id stringlengths 9 10 | abstract stringlengths 13 3.93k | embedding list |
|---|---|---|
1001.0001 | The Krotov combining construction of perfect 1-error-correcting binary codes from 2000 and a theorem of Heden saying that every non-full-rank perfect 1-error-correcting binary code can be constructed by this combining construction is generalized to the $q$-ary case. Simply, every non-full-rank perfect code $C$ is the union of a well-defined family of $\mu$-components $K_\mu$, where $\mu$ belongs to an "outer" perfect code $C^*$, and these components are at distance three from each other. Components from distinct codes can thus freely be combined to obtain new perfect codes. The Phelps general product construction of perfect binary code from 1984 is generalized to obtain $\mu$-components, and new lower bounds on the number of perfect 1-error-correcting $q$-ary codes are presented. | [
-0.015585657209157002,
0.016744695603847,
-0.014822055585682002,
-0.021612657234072002,
-0.025117043405771002,
0.007990547455847001,
-0.0015007843030610001,
-0.033080320805311,
-0.025062501430511003,
-0.027816921472549,
-0.0014505024300880002,
0.039052776992321,
-0.016867417842149002,
0.00... |
1001.0002 | Logarithmic conformal field theories with vanishing central charge describe systems with quenched disorder, percolation or dilute self-avoiding polymers. In these theories the energy momentum tensor acquires a logarithmic partner. In this talk we address the construction of possible gravity duals for these logarithmic conformal field theories and present two viable candidates for such duals, namely theories of massive gravity in three dimensions at a chiral point. | [
0.004695892333984,
0.01996518112719,
0.0027995395939790003,
-0.007442802656441001,
0.0007342636818060001,
0.030124336481094003,
-0.020399797707796003,
-0.030395971611142002,
-0.010919732041656001,
-0.014288007281720002,
0.027733946219086,
0.029798373579978003,
-0.009059031493961001,
0.0201... |
1001.0003 | We construct new families of non-supersymmetric sourceless type IIA AdS4 vacua on those coset manifolds that also admit supersymmetric solutions. We investigate the spectrum of left-invariant modes and find that most, but not all, of the vacua are stable under these fluctuations. Generically, there are also no massless moduli. | [
-0.0005790717550550001,
0.004832370672374,
-0.009515740908682001,
-0.008235687389969,
-0.027199441567063002,
0.023162869736552003,
-0.028228901326656,
-0.012360303662717,
0.0037588868290180004,
-0.017351834103465,
0.021754134446382002,
0.013775812461972,
-0.010924476198852002,
0.0290687251... |
1001.0004 | Examples of symmetric informationally complete positive operator valued measures (SIC-POVMs) have been constructed in every dimension less than or equal to 67. However, it remains an open question whether they exist in all finite dimensions. A SIC-POVM is usually thought of as a highly symmetric structure in quantum state space. However, its elements can equally well be regarded as a basis for the Lie algebra gl(d,C). In this paper we examine the resulting structure constants, which are calculated from the traces of the triple products of the SIC-POVM elements and which, it turns out, characterize the SIC-POVM up to unitary equivalence. We show that the structure constants have numerous remarkable properties. In particular we show that the existence of a SIC-POVM in dimension d is equivalent to the existence of a certain structure in the adjoint representation of gl(d,C). We hope that transforming the problem in this way, from a question about quantum state space to a question about Lie algebras, may help to make the existence problem tractable. | [
0.023628670722246004,
0.00021616531012100002,
0.022768700495362,
-0.037319920957088006,
-0.033497836440801,
0.030003359541296,
-0.024311184883117003,
-0.024201981723308,
-0.015056281350553001,
-0.029457347467541,
0.026891091838479,
0.017390482127666,
-0.011534503661096,
0.02154017426073500... |
1001.0005 | We aim to reveal environmental dependence of infrared luminosity functions (IR LFs) of galaxies at z~0.8 using the AKARI satellite. We construct restframe 8um IR LFs in the cluster region RXJ1716.4+6708 at z=0.81, and compare them with a blank field using the AKARI North Ecliptic Pole deep field data at the same redshift. AKARI's wide field of view (10'x10') is suitable to investigate wide range of galaxy environments. AKARI's 15um filter is advantageous here since it directly probes restframe 8um at z~0.8, without relying on a large extrapolation based on a SED fit, which was the largest uncertainty in previous work. We have found that cluster IR LFs at restframe 8um have a factor of 2.4 smaller L^* and a steeper faint-end slope than that of the field. Confirming this trend, we also found that faint-end slopes of the cluster LFs becomes flatter and flatter with decreasing local galaxy density. These changes in LFs cannot be explained by a simple infall of field galaxy population into a cluster. Physics that can preferentially suppress IR luminous galaxies in high density regions is required to explain the observed results. | [
0.021031482145190003,
0.007450645789504001,
-0.011589893139898002,
-0.006280709523707,
-0.011152022518217002,
0.027407977730035,
-0.035467535257339006,
-0.002709325635805,
-0.01588650047779,
-0.027572179213166,
0.0015334030613300001,
0.007861149497330001,
0.01052258349955,
0.00342086586169... |
1001.0006 | We present the first comparison of virial masses of galaxy clusters with their Sunyaev-Zel'dovich Effect (SZE) signals. We study 15 clusters from the Hectospec Cluster Survey (HeCS) with MMT/Hectospec spectroscopy and published SZE signals. We measure virial masses of these clusters from an average of 90 member redshifts inside the radius $r_{100}$. The virial masses of the clusters are strongly correlated with their SZE signals (at the 99% confidence level using a Spearman rank-sum test). This correlation suggests that $Y_{SZ}$ can be used as a measure of virial mass. Simulations predict a powerlaw scaling of $Y_{SZ}\propto M_{200}^\alpha$ with $\alpha\approx$1.6. Observationally, we find $\alpha$=1.11$\pm$0.16, significantly shallower (given the formal uncertainty) than the theoretical prediction. However, the selection function of our sample is unknown and a bias against less massive clusters cannot be excluded (such a selection bias could artificially flatten the slope). Moreover, our sample indicates that the relation between velocity dispersion (or virial mass estimate) and SZE signal has significant intrinsic scatter, comparable to the range of our current sample. More detailed studies of scaling relations are therefore needed to derive a robust determination of the relation between cluster mass and SZE. | [
-0.009176731109619,
-0.007445912342518001,
0.0035939933732150003,
-0.025887612253427002,
-0.017552534118294,
0.040154986083507004,
-0.023118302226066003,
0.010194859467446001,
-0.028263244777917,
-0.049304563552141,
-0.0037263499107210002,
0.042326990514993,
0.0016985775437200002,
0.018027... |
1001.0007 | We reveal cosmic star-formation history obscured by dust using deep infrared observation with the AKARI. A continuous filter coverage in the mid-IR wavelength (2.4, 3.2, 4.1, 7, 9, 11, 15, 18, and 24um) by the AKARI satellite allows us to estimate restframe 8um and 12um luminosities without using a large extrapolation based on a SED fit, which was the largest uncertainty in previous work. We found that restframe 8um (0.38<z<2.2), 12um (0.15<z<1.16), and total infrared (TIR) luminosity functions (LFs) (0.2<z<1.6) constructed from the AKARI NEP deep data, show a continuous and strong evolution toward higher redshift. In terms of cosmic infrared luminosity density (Omega_IR), which was obtained by integrating analytic fits to the LFs, we found a good agreement with previous work at z<1.2, with Omega_IR propto (1+z)^4.4+-1.0. When we separate contributions to Omega_IR by LIRGs and ULIRGs, we found more IR luminous sources are increasingly more important at higher redshift. We found that the ULIRG (LIRG) contribution increases by a factor of 10 (1.8) from z=0.35 to z=1.4. | [
0.019308622926473,
-0.0065242024138560005,
-0.018979499116539,
-0.018019553273916,
-0.002357009565457,
0.008872641250491,
-0.028716091066598,
-0.0036717923358080004,
-0.019966870546340002,
-0.018787508830428002,
0.015386559069156001,
0.012273591943085001,
0.007796130608767,
-0.003208961337... |
1001.0008 | In this Letter, we briefly review the multi-stream inflation scenario, and discuss its implications in the string theory landscape and the inflationary multiverse. In multi-stream inflation, the inflation trajectory encounters bifurcations. If these bifurcations are in the observable stage of inflation, then interesting observational effects can take place, such as domain fences, non-Gaussianities, features and asymmetries in the CMB. On the other hand, if the bifurcation takes place in the eternal stage of inflation, it provides an alternative creation mechanism of bubbles universes in eternal inflation, as well as a mechanism to locally terminate eternal inflation, which reduces the measure of eternal inflation. | [
-0.020563460886478,
-0.0077112978324290005,
-0.003916688263416001,
-0.013286219909787001,
-0.002027861075475,
0.007351844105869001,
-0.034236263483762006,
0.018501689657568002,
-0.031631920486688,
-0.0017870949814090002,
0.012404541485011002,
0.007256893906742,
-0.008355601690709001,
0.028... |
1001.0009 | Theoretical studies of stretching proteins with slipknots reveal a surprising growth of their unfolding times when the stretching force crosses an intermediate threshold. This behavior arises as a consequence of the existence of alternative unfolding routes that are dominant at different force ranges. Responsible for longer unfolding times at higher forces is the existence of an intermediate, metastable configuration where the slipknot is jammed. Simulations are performed with a coarsed grained model with further quantification using a refined description of the geometry of the slipknots. The simulation data is used to determine the free energy landscape (FEL) of the protein, which supports recent analytical predictions. | [
-0.018460078164935,
-0.012798245996236001,
0.010370752774178002,
-0.026737205684185004,
-0.013959825970232001,
0.020032037049531,
-0.018627012148499003,
0.0013728552730750002,
-0.037866115570068005,
-0.010516819544136,
0.00862490478903,
0.0019075645832340002,
0.014982294291257001,
0.021687... |
1001.0011 | Spatial separation of electrons and holes in graphene gives rise to existence of plasmon waves confined to the boundary region. Theory of such guided plasmon modes within hydrodynamics of electron-hole liquid is developed. For plasmon wavelengths smaller than the size of charged domains plasmon dispersion is found to be \omega ~ q^(1/4). Frequency, velocity and direction of propagation of guided plasmon modes can be easily controlled by external electric field. In the presence of magnetic field spectrum of additional gapless magnetoplasmon excitations is obtained. Our findings indicate that graphene is a promising material for nanoplasmonics. | [
-0.008414856158196002,
0.022923229262232003,
0.011329719796776001,
-0.001989955315366,
-0.0028159432113170004,
0.011870486661791002,
-0.024967590346932002,
-0.017594698816537,
-0.035769734531641,
-0.013440028764307001,
-0.0033088983036570004,
0.00039320986252200005,
-0.018188223242759,
0.0... |
1001.0012 | [Abridged] If both the day-side and night-side effective temperatures of a planet can be measured, it is possible to estimate its Bond albedo, 0<A_B<1, as well as its day-night heat redistribution efficiency, 0<epsilon<1. We attempt a statistical analysis of the albedo and redistribution efficiency for 24 transiting exoplanets that have at least one published secondary eclipse. For each planet, we show how to calculate a sub-stellar equilibrium temperature, T_0, and associated uncertainty. We then use a simple model-independent technique to estimate a planet's effective temperature from planet/star flux ratios. We use thermal secondary eclipse measurements -those obtained at lambda>0.8 micron- to estimate day-side effective temperatures, T_d, and thermal phase variations -when available- to estimate night-side effective temperature. We strongly rule out the "null hypothesis" of a single A_B and epsilon for all 24 planets. If we allow each planet to have different parameters, we find that low Bond albedos are favored (A_B<0.35 at 1 sigma confidence), which is an independent confirmation of the low albedos inferred from non-detection of reflected light. Our sample exhibits a wide variety of redistribution efficiencies. When normalized by T_0, the day-side effective temperatures of the 24 planets describe a uni-modal distribution. The dimensionless quantity T_d/T_0 exhibits no trend with the presence or absence of stratospheric inversions. There is also no clear trend between T_d/T_0 and T_0. That said, the 6 planets with the greatest sub-stellar equilibrium temperatures (T>2400 K) have low epsilon, as opposed to the 18 cooler planets, which show a variety of recirculation efficiencies. This hints that the very hottest transiting giant planets are qualitatively different from the merely hot Jupiters. | [
0.014126621186733001,
0.00617782305926,
-0.010021801106631001,
-0.036407969892024,
-0.004290154669433,
0.028170872479677003,
-0.024217065423727,
0.0011660640593610001,
-0.029900662600994003,
-0.023324713110923,
-0.005048654042184001,
0.015883868560194,
-0.007447708863765,
0.017325360327959... |
1001.0013 | Dust-obscured star-formation becomes much more important with increasing intensity, and increasing redshift. We aim to reveal cosmic star-formation history obscured by dust using deep infrared observation with the AKARI. We construct restframe 8um, 12um, and total infrared (TIR) luminosity functions (LFs) at 0.15<z<2.2 using 4128 infrared sources in the AKARI NEP-Deep field. A continuous filter coverage in the mid-IR wavelength (2.4, 3.2, 4.1, 7, 9, 11, 15, 18, and 24um) by the AKARI satellite allows us to estimate restframe 8um and 12um luminosities without using a large extrapolation based on a SED fit, which was the largest uncertainty in previous work. We have found that all 8um (0.38<z<2.2), 12um (0.15<z<1.16), and TIR LFs (0.2<z<1.6), show a continuous and strong evolution toward higher redshift. In terms of cosmic infrared luminosity density (Omega_IR), which was obtained by integrating analytic fits to the LFs, we found a good agreement with previous work at z<1.2, and that the Omega_IR evolves as propto (1+z)^4.4+-1.0. When we separate contributions to Omega_IR by LIRGs and ULIRGs, we found more IR luminous sources are increasingly more important at higher redshift. We found that the ULIRG (LIRG) contribution increases by a factor of 10 (1.8) from z=0.35 to z=1.4. | [
