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Suppose that you have an abstract for a scientific paper: using the @xmath0 extended linear sigma model with the ordinary ( pseudo)scalar and ( axial)vector mesons as well as a scalar glueball , we study the vacuum phenomenology of the scalar - isoscalar resonances @xmath1 and @xmath2 . we present here a solution , based only on the masses and not yet on decays , in which the resonances @xmath3 and @xmath4 are predominantly nonstrange and strange @xmath5 states respectively , and the resonance @xmath2 is predominantly a scalar glueball . . And you have already written the first three sentences of the full article: the experimental verification of many scalar - isoscalar resonances , @xmath6 , up to the energy of @xmath7 gev @xcite reenforced the idea that the scalar glueball lies among them . however , the remaining open question is which of these scalars - isoscalars is predominantly the glueball.in this paper we address this issue by studying the vacuum phenomenology of scalar - isoscalar states within the framework of the so called extended linear sigma model ( elsm ) @xcite . our numerical calculations of the effective lagrangian ( [ lagrangian ] ) are explicitly done in the case of three quark flavours . for @xmath8 two scalar - isoscalar @xmath5 states. Please generate the next two sentences of the article

exist , the nonstrange @xmath9 and the strange @xmath10 mesons . the scalar glueball @xmath11 is implemented in the elsm from the very beginning as the fluctuation of the dilaton field .

Suppose that you have an abstract for a scientific paper: we consider the problem of preparing specific encoded resource states for the toric code by local , time - independent interactions with a memoryless environment . we propose a construction of such a dissipative encoder which converts product states to topologically ordered ones while preserving logical information . the corresponding liouvillian is made up of four - local lindblad operators . for a qubit lattice of size @xmath0 , we show that this process prepares encoded states in time @xmath1 , which is optimal . this scaling compares favorably with known local unitary encoders for the toric code which take time of order @xmath2 and require active time - dependent control . . And you have already written the first three sentences of the full article: dissipation , while generally seen as detrimental for quantum computers , can nevertheless be a useful resource if suitably engineered . appropriately chosen system - bath couplings can result in a non - equilibrium dynamics where initial states converge towards some dynamical steady state . this kind of ` quantum reservoir engineering ' has been proposed as a viable approach towards the experimental preparation of interesting many - body states @xcite . remarkable examples include the preparation of pure states with long - range order in bose - einstein - condensates @xcite , photonic arrays @xcite , as well as topologically ordered states @xcite .. Please generate the next two sentences of the article

more generally , verstraete et al . @xcite argued that , at least in principle , an arbitrary quantum computation can be realized by dissipation .

Suppose that you have an abstract for a scientific paper: we revisit the power spectrum analysis of the complete sample of the two degree field ( 2df ) qso redshift ( 2qz ) survey , as a complementary test of the work by outram et al . ( 2003 ) . a power spectrum consistent with that of the 2qz group is obtained . differently from their approach , fitting of the power spectrum is investigated incorporating the nonlinear effects , the geometric distortion and the light - cone effect . it is shown that the qso power spectrum is consistent with the @xmath0 cold dark matter ( cdm ) model with the matter density parameter @xmath1 . our constraint on the density parameter is rather weaker than that of the 2qz group . we also show that the constraint slightly depends on the equation of state parameter @xmath2 of the dark energy . the constraint on @xmath2 from the qso power spectrum is demonstrated , though it is not very tight . . And you have already written the first three sentences of the full article: the 2df qso redshift ( 2qz ) survey has established that the qso sample is a useful probe of cosmological models as a tracer of the large scale distribution of mass ( croom , et al . 2001 ; , hoyle , et al . 2002 ) . in general ,. Please generate the next two sentences of the article

constraints on cosmological parameters from qso sample are not very tight . however , the cosmological parameters estimated from the qso sample have a unique implication for cosmology ( outram , et al . 2003 ; yamamoto 2003a ) .

Suppose that you have an abstract for a scientific paper: universal ( pointwise uniform and time shifted ) truncation error upper bounds are presented in whittaker kotelnikov shannon ( wks ) sampling restoration sum for bernstein function class @xmath0 @xmath1 when the sampled functions decay rate is unknown . the case of multidimensional irregular sampling is discussed . whittaker kotelnikov shannon sampling restoration formula ; approximation / interpolation error level ; nikolski placherel plya inequality ; truncation error upper bound ; irregular sampling ; multidimensional sampling primary 94a20 , 26d15 ; secondary 30d15 , 41a05 . And you have already written the first three sentences of the full article: the classical wks sampling theorem has been extended to the case of nonuniform sampling by numerous authors . for detailed information on the theory and its numerous applications , we refer to the book @xcite . most known irregular sampling results deal with paley wiener functions which have @xmath2 restrictions on the real line .. Please generate the next two sentences of the article

it seems that the best known nonuniform wks sampling results for entire functions in @xmath3spaces were given in @xcite . there are no multidimensional @xmath3wks sampling theorems with precise truncation error estimates in open literature

Suppose that you have an abstract for a scientific paper: the characteristics of the electron - photon showers initiated by 2 to 10 gev electrons aligned along the @xmath0 - axis of tungsten crystals are compared with those for the amorphous tungsten . in this energy range , as known , the positron yield at the optimal target thicknesses is larger in a crystal case only by several percent . however , the amount of the energy deposition in a crystal turns out to be considerably ( by 20 - 50@xmath1 ) lower than in an amorphous target providing the same positron yield , while the peak energy - deposition density is approximately of the same magnitude in the both cases . + + pacs numbers : 07.77.ka , 12.20.ds , 03.65.sq + . And you have already written the first three sentences of the full article: the formation of electromagnetic showers in aligned single crystals was actively studied during the last decade . the first experimental investigation of such showers has been performed in @xcite at very high energy of incident electrons . corresponding theoretical studies were started with @xcite where an analytic solution of the problem was obtained , assuming that energies of all charged particles and photons involved are very high .. Please generate the next two sentences of the article

this limitation was surmounted in @xcite by suggesting a specific form of the radiation spectrum at axial alignment and performing corresponding simulations . using this approach , the results of @xcite for ge crystal had been reproduced in@xcite .

Suppose that you have an abstract for a scientific paper: we have investigated the threshold of photodetachment of li@xmath0 leading to the formation of the residual li atom in the @xmath1 state . the excited residual atom was selectively photoionized via an intermediate rydberg state and the resulting li@xmath2 ion was detected . a collinear laser - ion beam geometry enabled both high resolution and sensitivity to be attained . we have demonstrated the potential of this state selective photodetachment spectroscopic method by improving the accuracy of li electron affinity measurements an order of magnitude . from a fit to the wigner law in the threshold region , we obtained a li electron affinity of @xmath3 ev . . And you have already written the first three sentences of the full article: the four - electron li@xmath0 ion is interesting because of the significant role played by electron correlation in the binding of the outermost electron in this weakly bound system . the major contribution to the correlation energy arises from the interaction of the two valence electrons . beyond the three - body h@xmath0 system , the li@xmath0 ion is most tractable to theory . in the frozen core approximation , for example. Please generate the next two sentences of the article

, the li@xmath0 ion becomes an effective three - body system consisting of a pair of highly correlated electrons interacting weakly with an inert core . such a model lends itself well to semi - empirical model potential calculations in which the potential experienced by the valence electrons is obtained via spectral information on the eigenvalue spectrum of the li atom .

Suppose that you have an abstract for a scientific paper: the recently detected linear polarization in the optical lightcurve of grb 990510 renewed the interest on how polarization can be produced in gamma ray burst fireballs . here we present a model based on the assumption that we are seeing a collimated fireball , observed slightly off axis . this introduces some degree of anisotropy , and makes it possible to observe a linearly polarized flux even if the magnetic field is completely tangled in the plane orthogonal to the line of sight . we construct the lightcurve of the polarization flux , showing that it is always characterized by two maxima , with the polarization position angle changing by @xmath0 between the first and the second maximum . the very same geometry here assumed implies that the total flux initially decays in time as a power law , but gradually steepens as the bulk lorentz factor of the fireball decreases . # 1#1 gamma rays : bursts polarization radiation mechanisms : non thermal . And you have already written the first three sentences of the full article: it is now widely believed that the afterglow emission of gamma ray bursts is due to the deceleration of the relativistic fireball in the circum burst matter ( for reviews see piran 1999 ; 1999 ) . this produces a shock that accelerates electrons to random relativistic energies and probably enhances the magnetic field , leading to the production of synchrotron emission .. Please generate the next two sentences of the article

if the magnetic field is completely tangled over the entire emission seen by the observer , the resulting synchrotron emission is unpolarized . on the other hand a very high degree of linear polarization can be expected if a fraction of the magnetic field is well ordered , reaching 6070% in the case of a completely ordered field .

Suppose that you have an abstract for a scientific paper: we report the results of extensive dynamical cluster approximation calculations , based on a quantum monte carlo solver , for the two - dimensional kondo lattice model . our particular cluster implementation renders possible the simulation of spontaneous antiferromagnetic symmetry breaking . by explicitly computing the single - particle spectral function both in the paramagnetic and antiferromagnetic phases , we follow the evolution of the fermi surface across this magnetic transition . the results , computed for clusters up to @xmath0 orbitals , show clear evidence for the existence of three distinct fermi surface topologies . the transition from the paramagnetic metallic phase to the antiferromagnetic metal is continuous ; kondo screening does not break down and we observe a back - folding of the paramagnetic heavy fermion band . within the antiferromagnetic phase and when the ordered moment becomes _ large _ the fermi surface evolves to one which is adiabatically connected to a fermi surface where the local moments are frozen in an antiferromagnetic order . . And you have already written the first three sentences of the full article: heavy - fermion systems @xcite are characterized by a hierarchy of distinctive energy scales @xcite . the kondo scale , @xmath1 with bandwidth @xmath2 and superexchange @xmath3 , marks the screening of local magnetic moments . this screening is a many - body effect which entangles the spins of the conduction electrons and local moments @xcite . below the coherence temperature , which is believed to track the kondo scale @xcite , the paramagnetic ( pm ) heavy - fermion liquid. Please generate the next two sentences of the article

@xcite emerges and corresponds to a coherent , bloch like , superposition of the screening clouds of the individual magnetic moments . even in the kondo limit , where charge fluctuations of the impurity spins are completely suppressed , this paramagnetic state is characterized by a large fermi surface with luttinger volume including both the magnetic moments and conduction electrons @xcite .

Suppose that you have an abstract for a scientific paper: in this paper , a computation of the input - redundancy weight enumerator is presented . this is used to improve the theoretical approximation of the information bit and symbol error rate , in terms of the channel bit - error rate , in a block transmission through a discrete memoryless channel . since a bounded distance reproducing encoder is assumed , the computation of the here - called false positive ( a decoding failure with no information - symbol error ) is provided . as a consequence , a new performance analysis of an mds code is proposed . lobillo , navarro and gmez - torrecillas mds code , bit - error rate ( ber ) , block error - correcting code , information bit error rate ( iber ) , false positive . . And you have already written the first three sentences of the full article: challenge when determining the performance of a block error - correcting code is to measure its bit - error rate ( ber ) , which quantifies the reliability of the system . in practice , the ber estimation for a single code is simple , just send data and divide the errors committed among the total number of bits . however , it would be too costly and time - consuming if a comparative between several codes is required .. Please generate the next two sentences of the article

mathematical software packages for encoding and decoding are very limited and restricted to specific codes and simulations would consume a huge amount of time when dealing with low bit - error rates . for this reason , a theoretical approach to the measurement of the ber is proposed by several authors in the literature , see for instance @xcite .

Suppose that you have an abstract for a scientific paper: recently observed anomalies in the @xmath0 decay and the like - sign dimuon asymmetry @xmath1 hint at possible new physics ( np ) in the @xmath2 mixing . we parameterize the np with four model - independent quantities : the magnitudes and phases of the dispersive part @xmath3 and the absorptive part @xmath4 of the np contribution to the effective hamiltonian . we constrain these parameters using the four observables @xmath5 , @xmath6 , the mixing phase @xmath7 , and @xmath1 . our quantitative fit indicates that the np should contribute a significant dispersive as well as absorptive part . in fact , models that do not contribute a new absorptive part are disfavored at more than 99% confidence level . we extend this formalism to include cpt violation , and show that cpt violation by itself , or even in presence of cpt - conserving new physics without an absorptive part , helps only marginally in the simultaneous resolution of these anomalies . the np absorptive contribution to @xmath2 mixing therefore seems to be essential , and would imply a large branching fraction for channels like @xmath8 . . And you have already written the first three sentences of the full article: the cabibbo - kobayashi - maskawa ( ckm ) paradigm of quark mixing in the standard model ( sm ) is yet to be accurately tested in the @xmath2 sector , and it is quite possible that the np can affect the @xmath2 system while keeping the @xmath9 system untouched . indeed , for most of the flavor - dependent np models , the couplings relevant for the second and third generations of sm fermions are much less constrained than those for the first generation fermions , allowing the np to play a significant role in the @xmath2 mixing , in principle . over the last few years , the tevatron experiments cdf and d , and to a smaller extent the b factories belle and babar , have provided a lot of data on the @xmath10 meson , most of which are consistent with the sm . there are some measurements , though , which show a significant deviation from the sm expectations , and hence point towards new physics ( np ) .. Please generate the next two sentences of the article

the major ones among these are the following . ( i ) measurements in the decay mode @xmath0 yield a large cp - violating phase @xmath11 @xcite .

Suppose that you have an abstract for a scientific paper: we examine the question of how well the physical properties of clumps in turbulent molecular clouds can be determined by measurements of observed clump structures . to do this , we compare simulated observations of three - dimensional numerical models of isothermal , magnetized , supersonic turbulence to the actual physical structure of the models . we begin by determining how changing the parameters of the turbulence changes the structure of the simulations . stronger driving produces greater density fluctuations , and longer wavelength driving produces larger structures . magnetic fields have a less pronounced effect on structure , and one that is not monotonic with field strength . aligned structures are seen only with low - density tracers , and when the intensity of the field is large . comparing different regions with the same tracers ( or conversely , the same region with different tracers ) can give information about the physical conditions of the region . in particular , different density tracers can help determine the size of the density fluctuations and thus the strength of the driving . nevertheless , velocity superposition of multiple physical clumps can fully obscure the physical properties of those clumps , and short wavelength ( compared to the size of the region under analysis ) driving worsens this effect . we then compare larson s relationships and mass spectra in physical and observational space for the same structure dataset . we confirm previous claims that the mean density - size relationship is an observational artifact due to limited dynamical range in column density : it is the inevitable consequence presence of a lower cutoff in column density . the velocity dispersion - size relationship , on the other hand , is reproduced in both physical and observed clumps , although with substantial scatter in the derived slope , consistent with observations . finally , we compute the mass spectra for the models and compare them to mass spectra derived from simulated.... And you have already written the first three sentences of the full article: this paper tries to understand whether concentrations of emission in observations of position - velocity space represent real clumps of gas in molecular clouds ; whether the properties inferred for the observed objects describe the actual clouds ; and what we can say about the mechanisms that drive interstellar turbulence by observing molecular clouds with different tracers . several papers have tried to address these points before . @xcite show that , in a galactic disk model , gas complexes in a longitude - velocity diagram do not necessarily correspond to real complexes .. Please generate the next two sentences of the article

more recently , based on numerical simulations , @xcite showed that observed clumps frequently come from the superposition of several physically disconnected regions in the line of sight at the same radial velocity ( see also @xcite , ) but not necessarily at the same three - dimensional velocity . moreover , the morphology seen in observed position - position - velocity maps seems to be more representative of the spatial distribution of the velocity field in the line of sight than of the distribution of the density field , as has been shown in 3d numerical simulations by @xcite .

Suppose that you have an abstract for a scientific paper: global second - order phase transitions are expected to produce scale - invariant gravitational wave spectra . in this manuscript we explore the dynamics of a symmetry - breaking phase transition using lattice simulations . we explicitly calculate the stochastic gravitational wave background produced during the transition and subsequent self - ordering phase . we comment on this signal as it compares to the scale - invariant spectrum produced during inflation . . And you have already written the first three sentences of the full article: a scale - invariant spectrum of gravitational radiation is a key prediction of inflation @xcite . measuring the ratio of the amplitude of gravitational radiation to the amplitude of density perturbations , @xmath0 , would be a direct probe of the inflationary energy scale . such a measurement has eluded observation in the cosmic microwave background ( cmb ) thus far @xcite and represents one of the key goals of future cmb observational missions @xcite . on the other hand , some authors have argued that phase transitions can mimic the scale - invariant inflationary signal @xcite . the mechanism through which this is accomplished is not trivial .. Please generate the next two sentences of the article

the phase transition itself is not the source . rather , energy is deposited into gravitational radiation via the self - ordering of fields as regions of spacetime become causally connected .

Suppose that you have an abstract for a scientific paper: driven by single photon detection requirements , the theory of arrays of off - on detectors has been developed and applied . however for a comprehensive characterization of nonclassicality one also needs phase sensitive properties . this missing link is introduced with the derived theory of phase sensitive click counting measurements . it unifies the balanced homodyne detection for high intensities with the click detection in the few photon regime . we formulate a hierarchy of nonlinear squeezing conditions to probe quantum effects beyond standard squeezing . imperfections stemming from fluctuations , detector efficiency , and dark count rates are considered . experimentally accessible sampling formulas are given . our theory paves the way towards novel applications of light in quantum metrology . . And you have already written the first three sentences of the full article: interference plays a crucial role for both quantum physics and classical wave theories . in quantum optics quantum interferences and superimposed electromagnetic field components occur simultaneously . therefore , a proper analysis and determination of the character of interference patterns is indispensable for separating classical wave phenomena from quantum effects .. Please generate the next two sentences of the article

as photons reflect the particle nature of the electromagnetic field , their generation and detection are of fundamental interest @xcite . in the low photon number regime , detectors are often based on avalanche photodiodes ( apd ) in the geiger mode . apds produce a `` click '' for any number of absorbed photons and remain silent otherwise , _

Suppose that you have an abstract for a scientific paper: we show that universality arguments , namely the svetitsky yaffe conjecture , allow one to obtain exact results on the critical behavior of @xmath0 @xmath1 gauge theory at the finite temperature deconfinement transition , through a mapping into the @xmath2 ising model . in particular , we consider the finite size scaling behavior of the plaquette operator , which can be mapped into the energy operator of the @xmath2 ising model . we obtain exact predictions for the dependence of the plaquette expectation value on the size and shape of the lattice and we compare them to monte carlo results , finding complete agreement . we discuss the application of this method to the computation of more general correlators of the plaquette operator at criticality , and its relevance to the study of the color flux tube structure . dftt 30/98 + dfcal - th 4/98 + june 1998 0.5 cm * critical behavior of @xmath0 @xmath1 gauge theory at finite temperature : exact results from universality * + 0.6 cm r. fiore@xmath3 , f. gliozzi@xmath4 and p. provero@xmath4 0.6 cm _ @xmath3 dipartimento di fisica , universit della calabria _ _ istituto nazionale di fisica nucleare , gruppo collegato di cosenza _ _ rende , i87030 cosenza , italy _ 0.2 cm _ @xmath4 dipartimento di fisica teorica delluniversit di torino _ _ istituto nazionale di fisica nucleare , sezione di torino _ _ via p.giuria 1 , i10125 torino , italy _ 0.6 cm .5 cm ' '' '' .3 cm @xmath5_work supported by the ministero italiano delluniversit e della ricerca scientifica e tecnologica _ . And you have already written the first three sentences of the full article: the idea of universality plays a major role in the modern understanding of critical phenomena . all the physical systems undergoing a continuous phase transition are believed to fall in a certain number of universality classes , depending on the dimensionality of the system and its symmetry group , but not on the details of the microscopic interactions ( as long as these are short ranged ) . all the systems in a given universality class display the same critical behavior , meaning that certain dimensionless quantities have the same value for all the physical systems in a given class .. Please generate the next two sentences of the article

critical indices and universal amplitude ratios are examples of these universal quantities . for gauge theories with a high temperature deconfinement transition , the universality hypothesis takes the form of the svetitsky yaffe conjecture , @xcite , which can be formulated as follows : suppose a @xmath6dimensional gauge theory with gauge group @xmath7 has a second order deconfinement transition at a certain temperature @xmath8 ; consider the @xmath9dimensional statistical model with global symmetry group coinciding with the center of the gauge group : if also this model displays a second order phase transition , then the two models belong to the same universality class .

