redshifts
|
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|
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|
707.1851
|
Three comments on the Fermi gas at unitarity in a harmonic trap
|
In this note we consider three issues related to the unitary Fermi gas in a
harmonic trap. We present a short proof of a virial theorem, which states that
the average energy of a particle system at unitarity in a harmonic trap is
twice larger than the average potential energy. The theorem is valid for all
systems with no intrinsic scale, at zero or finite temperature. We discuss the
odd-even splitting in a unitarity Fermi gas in a harmonic trap. We show that at
large number of particles N the odd-even splitting is proportional to
N^{1/9}\hbar\omega, with an undetermined numerical constant. We also show that
for odd N the lowest excitation energies are of order N^{-1/3}\hbar\omega.
|
cond-mat.other
|
in this note we consider three issues related to the unitary fermi gas in a harmonic trap we present a short proof of a virial theorem which states that the average energy of a particle system at unitarity in a harmonic trap is twice larger than the average potential energy the theorem is valid for all systems with no intrinsic scale at zero or finite temperature we discuss the oddeven splitting in a unitarity fermi gas in a harmonic trap we show that at large number of particles n the oddeven splitting is proportional to n19hbaromega with an undetermined numerical constant we also show that for odd n the lowest excitation energies are of order n13hbaromega
|
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|
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|
707.1852
|
The topology of terminal quartic 3-folds
|
In this thesis, I determine a bound on the defect of terminal Gorenstein
quartic 3-folds. More generally, I study the defect of terminal Gorenstein Fano
3-folds of Picard rank 1 and genus at least 3. I state a geometric "motivation"
of non Q-factoriality in the case of quartics.
|
math.AG
|
in this thesis i determine a bound on the defect of terminal gorenstein quartic 3folds more generally i study the defect of terminal gorenstein fano 3folds of picard rank 1 and genus at least 3 i state a geometric motivation of non qfactoriality in the case of quartics
|
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|
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|
707.1853
|
Jet/environment interactions in low-power radio galaxies
|
The interactions between low-power radio galaxies and their environments are
thought to play a crucial role in supplying energy to offset cooling in the
centres of groups and clusters. Such interactions are also important in
determining large-scale radio structures and radio-source dynamics. I will
discuss new XMM-Newton observations of the hot-gas environments of a
representative sample of nine FRI radio galaxies, which show strong evidence
for the importance of such interactions (including evidence for heating) and
provide important new constraints on source dynamics and particle content. In
particular I will show that the widely discussed apparent imbalance between the
internal lobe pressure available from relativistic electrons and magnetic field
and the external pressure of hot gas correlates with radio structure, so that
naked jets require a large contribution from non-radiating particles, whereas
lobed sources do not. This may provide the first direct observational evidence
that entrainment of the ICM supplies the missing pressure.
|
astro-ph
|
the interactions between lowpower radio galaxies and their environments are thought to play a crucial role in supplying energy to offset cooling in the centres of groups and clusters such interactions are also important in determining largescale radio structures and radiosource dynamics i will discuss new xmmnewton observations of the hotgas environments of a representative sample of nine fri radio galaxies which show strong evidence for the importance of such interactions including evidence for heating and provide important new constraints on source dynamics and particle content in particular i will show that the widely discussed apparent imbalance between the internal lobe pressure available from relativistic electrons and magnetic field and the external pressure of hot gas correlates with radio structure so that naked jets require a large contribution from nonradiating particles whereas lobed sources do not this may provide the first direct observational evidence that entrainment of the icm supplies the missing pressure
|
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|
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|
707.1854
|
Intermolecular Forces and the Glass Transition
|
Random first order transition theory is used to determine the role of
attractive and repulsive interactions in the dynamics of supercooled liquids.
Self-consistent phonon theory, an approximate mean field treatment consistent
with random first order transition theory, is used to treat individual glassy
configurations, while the liquid phase is treated using common liquid state
approximations. The transition temperature $T^{*}_{A} $, the temperature where
the onset of activated behavior is predicted by mean field theory, the lower
crossover temperature $T_{c}^{*}$ where barrierless motions actually occur
through fractal or stringy motions, and $T^{*}_{K} $, the Kauzmann temperature,
are calculated in addition to $T^{*}_{g} $, the glass transition temperature
that corresponds to laboratory cooling rates. Both the isobaric and isochoric
behavior in the supercooled regime are studied, providing results for $\Delta
C_{V} $ and $\Delta C_{p} $ that can be used to calculate the fragility as a
function of density and pressure, respectively. The predicted variations in the
$\alpha$-relaxation time with temperature and density conform to the empirical
density-temperature scaling relations found by Casalini and Roland. We thereby
demonstrate the microscopic origin of their observations. Finally, the
relationship first suggested by Sastry between the spinodal temperature and the
Kauzmann temperatures, as a function of density, is examined. The present
microscopic calculations support the existence of an intersection of these two
temperatures at sufficiently low temperatures.
|
cond-mat.soft
|
random first order transition theory is used to determine the role of attractive and repulsive interactions in the dynamics of supercooled liquids selfconsistent phonon theory an approximate mean field treatment consistent with random first order transition theory is used to treat individual glassy configurations while the liquid phase is treated using common liquid state approximations the transition temperature t_a the temperature where the onset of activated behavior is predicted by mean field theory the lower crossover temperature t_c where barrierless motions actually occur through fractal or stringy motions and t_k the kauzmann temperature are calculated in addition to t_g the glass transition temperature that corresponds to laboratory cooling rates both the isobaric and isochoric behavior in the supercooled regime are studied providing results for delta c_v and delta c_p that can be used to calculate the fragility as a function of density and pressure respectively the predicted variations in the alpharelaxation time with temperature and density conform to the empirical densitytemperature scaling relations found by casalini and roland we thereby demonstrate the microscopic origin of their observations finally the relationship first suggested by sastry between the spinodal temperature and the kauzmann temperatures as a function of density is examined the present microscopic calculations support the existence of an intersection of these two temperatures at sufficiently low temperatures
|
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|
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|
707.1855
|
The First Detailed Abundances for M giants in the inner Bulge from
Infrared Spectroscopy
|
We report the first abundance analysis of 17 M giant stars in the inner
Galactic bulge at $(l,b)=(0\deg,-1\deg)$, based on $R=25,000$ infrared
spectroscopy $(1.5-1.8 ~\mu \rm m)$ using NIRSPEC at the Keck telescope. Based
on their luminosities and radial velocities, we identify these stars with a
stellar population older than 1 Gyr. We find the iron abundance $\rm < [Fe/H] >
= -0.22 \pm 0.03$, with a $1\sigma$ dispersion of $0.14\pm 0.024$. We also find
the bulge stars have enhanced [$\rm alpha$/Fe] abundance ratio at the level of
+0.3 dex relative to the Solar stars, and low $\rm <^{12}C/^{13}C>\approx
6.5\pm 0.3$. The derived iron abundance and composition for this inner bulge
sample is indistinguishable from that of a sample of M giants our team has
previously studied in Baade's Window $(l,b)=(0.9,-4)$. We find no evidence of
any major iron abundance or abundance ratio gradient between this inner field
and Baade's window.
|
astro-ph
|
we report the first abundance analysis of 17 m giant stars in the inner galactic bulge at lb0deg1deg based on r25000 infrared spectroscopy 1518 mu rm m using nirspec at the keck telescope based on their luminosities and radial velocities we identify these stars with a stellar population older than 1 gyr we find the iron abundance rm feh 022 pm 003 with a 1sigma dispersion of 014pm 0024 we also find the bulge stars have enhanced rm alphafe abundance ratio at the level of 03 dex relative to the solar stars and low rm 12c13capprox 65pm 03 the derived iron abundance and composition for this inner bulge sample is indistinguishable from that of a sample of m giants our team has previously studied in baades window lb094 we find no evidence of any major iron abundance or abundance ratio gradient between this inner field and baades window
|
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|
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|
707.1856
|
The role of the Interstellar Medium in Galaxy Formation Simulations
|
There is a strong connection between the formation of a disk galaxy and the
properties of the interstellar medium (ISM). Theoretical work has typically
either focused on the cosmological buildup of a galaxy with a relatively crude
model for the gas physics, or examined local processes in the ISM and ignored
the global evolution of the galaxy itself. Here, I briefly review what has been
learned from both of these approaches, and what can be done to bridge the gap
between them. I argue that cosmological simulations need to learn from
observational and theoretical work on local ISM properties and adopt more
sophisticated models for the processes that they cannot resolve. Since the ISM
is still incompletely understood, there are a number of reasonable approaches
for these "subgrid" models, and I will discuss the strengths and limitations of
each.
|
astro-ph
|
there is a strong connection between the formation of a disk galaxy and the properties of the interstellar medium ism theoretical work has typically either focused on the cosmological buildup of a galaxy with a relatively crude model for the gas physics or examined local processes in the ism and ignored the global evolution of the galaxy itself here i briefly review what has been learned from both of these approaches and what can be done to bridge the gap between them i argue that cosmological simulations need to learn from observational and theoretical work on local ism properties and adopt more sophisticated models for the processes that they cannot resolve since the ism is still incompletely understood there are a number of reasonable approaches for these subgrid models and i will discuss the strengths and limitations of each
|
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|
[-0.046809083908114446, 0.08329490641481244, -0.10108850849127131, 0.12356007389358378, -0.09300847339576908, -0.10207969599203871, 0.025547518687588828, 0.4420944483950734, -0.25539334088139837, -0.30357325212763886, 0.0826477194130088, -0.2336716027231887, -0.09639591401210054, 0.16456722987641115, -0.014375560813849525, -0.0003806627821177244, 0.03297759545966983, -0.06243641912671072, -0.06605321645453971, -0.2559867176011072, 0.3523465728320714, 0.08872145832117115, 0.191281154086963, 0.04683576315998964, 0.06270470571429801, -0.11158096807609712, -0.08710761771071703, 0.035483523484851634, -0.17663615559213214, 0.09622624268564063, 0.2171375338443925, 0.15971805882873014, 0.2968310953350738, -0.5003058931391154, -0.2775760973404561, 0.08738844783511013, 0.17851399674878587, 0.10045133622895394, -0.07051106606418865, -0.23152439312211104, 0.05938410469763247, -0.16588246144820004, -0.09372949554318828, -0.022862488201021085, 0.019663577526807786, 0.022567217025373662, -0.20233340778920267, 0.07415842213751082, 0.06857499787251332, 0.06436000200254577, -0.04122090242786466, -0.09242922595502542, -0.019750939662169134, 0.13385636383318342, 0.06830983156853887, 0.03103842968620094, 0.15166551716559168, -0.19620914115969623, -0.054199070796104414, 0.43730017129065735, -0.030203826199950917, -0.13474427894689142, 0.2741792354624652, -0.15405082335429532, -0.16786707030675774, 0.05164929119221467, 0.14513594551743672, 0.05728466982421066, -0.16575328637513198, 0.06322073914883991, -0.0454899209218898, 0.16447538955004087, -0.024880637650910233, 0.044025073355442146, 0.283709688424798, 0.15215202805453112, 0.01899427341496838, 0.03816855554884699, -0.07675989211316586, -0.08083302801741021, -0.27573961856375845, -0.09987308474457157, -0.16420611269838575, 0.06560599506743268, -0.06515428788230306, -0.11524608409433443, 0.36279853031571424, 0.1850207593425044, 0.22325086152580167, 0.0145817244841185, 0.32237906622301254, 0.05552935721186389, 0.05070481434896854, 0.09078623341961897, 0.29548559683108966, 0.1262747168940093, 0.09097006980861937, -0.20388698753169074, 0.1312451513018459, 0.0012913853811499264]
|
707.1857
|
On the triplet vertex algebra W(p)
|
We study the triplet vertex operator algebra $\mathcal{W}(p)$ of central
charge $1-\frac{6(p-1)^2}{p}$, $p \geq 2$. We show that $\trip$ is
$C_2$-cofinite but irrational since it admits indecomposable and logarithmic
modules. Furthermore, we prove that $\trip$ is of finite-representation type
and we provide an explicit construction and classification of all irreducible
$\mathcal{W}(p)$-modules and describe block decomposition of the category of
ordinary $\trip$-modules. All this is done through an extensive use of Zhu's
associative algebra together with explicit methods based on vertex operators
and the theory of automorphic forms. Moreover, we obtain an upper bound for
${\rm dim}(A(\mathcal{W}(p)))$. Finally, for $p$ prime, we completely describe
the structure of $A(\trip)$. The methods of this paper are easily extendable to
other $\mathcal{W}$-algebras and superalgebras.
|
math.QA hep-th math-ph math.MP math.RT
|
we study the triplet vertex operator algebra mathcalwp of central charge 1frac6p12p p geq 2 we show that trip is c_2cofinite but irrational since it admits indecomposable and logarithmic modules furthermore we prove that trip is of finiterepresentation type and we provide an explicit construction and classification of all irreducible mathcalwpmodules and describe block decomposition of the category of ordinary tripmodules all this is done through an extensive use of zhus associative algebra together with explicit methods based on vertex operators and the theory of automorphic forms moreover we obtain an upper bound for rm dimamathcalwp finally for p prime we completely describe the structure of atrip the methods of this paper are easily extendable to other mathcalwalgebras and superalgebras
|
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|
[-0.1446224950650184, 0.060841989139142946, -0.08724087007392786, 0.05876107580588085, -0.11404553464646533, -0.17243004652361074, -0.010496035400776012, 0.38292756089287106, -0.3007471862722907, -0.2126456249725858, 0.12303171228421361, -0.2694716799040243, -0.18522619668306506, 0.1930633547078622, -0.08615984465608276, -0.041502946095230676, 0.06292633479461074, 0.1357605838216969, -0.0935600802359547, -0.28341957308932025, 0.40294020808824715, -0.007787762912349743, 0.20949160551913737, 0.07023921927126746, 0.147437789062806, 0.04181563953476909, -0.039385538576824364, -0.04770685243011828, -0.17512955868643762, 0.16155909175224797, 0.2848171419055577, 0.12071836648484398, 0.17873294646504514, -0.4113211881761488, -0.07284295411648743, 0.17545077841108045, 0.17034609747535892, 0.06417369180391624, -0.0228606772439538, -0.21234755633039432, 0.12787590637035146, -0.23337597610723032, -0.13749716084107363, -0.10902821579784677, 0.07631461912145217, -0.018219663828954492, -0.28420415120209536, 0.011415669649610655, 0.1152023505011018, 0.0995091822122432, -0.09345514406736025, -0.14521465236280245, -0.031635710448761914, 0.10338267958886399, -0.04369242385789556, 0.0038949302520210807, 0.06501835883235592, -0.08895122646680918, -0.15858940798952653, 0.29874679174993124, -0.028302596198300944, -0.19208686232664868, 0.1227665525236118, -0.13862674314530746, -0.16938925931115814, 0.0822621123097314, 0.08868186478094574, 0.13543504610935456, -0.0820421628789821, 0.18252316163546456, -0.1125618618537198, 0.08709074489633438, 0.05668486108219153, 0.016258517976670543, 0.09468298989936318, 0.11689030240175494, 0.08705511163887486, 0.13984721252059548, 0.011436768262156923, 0.007132930934363813, -0.36844824579658736, -0.19510930518108102, -0.1046265152654725, 0.09475669530506262, -0.09607899794686921, -0.1552958075741404, 0.40124521313006417, 0.13252494183140234, 0.18214301132646046, 0.12536248649682916, 0.2176427102010501, 0.1193450292605057, 0.08315934056187407, 0.09514855595485291, 0.13284342677389646, 0.17216527069869794, -0.03274167910332612, -0.16382655645353034, -0.03507968413708895, 0.18013030974390476]
|
707.1858
|
Anisotropic surface reaction limited phase transformation dynamics in
LiFePO4
|
A general continuum theory is developed for ion intercalation dynamics in a
single crystal of a rechargeable battery cathode. It is based on an existing
phase-field formulation of the bulk free energy and incorporates two crucial
effects: (i) anisotropic ionic mobility in the crystal and (ii) surface
reactions governing the flux of ions across the electrode/electrolyte
interface, depending on the local free energy difference. Although the phase
boundary can form a classical diffusive "shrinking core" when the dynamics is
bulk-transport-limited, the theory also predicts a new regime of
surface-reaction-limited (SRL) dynamics, where the phase boundary extends from
surface to surface along planes of fast ionic diffusion, consistent with recent
experiments on LiFePO4. In the SRL regime, the theory produces a fundamentally
new equation for phase transformation dynamics, which admits traveling-wave
solutions. Rather than forming a shrinking core of untransformed material, the
phase boundary advances by filling (or emptying) successive channels of fast
diffusion in the crystal. By considering the random nucleation of SRL
phase-transformation waves, the theory predicts a very different picture of
charge/discharge dynamics from the classical diffusion-limited model, which
could affect the interpretation of experimental data for LiFePO4.
|
cond-mat.mtrl-sci
|
a general continuum theory is developed for ion intercalation dynamics in a single crystal of a rechargeable battery cathode it is based on an existing phasefield formulation of the bulk free energy and incorporates two crucial effects i anisotropic ionic mobility in the crystal and ii surface reactions governing the flux of ions across the electrodeelectrolyte interface depending on the local free energy difference although the phase boundary can form a classical diffusive shrinking core when the dynamics is bulktransportlimited the theory also predicts a new regime of surfacereactionlimited srl dynamics where the phase boundary extends from surface to surface along planes of fast ionic diffusion consistent with recent experiments on lifepo4 in the srl regime the theory produces a fundamentally new equation for phase transformation dynamics which admits travelingwave solutions rather than forming a shrinking core of untransformed material the phase boundary advances by filling or emptying successive channels of fast diffusion in the crystal by considering the random nucleation of srl phasetransformation waves the theory predicts a very different picture of chargedischarge dynamics from the classical diffusionlimited model which could affect the interpretation of experimental data for lifepo4
|
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|
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|
707.1859
|
On the Degrees of Freedom in Cognitive Radio Channels
|
After receiving useful peer comments, we would like to withdraw this paper.
|
cs.IT math.IT
|
after receiving useful peer comments we would like to withdraw this paper
|
[['after', 'receiving', 'useful', 'peer', 'comments', 'we', 'would', 'like', 'to', 'withdraw', 'this', 'paper']]
|
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|
707.186
|
The Gauss-Bonnet-Grotemeyer Theorem in spaces of constant curvature
|
In 1963, K.P.Grotemeyer proved an interesting variant of the Gauss-Bonnet
Theorem. Let M be an oriented closed surface in the Euclidean space R^3 with
Euler characteristic \chi(M), Gauss curvature G and unit normal vector field n.
Grotemeyer's identity replaces the Gauss-Bonnet integrand G by the normal
moment <a,n>^2G, where $a$ is a fixed unit vector. Grotemeyer showed that the
total integral of this integrand is (2/3)pi times chi(M).
We generalize Grotemeyer's result to oriented closed even-dimesional
hypersurfaces of dimension n in an (n+1) ndimensional space form N^{n+1}(k).
|
math.DG
|
in 1963 kpgrotemeyer proved an interesting variant of the gaussbonnet theorem let m be an oriented closed surface in the euclidean space r3 with euler characteristic chim gauss curvature g and unit normal vector field n grotemeyers identity replaces the gaussbonnet integrand g by the normal moment an2g where a is a fixed unit vector grotemeyer showed that the total integral of this integrand is 23pi times chim we generalize grotemeyers result to oriented closed evendimesional hypersurfaces of dimension n in an n1 ndimensional space form nn1k
|
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|
[-0.26371539795748244, 0.13437762787406776, -0.056147617385665205, 0.031598829062092174, -0.09737296188882563, -0.14804813807347306, -0.0430086771174288, 0.29558622738185486, -0.2485320734113087, -0.21209004283365276, 0.03310239113102679, -0.2568759524499147, -0.15136903767577475, 0.16164583149136125, -0.14345041672227743, -0.04431118449932079, -0.012583976358543207, 0.14513284954483863, -0.061562774182630724, -0.3326536527156462, 0.33657728843850854, -0.09445054468089416, 0.21037699859359382, 0.01955443925086271, 0.13245135698651458, 0.046735220680726164, 0.04272495173377755, 0.05368205682693601, -0.16496597297454071, 0.10572408643309716, 0.2152619919463716, 0.05805706071529399, 0.20903301408606362, -0.3891175194516962, -0.17939749260341037, 0.16552270795391114, 0.12040063064332683, -0.0806682098104998, 0.03296619408798439, -0.24117905775338044, 0.08074119240965372, -0.052950425188482544, -0.2177926382843267, -0.014070263963169705, 0.12773114849416609, -0.056612596588416234, -0.26856153549189554, 0.0024319183322842474, 0.1286144632110257, 0.07701562113921952, -0.05581339400974505, -0.13138953337077924, -0.04792610726054804, 0.03643870578912075, 0.030174874746597108, 0.22680158917159762, 0.050117867696242706, -0.056882021071987206, -0.07826964226321398, 0.3275127207089997, -0.15558408144401548, -0.28098922533293563, 0.015545806646301055, -0.20023378491240704, -0.1225385494231258, 0.1503138436395445, 0.11057802684099217, 0.20040996478479586, -0.06583975669410494, 0.2691374123434214, -0.1074317024997723, 0.08953935887526583, 0.1382589749187047, -0.0746309802763992, 0.11957182457820041, 0.034720822524877244, 0.11852196757581061, 0.16356860165754447, -0.052511344790274715, -0.025069267621240867, -0.3695710353254352, -0.2900854922934539, -0.21503231499378603, 0.20494298970349778, -0.2042197702439246, -0.17341402835316128, 0.28288183221880947, -0.03761891852259452, 0.18278128987201203, 0.11448155498752992, 0.23980946464027153, 0.12542364862460045, 0.057085021498130155, 0.15367818965266147, 0.08677760601319649, 0.22857670902481508, 0.0009972271681935698, -0.15270633794321323, -0.052346296106137474, 0.21965192914308038]
|
707.1861
|
Global analysis of proton elastic form factor data with two-photon
exchange corrections
|
We use the world's data on elastic electron--proton scattering and
calculations of two-photon exchange effects to extract corrected values of the
proton's electric and magnetic form factors over the full Q^2 range of the
existing data. Our analysis combines the corrected Rosenbluth cross section and
polarization transfer data, and is the first extraction of G_Ep and G_Mp
including explicit two-photon exchange corrections and their associated
uncertainties. In addition, we examine the angular dependence of the corrected
cross sections, and discuss the possible nonlinearities of the cross section as
a function of epsilon.