0.010245432145893001,
-0.004603960085660001,
-0.018593309447169002,
-0.016368119046092002,
0.001377092557959,
0.010347818024456001,
-0.031780634075403005,
-0.004952072631567,
-0.024736473336815,
-0.022784311324357,
0.014074671082198,
0.008914412930607001,
0.009235222823917,
0.0035937507636... |
1001.0014 | Jet shapes are weighted sums over the four-momenta of the constituents of a jet and reveal details of its internal structure, potentially allowing discrimination of its partonic origin. In this work we make predictions for quark and gluon jet shape distributions in N-jet final states in e+e- collisions, defined with a cone or recombination algorithm, where we measure some jet shape observable on a subset of these jets. Using the framework of Soft-Collinear Effective Theory, we prove a factorization theorem for jet shape distributions and demonstrate the consistent renormalization-group running of the functions in the factorization theorem for any number of measured and unmeasured jets, any number of quark and gluon jets, and any angular size R of the jets, as long as R is much smaller than the angular separation between jets. We calculate the jet and soft functions for angularity jet shapes \tau_a to one-loop order (O(alpha_s)) and resum a subset of the large logarithms of \tau_a needed for next-to-leading logarithmic (NLL) accuracy for both cone and kT-type jets. We compare our predictions for the resummed \tau_a distribution of a quark or a gluon jet produced in a 3-jet final state in e+e- annihilation to the output of a Monte Carlo event generator and find that the dependence on a and R is very similar. | [
-0.017578911036252,
-0.00402620434761,
-0.0035853539593510004,
-0.027291396632790003,
-0.000715520931407,
-0.005879153963178001,
-0.021904755383729,
-0.0015093961264930002,
-0.035020057111978004,
-0.017964655533432003,
0.022070074453949002,
0.008596583269536,
-0.026271929964423003,
0.01324... |
1001.0015 | We conduct a comprehensive analysis of the relationship between central galaxies and their host dark matter halos, as characterized by the stellar mass-halo mass (SM-HM) relation, with rigorous consideration of uncertainties. Our analysis focuses on results from the abundance matching technique, which assumes that every dark matter halo or subhalo above a specific mass threshold hosts one galaxy. We discuss the quantitative effects of uncertainties in observed galaxy stellar mass functions (GSMFs) (including stellar mass estimates and counting uncertainties), halo mass functions (including cosmology and uncertainties from substructure), and the abundance matching technique used to link galaxies to halos (including scatter in this connection). Our analysis results in a robust estimate of the SM-HM relation and its evolution from z=0 to z=4. The shape and evolution are well constrained for z < 1. The largest uncertainties at these redshifts are due to stellar mass estimates; however, failure to account for scatter in stellar masses at fixed halo mass can lead to errors of similar magnitude in the SM-HM relation for central galaxies in massive halos. We also investigate the SM-HM relation to z=4, although the shape of the relation at higher redshifts remains fairly unconstrained when uncertainties are taken into account. These results will provide a powerful tool to inform galaxy evolution models. [Abridged] | [
-0.0025821144226930003,
0.00250843539834,
0.000308740185573,
-0.032499141991138,
-0.019745975732803,
0.014508066698908001,
-0.027194252237677,
0.0031112637370820004,
-0.0203488022089,
-0.030061036348342004,
0.010750437155365,
0.006992808077484001,
-0.006523941643536001,
0.01604862883687000... |
1001.0016 | Using localization, matrix model and saddle-point techniques, we determine exact behavior of circular Wilson loop in N=2 superconformal (quiver) gauge theories. Focusing at planar and large `t Hooft couling limits, we compare its asymptotic behavior with well-known exponential growth of Wilson loop in N=4 super Yang-Mills theory. For theory with gauge group SU(N) coupled to 2N fundamental hypermultiplets, we find that Wilson loop exhibits non-exponential growth -- at most, it can grow a power of `t Hooft coupling. For theory with gauge group SU(N) x SU(N) and bifundamental hypermultiplets, there are two Wilson loops associated with two gauge groups. We find Wilson loop in untwisted sector grows exponentially large as in N=4 super Yang-Mills theory. We then find Wilson loop in twisted sector exhibits non-analytic behavior with respect to difference of two `t Hooft coupling constants. By letting one gauge coupling constant hierarchically larger/smaller than the other, we show that Wilson loops in the second type theory interpolate to Wilson loop in the first type theory. We infer implications of these findings from holographic dual description in terms of minimal surface of dual string worldsheet. We suggest intuitive interpretation that in both type theories holographic dual background must involve string scale geometry even at planar and large `t Hooft coupling limit and that new results found in the gauge theory side are attributable to worldsheet instantons and infinite resummation therein. Our interpretation also indicate that holographic dual of these gauge theories is provided by certain non-critical string theories. | [
-0.010191120207309001,
0.002086275722831,
0.005475825630128,
-0.0007125660195010001,
-0.016330681741237002,
-0.012859893962740001,
-0.012272210791707,
-0.0046530691906800006,
-0.006626993883401,
-0.023853028193116,
-0.004780976567417001,
-0.0006671934388570001,
-0.017658155411481,
0.032937... |
1001.0017 | We give a test that can distinguish efficiently between product states of n quantum systems and states which are far from product. If applied to a state psi whose maximum overlap with a product state is 1-epsilon, the test passes with probability 1-Theta(epsilon), regardless of n or the local dimensions of the individual systems. The test uses two copies of psi. We prove correctness of this test as a special case of a more general result regarding stability of maximum output purity of the depolarising channel. A key application of the test is to quantum Merlin-Arthur games with multiple Merlins, where we obtain several structural results that had been previously conjectured, including the fact that efficient soundness amplification is possible and that two Merlins can simulate many Merlins: QMA(k)=QMA(2) for k>=2. Building on a previous result of Aaronson et al, this implies that there is an efficient quantum algorithm to verify 3-SAT with constant soundness, given two unentangled proofs of O(sqrt(n) polylog(n)) qubits. We also show how QMA(2) with log-sized proofs is equivalent to a large number of problems, some related to quantum information (such as testing separability of mixed states) as well as problems without any apparent connection to quantum mechanics (such as computing injective tensor norms of 3-index tensors). As a consequence, we obtain many hardness-of-approximation results, as well as potential algorithmic applications of methods for approximating QMA(2) acceptance probabilities. Finally, our test can also be used to construct an efficient test for determining whether a unitary operator is a tensor product, which is a generalisation of classical linearity testing. | [
0.014474469237029,
0.009861957281827,
-0.010344905778765,
-0.030096817761659,
-0.011898742057383001,
0.008476103655993,
-0.019961889833211,
-0.010225918143987002,
-0.036760114133358,
-0.025561297312378002,
0.010575881227850002,
0.014320485293865001,
0.0007401717011810001,
0.008042149245738... |
1001.0018 | We study the power of nonadaptive quantum query algorithms, which are algorithms whose queries to the input do not depend on the result of previous queries. First, we show that any bounded-error nonadaptive quantum query algorithm that computes some total boolean function depending on n variables must make Omega(n) queries to the input in total. Second, we show that, if there exists a quantum algorithm that uses k nonadaptive oracle queries to learn which one of a set of m boolean functions it has been given, there exists a nonadaptive classical algorithm using O(k log m) queries to solve the same problem. Thus, in the nonadaptive setting, quantum algorithms can achieve at most a very limited speed-up over classical query algorithms. | [
0.000378588534658,
0.0035135748330500003,
0.00975196249783,
-0.015365486964583001,
-0.017427876591682,
0.025390613824129,
-0.030812924727797,
-0.009021248668432002,
-0.043460428714752,
-0.006760814227163001,
0.024816969409585003,
0.013050420209765,
0.012811401858925,
0.001040584989823,
-... |
1001.0019 | Recent numerical investigations have uncovered a surprising result: Reissner-Nordstrom-de Sitter black holes are unstable for spacetime dimensions larger than 6. Here we prove the existence of such instability analytically, and we compute the timescale in the near-extremal limit. We find very good agreement with the previous numerical results. Our results may me helpful in shedding some light on the nature of the instability. | [
-0.000318771431921,
-0.008071484044194001,
0.019830800592899,
-0.029447000473737002,
-0.008704678155481,
-0.004547168035060001,
-0.029252171516418003,
-0.010819963179528,
-0.013978974893689001,
-0.004453232511878001,
0.016003804281353,
0.007549620699137001,
0.0049368259496980005,
0.0172701... |
1001.0021 | To analyze the ground-state phase diagram of Bose-Bose mixtures loaded into $d$-dimensional hypercubic optical lattices, we perform a strong-coupling power-series expansion in the kinetic energy term (plus a scaling analysis) for the two-species Bose-Hubbard model with onsite boson-boson interactions. We consider both repulsive and attractive interspecies interaction, and obtain an analytical expression for the phase boundary between the incompressible Mott insulator and the compressible superfluid phase up to third order in the hoppings. In particular, we find a re-entrant quantum phase transition from paired superfluid (superfluidity of composite bosons, i.e. Bose-Bose pairs) to Mott insulator and again to a paired superfluid in all one, two and three dimensions, when the interspecies interaction is sufficiently large and attractive. We hope that some of our results could be tested with ultracold atomic systems. | [
-0.014143070206046,
0.000871253781951,
0.00458127213642,
-0.024862028658390004,
0.004906089045107,
0.017837863415479,
-0.0019793531391760003,
-0.019759695976972,
-0.024090589955449,
-0.04336306080222101,
0.007829441688954001,
0.026594387367367002,
-0.0016790666850280001,
0.0010032106656580... |
1001.0022 | Motivated by large nu_mu-nu_tau flavor mixing, we consider mu-tau production at hadron colliders via dimension-6 effective operators, which can be attributed to new physics in the flavor sector at a higher scale Lambda. Current bounds on many of these operators from low energy experiments are very weak or nonexistent, and they may lead to clean mu+tau- and mu-tau+ signals at hadron colliders. At the Tevatron with 8 inverse femtobarns, one can exceed current bounds for most operators, with most 2 sigma sensitivities being in the 6-24 TeV range. We find that at the LHC with 1 (100) inverse femtobarns integrated luminosity, one can reach a 2 sigma sensitivity for Lambda \sim 3-10 TeV (Lambda =\sim 6-21 TeV), depending on the Lorentz structure of the operator. For some operators, an improvement of several orders of magnitude in sensitivity can be obtained with only a few tens of inverse picobarns at the LHC. | [
-0.011542682535946001,
-0.016122229397296,
-0.020722625777125,
-0.028825435787439003,
-0.011931840330362,
-0.002281086985021,
-0.04694904759526201,
-0.008478069677948001,
-0.05959665775299001,
-0.02305756881833,
0.014996454119682001,
0.028964420780539003,
-0.019596848636865002,
-0.01346067... |
1001.0023 | If $X$ is a smooth manifold then the $\mathbb R$-algebra $C^\infty(X)$ of smooth functions $c:X\to\mathbb R$ is a $C^\infty$-$ring$. That is, for each smooth function $f:{\mathbb R}^n\to\mathbb R$ there is an $n$-fold operation $\Phi_f:C^\infty(X)^n\to C^\infty(X)$ acting by $\Phi_f:(c_1,\ldots,c_n)\mapsto f(c_1,...,c_n)$, and these operations $\Phi_f$ satisfy many natural identities. Thus, $C^\infty(X)$ actually has a far richer structure than the obvious $\mathbb R$-algebra structure. We develop a version of algebraic geometry in which rings or algebras are replaced by $C^\infty$-rings. As schemes are the basic objects in algebraic geometry, the new basic objects are $C^\infty$-$schemes$, a category of geometric objects which generalize smooth manifolds, and whose morphisms generalize smooth maps. We also study quasicoherent and coherent sheaves on $C^\infty$-schemes, and $C^\infty$-$stacks$, in particular Deligne-Mumford $C^\infty$-stacks, a 2-category of geometric objects generalizing orbifolds. This enables us to use the tools of algebraic geometry in differential geometry, and to describe singular spaces such as moduli spaces occurring in differential geometric problems. This paper forms the foundations of the author's new theory of "derived differential geometry", surveyed in arXiv:1206.4207 and in more detail in arXiv:1208.4948, which studies d-manifolds and d-orbifolds, "derived" versions of smooth manifolds and smooth orbifolds. Derived differential geometry has applications to areas of symplectic geometry involving moduli spaces of $J$-holomorphic curves. Many of these ideas are not new: $C^\infty$-rings and $C^\infty$-schemes have long been part of synthetic differential geometry. But we develop them in new directions. This paper is surveyed in arXiv:1104.4951. | [
0.011757467873394,
0.012728142552077002,
-0.002271173754706,
-0.033604484051465,
-0.018278760835528002,
0.014136304147541,
-0.012598264031112002,
-0.004227903671562,
-0.005796705372631001,
-0.033713854849338004,
0.026303917169570003,
0.0029137330129740003,
0.005885569844394,
0.013322851620... |
1001.0024 | The hybrid Monte Carlo (HMC) algorithm is applied for the Bayesian inference of the stochastic volatility (SV) model. We use the HMC algorithm for the Markov chain Monte Carlo updates of volatility variables of the SV model. First we compute parameters of the SV model by using the artificial financial data and compare the results from the HMC algorithm with those from the Metropolis algorithm. We find that the HMC algorithm decorrelates the volatility variables faster than the Metropolis algorithm. Second we make an empirical study for the time series of the Nikkei 225 stock index by the HMC algorithm. We find the similar correlation behavior for the sampled data to the results from the artificial financial data and obtain a $\phi$ value close to one ($\phi \approx 0.977$), which means that the time series has the strong persistency of the volatility shock. | [