Suppose that you have an abstract for a scientific paper: a spin - polarizing electron beam splitter is described which relies on an arrangement of linearly polarized laser waves of nonrelativistic intensity . an incident electron beam is first coherently scattered off a bichromatic laser field , splitting the beam into two portions , with electron spin and momentum being entangled . afterwards , the partial beams are coherently superposed in an interferometric setup formed by standing laser waves . as a result , the outgoing electron beam is separated into its spin components along the laser magnetic field , which is shown by both analytical and numerical solutions of pauli s equation . the proposed laser field configuration thus exerts the same effect on free electrons like an ordinary stern - gerlach magnet does on atoms . . And you have already written the first three sentences of the full article: spin - polarized electron beams are useful for a number of applications in various fields of physics @xcite . they are utilized , for example , to study magnetic properties in condensed matter systems @xcite , electron - exchange processes in atomic collisions @xcite , and the inner structure of the nucleon in deep - inelastic scattering . spin - polarized electron ( and positron ) beams can also enhance the sensitivity of high - energy physics experiments @xcite .. Please generate the next two sentences of the article

there are various methods to generate spin - polarized electrons @xcite . at first sight , the most straightforward way would be to split an electron beam into its spin components , just as a stern - gerlach setup does with a beam of atoms . however , for charged particles , the spin - separating mechanism in an inhomogeneous static magnetic field is hindered by the influence of the lorentz force . instead ,

Suppose that you have an abstract for a scientific paper: we present new observations of the cluster - lens abell 370 : a deep hst / wfpc2 f675w image and eso 3.6 m spectroscopy of faint galaxies . these observations shed new light on the statistical properties of faint lensed galaxies . in particular , we spectroscopically confirm the multiple image nature of the b2b3 gravitational pair ( @xcite ) , and determine a redshift of @xmath0 which is in very good agreement with earlier predictions . a refined mass model of the cluster core ( that includes cluster galaxy halos ) is presented , based on a number of newly identified multiple images . following bzecourt et al . ( 1998a ) , we combine the new cluster mass model with a spectrophotometric prescription for galaxy evolution to predict the arclets number counts and redshift distribution in the hst image . in particular , the ellipticity distribution of background sources is taken into account , in order to properly estimate the statistical number and redshift distribution of arclets . we show that the redshift distribution of arclets , and particularly its high redshift tail can be used as a strong constraint to disentangle different galaxy evolution scenarios . a hierarchical model which includes number density evolution is favored by our analysis . finally , we compute the depletion curves for the faint galaxy number counts and discuss their wavelength dependence . . And you have already written the first three sentences of the full article: thanks to gravitational amplification , galaxy clusters are a powerful tool to probe distant galaxies . indeed , one of the most distant galaxy detected is a gravitational arc at @xmath1=4.92 in the cluster cl1358 + 62 ( @xcite ) . other very distant lensed sources ( @xmath23 ) have been identified behind cl0939 + 4713 ( @xcite ) and a2390 ( @xcite , @xcite ) leading to important results on the formation history and evolution of galaxies at large redshift . determining the redshift of arcs and arclets is of great importance as it fixes the angular scales of the optical configuration , hence giving an absolute cluster mass estimate within the arc radius ( _ e.g. _ @xcite , @xcite ) . but. Please generate the next two sentences of the article

despite the cluster magnification , measuring arclets redshifts is a difficult observational task due to their low surface brightness ( @xcite , @xcite ) , and the lack of strong spectral features in the optical domain for galaxies with @xmath3 . accurate modeling of cluster potentials based on the analysis of multiple images and weak shear distortions has shown that cluster mass distributions are best described by the sum of a smooth and large scale component ( the cluster ) and the contribution of cluster galaxy halos ( @xcite , @xcite , @xcite ) . for

Suppose that you have an abstract for a scientific paper: why sex evolved and it prevails in nature remains one of the great puzzles of evolution . most biologists would explain that it promotes genetic variability , however this explanation suffers from several difficulties . what advantages might sex confer ? the present communication aims at certain investigations related to this question , in this way we introduce sexual recombination on the htzel model ( with males and females ) and we compare these results with those from asexual reproduction without recombination . * sex and recombination in the htzel aging model * a.o . sousa _ institute for theoretical physics , cologne university , d-50937 k " oln , germany _ * keywords*:population dynamics ; aging ; monte carlo simulations ; evolution ; recombination . And you have already written the first three sentences of the full article: sex , which involves the alternation of meiosis and gamete fusion , is a rather inefficient means of self - propagation as compared to asexual reproduction , where offspring stem only from a mitotically produced cells . one of the most common reasons used to explain the origin and maintenance of sex is its ability to reduce the mutation load if consecutive mutations lead to an increasing decline in relative fitness , although it is not clear _ a priori _ that the heritable variance in fitness is significantly increased by sex . despite decades of developing theoretical models to explain why sex is such a widespread phenomenon and how sexual reproduction may confer advantages that outweigh its disadvantages , until now no such general clear advantage has been found . investigations of evolutionary problems by physicists have in fact boomed in the last few years . since computer simulations of natural systems can provide much insight into their fundamental mechanisms , they can be used to test theoretical ideas that could be otherwise viewed as too vague to deserve the status of scientific knowledge @xcite . in this way , many computer models in population dynamics have been proposed to investigate the evolution of sex and its justification , as well as the comparison between sexual and asexual reproduction , for instance , the redfield model @xcite , the penna bit - string model @xcite , a genomic bit - string model without aging @xcite and stauffer model @xcite . of particular interest here is the heumann - htzel model @xcite , which originally simulated the evolution of asexual population , composed of haploid individuals , without recombination .. Please generate the next two sentences of the article

thus now we introduce the recombination in this model , in order to find out if the sexual reproduction ( with males and females ) can produce better results than the simple asexual reproduction @xcite . in the next section , we describe the standard and the modified heumann - htzel model , in section 3 , we present our results and in section 4 , our conclusions .

Suppose that you have an abstract for a scientific paper: we present a review on the explanation of the rhic hbt puzzle by a granular pion - emitting source of quark - gluon plasma droplets . the evolution of the droplet is described by relativistic hydrodynamics with an equation of state suggested by lattice gauge results . the granular source evolution is obtained by superposing all of the evolutions of individual droplets . pions are assumed to be emitted thermally from the droplets at the freeze - out configuration characterized by a freeze - out temperature @xmath0 . we find that the average particle emission time scales with the initial radius of the droplet . pions will be emitted earlier if the droplet radius is smaller . an earlier emission time will lead to a smaller extracted hbt radius @xmath1 , while the extracted hbt radius @xmath2 is determined by the scale of the distribution of the droplet centers . however , a collective expansion of the droplets can further decrease @xmath1 . as a result , the value of @xmath3 can be close to , or even less than 1 for the granular source of qgp droplets . . And you have already written the first three sentences of the full article: hbt ( hanbury - brown - twiss ) interferometry is an indispensable tool to study the space - time structure of the particle - emitting source produced in high energy heavy ion collisions@xcite . the experimental pion hbt measurements at rhic give the ratio of @xmath4@xcite , which is much smaller than many earlier theoretical expectations . such a discrepancy between theory and experiment is referred to as the rhic hbt puzzle@xcite . on the other hand ,. Please generate the next two sentences of the article

hydrodynamical calculations give reasonably good descriptions of the elliptic flow , which has been considered as an evidence for a strongly - coupled quark - gluon plasma@xcite . the resolution of the hbt puzzle is important in finding out why traditional hydrodynamics succeed in explaining the elliptic flow but fails in explaining the hbt radii .

Suppose that you have an abstract for a scientific paper: we determine the optimal angle of release in shot put . the simplest model - mostly used in textbooks - gives a value of @xmath0 , while measurements of top athletes cluster around @xmath1 . including simply the height of the athlete the theory prediction goes down to about @xmath2 for typical parameters of top athletes . taking further the correlations of the initial velocity of the shot , the angle of release and the height of release into account we predict values around @xmath1 , which coincide perfectly with the measurements . do - th 10/12 . And you have already written the first three sentences of the full article: we investigate different effects contributing to the determination of the optimal angle of release at shot put . standard text - book wisdom tells us that the optimal angle is @xmath0 , while measurements of world - class athletes @xcite typically give values of below @xmath3 . in table [ tab1 ] we show the data from the olympic games in 1972 given by kuhlow ( 1975 ) @xcite with an average angle of release of about @xmath4 .. Please generate the next two sentences of the article

the measurements of dessureault ( 1978 ) @xcite , mccoy et al . ( 1984 ) @xcite , susanaka and stepanek ( 1988 ) @xcite , bartonietz and borgstrm ( 1995 ) @xcite , tsirakos et al .

Suppose that you have an abstract for a scientific paper: aggregation of a large number of responsive loads presents great power flexibility for demand response . an effective control and coordination scheme of flexible loads requires an accurate and tractable model that captures their aggregate flexibility . this paper proposes a novel approach to extract the aggregate flexibility of deferrable loads with heterogeneous parameters using polytopic projection approximation . first , an exact characterization of their aggregate flexibility is derived analytically , which in general contains exponentially many inequality constraints with respect to the number of loads . in order to have a tractable solution , we develop a numerical algorithm that gives a sufficient approximation of the exact aggregate flexibility . geometrically , the flexibility of each individual load is a polytope , and their aggregation is the minkowski sum of these polytopes . our method originates from an alternative interpretation of the minkowski sum as projection . the aggregate flexibility can be viewed as the projection of a high - dimensional polytope onto the subspace representing the aggregate power . we formulate a robust optimization problem to optimally approximate the polytopic projection with respect to the homothet of a given polytope . to enable efficient and parallel computation of the aggregate flexibility for a large number of loads , a muti - stage aggregation strategy is proposed . the scheduling policy for individual loads is also derived . finally , an energy arbitrage problem is solved to demonstrate the effectiveness of the proposed method . . And you have already written the first three sentences of the full article: the future power system will be modernized with advanced metering infrastructure , bilateral information communication network , and intelligent monitoring and control system to enable a smarter operation @xcite . the transformation to the smart grid is expected to facilitate the deep integration of renewable energy , improve the reliability and stability of the power transmission and distribution system , and increase the efficiency of power generation and energy consumption . demand response program is a core subsystem of the smart grid , which can be employed as a resource option for system operators and planners to balance the power supply and demand .. Please generate the next two sentences of the article

the demand side control of responsive loads has attracted considerable attention in recent years @xcite . an intelligent load control scheme should deliver a reliable power resource to the grid , while maintaining a satisfactory level of power usage to the end - user .

Suppose that you have an abstract for a scientific paper: homogeneous and isotropic models are studied in the jordan frame of the second order gravity theory . the late time evolution of the models is analysed with the methods of the dynamical systems . the normal form of the dynamical system has periodic solutions for a large set of initial conditions . this implies that an initially expanding closed isotropic universe may exhibit oscillatory behaviour . . And you have already written the first three sentences of the full article: quadratic gravitational lagrangians were proposed shortly after the formulation of general relativity ( gr ) as alternatives to einstein s theory . gravity modifications in the form of higher - order curvature invariants in the lagrangian are generally known as higher - order gravity ( hog ) theories . they arise in string - theoretic considerations , e.g. , brane models with gauss - bonett terms @xcite or models with a scalar field coupled to the gauss - bonett invariant @xcite ( see @xcite for a review ) and generally involve linear combinations of all possible second order invariants that can be formed from the riemann , ricci and scalar curvatures . a quarter of a century ago there was a resurgence of interest in such theories in an effort to explain inflation .. Please generate the next two sentences of the article

the reasons for considering hog theories were multiple . firstly , it was hoped that higher order lagrangians would create a first approximation to quantum gravity , due to their better renormalisation properties than gr @xcite .

Suppose that you have an abstract for a scientific paper: in this paper , we have studied @xmath0 gravity as an arbitrary function of curvature and torsion scalars in friedmann lematre robertson walker ( flrw ) background . then , we have considered interacting model between @xmath0 gravity and modified chaplygin gas . the novelty of this model is that the universe includes both cases curvature and torsion , and one dominated by a chaplygin gas . in order to calculate cosmological solutions , we obtained friedmann equations and also equation of state ( eos ) parameter of dark energy . by employing interacting model we considered the total energy density and the total pressure of universe as the combination of components of dark energy and chaplygin gas . subsequently , we reconstructed the model by an origin of a scalar field entitled quintessence model with a field potential . the field potential has been calculated in terms of free parameters of @xmath0 gravity and modified chaplygin gas . in what follows , we used a parametrization , and the cosmological parameters have been written in terms of redshift @xmath1 . next , we plotted cosmological parameters with respect to three variable of cosmic time , redshift @xmath1 and @xmath2-folding number @xmath3 , and the figures showed us an accelerated expansion of universe . also , we have described the scenario in three status early time , late time and future time by @xmath2-folding number . finally , the stability of scenario has been investigated by a useful function named sound speed , and the graph of sound speed versus @xmath2-folding number has been showed us that there is the stability in late time . . And you have already written the first three sentences of the full article: as we know , the universe is expanding and this expanding is undergoing an accelerating phase . this issue discovered in type ia supernova @xcite , associated with large scale structure @xcite and cosmic microwave background @xcite . it is noteworthy that the accelerated expansion of the universe is created from a mysterious energy called dark energy , which is about two thirds the total energy of universe . by using the einstein field equation , the accelerated expansion described by a small positive cosmological constant .. Please generate the next two sentences of the article

also this discovery demonstrates that geometry of the universe is very close to flat space @xcite . various candidates have been introduced to describe dark energy scenario , so that the universe dominates with a perfect fluid by a negative pressure and the eos parameter which is less than @xmath4 , the so - called phantom phase .

Suppose that you have an abstract for a scientific paper: we report on a search for differential shifts between electronic and vibronic transitions in carbon - rich white dwarfs bpm 27606 and procyon b. the absence of differential shifts within the spectral resolution and taking into account systematic effects such as space motion and pressure shifts allows us to set the first upper bound of astrophysical origin on the coupling between the higgs field and the kreschmann curvature invariant . our analysis provides the basis for a more general methodology to derive bounds to the coupling of long - range scalar fields to curvature invariants in an astrophysical setting complementary to the ones available from high - energy physics or table - top experiments . . And you have already written the first three sentences of the full article: the recent discovery at the large hadron collider ( lhc ) of a resonance at 125 gev compatible with the expectations for the higgs particle @xcite represents a major step towards understanding the origin of the mass of fundamental particles . eventually , this should also affect the other subfield in which mass has a pivotal role , _ i.e. _ gravitation .. Please generate the next two sentences of the article

this is particularly relevant in models in which the higgs field has nonminimal coupling to the general relativity sector , as invoked in various extensions of the standard model . nonminimal coupling between the higgs and spacetime curvature may be beneficial to have the higgs responsible for inflation @xcite , and as a suppression mechanism for the contribution to dark energy expected from quantum fields @xcite .

Suppose that you have an abstract for a scientific paper: multiwavelength data on star - forming galaxies provide strong evidence for large - scale galactic winds in both nearby and distant objects . the results from recent ground - based and space - borne programs are reviewed . the impact of these winds on the host galaxies and the surrounding environment is discussed in the context of galaxy evolution . # 1_#1 _ # 1_#1 _ = # 1 1.25 in .125 in .25 in . And you have already written the first three sentences of the full article: galactic winds that extend on a scale comparable to the host galaxies are now known to be a common feature both locally and at high redshifts . these winds are significant carriers of mass , momentum , and energies that may impact the formation and evolution of the host galaxies and the surrounding intergalactic medium . given the scope of this conference , the present review focusses exclusively on starburst - driven winds . agn - driven galactic winds , perhaps a very important phenomenon in the lives of galaxies with spheroids ( kormendy & gebhardt 2001 ) , are not discussed here ( see , e.g. , veilleux et al .. Please generate the next two sentences of the article

2002a for a recent review of this topic ) . due to space limitations , the emphasis of this review is on the recent ( @xmath0 1998 ) literature .

Suppose that you have an abstract for a scientific paper: this paper develops methods to obtain bounds on an @xmath0-divergence based on one or several other @xmath0-divergences , dealing with pairs of probability measures defined on arbitrary alphabets . functional domination is one such approach , where special emphasis is placed on finding the best possible constant upper bounding a ratio of @xmath0-divergences . another approach used for the derivation of bounds among @xmath0-divergences relies on moment inequalities and the logarithmic - convexity property , which is studied in this paper to obtain tight bounds on the relative entropy and bhattacharyya distance in terms of @xmath1 divergences . a rich variety of bounds are shown to hold under boundedness assumptions on the relative information . special attention is on the total variation distance and its relation to the relative information and relative entropy , including reverse pinsker inequalities , " as well as on the @xmath2 divergence , which generalizes the total variation distance . pinsker s inequality is extended for this type of @xmath0-divergence , a result which leads to an inequality that links the relative entropy and relative information spectrum . integral expressions of the rnyi divergence in terms of the relative information spectrum are derived , leading to bounds on the rnyi divergence in terms of either the variational distance or relative entropy . * keywords * : relative entropy , total variation distance , @xmath0-divergence , rnyi divergence , pinsker s inequality , relative information . . And you have already written the first three sentences of the full article: throughout their development , information theory , and more generally , probability theory , have benefitted from non - negative measures of dissimilarity , or loosely speaking , distances , between pairs of probability measures defined on the same measurable space ( see , e.g. , @xcite ) . notable among those measures are ( see section [ sec : preliminaries ] for definitions ) : * total variation distance @xmath3 ; * relative entropy @xmath4 ; * @xmath1-divergence @xmath5 ; * hellinger divergence @xmath6 ; * rnyi divergence @xmath7 . it is useful , particularly in proving convergence results , to give bounds of one measure of dissimilarity in terms of another .. Please generate the next two sentences of the article

the most celebrated among those bounds is pinsker s inequality : . ] @xmath8 proved by csiszr @xcite and kullback @xcite , with kemperman @xcite independently a bit later . improved and generalized versions of pinsker s inequality have been studied , among others , in @xcite , @xcite , @xcite , @xcite , @xcite , @xcite , @xcite . in this work , we find relationships among the various divergence measures outlined above as well as a number of other measures of dissimilarity between probability measures .

Suppose that you have an abstract for a scientific paper: a model describing the low density carrier state in an organic single crystal fet with high-@xmath0 gate dielectrics is studied . the interplay between charge carrier coupling with inter - molecular vibrations in the bulk of the organic material and the long - range interaction induced at the interface with a polar dielectric is investigated . this interplay is responsible for the stabilization of a polaronic state with an internal structure extending on few lattice sites , at much lower coupling strengths than expected from the polar interaction alone . this effect could give rise to polaron self - trapping in high-@xmath0 organic fet s without invoking unphysically large values of the carrier interface interaction . . And you have already written the first three sentences of the full article: organic field - effect transistors ( ofets ) are the elementary building blocks of `` plastic electronics''.@xcite in these devices , charges are induced in a thin conducting channel at the interface between an organic semiconductor and a gate insulator . while commercial applications have already appeared , mostly based on low - cost organic thin - films , the fundamental physical mechanisms governing the charge dynamics in these devices are not fully understood . as it has become clear in recent years , even when high purity crystalline semiconductors are used in order to minimize the effects of structural and chemical disorder , the electronic characteristics of ofets are strongly affected by interactions taking place both within the semiconducting material as well as with its close environment .. Please generate the next two sentences of the article

this can be traced back to the extremely narrow electronic bands resulting from the weak van der waals intermolecular bonding , that make organic semiconductors much more sensitive to electronic interactions than their inorganic counterparts . for this reason , polaronic effects have been shown to play an important role in these devices .