|
nucl-ex nucl-th
|
we use the worlds data on elastic electronproton scattering and calculations of twophoton exchange effects to extract corrected values of the protons electric and magnetic form factors over the full q2 range of the existing data our analysis combines the corrected rosenbluth cross section and polarization transfer data and is the first extraction of g_ep and g_mp including explicit twophoton exchange corrections and their associated uncertainties in addition we examine the angular dependence of the corrected cross sections and discuss the possible nonlinearities of the cross section as a function of epsilon
|
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|
[-0.09163681938029501, 0.07278277810774339, -0.057513132073876004, 0.13017907481179977, -0.020761902600972226, -0.028545394980186677, 0.03657602265720134, 0.3579146467432704, -0.23271591827759278, -0.3064435312079023, -0.007202076271388923, -0.37033846209574817, -0.03352426169136458, 0.1935886686753846, 0.08535113986505641, 0.0828108676323609, 0.051280618587043136, -0.015126173364241486, -0.07437606620078441, -0.17242825741034365, 0.3623907853768248, 0.08902225309841173, 0.2580127704422921, 0.1828331174986923, 0.1354472558305133, 0.12210042913363356, -0.11057223768844067, -0.03649085958528778, -0.1700013761368135, 0.14632567275143432, 0.2239526197132047, 0.04070760108753229, 0.11951260554158817, -0.3961769308105273, -0.11016960082697155, 0.06949278471343544, 0.10359367889949404, 0.14312521878467954, 0.005168740170673751, -0.233068007307694, -0.00862501000823534, -0.21036285429221133, -0.08953220024578394, -0.13863314211915206, 0.041119973762365786, 0.030961041217264923, -0.31066422573412245, 0.0880231319056095, -0.002962572378632815, 0.021476027587951925, -0.07324305192425686, -0.18094345981396898, -0.05000159534139802, 0.10563296631849169, 0.07087487448766099, 0.0056907192135796595, 0.1776416415206926, -0.1448619924207299, -0.11169522912393365, 0.36247672559693456, -0.07372804434018453, -0.14587454324709656, 0.05305069442028585, -0.18225085165392121, -0.05824878232543478, 0.16659307402163825, 0.24329963018080097, 0.09953338169472535, -0.13556419300806263, 0.10835139141177617, 0.06349546330570972, 0.17729956689088242, 0.09885410151606344, 0.038553962473879044, 0.0979984789357885, 0.1351498589425793, -0.07059712363305785, 0.07007809829614732, -0.18735207462210066, -0.06764000782846857, -0.3814245249428179, -0.12258872062818188, -0.08700996602925917, 0.05408851016925283, -0.10632784989976916, -0.12114976427477339, 0.32293948051064153, 0.1328006243414205, 0.26067290006397775, 0.006427291669356434, 0.3787657303290199, 0.1322215248137186, 0.10517833394798166, 0.030664765053307234, 0.3086951073745023, 0.20006565839993645, 0.12443591428809272, -0.238768936939659, 0.07920838453624722, -0.027487888962597302]
|
707.1862
|
Casimir forces between arbitrary compact objects
|
We develop an exact method for computing the Casimir energy between arbitrary
compact objects, either dielectrics or perfect conductors. The energy is
obtained as an interaction between multipoles, generated by quantum current
fluctuations. The objects' shape and composition enter only through their
scattering matrices. The result is exact when all multipoles are included, and
converges rapidly. A low frequency expansion yields the energy as a series in
the ratio of the objects' size to their separation. As an example, we obtain
this series for two dielectric spheres and the full interaction at all
separations for perfectly conducting spheres.
|
cond-mat.stat-mech hep-th quant-ph
|
we develop an exact method for computing the casimir energy between arbitrary compact objects either dielectrics or perfect conductors the energy is obtained as an interaction between multipoles generated by quantum current fluctuations the objects shape and composition enter only through their scattering matrices the result is exact when all multipoles are included and converges rapidly a low frequency expansion yields the energy as a series in the ratio of the objects size to their separation as an example we obtain this series for two dielectric spheres and the full interaction at all separations for perfectly conducting spheres
|
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|
[-0.15430061824201624, 0.14917772651898878, -0.054658374587568094, 0.07032186771999588, -0.020959548488240307, -0.08208065745135655, -0.004063459224903918, 0.39405250344045306, -0.25068259092846085, -0.30672564008273184, 0.053533321886789054, -0.29822640332906525, -0.07906888341246059, 0.2058701145686019, 0.04160586962172268, 0.0035907856511826416, 0.021705124023541505, 0.030528313603860383, -0.0661186342144252, -0.19573413801132417, 0.3018156028404946, 0.07308799462103076, 0.24162291377136597, 0.053456322114192406, 0.08722823490483725, 0.04380717831996402, 0.02490284341406457, 0.04497772158712757, -0.11267060987955453, 0.09494284570825343, 0.26455711219958694, 0.01561782170771336, 0.19472228996075538, -0.41678292551363, -0.15491172318745935, 0.08040586175701143, 0.11814173851969975, 0.13048369409896585, -0.05113574304161783, -0.23782413341912764, 0.068443716902818, -0.1873584179497533, -0.13662328260798692, -0.09661021411932093, 0.041754329634108106, 0.046367817159209936, -0.2751266218113656, 0.08775749852006533, 0.07533607000903207, 0.04442970023243403, -0.09386447034015948, -0.12595454666155334, 0.02906783959562225, 0.17903731534957212, 0.034555304154031435, -0.02728518591813591, 0.1323159675836107, -0.14406747430591482, -0.055389221626980116, 0.3744614313413598, -0.04507126977990324, -0.22345110023280187, 0.20706107144063451, -0.13113916897671107, -0.013311448411978021, 0.1464022522107983, 0.1353707183009888, 0.14114755306515264, -0.12672408786320188, 0.09556883674831253, 0.018567292993812233, 0.17629424562649232, 0.12392975557690525, 0.024715301675760016, 0.2672869258712293, 0.0948580965347474, 0.06038319679661369, 0.15649225670198091, -0.07021774657127657, -0.03945123170958642, -0.3001878638656772, -0.159924432062734, -0.24820967725767962, 0.045075151903022616, -0.12925982435322392, -0.2287645906552064, 0.3258667934367585, 0.0628171437419951, 0.23766918935603937, 0.0924129491548377, 0.33770123991773143, 0.12474376952860086, 0.03931460264423976, 0.08027661870927455, 0.2490053792693177, 0.1314441730691196, 0.08768160746204762, -0.18820437973564758, 0.0010886526314959843, 0.04928466889589113]
|
707.1863
|
A no-pure-boost uncertainty principle from spacetime noncommutativity
|
We study boost and space-rotation transformations in kappa-Minkowski
noncommutative spacetime, using the techniques that some of us had previously
developed (hep-th/0607221) for a description of translations in
kappa-Minkowski, which in particular led to the introduction of translation
transformation parameters that do not commute with the spacetime coordinates.
We find a similar description of boosts and space rotations, which allows us to
identify some associated conserved charges, but the form of the commutators
between transformation parameters and spacetime coordinates is incompatible
with the possibility of a pure boost.
|
hep-th
|
we study boost and spacerotation transformations in kappaminkowski noncommutative spacetime using the techniques that some of us had previously developed hepth0607221 for a description of translations in kappaminkowski which in particular led to the introduction of translation transformation parameters that do not commute with the spacetime coordinates we find a similar description of boosts and space rotations which allows us to identify some associated conserved charges but the form of the commutators between transformation parameters and spacetime coordinates is incompatible with the possibility of a pure boost
|
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|
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|
707.1864
|
Normal mode coupling and Bloch states in elliptically birefringent 1D
photonic crystals
|
An analysis is presented of frequency versus wave-vector dispersion in
elliptically birefringent one-dimensional layered periodic structures. The
presence of local normal mode polarization state variations from one layer to
the next is found to lead to mode coupling and to affect the wave-vector
dispersion and the character of the Bloch states of the system.
|
physics.optics
|
an analysis is presented of frequency versus wavevector dispersion in elliptically birefringent onedimensional layered periodic structures the presence of local normal mode polarization state variations from one layer to the next is found to lead to mode coupling and to affect the wavevector dispersion and the character of the bloch states of the system
|
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|
[-0.23145006022726497, 0.16359954771690322, -0.06833559650651834, -0.027906595078227972, -0.1068090507760644, -0.09624587396090781, 0.047932974420729337, 0.39508521805206936, -0.3281651458668488, -0.2215452269754476, 0.03144087349883867, -0.2798462087909381, -0.1154974756969346, 0.1849496393567986, 0.045538820740249425, 0.020881469663301552, -0.01762119575438124, -0.0003061250964593556, -0.027755560525865468, -0.14363942374647767, 0.3424475762165255, 0.04574737014869849, 0.38825140996939606, -0.015824924326605268, 0.0386897928374647, 0.03799958832786177, 0.06317748198354686, -0.030182960615665826, -0.06902532914170513, 0.08061854840855597, 0.21232926288050497, -0.05984390157930277, 0.16819369706542972, -0.4183388649727459, -0.20004562712791893, 0.023608433393140633, 0.13601790566463023, 0.1459177362008227, 0.015219206279316158, -0.28083817539219225, 0.03298658886234517, -0.10871567528401674, -0.21378060920095002, -0.046289712363095196, 0.004953596930674932, 0.006493274053489721, -0.24022830029328665, 0.13079388994999505, 0.06777815807058855, 0.042683214604578634, -0.09064650418305839, -0.07476963308700188, -0.11543977464100828, 0.08492785814666638, 0.07041756357756201, 0.019854044317509287, 0.09304752274302128, -0.12543209460650193, -0.07046653548497017, 0.3900739009388619, -0.09908321439029856, -0.19097280933918362, 0.15307219864593613, -0.18009671836194616, 0.013316149556043523, 0.1700642783953636, 0.18958165279279152, 0.05834050550711928, -0.05220080104751374, 0.016757569963509147, 0.007799165547583942, 0.2645576755398738, 0.09931399697368895, 0.10248892123086585, 0.23848249673567437, 0.1312914061860216, 0.038544288456991864, 0.12629081534773665, -0.14823066805385882, -0.07195992065869548, -0.24290670163032632, -0.1453500308993238, -0.1565850993124682, -0.012856725239005216, -0.03613147499951689, -0.2300485870455978, 0.4847045021511062, 0.07831716946222717, 0.162154385043929, -0.04608591287224381, 0.25025591960487265, 0.16881203152998178, 0.05646143324190268, 0.03279474263803826, 0.3268262824362696, 0.19572699185098624, 0.06977088788644997, -0.29619659238098256, 0.03499236283823848, -0.0161890159447298]
|
707.1865
|
Superhump periods in the UGSU-type dwarf nova SDSSp J082409.73+493124.4
|
We present observations and analysis of the first reported superoutburst of
the dwarf nova SDSSp J082409.73+493124.4 during February/March 2007. From a
maximum observed magnitude of 15.4C it declined at 0.09 mag/d for 7 days,
flattened out around magnitude 16 for a further 5 days and then returned
rapidly to quiescence at magnitude 19.4. The flattening of the light curve late
in the outburst was not associated with a re-growth of superhumps. For the
first 5 days we observed common superhumps with period 0.06954(5) d, thus
confirming its classification as a UGSU-type dwarf nova. This was followed by a
phase transition to late superhumps with period 0.06921(6) d. We found a small
but persistent signal at 0.0687(6) d which we interpret as the orbital period.
|
astro-ph
|
we present observations and analysis of the first reported superoutburst of the dwarf nova sdssp j082409734931244 during februarymarch 2007 from a maximum observed magnitude of 154c it declined at 009 magd for 7 days flattened out around magnitude 16 for a further 5 days and then returned rapidly to quiescence at magnitude 194 the flattening of the light curve late in the outburst was not associated with a regrowth of superhumps for the first 5 days we observed common superhumps with period 0069545 d thus confirming its classification as a ugsutype dwarf nova this was followed by a phase transition to late superhumps with period 0069216 d we found a small but persistent signal at 006876 d which we interpret as the orbital period
|
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|
[-0.08582382943773231, 0.14473195973846872, -0.12477078999913598, 0.0209930816584393, -0.0604726116378176, -0.13448376001363968, 0.11513023755426313, 0.380096604731881, -0.18077325684578804, -0.3651456128474388, 0.144836695303438, -0.3128122640773654, -0.10400834048987698, 0.1922053180445554, -0.08887746385535446, -0.006688191757194098, 0.11275205544148714, 0.00103719811886549, -0.11293038873443917, -0.3493178217371894, 0.18908616809876858, 0.03672243774694912, 0.10916628605405942, -0.0634467548225075, 0.04003279818758621, -0.03733196223975491, -0.06173659775823442, -0.10751816708499849, -0.12404754978478334, -0.04924056620605416, 0.21764441460698558, 0.08116708493838876, 0.2058545001782477, -0.3283288429601718, -0.17038627235629297, 0.08725364868316042, 0.14790313648922226, 0.018765628672307515, -0.0007364431048853923, -0.23373276539841445, 0.09894549914919851, -0.19332490602342445, -0.1795734426961675, 0.07599475713036323, 0.21506146916140945, -0.07765276194944726, -0.21723118787670856, 0.15162488160718043, 0.06324250317746931, 0.14003279394770074, -0.13237949566406562, -0.1161718777917578, -0.05309214376276201, 0.019287951807570407, 0.10062413840254737, 0.14582987132450662, 0.043691660340685966, -0.03138306851190972, -0.08940035472347764, 0.3260394552154309, -0.15548705041084943, 0.13334567521272575, 0.17729918130918138, -0.20399361266754568, -0.10642809454367448, 0.22218128034876564, 0.13788270946667072, 0.08758742513008795, -0.10190248863882054, -0.09315688992254594, 0.05339206487011417, 0.23561816451029252, 0.1182643960573379, -0.03540139079441206, 0.31145556260026613, 0.18175553174006706, -0.02898701126647766, 0.10865899917799822, -0.2409825843400756, -0.009439392388261601, -0.2346805061324168, -0.0971532530185591, -0.13820790594948804, 0.1032180459825845, -0.10104082779681618, -0.06620925315261139, 0.45557127765900757, 0.034023955764280536, 0.27993791915428967, 0.030418931231320976, 0.22951328285212108, 0.10209057373349886, 0.06944460208985019, 0.15349840776900114, 0.3482553576892715, 0.13110887265756285, 0.2107331601082016, -0.20985094378347177, 0.11171390965257345, -0.002065039523956129]
|
707.1866
|
Hotspots, Jets and Environments
|
I discuss the nature of `hotspots' and `jet knots' in the kpc-scale
structures of powerful radio galaxies and their relationship to jet-environment
interactions. I describe evidence for interaction between the jets of FRI
sources and their local environments, and discuss its relationship to particle
acceleration, but the main focus of the paper is the hotspots of FRIIs and on
new observational evidence on the nature of the particle acceleration
associated with them.
|
astro-ph
|
i discuss the nature of hotspots and jet knots in the kpcscale structures of powerful radio galaxies and their relationship to jetenvironment interactions i describe evidence for interaction between the jets of fri sources and their local environments and discuss its relationship to particle acceleration but the main focus of the paper is the hotspots of friis and on new observational evidence on the nature of the particle acceleration associated with them
|
[['i', 'discuss', 'the', 'nature', 'of', 'hotspots', 'and', 'jet', 'knots', 'in', 'the', 'kpcscale', 'structures', 'of', 'powerful', 'radio', 'galaxies', 'and', 'their', 'relationship', 'to', 'jetenvironment', 'interactions', 'i', 'describe', 'evidence', 'for', 'interaction', 'between', 'the', 'jets', 'of', 'fri', 'sources', 'and', 'their', 'local', 'environments', 'and', 'discuss', 'its', 'relationship', 'to', 'particle', 'acceleration', 'but', 'the', 'main', 'focus', 'of', 'the', 'paper', 'is', 'the', 'hotspots', 'of', 'friis', 'and', 'on', 'new', 'observational', 'evidence', 'on', 'the', 'nature', 'of', 'the', 'particle', 'acceleration', 'associated', 'with', 'them']]
|
[-0.13732925458073927, 0.09377723066265592, -0.07082014460158664, 0.16064334294221932, -0.1028252964735859, -0.08469356888154936, 0.04072336247352521, 0.44226761420981753, -0.21205228775054114, -0.3063383225687883, 0.05096117935318034, -0.2658000547801041, -0.09402138642811526, 0.17221944948929982, 0.02631134371040389, -0.07311853505234467, 0.009033319229880968, -0.08139885718830758, -0.005703316018399265, -0.1573218501936127, 0.39199059798071784, 0.11990905506536365, 0.23255528982796628, 0.06505947547783661, 0.10514041300888897, -0.07367377159082228, -0.13668430261572617, -0.009066057779515782, -0.11448007209320268, 0.13794290526614836, 0.15966563779268958, 0.14024712200949174, 0.2076054262650157, -0.4379696430793653, -0.17211063818023023, 0.0666256421051609, 0.1612937749240599, 0.014575745425342271, -0.09517991428987847, -0.26960008377985406, 0.07071776476611073, -0.1825105459946725, -0.1398104277258325, 0.03096714962480797, 0.062784404726699, 0.10072559986211774, -0.1460300917775991, 0.11988080287119374, 0.07177357134383379, 0.06344354397151619, -0.07129596994976357, -0.02506495977933001, 0.013228694882450832, 0.11439679878013623, 0.11663268857713167, 0.013857995224599209, 0.14455816423934367, -0.222599932561732, -0.1573726033158083, 0.4209902064046926, 0.06158244298745154, -0.07252212878019135, 0.34952840090004933, -0.18249205598193738, -0.1721003677100978, 0.09086855921325171, 0.22045786370937195, 0.07391543301572609, -0.09398588114870815, 0.01552534959288702, 0.020399450499098748, 0.12226563681744868, -0.03231395266549145, 0.0890301637377383, 0.2650689027375645, 0.10333081614226103, 0.028947750203466665, 0.1231828521963002, -0.171524693935175, -0.048308870561110474, -0.31284264726046884, -0.1670508733433154, -0.12440568575402722, 0.017330997047894117, -0.11804967857278825, -0.11596635290495921, 0.44018863710678285, 0.12438694315238132, 0.20972179251516032, 0.03216801197332744, 0.28201171418186277, 0.034550400295605264, 0.027985787200224068, 0.13245081604691222, 0.2987843192855103, 0.17207024016210604, 0.0873286457434814, -0.22417095348161334, 0.08266167118886693, 0.00400756918437158]
|
707.1867
|
Universal features of QCD dynamics in hadrons and nuclei at high
energies
|
We discuss the empirical evidence for a universal Color Glass Condensate and
outline prospects for further studies at future colliders. Some ramifications
for initial conditions in heavy ion collisions are pointed out.
|
hep-ph nucl-th
|
we discuss the empirical evidence for a universal color glass condensate and outline prospects for further studies at future colliders some ramifications for initial conditions in heavy ion collisions are pointed out
|
[['we', 'discuss', 'the', 'empirical', 'evidence', 'for', 'a', 'universal', 'color', 'glass', 'condensate', 'and', 'outline', 'prospects', 'for', 'further', 'studies', 'at', 'future', 'colliders', 'some', 'ramifications', 'for', 'initial', 'conditions', 'in', 'heavy', 'ion', 'collisions', 'are', 'pointed', 'out']]
|
[-0.07414269348373637, 0.22055855797952972, -0.13837431122374255, 0.18211022560717538, 0.00733635439974023, -0.16130613996938337, 0.027597561245784163, 0.4639167399145663, -0.15312692895531654, -0.17152483407699037, 0.11300214728908031, -0.29568449905491434, -0.033130689640529454, 0.2159957832773216, 0.04585642460733652, 0.12794989472604357, 0.1270089361059945, -0.04660158808110282, -0.09233700131881051, -0.24739414564101025, 0.3004073772463016, 0.08800490625435486, 0.2546021749731153, 0.2482898425660096, 0.011200997527339496, 0.03915270803554449, -0.06268977445142809, 0.0006132781272754073, -0.20222806234869495, -0.003313259606329666, 0.27459139708662406, 0.10666666826000437, 0.2468535165535286, -0.4214126194710843, -0.20236982111237012, 0.1271096547425259, 0.1417707089713076, 0.1956216954276897, -0.21356073505012318, -0.24774191147298552, 0.07931497561185097, -0.19600430026184767, -0.24478914457722567, -0.10911904132808559, 0.09241608847514726, 0.02213041635695845, -0.29216067140805535, 0.023743844125419855, -0.007024123537121341, 0.1208334645780269, -0.07029597704240587, -0.24440857046283782, 0.007671911138459109, -0.03327210486168042, 0.04096315530478023, -0.02193949387583416, 0.16362851021403912, -0.21570061368765892, -0.13480227938271128, 0.35110361967235804, -0.013255379715701565, -0.08054216316668317, 0.19927873314736644, -0.15683697949862108, -0.22296436793112662, 0.011292946632238454, 0.18504169568041107, 0.03411438659531996, -0.1539907481346745, 0.03280783092304773, -0.002637385972775519, 0.04972607138790863, 0.07415018828760367, 0.11909498821478337, 0.3796502299956046, 0.24827619470306672, -0.007296238138223998, 0.14216570610778945, -0.08784295237273909, -0.05571226074243896, -0.44113697367720306, -0.188130636990536, -0.0525797169393627, 0.0019071395945502445, -0.03950832321379494, 0.014455068128881976, 0.3359042515512556, 0.2305857670144178, 0.23482610355131328, -0.03414281806908548, 0.2301338630495593, 0.019543734641047195, -0.01732815956347622, 0.031129472627071664, 0.2897118884620795, 0.0909743053780403, 0.12688865146628814, -0.22629050028626807, -0.0013788707146886736, 0.016477229568408802]
|
707.1868
|
Experimental imaging and atomistic modeling of electron and hole
quasiparticle wave functions in InAs/GaAs quantum dots
|
We present experimental magnetotunneling results and atomistic
pseudopotential calculations of quasiparticle electron and hole wave functions
of self-assembled InAs/GaAs quantum dots. The combination of a predictive
theory along with the experimental results allows us to gain direct insight
into the quantum states. We monitor the effects of (i) correlations, (ii)
atomistic symmetry and (iii) piezoelectricity on the confined carriers and (iv)
observe a peculiar charging sequence of holes that violates the Aufbau
principle.
|
cond-mat.mtrl-sci
|
we present experimental magnetotunneling results and atomistic pseudopotential calculations of quasiparticle electron and hole wave functions of selfassembled inasgaas quantum dots the combination of a predictive theory along with the experimental results allows us to gain direct insight into the quantum states we monitor the effects of i correlations ii atomistic symmetry and iii piezoelectricity on the confined carriers and iv observe a peculiar charging sequence of holes that violates the aufbau principle
|
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|
[-0.11863648203880947, 0.1333456061754937, -0.10174264646556279, 0.0668159342077497, -0.02660048663718243, -0.18272635296038162, 0.1068630166198701, 0.3779208956618015, -0.22444239631295204, -0.2707989790464101, -0.03976751187053184, -0.339155153821307, -0.12783266377494965, 0.16435649923099946, 0.04979110220829918, 0.05383627185094081, 0.04490351651146153, -0.10452450356567405, -0.08917040714343423, -0.14223616905765582, 0.2670966378693813, 0.04957087715921847, 0.3185004584159549, 0.13524858877445534, 0.09230868772233594, 0.04626544045080265, 0.04523843498135062, 0.044217220188616076, -0.19533735085392373, 0.14485474309982885, 0.21312837684782196, 0.011477575822388881, 0.23167817161916054, -0.534034449760228, -0.19220394218876347, -0.043745256202895044, 0.12886906331022308, 0.1883006514247813, -0.0875702495591026, -0.30459791076790593, 0.04371578844697916, -0.16077745241935887, -0.10827447610511763, -0.08666906500719998, -0.03049026982705683, 0.02231559037447792, -0.25863980854006663, 0.10213784942058973, 0.036927067158003785, 0.009489879932965005, -0.09569499369356654, -0.06694559347241709, -0.015081636837288125, 0.09032464255770184, 0.007263165273486752, -0.02141015479111508, 0.20218642634078096, -0.07007918584603842, -0.17694735194058858, 0.36741173704958535, -0.02206182416069181, -0.1151989932771619, 0.1466909166782686, -0.18907839063976012, -0.08944392167286921, 0.11103221705208903, 0.11332590030888988, 0.08297525533181552, -0.098921012085518, 0.08591184044601269, 0.004501697894589248, 0.19155881464583416, -0.0038943405148305307, 0.1310463653915651, 0.2446891837466304, 0.1324227037393067, -0.0020350967278729565, 0.09881624391251435, -0.14292834437299162, -0.12574795951224763, -0.2981851647722803, -0.20910266859533444, -0.2168701674074751, 0.12284399290016552, -0.06607343989770464, -0.16245402742738593, 0.44394887298064895, 0.11736560043279234, 0.1153293124667994, 0.006812894448944151, 0.22331533625935027, 0.0930926132666534, 0.05953998762272196, -0.006183852722281462, 0.24046404496447682, 0.18411022545259498, 0.0701932311249412, -0.3269719449573592, 0.007185143705661574, 0.0043594024801142]
|
707.1869
|
New Phases of SU(3) and SU(4) at Finite Temperature
|
The addition of an adjoint Polyakov loop term to the action of a pure gauge
theory at finite temperature leads to new phases of SU(N) gauge theories. For
SU(3), a new phase is found which breaks Z(3) symmetry in a novel way; for
SU(4), the new phase exhibits spontaneous symmetry breaking of Z(4) to Z(2),
representing a partially confined phase in which quarks are confined, but
diquarks are not. The overall phase structure and thermodynamics is consistent
with a theoretical model of the effective potential for the Polyakov loop based
on perturbation theory.