-0.011047637090086,
-0.008642990142107001,
-0.010353724472224001,
-0.02219146117568,
-0.004902045708149,
0.013019448146224001,
-0.013555341400206,
-0.00041608986794000006,
-0.03382995352149,
-0.030037481337785003,
-0.006399797275662001,
0.039463698863983,
0.017890576273202,
0.0105048744007... |
1001.0025 | Increasing numbers of mobile computing devices, user-portable, or embedded in vehicles, cargo containers, or the physical space, need to be aware of their location in order to provide a wide range of commercial services. Most often, mobile devices obtain their own location with the help of Global Navigation Satellite Systems (GNSS), integrating, for example, a Global Positioning System (GPS) receiver. Nonetheless, an adversary can compromise location-aware applications by attacking the GNSS-based positioning: It can forge navigation messages and mislead the receiver into calculating a fake location. In this paper, we analyze this vulnerability and propose and evaluate the effectiveness of countermeasures. First, we consider replay attacks, which can be effective even in the presence of future cryptographic GNSS protection mechanisms. Then, we propose and analyze methods that allow GNSS receivers to detect the reception of signals generated by an adversary, and then reject fake locations calculated because of the attack. We consider three diverse defense mechanisms, all based on knowledge, in particular, own location, time, and Doppler shift, receivers can obtain prior to the onset of an attack. We find that inertial mechanisms that estimate location can be defeated relatively easy. This is equally true for the mechanism that relies on clock readings from off-the-shelf devices; as a result, highly stable clocks could be needed. On the other hand, our Doppler Shift Test can be effective without any specialized hardware, and it can be applied to existing devices. | [
-0.021956726908683003,
0.018349647521972,
0.0022988296113900003,
0.006322635803371001,
-0.011169647797942,
0.00252427207306,
-0.04129012301564201,
-0.007193663157522001,
-0.01963398605585,
-0.004218506161123001,
0.031698573380708,
0.01986626163125,
-0.015466718003153001,
0.012064586393535,... |
1001.0026 | Asteroseismology of stars in clusters has been a long-sought goal because the assumption of a common age, distance and initial chemical composition allows strong tests of the theory of stellar evolution. We report results from the first 34 days of science data from the Kepler Mission for the open cluster NGC 6819 -- one of four clusters in the field of view. We obtain the first clear detections of solar-like oscillations in the cluster red giants and are able to measure the large frequency separation and the frequency of maximum oscillation power. We find that the asteroseismic parameters allow us to test cluster-membership of the stars, and even with the limited seismic data in hand, we can already identify four possible non-members despite their having a better than 80% membership probability from radial velocity measurements. We are also able to determine the oscillation amplitudes for stars that span about two orders of magnitude in luminosity and find good agreement with the prediction that oscillation amplitudes scale as the luminosity to the power of 0.7. These early results demonstrate the unique potential of asteroseismology of the stellar clusters observed by Kepler. | [
0.009014149196445,
-0.008069227449595,
-0.006441106088459001,
-0.032168142497539,
-0.00039725820533900003,
0.030971692875027,
-0.012596696615219002,
0.008096419274806001,
-0.015757767483592002,
-0.01001345552504,
-0.010917589999735001,
0.019836567342281,
0.00864705722779,
0.008667451329529... |
1001.0027 | We present the results of the search for candidate Planetary Nebulae interacting with the interstellar medium (PN-ISM) in the framework of the INT Photometric H$\alpha$ Survey (IPHAS) and located in the right ascension range 18h-20h. The detection capability of this new Northern survey, in terms of depth and imaging resolution, has allowed us to overcome the detection problem generally associated to the low surface brightness inherent to PNe-ISM. We discuss the detection of 21 IPHAS PN-ISM candidates. Thus, different stages of interaction were observed, implying various morphologies i.e. from the unaffected to totally disrupted shapes. The majority of the sources belong to the so-called WZO2 stage which main characteristic is a brightening of the nebula's shell in the direction of motion. The new findings are encouraging as they would be a first step into the reduction of the scarcity of observational data and they would provide new insights into the physical processes occurring in the rather evolved PNe. | [
-0.004007388371974,
-0.0034598375204950003,
0.0018274512840430002,
-0.015304049476981002,
-0.030142679810523,
0.036959689110517,
-0.018958952277898,
0.002896886784583,
-0.022586476057767,
-0.002660755300894,
0.016768747940659003,
0.004202453419566,
0.011799722909927,
0.013688773848116,
-... |
1001.0028 | We present the proof of the cyclic sieving conjectures for generalised non-crossing partitions associated to well-generated complex reflection groups due to Armstrong, respectively to Bessis and Reiner, for the 26 exceptional well-generated complex reflection groups. The computational details are provided in the manuscript "Cyclic sieving for generalised non-crossing partitions associated to complex reflection groups of exceptional type - the details" [arXiv:1001.0030]. | [
-0.010629982687532001,
0.020059693604707003,
-0.0032041706144800004,
0.000237984684645,
0.008381200022995,
0.037774033844470006,
-0.019066367298364,
0.00042962271254500005,
-0.014596394263207002,
-0.013954870402812002,
0.024336520582437002,
0.013823806308209001,
-0.007891434244811,
0.00850... |
1001.0029 | In 1979 Louis Witten demonstrated that stationary axially symmetric Einstein field equations and those for static axially symmetric self-dual SU(2) gauge fields can both be reduced to the same (Ernst) equation. In this paper we use this result as point of departure to prove the existence of the mass gap for quantum source-free Yang-Mills (Y-M) fields. The proof is facilitated by results of our recently published paper, JGP 59 (2009) 600-619. Since both pure gravity, the Einstein-Maxwell and pure Y-M fields are described for axially symmetric configurations by the Ernst equation classically, their quantum descriptions are likely to be interrelated. Correctness of this conjecture is successfully checked by reproducing (by different methods) results of Korotkin and Nicolai, Nucl.Phys.B475 (1996) 397-439, on dimensionally reduced quantum gravity. Consequently, numerous new results supporting the Faddeev-Skyrme (F-S) -type models are obtained. We found that the F-S-like model is best suited for description of electroweak interactions while strong interactions require extension of Witten's results to the SU(3) gauge group. Such an extension is nontrivial. It is linked with the symmetry group SU(3)xSU(2)xU(1) of the Standard Model. This result is quite rigid and should be taken into account in development of all grand unified theories. Also, the alternative (to the F-S-like) model emerges as by-product of such an extension. Both models are related to each other via known symmetry transformation. Both models possess gap in their excitation spectrum and are capable of producing knotted/linked configurations of gauge/gravity fields. In addition, the paper discusses relevance of the obtained results to heterotic strings and to scattering processes involving topology change. It ends with discussion about usefulness of this information for searches of Higgs boson. | [
-0.005776507314294001,
0.015476679429411002,
-0.006427045445889,
0.004690005909651,
-0.010994437150657,
-0.002840570174157,
-0.02713868394494,
-0.011382716707885002,
-0.009393636137247,
-0.038882430642843004,
0.008187926374375001,
0.014495762996375,
0.0015420480631290001,
0.030817121267318... |
1001.0031 | Exact analytic expressions for planetary orbits and light trajectories in the Schwarzschild geometry are presented. A new parameter space is used to characterize all possible planetary orbits. Different regions in this parameter space can be associated with different characteristics of the orbits. The boundaries for these regions are clearly defined. Observational data can be directly associated with points in the regions. A possible extension of these considerations with an additional parameter for the case of Kerr geometry is briefly discussed. | [
0.015033024363219,
0.0069165392778810005,
0.0027521220035850004,
-0.025926910340785002,
-0.008581631816923,
0.027639193460345,
-0.014507205225527,
-0.028798690065741,
-0.025401093065738,
-0.008750163950026,
0.012511790730059001,
0.009134416468441,
-0.007840093225240001,
0.005386271979659,
... |
1001.0032 | In addition to its great potential for characterizing extra-solar planetary systems the Kepler mission is providing unique data on stellar oscillations. A key aspect of Kepler asteroseismology is the application to solar-like oscillations of main-sequence stars. As an example we here consider an initial analysis of data for three stars in the Kepler field for which planetary transits were known from ground-based observations. For one of these, HAT-P-7, we obtain a detailed frequency spectrum and hence strong constraints on the stellar properties. The remaining two stars show definite evidence for solar-like oscillations, yielding a preliminary estimate of their mean densities. | [
0.017952797934412002,
0.0008883598493410001,
-0.0076535614207380006,
-0.015482601709663,
-0.014537717215716001,
0.035419657826423,
-0.015685077756643,
0.003062437055632,
-0.010913412086665,
-0.0035163189750160003,
0.015442106872797002,
0.020530981943011003,
-0.001110238838009,
0.0228661969... |
1001.0033 | We present 5201 radial-velocity measurements of 1144 stars, as part of an ongoing study of the young (150 Myr) open cluster M35 (NGC 2168). We have observed M35 since 1997, using the Hydra Multi-Object Spectrograph on the WIYN 3.5m telescope. Our stellar sample covers main-sequence stars over a magnitude range of 13.0<V<16.5 (1.6 - 0.8 Msun) and extends spatially to a radius of 30 arcminutes (7 pc in projection at a distance of 805 pc or 4 core radii). Due to its youth, M35 provides a sample of late-type stars with a range of rotation periods. Therefore, we analyze the radial-velocity measurement precision as a function of the projected rotational velocity. For narrow-lined stars (v sin i < 10 km/s), the radial velocities have a precision of 0.5 km/s, which degrades to 1.0 km/s for stars with v sin i = 50 km/s. The radial-velocity distribution shows a well-defined cluster peak with a central velocity of -8.16 +/- 0.05 km/s, permitting a clean separation of the cluster and field stars. For stars with >=3 measurements, we derive radial-velocity membership probabilities and identify radial-velocity variables, finding 360 cluster members, 55 of which show significant radial- velocity variability. Using these cluster members, we construct a color-magnitude diagram for our stellar sample cleaned of field star contamination. We also compare the spatial distribution of the single and binary cluster members, finding no evidence for mass segregation in our stellar sample. Accounting for measurement precision, we place an upper limit on the radial-velocity dispersion of the cluster of 0.81 +/- 0.08 km/s. After correcting for undetected binaries, we derive a true radial-velocity dispersion of 0.65 +/- 0.10 km/s. | [
-0.019704977050423,
0.010541284456849001,
0.002696097129955,
-0.028524270281195002,
-0.017476517707109,
0.038923744112253,
-0.022649243474006,
0.0065739527344700005,
-0.030550140887498002,
-0.035196140408515,
-0.015680244192481003,
0.033467397093772,
-0.009832229465246001,
0.00858294218778... |
1001.0034 | In this paper we give new identities involving q-Euler polynomials of higher order. | [
0.0018771389732130002,
0.031249636784195,
-0.015935424715280002,
-0.012593036517500001,
-0.011438393965363001,
0.006428188178688001,
-0.015408745035529001,
-0.004125654231756,
-0.0019176527857780001,
0.007447785232216001,
0.026941670104861003,
0.0011082210112360001,
-0.001449212082661,
0.0... |
1001.0035 | In [1], the spectrum (eigenvalues and eigenstates) of a lattice regularizations of the Sine-Gordon model has been completely characterized in terms of polynomial solutions with certain properties of the Baxter equation. This characterization for cyclic representations has been derived by the use of the Separation of Variables (SOV) method of Sklyanin and by the direct construction of the Baxter Q-operator family. Here, we reconstruct the Baxter Q-operator and the same characterization of the spectrum by only using the SOV method. This analysis allows us to deduce the main features required for the extension to cyclic representations of other integrable quantum models of this kind of spectrum characterization. | [
0.011283011175692002,
-0.000638701487332,
0.0070827663876110005,
-0.013307639397680001,
-0.026244668290019,
0.024858312681317003,
-0.011358506046235001,
0.000455541303381,
-0.031350851058959,
0.0032788678072390005,
0.034398086369037004,
0.025846606120467002,
-0.007762217894196,
0.032998003... |
1001.0036 | Neurons perform computations, and convey the results of those computations through the statistical structure of their output spike trains. Here we present a practical method, grounded in the information-theoretic analysis of prediction, for inferring a minimal representation of that structure and for characterizing its complexity. Starting from spike trains, our approach finds their causal state models (CSMs), the minimal hidden Markov models or stochastic automata capable of generating statistically identical time series. We then use these CSMs to objectively quantify both the generalizable structure and the idiosyncratic randomness of the spike train. Specifically, we show that the expected algorithmic information content (the information needed to describe the spike train exactly) can be split into three parts describing (1) the time-invariant structure (complexity) of the minimal spike-generating process, which describes the spike train statistically; (2) the randomness (internal entropy rate) of the minimal spike-generating process; and (3) a residual pure noise term not described by the minimal spike-generating process. We use CSMs to approximate each of these quantities. The CSMs are inferred nonparametrically from the data, making only mild regularity assumptions, via the causal state splitting reconstruction algorithm. The methods presented here complement more traditional spike train analyses by describing not only spiking probability and spike train entropy, but also the complexity of a spike train's structure. We demonstrate our approach using both simulated spike trains and experimental data recorded in rat barrel cortex during vibrissa stimulation. | [