Suppose that you have an abstract for a scientific paper: the barrel part of the atlas pixel detector will consist of 112 carbon - carbon structures called `` staves '' with 13 hybrid detector modules being glued on each stave . the demands on the glue joints are high , both in terms of mechanical precision and thermal contact . to achieve this precision a custom - made semi - automated mounting machine has been constructed in wuppertal , which provides a precision in the order of tens of microns . as this is the last stage of the detector assembly providing an opportunity for stringent tests , a detailed procedure has been defined for assessing both mechanical and electrical properties . this note gives an overview of the procedure for affixation and tests , and summarizes the first results of the production . , , , , , , , , pixel detector , stave , mounting machine . And you have already written the first three sentences of the full article: atlas will be a particle physics experiment at the future large hadron collider ( lhc ) , which is being built at cern and is expected to start operation in 2007 . the pixel detector is the innermost component of the atlas inner tracker . in the barrel the detector modules are mounted on staves , while the modules in the end caps are organized in disk sectors .. Please generate the next two sentences of the article

the pixel detector consists of 1774 detector modules ( barrel : 1456 modules ; discs : 318 ) . @xmath0 + the most important components of a detector module are : * 46080 individual pixel sensors with size of @xmath1 * 16 front end read out chips * 1 module controller chip

Suppose that you have an abstract for a scientific paper: we present the first application of a spherical collapse model to a supercluster of galaxies . positions and redshifts of @xmath0 galaxies in the shapley supercluster ( ssc ) are used to define velocity caustics that limit the gravitationally collapsing structure in its central part . this is found to extend at least to @xmath1 mpc of the central cluster , a 3558 , enclosing 11 aco clusters . infall velocities reach @xmath2 km s@xmath3 . dynamical models of the collapsing region are used to estimate its mass profile . an upper bound on the mass , based on a pure spherical infall model , gives @xmath4 for an einstein - de sitter ( critical ) universe and @xmath5 for an empty universe . the model of diaferio & geller ( 1997 ) , based on estimating the escape velocity , gives a significantly lower value , @xmath6 , very similar to the mass found around the coma cluster by the same method ( geller et al . 1999 ) , and comparable to or slightly lower than the dynamical mass in the virialized regions of clusters enclosed in the same region of the ssc . in both models , the overdensity in this region is substantial , but far from the value required to account for the peculiar motion of the local group with respect to the cosmic microwave background . . And you have already written the first three sentences of the full article: this is the third in a series of papers analyzing the structure and physical parameters of the shapley supercluster ( ssc ) , based on galaxy redshifts . the first ( quintana et al . 1995 ; hereafter _ paper i _ ) presents and gives an initial analysis of the results of spectroscopic observations of the central region . the second ( quintana , carrasco , & reisenegger 2000 , hereafter _ paper ii _ ) presents a much extended sample of galaxy redshifts and gives a qualitative discussion of the ssc s morphology . here. Please generate the next two sentences of the article

, we use dynamical collapse models applied to this sample , in order to obtain the mass of the central region of the ssc . an upcoming paper ( carrasco , quintana , & reisenegger 2000 , hereafter _ paper iv _ ) will analyze the individual clusters of galaxies contained in the sample , to obtain their physical parameters ( velocity dispersion , size , mass ) , search for substructures within the clusters , and determine the total mass contained within the virialized regions of clusters in the whole shapley area . the shapley concentration ( shapley 1930 ) is the richest supercluster in the local universe ( zucca et al .

Suppose that you have an abstract for a scientific paper: dynamics of p53 is known to play important roles in the regulation of cell fate decisions in response to various stresses , and pdcd5 functions as a co - activator of p53 to modulate the p53 dynamics . in the present paper , we investigate how p53 dynamics are modulated by pdcd5 during the dna damage response using methods of bifurcation analysis and potential landscape . our results reveal that p53 activities can display rich dynamics under different pdcd5 levels , including monostability , bistability with two stable steady states , oscillations , and co - existence of a stable steady state and an oscillatory state . physical properties of the p53 oscillations are further shown by the potential landscape , in which the potential force attracts the system state to the limit cycle attractor , and the curl flux force drives the coherent oscillation along the cyclic . we also investigate the effect of pdcd5 efficiency on inducing the p53 oscillations . we show that hopf bifurcation is induced by increasing the pdcd5 efficiency , and the system dynamics show clear transition features in both barrier height and energy dissipation when the efficiency is close to the bifurcation point . this study provides a global picture of how pdcd5 regulates p53 dynamics via the interaction with the p53-mdm2 oscillator and can be helpful in understanding the complicate p53 dynamics in a more complete p53 pathway . . And you have already written the first three sentences of the full article: the tumor suppressor p53 plays a central role in cellular responses to various stress , including oxidative stress , hypoxia , telomere erosion and dna damage @xcite . in unstressed cells , p53 is kept at low level via its negative regulator mdm2 @xcite . under stressed conditions , such as dna damage , p53 is stabilized and activated to induce the express of downstream genes , including p21/waf1/cip1 and gadd45 that are involved in cell cycle arrest , and puma , bax and pig3 that can induce apoptosis @xcite .. Please generate the next two sentences of the article

the cell fate decisions after dna damage are closely related to the p53 dynamics that is regulated by p53-mdm2 interactions @xcite . oscillations of p53 level have been observed upon ir induced dna damage at the population level in several human cell lines and transgenic mice @xcite .

Suppose that you have an abstract for a scientific paper: metamaterials are artificially structured media that can focus ( lensing ) or reroute ( cloaking ) waves , and typically this is developed for electromagnetic waves at millimetric down to nanometric scales or for acoustics or thin elastic plates at centimeter scales . extending the concepts of @xcite we show that the underlying ideas are generic across wave systems and scales by generalizing these concepts to seismic waves at frequencies , and lengthscales of the order of hundreds of meters , relevant to civil engineering . by applying ideas from transformation optics we can manipulate and steer rayleigh surface wave solutions of the vector navier equations of elastodynamics ; this is unexpected as this vector system is , unlike maxwell s electromagnetic equations , not form invariant under transformations . as a paradigm of the conformal geophysics that we are creating , we design a square arrangement of luneburg lenses to reroute and then refocus rayleigh waves around a building with the dual aim of protection and minimizing the effect on the wavefront ( cloaking ) after exiting the lenses . to show that this is practically realisable we deliberately choose to use material parameters readily available and this metalens consists of a composite soil structured with buried pillars made of softer material . the regular lattice of inclusions is homogenized to give an effective material with a radially varying velocity profile that can be directly interpreted as a lens refractive index . we develop the theory and then use full 3d time domain numerical simulations to conclusively demonstrate the validity of the transformation seismology ideas : we demonstrate , at frequencies of seismological relevance @xmath0 hz , and for low speed sedimentary soil ( @xmath1 m / s ) , that the vibration of a structure is reduced by up to 6 db at its resonance frequency . this invites experimental study and opens the way to translating much of the current metamaterial literature into that of seismic surface waves . .... And you have already written the first three sentences of the full article: in his seminal work , luneburg @xcite derived a spherical optical lens with radially varying refractive index that focused a beam of parallel rays to a point at the opposite side of the lens ; a two dimensional variant is straightforward to deduce . of course this relies upon the governing equation being the helmholtz equation , which the full ela in the model configuration presented here the elastic energy is primarily carried by rayleigh surface waves ; they are a particular solution of navier s equation for elastodynamics for a half - space bounded by a traction - free surface , e.g. the earth s surface . well known in seismology , for the idealised situation of isotropic and homogeneous media they are non - dispersive , elliptically polarized and in practical terms @xcite they have a velocity very close to that of shear waves : @xmath6 where @xmath7 is the shear modulus and @xmath8 the density @xcite so for simplicity we will simply use the shear wave speed in our analysis .. Please generate the next two sentences of the article

shear horizontally polarized waves ( sh ) are also present in our numerical model , and they also propagate with wavespeed @xmath9 ; notably sh waves are governed by a helmholtz equation without any approximation . we do not consider love waves here , which can also be important is seismology , as they only exist for stratified layered media and we assume that our elastic half space is vertically homogeneous , that is , the material parameters do not vary with depth .

Suppose that you have an abstract for a scientific paper: = 0.75this review is intended to give a pedagogical and unified view on the subject of the statistics and scaling of physical quantities in disordered electron systems at very low temperatures . quantum coherence at low temperatures and randomness of microscopic details can cause large fluctuations of physical quantities . in such mesoscopic systems a localization - delocalization transition can occur which forms a critical phenomenon . accordingly , a one - parameter scaling theory was formulated stressing the role of conductance as the ( one - parameter ) scaling variable . the localized and delocalized phases are separated by a critical point determined by a critical value of conductance . however , the notion of an order parameter was not fully clarified in this theory . the one - parameter scaling theory has been questioned once it was noticed that physical quantities are broadly distributed and that average values are not characteristic for the distributions . based on presently available analytical and numerical results we focus here on the description of the total distribution functions and their flow with increasing system size . still , one - parameter scaling theory does work in terms of typical values of the local density of states and of the conductance which serve as order parameter and scaling variable of the localization - delocalization transition , respectively . below a certain length scale , @xmath0 , related to the value of the typical conductance , local quantities are multifractally distributed . this multifractal behavior becomes universal on approaching the localization - delocalization transition with @xmath0 playing the role of a correlation length . # 1#2#1 ; # 2 # 1#2 ( # 1 # 2 ) # 1#2 ( # 1 # 2 ) z * s * = 0.7 . And you have already written the first three sentences of the full article: this review is about mesoscopic conductors , statistics of related physical quantities and their scaling behavior under change of the size of the conductor . a few words about the terms used here shall tell the reader what to expect . mesoscopic systems are intermediate between microscopic and macroscopic systems .. Please generate the next two sentences of the article

the term goes back to van kampen and was widely used after a work on `` physics of mesoscopic systems '' by imry @xcite . mesoscopic conductors contain many ( e.g. @xmath1 ) elementary objects like electrons and atoms . on the other hand their properties

Suppose that you have an abstract for a scientific paper: at kamioka observatory many activities for low energy rare event search are ongoing . super - kamiokande(sk ) , the largest water cherenkov neutrino detector , currently continues data taking as the fourth phase of the experiment ( sk - iv ) . in sk - iv , we have upgraded the water purification system and tuned water flow in the sk tank . consequently the background level was lowered significantly . this allowed sk - iv to derive solar neutrino results down to 3.5 mev energy region . with these data , neutrino oscillation parameters are updated from global fit ; @xmath0 , @xmath1 , @xmath2 . newage , the directional sensitive dark matter search experiment , is currently operated as `` newage-0.3a '' which is a @xmath3 m@xmath4 micro - tpc filled with cf4 gas at 152 torr . recently we have developed `` newage-0.3b '' . it was succeeded to lower the operation pressure down to 76 torr and the threshold down to 50 kev ( f recoils ) . xmass experiment is looking for scintillation signals from dark matter interaction in 1 ton of liquid xenon . it was designed utilizing its self - shielding capability with fiducial volume confinement . however , we could lower the analysis threshold down to 0.3 kevee using whole volume of the detector . in february 2012 , low threshold and very large exposure data ( 5591 kg@xmath5days ) were collected . with these data , we have excluded some part of the parameter spaces claimed by dama / libra and cogent experiments . . And you have already written the first three sentences of the full article: kamioka observatory , institute for cosmic ray research , university of tokyo , is located in kamioka - town in the northern part of the gifu prefecture in japan . the location of the laboratories is under the peak of mt . ikenoyama providing 2,700 meters water equivalent ( or 1000 m of rock ) overburden .. Please generate the next two sentences of the article

this observatory was established in 1995 to push forward with the super - kamiokande experiment and has become a world frontier center of neutrino physics . many studies complementary to the flagship sk are also ongoing as illustrated in figure [ map ] .

Suppose that you have an abstract for a scientific paper: we present simultaneous high - resolution optical spectroscopy and x - ray data of the x - ray binary system grmus ( xb1254690 ) , obtained over a full range of orbital phases . the x - ray observations are used to re - establish the orbital ephemeris for this source . the optical data includes the first spectroscopic detection of the donor star in this system , through the use of the doppler tomography technique on the bowen fluorescence blend ( @xmath04630 - 4650 ) . in combination with an estimate for the orbital parameters of the compact object using the wings of the heii @xmath14686 emission line , dynamical mass constraints of 1.20 @xmath2 2.64 for the neutron star and 0.45 @xmath3 0.85 for the companion are derived . [ firstpage ] binaries : close - stars : binaries : individual : grmus , xb1254690 - binaries : spectroscopic - x - rays : binaries . . And you have already written the first three sentences of the full article: xb1254690 is a persistently bright , low - mass x - ray binary ( lmxb ) . it was identified with a faint blue star ( grmus , _ v _ = 19.1 ) , which exhibited the bowen blend of niii and ciii in emission @xcite . the object produced type 1 x - ray bursts @xcite , indicating the presence of a neutron star as the compact object .. Please generate the next two sentences of the article

dips of up to 95% of the 110 kev flux , with a recurrence period of _ @xmath4 _ = 3.88 @xmath5 0.15 hr and lasting @xmath0 0.8 hr per cycle , were discovered in _

Suppose that you have an abstract for a scientific paper: we report the discovery of two new pulsating extremely low - mass ( elm ) white dwarfs ( wds ) , sdss j161431.28 + 191219.4 ( hereafter j1614 ) and sdss j222859.93 + 362359.6 ( hereafter j2228 ) . both wds have masses @xmath0 0.25 @xmath1 and thus likely harbor helium cores . spectral fits indicate these are the two coolest pulsating wds ever found . j1614 has @xmath2 @xmath3 k and @xmath4 @xmath5 , which corresponds to a @xmath60.19 @xmath1 wd . j2228 is considerably cooler , with a @xmath2 @xmath7 k and @xmath4 @xmath8 , which corresponds to a @xmath60.16 @xmath1 wd , making it the coolest and lowest - mass pulsating wd known . there are multiple elm wds with effective temperatures between the warmest and coolest known elm pulsators that do not pulsate to observable amplitudes , which questions the purity of the instability strip for low - mass wds . in contrast to the co - core zz ceti stars , which are believed to represent a stage in the evolution of all such wds , elm wds may not all evolve as a simple cooling sequence through an instability strip . both stars exhibit long - period variability ( @xmath9 s ) consistent with non - radial @xmath10-mode pulsations . although elm wds are preferentially found in close binary systems , both j1614 and j2228 do not exhibit significant radial - velocity variability , and are perhaps in low - inclination systems or have low - mass companions . these are the fourth and fifth pulsating elm wds known , all of which have hydrogen - dominated atmospheres , establishing these objects as a new class of pulsating wd . [ firstpage ] stars : white dwarfs stars : oscillations ( including pulsations ) galaxy : stellar content stars : individual : sdss j161431.28 + 191219.4 , sdss j222859.93 + 362359.6 . And you have already written the first three sentences of the full article: white dwarf ( wd ) stars represent the end points of stellar evolution for all low - mass stars , and are the fate of more than 97% of all stars in our galaxy . roughly 80% of wds belong to the spectral class da , with atmospheres characteristically dominated by hydrogen @xcite . when da wds cool to the appropriate temperature to foster a hydrogen partial ionization zone , they begin their journey through the zz ceti ( or dav ) instability strip , where global pulsations are driven to observable amplitudes and their fundamental parameters can be determined using asteroseismology ( see reviews by @xcite , @xcite and @xcite ) . aside from their variability , the zz ceti stars discovered to date appear to be otherwise normal wds , and are therefore believed to be a natural phase in the evolution of all das . although some das within the empirical instability strip have been observed not to vary to modest limits ( e.g. , @xcite ) , follow - up observations have shown that some of these stars really do pulsate at low amplitude ( e.g. , @xcite ) . higher - quality optical and uv spectra have also moved some of these non - variable interlopers out of the instability strip @xcite .. Please generate the next two sentences of the article

thus , it is currently believed that the zz ceti instability strip is pure , and that all da wds will at some point pass through it and pulsate @xcite . much work has been devoted to observationally mapping the zz ceti instability strip , which runs in temperature from roughly @xmath11 k for standard @xmath4 = 8.0 wds @xcite .

Suppose that you have an abstract for a scientific paper: we generalize the classic bonnor - ebert stability analysis of pressure - truncated , self - gravitating gas spheres , to include clouds with arbitrary equations of state . a virial - theorem analysis is also used to incorporate mean magnetic fields into such structures . the results are applied to giant molecular clouds ( gmcs ) , and to individual dense cores , with an eye to accounting for recent observations of the internal velocity - dispersion profiles of the cores in particular . we argue that gmcs and massive cores are at or near their critical mass , and that in such a case the size - linewidth and mass - radius relations between them are only weakly dependent on their internal structures ; any gas equation of state leads to essentially the same relations . we briefly consider the possibility that molecular clouds can be described by polytropic pressure - density relations ( of either positive or negative index ) , but show that these are inconsistent with the apparent gravitational virial equilibrium , @xmath0 , of gmcs and of massive cores . this class of models would include clouds whose nonthermal support comes entirely from alfvn wave pressure . the simplest model consistent with all the salient features of gmcs and cores is a `` pure logotrope , '' in which @xmath1 . detailed comparisons with data are made to estimate the value of @xmath2 , and an excellent fit to the observed dependence of velocity dispersion on radius in cores is obtained with @xmath3 . . And you have already written the first three sentences of the full article: giant molecular clouds ( gmcs ; @xmath4 ) in the galaxy are highly inhomogeneous : they are often filamentary in appearance , consisting of discrete clumps , or cores ( @xmath5 ) , which contain most of the mass of a cloud ( including any young stars ) and are surrounded by a more diffuse component of predominantly atomic gas ( e.g. , williams , blitz , & stark 1995 ) . indeed , gmcs are clumpy on all scales observed , and are possibly even fractal in nature ( falgarone , phillips , & walker 1991 ) . remarkably enough , however , the gross properties of cloud complexes are rather simply interrelated .. Please generate the next two sentences of the article

total masses , mean densities , and average velocity dispersions vary with sizes ( effective radii ) roughly as @xmath6 , @xmath7 , and @xmath8 ( larson 1981 ; sanders , scoville , & solomon 1985 ; solomon et al . 1987 ) , with uncertainties in the exponents typically of order @xmath90.1 .

Suppose that you have an abstract for a scientific paper: dna cyclization is a powerful technique to gain insight into the nature of dna bending . the worm - like chain model provides a good description of small to moderate bending fluctuations , but some experiments on strongly - bent shorter molecules suggest enhanced flexibility over and above that expected from the worm - like chain . here , we use a coarse - grained model of dna to investigate the thermodynamics of dna cyclization for molecules with less than 210 base pairs . as the molecules get shorter we find increasing deviations between our computed equilibrium @xmath0-factor and the worm - like chain predictions of shimada and yamakawa . these deviations are due to sharp kinking , first at nicks , and only subsequently in the body of the duplex . at the shortest lengths , substantial fraying at the ends of duplex domains is the dominant method of relaxation . we also estimate the dynamic @xmath0-factor measured in recent fret experiments . we find that the dynamic @xmath0-factor is systematically larger than its equilibrium counterpart , with the deviation larger for shorter molecules , because not all the stress present in the fully cyclized state is present in the transition state . these observations are important for the interpretation of recent experiments , as only kinking within the body of the duplex is genuinely indicative of non - worm - like chain behaviour . . And you have already written the first three sentences of the full article: as the mechanical properties of dna play an important role in its biological capacities , there has been much activity to accurately characterize these properties , not only in the elastic regime of small to moderate fluctuations but also for more strongly stressed systems . for example , dna is found to overstretch beyond a salt - dependent critical force @xcite . similarly , in response to twist dna forms plectonemes beyond a critical buckling superhelical density @xcite . here , we are interested in the response of dna to strong bending .. Please generate the next two sentences of the article

the worm - like chain ( wlc ) model provides a good description of small to moderate bending fluctuations in dna @xcite . however , although there is a consensus that for sufficiently strong bending the stress will be localized within small regions , often termed `` kinks '' , much about this crossover to non - wlc behaviour remains controversial .