|
hep-lat
|
the addition of an adjoint polyakov loop term to the action of a pure gauge theory at finite temperature leads to new phases of sun gauge theories for su3 a new phase is found which breaks z3 symmetry in a novel way for su4 the new phase exhibits spontaneous symmetry breaking of z4 to z2 representing a partially confined phase in which quarks are confined but diquarks are not the overall phase structure and thermodynamics is consistent with a theoretical model of the effective potential for the polyakov loop based on perturbation theory
|
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|
[-0.1383938664315088, 0.277370044377148, -0.12318824064840878, 0.06373093080186155, -0.07364516662714142, -0.14716267425026144, 0.06456582980626012, 0.37898286998832736, -0.17017038735330745, -0.2314913877065704, 0.049010292994939995, -0.2525992780042592, -0.11335147899245063, 0.03816456337940068, -0.0020895575984351098, 0.012234968280980503, -0.08868173774211638, 0.0685525989129899, -0.1419235518582726, -0.21457820371424238, 0.2978242850031263, -0.00851938481472673, 0.2880744607918846, 0.08730143826374764, 0.08635364248547503, -0.07927972846414133, 0.039798968081032074, -0.005886235104132724, -0.03480446465834174, 0.05749087441732646, 0.15500109312274762, -0.03221490637208986, 0.13492906390268716, -0.40060184562518714, -0.24788523121907186, 0.0597556824445404, 0.14935504696181706, 0.17716575098244014, -0.09477182126839355, -0.31716481460038054, 0.04860736121754012, -0.18118559434929843, -0.18299718095260042, -0.11381576231290255, -0.021959037339735414, -0.14448210747251589, -0.284151173089706, 0.13148769152054052, -0.0002979801927683174, 0.08490141571539464, -0.034055046874889604, -0.06154633007983687, -0.094427062664181, 0.08537945191385926, 0.08377149248350492, 0.11952578139200967, 0.08879675334870255, -0.20097745515741608, -0.13534071586865892, 0.46185749965489553, -0.05977981562616043, -0.1253798013673194, 0.16028646982315006, -0.1298661300818929, -0.18170271714728686, 0.1466191919640668, 0.13220074728772205, 0.11573858798972221, -0.15643554584496225, 0.1488172042988471, -0.01113036615393495, 0.19840821563716857, -0.008761603843360659, 0.014613675494347849, 0.2836913329258721, 0.14758837383530873, 0.05135028389713136, 0.13777423788222573, 0.0022400566201496827, -0.21274278870713648, -0.3863285026683282, -0.1170152740487929, -0.10079111758449305, 0.03113139887676469, -0.12294329465000756, -0.19361858816957603, 0.43050658431464944, 0.11891116799100712, 0.17696422251862703, 0.0451333353781612, 0.22857112744422528, 0.1295349426086872, 0.09276494404841815, 0.016707353223796174, 0.25275379896003713, 0.19884244794832162, 0.06118418477095103, -0.28194206269077393, -0.08254238198541346, 0.16811096599645992]
|
707.187
|
Melting the Color Glass Condensate at the LHC
|
The charged particle multiplicity in central AA collisions and the production
of heavy flavors in pA collisions at the LHC is predicted in the CGC framework.
|
nucl-th
|
the charged particle multiplicity in central aa collisions and the production of heavy flavors in pa collisions at the lhc is predicted in the cgc framework
|
[['the', 'charged', 'particle', 'multiplicity', 'in', 'central', 'aa', 'collisions', 'and', 'the', 'production', 'of', 'heavy', 'flavors', 'in', 'pa', 'collisions', 'at', 'the', 'lhc', 'is', 'predicted', 'in', 'the', 'cgc', 'framework']]
|
[-0.028982681992392127, 0.2892519464859596, -0.19473595499920732, 0.15429619673299244, 0.18480274357044926, -0.08891699305520608, -0.15206470813315648, 0.3067554057790683, -0.16678423355691707, -0.24600343485004628, -0.13541077739612845, -0.39878459905202573, 0.1929217270360543, 0.003992934447104255, 0.025975658558309078, 0.1035521998643302, 0.13638464189492738, 0.06118801123319337, 0.042696826213684216, -0.2031262748552343, 0.26914284403364247, 0.11304355269441238, 0.22164166862001786, 0.24091779383329245, 0.00483038888957638, 0.17305224080784962, -0.007882531076365221, 0.006890930521946687, -0.10243010943612227, 0.08171389665893422, 0.27551259616246593, 0.03390343932551332, 0.10657703224569559, -0.33713100170000243, -0.0675729548272032, 0.12157305086461398, 0.17702953757431644, 0.11898285257988252, -0.12503761113979495, -0.17641833804261225, 0.1525966694148687, -0.29271699918004185, -0.19468157573674733, 0.11537951539055659, 0.028003613392894085, 0.00650905344921809, -0.3676169743904701, 0.11038542051727955, -0.051436178744412385, 0.12489541577927482, 0.02729326154356106, -0.188679758960811, -0.11349139511227034, -0.08646408432664779, 0.11772640288556711, 0.06651093975569193, 0.21994342017345703, -0.2512526628292667, -0.20129521855582985, 0.43908996478869367, -0.009469154308764981, -0.06743261544033885, 0.2653903972644072, -0.27428900833743125, -0.17459424054966524, 0.16757847383045232, 0.3375066638780901, 0.1332697278390137, -0.21484587316472942, 0.08015051261799482, -0.03880940800389418, 0.12633229182280886, 0.12760399006163844, 0.05078540667175101, 0.26476641773031306, 0.25201530647105896, -0.09890144540426823, 0.035821535624563694, -0.11390290939464019, -0.13414719285300145, -0.45402003967991245, -0.11348413894526087, -0.05961445948252311, -0.056807527802168176, -0.11611313449807661, 0.025661249143572953, 0.34044850116165787, 0.12002913241919416, 0.2826810000607601, -0.09058964703805171, 0.26786426076880443, 0.09548857116785187, 0.03004794678865717, 0.12082138412202206, 0.34613247215747833, 0.1665637645010765, 0.2889320499335344, -0.2821172491038361, -0.0179315848956601, 0.12849096953868866]
|
707.1871
|
Non-perturbative Yukawa Couplings from String Instantons
|
Non-perturbative D-brane instantons can generate perturbatively absent though
phenomenologically relevant couplings for Type II orientifold compactifications
with D-branes. We discuss the generation of the perturbatively vanishing SU(5)
GUT Yukawa coupling of type 10 10 5_H. Moreover, for a simple globally
consistent intersecting D6-brane model, we discuss the generation of mass terms
for matter fields. This can serve as a mechanism for decoupling exotic matter.
|
hep-th hep-ph
|
nonperturbative dbrane instantons can generate perturbatively absent though phenomenologically relevant couplings for type ii orientifold compactifications with dbranes we discuss the generation of the perturbatively vanishing su5 gut yukawa coupling of type 10 10 5_h moreover for a simple globally consistent intersecting d6brane model we discuss the generation of mass terms for matter fields this can serve as a mechanism for decoupling exotic matter
|
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|
[-0.17106972684450739, 0.25695043653831817, 0.02130130164732691, 0.2517369973411405, -0.10705238189257216, -0.22540500458853785, 0.003002075056429021, 0.29124808277993, -0.1454748618270969, -0.2716008333591162, 0.05947334295069595, -0.2104302692168858, -0.08208493002166506, 0.10563060680942726, -0.04282966026221402, -0.03878858387179207, -0.0542390420960146, -0.027294249361148104, -0.05788747168844566, -0.26417586345633026, 0.3496698500093771, -0.04074307589326054, 0.247251647466328, 0.08563236924237572, 0.07505157490231795, -0.07565440553844383, 0.030691769934492186, -0.0597374951466918, -0.10413052928561228, 0.0775793769498705, 0.2336057526699733, 0.003347829322592588, 0.0306214166485006, -0.45074977341573685, -0.22216690628556535, 0.1526215880876407, 0.2153290038841078, 0.19271889681112953, -0.09859636695182417, -0.26608241254871245, 0.08031166257569566, -0.2291394176754693, -0.1856905975510017, -0.16044129971123766, -0.033974528952967376, -0.08985674175437453, -0.32410053233616054, 0.07549224556714762, -0.05382188993644377, -0.02044521231437102, -0.027513983732205816, -0.08512747271743137, -0.09314149430883845, 0.009266094355552923, 0.1430620221344725, 0.02014247702754801, 0.15375071634298365, -0.22445570760373812, -0.13375096678646514, 0.40395320231618825, -0.1230105392751284, -0.19159324566135183, 0.1312647056984133, -0.034199099100078456, -0.1916772074837354, 0.07011862628860399, 0.10892556416001753, 0.16762125946115702, -0.1490596499061212, 0.2226991774950875, -0.0009040751174325123, 0.10403638766729273, 0.0855020937306108, 0.0888462482689647, 0.36335435797809623, 0.1849420960061252, 0.03348596931027714, 0.05213566766906297, -0.041092676867265254, -0.11216431741195265, -0.5114768703351729, -0.05321281171927694, -0.0410137897124514, 0.15691092654378735, -0.1476772022942896, -0.16575878018920776, 0.4125130177444589, 0.11503168309718603, 0.19385293475352228, 0.053607185633154586, 0.1851417282014154, 0.01822844129310397, 0.08093277872103499, -0.023383739511700696, 0.30572464046417736, 0.09735373202056508, 0.06326881264976691, -0.21621122228680179, -0.13216357740020612, 0.1875328671958414]
|
707.1872
|
Hypervelocity binary stars: smoking gun of massive binary black holes
|
The hypervelocity stars recently found in the Galactic halo are expelled from
the Galactic center through interactions between binary stars and the central
massive black hole or between single stars and a hypothetical massive binary
black hole. In this paper, we demonstrate that binary stars can be ejected out
of the Galactic center with velocities up to 10^3 km/s, while preserving their
integrity, through interactions with a massive binary black hole. Binary stars
are unlikely to attain such high velocities via scattering by a single massive
black hole or through any other mechanisms. Based on the above theoretical
prediction, we propose a search for binary systems among the hypervelocity
stars. Discovery of hypervelocity binary stars, even one, is a definitive
evidence of the existence of a massive binary black hole in the Galactic
center.
|
astro-ph
|
the hypervelocity stars recently found in the galactic halo are expelled from the galactic center through interactions between binary stars and the central massive black hole or between single stars and a hypothetical massive binary black hole in this paper we demonstrate that binary stars can be ejected out of the galactic center with velocities up to 103 kms while preserving their integrity through interactions with a massive binary black hole binary stars are unlikely to attain such high velocities via scattering by a single massive black hole or through any other mechanisms based on the above theoretical prediction we propose a search for binary systems among the hypervelocity stars discovery of hypervelocity binary stars even one is a definitive evidence of the existence of a massive binary black hole in the galactic center
|
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|
[-0.12115361756487027, 0.147615311497044, -0.03751647564036938, 0.1081939125016554, -0.14045501415576064, -0.07763143294532575, 0.13398164089633596, 0.33353370895136647, -0.16244887395191993, -0.34189218621867806, 0.02193701533520761, -0.3564220724432771, -0.03846317626633195, 0.21564316067587472, -0.0249167312972192, -0.01110889023663337, 0.12755578891860683, 0.05707062302685496, -0.08940645827870093, -0.2638446448315213, 0.36292555027488455, 0.0859666041015133, 0.09965694077841158, -0.09184002364749339, 0.09841339668926241, -0.029328884765394587, 0.018144403817132115, -0.022519741893690357, -0.09585751809811596, 0.048829513720111614, 0.21929953161821658, 0.18584982436775827, 0.2247776956950773, -0.35584500015004356, -0.24023149776925792, 0.07239458700572488, 0.2186960393229305, 0.1323981433498687, -0.2283474892880003, -0.2738569477197728, 0.15266400454205342, -0.26293052715569065, -0.16823510822506427, 0.04799369485951515, 0.05691963920383645, 0.04804429107427305, -0.1925031401967602, 0.1401019236098961, 0.08626971765657637, -0.026072411464332645, -0.13957204695777106, -0.05764319232678903, -0.08254655620514123, 0.05923027205350461, 0.076174385364362, 0.05831060262480334, 0.16887884027560923, -0.09527176829687417, -0.09349602776398855, 0.43307802711488375, -0.03876396146978238, -0.06528105485642245, 0.28120872426652976, -0.23036254389531244, -0.16083236188460975, 0.11166200052196187, 0.23379125754668642, 0.21463854252551892, -0.21291337527487594, -0.001196628750072542, -0.006864163430352042, 0.1879996636295135, 0.09088147279403325, 0.0556907343205565, 0.5183466129116158, 0.1355267653225247, -0.01654644613501741, 0.12203382520628885, -0.21374046370046518, -0.07028199101054568, -0.1584533008871906, -0.11372656276129853, -0.08655091468766053, 0.09419742248146169, -0.18340624115623555, -0.125599328393756, 0.2380954886216726, 0.06620265206725184, 0.22112543986582045, -0.02763601642887372, 0.2686541026124536, 0.04709186331966697, 0.1212606168084486, 0.1747390150453951, 0.3941035617365321, 0.17237504022786698, 0.0609525047718728, -0.231848578929637, 0.04580730712388767, 0.029633399189463748]
|
707.1873
|
The Landscape of Sparticle Mass Hierarchies and Their Signature Space at
the LHC
|
The minimal supersymmetric standard model with soft breaking has a large
landscape of supersymmetric particle mass hierarchies. This number is reduced
significantly in well-motivated scenarios such as minimal supergravity and
alternatives. We carry out an analysis of the landscape for the first four
lightest particles and identify at least 16 mass patterns, and provide
benchmarks for each. We study the signature space for the patterns at the CERN
Large Hadron Collider by analyzing the lepton + (jet $\geq 2$) + missing $P_T$
signals with 0, 1, 2 and 3 leptons. Correlations in missing $P_T$ are also
analyzed. It is found that even with 10 fb$^{-1}$ of data a significant
discrimination among patterns emerges
|
hep-ph
|
the minimal supersymmetric standard model with soft breaking has a large landscape of supersymmetric particle mass hierarchies this number is reduced significantly in wellmotivated scenarios such as minimal supergravity and alternatives we carry out an analysis of the landscape for the first four lightest particles and identify at least 16 mass patterns and provide benchmarks for each we study the signature space for the patterns at the cern large hadron collider by analyzing the lepton jet geq 2 missing p_t signals with 0 1 2 and 3 leptons correlations in missing p_t are also analyzed it is found that even with 10 fb1 of data a significant discrimination among patterns emerges
|
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|
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|
707.1874
|
Optimal Control of charge transfer
|
In this work, we investigate how and to which extent a quantum system can be
driven along a prescribed path in space by a suitably tailored laser pulse. The
laser field is calculated with the help of quantum optimal control theory
employing a time-dependent formulation for the control target. Within a
two-dimensional (2D) model system we have successfully optimized laser fields
for two distinct charge transfer processes. The resulting laser fields can be
understood as a complicated interplay of different excitation and de-excitation
processes in the quantum system.
|
cond-mat.other
|
in this work we investigate how and to which extent a quantum system can be driven along a prescribed path in space by a suitably tailored laser pulse the laser field is calculated with the help of quantum optimal control theory employing a timedependent formulation for the control target within a twodimensional 2d model system we have successfully optimized laser fields for two distinct charge transfer processes the resulting laser fields can be understood as a complicated interplay of different excitation and deexcitation processes in the quantum system
|
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|
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|
707.1875
|
An original interferometric study of NGC 1068 with VISIR BURST mode
images
|
We present 12.8 microns images of the core of NGC 1068 obtained with the
BURST mode of the VLT/VISIR. We trace structures under the diffraction limit of
one UT and we investigate the link between dust in the vicinity of the central
engine of NGC 1068, recently resolved by interferometry with MIDI, and more
extended structures. This step is mandatory for a multi-scale understanding of
the sources of mid-infrared emission in AGNs. A speckle processing of VISIR
BURST mode images was performed to extract very low spatial-frequency
visibilities, first considering the full field of VISIR BURST mode images and
then limiting it to the mask used for the acquisition of MIDI data. Extracted
visibilities are reproduced with a multi-component model. We identify two major
sources of emission: one compact < 85 mas, associated with the dusty torus, and
an elliptical one, (< 140) mas x 1187 mas at P.A.=-4 degrees from N to E. This
is consistent with previous deconvolution processes. The combination with MIDI
data reveals the close environment of the dusty torus to contribute to about 83
percent of the MIR flux seen by MIDI. This strong contribution has to be
considered in modeling long baseline interferometric data. It must be related
to the NS elongated component which is thought to originate from individually
unresolved dusty clouds and is located inside the ionization cone. Low
temperatures of the dusty torus are not challenged, emphasizing the scenarios
of clumpy torus.
|
astro-ph
|
we present 128 microns images of the core of ngc 1068 obtained with the burst mode of the vltvisir we trace structures under the diffraction limit of one ut and we investigate the link between dust in the vicinity of the central engine of ngc 1068 recently resolved by interferometry with midi and more extended structures this step is mandatory for a multiscale understanding of the sources of midinfrared emission in agns a speckle processing of visir burst mode images was performed to extract very low spatialfrequency visibilities first considering the full field of visir burst mode images and then limiting it to the mask used for the acquisition of midi data extracted visibilities are reproduced with a multicomponent model we identify two major sources of emission one compact 85 mas associated with the dusty torus and an elliptical one 140 mas x 1187 mas at pa4 degrees from n to e this is consistent with previous deconvolution processes the combination with midi data reveals the close environment of the dusty torus to contribute to about 83 percent of the mir flux seen by midi this strong contribution has to be considered in modeling long baseline interferometric data it must be related to the ns elongated component which is thought to originate from individually unresolved dusty clouds and is located inside the ionization cone low temperatures of the dusty torus are not challenged emphasizing the scenarios of clumpy torus
|
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|
[-0.07812285958862353, 0.045667929686452495, -0.08587584592534471, 0.06148987862407659, -0.06144424884216704, -0.12476779621047704, -4.680904318192763e-05, 0.456208986023667, -0.21292427615126183, -0.32165873395941497, 0.09589275476965024, -0.2791481825237398, -0.026709978332329992, 0.17310560442469275, -0.055823778239698404, -0.02207038341485603, 0.060419283949752496, -0.10387702847301968, -0.018403426820030398, -0.19321753455922164, 0.29517058785868394, 0.12862765158733128, 0.17623718441600392, -0.030493810325987622, 0.0953606545928063, -0.08005797204066645, -0.09778428461527351, -0.051125383218014846, -0.07552786191894233, 0.0707463985659712, 0.28180071953528224, 0.081970887710428, 0.17263290281388052, -0.3840699597704127, -0.21564335559171363, 0.03214517552366628, 0.14253755050972416, 0.004069754374057647, 0.01639131109382924, -0.3018510174317963, 0.06990414746368702, -0.13534244219675098, -0.17940618481222056, 0.04423749395042159, 0.035117065130682294, -0.003629450612237763, -0.22505113417107347, 0.09981254262169706, 0.023291392445712347, 0.10269723405523778, -0.061044175964468414, -0.09441082516712405, -0.030883303889225406, 0.11029785333754627, -0.00940153450621331, 0.11258994419299159, 0.15278672991480258, -0.12234017014148875, -0.05143898829552793, 0.3996146418871241, -0.07483585605643316, -0.058227075754847986, 0.22211491292786772, -0.22175251214889707, -0.15692045978975783, 0.22327057901520483, 0.12074108440701745, 0.11814721509759221, -0.13229540191497263, -0.026812787729833726, -0.05000410225350998, 0.24713348559294845, 0.0696782354055027, 0.07224186696891505, 0.2839986220933497, 0.15971233606022864, -0.016259266254511587, 0.149292991509287, -0.27670754663764097, -0.03669534957963802, -0.2531862611264754, -0.06526132818763476, -0.14734825467270463, 0.08340074198529228, -0.108125557021857, -0.09104176534940858, 0.3328464940710531, 0.11683142938354991, 0.22016332903000133, -0.014221407660131176, 0.3118628196605329, 0.07072295026205115, 0.11951580678042663, 0.10582005737396152, 0.2776230607166201, 0.1574914011886055, 0.11043566616961273, -0.21298258925717964, 0.0017638877039058251, -0.004573053867404182]
|
707.1876
|
Topologies on the space of holomorphic functions
|
We show that a fairly arbitrary Frechet space topology on the space of
holomorphic functions on a domain controls the topology of uniform convergence
on compact sets.
In fact it turns out that the result we present can be proved more simply
using the closed graph theorem. However, we believe that the techniques
presented here may be used to prove a more interesting result. Details to
appear later.
|
math.CV math.AP
|
we show that a fairly arbitrary frechet space topology on the space of holomorphic functions on a domain controls the topology of uniform convergence on compact sets in fact it turns out that the result we present can be proved more simply using the closed graph theorem however we believe that the techniques presented here may be used to prove a more interesting result details to appear later
|
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|
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|
707.1877
|
Horizons in 2+1-dimensional collapse of particles
|
A simple, geometrical construction is given for three-dimensional spacetimes
with negative cosmological constant that contain two particles colliding
head-on. Depending on parameters like particle masses and distance, the
combined geometry will the that of a particle, or of a black hole. In the black
hole case the horizon is calculated. It is found that that the horizon
typically starts at a point and spreads into a closed curve with corners, which
propagate along spacelike caustics and disappear as the horizon passes the
particles.
|
gr-qc
|
a simple geometrical construction is given for threedimensional spacetimes with negative cosmological constant that contain two particles colliding headon depending on parameters like particle masses and distance the combined geometry will the that of a particle or of a black hole in the black hole case the horizon is calculated it is found that that the horizon typically starts at a point and spreads into a closed curve with corners which propagate along spacelike caustics and disappear as the horizon passes the particles
|
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|
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|
707.1878
|
The Young and the Dustless: Interpreting Radio Observations of
UltraViolet Luminous Galaxies
|
Ultraviolet Luminous Galaxies (UVLGs) have been identified as intensely
star-forming, nearby galaxies. A subset of these, the supercompact UVLGs, are
believed to be local analogs of high redshift Lyman Break Galaxies. Here we
investigate the radio continuum properties of this important population for the
first time. We have observed 42 supercompact UVLGs with the VLA, all of which
have extensive coverage in the UV/optical by GALEX and SDSS. Our analysis
includes comparison samples of multiwavelength data from the Spitzer First Look
Survey and from the SDSS-Galex matched catalogs. In addition we have Spitzer
MIPS data for 24 of our galaxies and find that they fall on the radio-FIR
correlation of normal star-forming galaxies. We find that our galaxies have
lower radio-to-UV ratios and lower Balmer decrements than other local galaxies
with similar (high) star formation rates. Optical spectra show they have lower
Dn(4000) and HdeltaA indices, higher Hbeta emission-line equivalents widths,
and higher [OIII]5007/Hbeta emission-line ratios than normal star forming
galaxies. Comparing these results to galaxy spectral evolution models we
conclude that supercompact UVLGs are distinguished from normal star forming
galaxies firstly by their high specific star formation rates. Moreover,
compared to other types of galaxies with similar star formation rates, they
have significantly less dust attenuation. In both regards they are similar to
Lyman Break Galaxies. This suggests that the process that causes star formation
in the supercompact UVLGs differs from other local star forming galaxies, but
may be similar to Lyman Break Galaxies.
|
astro-ph
|
ultraviolet luminous galaxies uvlgs have been identified as intensely starforming nearby galaxies a subset of these the supercompact uvlgs are believed to be local analogs of high redshift lyman break galaxies here we investigate the radio continuum properties of this important population for the first time we have observed 42 supercompact uvlgs with the vla all of which have extensive coverage in the uvoptical by galex and sdss our analysis includes comparison samples of multiwavelength data from the spitzer first look survey and from the sdssgalex matched catalogs in addition we have spitzer mips data for 24 of our galaxies and find that they fall on the radiofir correlation of normal starforming galaxies we find that our galaxies have lower radiotouv ratios and lower balmer decrements than other local galaxies with similar high star formation rates optical spectra show they have lower dn4000 and hdeltaa indices higher hbeta emissionline equivalents widths and higher oiii5007hbeta emissionline ratios than normal star forming galaxies comparing these results to galaxy spectral evolution models we conclude that supercompact uvlgs are distinguished from normal star forming galaxies firstly by their high specific star formation rates moreover compared to other types of galaxies with similar star formation rates they have significantly less dust attenuation in both regards they are similar to lyman break galaxies this suggests that the process that causes star formation in the supercompact uvlgs differs from other local star forming galaxies but may be similar to lyman break galaxies
|
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|
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|
707.1879
|
The dark haloes of early-type galaxies in low-density environments:
XMM-Newton and Chandra observations of NGC 57, NGC 7796 and IC 1531
|
We present analysis of Chandra and XMM-Newton observations of three
early-type galaxies, NGC 57, NGC 7796 and IC 1531. All three are found in very
low density environments, and appear to have no neighbours of comparable size.