-0.010068903677165,
0.021342517808079,
0.017440902069211003,
-0.015182072296738002,
-0.0029159437399350003,
0.005400656256824001,
0.005383543670177,
-0.019891390576958,
-0.021575244143605003,
-0.042794551700353005,
0.007111890707165,
0.038934007287025,
-0.009788261726498,
0.022862093523144... |
1001.0037 | The notion of textile system was introduced by M. Nasu in order to analyze endomorphisms and automorphisms of topological Markov shifts. A textile system is given by two finite directed graphs $G$ and $H$ and two morphisms $p,q:G\to H$, with some extra properties. It turns out that a textile system determines a first quadrant two-dimensional shift of finite type, via a collection of Wang tiles, and conversely, any such shift is conjugate to a textile shift. In the case the morphisms $p$ and $q$ have the path lifting property, we prove that they induce groupoid morphisms $\pi, \rho:\Gamma(G)\to \Gamma(H)$ between the corresponding \'etale groupoids of $G$ and $H$. We define two families ${\mathcal A}(m,n)$ and $\bar{\mathcal A}(m,n)$ of $C^*$-algebras associated to a textile shift, and compute them in specific cases. These are graph algebras, associated to some one-dimensional shifts of finite type constructed from the textile shift. Under extra hypotheses, we also define two families of Fell bundles which encode the complexity of these two-dimensional shifts. We consider several classes of examples of textile shifts, including the full shift, the Golden Mean shift and shifts associated to rank two graphs. | [
-0.011629287153482002,
-0.010451813228428001,
-0.004398211836814,
0.008083012886345001,
0.0077990335412320005,
0.007771328557282001,
-0.020072469487786,
-0.010597266256809,
0.00850551854819,
-0.036460135132074,
0.004522885661572,
0.004851885605603,
0.0035566641017790003,
0.0265416502952570... |
1001.0038 | In this paper we study ``Bergman-type'' singular integral operators on Ahlfors regular metric spaces. The main result of the paper demonstrates that if a singular integral operator on a Ahlfors regular metric space satisfies an additional estimate, then knowing the ``T(1)'' conditions for the operator imply that the operator is bounded on $L^2$. The method of proof of the main result is an extension and another application of the work originated by Nazarov, Treil and the first author on non-homogeneous harmonic analysis. | [
0.010517691262066,
-0.005017456132918,
0.008234835229814,
-0.029187455773353,
-0.00177421385888,
0.024138962849974,
-0.023035468533635,
0.0040174131281670005,
-0.027035638689994004,
-0.024401044473052,
0.017117973417043002,
0.018414581194519,
0.006717528682202,
0.016166208311915002,
-0.0... |
1001.0039 | The recently released Chandra Transmission Grating Catalog and Archive, TGCat, presents a fully dynamic on-line catalog allowing users to browse and categorize Chandra gratings observations quickly and easily, generate custom plots of resulting response corrected spectra on-line without the need for special software and to download analysis ready products from multiple observations in one convenient operation. TGCat has been registered as a VO resource with the NVO providing direct access to the catalogs interface. The catalog is supported by a back-end designed to automatically fetch newly public data, process, archive and catalog them, At the same time utilizing an advanced queue system integrated into the archive's MySQL database allowing large processing projects to take advantage of an unlimited number of CPUs across a network for rapid completion. A unique feature of the catalog is that all of the high level functions used to retrieve inputs from the Chandra archive and to generate the final data products are available to the user in an ISIS written library with detailed documentation. Here we present a structural overview of the Systems, Design, and Accessibility features of the catalog and archive. | [
-0.007946773432195001,
0.0014367097755890001,
0.005064468830823001,
-0.045832552015781,
0.009844616055488,
0.011543435044586001,
-0.014770478941500001,
-0.025588894262909,
-0.021125053986907002,
-0.012232912704348,
0.009254650212824001,
0.007189768366515001,
-0.0047055133618410004,
0.00474... |
1001.0041 | It has been known since 1970's that the N-dimensional $\ell_1$-space contains nearly Euclidean subspaces whose dimension is $\Omega(N)$. However, proofs of existence of such subspaces were probabilistic, hence non-constructive, which made the results not-quite-suitable for subsequently discovered applications to high-dimensional nearest neighbor search, error-correcting codes over the reals, compressive sensing and other computational problems. In this paper we present a "low-tech" scheme which, for any $a > 0$, allows to exhibit nearly Euclidean $\Omega(N)$-dimensional subspaces of $\ell_1^N$ while using only $N^a$ random bits. Our results extend and complement (particularly) recent work by Guruswami-Lee-Wigderson. Characteristic features of our approach include (1) simplicity (we use only tensor products) and (2) yielding "almost Euclidean" subspaces with arbitrarily small distortions. | [
0.021129878237843,
0.0061123752966520005,
0.003075127489864,
-0.027397215366363,
0.0022538308985530003,
0.006852747406810001,
-0.013374910689890001,
0.002856459468603,
-0.031928982585668,
-0.026102425530552004,
0.010675134137272,
0.004466338548809,
-0.009504313580691,
-0.001747622853145,
... |
1001.0042 | We construct new seven-dimensional gravity by adding two topological terms to the Einstein-Hilbert action. For certain choice of the coupling constants, these terms may be related to the R^4 correction to the 3-form field equation of eleven-dimensional supergravity. We derive the full set of the equations of motion. We find that the static spherically-symmetric black holes are unmodified by the topological terms. We obtain squashed AdS_7, and also squashed seven spheres and Q^{111} spaces in Euclidean signature. | [
0.00031548028346100004,
0.003186771413311,
0.006824469193816,
-0.016125669702887,
-0.008668556809425,
0.004307357128709,
-0.035131882876157004,
-0.011851962655782,
-0.007807085290551001,
-0.027647849172353002,
0.019167739897966,
0.010310736484825,
0.005364005919545001,
0.015250736847519002... |
1001.0043 | We present new radial velocity measurements of the ultra-cool dwarf VB 10, which was recently announced to host a giant planet detected with astrometry. The new observations were obtained using optical spectrographs(MIKE/Magellan and ESPaDOnS/CHFT) and cover a 63% of the reported period of 270 days. We apply Least-squares periodograms to identify the most significant signals and evaluate their corresponding False Alarm Probabilities. We show that this method is the proper generalization to astrometric data because (1) it mitigates the coupling of the orbital parameters with the parallax and proper motion, and (2) it permits a direct generalization to include non-linear Keplerian parameters in a combined fit to astrometry and radial velocity data. In fact, our analysis of the astrometry alone uncovers the reported 270 d period and an even stronger signal at 50 days. We estimate the uncertainties in the parameters using a Markov Chain Monte Carlo approach. The nominal precision of the new Doppler measurements is about 150 s$^{-1}$ while their standard deviation is 250 ms$^{-1}$. However, the best fit solutions still have RMS of 200 ms$^{-1}$ indicating that the excess in variability is due to uncontrolled systematic errors rather than the candidate companions detected in the astrometry. Although the new data alone cannot rule-out the presence of a candidate, when combined with published radial velocity measurements, the False Alarm Probabilities of the best solutions grow to unacceptable levels strongly suggesting that the observed astrometric wobble is not due to an unseen companion. | [
-0.024096295237541,
0.0036213288549330003,
-0.011042987927794,
-0.021948281675577,
-0.031366489827632,
0.028364781290292,
-0.028612628579139,
-0.00003988259413745254,
-0.030953411012887004,
-0.011600644327700001,
-0.005741802975535001,
0.036874216049909,
-0.015104934573173,
0.0176522564142... |
1001.0044 | When modelling metapopulation dynamics, the influence of a single patch on the metapopulation depends on the number of individuals in the patch. Since the population size has no natural upper limit, this leads to systems in which there are countably infinitely many possible types of individual. Analogous considerations apply in the transmission of parasitic diseases. In this paper, we prove a law of large numbers for rather general systems of this kind, together with a rather sharp bound on the rate of convergence in an appropriately chosen weighted $\ell_1$ norm. | [
0.008048203773796,
0.019094228744506,
0.018972694873809003,
-0.017811378464102003,
-0.017541304230690002,
0.010850220918655,
-0.011883254162967,
0.004807316698133,
-0.024374173954129,
-0.030599379912018002,
0.017757363617420002,
0.002818896900862,
0.0034907059744,
0.015839837491512,
0.00... |
1001.0045 | In this work the analysis of mixing parameters of the system involving eta, eta' mesons and some third massive state G is carried out. We use the generalized mixing scheme with three angles. The framework of the dispersive approach to Abelian axial anomaly of isoscalar non-singlet current and the analysis of experimental data of charmonium radiative decays ratio allow us to get a number of quite strict constraints for the mixing parameters. The analysis shows that the equal values of axial current coupling constants f_8 and f_0 are preferable which may be considered as a manifestation of SU(3) and chiral symmetry. | [
-0.017270987853407003,
0.010825554840266,
-0.007471157237887001,
-0.027819318696856003,
-0.024451060220599,
0.0037113216239950003,
-0.027902485802769002,
-0.014956176280975002,
-0.016799708828330002,
-0.014651230536401001,
0.007526602130383001,
0.017659099772572,
-0.022884750738739003,
0.0... |
1001.0046 | The Cayley graph construction provides a natural grid structure on a finite vector space over a field of prime or prime square cardinality, where the characteristic is congruent to 3 modulo 4, in addition to the quadratic residue tournament structure on the prime subfield. Distance from the null vector in the grid graph defines a Manhattan norm. The Hermitian inner product on these spaces over finite fields behaves in some respects similarly to the real and complex case. An analogue of the Cauchy-Schwarz inequality is valid with respect to the Manhattan norm. With respect to the non-transitive order provided by the quadratic residue tournament, an analogue of the Cauchy-Schwarz inequality holds in arbitrarily large neighborhoods of the null vector, when the characteristic is an appropriate large prime. | [
0.006165786646306,
-0.002419614465907,
-0.0011556620011100001,
-0.019113261252641,
-0.013387405313551001,
0.006605716422200001,
-0.009861198253929001,
-0.014402627944946001,
-0.019438132643699,
-0.043045450001955005,
0.015593823045492,
0.010889956727623001,
-0.017570123076438002,
0.0083451... |
1001.0047 | We obtain and analyze the effect of electron-electron Coulomb interaction on the time dependent current flowing through a mesoscopic system connected to biased semi-infinite leads. We assume the contact is gradually switched on in time and we calculate the time dependent reduced density operator of the sample using the generalized master equation. The many-electron states (MES) of the isolated sample are derived with the exact diagonalization method. The chemical potentials of the two leads create a bias window which determines which MES are relevant to the charging and discharging of the sample and to the currents, during the transient or steady states. We discuss the contribution of the MES with fixed number of electrons N and we find that in the transient regime there are excited states more active than the ground state even for N=1. This is a dynamical signature of the Coulomb blockade phenomenon. We discuss numerical results for three sample models: short 1D chain, 2D lattice, and 2D parabolic quantum wire. | [
-0.028490522876381003,
0.004733609966933,
0.01825088635087,
-0.032619185745716005,
-0.012659416534006,
0.009884187951683,
-0.007874540053308001,
-0.017430622130632,
-0.05725446715950901,
-0.019918758422136,
0.008824679069221,
0.034888584166765005,
-0.0038723321631550004,
0.016514658927917,... |
1001.0048 | Extending results of Oh and Zumbrun in dimensions $d\ge 3$, we establish nonlinear stability and asymptotic behavior of spatially-periodic traveling-wave solutions of viscous systems of conservation laws in critical dimensions $d=1,2$, under a natural set of spectral stability assumptions introduced by Schneider in the setting of reaction diffusion equations. The key new steps in the analysis beyond that in dimensions $d\ge 3$ are a refined Green function estimate separating off translation as the slowest decaying linear mode and a novel scheme for detecting cancellation at the level of the nonlinear iteration in the Duhamel representation of a modulated periodic wave. | [
0.004098279401659,
0.019677285104990002,
0.00006966511864447966,
-0.00042048070463300005,
-0.005234573502093,
0.015520111657679001,
-0.012014228850603001,
-0.023585027083754,
-0.0047287838533520005,
-0.022947592660784003,
0.012388374656438002,
0.014563961885869002,
0.027520483359694002,
0.... |
1001.0049 | The Swift Burst Alert Telescope (BAT) survey of Active Galactic Nuclei (AGN) is providing an unprecedented view of local AGNs (<z> = 0.03) and their host galaxy properties. In this paper, we present an analysis of the optical spectra of a sample of 64 AGNs from the 9-month survey, detected solely based on their 14-195 keV flux. Our analysis includes both archived spectra from the Sloan Digital Sky Survey and our own observations from the 2.1-m Kitt Peak National Observatory telescope. Among our results, we include line ratio classifications utilizing standard emission line diagnostic plots, [O III] 5007 A luminosities, and H-beta derived black hole masses. As in our X-ray study, we find the type 2 sources to be less luminous (in [O III] 5007 A and 14-195 keV luminosities) with lower accretion rates than the type 1 sources. We find that the optically classified LINERs, H II/composite galaxies, and ambiguous sources have the lowest luminosities, while both broad line and narrow line Seyferts have similar luminosities. From a comparison of the hard X-ray (14-195 keV) and [O III] luminosities, we find that both the observed and extinction-corrected [O III] luminosities are weakly correlated with X-ray luminosity. In a study of the host galaxy properties from both continuum fits and measurements of the stellar absorption indices, we find that the hosts of the narrow line sources have properties consistent with late type galaxies. | [