Suppose that you have an abstract for a scientific paper: it is widely believed that the emergent magnetic gauge symmetry of sqcd is analogous to a hidden local symmetry ( hls ) . we explore this idea in detail , deriving the entire ( spontaneously broken ) magnetic theory by applying the hls formalism to spontaneously broken @xmath0 sqcd . we deduce the khler potential in the hls description , and show that gauge and flavour symmetry are smoothly restored along certain scaling directions in moduli space . we propose that it is these symmetry restoring directions , associated with the @xmath1-symmetry of the theory , that allow full seiberg duality . reconsidering the origin of the magnetic gauge bosons as the @xmath2-mesons of the electric theory , colour - flavour locking allows a simple determination of the parameter @xmath3 . its value continuously interpolates between @xmath4 on the baryonic branch of moduli space corresponding to vector meson dominance " and @xmath5 on the mesonic branch . both limiting values are consistent with previous results in the literature . the hls formalism is further applied to @xmath6 and @xmath7 groups , where the usual seiberg duals are recovered , as well as adjoint sqcd . finally we discuss some possible future applications , including ( naturally ) the unitarisation of composite @xmath8 scattering , blended higgs / technicolour models , real world qcd and non - supersymmetric dualities . . And you have already written the first three sentences of the full article: several ideas have been put forward for dealing with strongly coupled theories . an early example , that works surprisingly well for qcd , is the notion of hidden local symmetry ( hls ) . take a theory with flavour symmetry @xmath9 spontaneously broken to a subgroup @xmath10 .. Please generate the next two sentences of the article

the strategy is to first use low energy theorems describing the associated nambu - goldstone bosons ( ngbs ) to construct an effective , nonlinear sigma model description on the manifold @xmath11 @xcite . as it happens , this model is gauge equivalent to a linear model with flavour symmetry @xmath9 and a broken _ gauge _ symmetry @xmath10 , thus providing an alternative effective description @xcite . the broken gauge symmetry is the hls , in the sense that it was not present in the original theory but `` emerges '' in the low energy physics .

Suppose that you have an abstract for a scientific paper: many high - temperature superconductors are highly polarizable ionic lattices where the frhlich electron - phonon interaction ( epi ) with longitudinal optical phonons creates an effective attraction of doped carriers virtually equal to their coulomb repulsion . the general multi - polaron theory is given with both interactions being strong compared with the carrier kinetic energy so that the conventional bcs - eliashberg approximation is inapplicable . the many - electron system is described by the polaronic t - j@xmath0 hamiltonian with reduced hopping integral , @xmath1 , allowed double on - site occupancy , large phonon - induced antiferromagnetic exchange , @xmath2 , and a high - temperature superconducting state of small superlight bipolarons protected from clustering . . And you have already written the first three sentences of the full article: it seems plausible that the true origin of high - temperature superconductivity is found in a proper combination of the finite - range coulomb repulsion with a significant finite - range epi as suggested by a growing number of experimental and theoretical studies @xcite . in highly polarizable ionic lattices like cuprate superconductors both interactions are quite strong ( of the order of 1 ev ) compared with the low fermi energy of doped carriers because of a poor screening by non- or near - adiabatic carriers @xcite . in those conditions the bcs - eliashberg theory @xcite breaks down because of the polaronic collapse of the electron bandwidth @xcite . the many - body theory for polarons has been developed for extremely weak and strong epi . in the weak - coupling limit this problem. Please generate the next two sentences of the article

is reduced to the study of a structure factor of the uniform large polaron gas @xcite . for strong coupling the problem is reduced to on - site @xcite or inter - site @xcite small bipolarons on a lattice .

Suppose that you have an abstract for a scientific paper: seven high - resolution and high s / n ccd spectra were used to derive elemental abundances in the atmosphere of vw ari a ( t@xmath0=7200 , @xmath1=3.7 ) which is the primary component of a visual binary system . the synthetic spectrum technique applied in the analysis allowed to reveal the following feature : the atmosphere of this star is strongly deficient in some metals , while light elements have solar - like abundances . taking into account these results , one can suggest that vw ari a is a @xmath2 boo - type star . another argument supporting this supposition is the following : on the diagrams `` @xmath3 '' , `` @xmath4 '' and `` @xmath5 '' ( paunzen et al . 1997 ) vw ari a falls exactly in the region occupied by the @xmath2 boo stars . note also , that a previous analysis ( andrievsky et al . 1995 ) has shown that the secondary component of vw ari has a normal metallicity . differences in chemical compositions of the two components appear to be due to the specific evolution of the primary vw ari a. . And you have already written the first three sentences of the full article: vw ari ( hd 15165 , bds 1269 ) is a remarkable visual binary system consisting of two components : vw ari a ( v=6.@xmath671 , a - type ) and its companion ( v=8.@xmath633 , f - type ) . the primary vw ari a is a multiperiodic pulsating star ( probably of @xmath7 sct - type ) having non - radial modes . this star shows the spectrum typical of very metal - deficient stars . the rather high @xmath8 value found for this star , makes it difficult to derive accurate elemental abundances .. Please generate the next two sentences of the article

a first attempt was undertaken by andrievsky et al . ( 1995 ) , who showed that calcium and iron are strongly deficient in the atmosphere of vw ari a , while the secondary component possesses a solar - like chemical composition .

Suppose that you have an abstract for a scientific paper: to understand the conditions under which dense , molecular gas is able to form within a galaxy , we post - process a series of three - dimensional galactic - disk - scale simulations with ray - tracing based radiative transfer and chemical network integration to compute the equilibrium chemical and thermal state of the gas . in performing these simulations we vary a number of parameters , such as the isrf strength , vertical scale height of stellar sources , cosmic ray flux , to gauge the sensitivity of our results to these variations . self - shielding permits significant molecular hydrogen ( @xmath0 ) abundances in dense filaments around the disk midplane , accounting for approximately @xmath1% of the total gas mass . significant co fractions only form in the densest , @xmath2 , gas where a combination of dust , @xmath0 , and self - shielding attenuate the fuv background . we additionally compare these ray - tracing based solutions to photochemistry with complementary models where photo - shielding is accounted for with locally computed prescriptions . with some exceptions , these local models for the radiative shielding length perform reasonably well at reproducing the distribution and amount of molecular gas as compared with a detailed , global ray tracing calculation . specifically , an approach based on the jeans length with a @xmath3 temperature cap performs the best in regards to a number of different quantitative measures based on the @xmath0 and co abundances . [ firstpage ] -1 cm stars : formation stars : mass function . And you have already written the first three sentences of the full article: the interstellar medium ( ism ) of a typical disk galaxy is divided into variety of distinct phases , generally classified into hot ionized ( @xmath4 ) gas , the warm neutral medium ( wnm ; @xmath5 ) , and the cold neutral medium ( cnm ; @xmath6 ) . star formation , however , appears to be restricted to cold dense gas with a star formation rate ( sfr ) that strongly correlates with the molecular gas content @xcite . this link between star formation and molecular gas is probably not causal , in the sense that the presence of molecules simply marks those parts of the ism that are cold and dense enough to undergo gravitational collapse @xcite , but the molecular gas nonetheless represents an indispensable tracer of star forming regions in the local and distant universe .. Please generate the next two sentences of the article

understanding these crucial links between star formation , the ism , and galaxy evolution , all intricately coupled through a variety of energetic stellar feedback mechanisms , must rely on identifying the pathways and conditions under which cold , molecular gas is able to develop . furthermore , the gas temperature sets the characteristic size ( @xmath7 ) and mass ( @xmath8 ) of prestellar cores that develop in post - shock regions within magnetized , star - forming clouds ( e.g. , * ? ? ?

Suppose that you have an abstract for a scientific paper: we study theoretically dynamical phases of vortices in superconducting films with arrays of obstacles . by performing a series of molecular dynamics simulations and analytical calculations , we demonstrate the existence of a phase of soliton - like vortex - density waves existing in a wide range of parameters . these waves are formed by a self - assembled phase separation process induced by strongly nonlinear density fluctuations of the moving vortex matter above a certain critical driving current . at high vortex concentrations , the waves move at an approximately current - independent speed resulting in a wide plateau in the voltage - current characteristics . at stronger drives , the vortex system enters into a fully jammed ( zero - voltage ) phase . by combining ac and dc drives , the interplay between the vortex - density - wave and jammed phases leads to the observation of negative absolute mobility of vortices , which induces the superconducting film into a negative resistance state . . And you have already written the first three sentences of the full article: driven many - particle systems are often affected by strongly nonlinear fluctuations which can lead to dramatic phenomena such as self - organized density waves @xcite , jamming @xcite , and spontaneous segregation @xcite . in inhomogeneous type - ii superconductors , nonlinear phenomena resulting from the motion of magnetic flux quanta ( vortices ) have been investigated , for instance , in the context of dendritic flux instabilities stemming from the breakdown of the bean critical state @xcite . in a superconductor , vortices are subjected to the lorentz force induced by an applied current density @xmath0 and to the pinning force produced by sample inhomogeneities . a dissipative dynamical state of moving vortices is established at the critical current @xmath1 when the lorentz force overcomes pinning.@xcite just above @xmath1 , motion is usually plastic with vortices moving at different velocities , which results in a nonlinear velocity - force ( voltage - current ) characteristic . at a stronger drive , the pinning potential is washed out and the corresponding dynamical state , coined _ flux flow _ ,. Please generate the next two sentences of the article

is essentially linear . these dynamical regimes have been extensively investigated in disordered superconductors @xcite and , more recently , in films with periodic arrays of nanoengineered pinning centers.@xcite however , much less attention has been given to the dynamics of vortices in arrays of obstacles ( or antipinning centers).@xcite because in this configuration vortices are not trapped individually , it renders a very small critical current , which , in principle , has limited interest for applications . on the other hand a small @xmath1 allows for investigation of vortex motion in a much wider current range .

Suppose that you have an abstract for a scientific paper: in this paper , we present a new method for finding identities for hypergeoemtric series , such as the ( gauss ) hypergeometric series , the generalized hypergeometric series and the appell - lauricella hypergeometric series . furthermore , using this method , we get identities for the hypergeometric series @xmath0 ; we show that values of @xmath0 at some points @xmath1 can be expressed in terms of gamma functions , together with certain elementary functions . we tabulate the values of @xmath0 that can be obtained with this method . we find that this set includes almost all previously known values and many previously unknown values . key words and phrases : hypergeometric series , three term relation , special value , solving polynomial systems . 2010 mathematics subject classification numbers : primary 33c05 secondary 13p10 , 13p15 , 33c20 , 33c65 . . And you have already written the first three sentences of the full article: the series @xmath2 where @xmath3 , can be expressed as @xmath4 this identity ( [ binomial_thm ] ) is called the binomial theorem . the binomial theorem ( [ binomial_thm ] ) has many applications . for example , because @xmath5 from ( [ binomial_thm ] ) , we can perform numerical calculation of @xmath6 effectively ( cf .. Please generate the next two sentences of the article

292 page in chapter 4 in part ii of [ eu ] ) : @xmath7 using ( [ binomial_thm ] ) like this , we are able to do numerical calculations of algebraic numbers . moreover , we obtain , for non - negative integer @xmath8 , @xmath9 thus , we can obtain combinatorial identities from ( [ binomial_thm ] ) . as seen above

Suppose that you have an abstract for a scientific paper: room temperature ferromagnetic hysteresis is observed in commercial srtio@xmath0 substrates purchased from a variety of suppliers . it is shown that the ferromagnetic signal comes from the unpolished surfaces . surface impurity phases can not be detected using either x - ray diffraction or energy dispersive x - ray spectra on the unpolished surfaces . however , a possible correlation between surface disorder ( xray diffraction peak linewidth ) and ferromagnetism is observed . ar ion bombardment ( 10kev-90 kev ) can be used to produce surface layer disorder but is not found to induce ferromagnetism . annealing of the substrates at temperatures ranging from 600 to 1100 @xmath1c is found to alter the hysteresis curves differently depending on whether the annealing is performed in air or in vacuum . identical annealing behaviour is observed if the substrates are artificially spiked with iron . this suggests that the ferromagnetic hysteresis of as purchased srtio@xmath0 could be due to fe contamination of the unpolished surfaces . in addition , it is shown that no ferromagnetism is observed in samples that contain 10@xmath2 - 10@xmath3 @xmath4 of oxygen vacancies if all the faces are polished . . And you have already written the first three sentences of the full article: claims of room temperature ferromagnetism ( fm ) have been made for several semiconducting oxides that do not contain any magnetic ions . the phenomenon has been observed in a variety of binary oxides prepared in nanoparticle@xcite and thin - film form @xcite . there has been considerable interest in these otherwise non - magnetic oxides as a part of the effort to develop suitable materials for spintronic devices . this work is concerned with the origin of room temperature magnetic hysteres is observed in single crystal srtio@xmath0 ( 001 ) substrates ( sto ) purchased from a variety of suppliers .. Please generate the next two sentences of the article

the hysteresis , which can not be explained by non - interacting paramagnetic impurities , is interesting in light of recent work which highlights the considerable potential of sto surfaces for electronic and spintronic devices . consider , for example , the two dimensional electron gas formed at the interfaces of laalo@xmath0/sto heterostructures @xcite as well as other phenomena such as blue luminescence @xcite and high conductivity @xcite produced by ar@xmath5 irradiation .

Suppose that you have an abstract for a scientific paper: we examine the morphology of the color - magnitude diagram ( cmd ) for core helium - burning ( red clump ) stars to test the recent suggestion by zaritsky & lin ( 1997 ) that an extension of the red clump in the large magellanic cloud ( lmc ) toward brighter magnitudes is due to an intervening population of stars that is responsible for a significant fraction of the observed microlensing toward the lmc . using our own ccd photometry of several fields across the lmc , we confirm the presence of this additional red clump feature , but conclude that it is caused by stellar evolution rather than a foreground population . we do this by demonstrating that the feature ( 1 ) is present in all our lmc fields , ( 2 ) is in precise agreement with the location of the blue loops in the isochrones of intermediate age red clump stars with the metallicity and age of the lmc , ( 3 ) has a relative density consistent with stellar evolution and lmc star formation history , and ( 4 ) is present in the hipparcos cmd for the solar neighborhood where an intervening population can not be invoked . assuming there is no systematic shift in the model isochrones , which fit the hipparcos data in detail , a distance modulus of @xmath0 provides the best fit to our dereddened cmd . _ accepted for publication in the astronomical journal _ . And you have already written the first three sentences of the full article: the recent discovery of an overdensity of stars in the color - magnitude diagram ( cmd ) of the large magellanic cloud ( lmc ) having nearly the same color as the `` red clump '' of core he - burning stars but extending @xmath10.9 mag brighter has been interpreted as an intervening population of stars at @xmath2 kpc that may represent a dwarf galaxy or tidal debris sheared from a small milky way satellite ( zaritsky & lin 1997 , hereafter zl ) . zaritsky & lin label this overdensity the vrc ( vertical extension of the red clump ) , and reject other possible explanations to conclude that the vrc represents a massive foreground population with about 5% of angular surface density of the lmc itself . if true , this conclusion would have profound consequences for the interpretation of galactic microlensing studies ( renault 1997 , alcock 1997a ) since such debris could , in principle , be responsible for a sizable fraction of the microlensing signal toward the lmc ( zhao 1996 , 1998 ) that is generally attributed to microlensing by compact objects in the smoothly - distributed halo of the milky way itself .. Please generate the next two sentences of the article

this particular stellar foreground population as an explanation for the lmc microlensing optical depth has been challenged on several grounds . the macho team find no evidence for a foreground population at @xmath3 kpc in their extensive photometric database , confirming the lmc membership of their cepheids ( alcock 1997b , minniti 1997 ) .

Suppose that you have an abstract for a scientific paper: in this paper we address the statistical problem of testing if a stationary process is gaussian . the observation consists in a finite sample path of the process . using a random projection technique introduced and studied in @xcite in the frame of goodness of fit test for functional data , we perform some decision rules . these rules really stand on the whole distribution of the process and not only on its marginal distribution at a fixed order . the main idea is to test the gaussianity on the marginal distribution of some random linear combinations of the process . this leads to consistent decision rules . some numerical simulations show the pertinence of our approach . [ section ] [ prop ] lemma [ prop]theorem [ prop ] corollary [ prop ] claim [ prop ] [ prop ] example [ prop]definition [ prop]figure [ prop]table _ key words and phrases : gaussianity test , strictly stationary random process , random projection , consistent test _ _ a.m.s . 1980 subject classification : a60 g _ . And you have already written the first three sentences of the full article: in many concrete situations the statistician observes a finite path @xmath0 of a real temporal phenomena . a common modeling is to assume that the observation is a finite path of a second order weak stationary process @xmath1 ( see , for example , @xcite ) . this means that the random variable ( r.v . ). Please generate the next two sentences of the article

@xmath2 is , for any @xmath3 , square integrable and that the mean and the covariance structure of the process is invariant by any translation on the time index . that is , for any @xmath4 @xmath5 does not depend on @xmath6 and @xmath7 only depends on the distance between @xmath6 and @xmath8 .

Suppose that you have an abstract for a scientific paper: we present the global phase diagram of the extended boson hubbard model on a simple cubic lattice by quantum monte carlo simulation with worm update algorithm . four kinds of phases are supported by this model , including superfluid , supersolid , mott , and charge density wave ( cdw ) states , which are identified in the phase diagram of chemical potential @xmath0 versus nearest neighbor interaction @xmath1 . by changing the chemical potential , a continuous transition is found from the mott phase to a superfluid phase without breaking the translational symmetry . for an insulating cdw state , adding particles to it gives rise to a continuous transition to a supersolid phase , while removing particles usually leads to a first - order one to either supersolid or superfluid phase . by tuning the nearest neighbor interaction , one can realize the transition between two insulating phases , mott and cdw with the same particle density , which turns out to be of the first - order . we also demonstrate that a supersolid phase with average particle density less than 1/2 can exist in a small region of @xmath2 phase diagram . . And you have already written the first three sentences of the full article: lattice models of interacting bosons and fermions such as hubbard model and its various generalizations are usually strongly correlated systems exhibiting various phases with competing orders , which are of fundamental interest in fields of both condensed matter and cold atomic physics . interests on both types of hubbard models are renewed recently , since they can be realized in cold atomic gases loaded in optical lattices ( for a review see refs . [ ] and [ ] and references therein ) . unlike fermions. Please generate the next two sentences of the article

, there is a natural superfluid order for free bosons at zero temperature driven by the kinetic energy . when the interaction is switched on , the bosons are likely to be localized in various crystalline patterns , which may coexist with superfluid order @xcite to give a realization of intriguing `` supersolid '' state that has been pursued for decades since 1950s @xcite .

Suppose that you have an abstract for a scientific paper: we study the radio far infrared ( fir ) correlation in `` blue cloud '' galaxies chosen from the prism multiobject survey ( primus ) up to redshift ( @xmath0 ) of 1.2 in the xmm - lss field . we use rest - frame emission at 1.4 ghz in the radio and both monochromatic ( at 70@xmath1 m ) and bolometric ( between @xmath2 m ) emission in the fir . to probe the nature of the correlation up to @xmath3 , where direct detection of blue star - forming galaxies is impossible with current technology , we employ the technique of image stacking at 0.325 and 1.4 ghz in the radio and in six infrared bands , viz . 24 , 70 , 160 , 250 , 350 and @xmath4 m . for comparison , we also study the correlation for more luminous galaxies that are directly detected . the stacking analysis allows us to probe the radio fir correlation for galaxies that are up to 2 orders of magnitude fainter than the ones detected directly . the @xmath5correction in the infrared wavebands is obtained by fitting the observed spectral energy distribution ( sed ) with a composite mid - ir power law and a single temperature greybody model . we find that the radio luminosity at 1.4 ghz ( @xmath6 ) is strongly correlated with monochromatic fir luminosity at 70 @xmath1 m ( @xmath7 ) having slope @xmath8 and with bolometric luminosity ( @xmath9 ) having slope @xmath10 . the quantity @xmath11)$ ] is observed to decrease with redshift as @xmath12 probably caused due to the non - linear slope of the radio fir correlation . within the uncertainties of our measurement and the limitations of our flux - limited and color - selected sample , we do not find any evolution of the radio fir correlation with redshift . . And you have already written the first three sentences of the full article: the radio far infrared ( fir ) correlation is one of the tightest observed correlations in astrophysics that connects several independent physical parameters in the interstellar medium ( ism ) . the radio luminosity and the fir luminosity of star - forming galaxies are observed to be correlated over five orders of magnitude for the global scale @xcite with dispersion less than a factor of 2 . the radio luminosity is typically measured at 1.4 ghz and the fir luminosity can be both monochromatic ( at 24 , 60 or 70@xmath1 m ) or bolometric ( between 40 and 120@xmath1 m or between 8 and 1000@xmath1 m ) . the radio fir correlation is well studied for galaxies in the local universe for several classes of galaxy morphology like spirals , ellipticals , dwarf irregulars , etc .. Please generate the next two sentences of the article

it is known to hold good at global @xcite as well as at local scales ( few 100 pc to few kpc ) within galaxies @xcite . at the brightest end of fir luminosity , the relationship is observed to hold for ( ultra ) luminous infrared galaxies [ ( u)lirg ] and star - burst galaxies . at the faintest end it holds in dwarf galaxies @xcite .