NGC 57 has a halo of kT~0.9 keV, solar metallicity gas, while NGC 7796 and IC
1531 both have ~0.55 keV, 0.5-0.6 Zsol haloes. IC 1531 has a relatively compact
halo, and we consider it likely that gas has been removed from the system by
the effects of AGN heating. For NGC 57 and NGC 7796 we estimate mass, entropy
and cooling time profiles and find that NGC 57 has a fairly massive dark halo
with a mass-to-light ratio of 44.7 (4.0,-8.5) Msol/Lsol (1 sigma uncertainties)
at 4.75 Re. This is very similar to the mass-to-light ratio found for NGC 4555
and confirms that isolated ellipticals can possess sizable dark matter haloes.
We find a significantly lower mass-to-light ratio for NGC 7796, 10.6
(+2.5,-2.3) Msol/Lsol at 5 Re, and discuss the possibility that NGC 7796 hosts
a galactic wind, causing us to underestimate its mass.
|
astro-ph
|
we present analysis of chandra and xmmnewton observations of three earlytype galaxies ngc 57 ngc 7796 and ic 1531 all three are found in very low density environments and appear to have no neighbours of comparable size ngc 57 has a halo of kt09 kev solar metallicity gas while ngc 7796 and ic 1531 both have 055 kev 0506 zsol haloes ic 1531 has a relatively compact halo and we consider it likely that gas has been removed from the system by the effects of agn heating for ngc 57 and ngc 7796 we estimate mass entropy and cooling time profiles and find that ngc 57 has a fairly massive dark halo with a masstolight ratio of 447 4085 msollsol 1 sigma uncertainties at 475 re this is very similar to the masstolight ratio found for ngc 4555 and confirms that isolated ellipticals can possess sizable dark matter haloes we find a significantly lower masstolight ratio for ngc 7796 106 2523 msollsol at 5 re and discuss the possibility that ngc 7796 hosts a galactic wind causing us to underestimate its mass
|
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|
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|
707.188
|
Superorbital variability of X-ray and radio emission of Cyg X-1. I.
Emission anisotropy of precessing sources
|
We study theoretical interpretations of the 150-d (superorbital) modulation
observed in X-ray and radio emission of Cyg X-1 in the framework of models
connecting this phenomenon to precession. Precession changes the orientation of
the emission source (either disc or jet) relative to the observer. This leads
to emission modulation due to an anisotropic emission pattern of the source or
orientation-dependent amount of absorbing medium along the line of sight or
both. We consider, in particular, anisotropy patterns of blackbody-type
emission, thermal Comptonization in slab geometry, jet/outflow beaming, and
absorption in a coronal-type medium above the disc. We then fit these models to
the data from the RXTE/ASM, CGRO/BATSE, and the Ryle and Green Bank radio
telescopes, and find relatively small best-fit angles between the precession
and orbital planes, ~10-20 degrees. The thermal Comptonization model for the
X-ray emission explains well the observed decrease of the variability amplitude
from 1 to 300 keV as a result of a reduced anisotropy of the emission due to
multiple scatterings. Our modeling also yield the jet bulk velocity of
~(0.3-0.5)c, which is in agreement with the previous constraint from the lack
of an observed counterjet and lack of short-term X-ray/radio correlations.
|
astro-ph
|
we study theoretical interpretations of the 150d superorbital modulation observed in xray and radio emission of cyg x1 in the framework of models connecting this phenomenon to precession precession changes the orientation of the emission source either disc or jet relative to the observer this leads to emission modulation due to an anisotropic emission pattern of the source or orientationdependent amount of absorbing medium along the line of sight or both we consider in particular anisotropy patterns of blackbodytype emission thermal comptonization in slab geometry jetoutflow beaming and absorption in a coronaltype medium above the disc we then fit these models to the data from the rxteasm cgrobatse and the ryle and green bank radio telescopes and find relatively small bestfit angles between the precession and orbital planes 1020 degrees the thermal comptonization model for the xray emission explains well the observed decrease of the variability amplitude from 1 to 300 kev as a result of a reduced anisotropy of the emission due to multiple scatterings our modeling also yield the jet bulk velocity of 0305c which is in agreement with the previous constraint from the lack of an observed counterjet and lack of shortterm xrayradio correlations
|
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|
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|
707.1881
|
Dynamical systems associated with crossed products
|
In this paper, we consider both algebraic crossed products of commutative
complex algebras A with the integers under an automorphism of A, and Banach
algebra crossed products of commutative C^*-algebras A with the integers under
an automorphism of A. We investigate, in particular, connections between
algebraic properties of these crossed products and topological properties of
naturally associated dynamical systems. For example, we draw conclusions about
the ideal structure of the crossed product by investigating the dynamics of
such a system. To begin with, we recall results in this direction in the
context of an algebraic crossed product and give simplified proofs of
generalizations of some of these results. We also investigate new questions,
for example about ideal intersection properties of algebras properly between
the coefficient algebra A and its commutant A'. Furthermore, we introduce a
Banach algebra crossed product and study the relation between the structure of
this algebra and the topological dynamics of a naturally associated system.
|
math.OA math.DS
|
in this paper we consider both algebraic crossed products of commutative complex algebras a with the integers under an automorphism of a and banach algebra crossed products of commutative calgebras a with the integers under an automorphism of a we investigate in particular connections between algebraic properties of these crossed products and topological properties of naturally associated dynamical systems for example we draw conclusions about the ideal structure of the crossed product by investigating the dynamics of such a system to begin with we recall results in this direction in the context of an algebraic crossed product and give simplified proofs of generalizations of some of these results we also investigate new questions for example about ideal intersection properties of algebras properly between the coefficient algebra a and its commutant a furthermore we introduce a banach algebra crossed product and study the relation between the structure of this algebra and the topological dynamics of a naturally associated system
|
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|
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|
707.1882
|
A Chandra X-ray detection of the L dwarf binary Kelu-1: Simultaneous
Chandra and Very Large Array observations
|
Magnetic activity in ultracool dwarfs, as measured in X-rays and H$\alpha$,
shows a steep decline after spectral type M7-M8. So far, no L dwarf has been
detected in X-rays. In contrast, L dwarfs may have higher radio activity than M
dwarfs. We observe L and T dwarfs simultaneously in X-rays and radio to
determine their level of magnetic activity in the context of the general
decline of magnetic activity with cooler effective temperatures. The field L
dwarf binary Kelu-1 was observed simultaneously with Chandra and the Very Large
Array. Kelu-1AB was detected in X-rays with $L_{\rm X} = 2.9_{-1.3}^{+1.8}
\times 10^{25}$ erg/s, while it remained undetected in the radio down to a $3
\sigma$ limit of $L_{\rm R} \leq 1.4 \times 10^{13}$ erg/s/Hz. We argue that,
whereas the X-ray and H$\alpha$ emissions decline in ultracool dwarfs with
decreasing effective temperature, the radio luminosity stays (more or less)
constant across M and early-L dwarfs. The radio surface flux or the luminosity
may better trace magnetic activity in ultracool dwarfs than the ratio of the
luminosity to the bolometric luminosity. Deeper radio observations (and at
short frequencies) are required to determine if and when the cut-off in radio
activity occurs in L and T dwarfs, and what kind of emission mechanism takes
place in ultracool dwarfs.
|
astro-ph
|
magnetic activity in ultracool dwarfs as measured in xrays and halpha shows a steep decline after spectral type m7m8 so far no l dwarf has been detected in xrays in contrast l dwarfs may have higher radio activity than m dwarfs we observe l and t dwarfs simultaneously in xrays and radio to determine their level of magnetic activity in the context of the general decline of magnetic activity with cooler effective temperatures the field l dwarf binary kelu1 was observed simultaneously with chandra and the very large array kelu1ab was detected in xrays with l_rm x 29_1318 times 1025 ergs while it remained undetected in the radio down to a 3 sigma limit of l_rm r leq 14 times 1013 ergshz we argue that whereas the xray and halpha emissions decline in ultracool dwarfs with decreasing effective temperature the radio luminosity stays more or less constant across m and earlyl dwarfs the radio surface flux or the luminosity may better trace magnetic activity in ultracool dwarfs than the ratio of the luminosity to the bolometric luminosity deeper radio observations and at short frequencies are required to determine if and when the cutoff in radio activity occurs in l and t dwarfs and what kind of emission mechanism takes place in ultracool dwarfs
|
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|
[-0.061589597405334234, 0.19979237706207162, 0.008946866745937546, 0.15349128390750233, -0.12091196859958318, -0.11201504671744089, 0.0951231106256908, 0.47361110229888614, -0.08469624007076798, -0.3861842415084676, 0.04502687950174869, -0.31874921141227464, -0.007156351230871635, 0.20606134626091863, -0.045966041118416165, -0.07328856809565551, 0.016853816741374584, -0.03678125939425301, -0.06725636095616896, -0.24914028866761276, 0.22416962103320742, 0.0777452725989586, 0.14669247197848306, -0.01858776569902405, 0.019847269815761806, -0.13428218954551033, -0.06885306961573046, -0.04477643674757894, -0.1000729011041774, -0.07154078980499246, 0.29109489299875313, 0.09126772827859793, 0.1952033533785, -0.3632163167535767, -0.2109079872596271, 0.09156707991222095, 0.17324048734296393, -0.09415675066565252, 0.031960125841990546, -0.22046818734719945, 0.10186728391080287, -0.17522596786861783, -0.1477302744180702, 0.11683870786976702, 0.15877893481476074, 0.0006275347882622571, -0.2316855419485364, 0.11145987898635212, 0.06672506060457858, 0.1369805100576003, -0.13931418619808336, -0.1098675974024205, -0.03088218325371239, 0.03750435340633936, 0.04620023007847299, 0.13290008901080824, 0.157240474440667, -0.12222291581949904, -0.015774895020822098, 0.32940933465483196, -0.13252398678014288, 0.08655286574832884, 0.26256176767725814, -0.2619072936040367, -0.16678681369554602, 0.17479236464385153, 0.11691214839646698, 0.11663399137477479, -0.14129503158653947, 0.02313139863072824, 0.02375186575611807, 0.21322283490104074, 0.0569436883900912, 0.11812810593296748, 0.32400870146361654, 0.12288019077178038, 0.050770885792104, 0.06872798716330919, -0.280271798561169, 0.07852691802018287, -0.18723868776358804, -0.0661713913860643, -0.132027985871317, 0.17228707037251093, -0.09238532775030625, -0.10202147569155919, 0.34067945771648567, 0.08808692245807867, 0.2190441206157458, 0.07806421560221594, 0.2858679983677026, 0.13879535310047256, 0.14875318877451685, 0.1969363129761439, 0.3053749525163955, 0.19932996389732854, 0.15032315854189637, -0.23593751630275775, 0.03593683017984489, -0.00867312413174659]
|
707.1883
|
Quantum Optimal Control Theory
|
The control of quantum dynamics via specially tailored laser pulses is a
long-standing goal in physics and chemistry. Partly, this dream has come true,
as sophisticated pulse shaping experiments allow to coherently control product
ratios of chemical reactions. The theoretical design of the laser pulse to
transfer an initial state to a given final state can be achieved with the help
of quantum optimal control theory (QOCT). This tutorial provides an
introduction to QOCT. It shows how the control equations defining such an
optimal pulse follow from the variation of a properly defined functional. We
explain the most successful schemes to solve these control equations and show
how to incorporate additional constraints in the pulse design. The algorithms
are then applied to simple quantum systems and the obtained pulses are
analyzed. Besides the traditional final-time control methods, the tutorial also
presents an algorithm and an example to handle time-dependent control targets.
|
quant-ph
|
the control of quantum dynamics via specially tailored laser pulses is a longstanding goal in physics and chemistry partly this dream has come true as sophisticated pulse shaping experiments allow to coherently control product ratios of chemical reactions the theoretical design of the laser pulse to transfer an initial state to a given final state can be achieved with the help of quantum optimal control theory qoct this tutorial provides an introduction to qoct it shows how the control equations defining such an optimal pulse follow from the variation of a properly defined functional we explain the most successful schemes to solve these control equations and show how to incorporate additional constraints in the pulse design the algorithms are then applied to simple quantum systems and the obtained pulses are analyzed besides the traditional finaltime control methods the tutorial also presents an algorithm and an example to handle timedependent control targets
|
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|
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|
707.1884
|
Soluble Models of Strongly Interacting Two-level Ultracold Gases in
Tight Waveguides with Coupling to the Quantized Electromagnetic Field
|
A generalized Fermi-Bose mapping method is used to determine the exact ground
states of six models of strongly interacting ultracold gases of two-level atoms
in tight waveguides, which are generalizations of the Tonks-Girardeau (TG) gas
(1D Bose gas with point hard cores) and fermionic Tonks-Girardeau (FTG) gas (1D
spin-aligned Fermi gas with infinitely strong zero-range attractions). Three of
these models exhibit a quantum phase transition in the presence of an external
magnetic field, associated with a cooperative ground state rearrangement
wherein Fermi energy is traded for internal excitation energy. After
investigation of these models in the absence of an electromagnetic field, one
is generalized to include resonant interactions with a single photon mode,
leading to a possible thermal phase transition associated with Dicke
superradiance.
|
cond-mat.other
|
a generalized fermibose mapping method is used to determine the exact ground states of six models of strongly interacting ultracold gases of twolevel atoms in tight waveguides which are generalizations of the tonksgirardeau tg gas 1d bose gas with point hard cores and fermionic tonksgirardeau ftg gas 1d spinaligned fermi gas with infinitely strong zerorange attractions three of these models exhibit a quantum phase transition in the presence of an external magnetic field associated with a cooperative ground state rearrangement wherein fermi energy is traded for internal excitation energy after investigation of these models in the absence of an electromagnetic field one is generalized to include resonant interactions with a single photon mode leading to a possible thermal phase transition associated with dicke superradiance
|
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|
[-0.17044931909843017, 0.2671840191058788, -0.02147681435951287, 0.05076158670764867, 0.01956906838102206, -0.20986073300047148, 0.0436477689729673, 0.37391875840483174, -0.19200758536856982, -0.24265523434376285, -0.011528427538935156, -0.3111475664190948, -0.05596962771397234, 0.13615935009851632, 0.09551884110776647, 0.054356818718294946, 0.01988803397961742, 0.019883757566041764, -0.06819237148315992, -0.19928897239620827, 0.34752086403539345, 0.03577941240115662, 0.25434343834903334, 0.05537346140162328, 0.0601868667008896, -0.01241652388970608, 0.10027993444518576, -0.031881128730733066, -0.10915983167491973, 0.05960248992543653, 0.22957400675327774, -0.06257038754824128, 0.20715184947626003, -0.4521964001769741, -0.2282601488874324, 0.12477293485520227, 0.14976789700543328, 0.15301149072324588, -0.030060748395044357, -0.33367507158958865, -0.11862673203746278, -0.2378734290419567, -0.2139947505249086, -0.10799391684497917, -0.01471177652861262, 0.052283765800717856, -0.23411866204696707, 0.10987046576525655, 0.06920249185021667, 0.03857675914637624, -0.10923236677368667, -0.023540480037955867, -0.017355867639003743, 0.016701432267924952, -0.016732918453447883, 0.022394695090160014, 0.17592409196414896, -0.17675590571466712, -0.10261762550010556, 0.4038613350590646, -0.11238923491046374, -0.1269707465769663, 0.289989510460967, -0.1382190480587944, -0.10270124824150585, 0.23610506127137812, 0.12025492649615532, 0.02938193334369815, -0.14112800700710185, 0.07291012348357453, -0.07469049998889526, 0.172320282794845, 0.042071332655576686, 0.07883873901089593, 0.3041883657673269, 0.14009243280311384, 0.020761382075086716, 0.22073901701538312, -0.10525043799838561, -0.1670640771236879, -0.22163804946091747, -0.142737430924054, -0.2102458305108162, 0.04641778277789032, -0.04880478688597401, -0.20791150956609916, 0.3406715801684186, 0.09269906432675798, 0.15861930973797797, -0.040241040677140134, 0.256801946193821, 0.15206603440380986, 0.013135697181907392, 0.05145410465775058, 0.24972405343226367, 0.1858554937381057, 0.03209246955286231, -0.29705160219718013, -0.0663731589673027, 0.06138311902947363]
|
707.1885
|
Macroscopic Screening of Coulomb Potentials From UV/IR-Mixing
|
We compute the static potential in a non-commutative theory including a term
due to UV/IR-mixing. As a result, the potential decays exponentially fast with
distance rather than like a power law Coulomb type potential due to the
exchange of massless particles. This shows that when quantum effects are taken
into account the introduction of non-commutativity not only modifies physics at
short distances but has dramatic macroscopic consequences as well. As a result,
we give a lower bound on the scale of non-commutativity (if present at all) to
be compatible with observations.
|
hep-th
|
we compute the static potential in a noncommutative theory including a term due to uvirmixing as a result the potential decays exponentially fast with distance rather than like a power law coulomb type potential due to the exchange of massless particles this shows that when quantum effects are taken into account the introduction of noncommutativity not only modifies physics at short distances but has dramatic macroscopic consequences as well as a result we give a lower bound on the scale of noncommutativity if present at all to be compatible with observations
|
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|
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|
707.1886
|
First Steps in Direct Imaging of Planetary Systems Like our Own: The
Science Potential of 2-m Class Optical Space Telescopes
|
We summarize the scientific potential of high contrast optical space imaging
for studies of extrasolar planets, debris disks, and planet formation. The
unique scientific capabilities offered by a 2-m class optical telescope, the
technical requirements to achieve 10^-9 contrast, and the programmatic means
needed to advance such a mission are discussed.
|
astro-ph
|
we summarize the scientific potential of high contrast optical space imaging for studies of extrasolar planets debris disks and planet formation the unique scientific capabilities offered by a 2m class optical telescope the technical requirements to achieve 109 contrast and the programmatic means needed to advance such a mission are discussed
|
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|
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|
707.1887
|
The Hahn polynomials in the nonrelativistic and relativistic Coulomb
problems
|
We derive closed formulas for mean values of all powers of r in
nonrelativistic and relativistic Coulomb problems in terms of the Hahn and
Chebyshev polynomials of a discrete variable. A short review on special
functions and solution of the Coulomb problems in quantum mechanics is given.
|
quant-ph
|
we derive closed formulas for mean values of all powers of r in nonrelativistic and relativistic coulomb problems in terms of the hahn and chebyshev polynomials of a discrete variable a short review on special functions and solution of the coulomb problems in quantum mechanics is given
|
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|
[-0.14441040245459436, 0.09526181345845157, -0.07024395933493655, 0.08799005127660534, -0.024962554061587188, -0.12957967015260713, 0.0019090095723166744, 0.32186603425268795, -0.2602115013448403, -0.2052056706966238, 0.049540431270910866, -0.24983706658686253, -0.12220658543222446, 0.2350366042500877, -0.0580092679515377, 0.07267493707842461, 0.03907068549318517, 0.07559324539405235, -0.18024130706536642, -0.24861527087682106, 0.29352634091009483, -0.015262122734132758, 0.1564755512480723, 0.09062272141578588, 0.1521581635671727, 0.05499303893760798, -0.029849153180467956, 0.0016273291127637346, -0.1296007167746095, 0.10325940561659158, 0.2625322274546674, 0.07879206961258611, 0.30881366652852676, -0.43411697162453955, -0.1552797511140717, 0.10385281483622942, 0.12236215946997733, 0.07902877115981376, 0.02411193987899559, -0.23272430254740917, 0.017504287883639336, -0.160272169422279, -0.1586752800627592, -0.04558462155190237, 0.0915746918800188, 0.1364289318072669, -0.27866254378347954, 0.10263673180436834, 0.05040649249357112, 0.08356361338829106, -0.074775210482643, -0.1510747804286632, 0.11298465973479634, 0.03701520140500779, 0.028370538860202788, -0.013098865806897904, 0.02220517112576264, -0.18089231711990655, -0.14276821344615298, 0.4461025815813782, -0.03948339711914354, -0.25716478813518867, 0.09314223646404261, -0.16660906582515925, -0.1511901884557719, 0.09322177659611199, 0.15195372928568024, 0.21227037976000537, -0.11866894798313683, 0.18680446899738756, -0.05629918934341441, 0.04646012995471346, 0.09174965767863583, 0.08283258356312488, 0.15576582938987524, 0.009929086101499009, 0.0023355840685519765, 0.17092241029790106, -0.01900434710749207, -0.17241403398084196, -0.3968350188212192, -0.16448108711220483, -0.210646634369078, 0.07495374900308695, -0.1713790500012073, -0.21820448382579266, 0.4072496386683308, 0.05179379682274575, 0.13093750969447354, 0.07563830117516696, 0.21919010682625972, 0.2196341637086044, -0.012181612266663542, 0.0550945112679867, 0.1799050102684092, 0.2418914067093283, 0.07648756013232026, -0.1910907562841919, -0.03787849222290072, 0.19678253519963076]
|
707.1888
|
Scaling of exciton binding energy with external dielectric function in
carbon nanotubes
|
We develop a scaling relationship between the exciton binding energy and the
external dielectric function in carbon nanotubes. We show that the
electron-electron and electron-hole interaction energies are strongly affected
by screening yet largely counteract each other, resulting in much smaller
changes in the optical transition energy. The model indicates that the relevant
particle interaction energies are reduced by as much as 50 percent upon
screening by water and that the unscreened electron-electron interaction energy
is larger than the unscreened electron-hole interaction energy, in agreement
with explanations of the "ratio problem." We apply the model to measurements of
the changes in the optical transistion energies in single, suspended carbon
nanotubes as the external dielectric environment is altered.
|
cond-mat.other
|
we develop a scaling relationship between the exciton binding energy and the external dielectric function in carbon nanotubes we show that the electronelectron and electronhole interaction energies are strongly affected by screening yet largely counteract each other resulting in much smaller changes in the optical transition energy the model indicates that the relevant particle interaction energies are reduced by as much as 50 percent upon screening by water and that the unscreened electronelectron interaction energy is larger than the unscreened electronhole interaction energy in agreement with explanations of the ratio problem we apply the model to measurements of the changes in the optical transistion energies in single suspended carbon nanotubes as the external dielectric environment is altered
|
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|
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|
707.1889
|
Non-Abelian Anyons and Topological Quantum Computation
|
Topological quantum computation has recently emerged as one of the most
exciting approaches to constructing a fault-tolerant quantum computer. The
proposal relies on the existence of topological states of matter whose
quasiparticle excitations are neither bosons nor fermions, but are particles
known as {\it Non-Abelian anyons}, meaning that they obey {\it non-Abelian
braiding statistics}. Quantum information is stored in states with multiple
quasiparticles, which have a topological degeneracy. The unitary gate
operations which are necessary for quantum computation are carried out by
braiding quasiparticles, and then measuring the multi-quasiparticle states. The
fault-tolerance of a topological quantum computer arises from the non-local
encoding of the states of the quasiparticles, which makes them immune to errors
caused by local perturbations. To date, the only such topological states
thought to have been found in nature are fractional quantum Hall states, most
prominently the \nu=5/2 state, although several other prospective candidates
have been proposed in systems as disparate as ultra-cold atoms in optical
lattices and thin film superconductors. In this review article, we describe
current research in this field, focusing on the general theoretical concepts of
non-Abelian statistics as it relates to topological quantum computation, on
understanding non-Abelian quantum Hall states, on proposed experiments to
detect non-Abelian anyons, and on proposed architectures for a topological
quantum computer. We address both the mathematical underpinnings of topological
quantum computation and the physics of the subject using the \nu=5/2 fractional
quantum Hall state as the archetype of a non-Abelian topological state enabling
fault-tolerant quantum computation.