0.001472159288823,
-0.005157345905900001,
-0.014918345026671002,
-0.010621136985719001,
-0.010753466747701002,
0.029028788208961,
-0.018484260886907,
0.006445811595767001,
-0.026493644341826002,
-0.024376381188631002,
0.027677638456225003,
0.015976976603269,
0.0010307726915920001,
-0.00734... |
1001.0051 | We discuss the thermal evolution and Bose-Einstein condensation of ultra-light dark matter particles at finite, realistic cosmological temperatures. We find that if these particles decouple from regular matter before Standard model particles annihilate, their temperature will be about 0.9 K. This temperature is substantially lower than the temperature of CMB neutrinos and thus Big Bang Nucleosynthesis remains unaffected. In addition the temperature is consistent with WMAP 7-year+BAO+H0 observations without fine-tuning. We focus on particles of mass of $m\sim 10^{-23}$ eV, which have Compton wavelengths of galactic scales. Agglomerations of these particles can form stable halos and naturally prohibit small scale structure. They avoid over-abundance of dwarf galaxies and may be favored by observations of dark matter distributions. We present numerical as well as approximate analytical solutions of the Friedmann-Klein-Gordon equations and study the cosmological evolution of this scalar field dark matter from the early universe to the era of matter domination. Today, the particles in the ground state mimic presureless matter, while the excited state particles are radiation like. | [
0.007580397184938001,
-0.001082188100554,
-0.0036242292262610005,
-0.025064762681722003,
-0.015255633741617002,
0.007099424954503001,
-0.028153825551271,
-0.008400082588195001,
-0.017396301031112,
-0.024698952212929,
-0.0043389135971660005,
0.038261022418737,
-0.014754339121282002,
0.00788... |
1001.0052 | The phase-integral method (PIM) is an asymptotic method of the geometrical optics or semi-classical type for solving approximately, but in many cases very accurately, a wide class of differential equations in physics. Unlike the related (J)WKB method, the higher-order corrections in the PIM can be generated from a generic, unspecified base function, providing added symmetry and flexibility. However, with the conventional approach of using the next-to-lowest (third) order correction to the integrand in the phase integral as a platform for calculating higher (fifth, seventh, ninth,...) order corrections, the higher-order calculations very often become quite complicated. We therefore introduce a new platform function, which considerably simplifies the calculation of the third-order contribution for a wide range of problems. We also present directly integrable conditions for the phase integral, which so far seem to have gone unnoticed. For a large number of observables, our analysis makes a clearer distinction between physical and, in a sense, unphysical contributions. | [
0.008976086042821001,
0.01046869251877,
-0.0087716197595,
-0.008137772791087001,
-0.018061222508549,
0.031760487705469,
-0.00694164307788,
-0.034513972699642,
-0.018088484182953002,
-0.018347475677728,
0.038657829165458006,
0.019206235185265,
0.00043832539813500005,
0.017515977844595,
-0... |
1001.0053 | Rotation vectors, as defined for homeomorphisms of the torus that are isotopic to the identity, are generalized to such homeomorphisms of any complete Riemannian manifold with non-positive sectional curvature. These generalized rotation vectors are shown to exist for almost every orbit of such a dynamical system with respect to any invariant measure with compact support. The concept is then extended to flows and, as an application, it is shown how non-null rotation vectors can be used to construct a measurable semi-conjugacy between a given flow and the geodesic flow of a manifold. | [
-0.014649042859673,
-0.015482290647923001,
-0.014958150684833001,
-0.017215983942151,
0.0025652623735360003,
0.00040297466330200003,
-0.013459648005664002,
0.0041024037636810005,
-0.002212475752457,
-0.029513116925954003,
0.025024328380823004,
0.007479075342416001,
-0.014635602943599,
0.00... |
1001.0054 | There is currently an intersection in the research of game theory and cryptography. Generally speaking, there are two aspects to this partnership. First there is the application of game theory to cryptography. Yet, the purpose of this paper is to focus on the second aspect, the converse of the first, the application of cryptography to game theory. Chiefly, there exist a branch of non-cooperative games which have a correlated equilibrium as their solution. These equilibria tend to be superior to the conventional Nash equilibria. The primary condition for a correlated equilibrium is the presence of a mediator within the game. This is simply a neutral and mutually trusted entity. It is the role of the mediator to make recommendations in terms of strategy profiles to all players, who then act (supposedly) on this advice. Each party privately provides the mediator with the necessary information, and the referee responds privately with their optimized strategy set. However, there seem to be a multitude of situations in which no mediator could exist. Thus, games modeling these sorts of cases could not use these entities as tools for analysis. Yet, if these equilibria are in the best interest of players, it would be rational to construct a machine, or protocol, to calculate them. Of course, this machine would need to satisfy some standard for secure transmission between a player and itself. The requirement that no third party could detect either the input or strategy profile would need to be satisfied by this scheme. Here is the synthesis of cryptography into game theory; analyzing the ability of the players to construct a protocol which can be used successfully in the place of a mediator. | [
-0.013519381172955001,
-0.0046195699833330005,
0.006262456998229001,
-0.025533623993396003,
0.010798035189509001,
0.007787755224853,
-0.007673525717109,
0.0019486186793070002,
-0.0036419010721140004,
-0.031527306884527005,
0.028086986392736,
0.00394763238728,
-0.003253857139497,
0.01403005... |
1001.0055 | Fortuin-Kastelyn clusters in the critical $Q$-state Potts model are conformally invariant fractals. We obtain simulation results for the fractal dimension of the complete and external (accessible) hulls for Q=1, 2, 3, and 4, on clusters that wrap around a cylindrical system. We find excellent agreement between these results and theoretical predictions. We also obtain the probability distributions of the hull lengths and maximal heights of the clusters in this geometry and provide a conjecture for their form. | [
0.011436742730438001,
-0.0037345178425310004,
-0.0042809476144610005,
-0.026019807904958003,
-0.0036997133865950002,
0.020409330725669,
-0.022497598081827,
-0.006271762307733001,
-0.017318695783615,
-0.026423539966344,
0.015216506086289001,
0.019587945193052,
0.014395121484994002,
0.017485... |
1001.0056 | Let G denote a complex, semisimple, simply-connected group. We identify the equivariant quantum differential equation for the cotangent bundle to the flag variety of G with the affine Knizhnik-Zamolodchikov connection of Cherednik and Matsuo. This recovers Kim's description of quantum cohomology of the flag variety itself as a limiting case. A parallel result is proven for resolutions of the Slodowy slices. Extension to arbitrary symplectic resolutions is discussed. | [
-0.003126874100416,
0.011324169114232,
0.00015296830679200002,
-0.003011637367308,
-0.007237561047077,
0.027753157541155003,
-0.022483222186565,
0.014819113537669001,
0.0064223036170000004,
-0.027725638821721,
0.014530161395668002,
0.026377195492386003,
0.01350506953895,
0.019442345947027,... |
1001.0057 | We present a generic mechanism by which reproducing microorganisms, with a diffusivity that depends on the local population density, can form stable patterns. It is known that a decrease of swimming speed with density can promote separation into bulk phases of two coexisting densities; this is opposed by the logistic law for birth and death which allows only a single uniform density to be stable. The result of this contest is an arrested nonequilibrium phase separation in which dense droplets or rings become separated by less dense regions, with a characteristic steady-state length scale. Cell division mainly occurs in the dilute regions and cell death in the dense ones, with a continuous flux between these sustained by the diffusivity gradient. We formulate a mathematical model of this in a case involving run-and-tumble bacteria, and make connections with a wider class of mechanisms for density-dependent motility. No chemotaxis is assumed in the model, yet it predicts the formation of patterns strikingly similar to those believed to result from chemotactic behavior. | [
-0.010399687103927,
0.026775261387228,
0.005828884430229,
-0.013996159657835001,
-0.010023629292845001,
0.027404302731156002,
0.003938342910259,
0.022262576967477,
-0.022905291989445003,
-0.041079103946685,
0.009182629175484,
0.019746413454413,
0.017872964963316,
0.025900075212121003,
0.... |
1001.0058 | The $C$-function of $T$-adic exponential sums is studeid. An explicit arithmetic bound is established for the Newton polygon of the $C$-function. This polygon lies above the Hodge polygon. It gives a sup-Hodge bound of the $C$-function of $p$-power order exponential sums. | [
0.009406547993421001,
0.01661523990333,
0.012924499809741,
0.0035801555495700004,
-0.028558306396007004,
0.0013883470091960001,
-0.009213025681674,
-0.024646399542689,
-0.00568125071004,
-0.016131434589624002,
0.024867566302418,
0.017181981354951,
0.013843728229403001,
0.016573769971728002... |
1001.0059 | The TANAMI (Tracking AGN with Austral Milliarcsecond Interferometry) and associated programs provide comprehensive radio monitoring of extragalactic gamma-ray sources south of declination -30 degrees. Joint quasi-simultaneous observations between the Fermi Gamma-ray Space Telescope and ground based observatories allow us to discriminate between competing theoretical blazar emission models. High resolution VLBI observations are the only way to spatially resolve the sub-parsec level emission regions where the high-energy radiation originates. The gap from radio to gamma-ray energies is spanned with near simultaneous data from the Swift satellite and ground based optical observatories. We present early results from the TANAMI program in the context of this panchromatic suite of observations. | [
-0.009356218390166001,
-0.018519951030611003,
-0.006912327371537,
-0.013927772641181,
-0.012305386364459001,
0.029367940500378,
-0.037699855864048004,
-0.007039505988359,
-0.021833468228578002,
-0.014615224674344,
0.012697233818471002,
0.012697233818471002,
-0.002304682042449,
-0.008338790... |
1001.0061 | The energy density of the Universe is dominated by dark energy and dark matter, two mysterious components which pose some of the most important questions in fundamental science today. Euclid is a high-precision survey mission designed to answer these questions by mapping the geometry of the dark Universe. Euclid's Visible-NIR imaging and spectroscopy of the entire extragalactic sky will further produce extensive legacy science for various fields of astronomy. Over the 2008-2009 period, Euclid has been the object of an ESA Assessment Phase in which the study of the Euclid Imaging instrument was under the responsibility of the Euclid Imaging Consortium (EIC). The EIC Science Book presents the studies done by the EIC science working groups in the context of this study phase. We first give a brief description of the Euclid mission and of the imaging instrument and surveys. We then summarise the primary and legacy science which will be achieved with the Euclid imaging surveys, along with the simulations and data handling scheme which have been developed to optimise the instrument and ensure its science performance. | [
0.033846803009510006,
0.007791331503540001,
-0.0031021675094960004,
-0.031958822160959,
0.0017580089624970002,
0.025104640051722003,
-0.021410770714282,
-0.025241451337933003,
-0.009364646859467,
-0.028538573533296002,
0.009624585509300001,
-0.004617338534444001,
-0.006741314195096,
0.0156... |
1001.0062 | Unfolded equations of motion for symmetric massive bosonic fields of any spin in Minkowski and (A)dS spaces are presented. Manifestly gauge invariant action for a spin $s \ge 2$ massive field in any dimension is constructed in terms of gauge invariant curvatures. | [
-0.021759700030088,
-0.014457337558269001,
-0.011054034344851001,
0.004622596316039,
-0.01312415394932,
-0.0005564701277760001,
-0.026717266067862,
-0.005781595129519,
-0.007818217389285,
-0.026958445087075,
0.013961580581963002,
0.002421838464215,
0.010913346894085001,
0.026275105774402,
... |
1001.0063 | In this paper we give a thorough presentation of a model proposed by Tononi et al. for modeling \emph{integrated information}, i.e. how much information is generated in a system transitioning from one state to the next one by the causal interaction of its parts and \emph{above and beyond} the information given by the sum of its parts. We also provides a more general formulation of such a model, independent from the time chosen for the analysis and from the uniformity of the probability distribution at the initial time instant. Finally, we prove that integrated information is null for disconnected systems. | [
-0.012458964250981001,
0.020835950970649,
0.010926504619419,
-0.01698762178421,
-0.015626963227987,
-0.000119508644274,
-0.012726972810924001,
0.004463374149054,
-0.023103715851902,
-0.040050104260444,
0.01295374892652,
0.029219809919595004,
-0.0041163372807200005,
0.016190467402338,
0.0... |
1001.0064 | In this paper, we develop some of the theory of SSD spaces and SSDB spaces, and deduce some results on maximally monotone multifunctions on a reflexive Banach space. | [
-0.004639245104044,
0.013154657557606001,
0.008900327607989,
-0.018867613747715003,
-0.01935382373631,
0.019016178324818,
-0.020758427679538,
0.006256565451622001,
-0.015234551392495,
-0.011932381428778002,
0.015842312946915002,
0.014316156506538,
0.019907562062144002,
0.011304361745715,
... |