Suppose that you have an abstract for a scientific paper: we present results from a systematic study of star formation in local galaxy clusters using 22@xmath0 m data from the wide - field infrared survey explorer ( wise ) . the 69 systems in our sample are drawn from the cluster infall regions survey ( cirs ) , and all have robust mass determinations . the all - sky wise data enables us to quantify the amount of star formation , as traced by 22@xmath0 m , as a function of radius well beyond , and investigate the dependence of total star formation rate upon cluster mass . we find that the fraction of star - forming galaxies increases with cluster radius but remains below the field value even at 3 . we also find that there is no strong correlation between the mass - normalized total specific star formation rate and cluster mass , indicating that the mass of the host cluster does not strongly influence the total star formation rate of cluster members . . And you have already written the first three sentences of the full article: it is well - established that the fraction of star - forming galaxies declines as a function of increasing local galaxy density in the low redshift universe . also known as the star formation - density relation @xcite , this correlation has been confirmed in many studies , primarily using optical and uv data to trace star formation in massive galaxy clusters and field environments . mid - infrared data from the infrared satellite observatory ( iso ) and the multi- band imaging photometer for spitzer ( mips ) have also revealed the presence of highly obscured , dusty star forming galaxies , previously undetected by optical or uv surveys ( e.g. * ? ? ?. Please generate the next two sentences of the article

* ; * ? ? ? * ) . while the sensitivity of mips has enabled detailed studies of obscured star formation in individual local and distant galaxy clusters ( e.g. *

Suppose that you have an abstract for a scientific paper: in the last decade the quality and the amount of observational asteroseismic data that has been made available by space based missions had a tremendous upgrowth . the determination of asteroseismic parameters to estimate the fundamental physical processes occurring in stars interiors , can be done today in a way that has never been possible before . in this work we propose to compute the seismic observable @xmath0 , which is a proxy of the phase shift of the acoustic modes propagating in the envelope of the sun - like stars . this seismic parameter @xmath0 can be used to identify rapid variation regions usually known as glitches . we show that a small variation in the structure , smaller than 1% in the sound speed , produces a glitch in the acoustic potential that could explain the oscillatory character of @xmath0 . this method allows us to determine the location and the thickness of the glitch with precision . we applied this idea to the sun - like star @xmath1 centauri a and found a glitch located at approximately @xmath2 ( 1400 s ) and with a thickness of 0.2% of the stars radius . this is fully consistent with the data and also validates other seismic tests . . And you have already written the first three sentences of the full article: asteroseismology was born as a natural extension of helioseismology ( for a recent review see @xcite ) . the success of helioseismology results from the ability to extract information from the sun s interior through accurately measured frequencies of more than 7000 acoustic oscillation modes ( e.g. , @xcite ; @xcite ; @xcite ) . the development of this discipline was instrumental to improve the physics of the solar standard model that led to the resolution of the solar neutrino problem ( e.g. , ; @xcite ) .. Please generate the next two sentences of the article

similarly , asteroseismology is expected to extract information from the interiors of stars at different stages of their evolution , through the study of their observed oscillation spectrum . however , in this case , only global , low degree modes are expected to be detected , due to observational limitations . in the next decade , an unprecedented progress is expected in this research field , in part due to the large amount of data that has been made available by the missions _ @xcite and _ kepler _ @xcite .

Suppose that you have an abstract for a scientific paper: we show that if an interlacing particle system in a two - dimensional lattice is a determinantal point process , and the correlation kernel can be expressed as a double integral with certain technical assumptions , then the moments of the fluctuations of the height function converge to that of the gaussian free field . in particular , we examine a specific particle system that was previously studied in @xcite and compute the corresponding green s function . . And you have already written the first three sentences of the full article: the gaussian free field is widely considered to be a universal object describing the flucutations of heights of random surfaces . previous work has rigorously shown this to be the case in specific models ( @xcite,@xcite ) . in this paper , we show that if an interlacing particle system in two dimensions can be described as a determinantal point process , and mild assumptions are made about the correlation kernel , then the covariances of the fluctuations of the height function are governed by a particular green s function . a general formula for the green s function is given .. Please generate the next two sentences of the article

in particular , we will use this general theorem to show that in an interlacing particle system that arises from the representation theory of the orthogonal groups , the green s function is @xmath0 note that @xmath1 is the green s function for the laplace operator with dirichlet boundary conditions on the set @xmath2 . it turns out that there is a map @xmath3 from the surface to @xmath4 .

Suppose that you have an abstract for a scientific paper: we use the tapering effect of / [ ] rotation curves of spiral galaxies first noted by goad & roberts ( 1981 ) to investigate the internal extinction in disks . the scale length of exponential fits to the inner part of rotation curves depends strongly on the disk axial ratio . preliminary modelling of the effect implies substantial opacity of the central parts of disks at a wavelength of 0.66 @xmath0 . in addition , the average kinematic scale length of rotation curves , when corrected to face on perspective , has a nearly constant value of about @xmath1 kpc , for all luminosity classes . the interpretation of that effect , as the result of the increasing dominance of the baryonic mass in the inner parts of galaxies , yields a mean baryonic mass to light ratio in the i band @xmath2 @xmath3 , within the inner @xmath1 kpc of disks . 83@xmath4 50w@xmath5 = cmr8 = cmbx8 = cmti8 = cmsl8 = cmmi8 + 584 _ use346 6.5 truein . And you have already written the first three sentences of the full article: at optical and near infrared wavelengths , interstellar dust depresses the observed flux of galaxy disks by both scattering and absorption . several authors have proposed that , even in the face on perspective , normal , non starburst disks are optically thick at optical wavelengths , while others have argued for substantial transparency ( see the volume edited by davies & burstein 1995 and the review by calzetti 2001 for details ) . using a sample of spiral galaxies within @xmath6 , we statistically derived photometric solutions for the degree of internal extinction at i band as a function of disk inclination ( giovanelli 1994 ) , finding a difference of more than a magnitude of flux between face on and edge on systems . at the same time , we found evidence for transparency of the outer parts of disks , at radii @xmath7 disk scale lengths from the center . we later reported that the amount of internal extinction is luminosity dependent : more luminous disks being more opaque than less luminous ones ( giovanelli 1995 ) .. Please generate the next two sentences of the article

these results have been confirmed by more recent analyses ( e.g. tully 1998 ; wang & heckman 1996 ) . purely photometric techniques are subject to a peculiar set of selection effects , that can severely affect quantitative conclusions on internal extinction , as witnessed by the liveliness of the debate over the last decade . in 1981 , goad & roberts noted a kinematic effect which can provide an independent test for disk extinction .

Suppose that you have an abstract for a scientific paper: cylindrically symmetric electron beams in spin polarization are reported for the first time . they are shown to be the eigen states of total angular momentum in the @xmath0 direction . but they are neither the eigen states of spin nor the eigen states of orbital angular momentum in that direction . . And you have already written the first three sentences of the full article: both photon beams and electron beams can carry orbital angular momentum . in the case of photon beams , the orbital angular momentum is carried by the spiral wavefront @xcite . photon beams that carry orbital angular momentum have important applications @xcite in micro - machines , atom manipulation , and quantum information . in the case of electron beams ,. Please generate the next two sentences of the article

the orbital angular momentum was also shown @xcite to be carried by the spiral structure of the beam s wavefront when the spin polarization is uniformly distributed . electron beams that carry orbital angular momentum were generated very recently in experiments @xcite by making use of techniques that are similar to those @xcite used for generating photon beams of orbital angular momentum .

Suppose that you have an abstract for a scientific paper: we summarize the x - ray properties of the complete samples of millisecond pulsars ( msps ) detected in our _ chandra _ observations of the globular clusters 47 tuc and ngc 6397 . the 47 tuc msps are predominantly soft sources suggestive of thermal emission from the neutron star polar cap and have x - ray luminosities in a surprisingly narrow range ( 14 10@xmath0 erg s^-1erg s@xmath1 ) . the single msp in ngc 6397 is both hard and apparently extended , probably due to shocked hot gas evaporating from its main sequence companion . in contrast to msps in the field and the cluster m28 , which show correlation between x - ray luminosity and spindown luminosity @xmath2 @xmath3 with @xmath4 1 - 1.4 , the 47 tuc ( and ngc 6397 ) sample display a relatively tight correlation with @xmath5 . the correlations of vs. and light cylinder magnetic field values are also different . it is possible the magnetic field configuration has been altered ( by episodic accretion ) for old msps in dense cluster cores . /cm2secerg @xmath6 s@xmath1 2erg @xmath6 3pc@xmath7 -3cm@xmath7 /skm s@xmath1 a&a 1.25 in .125 in .25 in . And you have already written the first three sentences of the full article: x - ray studies of millisecond pulsars ( msps ) can constrain fundamental properties of their emission regions and , when combined with radio timing studies , their underlying neutron stars ( nss ) . in globular clusters both msps and low mass x - ray binaries ( lmxbs ) , their likely progenitors , are significantly enhanced ( per unit mass ) over their values in the galactic disk by stellar and binary interactions . the dense cluster ( core ) environment needed for their excess formation may also alter their evolution . thus cluster vs. field msps , as studied in x - rays and radio , can constrain intrinsic vs. extrinsic ( evolutionary ) properties of these oldest ns systems .. Please generate the next two sentences of the article

we have conducted a deep _ chandra _ survey for msps as well as quiescent lmxbs and cataclysmic variables ( cvs ) in the globular clusters 47 tuc ( grindlay et al . 2001a ; ghe01a ) and ngc 6397 ( grindlay et al . 2001b ; ghe01b ) .

Suppose that you have an abstract for a scientific paper: electron - deuteron elastic scattering data ( @xmath0 and @xmath1 structure functions and polarization observables @xmath2 , @xmath3 and @xmath4 ) are fit with a model that respects asymptotic properties of pqcd at high momentum transfer . the data analysis shows that pqcd starts from @xmath5 . predictions for the magnetic structure function @xmath1 and the polarization observables at high momentum transfer are given . + * pacs * number(s ) : 13.40.fn , 12.38.bx , 25.30.bf * pqcd phenomenology of elastic @xmath6 scattering * a.p . kobushkin @xmath7 and ya.d . krivenko @xmath8 + @xmath9_n n bogolyubov institute for theoretical physics _ + _ metrologicheskaya str . 14b , kiev , 03143 , ukraine _ + @xmath10_research center for nuclear physics , osaka university ( suita campus ) _ + _ 10 - 1 , mihogaoka ibaraki osaka 567 - 0047 , japan _ + @xmath8_institute for nuclear research _ + _ prospekt nauki 47,kiev , 03028 , ukraine _ . And you have already written the first three sentences of the full article: in recent few years new data from tjinaf on the @xmath6 elastic scattering were reported . they include the electric structure function , @xmath0 , measured with high precision up to @xmath11 @xcite and measurements of tensor polarization observables , @xmath2 , @xmath3 and @xmath4 , up to @xmath12 @xcite . this data , together with data on the magnetic structure function , @xmath1 @xcite , restrict the deuteron structure at scales where quark - gluon degrees of freedom are expected to become defrozen .. Please generate the next two sentences of the article

for example , according to optimistic estimations pqcd should start from @xmath13 of order of few @xmath14 @xcite . it is nice that this prediction was confirmed by analysis of tjinaf data on @xmath0 at @xmath15 @xcite . for further conclusions one also should consider the spin structure of the deuteron from pqcd point of view .

Suppose that you have an abstract for a scientific paper: there is an apparent tension between cosmological parameters obtained from _ planck _ cosmic microwave background radiation observations and that derived from the observed magnitude - redshift relation for the type ia supernova ( sne ia ) . here , we show that the tension can be alleviated , if we first calibrate , with the help of the distance - duality relation , the light - curve fitting parameters in the distance estimation in sne ia observations with the angular diameter distance data of the galaxy clusters and then re - estimate the distances for the sne ia with the corrected fitting parameters . this was used to explore their cosmological implications in the context of the spatially flat cosmology . we find a higher value for the matter density parameter , @xmath0 , as compared to that from the original snls3 , which is in agreement with _ planck _ observations at 68.3% confidence . therefore , the tension between _ planck _ measurements and sne ia observations regarding @xmath0 can be effectively alleviated without invoking new physics or resorting to extensions for the standard concordance model . moreover , with the absolute magnitude of a fiducial sne ia , @xmath1 , determined first , we obtained a constraint on the hubble constant with snls3 alone , which is also consistent with _ planck_. . And you have already written the first three sentences of the full article: the cosmic microwave background radiation ( cmbr ) measurements play a crucial and irreplaceable role in establishing the favored cosmological model , that is , a flat cosmological constant - dominated , cold dark matter model ( @xmath2cdm ) , and constraining the cosmological parameters . it is important , however , to bear in mind that cmbr observations predominantly probe the early universe at high redshift ( @xmath3 ) . as a result , a projection within a given cosmological model is needed when we interpret these observations in terms of the standard cosmological parameters defined at @xmath4 , for instance , the hubble constant , @xmath5 , and the matter density parameter , @xmath0 , which provide basic information and are key parameters of the universe .. Please generate the next two sentences of the article

recently , one of the most exciting events is the release of scientific findings based on data from the first 15.5 months of _ planck _ operations @xcite . because of the high precision , the new _ data could constrain several cosmological parameters at few percent level @xcite . within the context of the spatially flat @xmath2cdm cosmology ,

Suppose that you have an abstract for a scientific paper: in this paper we introduce the strong bishop - phelps - bollobs property ( sbpbp ) for bounded linear operators between two banach spaces @xmath0 and @xmath1 . this property is motivated by a kim - lee result which states , under our notation , that a banach space @xmath0 is uniformly convex if and only if the pair @xmath2 satisfies the sbpbp . positive results of pairs of banach spaces @xmath3 satisfying this property are given and concrete pairs of banach spaces @xmath4 failing it are exhibited . a complete characterization of the sbpbp for the pairs @xmath5 is also provided . . And you have already written the first three sentences of the full article: let @xmath0 and @xmath1 be banach spaces over a real or complex field @xmath6 . we use the traditional notations @xmath7 and @xmath8 for the unit sphere and the closed unit ball of the space @xmath0 , respectively . the banach space of all bounded linear operators @xmath9 will be represented by @xmath10 .. Please generate the next two sentences of the article

in particular , when @xmath11 we denote @xmath12 simply by putting @xmath13 called the dual space of @xmath0 . we say that an operator @xmath14 attains its norm if there exists @xmath15 such that @xmath16 . in this case

Suppose that you have an abstract for a scientific paper: we propose a novel approach , based on principal components analysis , to the use of gamma - ray bursts ( grbs ) as probes of cosmic star formation history ( sfh ) up to very high redshifts . the main advantage of such approach is to avoid the necessity of assuming an _ ad hoc _ parameterization of the sfh . we first validate the method by reconstructing a known sfh from monte carlo - generated mock data . we then apply the method to the most recent _ swift _ data of grbs with known redshift and compare it against the sfh obtained by independent methods . the main conclusion is that the level of star formation activity at @xmath0 could have been already as high as the present - day one ( @xmath1 yr@xmath2 mpc@xmath3 ) . this is a factor 3 - 5 times higher than deduced from high-@xmath4 galaxy searches through drop - out techniques . if true , this might alleviate the long - standing problem of a photon - starving reionization ; it might also indicate that galaxies accounting for most of the star formation activity at high redshift go undetected by even the most deep searches . [ firstpage ] methods : statistical , gamma - ray burst , star formation . And you have already written the first three sentences of the full article: the cosmic star formation history ( sfh ) is an important test for galaxy formation models . experimentally our knowledge of the sfh comes from @xcite up to @xmath5 and from observations of color - selected lyman break galaxies @xcite , ly@xmath6 emitters @xcite , uv+ir measurements @xcite , and grb observations @xcite at higher @xmath4 ( hereafter , these will be refereed to as h2006 , m2007 , b2008 , o2008 , r2008 , c2007 , y2008 and w2009 , respectively ) . however , direct high-@xmath4 measurements constitute an extreme challenge even for the most powerful telescopes and remain sparse . due to their high luminosity grbs. Please generate the next two sentences of the article

can be used as sfh probes into the very distant universe @xcite , potentially to higher redshifts than allowed by galaxies alone . for example , grb 090429b at @xmath7 @xcite is the current record - holder object , followed by a @xmath8 galaxy @xcite and grb 090423 , at @xmath9 @xcite . in principle

Suppose that you have an abstract for a scientific paper: we establish the equivalence between the family of uniformly regular riemannian manifolds without boundary and the class of manifolds with bounded geometry . . And you have already written the first three sentences of the full article: in 2012 , h. amann introduced a class of ( possibly noncompact ) manifolds , called . roughly speaking , an @xmath0-dimensional riemannian manifold @xmath1 is _ uniformly regular _ if its differentiable structure is induced by an atlas such that all its local patches are of approximately the same size , all derivatives of the transition maps are bounded , and the pull - back metric of @xmath2 in every local coordinate is comparable to the euclidean metric @xmath3 . the precise definition of will be presented in section 2 below . in the sequel , we understand all our manifolds to be smooth and without boundary , unless stated otherwise . the main objective of this short note is to prove that the family of coincides with the class of .. Please generate the next two sentences of the article

a manifold is said to be of bounded geometry if it has positive injectivity radius , and all covariant derivatives of the curvature tensor are bounded . the precise definition of bounded geometry will be given later in this introductory section .

Suppose that you have an abstract for a scientific paper: intuitively , the default risk of a single borrower is higher when her or his assets and debt are denominated in different currencies . additionally , the default dependence of borrowers with assets and debt in different currencies should be stronger than in the one - currency case . by combining well - known models by @xcite , @xcite , and @xcite we develop simple representations of pds and asset correlations that take into account exchange rate risk . from these results , consistency conditions can be derived that link the changes in pd and asset correlation and do not require knowledge of hard - to - estimate parameters like asset value volatility . . And you have already written the first three sentences of the full article: if borrowers have only assets that when liquidated generate cash in a local currency different from the currency in which their debt is due , their default risk will be higher than in the one currency case , as a consequence of the additional exchange rate risk . the increase in default risk is reflected both in higher probabilities of default ( pds ) as well as in higher asset correlations between the borrowers . in this note , by modifying merton s model of the default of a firm , we derive some simple relations between the pds without and with exchange rate risk , between the borrowers asset correlations without and with exchange rate risk , and pds and asset correlations when taking account of exchange rate risk . in general , the formulae we derive include as parameters the borrowers asset volatilities , the exchange rate volatility , and the mean logarithmic ratio of the exchange rates at times 1 and 0 . however , assuming independence of the exchange rate and the borrowers asset values as well as zero mean logarithmic ratio of exchange rates at times 1 and 0 yields a relation between the borrowers asset correlation without and with exchange rate risk and the borrowers pds without and with exchange rate risk that does not require knowledge of additional parameters ( see equation ) .. Please generate the next two sentences of the article

in the special case of borrowers with identical individual risk characteristics (= pds ) , relation can be stated as follows : @xmath0 where @xmath1 and @xmath2 denote the original pd and asset correlation without exchange rate risk and @xmath3 and @xmath4 denote the pd and asset correlation when there is additional exchange rate risk . both and can be understood as consistency conditions that should be satisfied when the risk parameters pd and asset correlation are to be adjusted for incorporating exchange rate risk .