|
cond-mat.str-el cond-mat.mes-hall
|
topological quantum computation has recently emerged as one of the most exciting approaches to constructing a faulttolerant quantum computer the proposal relies on the existence of topological states of matter whose quasiparticle excitations are neither bosons nor fermions but are particles known as it nonabelian anyons meaning that they obey it nonabelian braiding statistics quantum information is stored in states with multiple quasiparticles which have a topological degeneracy the unitary gate operations which are necessary for quantum computation are carried out by braiding quasiparticles and then measuring the multiquasiparticle states the faulttolerance of a topological quantum computer arises from the nonlocal encoding of the states of the quasiparticles which makes them immune to errors caused by local perturbations to date the only such topological states thought to have been found in nature are fractional quantum hall states most prominently the nu52 state although several other prospective candidates have been proposed in systems as disparate as ultracold atoms in optical lattices and thin film superconductors in this review article we describe current research in this field focusing on the general theoretical concepts of nonabelian statistics as it relates to topological quantum computation on understanding nonabelian quantum hall states on proposed experiments to detect nonabelian anyons and on proposed architectures for a topological quantum computer we address both the mathematical underpinnings of topological quantum computation and the physics of the subject using the nu52 fractional quantum hall state as the archetype of a nonabelian topological state enabling faulttolerant quantum computation
|
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|
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|
707.189
|
Decay of a charged scalar and Dirac fields in the Kerr-Newman-de Sitter
background
|
We find the quasinormal modes of the charged scalar and Dirac fields in the
background of the rotating charged black holes, described by the Kerr-Newman-de
Sitter solution. The dependence of the quasinormal spectrum upon the black hole
parameters mass M, angular momentum a, charge Q, as well as on values of the
\Lambda-term and field charge q is investigated. Special attention is given to
the near extremal limit of the black hole charge. In particular, we find that
for both scalar and Dirac fields, charged perturbations decay quicker for q>0
and slower for q<0 for values of black holes charge Q less than than some
threshold value, which is close to the extremal value of charge and depend on
parameters of the black holes.
|
hep-th astro-ph gr-qc
|
we find the quasinormal modes of the charged scalar and dirac fields in the background of the rotating charged black holes described by the kerrnewmande sitter solution the dependence of the quasinormal spectrum upon the black hole parameters mass m angular momentum a charge q as well as on values of the lambdaterm and field charge q is investigated special attention is given to the near extremal limit of the black hole charge in particular we find that for both scalar and dirac fields charged perturbations decay quicker for q0 and slower for q0 for values of black holes charge q less than than some threshold value which is close to the extremal value of charge and depend on parameters of the black holes
|
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|
[-0.15618061902369523, 0.18061400565408892, -0.00227933555030294, 0.11275985127130914, -0.05759519793003077, -0.1502590791074439, 0.017328151603109174, 0.2733219878507718, -0.10663306902373029, -0.285974758196502, 0.05467777450629059, -0.3444888737492053, -0.04467589448716852, 0.1973428926411866, 0.00609073948280345, 0.04396967325597108, -0.04461095829479276, 0.11301297759036383, -0.11322138976538554, -0.17241717332733736, 0.4031366485456425, 0.09511554954693682, 0.23429997838402708, 0.005605781281877669, 0.05909083229714945, 0.027500598387221895, 0.0674311228682317, 0.03742947895079851, -0.19605834494682167, 0.009145587134445387, 0.17744396440344468, 0.06846321562695648, 0.183159708394669, -0.36134916452330446, -0.17593199553553976, 0.09729498083282623, 0.1764576304027991, 0.1491776198522383, -0.12537454244598084, -0.23066685606365003, 0.10896139039147285, -0.18072913554421957, -0.16972087194763816, -0.05356248906971286, 0.11560944598186912, -0.01997881416877311, -0.2781201157598726, 0.14504891035387352, 0.07292288319008695, -0.08827862546088235, -0.14106340806240275, -0.1276867189932795, -0.11602866425434308, 0.06653883853446572, 0.19911174272795418, 0.03362483469273655, 0.21560938414111133, -0.16104400296875787, -0.0847807599235356, 0.32390334185272934, -0.06751012521342473, -0.2292585956954187, 0.09449562242615127, -0.2928812527473295, -0.030321391945284222, 0.12388229734478368, 0.15109357439383353, 0.24731349823771104, -0.07851969635099053, 0.1637345756711687, 0.015028312734718765, 0.1569591880468051, 0.16107374871329916, 0.1004514369940866, 0.3704861308478059, 0.08105487030022027, 0.02453461625602006, 0.11782881082035601, -0.044619366244953725, -0.08160820406497336, -0.2831010338099253, -0.15690793117297994, -0.1947826707750679, 0.11152560702213386, -0.18230865195319865, -0.1944180217969622, 0.3965216586816936, 0.08381697165614535, 0.22355932645469664, -0.00491199441040085, 0.21815806203387417, 0.12235171426530747, 0.031303265898097905, 0.124014817444878, 0.34393579560081333, 0.1448372121629936, 0.15573788018927218, -0.2652595215439496, -0.10033668341460608, 0.0830216444690802]
|
707.1891
|
The Geneva-Copenhagen Survey of the Solar neighbourhood II. New uvby
calibrations and rediscussion of stellar ages, the G dwarf problem,
age-metallicity diagram, and heating mechanisms of the disk
|
Ages, metallicities, space velocities, and Galactic orbits of stars in the
Solar neighbourhood are fundamental observational constraints on models of
galactic disk evolution. We aim to consolidate the calibrations of uvby
photometry into Te, [Fe/H], distance, and age for F and G stars and rediscuss
the results of the Geneva-Copenhagen Survey (Nordstrom et al. 2004; GCS) in
terms of the evolution of the disk.
We substantially improve the Te and [Fe/H] calibrations for early F stars,
where spectroscopic temperatures have large systematic errors. Our recomputed
ages are in excellent agreement with the independent determinations by Takeda
et al. (2007), indicating that isochrone ages can now be reliably determined.
The revised G-dwarf metallicity distribution remains incompatible with
closed-box models, and the age-metallicity relation for the thin disk remains
almost flat, with large and real scatter at all ages (sigma intrinsic = 0.20
dex). Dynamical heating of the thin disk continues throughout its life;
specific in-plane dynamical effects dominate the evolution of the U and V
velocities, while the W velocities remain random at all ages. When assigning
thick and thin-disk membership for stars from kinematic criteria, parameters
for the oldest stars should be used to characterise the thin disk.
|
astro-ph
|
ages metallicities space velocities and galactic orbits of stars in the solar neighbourhood are fundamental observational constraints on models of galactic disk evolution we aim to consolidate the calibrations of uvby photometry into te feh distance and age for f and g stars and rediscuss the results of the genevacopenhagen survey nordstrom et al 2004 gcs in terms of the evolution of the disk we substantially improve the te and feh calibrations for early f stars where spectroscopic temperatures have large systematic errors our recomputed ages are in excellent agreement with the independent determinations by takeda et al 2007 indicating that isochrone ages can now be reliably determined the revised gdwarf metallicity distribution remains incompatible with closedbox models and the agemetallicity relation for the thin disk remains almost flat with large and real scatter at all ages sigma intrinsic 020 dex dynamical heating of the thin disk continues throughout its life specific inplane dynamical effects dominate the evolution of the u and v velocities while the w velocities remain random at all ages when assigning thick and thindisk membership for stars from kinematic criteria parameters for the oldest stars should be used to characterise the thin disk
|
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|
[-0.023603879284056915, 0.1483028226361851, -0.0642663117422519, 0.07572476086230372, -0.10181852339100339, -0.04368242008143535, 0.08708519837700851, 0.42906762801375486, -0.18846381457078124, -0.38827410493185505, -0.0004539996448214057, -0.2779559655337202, 0.027804591924632867, 0.22338783592553005, -0.10968600556509674, 0.0026321702227256436, 0.09057782514807934, -0.1107460927524897, -0.05592273369544956, -0.3210677687305636, 0.2767197215683796, 0.028201569830242374, 0.1277262340940956, -0.09367075809253957, -0.001052842470746355, -0.12346902009936495, -0.0833814343470645, 0.0010813132617185318, -0.24204823419796379, 0.019201830847349565, 0.24466345505245995, 0.11359359199980594, 0.192875341131697, -0.3193729953523631, -0.21265340461466595, 0.04336268519557218, 0.19437813079977398, 0.03492375644902476, -0.06278004871000568, -0.2417646378212547, 0.08049662485671452, -0.14847064198840995, -0.1899333599521093, 0.06768402686729072, 0.10555180521246972, 0.02884992401128597, -0.23804568692889339, 0.15828633568956407, 0.03361696359816097, 0.1534858863297135, -0.16443017623470008, -0.19800953958939932, -0.1218141603684242, 0.1321713387084768, -0.009814142628908536, 0.07637669770803472, 0.13680323036293013, -0.07095916269271431, 0.0191578047071125, 0.3960144592137052, -0.09889329433899732, -0.013769999726026598, 0.20691472873904831, -0.19547343663936292, -0.1498646690595309, 0.037613296055773904, 0.15251286412697984, 0.11917682031056073, -0.19616963095919568, 0.1060986251066212, 0.01597938614987253, 0.18505830351064728, 0.07018574902570339, 0.025730899619882595, 0.3201429779017297, 0.07518112678541732, 0.006851856155926125, -0.02667731463171655, -0.17929118982431133, -0.06026432490470313, -0.21318918611703033, -0.10019008830062062, -0.06976905017074783, 0.0733588954840366, -0.19351559754177103, -0.1532789153415653, 0.32877321251275654, 0.13414094324278655, 0.2182057798677006, 0.07233879071632861, 0.2837191541906125, 0.06605668623900977, 0.08180280745209022, 0.15951863057358276, 0.3151542312148864, 0.230586416453246, 0.06577611517722229, -0.25607512108296115, 0.13575707429542494, 0.004427197337301855]
|
707.1892
|
Maltsiniotis's first conjecture for K_1
|
We show that K_1 of an exact category agrees with K_1 of the associated
triangulated derivator. More generally we show that K_1 of a Waldhausen
category with cylinders and a saturated class of weak equivalences coincides
with K_1 of the associated right pointed derivator.
|
math.KT math.AT
|
we show that k_1 of an exact category agrees with k_1 of the associated triangulated derivator more generally we show that k_1 of a waldhausen category with cylinders and a saturated class of weak equivalences coincides with k_1 of the associated right pointed derivator
|
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|
[-0.2471351286010097, 0.06276748083109851, -0.01903708109801466, 0.09748485963791609, -0.09354889109751886, -0.16486891517838972, -0.04602090023796667, 0.4433337930928577, -0.35721135715192015, -0.1345951891800558, 0.04447440429992804, -0.23262279091233556, -0.1138376196296039, 0.20663557094733484, -0.13944274273870344, -0.1031375542727553, 0.1460770832332359, 0.1818261262960732, -0.05808168849696151, -0.14883098751306534, 0.41750388050621207, -0.09656210962831127, 0.16759747961028057, 0.015078734267841686, 0.09623889504423873, -0.05164385261014104, 0.008888944560153917, 0.12328866640613838, -0.22520701272514998, 0.18656846385618503, 0.22397086206315595, 0.04395631736737083, 0.17522247512930667, -0.35605374622074043, -0.03577806315156935, 0.1502687756966969, 0.05205816561779515, -0.0002655201718549837, 0.022130831815130394, -0.3348652223463763, 0.20930693031881342, -0.23186452602120963, -0.1308098604944958, -0.08307286696931855, 0.09244975011626427, 0.01524329255339167, -0.2970786763524467, 0.032438110136850315, 0.11944193490357562, 0.10010945229706439, -0.08562316836535254, -0.11021812373391268, -0.14858953565867108, 0.05466540945185856, 0.012867253104394133, 0.06393964180130172, 0.06435483117291535, -0.1553617260757495, -0.11715497319925237, 0.3858949165918272, -0.12857859871688893, -0.13625439832156355, 0.14021817527034067, -0.12746517021547665, -0.16664967391724614, 0.19658168362961573, -0.1026740952564234, 0.17437756226652049, 0.04802283828824081, 0.185757999285918, -0.20213373354636133, 0.10277911525389011, 0.10332660959102213, 0.022041285114193506, 0.14462305541912263, 0.05056367237755859, 0.07209287016567859, 0.19928167688406326, 0.00023052910480394283, -0.048665199198611925, -0.3981572376902808, -0.1497983106872363, -0.04620401010933248, 0.15233544057628023, -0.08918941250588185, -0.19042197718623688, 0.28052403269843623, 0.06839885370043869, 0.2542333339594982, 0.18741907920180398, 0.21456479281187057, 0.002330034579658373, 0.034670195415277376, 0.04633081005886197, 0.1575112404217097, 0.29413054612549866, -0.06403009274932132, -0.11486786157316105, -0.0159552647118372, 0.13472380389628763]
|
707.1893
|
Tube formula, Berezinians, and Dwork formula
|
We consider an example of tubes of hypersurfaces in Euclidean space and
generalise the tube formula to supercase. By this we assign to a point of the
hypersurface in superspace a rational characteristic function. Does this
rational function appear when we calculate the zeta-function of an arithmetic
variety?
|
math-ph hep-th math.DG math.MP
|
we consider an example of tubes of hypersurfaces in euclidean space and generalise the tube formula to supercase by this we assign to a point of the hypersurface in superspace a rational characteristic function does this rational function appear when we calculate the zetafunction of an arithmetic variety
|
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|
[-0.182101255399175, 0.042721955111119314, -0.11470254708547145, 0.10055723523934527, -0.06573918894476567, -0.07841816864674911, 0.004009160872859259, 0.33634039383226383, -0.25628464051987976, -0.19662705956337354, 0.0590670322853839, -0.23561319935834035, -0.1916558367665857, 0.16720230378753817, -0.16121337403698513, 0.012690464868986359, -0.038557824819387555, 0.0652691219584085, -0.1355104041819383, -0.27853785446010687, 0.402986045461148, -0.03943661670200527, 0.20559720896805325, 0.09090112912235782, 0.142417594906874, 0.0540772218858668, 0.019524232057544093, -0.017865230106811698, -0.18812178038448715, 0.09949690180656034, 0.2666581967302288, 0.10098761378321797, 0.2066066046633447, -0.4301839092125495, -0.17322024131620614, 0.2171764209633693, 0.1866971182753332, 0.055260230670683086, 0.0652820051764138, -0.19177052685214827, 0.07969316287684099, -0.14488686258361363, -0.23758086549545018, -0.06980250167058936, 0.018106119357980788, 0.02373788813808157, -0.21468331439731023, -0.03529179453228911, 0.045714170283948384, 0.1317097217349025, -0.07641568103281315, -0.08440353529294953, 0.030263898433380138, 0.06137093665711291, 0.03731317536585266, 0.11584872012220633, 0.10824260784041446, -0.11392560699217331, -0.09723430648834135, 0.3540022885426879, -0.07763776603193644, -0.2798502783019406, 0.08105626715890442, -0.1915664478049924, -0.11554852193997552, 0.10569667734671384, 0.14598990399584486, 0.19013672258976536, -0.0531703423879056, 0.1350238838143317, -0.08590961199176188, 0.08542751747215031, 0.08989724615821615, -0.08019237734454994, 0.18216326174539668, 0.04646478147575787, 0.06143986711200947, 0.1961012223813062, -0.05813354338170029, -0.07233632108424597, -0.40796291719501215, -0.26936597656458616, -0.17213569324909864, 0.12976320669986308, -0.1142617344445777, -0.2746821173180554, 0.39388796336910065, 0.0866903936645637, 0.23975238244747743, 0.11018018300334613, 0.22851054756514108, 0.15072104197073108, 0.044240471586817876, 0.0221038960153237, 0.14816823179717176, 0.12368567250571989, 0.03940775572361114, -0.12892743488191627, -0.05736675269266319, 0.16538698574489294]
|
707.1894
|
Polynomial-time algorithm for simulation of weakly interacting quantum
spin systems
|
We describe an algorithm that computes the ground state energy and
correlation functions for 2-local Hamiltonians in which interactions between
qubits are weak compared to single-qubit terms. The running time of the
algorithm is polynomial in the number of qubits and the required precision.
Specifically, we consider Hamiltonians of the form $H=H_0+\epsilon V$, where
H_0 describes non-interacting qubits, V is a perturbation that involves
arbitrary two-qubit interactions on a graph of bounded degree, and $\epsilon$
is a small parameter. The algorithm works if $|\epsilon|$ is below a certain
threshold value that depends only upon the spectral gap of H_0, the maximal
degree of the graph, and the maximal norm of the two-qubit interactions. The
main technical ingredient of the algorithm is a generalized Kirkwood-Thomas
ansatz for the ground state. The parameters of the ansatz are computed using
perturbative expansions in powers of $\epsilon$. Our algorithm is closely
related to the coupled cluster method used in quantum chemistry.
|
quant-ph
|
we describe an algorithm that computes the ground state energy and correlation functions for 2local hamiltonians in which interactions between qubits are weak compared to singlequbit terms the running time of the algorithm is polynomial in the number of qubits and the required precision specifically we consider hamiltonians of the form hh_0epsilon v where h_0 describes noninteracting qubits v is a perturbation that involves arbitrary twoqubit interactions on a graph of bounded degree and epsilon is a small parameter the algorithm works if epsilon is below a certain threshold value that depends only upon the spectral gap of h_0 the maximal degree of the graph and the maximal norm of the twoqubit interactions the main technical ingredient of the algorithm is a generalized kirkwoodthomas ansatz for the ground state the parameters of the ansatz are computed using perturbative expansions in powers of epsilon our algorithm is closely related to the coupled cluster method used in quantum chemistry
|
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|
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|
707.1895
|
Embedded Star Formation in the Eagle Nebula with Spitzer/GLIMPSE
|
We present new Spitzer photometry of the Eagle Nebula (M16, containing the
optical cluster NGC 6611) combined with near-infrared photometry from 2MASS. We
use dust radiative transfer models, mid-infrared and near-infrared color-color
analysis, and mid-infrared spectral indices to analyze point source spectral
energy distributions, select candidate young stellar objects (YSOs), and
constrain their mass and evolutionary state. Comparison of the different
protostellar selection methods shows that mid-infrared methods are consistent,
but as has been known for some time, near-infrared-only analysis misses some
young objects. We reveal more than 400 protostellar candidates, including one
massive young stellar object (YSO) that has not been previously highlighted.
The YSO distribution supports a picture of distributed low-level star
formation, with no strong evidence of triggered star formation in the
``pillars''. We confirm the youth of NGC 6611 by a large fraction of
infrared-excess sources, and reveal a younger cluster of YSOs in the nearby
molecular cloud. Analysis of the YSO clustering properties shows a possible
imprint of the molecular cloud's Jeans length. Multiwavelength mid-IR imaging
thus allows us to analyze the protostellar population, to measure the dust
temperature and column density, and to relate these in a consistent picture of
star formation in M16.
|
astro-ph
|
we present new spitzer photometry of the eagle nebula m16 containing the optical cluster ngc 6611 combined with nearinfrared photometry from 2mass we use dust radiative transfer models midinfrared and nearinfrared colorcolor analysis and midinfrared spectral indices to analyze point source spectral energy distributions select candidate young stellar objects ysos and constrain their mass and evolutionary state comparison of the different protostellar selection methods shows that midinfrared methods are consistent but as has been known for some time nearinfraredonly analysis misses some young objects we reveal more than 400 protostellar candidates including one massive young stellar object yso that has not been previously highlighted the yso distribution supports a picture of distributed lowlevel star formation with no strong evidence of triggered star formation in the pillars we confirm the youth of ngc 6611 by a large fraction of infraredexcess sources and reveal a younger cluster of ysos in the nearby molecular cloud analysis of the yso clustering properties shows a possible imprint of the molecular clouds jeans length multiwavelength midir imaging thus allows us to analyze the protostellar population to measure the dust temperature and column density and to relate these in a consistent picture of star formation in m16
|
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|
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|
707.1896
|
On the ultra high energy cosmic rays and the origin of the cosmic
microwave background radiation
|
Some inconsistencies to the assumption of a cosmological origin of the cosmic
microwave background CMB, such as the absence of gravitational lensing in the
WMAP data, open the doors to some speculations such as a local origin to the
CMB. We argue here that this assumption agrees with the absence of the GZK
cutoff (at least according to AGASA data) in the energy spectrum of the cosmic
ray due to the cosmic interaction with the CMB at $6\times 10^{19} eV$ or
above. Within 50 Mpc from Earth, the matter and light distributions are close
to an anisotropic distribution, where the local cluster and local
super-clusters of galaxies can be identified. In contrast, the ultra high
energy comic rays data is consistent to an almost isotropic distribution, and
there is no correlation between their arrival direction and astronomical
sources within our local cluster. This means that the events above the GZK
cutoff come from distances above 50 Mpc, without an apparent energy loss. This
scenario is plausible under the assumption of the CMB concentrated only within
3-4 Mpc from Earth. In other words, the CMB has a local origin linked only to
the local super-cluster of galaxies. In addition, the galactic and
extragalactic energy spectra index within the energy equipartition theorem
strongly constrains the dark matter and dark energy hypothesis, essential in
the Big Bang cosmology.
|
astro-ph
|
some inconsistencies to the assumption of a cosmological origin of the cosmic microwave background cmb such as the absence of gravitational lensing in the wmap data open the doors to some speculations such as a local origin to the cmb we argue here that this assumption agrees with the absence of the gzk cutoff at least according to agasa data in the energy spectrum of the cosmic ray due to the cosmic interaction with the cmb at 6times 1019 ev or above within 50 mpc from earth the matter and light distributions are close to an anisotropic distribution where the local cluster and local superclusters of galaxies can be identified in contrast the ultra high energy comic rays data is consistent to an almost isotropic distribution and there is no correlation between their arrival direction and astronomical sources within our local cluster this means that the events above the gzk cutoff come from distances above 50 mpc without an apparent energy loss this scenario is plausible under the assumption of the cmb concentrated only within 34 mpc from earth in other words the cmb has a local origin linked only to the local supercluster of galaxies in addition the galactic and extragalactic energy spectra index within the energy equipartition theorem strongly constrains the dark matter and dark energy hypothesis essential in the big bang cosmology
|
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|
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|
707.1897
|
Maximum Entropy, the Collective Welfare Principle and the Globalization
Process
|
Although both systems analyzed are described through two theories apparently
different (quantum mechanics and game theory) it is shown that both are
analogous and thus exactly equivalents. The quantum analogue of the replicator
dynamics is the von Neumann equation. Quantum mechanics could be used to
explain more correctly biological and economical processes. It could even
encloses theories like games and evolutionary dynamics. We can take some
concepts and definitions from quantum mechanics and physics for the best
understanding of the behavior of economics and biology. Also, we could maybe
understand nature like a game in where its players compete for a common welfare
and the equilibrium of the system that they are members. All the members of our
system will play a game in which its maximum payoff is the equilibrium of the
system. They act as a whole besides individuals like they obey a rule in where
they prefer to work for the welfare of the collective besides the individual
welfare. A system where its members are in Nash Equilibrium (or ESS) is exactly
equivalent to a system in a maximum entropy state. A system is stable only if
it maximizes the welfare of the collective above the welfare of the individual.