1001.0065 | Magnetic field in the solar lower atmosphere can be measured by the use of the Zeeman and Hanle effects. In contrast, the coronal magnetic field well above the solar surface, which directly controls various eruptive phenomena, can not be precisely measureed with the traditional techniques. Several attempts are being made to probe the coronal magnetic field, such as force-free extrapolation based on the photospheric magnetograms, gyroresonance radio emissions, and coronal seismology based on MHD waves in the corona. Compared to the waves trapped in the localized coronal loops, EIT waves are the only global-scale wave phenomenon, and thus are the ideal tool for the coronal global seismology. In this paper, we review the observations and modelings of EIT waves, and illustrate how they can be applied to probe the global magnetic field in the corona. | [
-0.016557751223444002,
0.007731784135103,
0.008746869862079001,
-0.036463964730501,
-0.025851711630821003,
0.015463568270206,
-0.031217161566019003,
-0.015068081207573001,
-0.003951581194996,
-0.009821278043091,
-0.009742179885506,
0.024981638416647002,
-0.013202697038650001,
0.01711143366... |
1001.0066 | We investigate a matter dominated navigation cosmological model. The influence of a possible drift (wind) in the navigation cosmological model makes the spacetime geometry change from Riemannian to Finslerian. The evolution of the Finslerian Universe is governed by the same gravitational field equation with the familiar Friedmann-Robertson-Walker one. However, the change of space geometry from Riemannian to Finslerian supplies us a new relation between the luminosity distant and redshift. It is shown that the Hubble diagram based on this new relation could account for the observations on distant Type Ia supernovae. | [
0.025887044146656,
0.00718624331057,
0.013564811088144,
-0.0035206379834560003,
-0.010334108024835,
0.005063505843281,
-0.030291292816400004,
0.006489018909633001,
-0.0050980220548800005,
-0.040231917053461005,
0.002000205684453,
0.013792617246508002,
0.019121896475553003,
0.02632884867489... |
1001.0067 | We demonstrate an efficient numerical method to calculate three-tangle of general mixed states. We construct a "energy function" (target function) for the three-tangle of the mixed state under certain constrains. The "energy function" (target function) is then optimized via a replica exchange Monte Carlo method. We have extensively tested the method for the examples with known analytical results, showing remarkable agreement. The method can be applied to other optimization problems in quantum information theory. | [
-0.017416687682271,
-0.010821550153195001,
0.011463798582553001,
-0.007727705407887001,
-0.00419533625245,
0.008079906925559,
-0.014460960403084,
-0.0037360934074960003,
-0.037706229835748006,
-0.024792192503809003,
-0.00336144817993,
0.02686396241188,
0.0015857679536560002,
0.013369828462... |
1001.0068 | Bayesian methods since the time of Laplace have been understood by their practitioners as closely aligned to the scientific method. Indeed a recent champion of Bayesian methods, E. T. Jaynes, titled his textbook on the subject Probability Theory: the Logic of Science. Many philosophers of science including Karl Popper and Donald Campbell have interpreted the evolution of Science as a Darwinian process consisting of a 'copy with selective retention' algorithm abstracted from Darwin's theory of Natural Selection. Arguments are presented for an isomorphism between Bayesian Methods and Darwinian processes. Universal Darwinism, as the term has been developed by Richard Dawkins, Daniel Dennett and Susan Blackmore, is the collection of scientific theories which explain the creation and evolution of their subject matter as due to the operation of Darwinian processes. These subject matters span the fields of atomic physics, chemistry, biology and the social sciences. The principle of Maximum Entropy states that systems will evolve to states of highest entropy subject to the constraints of scientific law. This principle may be inverted to provide illumination as to the nature of scientific law. Our best cosmological theories suggest the universe contained much less complexity during the period shortly after the Big Bang than it does at present. The scientific subject matter of atomic physics, chemistry, biology and the social sciences has been created since that time. An explanation is proposed for the existence of this subject matter as due to the evolution of constraints in the form of adaptations imposed on Maximum Entropy. It is argued these adaptations were discovered and instantiated through the operations of a succession of Darwinian processes. | [
-0.013773337006568001,
0.0031096711754790003,
0.001094143604859,
-0.011104032397270001,
-0.009972627274692001,
0.012987449765205002,
-0.015690628439188,
-0.001654765103012,
-0.005718001164495,
-0.027289226651191004,
-0.010412994772195,
0.026706587523221,
-0.003827808657661,
0.0230887997895... |
1001.0069 | Physical-layer Network Coding (PNC) makes use of the additive nature of the electromagnetic (EM) waves to apply network coding arithmetic at the physical layer. With PNC,the destructive effect of interference in wireless networks is eliminated and the capacity of networks can be boosted significantly. This paper addresses a key outstanding issue in PNC: synchronization among transmitting nodes. We first investigate the impact of imperfect synchronization (i.e., finite synchronization errors) in a 3-node network. It is shown that with QPSK modulation, PNC still yields significantly higher capacity than straightforward network coding when there are synchronization errors. Significantly, this remains to be so even in the extreme case when synchronization is not performed at all. Moving beyond a 3-node network, we propose and investigate a synchronization scheme for PNC in a general chain network. At last, numerical simulation verifies that PNC is robust to synchronization errors. In particular, for the mutual information performance, there is about 0.5dB loss without time synchronization and there is at most 2dB loss without phase synchronization. | [
0.005432225298136,
0.002541372086852,
0.019557368010282003,
-0.008387546055018002,
0.003667854703962,
0.005632413551211001,
-0.024212591350078003,
-0.001148537266999,
-0.041856296360492005,
-0.021240305155515,
0.011366616934537001,
0.026112683117389002,
-0.005941178184002,
0.00566295068711... |
1001.0071 | An all-sky comprehensive catalog of calculated radio and X-ray associations to optical objects is presented. Included are X-ray sources from XMM-Newton, Chandra and ROSAT catalogs, radio sources from NVSS, FIRST and SUMSS catalogs, and optical data, identifications and redshifts from the APM, USNO-A, SDSS-DR7 and the extant literature. This "Atlas of Radio/X-ray Associations" inherits many techniques from the predecessor Quasars.org (2004) catalog, but object selection is changed and processing tweaked. Optical objects presented are those which are calculated with >=40% confidence to be associated with radio/X-ray detections, totalling 602570 objects in all, including 23681 double radio lobe detections. For each of these optical objects I display the calculated percentage probabilities of its being a QSO, galaxy, star, or erroneous radio/X-ray association, plus any identification from the literature. The catalogue includes 105568 uninvestigated objects listed as 40% to >99% likely to be a QSO. The catalog is available at http://quasars.org/arxa.htm . | [
0.007623176090419001,
0.014528877101838,
0.007857735268771001,
-0.048677947372198,
-0.047215402126312006,
0.028202302753925,
-0.007154057733714,
0.003340744879096,
-0.023331748321652003,
-0.013776907697319,
0.0018919964786610001,
-0.011341630481183002,
-0.013563044369220002,
0.009216799400... |
1001.0072 | Polya Enumeration Theorem is one of the most useful tools dealing with the enumeration of patterns that are symmetric in some ways. What follows is a procedure for obtaining the results of Polya Theorem directly, bypassing the usual preliminaries. | [
-0.014700132422149001,
0.004034942016005,
-0.008109507150948,
-0.029928572475910003,
-0.029928572475910003,
0.017117135226726,
-0.023602100089192002,
-0.0065774177201090005,
-0.012956720776855,
-0.014620887115597002,
0.021000189706683003,
-0.010552925989031,
0.010434056632220001,
0.0032309... |
1001.0073 | We show that for a $\sigma $-ideal $\ci$ with a Steinhaus property defined on Banach space, if two non-homeomorphic Banach with the same cardinality of the Hamel basis then there is a $\ci$ nonmeasurable subset as image by any isomorphism between of them. Our results generalize results from [2] | [
-0.008092877455055,
-0.014043921604752001,
-0.0028111564461140003,
-0.018015801906585003,
-0.0075235292315480005,
0.018503814935684003,
-0.019886517897248,
0.013250900432467001,
-0.007896317169070001,
-0.021540338173508002,
-0.0019317170372230002,
0.011122623458504,
0.005280026234686001,
0... |
1001.0074 | We explain how Lie superalgebras of types gl and osp provide a natural framework generalizing the classical Schur and Howe dualities. This exposition includes a discussion of super duality, which connects the parabolic categories O between classical Lie superalgebras and Lie algebras. Super duality provides a conceptual solution to the irreducible character problem for these Lie superalgebras in terms of the classical Kazhdan-Lusztig polynomials. | [
0.020313909277319003,
0.048628620803356004,
0.0066311759874220005,
-0.044506173580884004,
-0.019066326320171002,
0.016842372715473,
0.003410512814298,
-0.007051557302474001,
0.001728987554088,
-0.033874593675136004,
0.004251275211572,
0.031623519957065,
-0.010109491646289001,
0.03308807685... |
1001.0075 | We prove that the class of principal coactions is closed under one-surjective pullbacks in an appropriate category of algebras equipped with left and right coactions. This allows us to handle cases of C*-algebras lacking two different non-trivial ideals. It also allows us to go beyond the category of comodule algebras. As an example of the former, we carry out an index computation for noncommutative line bundles over the standard Podles sphere using the Mayer-Vietoris type arguments afforded by a one-surjective pullback presentation of the C*-algebra of this quantum sphere. To instantiate the latter, we define a family of coalgebraic noncommutative deformations of the U(1)-principal bundle S^7 --> CP^3. | [
0.012812552042305001,
0.014163821004331001,
0.013764741830527002,
-0.020752133801579,
-0.025233026593923003,
0.020612105727195,
-0.004785453435033,
-0.004134323447942,
0.0054750903509550005,
-0.035147000104188,
-0.006570809055119001,
0.023552691563963002,
0.014030794613063,
0.0186517145484... |
1001.0076 | GLACIER (Giant Liquid Argon Charge Imaging ExpeRiment) is a large underground observatory for proton decay search, neutrino astrophysics and CP-violation studies in the lepton sector. Possible underground sites are studied within the FP7 LAGUNA project (Europe) and along the JPARC neutrino beam in collaboration with KEK (Japan). The concept is scalable to very large masses. | [
0.0007356107234950001,
-0.012214559130370001,
0.006552067585289,
-0.030683521181344004,
0.001907455734908,
0.009142101742327,
-0.031860496848821,
0.007725622970610001,
-0.010873353108763001,
-0.025387123227119,
0.00434865662828,
0.016806138679385,
-0.016149220988154002,
-0.0083620119839900... |
1001.0077 | The feasibility of a next generation neutrino observatory in Europe is being considered within the LAGUNA design study. To accommodate giant neutrino detectors and shield them from cosmic rays, a new very large underground infrastructure is required. Seven potential candidate sites in different parts of Europe and at several distances from CERN are being studied: Boulby (UK), Canfranc (Spain), Fr\'ejus (France/Italy), Pyh\"asalmi (Finland), Polkowice-Sieroszowice (Poland), Slanic (Romania) and Umbria (Italy). The design study aims at the comprehensive and coordinated technical assessment of each site, at a coherent cost estimation, and at a prioritization of the sites within the summer 2010. | [
0.009787550196051,
-0.011110937222838001,
0.017176462337374,
-0.006289535202085,
0.002157396636903,
0.013571610674262002,
-0.026150681078433,
-0.010966191999614001,
-0.013978276401758001,
-0.009704838506877,
0.005958688445389,
-0.0029466040432450003,
0.005793265067040001,
-0.00511433975771... |
1001.0078 | We extend the matrix decomposition method(MDM) in classifying the $2\times N\times N$ truly entangled states to $2\times M\times N$ system under the condition of stochastic local operations and classical communication. It is found that the MDM is quite practical and convenient in operation for the asymmetrical tripartite states, and an explicit example of the classification of $2\times 6\times 7$ quantum system is presented. | [
-0.014485986903309002,
0.025722526013851003,
-0.014363109134137,
-0.035334341228008,
0.000354981777491,
0.024794112890958002,
-0.032112199813127004,
-0.006055170204490001,
-0.036399286240339,
-0.013530267402529002,
0.008785799145698001,
0.042952794581651,
-0.006567162927240001,
0.016001487... |
1001.0079 | Based on perturbation theory, we study the dynamics of how dark matter and dark energy in the collapsing system approach dynamical equilibrium while interacting. We find that the interaction between dark sectors cannot ensure the dark energy to fully cluster along with dark, leading to the energy non-conservation problem in the collapsing system We examine the cluster number counts dependence on the interaction between dark sectors. Furthermore, we analyze how dark energy inhomogeneities affect cluster abundances. It is shown that cluster number counts can provide specific signature of dark sectors interaction and dark energy inhomogeneities. | [
-0.005878811702132,
-0.00864828005433,
0.0021889908239240002,
-0.02121352404356,
0.011104796081781,
0.022371115162968,
-0.031174190342426,
-0.00537741323933,
-0.02048666588962,
-0.011273049749433,
0.018777200952172002,
0.014483345672488001,
-0.001057479414157,
0.025776585564017,
-0.00432... |
1001.0081 | In the present work we explore electron transport properties through a quantum interferometer attached symmetrically to two one-dimensional semi-infinite metallic electrodes, namely, source and drain. The interferometer is made up of two sub-rings where individual sub-rings are penetrated by Aharonov-Bohm fluxes $\phi_1$ and $\phi_2$, respectively. We adopt a simple tight-binding framework to describe the model and all the calculations are done based on the single particle Green's function formalism. Our exact numerical calculations describe two-terminal conductance and current as functions of interferometer-to-electrode coupling strength, magnetic fluxes threaded by left and right sub-rings of the interferometer and the difference of these two fluxes. Our theoretical results provide several interesting features of electron transport across the interferometer, and these aspects may be utilized to study electron transport in Aharonov-Bohm geometries. | [