Suppose that you have an abstract for a scientific paper: it is well known that the schwarzschild solution describes the gravitational field outside compact spherically symmetric mass distribution in general relativity . in particular , it describes the gravitational field outside a point particle . nevertheless , what is the exact solution of einstein s equations with @xmath0-type source corresponding to a point particle is not known . in the present paper , we prove that the schwarzschild solution in isotropic coordinates is the asymptotically flat static spherically symmetric solution of einstein s equations with @xmath0-type energy - momentum tensor corresponding to a point particle . solution of einstein s equations is understood in the generalized sense after integration with a test function . metric components are locally integrable functions for which nonlinear einstein s equations are mathematically defined . the schwarzschild solution in isotropic coordinates is locally isometric to the schwarzschild solution in schwarzschild coordinates but differs essentially globally . it is topologically trivial neglecting the world line of a point particle . gravity attraction at large distances is replaced by repulsion at the particle neighborhood . . And you have already written the first three sentences of the full article: in this article , we consider the classic problem : find the gravitational field which is produced by a point massive particle . if particle is at rest , then the gravitational field is spherically symmetric and static . the spherically symmetric solution of the vacuum einstein s equations is well known : it is the schwarzschild solution @xcite . therefore , it is often stated that the schwarzschild solution ( in the schwarzschild coordinates ) describes gravitational field of a point particle .. Please generate the next two sentences of the article

this statement is incorrect because there is no @xmath0-type energy - momentum tensor corresponding to a particle on the right hand side of einstein s equations . on the other hand , the solution of einstein s equations outside point massive particle must be isometric to the schwarzschild solution . therefore the natural question arises : `` where is the @xmath0-function ? '' .

Suppose that you have an abstract for a scientific paper: three nearby galaxies which have abnormally high infrared to radio continuum ratios , ngc1377 , ic1953 and ngc4491 , are investigated with a view to understanding the physical origin of their peculiarity . we review the existing data and present new radio continuum measurements along with near - infrared integral - field spectroscopy and molecular gas observations . the three galaxies have low luminosities but starburst - like infrared colors ; in ngc1377 , no synchrotron emission is detected at any wavelength ; in ic1953 , the observed synchrotron component is attributable to the spiral disk alone , and is lacking in the central regions ; the radio spectrum of ngc4491 is unusually flat . we also compare and contrast them with ngc4418 , a heavily extinguished galaxy which shares some attributes with them . after examining various scenarios , we conclude that these galaxies are most likely observed within a few myr of the onset of an intense star formation episode after being quiescent for at least @xmath0myr . this starburst , while heating the dust , has not produced optical signatures nor a normal amount of cosmic rays yet . we briefly discuss the statistics of such galaxies and what they imply for star formation surveys . . And you have already written the first three sentences of the full article: one of the implications from the data collected by the iras mission , combined with extensive radio surveys , is a nearly universal and tight correlation between the far - infrared thermal dust emission and the optically - thin total radio continuum emission ( mixing thermal and synchrotron components ) in normal star - forming galaxies . @xcite have reached this conclusion comparing 60@xmath1 m fluxes with 6.3 cm fluxes from the effelsberg dish , @xcite comparing 40120@xmath1 m fluxes with 21 cm fluxes from westerbork . although the correlation is generally expressed between luminosities , it holds when they are normalized to cancel size and distance effects , and is valid for a very broad range of star formation rate densities ( review by @xcite ) . at centimeter wavelengths ,. Please generate the next two sentences of the article

the radio emission is dominated by non - thermal processes . all models accounting for the constancy of the infrared to radio flux ratios invoke the star formation process as the indirect source of both types of emission , via a production rate of cosmic rays by type - ii supernov proportional to the production rate of heating photons .

Suppose that you have an abstract for a scientific paper: the polyakov loop is the appropriate deconfinement order parameter for yang - mills theories without quarks or with quarks in the adjoint representation of the gauge group . however it is not a physical state of the theory so the information regarding the center group symmetry must be transferred to the physical states . we briefly review how this transfer of information takes place . when adding quarks the center group is no longer a symmetry for matter in the fundamental representation . this feature allows us to explain why color deconfines when chiral symmetry is restored in hot gauge theories with massless quarks . for quarks in the adjoint representation we show that while deconfinement and the chiral transition do not coincide , entanglement between them is still present . finally , we discuss also the chemical potential driven phase transition . recently in we have analyzed the problem of how , and to what extent the information encoded in the order parameter of a generic theory is transferred to the non - order parameter fields . this is a fundamental problem since in nature most fields are non - order parameter fields . this problem is especially relevant in qcd and qcd - like theories since there is no physical observable for deconfinement which is directly linked to the order parameter field . at nonzero temperature the @xmath0 center of @xmath1 is a relevant global symmetry @xcite , and it is possible to construct the polyakov loop @xmath2 operator . this object is charged with respect to the center @xmath0 of the @xmath3 gauge group @xcite , under which it transforms as @xmath4 with @xmath5 . a relevant feature of the polyakov loop is that its expectation value vanishes in the low temperature regime , and is non - zero in the high temperature phase . the polyakov loop is thus a suitable order parameter for the yang - mills temperature driven phase transition @xcite . the question is : how can the information about the yang - mills phase transition encoded in the.... And you have already written the first three sentences of the full article: here we study the behavior of the polyakov loop by treating it as a heavy field that is a singlet under chiral symmetry transformations . we take the underlying theory to be two colors and two flavors in the fundamental representation . the degrees of freedom in the chiral sector of the effective theory are @xmath14 goldstone fields @xmath15 and a scalar field @xmath16 . for @xmath17. Please generate the next two sentences of the article

the potential is @xcite : @xmath18&=&\frac{m^2}{2}{\rm tr } \left[m^{\dagger}m\right]+ { \lambda_1}{\rm tr } \left[m^{\dagger}m\right]^2 + \frac{\lambda_2}{4}{\rm tr } \left[m^{\dagger}mm^{\dagger}m\right ] \label{chiralpot}\end{aligned}\ ] ] with @xmath19 , @xmath20 and @xmath21 . @xmath22 are the generators provided explicitly in equation ( a.5 ) and ( a.6 ) of @xcite .

Suppose that you have an abstract for a scientific paper: three observables of early - type galaxies - size ( @xmath0 ) , surface brightness ( @xmath1 ) , and velocity dispersion ( @xmath2 ) - form a tight planar correlation known as the fundamental plane ( fp ) , which has provided great insights into the galaxy formation and the evolution processes . however , the fp has been found to be tilted against the simple virial expectation , prompting debates on its origin . in order to investigate the contribution of systematic stellar population variation to the fp tilt , we study here the fp relations of early - type galaxies in mid - infrared ( mir ) which may represent the stellar mass well . we examined the wavelength dependence of the fp coefficients , @xmath3 and @xmath4 in @xmath5 , using a sample of 56 early - type galaxies for which visible ( @xmath6-band ) , near - infrared ( @xmath7-band ) , and mir ( spitzer irac , 3.68.0@xmath8 m ) data are available . we find that the coefficient @xmath3 increases as a function of wavelength as @xmath9 , while the coefficient @xmath4 reaches the closest to -1 at 3.65.8@xmath8 m . when applied to the visible fp coefficients derived from a larger sample of nearby early - type galaxies , we get the fp relation with @xmath10 ( 1.61.8,-0.9 ) at 3.6@xmath8 m . our result suggests that the stellar population effect can explain more than half of the fp tilt , closing the gap between the virial expectation and the optical fp . the reduction in the fp tilt is reflected in the dynamical mass - to - light ratio , @xmath11 , dependence on @xmath12 which decreases toward 3.65.8@xmath8 m , suggesting that the mir light better represents mass than the shorter wavelengths . . And you have already written the first three sentences of the full article: in the search for correlations among physical parameters of early - type galaxies , it has been recognized that the effective radius ( @xmath13 ) , the effective mean surface brightness ( @xmath14 ) , and the central velocity dispersion ( @xmath2 ) form a planar relation ( in logarithmic space ) known as the fundamental plane ( hereafter fp ; @xcite ; @xcite ) , in the form of @xmath15 where @xmath3 and @xmath4 are found to be @xmath10 ( 1.21.5,-0.8 ) at visible wavelengths ( @xcite ; @xcite ) . under the assumption of structural homology and a constant mass - to - light ratio , the virial theorem implies that the fp coefficients should be @xmath16=(2,-1 ) the so - called ` virial expectation ' . the observed discrepancy , or tilt of the fp with respect to the virial expectation has prompted many discussions to explain its origin ( see @xcite for a review of this field ) . one of the ideas is that the tilt is caused by the systematic variation in the stellar population as a function of physical parameters such as galaxy luminosity .. Please generate the next two sentences of the article

@xcite investigated this effect by constructing the fp in @xmath7-band , which is supposedly a good tracer of the stellar mass less affected by age and dust . meanwhile , @xcite examined the wavelength dependence on the fp coefficients , and concluded that some of the tilt is caused by the stellar population manifested by the color - magnitude relation .

Suppose that you have an abstract for a scientific paper: sharir and welzl introduced an abstract framework for optimization problems , called _ lp - type problems _ or also _ generalized linear programming problems _ , which proved useful in algorithm design . we define a new , and as we believe , simpler and more natural framework : _ violator spaces _ , which constitute a proper generalization of lp - type problems . we show that clarkson s randomized algorithms for low - dimensional linear programming work in the context of violator spaces . for example , in this way we obtain the fastest known algorithm for the _ @xmath0-matrix generalized linear complementarity problem _ with a constant number of blocks . we also give two new characterizations of lp - type problems : they are equivalent to _ acyclic _ violator spaces , as well as to _ concrete _ lp - type problems ( informally , the constraints in a concrete lp - type problem are subsets of a linearly ordered ground set , and the value of a set of constraints is the minimum of its intersection ) . , , , lp - type problem , generalized linear programming , violator space , clarkson s algorithms , unique sink orientation , generalized linear complementarity problem . And you have already written the first three sentences of the full article: the framework of lp - type problems , invented by sharir and welzl in 1992 @xcite , has become a well - established tool in the field of geometric optimization . its origins are in linear programming : sharir and welzl developed a randomized variant of the dual simplex algorithm for linear programming and showed that this algorithm actually works for a more general class of problems they called lp - type problems . for the theory of linear programming , this algorithm constituted an important progress , since it was later shown to be _ subexponential _ in the ram model @xcite . together with a similar result independently obtained by kalai @xcite , this was the first linear programming algorithm provably requiring a number of arithmetic operations subexponential in the dimension and number of constraints ( independent of the precision of the input numbers ) .. Please generate the next two sentences of the article

for many other geometric optimization problems in fixed dimension , the algorithm by sharir and welzl was the first to achieve expected linear runtime , simply because these problems could be formulated as lp - type problems . the class of lp - type problems for example includes the problem of computing the minimum - volume ball or ellipsoid enclosing a given point set in @xmath1 , and the problem of finding the distance of two convex polytopes in @xmath1 .

Suppose that you have an abstract for a scientific paper: we study the dynamics of a beam of fermions diffracted off a density grating formed by fermionic atoms in the limit of a large grating . an exact description of the system in terms of particle - hole operators is developed . we use a combination of analytical and numerical methods to quantitatively explore the raman - nath and the bragg regimes of diffraction . we discuss the limits in diffraction efficiency resulting from the dephasing of the grating due to the distribution of energy states occupied by the fermions . we propose several methods to overcome these limits , including the novel technique of `` atom echoes '' . . And you have already written the first three sentences of the full article: the availability of quantum - degenerate bosonic atomic systems has recently allowed the extension of atom optics to the nonlinear @xcite and the quantum regimes . matter - wave four - wave mixing @xcite , coherent matter - wave amplification @xcite and superradiance @xcite , the generation of dark @xcite and bright @xcite atomic solitons and of correlated atomic pairs @xcite have been demonstrated , and so has the matter - wave analog of second - harmonic generation , the creation of a molecular condensate component @xcite . in contrast , the development of the nonlinear atom optics of fermionic atomic systems is not nearly as far along .. Please generate the next two sentences of the article

while it has been shown theoretically @xcite that the four - wave mixing of fermionic matter waves is possible in principle , these predictions have not been verified experimentally so far . still , the recent achievement of temperatures as low as @xmath0 , where @xmath1 is the fermi temperature , for the fermions @xmath2k and @xmath3li @xcite is encouraging , and it is hoped that first experiments on fermionic nonlinear atom optics will take place in the near future . in addition to the fundamental goal of achieving a bcs phase transition into pairing and superfluidity @xcite , research along these lines is also motivated by recent results that hint at the possibility to lower the phase noise in interferometric measurements below the bosonic standard quantum limit by using instead degenerate fermionic beams @xcite .

Suppose that you have an abstract for a scientific paper: * globular clusters ; stellar populations ; galaxy formation * the ensemble of all star clusters in a galaxy constitutes its _ star cluster system_. in this review , the focus of the discussion is on the ability of star clusters , particularly the systems of old massive globular clusters ( gcss ) , to mark the early evolutionary history of galaxies . i review current themes and key findings in gcs research , and highlight some of the outstanding questions that are emerging from recent work . [ firstpage ] . And you have already written the first three sentences of the full article: the observational evidence available to date indicates that a major star - forming epoch in a galaxy s history will generate a new set of star clusters that accompanies its population of ` field ' stars . thus , it is physically meaningful to think of a _ subsystem _ of star clusters as consisting of all clusters formed in a given starburst , and to treat the clusters as a proxy for the stellar subpopulation formed in the same burst ( see de grijs 2010 and larsen 2010 for more extensive treatments of cluster formation in starburst environments ) . the huge advantage offered by star clusters is that they are easily bright enough to be measured individually within galaxies as distant as 100 mpc and even beyond , and in giant galaxies particularly , they can be found in large numbers ( see figure 1 ) .. Please generate the next two sentences of the article

we can then construct _ distribution functions _ of such key parameters as mass , age and heavy - element abundance ( metallicity ) for the clusters , instead of just the luminosity - weighted averages that we get from the unresolved field - star light . the milky way star cluster system ( our starting point for all such work and the ` baseline ' comparison system for all other galaxies ) separates out rather cleanly into the two classic subsystems : the _ open clusters _ ( found throughout the disc and spiral arms along low - eccentricity orbits ) and the _ globular clusters _ ( gcs , inhabiting the galactic bulge and halo in a roughly isotropic distribution of orbits ) . in addition , the gcs are distinctly older than the open clusters ( although with a small range of overlap around @xmath010 gyr ) , as well as more massive and less enriched in heavy elements , indicating that they belonged to a brief early stage of rapid star formation and chemical enrichment .

Suppose that you have an abstract for a scientific paper: we study step bunching under conditions of attachment / detachment limited kinetics in the presence of a deposition or sublimation flux , which leads to bunch motion . analysis of the discrete step dynamics reveals that the bunch velocity is inversely proportional to the bunch size for general step - step interactions . the shape of steadily moving bunches is studied within a continuum theory , and analytic expressions for the bunch profile are derived . scaling laws obtained previously for non - moving bunches are recovered asymptotically , but singularities of the static theory are removed and strong corrections to scaling are found . the size of the largest terrace between two bunches is identified as a central scaling parameter . our theory applies to a large class of bunching instabilities , including sublimation with attachment asymmetry and surface electromigration in the presence of sublimation or growth . . And you have already written the first three sentences of the full article: there is much current interest in exploiting morphological instabilities to form periodic nanoscale patterns at crystal surfaces @xcite . because of their natural in - plane anisotropy , vicinal surfaces @xcite prepared at a miscut relative to a high symmetry orientation provide ideal substrates for the formation of ripple patterns parallel or perpendicular to the mean step orientation @xcite . here we specifically consider patterns formed by _. Please generate the next two sentences of the article

step bunching _ , the process in which a train of initially equally spaced ( straight ) steps splits into regions of densely packed steps ( step bunches ) , and almost flat regions @xcite . bunched semiconductor surfaces are promising templates for the growth of metallic nanowires @xcite . step bunching can be induced by growth @xcite , sublimation @xcite , or surface migration of adatoms driven by an electric current @xcite .

Suppose that you have an abstract for a scientific paper: we report the first ground - based detections of the shallow transit of the super - earth exoplanet 55 cnc e using a 2-meter - class telescope . using differential spectrophotometry , we observed one transit in 2013 and another in 2014 , with average spectral resolutions of @xmath0700 and @xmath0250 , spanning the johnson bvr photometric bands . we find a white - light planet - to - star radius ratio of 0.0190@xmath1 from the 2013 observations and 0.0200@xmath2 from the 2014 observations . the two datasets combined results in a radius ratio of 0.0198@xmath3 . these values are all in agreement with previous space - based results . scintillation noise in the data prevents us from placing strong constraints on the presence of an extended hydrogen - rich atmosphere . nevertheless , our detections of 55 cnc e in transit demonstrate that moderate - size telescopes on the ground will be capable of routine follow - up observations of super - earth candidates discovered by the transiting exoplanet survey satellite ( tess ) around bright stars . we expect it will be also possible to place constraints on the atmospheric characteristics of those planets by devising observational strategies to minimize scintillation noise . . And you have already written the first three sentences of the full article: confirmation , follow - up , and atmospheric characterization of a large number of super - earths and smaller planets will be among the main challenges facing exoplanet researchers in the next decade , especially once missions such as tess @xcite start identifying numerous candidates around bright , nearby stars . current follow - up plans include the confirmation of those planet candidates using well tested ultra - high precision radial velocity instruments like harps and harps - n ( see e.g. * ? ? ? * ) , and future instruments like espresso on the vlt @xcite , g - clef on the gmt @xcite , and codex on the e - elt @xcite and the atmospheric characterization of the most interesting confirmed planets using future ground - based ( e.g. gmt , tmt , and e - elt ) , and space - based ( e.g. jwst ) facilities .. Please generate the next two sentences of the article

however , not much attention is being paid to the potential role of smaller ground - based telescopes in the confirmation and follow - up of those planets . while there is some work underway to build small arrays of robotic telescopes for radial velocity and photometric follow - up , e.g. project minerva , the full capacity of moderate - size existing telescopes and instruments for this task has not been explored yet . in this letter

Suppose that you have an abstract for a scientific paper: we present a theoretical analysis of the proximity effect at a graphene - superconductor interface . we use a tight - binding model for the electronic states in this system which allows to describe the interface at the microscopic level . two different interface models are proposed : one in which the superconductor induces a finite pairing in the graphene regions underneath , thus maintaining the honeycomb structure at the interface and one that assumes that the graphene layer is directly coupled to a bulk superconducting electrode . we show that properties like the andreev reflection probability and its channel decomposition depend critically on the model used to describe the interface . we also study the proximity effect on the local density of states on the graphene . for finite layers we analyze the induced _ minigap _ and how it is reduced when the length of the layer increases . results for the local density of states profiles for finite and semi - infinite layers are presented . . And you have already written the first three sentences of the full article: the possibility to isolate and perform direct transport measurements on few or even single graphite layers @xcite has triggered a large activity in the condensed matter community . the case of a single layer of carbon atoms , known as graphene , is of particular interest because of its unique electronic structure which , under certain conditions corresponds to massless dirac fermions confined in two dimensions @xcite . on the other hand , the coupling to a superconductor provides an interesting way to test the electronic properties of graphene . in a recent work by beenakker. Please generate the next two sentences of the article

@xcite it was shown that for an ideal interface between a superconductor and graphene an unusual type of andreev reflection , in which the hole is specularly reflected , appears . several other effects involving graphene and superconductors like josephson transport @xcite , re - entrance effect @xcite , and quasiparticle transport mediated by multiple andreev processes @xcite have been theoretically analyzed .