If it is maximized the welfare of the individual above the welfare of the
collective the system gets unstable an eventually collapses. The results of
this work shows that the "globalization" process has a behavior exactly
equivalent to a system that is tending to a maximum entropy state and predicts
the apparition of big common markets and strong common currencies that will
find its "equilibrium" by decreasing its number until they get a state
characterized by only one common currency and only one common market around the
world.
|
q-fin.GN physics.soc-ph
|
although both systems analyzed are described through two theories apparently different quantum mechanics and game theory it is shown that both are analogous and thus exactly equivalents the quantum analogue of the replicator dynamics is the von neumann equation quantum mechanics could be used to explain more correctly biological and economical processes it could even encloses theories like games and evolutionary dynamics we can take some concepts and definitions from quantum mechanics and physics for the best understanding of the behavior of economics and biology also we could maybe understand nature like a game in where its players compete for a common welfare and the equilibrium of the system that they are members all the members of our system will play a game in which its maximum payoff is the equilibrium of the system they act as a whole besides individuals like they obey a rule in where they prefer to work for the welfare of the collective besides the individual welfare a system where its members are in nash equilibrium or ess is exactly equivalent to a system in a maximum entropy state a system is stable only if it maximizes the welfare of the collective above the welfare of the individual if it is maximized the welfare of the individual above the welfare of the collective the system gets unstable an eventually collapses the results of this work shows that the globalization process has a behavior exactly equivalent to a system that is tending to a maximum entropy state and predicts the apparition of big common markets and strong common currencies that will find its equilibrium by decreasing its number until they get a state characterized by only one common currency and only one common market around the world
|
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|
[-0.11183959598768234, 0.1272118607351634, -0.14892106572137281, 0.11173416640235778, -0.03321178884747921, -0.17950270981351843, 0.08087647152477331, 0.33739790048600654, -0.2933509447307828, -0.26612695164000777, 0.10927364439583509, -0.32276853036433073, -0.1703842155294512, 0.13333484050545752, -0.07601448522938281, 0.0009044210914173563, 0.051444000799346495, 0.10818588714230537, 0.024434107252959917, -0.2566543777586886, 0.30370471511465014, 0.05273064174865376, 0.2587241014614509, 0.02054382919468293, 0.08676360291028812, -0.02427379921709715, 0.0737054018880628, 0.07746672638631154, -0.09719882241698383, 0.08528047510345955, 0.2728963326790796, 0.19229773588196927, 0.3473330663030654, -0.39531200190788435, -0.17494291187939315, 0.13357229486965538, 0.12187831507934917, 0.10186344749074992, 0.015625186592208053, -0.23863159261861516, 0.054273700755424266, -0.18470865509255158, -0.13277001720229067, -0.06772647231186762, 0.017290988480160172, 0.019855766289921868, -0.23386376290790148, 0.043731075549026936, 0.07813046652046785, 0.021538739367884255, -0.0653023321563186, -0.10967688610228386, -0.06544002246582094, 0.17872981326350512, 0.038235903287420846, -0.02634167300434815, 0.1595929144350396, -0.17175169891511374, -0.13548095851714156, 0.4370385423251444, -0.018225909170736253, -0.1524398802704405, 0.20628751355264963, -0.13680921567610346, -0.10848828752507549, 0.09320789055748366, 0.13092891335498566, 0.09164503331398559, -0.1555214571635338, 0.04104910501704693, -0.07608245397018608, 0.17119368549021877, 0.03548759122257508, 0.03524043899560763, 0.22763243671730674, 0.1407313962719848, 0.1132532662153564, 0.10972567684220348, 0.031189942112371735, -0.22016704245150423, -0.2649466250303019, -0.1846538239440327, -0.1612764478311474, 0.08076635885856089, -0.07022331766585165, -0.13671810862468636, 0.36736045202361967, 0.12599886267820432, 0.13616947972302124, 0.034477452604704986, 0.25002927026676197, 0.12761316975399442, 0.032326789363207376, 0.08717390065500673, 0.27090317854400536, 0.0780882447673155, 0.1174841327960779, -0.22196837648336498, 0.12561735355765702, 0.003203703326979633]
|
707.1898
|
Evolution of pion HBT radii from RHIC to LHC -- Predictions from ideal
hydrodynamics
|
We present hydrodynamic predictions for the charged pion HBT radii for a
range of initial conditions covering those presumably reached in Pb+Pb
collisions at the LHC. We study central (b=0) and semi-central (b=7fm)
collisions and show the expected increase of the HBT radii and their azimuthal
oscillations. The predicted trends in the oscillation amplitudes reflect a
change of the final source shape from out-of-plane to in-plane deformation as
the initial entropy density is increased.
|
nucl-th
|
we present hydrodynamic predictions for the charged pion hbt radii for a range of initial conditions covering those presumably reached in pbpb collisions at the lhc we study central b0 and semicentral b7fm collisions and show the expected increase of the hbt radii and their azimuthal oscillations the predicted trends in the oscillation amplitudes reflect a change of the final source shape from outofplane to inplane deformation as the initial entropy density is increased
|
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|
[-0.12681770576993387, 0.22476726926046692, -0.16394687332978394, 0.13640321253588397, 0.047586203830265635, -0.06549578227664102, -0.06111201834354601, 0.3253467555910553, -0.21468273274702568, -0.308676124154909, -0.008326861066488575, -0.3394979610018534, 0.053876546160509325, 0.16680785906437326, 0.02852790363847393, 0.07930593345033592, 0.13247409450330402, -0.005111787646804771, -0.11544633083913015, -0.14588382127949942, 0.284157306517232, 0.0883453230003584, 0.23681655101325005, 0.1317555337940177, -0.004879271688118373, 0.026402049953092453, -0.036060040746496554, 0.05026860223853425, -0.1929550437332045, 0.041563954479411906, 0.24082220187538292, 0.0172326556177274, 0.14889446092284706, -0.3567368051624053, -0.1218345343479759, 0.11111926596152456, 0.15379341016842485, 0.1678990632652828, -0.04354990478636927, -0.24152138354639485, 0.08622259609656382, -0.21340739571374573, -0.19084791655409827, 0.004496369919140045, 0.09844141683145745, 0.05801767902129827, -0.3011179378556011, 0.19301468711218808, 0.0010028807063625284, 0.10500061638933951, -0.09237231898491513, -0.19053829102840733, -0.08699871688341237, 0.060022881790383224, 0.10158057651189092, 0.0774723732531428, 0.2607073269095527, -0.14316930714037832, -0.06121721544800556, 0.35326999198479503, -0.009703630881307468, -0.0933033730707144, 0.16467297115452487, -0.2562884436154815, -0.07465764399847552, 0.14886622009033415, 0.2464645427925997, 0.05776102405220066, -0.11639733171116, -0.03878115744518167, 0.006337650405715079, 0.17771780672036622, 0.15609737004676502, 0.051424748107969556, 0.27074178081158906, 0.15892041442526683, -0.003593090207201161, 0.11595584660105102, -0.1351312504991991, -0.05265378435971598, -0.3768676199427206, -0.034644150162396366, -0.11137023973852804, 0.048085141397553356, -0.10345216957180066, -0.09359480930517798, 0.3649712339081891, 0.11990771766700974, 0.287831882882404, 0.011038687029113509, 0.25314738484711885, 0.07054431923850095, 0.06701347731653448, 0.07522400453916356, 0.33030511484774827, 0.18079423439076603, 0.2516657902208501, -0.33219319603992753, 0.05510269208135058, 0.029409965158963245]
|
707.1899
|
The $\ell^2$-homology of even Coxeter groups
|
Given a Coxeter system (W,S), there is an associated CW-complex, Sigma, on
which W acts properly and cocompactly. We prove that when the nerve L of (W,S)
is a flag triangulation of the 3-sphere, then the reduced $\ell^2$-homology of
Sigma vanishes in all but the middle dimension.
|
math.GT math.AT math.GR
|
given a coxeter system ws there is an associated cwcomplex sigma on which w acts properly and cocompactly we prove that when the nerve l of ws is a flag triangulation of the 3sphere then the reduced ell2homology of sigma vanishes in all but the middle dimension
|
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|
[-0.18061667595038863, 0.15994042492294536, -0.05038154648339495, 0.02361014518549943, -0.09778172041269693, -0.2148487235994098, 0.03141506728988656, 0.3235733035872591, -0.33799540838028524, -0.13810662526954362, 0.07139178186882922, -0.2969473824697606, -0.14687139476510755, 0.16681302690561464, -0.17006658092933766, -0.09468316531026776, 0.10278611233893861, 0.1685947400289885, -0.02473627743707534, -0.2883484536345969, 0.3485917110947218, -0.062329735864508656, 0.19615012956188715, 0.06748941590256513, 0.15528311287152005, 0.026742807217933078, -0.004595296338517615, 0.06817561487092617, -0.17220830503789872, 0.06782176660651222, 0.21468107388453914, 0.04797162269143031, 0.16795480877478072, -0.3153882133972613, -0.1671516728993664, 0.19593690736021133, 0.15201353426388603, -0.017143098639938584, 0.0371927234388769, -0.27890401036339874, 0.1289215781032405, -0.16382630997674263, -0.16415628529292473, 0.06729118866806334, 0.1256837777773592, -0.03582363524176973, -0.22120917679623087, -0.026957663638081324, 0.15429871668048362, 0.07631352581480082, -0.019586407455635516, -0.10616036361588681, -0.1619313394928232, 0.14317723923979545, -0.06918735149257044, 0.12459576894786764, 0.12428615375005818, -0.0749392939057756, -0.06028523865809783, 0.4256525882916089, -0.06471959599095614, -0.31530284133066044, 0.11856098243213714, -0.18705562074133691, -0.12219893226915217, 0.14286313887606275, 0.09309979225013484, 0.056782457254272195, 0.002429130946303361, 0.23641030957917386, -0.13790462995344338, 0.16487731166652086, 0.09224607141569574, -0.07135134221034799, 0.0694997621343491, 0.15741244257933043, 0.11372573331909928, 0.10396789236271635, -0.02892735902779795, 0.05223613190266522, -0.3792569395551022, -0.22760535871728937, -0.15552064360545434, 0.13582435551475971, -0.10597885169176771, -0.19485122114023629, 0.34217251096158585, -0.007278952331460537, 0.20402117826520128, 0.08436762173214253, 0.19073237415323865, 0.08173867378463136, 0.0741980577957757, 0.07407149666563627, 0.09058079496026039, 0.18435355955536695, -0.06186847050892229, -0.17583072422062385, -0.011732782346216287, 0.2040019704504533]
|
707.19
|
The complete catalogue of gamma-ray bursts observed by the Wide Field
Cameras on board BeppoSAX
|
We present the complete on-line catalogue of gamma-ray bursts observed by the
two Wide Field Cameras on board \sax in the period 1996-2002. Our aim is to
provide the community with the largest published data set of GRB's prompt
emission X-ray light curves and other useful data. This catalogue
(BS-GRBWFCcat) contains data on 77 bursts and a collection of the X-ray light
curves of 56 GRB discovered or noticed shortly after the event and of other
additional bursts detected in subsequent searches. Light curves are given in
the three X-ray energy bands (2-5, 5-10, 10-26 keV). The catalogue can be
accessed from the home web page of the ASI Science Data Center-ASDC
(http://www.asdc.asi.it)
|
astro-ph
|
we present the complete online catalogue of gammaray bursts observed by the two wide field cameras on board sax in the period 19962002 our aim is to provide the community with the largest published data set of grbs prompt emission xray light curves and other useful data this catalogue bsgrbwfccat contains data on 77 bursts and a collection of the xray light curves of 56 grb discovered or noticed shortly after the event and of other additional bursts detected in subsequent searches light curves are given in the three xray energy bands 25 510 1026 kev the catalogue can be accessed from the home web page of the asi science data centerasdc httpwwwasdcasiit
|
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|
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|
707.1901
|
Dimensionally hybrid Green's functions and density of states for
interfaces
|
The energy dependent Green's function for an interface Hamiltonian which
interpolates between two and three dimensions can be calculated explicitly.
This yields an expression for the density of states on the interface which
interpolates continuously between the two-dimensional behavior for high
energies and the three-dimensional behavior for low energies.
|
cond-mat.other
|
the energy dependent greens function for an interface hamiltonian which interpolates between two and three dimensions can be calculated explicitly this yields an expression for the density of states on the interface which interpolates continuously between the twodimensional behavior for high energies and the threedimensional behavior for low energies
|
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|
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|
707.1902
|
The Cauchy Problem for a Forced Harmonic Oscillator
|
We construct an explicit solution of the Cauchy initial value problem for the
one-dimensional Schroedinger equation with a time-dependent Hamiltonian
operator for the forced harmonic oscillator. The corresponding Green function
(propagator) is derived with the help of the generalized Fourier transform and
a relation with representations of the Heisenberg-Weyl group N(3) in a certain
special case first, and then is extended to the general case. A three parameter
extension of the classical Fourier integral is discussed as a by-product.
Motion of a particle with a spin in uniform perpendicular magnetic and electric
fields is considered as an application; a transition amplitude between Landau
levels is evaluated in terms of Charlier polynomials. In addition, we also
solve an initial value problem to a similar diffusion-type equation.
|
math-ph math.MP
|
we construct an explicit solution of the cauchy initial value problem for the onedimensional schroedinger equation with a timedependent hamiltonian operator for the forced harmonic oscillator the corresponding green function propagator is derived with the help of the generalized fourier transform and a relation with representations of the heisenbergweyl group n3 in a certain special case first and then is extended to the general case a three parameter extension of the classical fourier integral is discussed as a byproduct motion of a particle with a spin in uniform perpendicular magnetic and electric fields is considered as an application a transition amplitude between landau levels is evaluated in terms of charlier polynomials in addition we also solve an initial value problem to a similar diffusiontype equation
|
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|
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|
707.1903
|
Four-Loop Collinear Anomalous Dimension in N = 4 Yang-Mills Theory
|
We report a calculation in N = 4 Yang-Mills of the four-loop term g^4 in the
collinear anomalous dimension g(lambda) which governs the universal subleading
infrared structure of gluon scattering amplitudes. Using the method of
obstructions to extract this quantity from the 1/epsilon singularity in the
four-gluon iterative relation at four loops, we find g^4 = -1240.9 with an
estimated numerical uncertainty of 0.02%. We also analyze the implication of
our result for the strong coupling behavior of g(lambda), finding support for
the string theory prediction computed recently by Alday and Maldacena using
AdS/CFT.
|
hep-th
|
we report a calculation in n 4 yangmills of the fourloop term g4 in the collinear anomalous dimension glambda which governs the universal subleading infrared structure of gluon scattering amplitudes using the method of obstructions to extract this quantity from the 1epsilon singularity in the fourgluon iterative relation at four loops we find g4 12409 with an estimated numerical uncertainty of 002 we also analyze the implication of our result for the strong coupling behavior of glambda finding support for the string theory prediction computed recently by alday and maldacena using adscft
|
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|
[-0.15247112636935417, 0.09968347597376644, -0.12338488528269578, 0.11633340585439537, -0.026291300005351122, -0.09582470196227615, 0.04707744256925902, 0.30159381179364175, -0.20365826246216073, -0.26748681685549547, 0.031287546654661685, -0.3161737065107285, -0.19401305397859886, 0.13623703241471077, 0.01838277840147634, 0.0736746374609788, 0.014485923931575738, 0.04807587477102221, -0.09854544195663797, -0.23622483762677063, 0.33624780792640624, 0.011706083314493299, 0.24682919409734985, 0.14885547800132862, 0.10183507777689087, 0.03554728362647878, -0.05164292918333968, -0.01132007186802534, -0.15750844308922252, 0.10448872439747492, 0.22344344012582532, 0.040303835248738366, 0.11612898732694173, -0.37450260034465527, -0.15211287287196942, 0.01383300517573134, 0.1784910783273997, 0.110991878812406, 0.014886570741309897, -0.2180995426580801, 0.07825214542694144, -0.19295141518443495, -0.18910590263728339, -0.09545813774904953, 0.03733491144337497, -0.12053812893138237, -0.2953152614453767, 0.09120345084159123, 0.008359564770176842, 0.03902382832429894, -0.018284102103539875, -0.11580291277329836, -0.0023575944641789238, 0.10516805250253938, 0.10183939245621582, 0.1152195712438897, 0.0613787696277211, -0.19604407499319168, -0.16393380134704186, 0.30224413057574284, -0.0951436005154072, -0.12350579653610731, 0.09429065244026728, -0.1821437750451758, -0.20224422949704005, 0.1462708809131572, 0.09561982623987146, 0.14320186449465558, -0.13252834499376098, 0.17568257634699405, -0.016880211476645954, 0.15187881375499235, 0.12258258065852275, 0.032673253831300104, 0.158969004669196, 0.1260019897861959, -0.03966713541156643, 0.1501007815106557, -0.08258793672935648, -0.06266682951680415, -0.39937861456157087, -0.09292128342869026, -0.13669486789053287, 0.07911877079795186, -0.19727583491524225, -0.18024410502882776, 0.3127910984951266, 0.1553667851897714, 0.20992884021201222, 0.08244503070574745, 0.2520823505307947, 0.14538124226837082, 0.07550496880251628, 0.1063176478261824, 0.2961068379355001, 0.1668981333380913, 0.055356854757109844, -0.3238353419839149, -0.04708269265081201, 0.2073847666986614]
|
707.1904
|
Generalized Solution Concepts in Games with Possibly Unaware Players
|
Most work in game theory assumes that players are perfect reasoners and have
common knowledge of all significant aspects of the game. In earlier work, we
proposed a framework for representing and analyzing games with possibly unaware
players, and suggested a generalization of Nash equilibrium appropriate for
games with unaware players that we called generalized Nash equilibrium. Here,
we use this framework to analyze other solution concepts that have been
considered in the game-theory literature, with a focus on sequential
equilibrium. We also provide some insight into the notion of generalized Nash
equilibrium by proving that it is closely related to the notion of
rationalizability when we restrict the analysis to games in normal form and no
unawareness is involved.
|
cs.GT
|
most work in game theory assumes that players are perfect reasoners and have common knowledge of all significant aspects of the game in earlier work we proposed a framework for representing and analyzing games with possibly unaware players and suggested a generalization of nash equilibrium appropriate for games with unaware players that we called generalized nash equilibrium here we use this framework to analyze other solution concepts that have been considered in the gametheory literature with a focus on sequential equilibrium we also provide some insight into the notion of generalized nash equilibrium by proving that it is closely related to the notion of rationalizability when we restrict the analysis to games in normal form and no unawareness is involved
|
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|
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|
707.1905
|
s-Wave superconductivity in non-centrosymmetric Re_3W probed by magnetic
penetration depth
|
We report measurements of the temperature dependence of the magnetic
penetration depth \lambda(T) in non-centrosymmetric superconductor Re_3W. We
employed two experimental techniques: extraction of \lambda(T) from magnetic
{\em dc}-susceptibility, measured on a powder sample, and the rf tunnel diode
resonator technique, where a bulk polycrystalline sample was used. The results
of both techniques agree: the temperature dependence of the penetration depth
can be well described by weak-coupling, dirty-limit, s-wave BCS theory where we
obtain $\Delta(0)/k_BT_C=1.76$. No evidence for unconventional pairing
resulting from the absence of the inversion symmetry is found.
|
cond-mat.supr-con
|
we report measurements of the temperature dependence of the magnetic penetration depth lambdat in noncentrosymmetric superconductor re_3w we employed two experimental techniques extraction of lambdat from magnetic em dcsusceptibility measured on a powder sample and the rf tunnel diode resonator technique where a bulk polycrystalline sample was used the results of both techniques agree the temperature dependence of the penetration depth can be well described by weakcoupling dirtylimit swave bcs theory where we obtain delta0k_bt_c176 no evidence for unconventional pairing resulting from the absence of the inversion symmetry is found
|
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|
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|
707.1906
|
Materializing Superghosts
|
We construct the off-shell BV realization of N=1, d=10 SYM with 7 auxillary
fields. This becomes possible due to materialized ghost phenomenon. Namely,
supersymmetry ghosts are coordinates on a manifold B of 10-dimensional spinors
with pure spinors cut out. Auxillary fields are sections of a bundle over B,
and supersymmetry transformations are nonlinear in ghosts. By integrating out
axillary fields we obtain on-shell supersymmetric BV action with terms
quadratic in antifields. Exactly this on-shell BV action was obtained in our
previous paper after integration out of auxiliary fields in the framework of
Pure Spinor Superfield Formalism.
|
hep-th math-ph math.MP math.QA
|
we construct the offshell bv realization of n1 d10 sym with 7 auxillary fields this becomes possible due to materialized ghost phenomenon namely supersymmetry ghosts are coordinates on a manifold b of 10dimensional spinors with pure spinors cut out auxillary fields are sections of a bundle over b and supersymmetry transformations are nonlinear in ghosts by integrating out axillary fields we obtain onshell supersymmetric bv action with terms quadratic in antifields exactly this onshell bv action was obtained in our previous paper after integration out of auxiliary fields in the framework of pure spinor superfield formalism
|
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|
707.1907
|
A Catalog of Diffuse X-ray-Emitting Features within 20 pc of Sgr A*:
Twenty Pulsar Wind Nebulae?
|
We present a catalog of 34 diffuse features identified in X-ray images of the
Galactic center taken with the Chandra X-ray Observatory. Several of the
features have been discussed in the literature previously, including 7 that are
associated with a complex of molecular clouds that exhibits fluorescent line
emission, 4 that are superimposed on the supernova remnant Sgr A East, 2 that
are coincident with radio features that are thought to be the shell of another
supernova remnant, and one that is thought to be a pulsar wind nebula only a
few arcseconds in projection from Sgr A*. However, this leaves 20 features that
have not been reported previously. Based on the weakness of iron emission in
their spectra, we propose that most of them are non-thermal. One long, narrow
feature points toward Sgr A*, and so we propose that this feature is a jet of
synchrotron-emitting particles ejected from the supermassive black hole. For
the others, we show that their sizes (0.1-2 pc in length for D=8 kpc), X-ray
luminosities (between 10^32 and 10^34 erg/s, 2-8 keV), and spectra (power laws
with Gamma=1-3) are consistent with those of pulsar wind nebulae. Based on the
star formation rate at the Galactic center, we expect that ~20 pulsars have
formed in the last 300 kyr, and could be producing pulsar wind nebulae. Only
one of the 19 candidate pulsar wind nebulae is securely detected in an archival
radio image of the Galactic center; the remainder have upper limits
corresponding to L_R<la10^31 erg/s. These radio limits do not strongly
constrain their natures, which underscores the need for further multi-
wavelength studies of this unprecedented sample of Galactic X-ray emitting
structures.
|
astro-ph
|
we present a catalog of 34 diffuse features identified in xray images of the galactic center taken with the chandra xray observatory several of the features have been discussed in the literature previously including 7 that are associated with a complex of molecular clouds that exhibits fluorescent line emission 4 that are superimposed on the supernova remnant sgr a east 2 that are coincident with radio features that are thought to be the shell of another supernova remnant and one that is thought to be a pulsar wind nebula only a few arcseconds in projection from sgr a however this leaves 20 features that have not been reported previously based on the weakness of iron emission in their spectra we propose that most of them are nonthermal one long narrow feature points toward sgr a and so we propose that this feature is a jet of synchrotronemitting particles ejected from the supermassive black hole for the others we show that their sizes 012 pc in length for d8 kpc xray luminosities between 1032 and 1034 ergs 28 kev and spectra power laws with gamma13 are consistent with those of pulsar wind nebulae based on the star formation rate at the galactic center we expect that 20 pulsars have formed in the last 300 kyr and could be producing pulsar wind nebulae only one of the 19 candidate pulsar wind nebulae is securely detected in an archival radio image of the galactic center the remainder have upper limits corresponding to l_rla1031 ergs these radio limits do not strongly constrain their natures which underscores the need for further multi wavelength studies of this unprecedented sample of galactic xray emitting structures
|
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|
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|
707.1908
|
The Transit Light Curve Project. VII. The Not-So-Bloated Exoplanet
HAT-P-1b
|
We present photometry of the G0 star HAT-P-1 during six transits of its
close-in giant planet, and we refine the estimates of the system parameters.