-0.016740493476390002,
0.001336264424026,
0.003097058041021,
-0.007708381861448001,
-0.006702214013785001,
0.023706784471869,
-0.013197177089750002,
-0.013043411076068,
-0.024923544377088002,
-0.026795485988259003,
0.007541244383901,
0.004843644797801,
0.002177801681682,
0.0192274991422890... |
1001.0082 | Detailed comparisons are reported between laboratory observations of electron-scale dissipation layers near a reconnecting X-line and direct two-dimensional full-particle simulations. Many experimental features of the electron layers, such as insensitivity to the ion mass, are reproduced by the simulations; the layer thickness, however, is about 3-5 times larger than the predictions. Consequently, the leading candidate 2D mechanism based on collisionless electron nongyrotropic pressure is insufficient to explain the observed reconnection rates. These results suggest that, in addition to the residual collisions, 3D effects play an important role in electron-scale dissipation during fast reconnection. | [
-0.015156625770032002,
0.029109476134181002,
0.005745291244238,
-0.013227849267423,
-0.015854267403483002,
0.0014559867559000002,
0.006733618211001001,
-0.006716519128531001,
-0.042186852544546,
-0.02458163909614,
0.007653548847883,
0.027604756876826002,
0.001202065381221,
0.01017737295478... |
1001.0083 | We present a study of tau->pipipinu, tau->Kpipinu, tau->KKpinu, and tau->KKKnu decays using a 666 fb-1 data sample collected with the Belle detector at the KEKB asymmetric-energy e+e- collider at and near a center-of-mass energy of 10.58 GeV. The branching fractions are measured to be: B(tau->pipipinu) = (8.42+-0.01+0.26-0.25) x 10^-2, B(tau->Kpipinu) = (3.30+-0.01+0.16-0.17) x 10^-3, B(tau->KKpinu) = (1.55+-0.01+0.06-0.05) x 10^-3, and B(tau->KKKnu) = (3.29+-0.17+0.19-0.20) x 10^-5, where the first uncertainty is statistical and the second is systematic. These branching fractions do not include contributions from modes in which a pi^+pi^- pair originates from a Ks decay. We also present the unfolded invariant mass distributions for these decays. | [
-0.014259782619774002,
-0.011510169133543,
0.008630921132862,
-0.037034496665,
-0.020618690177798,
0.0007428391836580001,
-0.028164776042103,
0.0015351440524680002,
-0.019881822168827,
-0.032422244548797004,
0.007921343669295,
0.021996909752488,
-0.008126029744744,
-0.0023590046912430004,
... |
1001.0084 | We consider a time independent Schrodinger type equation derived from the equations of motion that drives a single scalar field in a standard cosmology model for inflation in a flat space-time with a Friedman-Robertson-Walker (FRW) metric with a cosmological constant. We find that all the 1-dimensional bound state solutions of quantum mechanics lead to at least one exact solution for the dynamical equations of standard cosmology, and that these solutions resemble the most recurrent inflationary solutions found in the literature. The analogies derived from this approach may be used to realize a deeper understanding of the dynamics of the model. | [
0.022915510460734003,
0.007834934629499,
-0.007667521480470001,
-0.013794842176139,
-0.014598425477743001,
-0.013634125702083002,
-0.021013697609305,
-0.016861850395798,
-0.015428794547915,
-0.023478018119931002,
0.011176501400768,
0.027750400826334003,
0.014102882705628001,
0.033830847591... |
1001.0085 | In this short paper, we show a certain matrix trace inequality and then give a refinement of the trace inequality proven by Belmega, Lasaulce and Debbah. In addition, we give an another improvement of their trace inequality. | [
-0.011088334023952,
0.007977021858096001,
-0.00006569349352503195,
-0.035499114543199005,
-0.000755983812268,
0.004074174445122001,
-0.028317056596279002,
0.007154648192226,
-0.020216677337884,
-0.007188913878053001,
0.015707330778241,
0.007915343157947001,
0.001404031179845,
-0.0042831944... |
1001.0086 | We show that the maximum slope invariant for tubular groups is easy to calculate, and give an example of two tubular groups that are distinguishable by their maximum slopes but not by edge pattern considerations or isoperimetric function. | [
-0.00024361856048900002,
0.016576880589127003,
0.014433203265070001,
-0.013301448896527,
0.003525083651766,
0.010458746924996001,
-0.0009012430673460001,
-0.0034851392265400002,
-0.013993816450238,
-0.00047267408808600005,
0.010618523694574,
0.0062579386867580005,
0.025843955576419,
0.0289... |
1001.0087 | We discuss the information that can be obtained from an analysis of fluctuations in heavy ion collisions within the context of the statistical model of particle production. We then examine the recently published experimental data on ratio fluctuations, and use it to obtain constraints on the statistical properties (physically relevant ensemble, degree of chemical equilibration, scaling across energies and system sizes) and freeze-out dynamics (amount of reinteraction between chemical and thermal freeze-out) of the system. | [
-0.021285332739353003,
0.007279692217707001,
0.0035453045275060002,
-0.046433359384536,
0.002517166314646,
0.0046899314038450005,
-0.013749028556048001,
0.014194724150002001,
-0.028173353523015,
-0.032684329897165,
0.015680376440286,
0.024810379371047003,
-0.011723140254616,
0.008002258837... |
1001.0088 | A careful look at an allegedly well-known century-old concept reveals interesting aspects in it that have generally avoided recognition in literature. There are four different kinds of physical observables known or proclaimed as relativistic invariants under space-time rotations. Only observables in the first three categories are authentic invariants, whereas the single "invariant" - proper length - in the fourth category is actually not an invariant. The proper length has little is anything to do with proper distance which is a true invariant. On the other hand, proper distance, proper time, and rest mass have more in common than usually recognized, and particularly, mass - time analogy opens another view of the twin paradox. | [
0.023609599098563003,
-0.008564266376197,
-0.004663372412323,
-0.016556674614548,
-0.0012756196083500001,
-0.0031435214914380004,
-0.014160313643515,
-0.024412924423813,
-0.029300956055521004,
-0.008911466225981001,
0.021594477817416,
0.015018101781606001,
-0.011382712982594,
0.00552796851... |
1001.0089 | We describe a method to enhance the sensitivity of precision measurements that takes advantage of a quantum sensor's environment to amplify its response to weak external perturbations. An individual qubit is used to sense the dynamics of surrounding ancillary qubits, which are in turn affected by the external field to be measured. The resulting sensitivity enhancement is determined by the number of ancillas that are coupled strongly to the sensor qubit; it does not depend on the exact values of the coupling strengths and is resilient to many forms of decoherence. The method achieves nearly Heisenberg-limited precision measurement, using a novel class of entangled states. We discuss specific applications to improve clock sensitivity using trapped ions and magnetic sensing based on electronic spins in diamond. | [
-0.023450378328561002,
0.015163195319473001,
0.015356885269284002,
-0.014429938048124001,
-0.00828718394041,
0.040702663362026006,
-0.022412750869989003,
-0.026839962229132003,
-0.038267698138952005,
-0.024709366261959003,
0.012264755554497,
0.030271049588918002,
-0.010964263230562,
0.0176... |
1001.0091 | Making use of the Lagrange anchor construction introduced earlier to quantize non-Lagrangian field theories, we extend the Noether theorem beyond the class of variational dynamics. | [
-0.003905261633917,
0.003250456880778,
0.00987088587135,
-0.001824699807912,
0.014409068971872002,
0.010867400094866001,
-0.057205349206924,
-0.013870411552488,
-0.009237963706254002,
-0.020913349464535002,
-0.002742099575698,
0.023889428004622,
0.018543260172009003,
0.016105838119983,
0... |
1001.0092 | A general feature of TeV-scale radiative seesaw models, in which tiny neutrino masses are generated via loop corrections, is an extended scalar (Higgs) sector. Another feature is the Majorana nature; e.g., introducing right-handed neutrinos with TeV-scale Majorana masses under the discrete symmetry, or otherwise introducing some lepton number violating interactions in the scalar sector. We study phenomenological aspects of these models at collider experiments. We find that, while properties of the extended Higgs sector of these models can be explored to some extent, the Majorana nature of the models can also be tested directly at the International Linear Collider via the electron-positron and electron-electron collision experiments. | [
-0.013785109855234002,
-0.001003819634206,
0.0057579502463340005,
-0.007738413289189,
-0.014892539009451,
0.00122802297119,
-0.024526489898562,
-0.008764313533902,
-0.025898886844515003,
-0.038834739476442004,
0.012059424072504,
0.013581288978457002,
-0.016061114147305003,
0.00786750018596... |
1001.0093 | By analysing the Chandra and XMM-Newton archived data of the nearby galaxy cluster Abell 3158, which was reported to possess a relatively regular, relaxed morphology in the X-ray band in previous works, we identify a bow edge-shaped discontinuity in the X-ray surface brightness distribution at about $120h_{71}^{-1}$ kpc west of the X-ray peak. This feature is found to be associated with a massive, off-centre cool gas clump, and actually forms the west boundary of the cool clump. We find that the cool gas clump is moving at a subsonic velocity of ~700 km/s toward west on the sky plane. We exclude the possibility that this cool clump was formed by local inhomogeneous radiative cooling in the intra-cluster medium, due to the effectiveness of the thermal conduction on the time-scale of $\sim 0.3$ Gyr. Since no evidence for central AGN activity has been found in Abell 3158, and this cool clump bears many similarities to the off-centre cool gas clumps detected in other merging clusters in terms of their mass, size, location, and thermal properties (e.g. lower temperature and higher abundance as compared with the environment), we speculate that the cool clump in Abell 3158 was caused by a merger event, and is the remnant of the original central cool-core of the main cluster or the infalling sub-cluster. This idea is supported not only by the study of line-of-sight velocity distribution of the cluster member galaxies, but also by the study of gas entropy-temperature correlation. This example shows that the appearance of such massive, off-centre cool gas clumps can be used to diagnose the dynamical state of a cluster, especially when prominent shocks and cold fronts are absent. | [
-0.0007209144532680001,
0.00833745766431,
0.016564667224884002,
-0.027024388313293003,
-0.028967497870326,
0.021429333835840003,
-0.015944527462124002,
-0.007800001651048,
-0.012099649757146001,
-0.022876329720020003,
0.010824914090335001,
-0.000159018920385,
0.01285070925951,
0.0166335720... |
1001.0094 | In this article we prove the existence of a stochastic optimal transference plan for a stochastic Monge-Kantorovich problem by measurable selection theorem. A stochastic version of Kantorovich duality and the characterization of stochastic optimal transference plan are also established. Moreover, Wasserstein distance between two probability kernels are discussed too. | [
0.0019119575154030002,
-0.01954598352313,
0.017909128218889,
-0.020866472274065,
0.015639537945389,
0.02273716405034,
-0.013026070781052002,
0.006141647696495001,
-0.036891151219606004,
-0.019848594442009003,
0.006282637361437001,
0.039669681340456,
-0.006145086605101001,
0.014869252219796... |
1001.0095 | Asymptotics of the variances of many cost measures in random digital search trees are often notoriously messy and involved to obtain. A new approach is proposed to facilitate such an analysis for several shape parameters on random symmetric digital search trees. Our approach starts from a more careful normalization at the level of Poisson generating functions, which then provides an asymptotically equivalent approximation to the variance in question. Several new ingredients are also introduced such as a combined use of the Laplace and Mellin transforms and a simple, mechanical technique for justifying the analytic de-Poissonization procedures involved. The methodology we develop can be easily adapted to many other problems with an underlying binomial distribution. In particular, the less expected and somewhat surprising $n(\log n)^2$-variance for certain notions of total path-length is also clarified. | [
-0.0022893103305250003,
0.008577581495046002,
0.005561971571296001,
-0.010468375869095001,
-0.011186049319803,
0.024042071774601003,
-0.001136029255576,
-0.013214858248829,
-0.039444454014301,
-0.024663135409355,
0.005172081757336001,
0.011910623870790001,
-0.005610276479274001,
0.00881910... |
1001.0096 | Mirror dark matter offers a framework to explain the existing dark matter direct detection experiments, including the impressive DAMA annual modulation signal. Here we examine the implications of mirror dark matter for experiments like CDMSII/Ge and XENON10 which feature higher recoil energy threshold than the DAMA NaI experiments. We show that the two events seen in the CDMSII/Ge experiment are consistent with the interactions of the anticipated heavy $\sim Fe'$ component. This interpretation of the CDMSII/Ge events is a natural one given that a) mirror dark matter predicts an event rate which is sharply falling with respect to recoil energy and b) that the two observed events are in the low energy region near threshold. Importantly this interpretation of the CDMSII events can be checked by on-going and future experiments, and we hereby predict that the bulk of the events will be in the $E_R \stackrel{<}{\sim} 18$ keV region. | [
-0.014463969506323001,
-0.010100536979734,
-0.021345801651477002,
-0.013925273902714001,
-0.018207902088761,
0.020834041759371,
-0.037708673626184006,
-0.008295907638967,
-0.021642085164785,
-0.016632217913866,
0.013884872198104001,
0.026247929781675002,
-0.020416552200913003,
0.0069020339... |
1001.0097 | When the Moon was formed it was much closer to the Earth than it is today. It just needed about 20 days then to go around the Earth. Now it takes the Moon 29.5 days to make one revolution. In order to follow the conservation of angular momentum the Moon had to either move closer to the Earth or recede from Earth. The data from the Lunar Laser Ranging Experiment confirms it to be moving away and the velocity of recession of the Moon have been found to be 3.8 cm/year. This rate is not constant though. At present the Moon's orbit has a radius of 384,000km. But what is not yet known to all is that the orbital motion of the moon is actually a spiral motion. The moon is spiralling out and a very simple mathematical equation can describe the actual spiral motion of the Moon. The generalisation of this differential equation is the basic aim of this paper here. | [