Suppose that you have an abstract for a scientific paper: we construct default - free interest rate models in the spirit of the well - known markov funcional models : our focus is analytic tractability of the models and generality of the approach . we work in the setting of state price densities and construct models by means of the so called propagation property . the propagation property can be found implicitly in all of the popular state price density approaches , in particular heat kernels share the propagation property ( wherefrom we deduced the name of the approach ) . as a related matter , an interesting property of heat kernels is presented , too . * key wordes * : interest rate models , markov - functional , state price density , heat kernel . . And you have already written the first three sentences of the full article: the _ heat kernel approach _ ( hka for short ) , which will be presented and discussed in this paper , is a systematic method to construct state price densities which are analytically tractable . to be precise on analytic tractability , we mean with this notion that bond prices can be calculated explicitly , and that caps , swaptions or other derivatives on bonds can be calculated up to one integration with respect to the law of the underlying factor markov process . therefore such models can be easily calibrated to market data and are useful for pricing and hedging purposes , but also for purposes of risk management . the original motivation of introducing the hka was in modelling of interest rates with jumps .. Please generate the next two sentences of the article

in the hjm framework @xcite , the drift condition becomes quite complicated ( see h. shirakawa s pioneering work @xcite , see also @xcite and references therein ) if taking jumps into account , while in the spot rate approach , one will find it hard to obtain explicit expressions of the bond prices ( the affine class is almost the only exception ) . in @xcite , the state price density approach . ] is applied and by means of transition probability densities of some lvy processes explicit expressions of the zero coupon bond prices are obtained .

Suppose that you have an abstract for a scientific paper: in a previous paper , a bound on the negative energy density seen by an arbitrary inertial observer was derived for the free massless , quantized scalar field in four - dimensional minkowski spacetime . this constraint has the form of an uncertainty principle - type limitation on the magnitude and duration of the negative energy density . that result was obtained after a somewhat complicated analysis . the goal of the current paper is to present a much simpler method for obtaining such constraints . similar `` quantum inequality '' bounds on negative energy density are derived for the electromagnetic field , and for the massive scalar field in both two and four - dimensional minkowski spacetime . = cmbx10 scaled 4 -36pt 0.64 cm 0.64 cm gr - qc/9607003 + tutp-96 - 2 + july 1 , 1996 + revised oct . 2 , 1996 restrictions + + + + .7 in l.h . ford and thomas a. roman + .2 in institute of cosmology + department of physics and astronomy + tufts university + medford , massachusetts 02155 + . And you have already written the first three sentences of the full article: in quantum field theory , unlike in classical physics , the energy density may be unboundedly negative at a spacetime point . such situations entail violations of all the known classical pointwise energy conditions , such as the weak energy condition @xcite . this fact has been known for quite sometime @xcite .. Please generate the next two sentences of the article

specific examples include the casimir effect @xcite and squeezed states of light @xcite , both of which have observational support . the theoretical prediction of black hole evaporation @xcite also involves negative energy densities and fluxes in a crucial way . on the other hand ,

Suppose that you have an abstract for a scientific paper: a complete scheme for production , cooling , acceleration , and ring for a 1.5 tev center of mass muon collider is presented , together with parameters for two higher energy machines . the schemes starts with the front end of a proposed neutrino factory that yields bunch trains of both muon signs . six dimensional cooling in long - period helical lattices reduces the longitudinal emittance until it becomes possible to merge the trains into single bunches , one of each sign . further cooling in all dimensions is applied to the single bunches in further helical lattices . final transverse cooling to the required parameters is achieved in 50 t solenoids . .5 in .parameters of three muon colliders . note 1 : depth is relative to any nearby low land , e.g. fox river at fnal . note 2 : survival is from the end of phase rotation to the collider ring . [ cols="<,^,^,^ " , ] [ tuneshift ] note that @xmath0 is larger at earlier cooling stages to allow for losses . the first order shifts can be corrected by increasing the focus strength , but tune spreads of half the shifts can not be corrected . before the merge , the shifts are small because the numbers of muons per bunch are small . the only 6d cooling stage with significant tune shift is the last ( # 8) . its tune accepted @xmath1 which is 5 times the calculated maximum full tune spread of @xmath2 7.3% , and is not expected to be a problem . the tune shifts in the 50 t cooling will be significant only during the reaccelerations , where we have assumed @xmath3s corresponding to 3 t focusing fields . the design of these lattices to accept such tune shifts appears possible , although we are clearly nearing the limit . . And you have already written the first three sentences of the full article: there is a serious question as to whether the specified gradients of rf cavities operating under vacuum would operate in the specified magnetic fields . this is under study by nfmcc collaboration @xcite and alternative designs using high pressure hydrogen gas , or open cell rf with solenoids in the irises , are being considered . the bunching and phase rotation will be optimized for the muon collider , instead of being copied from a neutrino factory . instead of the slow helices. Please generate the next two sentences of the article

, a planar wiggler lattice is being studied that would cool both muon signs simultaneously , thus greatly simplifying the system . the use of more , but lower field ( e.g. , 35 t ) final cooling solenoids is also under study .

Suppose that you have an abstract for a scientific paper: an isospin analysis of @xmath0 decays yields @xmath1 , where @xmath2 is the usual ckm angle @xmath3 $ ] without hadronic uncertainty if isospin is a perfect symmetry . yet isospin symmetry is broken not only by electroweak effects but also by the @xmath4 and @xmath5 quark mass difference the latter drives @xmath6 mixing and converts the isospin - perfect triangle relation between the @xmath7 amplitudes to a quadrilateral . the error incurred in @xmath1 through the neglect of the resulting isospin - violating effects can be significant , particularly if @xmath1 is small . . And you have already written the first three sentences of the full article: in the standard model , cp violation is characterized by a single phase in the cabibbo - kobayashi - maskawa ( ckm ) matrix , rendering its elements complex . the ckm matrix is also unitary , so that determining whether or not this is empirically so is a central test of the standard model s veracity @xcite . ascertaining whether the angles of the unitarity triangle , @xmath2 , @xmath8 , and @xmath9 , empirically sum to @xmath10 and whether its angles are compatible with the measured lengths of its sides lie at the heart of these tests of the standard model .. Please generate the next two sentences of the article

we study the impact of isospin violation on the extraction of @xmath1 from an isospin analysis in decays @xcite . isospin is broken not only by electroweak effects but also by the @xmath4 and @xmath5 quark mass difference .

Suppose that you have an abstract for a scientific paper: we propose a novel technique for analyzing the long - time asymptotics of integrable wave equations in the case when the underlying isospectral problem has purely discrete spectrum . to this end , we introduce a natural coupling problem for entire functions , which serves as a replacement for the usual riemann hilbert problem , which does not apply in these cases . as a prototypical example , we investigate the long - time asymptotics of the dispersionless camassa holm equation . . And you have already written the first three sentences of the full article: integrable wave equations play a key role in understanding numerous phenomena in science . in this connection , understanding the long - time asymptotics of solutions is crucial . roughly speaking , the typical behavior is that any ( sufficiently fast ) decaying initial profile splits into a number of solitons plus a decaying dispersive part . this has been first observed numerically for the korteweg de vries equation @xcite .. Please generate the next two sentences of the article

corresponding asymptotic formulas were derived and justified with increasing level of rigor over the last thirty years . to date , the most powerful method for deriving such long - time asymptotics is the nonlinear steepest descent method from deift and zhou @xcite , which was inspired by earlier work of manakov @xcite and its @xcite . more on this method and its history can be found in the survey @xcite ; an expository introduction to this method for the korteweg de vries equation can be found in @xcite .

Suppose that you have an abstract for a scientific paper: the problem of determining the angle at which a point mass launched from ground level with a given speed is a standard exercise in mechanics . similar , yet conceptually and calculationally more difficult problems have been suggested to improve student proficiency in projectile motion . the problem of determining the maximum distance of a rock thrown from a rotating arm motion is presented and analyzed in detail in this text . the calculational results confirm several conceptually derived conclusions regarding the initial throw position and provide some details on the angles and the way of throwing ( underhand or overhand ) which produce the maximum throw distance . + + to be published in * the physics teacher . * . And you have already written the first three sentences of the full article: the problem of determining the angle @xmath0 at which a point mass launched from ground level with a given speed @xmath1 will reach a maximum distance is a standard exercise in mechanics . there are many possible ways of solving this problem @xcite , leading to the well - known answer of @xmath2 , producing a maximum range of @xmath3 , with @xmath4 being the free - fall acceleration . conceptually and calculationally more difficult problems have been suggested to improve student proficiency in projectile motion @xcite , with the most famous example being the tarzan swing problem @xcite .. Please generate the next two sentences of the article

the problem of determining the maximum distance of a point mass thrown from constant - speed circular motion is presented and analyzed in detail in this text . the calculational results confirm several conceptually derived conclusions regarding the initial throw position and provide some details on the angles and the way of throwing ( underhand or overhand ) which produce the maximum throw distance . the situation analyzed in this text

Suppose that you have an abstract for a scientific paper: we provide the first non - trivial result on dynamic breadth - first search ( bfs ) in external - memory : for general sparse undirected graphs of initially @xmath0 nodes and @xmath1 edges and monotone update sequences of either @xmath2 edge insertions or @xmath2 edge deletions , we prove an amortized high - probability bound of @xmath3 i / os per update . in contrast , the currently best approach for static bfs on sparse undirected graphs requires @xmath4 i / os . ulrich meyer . And you have already written the first three sentences of the full article: breadth first search ( bfs ) is a fundamental graph traversal strategy . it can also be viewed as computing single source shortest paths on unweighted graphs . it decomposes the input graph @xmath5 of @xmath0 nodes and @xmath6 edges into at most @xmath0 levels where level @xmath7 comprises all nodes that can be reached from a designated source @xmath8 via a path of @xmath7 edges , but can not be reached using less than @xmath7 edges .. Please generate the next two sentences of the article

the objective of a dynamic graph algorithm is to efficiently process an online sequence of update and query operations ; see @xcite for overviews of classic and recent results . in our case we consider bfs under a sequence of either @xmath2 edge insertions , but not deletions ( _ incremental _ version ) or @xmath2 edge deletions , but not insertions ( _ decremental _ version ) .

Suppose that you have an abstract for a scientific paper: environmental monitoring is often performed through a wireless sensor network , whose nodes are randomly deployed over the geographical region of interest . sensors sample a physical phenomenon ( the so - called field ) and send their measurements to a _ sink _ node , which is in charge of reconstructing the field from such irregular samples . in this work , we focus on scenarios of practical interest where the sensor deployment is unfeasible in certain areas of the geographical region , e.g. , due to terrain asperities , and the delivery of sensor measurements to the sink may fail due to fading or to transmission collisions among sensors simultaneously accessing the wireless medium . under these conditions , we carry out an asymptotic analysis and evaluate the quality of the estimation of a @xmath0-dimensional field ( @xmath1 ) when the sink uses linear filtering as a reconstruction technique . specifically , given the matrix representing the sampling system , @xmath2 , we derive both the moments and an expression of the limiting spectral distribution of @xmath3 , as the size of @xmath2 goes to infinity and its aspect ratio has a finite limit bounded away from zero . by using such asymptotic results , we approximate the mean square error on the estimated field through the @xmath4-transform of @xmath3 , and derive the sensor network performance under the conditions described above . . And you have already written the first three sentences of the full article: recently , a great deal of attention has been payed to wireless sensor networks whose nodes sample a physical phenomenon ( hereinafter referred to as field ) , i.e. , air temperature , light intensity , pollution levels or rain falls , and send their measurements to a central processing unit ( or _ sink _ node ) . the sink is in charge of reconstructing the sensed field : if the field can be approximated as bandlimited in the time and space domain , then an estimate of the discrete spectrum can be obtained . however , the sensors measurements typically represent an irregular sampling of the field of interest , thus the sink operates based on a set of field samples that are not regularly spaced in the time and space domain .. Please generate the next two sentences of the article

the reasons for such an irregular sampling are multifold . ( i ) the sensors may be irregularly deployed in the geographical region of interest , either due to the adopted deployment procedure ( e.g. , sensors thrown out of an airplane @xcite ) , or due to the presence of terrain asperities and obstacles .

Suppose that you have an abstract for a scientific paper: accurate qed calculations of the interelectron interaction corrections for the @xmath0 , @xmath1 two - electron configurations for ions with nuclear charge numbers @xmath2 are performed within the line profile approach . total energies of these configurations are evaluated . employing the fully relativistic treatment based on the coupling scheme these energy levels become quasi - degenerate in the region @xmath3 . to treat such states within the framework of qed we utilize the line profile approach . the calculations are performed within the coulomb gauge . . And you have already written the first three sentences of the full article: to provide accurate quantum - electrodynamical ( qed ) evaluations of energy levels for two- and three - electron configurations of highly charged ions ( hci ) become now an urgent problem in atomic physics . this can be explained by the growing number of experimental data and the necessity to use the energy levels for the evaluation of important characteristics of hci , such as e.g. transition probabilities and recombination cross sections . in the past an approximate relativistic approach based on variational non - relativistic wave functions has been used for evaluating energy levels @xcite .. Please generate the next two sentences of the article

numerous theoretical results for few - electron ions have been obtained within the framework of fully relativistic many - body perturbation theory ( rmbpt ) and relativistic all - order many - body theory ( ao ) @xcite . however , rigorous qed results , which allow for a consequent order - by - order improvement of the accuracy of the calculations become more and more desirable .

Suppose that you have an abstract for a scientific paper: using recent observational constraints on cosmological density parameters , together with recent mathematical results concerning small volume hyperbolic manifolds , we argue that , by employing pattern repetitions , the topology of nearly flat small hyperbolic universes can be observationally undetectable . this is important in view of the facts that quantum cosmology may favour hyperbolic universes with small volumes , and from the expectation , coming from inflationary scenarios , that @xmath0 is likely to be very close to one . it is well known that general relativity is a local metrical theory and therefore the corresponding einstein field equations do not fix the global topology of spacetime . this freedom has resulted in a great deal of interest in the possibility that the universe may possess compact spatial sections with a non - trivial topology , which do not necessarily have positive curvature ( see for example @xcite @xcite and references therein ) . interest in such spaces has also come from quantum cosmology , where the existence of the wave function of the universe may require finiteness of the spatial sections ( see for example @xcite ) . also , in the ` tunnelling from nothing ' scenario , manifolds with small compact spatial sections may be more likely to emerge @xcite . furthermore , there is a precise sense in which most compact @xmath1-manifolds are hyperbolic @xcite . together these facts have motivated the study of hyperbolic manifolds with non - trivial topology as possible models for our universe . there has also been two other important developments recently : one observational , the other mathematical . regarding the former , recent observations seem to indicate that the ratio of the total density to the critical density of the universe , @xmath0 , is likely to be very close to one @xcite , with a significant proportion of this energy being in the form of a dark component with negative pressure @xcite . regarding the latter , we first of all.... And you have already written the first three sentences of the full article: we are grateful to andrew przeworski for very helpful correspondence concerning his work , jeff weeks for many useful comments , and neil cornish for drawing our attention to the reference @xcite . we also thank faperj and cnpq for the grants under which this work was carried out . figure 1 : : the solutions curve of @xmath34 , as plots of @xmath0 ( vertical axis ) versus @xmath48 ( horizontal axis ) , with @xmath2 taken as @xmath10 ( upper curve ) and @xmath38 ( lower curve ) , respectively .. Please generate the next two sentences of the article

the depth of the survey in both cases correspond to a redshift @xmath51 ( cmbr ) . included also is a dashed rectangular box , representing the relevant part , for our purposes , of the hyperbolic region of the parameter space given by recent observations .

Suppose that you have an abstract for a scientific paper: the major biochemical networks of the living cell , the network of interacting genes and the network of biochemical reactions , are highly interdependent , however , they have been studied mostly as separate systems so far . in the last years an appropriate theoretical framework for studying interdependent networks has been developed in the context of statistical physics . here we study the interdependent network of gene regulation and metabolism of the model organism _ escherichia coli _ using the theoretical framework of interdependent networks . in particular we aim at understanding how the biological system can consolidate the conflicting tasks of reacting rapidly to ( internal and external ) perturbations , while being robust to minor environmental fluctuations , at the same time . for this purpose we study the network response to localized perturbations and find that the interdependent network is sensitive to gene regulatory and protein - level perturbations , yet robust against metabolic changes . this first quantitative application of the theory of interdependent networks to systems biology shows how studying network responses to localized perturbations can serve as a useful strategy for analyzing a wide range of other interdependent networks . a main conceptual approach of current research in the life sciences is to advance from a detailed analysis of individual molecular components and processes towards a description of biological _ systems _ and to understand the emergence of biological function from the interdependencies on the molecular level . supported by the diverse high - throughput omics technologies , the relatively recent discipline of systems biology has been the major driving force behind this new perspective which becomes manifest , for example , in the effort to compile extensive databases of biological information to be used in genome - scale models @xcite . despite its holistic game plan , however , systems biology frequently operates on the level.... And you have already written the first three sentences of the full article: the core object of our investigation is an _ e. coli _ network representation of its combined gene regulation and metabolism , which can be thought of as functionally divided into three _ domains _ : the representation captures both gene regulatory and metabolic processes , with these processes being connected by an intermediate layer that models both , the enzymatic influence of genes on metabolic processes , as well as signaling - effects of the metabolism on the activation or inhibition of the expression of certain genes . the underlying interaction graph @xmath1 with its set of nodes ( vertices ) @xmath2 and links ( edges ) @xmath3 consists of three interconnected subgraphs , the gene regulatory domain @xmath4 , the interface domain @xmath5 and the metabolic domain @xmath6 . from the functional perspective , @xmath7 is the union of gene regulatory ( @xmath4 ) and metabolic processes ( @xmath6 ) , and their interactions and preparatory steps form the interface ( @xmath5 ). Please generate the next two sentences of the article

. figure [ fig : sketch ] shows a sketch of the network model . a sketch of the domain organization of the integrative _ e. coli _ network . the regulatory domain , @xmath4 , at the top is connected to the metabolic domain , @xmath6 , shown at the bottom via a protein - interface layer , @xmath5 .

Suppose that you have an abstract for a scientific paper: we demonstrate that the presence of a velocity - dependent term in the phenomenological optical potential simulates a source of nonlocality . this is achieved by showing that , in the interior of the nucleus , the nonlocal wave functions are different from the corresponding local ones obtained in the absence of the velocity - dependent term in accordance with the perey effect . it is also shown that the enhancement or suppression of the nonlocal wave function is energy as well as angular momentum dependent . the latter is in line with the results of previous works that introduced parity dependent terms in the conventional optical potential . keywords : damping factor , perey effect , optical potential . . And you have already written the first three sentences of the full article: it is a well known fact that the nonrelativistic nucleon - nucleus optical potential is nonlocal and energy dependent feschbach_ann , feschbach_book . nevertheless , a common approach to studying the elastic @xmath0 scattering is the use of phenomenological local optical models , and a variation of the model parameters with the incident projectile energy can be taken as a sign of the presence of nonlocal effects in the scattering process @xcite . for example , a recent work presented local and global optical potentials for neutron and proton elastic scattering from nuclei that fall in the mass range @xmath1 @xcite , while nucleon incident energies ranged from 1 kev to 200 mev .. Please generate the next two sentences of the article

the authors obtained excellent elastic angular distribution fits using local optical potentials each consisting of 20 fit parameters , however , the strength of the central real part showed the largest variation with incident energy . another measure of nonlocality is given by the size of the perey damping factor , as will be discussed in the present study for the case of the presence of a gradient term in the optical potential .

Suppose that you have an abstract for a scientific paper: we present a fast and efficient method to compute the inclusive two - particle two - hole ( 2p-2h ) electroweak responses in the neutrino and electron quasielastic inclusive cross sections . the method is based on two approximations . the first neglects the motion of the two initial nucleons below the fermi momentum , which are considered to be at rest . this approximation , which is reasonable for high values of the momentum transfer , turns out also to be quite good for moderate values of the momentum transfer @xmath0 . the second approximation involves using in the `` frozen '' meson - exchange currents ( mec ) an effective @xmath1-propagator averaged over the fermi sea . within the resulting `` frozen nucleon approximation '' , the inclusive 2p-2h responses are accurately calculated with only a one - dimensional integral over the emission angle of one of the final nucleons , thus drastically simplifying the calculation and reducing the computational time . the latter makes this method especially well - suited for implementation in monte carlo neutrino event generators . neutrino scattering , meson - exchange currents , 2p-2h . 25.30.pt , 25.40.kv , 24.10.jv . And you have already written the first three sentences of the full article: the analysis of modern accelerator - based neutrino oscillation experiments requires good control over the intermediate - energy neutrino - nucleus scattering cross section @xcite . in particular the importance of multi - nucleon events has been suggested in many calculations of charge - changing quasielastic cross sections @xmath2 , at typical neutrino energies of @xmath3 gev @xcite . the contribution of two - particle - two - hole ( 2p-2h ) excitations is now thought to be essential for a proper description of data @xcite .. Please generate the next two sentences of the article

thus a growing interest has arisen in including 2p-2h models into the monte carlo event generators used by the neutrino collaborations @xcite . the only 2p-2h model implemented up to date in some of the monte carlo neutrino event generators corresponds to the so - called ific valencia model @xcite , which has been incorporated in genie @xcite .