Relative to Jupiter's properties, HAT-P-1b is 1.20 +/- 0.05 times larger and
its surface gravity is 2.7 +/- 0.2 times weaker. Although it remains the case
that HAT-P-1b is among the least dense of the known sample of transiting
exoplanets, its properties are in accord with previously published models of
strongly irradiated, coreless, solar-composition giant planets. The times of
the transits have a typical accuracy of 1 min and do not depart significantly
from a constant period.
|
astro-ph
|
we present photometry of the g0 star hatp1 during six transits of its closein giant planet and we refine the estimates of the system parameters relative to jupiters properties hatp1b is 120 005 times larger and its surface gravity is 27 02 times weaker although it remains the case that hatp1b is among the least dense of the known sample of transiting exoplanets its properties are in accord with previously published models of strongly irradiated coreless solarcomposition giant planets the times of the transits have a typical accuracy of 1 min and do not depart significantly from a constant period
|
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|
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|
707.1909
|
Interstitial Fractionalization and Spherical Crystallography
|
Finding the ground states of identical particles packed on spheres has
relevance for stabilizing emulsions and a venerable history in the literature
of theoretical physics and mathematics. Theory and experiment have confirmed
that defects such as disclinations and dislocations are an intrinsic part of
the ground state. Here we discuss the remarkable behavior of vacancies and
interstitials in spherical crystals. The strain fields of isolated
disclinations forced in by the spherical topology literally rip interstitials
and vacancies apart, typically into dislocation fragments that combine with the
disclinations to create small grain boundary scars. The fractionation is often
into three charge-neutral dislocations, although dislocation pairs can be
created as well. We use a powerful, freely available computer program to
explore interstitial fractionalization in some detail, for a variety of power
law pair potentials. We investigate the dependence on initial conditions and
the final state energies, and compare the position dependence of interstitial
energies with the predictions of continuum elastic theory on the sphere. The
theory predicts that, before fragmentation, interstitials are repelled from
5-fold disclinations and vacancies are attracted. We also use vacancies and
interstitials to study low energy states in the vicinity of "magic numbers"
that accommodate regular icosadeltahedral tessellations.
|
cond-mat.soft
|
finding the ground states of identical particles packed on spheres has relevance for stabilizing emulsions and a venerable history in the literature of theoretical physics and mathematics theory and experiment have confirmed that defects such as disclinations and dislocations are an intrinsic part of the ground state here we discuss the remarkable behavior of vacancies and interstitials in spherical crystals the strain fields of isolated disclinations forced in by the spherical topology literally rip interstitials and vacancies apart typically into dislocation fragments that combine with the disclinations to create small grain boundary scars the fractionation is often into three chargeneutral dislocations although dislocation pairs can be created as well we use a powerful freely available computer program to explore interstitial fractionalization in some detail for a variety of power law pair potentials we investigate the dependence on initial conditions and the final state energies and compare the position dependence of interstitial energies with the predictions of continuum elastic theory on the sphere the theory predicts that before fragmentation interstitials are repelled from 5fold disclinations and vacancies are attracted we also use vacancies and interstitials to study low energy states in the vicinity of magic numbers that accommodate regular icosadeltahedral tessellations
|
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|
[-0.0831998624955304, 0.20929160309671715, -0.05976705586304888, 0.07969796281598975, -0.006986450996482745, -0.10070588745322312, 0.039074371185270136, 0.4056629677582532, -0.2410662435600534, -0.2886518023593817, 0.03439484925533179, -0.3309254566114396, -0.10987129142391495, 0.07953711725771427, -0.009033331897226162, 0.013195541747845709, 0.053683481664629655, -0.013854298128280788, -0.0332232096788357, -0.22898900869302452, 0.29373200294096025, 0.06015880456659943, 0.3075201283302158, 0.08308496564626694, 0.029327905949321574, 0.0007021884221467189, 0.06450559523887932, 0.07661013988312333, -0.19170863579041908, 0.08689606439962518, 0.2319744820566848, 0.007321466709254309, 0.19284937311895192, -0.5447348140086978, -0.20300361195812003, 0.06957311704754829, 0.1538276796846185, 0.17685602817102336, -0.09909840322099626, -0.2836703386902809, 0.07330331755336374, -0.12288805351592601, -0.14856973456102424, -0.07893122559413314, 0.05026747321011499, 0.051127670551650226, -0.19450749232899398, 0.09839935953132226, 0.03970253301420598, 0.06643053251318634, -0.13490508410846813, -0.12157246912131087, -0.1199179177370388, 0.07971595443203114, 0.05804460233892314, -0.008132444181246683, 0.20234112253412603, -0.13132162048481405, -0.13388638100354, 0.41321897813118996, 0.042982604927383365, -0.1600594918942079, 0.2027916407980956, -0.13794356926693582, -0.12977373836096376, 0.17082695170887746, 0.15770141828339546, 0.08579842502211249, -0.08645969858160242, 0.06461783229213325, -0.00350845908455085, 0.14734743107343093, 0.10585455648368225, 0.023255124119459653, 0.25509838659781964, 0.1509776745142881, 0.039597719149896876, 0.15396663273160813, -0.10415103600333168, -0.11444976857630536, -0.2753465892933309, -0.20300721342675387, -0.20753438630439633, 0.02163815133506432, -0.06120240240517887, -0.2062206549034454, 0.32064826937858015, 0.06886302708182485, 0.18309474221197888, -0.03476992483017966, 0.18411486545577646, 0.0232902276981622, 0.06570302698062733, 0.018099731751717626, 0.22273070134993758, 0.14597390850656666, 0.08555623473366722, -0.1979915956617333, 0.04100020375335589, 0.05201216143206693]
|
707.191
|
Dispersive, superfluid-like shock waves in nonlinear optics
|
In most classical fluids, shock waves are strongly dissipative, their energy
being quickly lost through viscous damping. But in systems such as cold
plasmas, superfluids, and Bose-Einstein condensates, where viscosity is
negligible or non-existent, a fundamentally different type of shock wave can
emerge whose behaviour is dominated by dispersion rather than dissipation.
Dispersive shock waves are difficult to study experimentally, and analytical
solutions to the equations that govern them have only been found in one
dimension (1D). By exploiting a well-known, but little appreciated,
correspondence between the behaviour of superfluids and nonlinear optical
materials, we demonstrate an all-optical experimental platform for studying the
dynamics of dispersive shock waves. This enables us to observe the propagation
and nonlinear response of dispersive shock waves, including the interaction of
colliding shock waves, in 1D and 2D. Our system offers a versatile and more
accessible means for exploring superfluid-like and related dispersive
phenomena.
|
physics.optics cond-mat.other physics.flu-dyn
|
in most classical fluids shock waves are strongly dissipative their energy being quickly lost through viscous damping but in systems such as cold plasmas superfluids and boseeinstein condensates where viscosity is negligible or nonexistent a fundamentally different type of shock wave can emerge whose behaviour is dominated by dispersion rather than dissipation dispersive shock waves are difficult to study experimentally and analytical solutions to the equations that govern them have only been found in one dimension 1d by exploiting a wellknown but little appreciated correspondence between the behaviour of superfluids and nonlinear optical materials we demonstrate an alloptical experimental platform for studying the dynamics of dispersive shock waves this enables us to observe the propagation and nonlinear response of dispersive shock waves including the interaction of colliding shock waves in 1d and 2d our system offers a versatile and more accessible means for exploring superfluidlike and related dispersive phenomena
|
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|
[-0.18280367757332036, 0.193853200482921, -0.0799454362256665, 0.08905243168931905, -0.12805275162744442, -0.18034595180140345, -0.04592805831527475, 0.36135810273605706, -0.278943774006767, -0.245932783806484, 0.05483557602926626, -0.28693571069821616, -0.139944813984615, 0.2549330049878824, 0.0883375278661565, 0.07894121726502933, 0.014457864506363919, -0.06613251852690423, -0.018032866022268296, -0.1364344801111522, 0.3138194028288126, 0.04629454870345758, 0.25923973399108186, 0.051453028844619456, 0.08024891825930384, -0.041189604282579166, 0.010851040414937665, 0.017272035431916882, -0.13243290577139494, 0.045307347758816896, 0.25131373712832056, 0.013829504735080288, 0.23810602025435174, -0.5247152891235064, -0.3225228874787888, 0.03466188619632099, 0.20233010530671816, 0.1697036131541401, -0.04563123760199965, -0.29955433459714953, -0.04574714451653245, -0.158791429483513, -0.1749787688217807, -0.08447409426362172, 0.056645852276092805, 0.058596878723497656, -0.20913691268515017, 0.1429547503490576, 0.0631833297904462, 0.022905980955634342, -0.05824265006192079, -0.003168333042881783, -0.04820764303401163, 0.03496671690927481, 0.05568241146658766, -0.02324812230966585, 0.10473891024027744, -0.20126043028126303, -0.04762156653661756, 0.4490773188256527, -0.06396514148306455, -0.16935540748378825, 0.322000594150225, -0.16263589919322083, -0.0026606848204020887, 0.18974679219067697, 0.17584302372005362, 0.08684516638117348, -0.13843478223046402, -0.011969660188074554, -0.01623400397613979, 0.14589751123891356, 0.11485959266799958, 0.07880475638971833, 0.24094909617689833, 0.19764684067238997, -0.008138294777076616, 0.13240988357906736, -0.0343922083104934, -0.06382646875443475, -0.23232353853621213, -0.1431824015906618, -0.15517189250571417, 0.03880954195693332, -0.043631334400102154, -0.16102797114884093, 0.3738184958280708, 0.16713808644242623, 0.10887300470006346, -0.03154551729266125, 0.2731433128500545, 0.1495979857270062, 0.015720372546101678, 0.11157379631161488, 0.3386846996293772, 0.16329354437493138, 0.13656397392323252, -0.2432496842858694, 0.043069151534867664, 0.02822511212903406]
|
707.1911
|
Dispersive shock waves with nonlocal nonlinearity
|
We consider dispersive optical shock waves in nonlocal nonlinear media.
Experiments are performed using spatial beams in a thermal liquid cell, and
results agree with a hydrodynamic theory of propagation.
|
physics.optics nlin.PS physics.flu-dyn
|
we consider dispersive optical shock waves in nonlocal nonlinear media experiments are performed using spatial beams in a thermal liquid cell and results agree with a hydrodynamic theory of propagation
|
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|
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|
707.1912
|
Throughput Scaling Laws for Wireless Networks with Fading Channels
|
A network of n communication links, operating over a shared wireless channel,
is considered. Fading is assumed to be the dominant factor affecting the
strength of the channels between transmitter and receiver terminals. It is
assumed that each link can be active and transmit with a constant power P or
remain silent. The objective is to maximize the throughput over the selection
of active links. By deriving an upper bound and a lower bound, it is shown that
in the case of Rayleigh fading (i) the maximum throughput scales like $\log n$
(ii) the maximum throughput is achievable in a distributed fashion. The upper
bound is obtained using probabilistic methods, where the key point is to upper
bound the throughput of any random set of active links by a chi-squared random
variable. To obtain the lower bound, a decentralized link activation strategy
is proposed and analyzed.
|
cs.IT math.IT
|
a network of n communication links operating over a shared wireless channel is considered fading is assumed to be the dominant factor affecting the strength of the channels between transmitter and receiver terminals it is assumed that each link can be active and transmit with a constant power p or remain silent the objective is to maximize the throughput over the selection of active links by deriving an upper bound and a lower bound it is shown that in the case of rayleigh fading i the maximum throughput scales like log n ii the maximum throughput is achievable in a distributed fashion the upper bound is obtained using probabilistic methods where the key point is to upper bound the throughput of any random set of active links by a chisquared random variable to obtain the lower bound a decentralized link activation strategy is proposed and analyzed
|
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|
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|
707.1913
|
Removing Manually-Generated Boilerplate from Electronic Texts:
Experiments with Project Gutenberg e-Books
|
Collaborative work on unstructured or semi-structured documents, such as in
literature corpora or source code, often involves agreed upon templates
containing metadata. These templates are not consistent across users and over
time. Rule-based parsing of these templates is expensive to maintain and tends
to fail as new documents are added. Statistical techniques based on frequent
occurrences have the potential to identify automatically a large fraction of
the templates, thus reducing the burden on the programmers. We investigate the
case of the Project Gutenberg corpus, where most documents are in ASCII format
with preambles and epilogues that are often copied and pasted or manually
typed. We show that a statistical approach can solve most cases though some
documents require knowledge of English. We also survey various technical
solutions that make our approach applicable to large data sets.
|
cs.DL cs.CL
|
collaborative work on unstructured or semistructured documents such as in literature corpora or source code often involves agreed upon templates containing metadata these templates are not consistent across users and over time rulebased parsing of these templates is expensive to maintain and tends to fail as new documents are added statistical techniques based on frequent occurrences have the potential to identify automatically a large fraction of the templates thus reducing the burden on the programmers we investigate the case of the project gutenberg corpus where most documents are in ascii format with preambles and epilogues that are often copied and pasted or manually typed we show that a statistical approach can solve most cases though some documents require knowledge of english we also survey various technical solutions that make our approach applicable to large data sets
|
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|
[-0.052433923397351194, 0.014236512497343399, -0.022958713390485004, 0.10981041876754413, -0.18769495899582075, -0.13693038755682885, 0.08528703334051425, 0.4281341268508523, -0.24104447412580526, -0.38803946587981447, 0.11042032832693723, -0.34022010164680305, -0.0752605279480728, 0.2140908230130595, -0.11946719674807456, 0.04208453796821198, 0.12416023115317026, 0.033828355068409886, -0.007641131527014767, -0.2939950613098012, 0.3343602315091562, 0.029905585751489355, 0.29666980300098655, -0.01537264368876263, 0.01900923341874861, -0.0633867393506484, -0.13093190821646541, -0.0048691245916011715, -0.05503683523873203, 0.12769963511576254, 0.39216559480323837, 0.2569623012492364, 0.279835269600153, -0.4474836199509877, -0.15057313944454545, 0.06344246695645982, 0.15844201097368366, 0.1599141300862862, -0.012311083709614144, -0.29803980612885894, 0.11307341564032766, -0.1815472042877917, 0.008817413366503185, -0.14564313931580358, -0.011794794043008651, 0.05829723041711582, -0.22925297067742104, 0.025529388243254895, 0.05726865952213605, 0.08023795935635765, -0.006984211844219654, -0.15359592032101418, 0.010161059968070024, 0.16154528291102638, 0.06474535297602416, 0.028449422314211173, 0.11879070933425316, -0.1212934540912371, -0.09855627872532717, 0.4158623425221002, -0.016590482072421798, -0.22649047979050213, 0.224083816713688, -0.024780979980628386, -0.18114483246786728, 0.10885500008740497, 0.22123766435586192, 0.11649131664523373, -0.19881988947314244, 0.031286409067817864, -0.014983769557956193, 0.28198086517621523, 0.10329967816360294, 0.0062458512718202895, 0.19711062267974572, 0.15828667366877197, -0.020003172675044173, 0.11456248968218764, -0.0417972028746994, -0.05575339114120989, -0.24093166157534276, -0.10428123380988837, -0.1836532308685559, -0.014010827786491804, -0.07346596523938287, -0.21708247050022086, 0.33255780658650175, 0.23486118319754798, 0.14265182974782806, 0.08531712198315222, 0.30505445789959695, -0.03173816701811221, 0.15156224580800712, 0.09148083588246395, 0.0998362548772194, -0.0515544173359457, 0.13200780178627206, -0.08933014822261477, 0.13098595793029139, 0.003767446532017655]
|
707.1914
|
Towards a New Standard Theory for Astrophysical Disk Accretion
|
We briefly review recent developments in black hole accretion disk theory,
placing new emphasis on the vital role played by magnetohydrodynamic (MHD)
stresses in transporting angular momentum. The apparent universality of
accretion-related outflow phenomena is a strong indicator that vertical
transport of angular momentum by large-scale MHD torques is important and may
even dominate radial transport by small-scale MHD turbulence. This leads to an
enhanced overall rate of angular momentum transport and allows accretion of
matter to proceed at an interesting rate. Furthermore, we argue that when
vertical transport is important, the radial structure of the accretion disk is
modified and this affects the disk emission spectrum. We present a simple model
demonstrating that energetic, magnetically-driven outflows give rise to a disk
spectrum that is dimmer and redder than a standard accretion disk accreting at
the same rate. We briefly discuss the implications of this key result for
accreting black holes in different astrophysical systems.
|
astro-ph
|
we briefly review recent developments in black hole accretion disk theory placing new emphasis on the vital role played by magnetohydrodynamic mhd stresses in transporting angular momentum the apparent universality of accretionrelated outflow phenomena is a strong indicator that vertical transport of angular momentum by largescale mhd torques is important and may even dominate radial transport by smallscale mhd turbulence this leads to an enhanced overall rate of angular momentum transport and allows accretion of matter to proceed at an interesting rate furthermore we argue that when vertical transport is important the radial structure of the accretion disk is modified and this affects the disk emission spectrum we present a simple model demonstrating that energetic magneticallydriven outflows give rise to a disk spectrum that is dimmer and redder than a standard accretion disk accreting at the same rate we briefly discuss the implications of this key result for accreting black holes in different astrophysical systems
|
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|
[-0.16146484052071408, 0.15714700955676006, -0.05260922283369807, 0.1404726827532173, -0.10871935129886673, -0.07780986975037282, -0.04472845702191755, 0.3650933055026877, -0.24795712043320942, -0.2870646121581235, 0.0528469753819668, -0.2252341172414749, -0.06844736694568587, 0.24737081624897977, -0.03384088699014917, 0.015328290610904655, 0.048648496287604495, -0.12067474410118115, -0.05016054178948604, -0.17452556246050424, 0.3612602934151167, 0.17872649243762417, 0.18911471721986609, 0.038983643652811165, 0.06438284881653324, -0.08083528949158086, -0.05999069655494344, 0.008166935650872127, -0.209438729900003, 0.05892729562286648, 0.1893587363343085, 0.059971340685602156, 0.2365768285933882, -0.4533395628249573, -0.24908517086765758, 0.00422290826757108, 0.22190554449034314, 0.10050467615045848, -0.11845144149772222, -0.15216752468578276, 0.03360015161095127, -0.233473346556627, -0.15854826317874776, -0.014277258611494495, 0.07853251802584817, -0.010394016521111611, -0.2311470591662181, 0.1607786242286825, 0.1504676472448233, 0.02883189097046852, -0.1048818570956017, -0.05354447083908223, -0.09542648695529468, 0.060500648442933694, 0.12458795821669721, 0.06276673526360443, 0.23436421746568334, -0.16674044135987998, -0.08056070976439983, 0.39491929421501776, -0.05900460597805514, -0.10583303604695586, 0.2163597323969307, -0.2500673482014287, -0.12254786651221014, 0.14133997302832862, 0.19447744270005535, 0.1170652226199426, -0.10373924477260575, 0.015014393496957998, -0.062192935208159106, 0.13842494988573656, 0.0272491414340273, 0.07764189989576417, 0.40283626591967, 0.15208886730364493, 0.03252718726909089, 0.126680258835756, -0.15324996903448576, -0.09026302804028796, -0.2540875436993496, -0.1456517837821476, -0.1151546282517243, 0.14282222784935467, -0.10800588757753553, -0.1009148474632492, 0.333640411288868, 0.158495125835461, 0.20871925504217226, -0.03896785499828477, 0.31972019812517005, 0.12566554119750376, 0.028116748346045852, 0.18310401923053207, 0.3308134840440846, 0.16437194330407487, 0.16378157441654512, -0.3096928564681401, 0.06946544022704926, 0.05936881890182474]
|
707.1915
|
MICE: The International Muon Ionization Cooling Experiment
|
Muon storage rings have been proposed for use as a source of high-energy
neutrino beams (the Neutrino Factory) and as the basis for a high-energy
lepton-antilepton collider (the Muon Collider). The Neutrino Factory is widely
believed to be the machine of choice for the search for leptonic CP violation
while the Muon Collider may prove to be the most practical route to multi-TeV
lepton-antilepton collisions. The baseline conceptual designs for each of these
facilities requires the phase-space compression (cooling) of the muon beams
prior to acceleration. The short muon lifetime makes it impossible to employ
traditional techniques to cool the beam while maintaining the muon-beam
intensity. Ionization cooling, a process in which the muon beam is passed
through a series of liquid-hydrogen absorbers followed by accelerating RF
cavities, is the technique proposed to cool the muon beam. The international
Muon Ionization Cooling Experiment (MICE) collaboration will carry out a
systematic study of ionization cooling. The MICE experiment, which is under
construction at the Rutherford Appleton Laboratory, will begin to take data
late this year. The MICE cooling channel, the instrumentation and the
implementation at the Rutherford Appleton Laboratory are described together
with the predicted performance of the channel and the measurements that will be
made.
|
physics.acc-ph hep-ph
|
muon storage rings have been proposed for use as a source of highenergy neutrino beams the neutrino factory and as the basis for a highenergy leptonantilepton collider the muon collider the neutrino factory is widely believed to be the machine of choice for the search for leptonic cp violation while the muon collider may prove to be the most practical route to multitev leptonantilepton collisions the baseline conceptual designs for each of these facilities requires the phasespace compression cooling of the muon beams prior to acceleration the short muon lifetime makes it impossible to employ traditional techniques to cool the beam while maintaining the muonbeam intensity ionization cooling a process in which the muon beam is passed through a series of liquidhydrogen absorbers followed by accelerating rf cavities is the technique proposed to cool the muon beam the international muon ionization cooling experiment mice collaboration will carry out a systematic study of ionization cooling the mice experiment which is under construction at the rutherford appleton laboratory will begin to take data late this year the mice cooling channel the instrumentation and the implementation at the rutherford appleton laboratory are described together with the predicted performance of the channel and the measurements that will be made
|
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|
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|
707.1916
|
Lattice with a Twist : Helical Waveguides for Ultracold Matter
|
We investigate the waveguiding properties of the optical interference pattern
of two counter-propagating Laguerre-Gaussian beams. The number, helicity,
radius, pitch, depth and frequencies of transverse confinement of the
waveguides are simply related to the beam parameters. Quantitative connections
to the familiar Gaussian optical lattice are made and an application to quantum
transport is suggested.
|
physics.atom-ph physics.optics
|
we investigate the waveguiding properties of the optical interference pattern of two counterpropagating laguerregaussian beams the number helicity radius pitch depth and frequencies of transverse confinement of the waveguides are simply related to the beam parameters quantitative connections to the familiar gaussian optical lattice are made and an application to quantum transport is suggested
|
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|
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|
707.1917
|
A New Experiment to Study Hyperon CP Violation, Charmonium, and Charm
|
Fermilab operates the world's most intense antiproton source, now exclusively
dedicated to serving the needs of the Tevatron Collider. The anticipated 2009
shutdown of the Tevatron presents the opportunity for world-leading low- and
medium-energy antiproton programs. We summarize the status of the Fermilab
antiproton facility and review physics topics for which a future experiment
could make the world's best measurements.