0.0048299715854220006,
0.010497731156647,
0.022188674658536002,
-0.0034685670398170005,
-0.021262031048536002,
-0.027926249429583,
-0.030134961009025,
0.0011717918096110001,
-0.006378609221428,
-0.020259223878383,
0.009025256149470001,
0.022937605157494,
0.006223110482096001,
0.01463589351... |
1001.0098 | We study the dynamics of the relative phase of a bilayer of two-dimensional superfluids after the two superfluids have been decoupled. We find that on short time scales the relative phase shows "light cone" like dynamics and creates a metastable superfluid state, which can be supercritical. We also demonstrate similar light cone dynamics for the transverse field Ising model. On longer time scales the supercritical state relaxes to a disordered state due to dynamical vortex unbinding. This scenario of dynamically suppressed vortex proliferation constitutes a reverse-Kibble-Zurek effect. We study this effect both numerically using truncated Wigner approximation and analytically within a newly suggested time dependent renormalization group approach (RG). In particular, within RG we show that there are two possible fixed points for the real time evolution corresponding to the superfluid and normal steady states. So depending on the initial conditions and the microscopic parameters of the Hamiltonian the system undergoes a non-equilibrium phase transition of the Kosterlitz-Thouless type. The time scales for the vortex unbinding near the critical point are exponentially divergent, similar to the equilibrium case. | [
-0.009136757813394,
0.0034314133226870003,
0.009150435216724,
0.011147391982376001,
0.007256062701344001,
0.01659114845097,
-0.015537959523499002,
-0.000874095712788,
-0.031103273853659002,
-0.036437608301639,
0.020420927554368,
0.011974897235631,
-0.000840328691992,
0.012617752887308,
0... |
1001.0099 | Simultaneous imaging of the piezoresponse phase, amplitude and bare surface topography of displacive ferroelectric thin films by scanning probe microscopy directly shows the nature of domain wall pinning and its relation to morphological disorder. Strong and stable pinning of walls occurs at grain boundaries while weak and unstable pinning occurs within the grains. The results show that polarization reversal consists of both nucleation of domains and spreading of domain walls, the latter being the dominant process in multi-grain regions. A characteristic single-grain switching in faceted grains is observed as the motion of a single domain wall parallel to one of the facets. | [
-0.007293413858860001,
0.012155690230429,
0.021355878561735,
-0.01062345970422,
-0.020320773124694002,
0.027784433215856,
-0.018645534291863,
-0.007940355688333001,
-0.016806859523057,
-0.045953273773193005,
0.024556536227464003,
0.013429143466055001,
0.027280500158667002,
0.02286767959594... |
1001.0101 | Using the exact solutions for the Dirac neutrino wave function in presence of matter we study the spin light mode in the process of neutrino transition from initial heavier to final lighter state. The spin light is emitted due to the neutrino nonzero transitional magnetic moment. | [
0.020329479128122,
-0.00026726108626400004,
0.0032180503476410003,
0.0064058685675260005,
-0.005952385254204001,
0.008135822601616001,
-0.009560095146298,
-0.016123842447996,
-0.027759883552789,
-0.026483412832021002,
0.012126473709940001,
0.014390530064702001,
-0.010144584812223,
0.007531... |
1001.0102 | In order to study an intrinsic chemical potential jump between the hole- and electron-doped high-Tc superconductors, we have performed core-level X-ray photoemission spectroscopy (XPS) measurements of Y0.38La0.62Ba1.74La0.26Cu3Oy (YLBLCO), into which one can dope both holes and electrons with maintaining the same crystal structure. Unlike the case between the hole-doped system La_2-xSrxCuO4 and the electron-doped system Nd_2-xCexCuO4, we have estimated the true chemical potential jump between the hole- and electron-doped YLBLCO to be ~0.8 eV, which is much smaller than the optical gaps of 1.4-1.7 eV reported for the parent insulating compounds. We attribute the reduced jump to the indirect nature of the charge-excitation gap as well as to the polaronic nature of the doped carriers. | [
-0.005511609371751,
0.001860252581536,
0.024421084672212,
-0.028333855792880003,
-0.019658299162983003,
0.022653592750430003,
-0.016973327845335,
-0.030060870572924003,
-0.034864135086536005,
-0.011326796375215002,
0.014571697451174,
0.017040790989995003,
0.0006324521382330001,
0.008574364... |
1001.0103 | The latest determination of the extragalactic gamma-ray background (EGRB) radiation by Fermi is compared with the theoretical prediction of the blazar component by Inoue & Totani (2009; hereafter IT09). The Fermi EGRB spectrum is in excellent agreement with IT09, indicating that blazars are the dominant component of the EGRB, and contributions from any other sources (e.g., dark matter annihilations) are minor. It also indicates that the blazar SED (spectral energy distribution) sequence taken into account in IT09 is a valid description of mean blazar SEDs. The possible contribution of MeV blazars to the EGRB in the MeV band is also discussed. In five total years of observations, we predict that Fermi will detect ~1200 blazars all sky down to the corresponding sensitivity limit. We also address the detectability of the highest-redshift blazars. Updating our model with regard to high-redshift evolution based on SDSS quasar data, we show that Fermi may find some blazars up to z~6 during the five-year survey. Such blazars could provide a new probe of early star and galaxy formation through GeV spectral attenuation signatures induced by high-redshift UV background radiation. | [
-0.0015506914351130002,
-0.024661762639880003,
-0.022612269967794002,
-0.029534393921494,
-0.004550278186798,
0.016667388379573,
-0.039659697562456006,
-0.025068946182727002,
-0.030945964157581003,
-0.007146074436604001,
0.000799522211309,
0.015011507086455001,
-0.007112142629921001,
0.019... |
1001.0104 | For the first time the process-independent parameter of double parton scattering, $\sigma_{\rm eff}^{\rm exp}$, has been measured newly in the D0 experiment at the three different resolution scales.If we interpret the measurement as a decrease of the effective cross section with a growth of the resolution scale it can indicate the QCD evolution of double parton distributions. | [
-0.019882660359144003,
0.007366694509983,
-0.008687711320817,
-0.03890261799097,
-0.020421851426362003,
0.006635416764765,
-0.016270082443952002,
0.0023572747595600003,
-0.043836213648319,
-0.024411862716078002,
0.029574615880846002,
0.012846221216022,
0.001957936678081,
0.0008075224468480... |
1001.0105 | The strong interaction between electrons reveals the duality of the itinerancy and the localization of quasiparticles. The physical phenomena corresponding to each component of the duality could be realized and coexist within the category of the uncertainty principle of the carrier dynamics, which can be a strong reason of the complexity appearing in the strongly correlated system. A possible mechanism for the high-temperature superconductivity is proposed on the basis of the interplay between the renormalized expectation quantities of both parts. | [
0.009998625144362,
0.009698666632175001,
0.012271646410226001,
-0.020343869924545,
-0.015971137210726002,
0.009358713403344,
-0.027782846242189,
-0.01723762974143,
-0.037354864180088,
-0.0296225938946,
0.012378297746181,
0.015104589983820001,
-0.0012248315615570001,
0.025196535512804003,
... |
1001.0106 | The structural profiles and electronic properties of pentacene (C$_{22}$H$_{14}$) multilayers on Ag(111) surface has been studied within the density functional theory (DFT) framework. We have performed first-principle total energy calculations based on the projector augmented wave (PAW) method to investigate the initial growth patterns of pentacene (Pn) on Ag(111) surface. In its bulk phase, pentacene crystallizes with a triclinic symmetry while a thin film phase having an orthorhombic unit cell is energetically less favorable by 0.12 eV/cell. Pentacene prefers to stay planar on Ag(111) surface and aligns perfectly along silver rows without any molecular deformation at a height of 3.9 {\AA}. At one monolayer (ML) coverage the separation between the molecular layer and the surface plane extends to 4.1 {\AA} due to intermolecular interactions weakening surface--pentacene attraction. While the first ML remains flat, the molecules on a second full pentacene layer deposited on the surface rearrange so that they become skewed with respect to each other. This adsorption mode is energetically more preferable than the one for which the molecules form a flat pentacene layer by an energy difference similar to that obtained for bulk and thin film phases. Moreover, as new layers added, pentacenes assemble to maintain this tilting for 3 and 4 ML similar to its bulk phase while the contact layer always remains planar. Therefore, our calculations indicate bulk-like initial stages for the growth pattern. | [
-0.004579776898026001,
0.000159367235028,
0.000489142839796,
-0.030025202780961,
0.006209697108715001,
0.028078630566596003,
-0.009339544922113,
-0.020612329244613002,
-0.017039168626070002,
-0.015532576479017,
0.003986472263932,
0.03077183291316,
-0.009179552085697,
0.009039559401571001,
... |
1001.0107 | The high repair cost of (n,k) Maximum Distance Separable (MDS) erasure codes has recently motivated a new class of codes, called Regenerating Codes, that optimally trade off storage cost for repair bandwidth. On one end of this spectrum of Regenerating Codes are Minimum Storage Regenerating (MSR) codes that can match the minimum storage cost of MDS codes while also significantly reducing repair bandwidth. In this paper, we describe Exact-MSR codes which allow for any failed nodes (whether they are systematic or parity nodes) to be regenerated exactly rather than only functionally or information-equivalently. We show that Exact-MSR codes come with no loss of optimality with respect to random-network-coding based MSR codes (matching the cutset-based lower bound on repair bandwidth) for the cases of: (a) k/n <= 1/2; and (b) k <= 3. Our constructive approach is based on interference alignment techniques, and, unlike the previous class of random-network-coding based approaches, we provide explicit and deterministic coding schemes that require a finite-field size of at most 2(n-k). | [
-0.017726402729749003,
0.016081972047686,
-0.0038706827908750003,
-0.00021763880795300003,
-0.011037194170057002,
0.011134745553135001,
-0.007985242642462,
-0.009671480394899,
-0.017378006130456,
-0.016723021864891,
0.0034491231199350004,
0.043619215488433005,
-0.012214773334562001,
0.0145... |
1001.0108 | Surface waves on a thin metal filament are described in terms of quantum electrodynamics. The interaction of surface waves with a quantum oscillator is discussed in the dipole approximation. The increase in the spontaneous emission rate of the excited quantum oscillator, the so called Purcell factor, is evaluated to be as high as ten to the five times. | [
-0.006425260566174,
0.008219822309911001,
0.003094872459769,
-0.007257857359945,
-0.025780653581023,
0.014701473526656001,
-0.027757655829191003,
-0.011775773949921001,
-0.040734227746725006,
-0.015670072287321,
-0.0102034593001,
0.019265830516815,
-0.006547993980348001,
0.0329588986933230... |
1001.0109 | The formation mechanism of planetesimals in protoplanetary discs is hotly debated. Currently, the favoured model involves the accumulation of meter-sized objects within a turbulent disc, followed by a phase of gravitational instability. At best one can simulate a few million particles numerically as opposed to the several trillion meter-sized particles expected in a real protoplanetary disc. Therefore, single particles are often used as super-particles to represent a distribution of many smaller particles. It is assumed that small scale phenomena do not play a role and particle collisions are not modeled. The super-particle approximation can only be valid in a collisionless or strongly collisional system, however, in many recent numerical simulations this is not the case. In this work we present new results from numerical simulations of planetesimal formation via gravitational instability. A scaled system is studied that does not require the use of super-particles. We find that the scaled particles can be used to model the initial phases of clumping if the properties of the scaled particles are chosen such that all important timescales in the system are equivalent to what is expected in a real protoplanetary disc. Constraints are given for the number of particles needed in order to achieve numerical convergence. We compare this new method to the standard super-particle approach. We find that the super-particle approach produces unreliable results that depend on artifacts such as the gravitational softening in both the requirement for gravitational collapse and the resulting clump statistics. Our results show that short range interactions (collisions) have to be modelled properly. | [
-0.010922388173639,
0.009758526459336002,
-0.003532903501763,
-0.020054221153259003,
-0.0072310888208440005,
0.025536075234413,
-0.010571163147687001,
0.011046349070966001,
-0.025012681260704002,
-0.043634455651044006,
0.009193813428282,
0.017519894987344003,
-0.0076925014145670005,
0.0098... |
1001.0111 | This articles presents a simulation study of the applicability of the Rosenfeld entropy scaling to the systems which can not be approximated by effective hard spheres. Three systems are studied: Herzian spheres, Gauss Core Model and soft repulsive shoulder potential. These systems demonstrate the diffusion anomalies at low temperatures: the diffusion increases with increasing density or pressure. It is shown that for the first two systems which belong to the class of bounded potentials the Rosenfeld scaling formula is valid only in the infinite temperature limit where there are no anomalies. For the soft repulsive shoulder the scaling formula is valid already at sufficiently low temperatures, however, out of the anomaly range. | [
-0.004947294946759001,
0.006973526440560001,
0.010525430552661,
-0.03881038352847,
0.02339594066143,
0.029046073555946003,
-0.013947052881121,
-0.014495609328150002,
-0.040702901780605004,
-0.040346339344978006,
0.016278417780995,
0.034723635762929,
-0.0024376485962420004,
0.02387592755258... |
Subsets and Splits
No community queries yet
The top public SQL queries from the community will appear here once available.