|
hep-ex hep-ph
|
fermilab operates the worlds most intense antiproton source now exclusively dedicated to serving the needs of the tevatron collider the anticipated 2009 shutdown of the tevatron presents the opportunity for worldleading low and mediumenergy antiproton programs we summarize the status of the fermilab antiproton facility and review physics topics for which a future experiment could make the worlds best measurements
|
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|
[-0.058358544018119574, 0.186622815237691, -0.1231105518527329, 0.13130591929657384, -0.1811878284594665, -0.13810910746299973, 0.05677960853402813, 0.2892685509209211, -0.16207550578789476, -0.35421773242608956, 0.06682534168940038, -0.39821603503078223, 0.110792391297097, 0.22720535644330084, 0.04410619324383636, 0.13426333839888685, 0.17504946548918573, -0.052380142252271375, 0.017617445020005108, -0.26733363583528746, 0.1890536311858644, 0.2875148865394294, 0.3021546266041696, 0.15514672870437304, 0.08399675354982415, 0.00310569731615639, -0.12942216504986087, -0.14023671531273674, -0.06822492460050852, 0.09387877848154555, 0.3901925522213181, 0.24975467013816038, 0.16871311234814737, -0.474289857596159, -0.04597161915153265, 0.12335595218076681, 0.05342628139769658, 0.05842891401262022, -0.11286221733316779, -0.2771637922890174, 0.004748135078504371, -0.25205924857097367, -0.1712928155126671, 0.03952772000338882, 0.008710621568995217, -0.012907674994009237, -0.2666535671489934, -0.10536143898498267, -0.08586331992410123, 0.08947517837708195, -0.008384704834315925, -0.26302486314283063, 0.06776360179064796, 0.03908132875803858, 0.040295569024359185, 0.108242528901125, 0.16098880406158667, -0.1519860029608632, -0.22555802419471244, 0.3630989331752062, -0.0351802472025156, 0.01382907228350329, 0.21726800790056586, -0.2653946784984631, -0.14311237237416208, 0.04336503143907369, 0.2694820042078694, 0.055244595479841035, -0.2592502173036337, 0.11481414506609629, 0.005749226299424966, 0.13134419380221515, 0.03616555139111976, 0.04006165135651827, 0.3082617059970895, 0.30309473543117443, 0.09506528144702316, 0.04216779905060927, -0.16935598949203268, -0.020678554739182193, -0.45919569707475605, -0.08438231190666556, -0.047709874374171096, 0.012683772450933854, 0.17883706645467706, 0.002466306524972121, 0.4085959939286113, 0.15537525868664184, 0.16072255176162192, -0.08464203084780214, 0.35845559236283103, -0.04464605526106122, 0.07731852560779467, 0.05813932651338594, 0.34355120323598387, 0.05154903040420322, 0.3020253601484001, -0.21273477027813595, 0.09188957103372862, -0.009764928898463646]
|
707.1918
|
Application of Extended Kalman Filter to Tactical Ballistic Missile
Re-entry Problem
|
The objective is to investigate the advantages and performance of Extended
Kalman Filter for the estimation of non-linear system where linearization takes
place about a trajectory that was continually updated with the state estimates
resulting from the measurement. Here tactile ballistic missile Re-entry problem
is taken as a nonlinear system model and Extended Kalman Filter technique is
used to estimate the positions and velocities at the X and Y direction at
different values of ballistic coefficients. The result shows that the method
gives better estimation with the increase of ballistic coefficient.
|
math.OC
|
the objective is to investigate the advantages and performance of extended kalman filter for the estimation of nonlinear system where linearization takes place about a trajectory that was continually updated with the state estimates resulting from the measurement here tactile ballistic missile reentry problem is taken as a nonlinear system model and extended kalman filter technique is used to estimate the positions and velocities at the x and y direction at different values of ballistic coefficients the result shows that the method gives better estimation with the increase of ballistic coefficient
|
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|
[-0.07271315125175394, 0.032081465518286265, -0.13870910903090958, -0.017811779985664883, -0.07274111984092947, -0.17467290417874579, 0.006492894531770067, 0.37390369418394437, -0.2926674849957555, -0.29400700936605645, 0.11022195559772817, -0.28087398170360495, -0.12798292261284808, 0.21410612614344354, -0.07331506864444076, 0.07483846279117662, 0.08319337810338526, 0.051460022306335826, -0.07305074656627826, -0.2090067763168078, 0.21813830744045284, 0.07626012297203907, 0.2692951163696637, -0.027596729674509594, 0.19802394915489827, 0.053305838855781724, -0.01828116182606299, 0.009520597520519744, -0.12089373369187573, 0.06393675400573597, 0.21752075208248672, 0.062311956249586825, 0.29957364241664225, -0.36132378565086115, -0.21256908700688854, 0.053893454265422545, 0.15325284746199191, 0.10767777495413691, 0.01148802501911932, -0.3390603086164037, 0.06526322314863676, -0.14953203817604335, -0.1221333517396188, 0.0071905023356961025, -0.008164911303198435, 0.008805354161617847, -0.32573823853917827, 0.1043885652037276, 0.05978782415891496, 0.009155433604514205, -0.08082255662756634, -0.13193332134479924, -0.0146077278141792, 0.14257040083060388, 0.027827371660220836, 0.025241536538597648, 0.17188679894616643, -0.09523570906514159, -0.06673999022242132, 0.35149204896783437, -0.07775040575594815, -0.19105400973521583, 0.14411226127317156, -0.1268319025594782, -0.03710843917432722, 0.1838289056546413, 0.21512990358930367, 0.07210772665688298, -0.13985474299189155, 0.027859444169655113, -0.014165173868065352, 0.16841442455220354, 0.003817594410585506, 0.01474993860676557, 0.1413306408884147, 0.16595409364071112, 0.11784400228810098, 0.11816152265541009, -0.16096141254836385, -0.08454246700045417, -0.2546724875631568, -0.14406450904117754, -0.1781166761289709, -0.011310404302183908, -0.08955095433003198, -0.12279029520980728, 0.3992882141188442, 0.2344417806157003, 0.2110078636925299, 0.04170050373515831, 0.33562500260074385, 0.1690054744070109, 0.013578679995959277, 0.055853727202002816, 0.23154612261146962, 0.12111838383006525, 0.14827364760932032, -0.2356314283544914, 0.11138963843644648, 0.0940459761819751]
|
707.1919
|
Search for Effect of Influence from Future in Large Hadron Collider
|
We propose an experiment which consists of drawing a card and using it to
decide restrictions on the running of Large Hadron Collider (LHC for short) at
CERN, such as luminosity, and beam energy. There may potentially occur total
shut down. The purpose of such an experiment is to search for influence from
the future, that is, backward causation. Since LHC will produce particles of a
mathematically new type of fundamental scalars, i.e., the Higgs particles,
there is potentially a chance to find unseen effects, such as on influence
going from future to past, which we suggest in the present paper.
|
hep-ph hep-th physics.gen-ph
|
we propose an experiment which consists of drawing a card and using it to decide restrictions on the running of large hadron collider lhc for short at cern such as luminosity and beam energy there may potentially occur total shut down the purpose of such an experiment is to search for influence from the future that is backward causation since lhc will produce particles of a mathematically new type of fundamental scalars ie the higgs particles there is potentially a chance to find unseen effects such as on influence going from future to past which we suggest in the present paper
|
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|
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|
707.192
|
Magnetic Flux Effects in Statistical Magnetism of Electron Gas
|
The effects of magnetic flux in statistical magnetisms, including Pauli
paramagnetism, Landau diamagnetism, and De Hass-van Alphen oscillation, are
discussed. It is shown that the diamagnetism could be much increased by the
fractional magnetic flux, and the amplitude of the magnetic oscillation of De
Hass-van Alphen can be amplified by the quantum effect of the flux.
|
cond-mat.stat-mech cond-mat.mes-hall
|
the effects of magnetic flux in statistical magnetisms including pauli paramagnetism landau diamagnetism and de hassvan alphen oscillation are discussed it is shown that the diamagnetism could be much increased by the fractional magnetic flux and the amplitude of the magnetic oscillation of de hassvan alphen can be amplified by the quantum effect of the flux
|
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|
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|
707.1921
|
Symmetry-mode-based classical and quantum mechanical formalism of
lattice dynamics
|
We present classical and quantum mechanical descriptions of lattice dynamics,
from the atomic to the continuum scale, using atomic scale symmetry modes and
their constraint equations. This approach is demonstrated for a one-dimensional
chain and a two-dimensional square lattice with a monatomic basis. For the
classical description, we find that rigid modes, in addition to the
distortional modes found before, are necessary to describe the kinetic energy.
The long wavelength limit of the kinetic energy terms expressed in terms of
atomic scale modes is shown to be consistent with the continuum theory, and the
leading order corrections are obtained. For the quantum mechanical description,
we find conjugate momenta for the atomic scale symmetry modes. In direct space,
graphical rules for their commutation relations are obtained. Commutation
relations in the reciprocal space are also calculated. As an example, phonon
modes are analyzed in terms of symmetry modes. We emphasize that the approach
based on atomic scale symmetry modes could be useful, for example, for the
description of multiscale lattice dynamics and the dynamics near structural
phase transition.
|
cond-mat.mtrl-sci
|
we present classical and quantum mechanical descriptions of lattice dynamics from the atomic to the continuum scale using atomic scale symmetry modes and their constraint equations this approach is demonstrated for a onedimensional chain and a twodimensional square lattice with a monatomic basis for the classical description we find that rigid modes in addition to the distortional modes found before are necessary to describe the kinetic energy the long wavelength limit of the kinetic energy terms expressed in terms of atomic scale modes is shown to be consistent with the continuum theory and the leading order corrections are obtained for the quantum mechanical description we find conjugate momenta for the atomic scale symmetry modes in direct space graphical rules for their commutation relations are obtained commutation relations in the reciprocal space are also calculated as an example phonon modes are analyzed in terms of symmetry modes we emphasize that the approach based on atomic scale symmetry modes could be useful for example for the description of multiscale lattice dynamics and the dynamics near structural phase transition
|
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|
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|
707.1922
|
Reconfigurable Logic Gates Using Single-Electron Spin Transistors
|
We propose and numerically analyze novel reconfigurable logic gates using
"single-electron spin transistors" (SESTs), which are single-electron
transistors (SETs) with ferromagnetic electrodes and islands. The output
characteristics of a SEST depend on the relative magnetization configuration of
the ferromagnetic island with respect to the magnetization of the source and
the drain, i.e., high current drive capability in parallel magnetization and
low current drive capability in antiparallel magnetization. The summation of
multiple input signals can be achieved by directly coupling multiple input gate
electrodes to the SEST island, without using a floating gate. A Tucker-type
inverter with a variable threshold voltage, a reconfigurable AND/OR logic gate,
and a reconfigurable logic gate for all symmetric Boolean functions are
proposed and simulated using the Monte Carlo method.
|
cond-mat.mtrl-sci
|
we propose and numerically analyze novel reconfigurable logic gates using singleelectron spin transistors sests which are singleelectron transistors sets with ferromagnetic electrodes and islands the output characteristics of a sest depend on the relative magnetization configuration of the ferromagnetic island with respect to the magnetization of the source and the drain ie high current drive capability in parallel magnetization and low current drive capability in antiparallel magnetization the summation of multiple input signals can be achieved by directly coupling multiple input gate electrodes to the sest island without using a floating gate a tuckertype inverter with a variable threshold voltage a reconfigurable andor logic gate and a reconfigurable logic gate for all symmetric boolean functions are proposed and simulated using the monte carlo method
|
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|
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|
707.1923
|
Photon Antibunching in the Photoluminescence Spectra of a Single Carbon
Nanotube
|
We report the first observation of photon antibunching in the
photoluminescence from single carbon nanotubes. The emergence of a fast
luminescence decay component under strong optical excitation indicates that
Auger processes are partially responsible for inhibiting two-photon generation.
Additionally, the presence of exciton localization at low temperatures ensures
that nanotubes emit photons predominantly one by one. The fact that multiphoton
emission probability can be smaller than 5% suggests that carbon nanotubes
could be used as a source of single photons for applications in quantum
cryptography.
|
cond-mat.mes-hall
|
we report the first observation of photon antibunching in the photoluminescence from single carbon nanotubes the emergence of a fast luminescence decay component under strong optical excitation indicates that auger processes are partially responsible for inhibiting twophoton generation additionally the presence of exciton localization at low temperatures ensures that nanotubes emit photons predominantly one by one the fact that multiphoton emission probability can be smaller than 5 suggests that carbon nanotubes could be used as a source of single photons for applications in quantum cryptography
|
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|
[-0.09554934799671173, 0.25495511030449586, -0.03551421059459886, 0.05344235430855085, 0.03295383850276908, -0.18006700332660008, 0.05235624488936189, 0.4836020998437615, -0.22882445581695612, -0.26314009741729344, -0.0005883350584875135, -0.3048307381789474, -0.06942995425094577, 0.23798691537779043, 0.040637242941952804, -0.005258233371355078, 0.09384559422649225, -0.07826612289132112, 0.06621498999678914, -0.14738122067578574, 0.2623616940382978, 0.07271887434728663, 0.3384891223162413, 0.1431167350280756, 0.050840340642368094, 0.010953630978131996, 0.06752344797201017, -0.08275584658087395, 0.0025775345463497456, 0.09926451885908404, 0.24210212972453413, 0.010765565842773547, 0.22766383267281687, -0.43027573900625987, -0.23910328173763393, 0.09524570630096338, 0.21450569768271902, 0.1684796864331207, -0.10929470580235562, -0.26740383841097354, 0.05538865436306771, -0.12417310949634103, -0.09580551355748493, -0.0018825420561958761, -0.015867310992496855, -0.010540067640078418, -0.2219318776665365, 0.10172251213122817, 0.027151851831277943, 0.010414052792989155, -0.04010103680193424, -0.055934236469500534, -0.04503777693025768, 0.057647300150026295, 0.02047974155010546, -0.03463648314971258, 0.25093514329192285, -0.132065729566795, -0.18468354173990734, 0.3849756675772369, -0.14204542788433816, -0.033165045739973295, 0.16160397964584478, -0.19159651011338127, -0.14309818500461166, 0.29012797938331086, 0.08993630124365583, 0.14683829201933216, -0.1438922906294465, -0.04362430607263163, 0.012483171691351077, 0.22375144829754443, 0.1169800545746351, 0.19499525124316705, 0.2851557030342519, 0.14673236119834815, 0.0198816523722866, 0.16920481490464334, -0.14691240270348155, -0.0068496567580629796, -0.24870963422033718, -0.1793326062403674, -0.20484499058083577, 0.1504550945452031, -0.03505339759456761, -0.13043600808390798, 0.36932399704614105, 0.1087742666604326, 0.1527931443644989, -0.012248564905980055, 0.27845757637611207, 0.14794213973588793, 0.104729253869942, 0.008236016519367695, 0.3160670791478718, 0.15540977766572991, 0.08022512527292265, -0.2478779861018719, 0.10344828979714829, -0.05234419790863552]
|
707.1924
|
Hopping Conduction and Bacteria: Transport in Disordered
Reaction-Diffusion Systems
|
We report some basic results regarding transport in disordered
reaction-diffusion systems with birth (A->2A), death (A->0), and binary
competition (2A->A) processes. We consider a model in which the growth process
is only allowed to take place in certain areas--"oases"--while the rest of
space--the "desert"--is hostile to growth. In the limit of low oasis density,
transport is mediated through rare "hopping" events, necessitating the
inclusion of discreteness effects in the model. By first considering transport
between two oases, we are able to derive an approximate expression for the
average time taken for a population to traverse a disordered medium.
|
cond-mat.dis-nn
|
we report some basic results regarding transport in disordered reactiondiffusion systems with birth a2a death a0 and binary competition 2aa processes we consider a model in which the growth process is only allowed to take place in certain areasoaseswhile the rest of spacethe desertis hostile to growth in the limit of low oasis density transport is mediated through rare hopping events necessitating the inclusion of discreteness effects in the model by first considering transport between two oases we are able to derive an approximate expression for the average time taken for a population to traverse a disordered medium
|
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|
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|
707.1925
|
A note on minimal matching covered graphs
|
A graph is called matching covered if for its every edge there is a maximum
matching containing it. It is shown that minimal matching covered graphs
contain a perfect matching.
|
cs.DM
|
a graph is called matching covered if for its every edge there is a maximum matching containing it it is shown that minimal matching covered graphs contain a perfect matching
|
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|
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|
707.1926
|
On trees with a maximum proper partial 0-1 coloring containing a maximum
matching
|
I prove that in a tree in which the distance between any two endpoints is
even, there is a maximum proper partial 0-1 coloring such that the edges
colored by 0 form a maximum matching.
|
cs.DM
|
i prove that in a tree in which the distance between any two endpoints is even there is a maximum proper partial 01 coloring such that the edges colored by 0 form a maximum matching
|
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|
[-0.2070783524907061, 0.16995526371257647, -0.07235557490161487, 0.051184164526473196, -0.08288942077862364, -0.15184620566266988, 0.09550904086125749, 0.4039894403091499, -0.3117048601486853, -0.2722251074122531, 0.10047954759294433, -0.32515568573560033, -0.12888657229819467, 0.049876768248421806, -0.06819843949217881, -0.009463053569197655, 0.13793645018844733, 0.10302184990474156, -0.011555831633242114, -0.1734316877488579, 0.28042195143976384, -0.13641028244580541, 0.1564483527892402, 0.08846590095864874, 0.11587736710373844, 0.029561210982501508, 0.04445918868961079, 0.1156930184257882, -0.14316427126468625, 0.04719293000442641, 0.22840313805001122, 0.17425713507857707, 0.28045821764639445, -0.32678994185158183, -0.17808593224201882, 0.20715151567544257, 0.08895635340761926, 0.03913789480325899, -0.048243418475613, -0.14970921352505684, 0.2020022348367742, -0.09021253947700773, -0.05278289920783469, 0.1185348020600421, 0.13007815831473896, 0.008696782801832472, -0.3134012940206698, -0.006499202975205013, 0.11523614291633878, 0.026858381268435292, 0.06633597958300795, -0.1456588271340089, -0.061467974579760006, 0.09365482539204614, -0.05283999172970653, 0.1431952239945531, -0.030823544186672994, -0.17392751835286618, -0.14787582997232676, 0.3669499180146626, -0.09291979635932616, -0.21907658781856298, 0.13940493389964104, -0.1391050889688943, -0.13922798545765025, 0.11647457004125629, 0.06035651111160405, 0.1486521329198565, -0.16532769087435945, 0.08570515928523881, -0.10929160173982382, 0.1501679675919669, 0.18467882052063941, -0.005713769713682788, 0.18766608291438647, 0.071939656617386, 0.20997737739235162, 0.11505661835627896, -0.04139269909688405, -0.02661430487143142, -0.3520318339179669, -0.1720439447356122, -0.23002068450940508, 0.05881217244480338, -0.2198096586632476, -0.20749004008248448, 0.34842214666173926, 0.13771639711090497, 0.2891061939831291, 0.09202362759637513, 0.2744130049433027, 0.14042431130739194, 0.05267086076949324, 0.18891852144151927, 0.18108175471425056, 0.10158376218085842, -0.0721416676150901, -0.15371146665087768, 0.10605067110487393, 0.10624395406671933]
|
707.1927
|
Quantized dynamics of a coherent capacitor
|
A quantum coherent capacitor subject to large amplitude pulse cycles can be
made to emit or reabsorb an electron in each half cycle. Quantized currents
with pulse cycles in the GHz range have been demonstrated experimentally. We
develop a non-linear dynamical scattering theory for arbitrary pulses to
describe the properties of this very fast single electron source. Using our
theory we analyze the accuracy of the current quantization and investigate the
noise of such a source. Our results are important for future scientific and
possible metrological applications of this source.
|
cond-mat.mes-hall
|
a quantum coherent capacitor subject to large amplitude pulse cycles can be made to emit or reabsorb an electron in each half cycle quantized currents with pulse cycles in the ghz range have been demonstrated experimentally we develop a nonlinear dynamical scattering theory for arbitrary pulses to describe the properties of this very fast single electron source using our theory we analyze the accuracy of the current quantization and investigate the noise of such a source our results are important for future scientific and possible metrological applications of this source
|
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|
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|
707.1928
|
The Elements of an Analysis of the Functions of a Set
|
The variant of calculation of functions of set and their application is
offered. In particular: the new measure of system of sets generalizing
classical concept of a measure is entered; the variation of set that has
allowed to construct a derivative of function of set on a measure is entered,
and to receive necessary conditions of optimization in terms of function of
set.
|
math.FA
|
the variant of calculation of functions of set and their application is offered in particular the new measure of system of sets generalizing classical concept of a measure is entered the variation of set that has allowed to construct a derivative of function of set on a measure is entered and to receive necessary conditions of optimization in terms of function of set
|
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|
[-0.12233741343435314, 0.03495017440605258, -0.12442650205256152, 0.02222636547346141, -0.07381336736522379, -0.05223553128806608, 0.0938533010397343, 0.2911058441987113, -0.27349438488719957, -0.3082482225764247, 0.11174827921093397, -0.26976094637361786, -0.1312042510188702, 0.2217379274615456, -0.08150243158969614, 0.05102599239982073, 0.02654543651327018, 0.08595879490132488, -0.07140705666120445, -0.23327398483478834, 0.3711935363613838, 0.010082005419664912, 0.2276958922249457, 0.07033528006147771, 0.17978108934466802, 0.011423380746107017, -0.0644841128221107, 0.04486427855278764, -0.12034166482009737, 0.15348838552063893, 0.13688210486656144, 0.2331511193206386, 0.3190110914172634, -0.3454182199128563, -0.1650807234746892, 0.15071165419760205, 0.07673165349969788, 0.04111892044071167, -0.007171878496938873, -0.23208750408911516, 0.12846389788365553, -0.18440188956077372, -0.14699647042693365, -0.0866954819214279, 0.06621582747717934, 0.038393641718559794, -0.3126244812849022, -0.001948010405555131, 0.0013708875972836736, 0.04018677880484906, -0.0670526535028503, -0.08598316884193097, 0.0022655807745953402, 0.13657294527908403, 0.01056499253322799, 0.07254664931771537, 0.09225357300971472, -0.09801873171495067, -0.10316123497036714, 0.39012198692690286, -0.07593270421900328, -0.2226275848963904, 0.19206860599418482, -0.17962099444712437, -0.09931917500401301, 0.0906839932566303, 0.19959931236336984, 0.11661265506630852, -0.1589950207206938, 0.11598326650721627, -0.062077531738886756, 0.1211195918657477, 0.06663583174702667, 0.09951456891472585, 0.15705601511050074, 0.18584132157192226, 0.12463234843952316, 0.20733855179851018, -0.037826502632852345, -0.08359091350483516, -0.3394414165633775, -0.17653171134935247, -0.22134858079712896, 0.009968950501864865, -0.04195289331486463, -0.23713352826852646, 0.4423802244876112, 0.11099652592961248, 0.17552871585247062, 0.046824448017610446, 0.22585970825619167, 0.169453962684779, 0.05769511012338279, -0.013853110003447721, 0.18597343880757097, 0.14037483520362348, 0.03890411914252336, -0.1559997406965565, 0.08521309897436627, 0.09830763162158075]
|
707.1929
|
Quantum Monte Carlo diagonalization for many-fermion systems
|
In this study we present an optimization method based on the quantum Monte
Carlo diagonalization for many-fermion systems. Using the Hubbard-Stratonovich
transformation, employed to decompose the interactions in terms of auxiliary
fields, we expand the true ground-state wave function. The ground-state wave
function is written as a linear combination of the basis wave functions. The
Hamiltonian is diagonalized to obtain the lowest energy state, using the
variational principle within the selected subspace of the basis functions. This
method is free from the difficulty known as the negative sign problem. We can
optimize a wave function using two procedures. The first procedure is to
increase the number of basis functions. The second improves each basis function
through the operators, $e^{-\Delta\tau H}$, using the Hubbard-Stratonovich
decomposition. We present an algorithm for the Quantum Monte Carlo
diagonalization method using a genetic algorithm and the renormalization
method. We compute the ground-state energy and correlation functions of small
clusters to compare with available data.
|
cond-mat.str-el
|
in this study we present an optimization method based on the quantum monte carlo diagonalization for manyfermion systems using the hubbardstratonovich transformation employed to decompose the interactions in terms of auxiliary fields we expand the true groundstate wave function the groundstate wave function is written as a linear combination of the basis wave functions the hamiltonian is diagonalized to obtain the lowest energy state using the variational principle within the selected subspace of the basis functions this method is free from the difficulty known as the negative sign problem we can optimize a wave function using two procedures the first procedure is to increase the number of basis functions the second improves each basis function through the operators edeltatau h using the hubbardstratonovich decomposition we present an algorithm for the quantum monte carlo diagonalization method using a genetic algorithm and the renormalization method we compute the groundstate energy and correlation functions of small clusters to compare with available data
|
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|
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|
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