Suppose that you have an abstract for a scientific paper: recent researches on the solution of schwinger - dyson equations , as well as lattice simulations of pure qcd , suggest that the gluon propagator is massive . in this letter , we assume that the classical counterpart of this massive gluon field may be represented with the equation of motion for yang - mills theory with a mass term added . a new classical solution is given for this equation . it is discussed that this solution may have some role in confinement . these days , evidences are accumulating that the lattice qcd , which is equivalent to the real qcd , dynamically acquires mass from analytical and lattice studies@xcite ( and see @xcite for a list of references ) . the analytical studies with the schwinger - dyson equation ( sde ) nicely agree @xcite with the lattice data . those sde analyses are based on landau gauge . in this letter , the classical counterpart of massive gluons in the landau gauge is considered . in the next section , a new classical solution is given for the equation of motion , and its relation to confinement is discussed . the mechanism here will equally be valid as far as the theory has a mass but the color symmetry is unbroken . though this theory is intended to give insight into real qcd , a non - qcd toy model is additionally analyzed in section 2 . this model is not for the real world but for facilitating analysis in a toy world . this model shows interesting behavior of the mass gap and absence of colored states . . And you have already written the first three sentences of the full article: we assume that the classical limit of the massive gluons is represented by the equation of motion with a mass : - d _ f _ - m^2 a _ = 0 , [ eqm ] where f_^a = _ a_^a - _ a_^a + g f_abc a_^b a_^c , and @xmath0 is the covariant derivative . the landau - gauge condition @xmath1 follows from this equation by applying @xmath2 on the equation . at the zeroth order in @xmath3 , we find the following solution & & a_0 = 0 , + & & a = ^-1(_2 t + _ 3 t ) h_0(z , r ) , [ h0 ] where h_0 = ( _ x , _ y , _ z - ( m^2 -^2 ) dz ) ( z , r ) , with @xmath4 and @xmath5 . the electric and magnetic field is e^a & = & -a_0^a - i g f_abca^b a_0^c - ^a , + b^a & = & a^a .. Please generate the next two sentences of the article

this solution may be interpreted as having two point charges placed at @xmath6 and @xmath7 with the opposite signs . this electric field has no divergence @xmath8 except for the points on the charges with the magnitude @xmath9 .

Suppose that you have an abstract for a scientific paper: we show existence of a global weak dissipative solution of the cauchy problem for the two - component camassa holm ( 2ch ) system on the line with nonvanishing and distinct spatial asymptotics . the influence from the second component in the 2ch system on the regularity of the solution , and , in particular , the consequences for wave breaking , is discussed . furthermore , the interplay between dissipative and conservative solutions is treated . . And you have already written the first three sentences of the full article: we show existence of a weak global dissipative solution of the cauchy problem for the two - component camassa holm ( 2ch ) system with arbitrary @xmath0 and @xmath1 , given by [ eq : chsys2a ] @xmath2 with initial data @xmath3 and @xmath4 . the initial data may have nonvanishing limits at infinity , that is , @xmath5 the 2ch system was first analyzed by constantin and ivanov @xcite . global existence , well - posedness and blow - up conditions have been further studied in a sobolev setting in @xcite and in besov spaces in @xcite . the scalar ch equation. Please generate the next two sentences of the article

( i.e. , with @xmath6 identically equal to zero ) , was introduced and studied by camassa and holm in the fundamental paper @xcite , see also @xcite , and its analysis has been pervasive . the ch equation possesses many intriguing properties .

Suppose that you have an abstract for a scientific paper: we present a theory of the electron structure and the zeeman effect for the helical edge states emerging in two - dimensional topological insulators based on hgte / hgcdte quantum wells with strong natural interface inversion asymmetry . the interface inversion asymmetry , reflecting the real atomistic structure of the quantum well , drastically modifies both bulk and edge states . for the in - plane magnetic field , this asymmetry leads to a strong anisotropy of the edge - state effective @xmath0-factor which becomes dependent on the edge orientation . the interface inversion asymmetry also couples the counter propagating edge states in the out - of - plane magnetic field leading to the opening of the gap in the edge - state spectrum by arbitrary small fields . . And you have already written the first three sentences of the full article: hgte / cdhgte quantum wells ( qws ) of thickness above a critical value belong to the class of @xmath1 two - dimensional topological insulators characterized by the existence of counter propagating helical edge modes @xcite . continuous advance in the technology of cdhgte - based heterostructures stimulates experimental and theoretical studies of their electronic properties related to the non - trivial band topology . the structure of the edge states responsible for the emergence of the quantum spin hall effect was theoretically studied at zero magnetic field @xcite , in the presence of magnetic field lying in the qw plane @xcite , and in magnetic field normal to the qw plane @xcite .. Please generate the next two sentences of the article

most of the theoretical papers consider simplified models which do not take into account the natural inversion asymmetry of the hgte / cdhgte qws caused by their atomic structure or treat this asymmetry as a small perturbation @xcite . contrary , atomistic calculations performed recently @xcite have revealed very strong level repulsion in hgte / cdhgte qws , mostly driven by the natural interface inversion asymmetry of the zinc - blende heterostructures , which results in a considerable modification of the `` bulk '' ( two - dimensional ) electron states and dispersion .

Suppose that you have an abstract for a scientific paper: the more than 80 nearby galaxies imaged with the chandra advanced ccd imaging spectrometer have been analyzed in a search for ultra - luminous x - ray ( ulx ) sources . the sample of galaxies span the range of hubble morphological types and include galaxies of various mass , gas content , and dynamical state . x - ray characteristics of the resulting ensemble of ulx candidates are reported and correlations with properties of the host galaxies are presented . support for this research was provided in part by nasa / chandra grant ar2 - 3008x to d.a.s . . And you have already written the first three sentences of the full article: among the most intriguing objects in the x - ray sky are the non - nuclear ultra - luminous x - ray ( ulx ) sources in nearby galaxies . this name describes those sources considerably more luminous than expected for a spherically - accreting object of typical neutron star mass . here , we define ulx sources to be those with apparent ( i.e. , assumed isotropically emitting ) intrinsic luminosities in excess of @xmath0 erg / s in the 0.5 - 8.0 kev bandpass . through the first 2 years or so of operation , the chandra x - ray observatory ( cxo ) has imaged enough nearby galaxies using the acis ccd imaging spectrometer to undertake a systematic and uniform analysis of their ulx population . ultimately , we wish to know the full pedigree of these extreme objects : what are their origins and history ; why and how do they differ from their more - common low - lumiosity cousins ; what does the population of ulx sources reveal about the nature of galaxy formation and evolution ; and what influence do ulx sources have on their local environments ? here , we report principally the correlations between ulxs and global properties of their host galaxies .. Please generate the next two sentences of the article

based on integration time and the best distance estimate available , we selected all those galaxies for which @xmath1100 source counts are expected from a ulx . in integration time units of ks and distances in mpc , this corresponds to observations with @xmath20.12 . to date , 85 galaxies in the cxc public archive meet this selection criterion . for all candidate galaxy acis images ,

Suppose that you have an abstract for a scientific paper: if neutrino conversions within the sun result in partial polarization of initial solar neutrino fluxes then a new opportunity to distinguish majorana and dirac neutrinos by measuring the differential @xmath0-scattering cross section in solar neutrino detectors arises . the experiment like hellaz would be preferable in testing of recoil electron spectra differences initiated by majorana and dirac neutrinos since low energy recoil electrons ( @xmath1 ) can be detected and electron energy and direction can be determined with good precision . pacs codes : 13.10.+q ; 13.15.-f ; 13.40.fn ; 14.60.gh ; 96.60.kx . * key words * : neutrino , magnetic moment , magnetic fields , polarization . -1 cm 8.5 in 0.3 cm * can we distinguish majorana and dirac neutrinos in solar neutrino experiments ? * * v.b . semikoz * . And you have already written the first three sentences of the full article: lower bounds on neutrino masses have not been found yet in direct laboratory experiments . in particular , in the case of neutrinoless double - beta decay one expects a decrease of an upper bound on the majorana mass @xmath2 only . this current improvement of upper limits on neutrino masses takes a long time and strong efforts .. Please generate the next two sentences of the article

however , we can not justify on this way whether neutrino is really the majorana particle or it can be the dirac one , or a mixture of them ( zkm - neutrino ) . in this connection let us recall the old experiment by davis@xcite who demonstrated that neutrino and antineutrino are indeed different particles if we are using @xmath3 from the beta - decay @xmath4 as the incident `` neutrino '' for the capture process @xmath5 .

Suppose that you have an abstract for a scientific paper: gw vir variables are the pulsating members in the spectroscopic class of the pg 1159 stars . in order to understand the characteristic differences between pulsating and non - pulsating pg1159 stars , we analyse fuse spectra of eleven objects , of which six are pulsating , by means of state - of - the - art nlte model atmospheres . the numerous metal lines in the fuv spectra of these stars allow a precise determination of the photospheric parameters . we present here preliminary results of our analysis . . And you have already written the first three sentences of the full article: gw vir variables belong to the spectroscopic class of the pg 1159 stars ( wesemael , green & liebert 1985 ) , which is named after the prototype pg 1159@xmath0035 . these objects are strongly hydrogen - deficient post - agb stars which pass through the hottest stage of stellar evolution . their effective temperatures range between 75 000 and 200 000k , surface gravities vary from @xmath1 $ ] .. Please generate the next two sentences of the article

the so - called born - again scenario ( a late thermal pulse which transferred these objects back to the agb followed by a second post - agb evolution , iben et al . 1983 ) is mainly accepted as an explanation for the h - deficiency and can reproduce well the observed abundances .

Suppose that you have an abstract for a scientific paper: the saturation mechanism of magneto - rotational instability ( mri ) is examined through analytical quasilinear theory and through nonlinear computation of a single mode in a rotating disk . we find that large - scale magnetic field is generated through the alpha effect ( the correlated product of velocity and magnetic field fluctuations ) and causes the mri mode to saturate . if the large - scale plasma flow is allowed to evolve , the mode can also saturate through its flow relaxation . in astrophysical plasmas , for which the flow can not relax because of gravitational constraints , the mode saturates through field generation only . . And you have already written the first three sentences of the full article: it is well known that collisional hydrodynamic viscosity is too small to explain the inferred rate of angular momentum transport in accretion disks ( shakura & sunyaev 1973 ) . one possible source of anomalous viscosity is turbulence resulting from the magneto - rotational instability , or mri ( velikhov 1959 ; balbus & hawley 1991 ) . in the linear phase , this instability derives its source of free energy from the radial gradient of the rotational flow in the presence of a _ weak _ magnetic field , i.e. , the mri requires the presence of a magnetic field , but is linearly stable if the field is too large . the properties of mri turbulence , and its effect on angular momentum transport , depend in a fundamental way on the amplitude of the fluctuations in the non - linear state .. Please generate the next two sentences of the article

we expect this amplitude to be related to the non - linear saturation mechanism of a _ single _ mri mode . a common saturation mechanism for linear instabilities is the relaxation of the free energy source through quasi - linear processes . for the case of the mri

Suppose that you have an abstract for a scientific paper: we present the results of our optical monitoring campaign of the x - ray source h 0507 + 164 , a low luminosity seyfert 1.5 galaxy at a redshift , @xmath0 . spectroscopic observations were carried out during 22 nights in 2007 , from the 21 of november to the 26 of december . photometric observations in the r - band for 13 nights were also obtained during the same period . the continuum and broad line fluxes of the galaxy were found to vary during our monitoring period . the r - band differential light curve with respect to a companion star also shows a similar variability . using cross correlation analysis , we estimated a time delay of @xmath1 days ( in the rest frame ) , of the response of the broad h@xmath2 line fluxes to the variations in the optical continuum at 5100 . using this time delay and the width of the h@xmath2 line , we estimated the radius for the broad line region ( blr ) of @xmath3 parsec , and a black hole mass of @xmath4m@xmath5 . [ firstpage ] galaxies : active - galaxies : individual ( h 0507 + 164 ) - galaxies : seyfert . And you have already written the first three sentences of the full article: accretion of gas onto a super massive black hole ( smbh ) in the nucleus of galaxies is believed to be the source of activity in quasars and seyfert galaxies ( commonly known as active galactic nuclei ( agns ) ; cf . rees 1984 ) . several studies have suggested that the mass of the smbh in these objects is correlated with the luminosity , mass and velocity dispersion of the stellar spheroid of the galaxies ( kormendy & richstone 1995 ; magorrian et al .. Please generate the next two sentences of the article

1998 ; ferrarese & merritt 2000 ; gebhardt et al . 2000 ; marconi & hunt 2003 ; hring & rix 2004 ) . such correlations may imply an evolutionary relation between the growth of the smbh and the host galaxy itself ( e.g. somerville et al . 2008 ; shankar et al . 2009

Suppose that you have an abstract for a scientific paper: the analysis of the broad iron line profile in the x - ray spectra of active galactic nuclei and black hole x - ray binaries allows us to constrain the spin parameter of the black hole . we compare the constraints on the spin value for two x - ray sources , mcg-6 - 30 - 15 and gx 339 - 4 , with a broad iron line using present relativistic line models in xspec laor and . the laor model has the spin value set to the extremal value @xmath0 , while the model enables direct fitting of the spin parameter . the spin value is constrained mainly by the lower boundary of the broad line , which depends on the inner boundary of the disc emission where the gravitational redshift is maximal . the position of the inner disc boundary is usually identified with the marginally stable orbit which is related to the spin value . in this way the laor model can be used to estimate the spin value . we investigate the consistency of the laor and models . we find that the spin values evaluated by both models agree within the general uncertainties when applied on the current data . however , the results are apparently distinguishable for higher quality data , such as those simulated for the international x - ray observatory ( ixo ) mission . we find that the laor model tends to overestimate the spin value and furthermore , it has insufficient resolution which affects the correct determination of the high - energy edge of the broad line . + . And you have already written the first three sentences of the full article: the broad emission iron lines are well - known features found in about two dozens of spectra of active galactic nuclei and black hole binaries . they are supposed to originate close to the black hole by the reflection of the primary radiation on the accretion disc . the spin of the black hole plays an important role in the forming of the line shape .. Please generate the next two sentences of the article

especially , it determines the position of the marginally stable orbit which is supposed to confine the inner edge of the accretion disc ( see figure [ intro ] ) . the innermost stable orbit occurs closer to a black hole with a higher spin value .

Suppose that you have an abstract for a scientific paper: the thermodynamic bethe ansatz ( tba ) and the excited state tba equations for an integrable spin chain related to the lie superalgebra @xmath0 are proposed by the quantum transfer matrix ( qtm ) method . we introduce the fusion hierarchy of the qtm and derive the functional relations among them ( @xmath1-system ) and their certain combinations ( @xmath2-system ) . their analytical property leads to the non - linear integral equations which describe the free energy and the correlation length at any finite temperatures . with regard to the free energy , they coincide with the tba equation based on the string hypothesis . int . j. mod . phys . a , vol . 15 , p. 2329 - 2346 ( 2000 ) . And you have already written the first three sentences of the full article: solvable lattice models related to the lie superalgebras @xcite have attracted a great deal of attention @xcite . for example , the supersymmetric @xmath3 model in strongly correlated electron system has received much attentions in relation with the high @xmath4 superconductivity . these models have both fermionic and bosonic degree of freedom , and are given as solutions of the graded yang - baxter equations @xcite . to solve such models , the bethe ansatz is widely used in many literatures ( see , for example , @xcite and references therein ) . however , many of them deal only with models related to simple representations like fundamental ones ; there was few _ systematic _. Please generate the next two sentences of the article

study by the bethe ansatz on more complicated models such as fusion models @xcite . in view of such situations , we have recently carried out @xcite _ systematically _ an analytic bethe ansatz @xcite related to the lie superalgebras @xmath5 and @xmath6 .

Suppose that you have an abstract for a scientific paper: we present a follow - up analysis of the unique magnetic luminosity - variable carbon - atmosphere white dwarf sdss j142625.71 + 575218.3 . this includes the results of some 106.4 h of integrated light photometry which have revealed , among other things , the presence of a new periodicity at 319.720 s which is not harmonically related to the dominant oscillation ( 417.707 s ) previously known in that star . using our photometry and available spectroscopy , we consider the suggestion made by montgomery et al . ( 2008 ) that the luminosity variations in sdss j142625.71 + 575218.3 may not be caused by pulsational instabilities , but rather by photometric activity in a carbon - transferring analog of am cvn . this includes a detailed search for possible radial velocity variations due to rapid orbital motion on the basis of mmt spectroscopy . at the end of the exercise , we unequivocally rule out the interacting binary hypothesis and conclude instead that , indeed , the luminosity variations are caused by @xmath0-mode pulsations as in other pulsating white dwarfs . this is in line with the preferred possibility put forward by montgomery et al . ( 2008 ) . . And you have already written the first three sentences of the full article: the rather faint ( @xmath1 ) star sdss j142625.71 + 575218.3 ( referred to hereafter as sdss j1426 + 5752 ) is a fascinating object in several aspects . first , it belongs to the newly - discovered type of carbon - atmosphere white dwarfs , also known as hot dq stars ( dufour et al . 2007 , 2008a ) .. Please generate the next two sentences of the article

these are exceedingly rare stars whose unexpected existence was revealed thanks to the availability of some of the data products that came out of the sloan digital sky survey ( e.g. , liebert et al . 2003 and eisenstein et al .

Suppose that you have an abstract for a scientific paper: we study the two - alpha - particle ( @xmath0 ) system in an effective field theory ( eft ) for halo - like systems . we propose a power counting that incorporates the subtle interplay of strong and electromagnetic forces leading to a narrow resonance at an energy of about 0.1 mev . we investigate the eft expansion in detail , and compare its results with existing low - energy @xmath0 phase shifts and previously determined effective - range parameters . good description of the data is obtained with a surprising amount of fine - tuning . this scenario can be viewed as an expansion around the limit where , when electromagnetic interactions are turned off , the @xmath1be ground state is at threshold and exhibits conformal invariance . we also discuss possible extensions to systems with more than two alpha particles . . And you have already written the first three sentences of the full article: nucleons in light nuclei have typical momenta that are small compared to the characteristic qcd scale of 1 gev . at these low momenta , qcd can conveniently be represented by a hadronic theory containing all possible interactions consistent with the qcd symmetries . effective field theory ( eft ) provides a controlled framework for exploiting the separation of scales in nuclei .. Please generate the next two sentences of the article

it is crucial to formulate a power counting that justifies a systematic truncation of the lagrangian leading to observables with the desired accuracy . nuclei offer a non - trivial challenge because one wants such a perturbative expansion in addition to the non - perturbative treatment of certain leading operators , which is required by the existence of shallow bound states . by now , mainly few - body systems have been studied within eft , and , while much remains to be understood , many successes have been achieved @xcite .

Suppose that you have an abstract for a scientific paper: amorphous silicon - nitrogen thin films doped with rare - earth elements ( _ a_-sin : re ; re = y , la , pr , nd , sm , gd , tb , dy , ho , er , yb , and lu ) have been prepared by co - sputtering and studied by means of electron spin resonance ( esr ) . it was found that the neutral dangling - bond density [ d@xmath0 of _ a_-sin films decreases with the presence of magnetic res and the drop of [ d@xmath1 approximately scales with the spin and/or the de gennes factor of each rare - earth element . these results suggest that a strong exchange - like interaction , @xmath2 , between the spin of the magnetic res and d@xmath3 may be responsible for this behaviour , similarly to the decrease of @xmath4 in re - doped superconductors . . And you have already written the first three sentences of the full article: taking into account the recent technological advances , and needs of our modern society , the study of the magnetic properties of new materials is of fundamental importance to develop devices for different applications such as , for example , memory structures.@xcite in view of their characteristics , amorphous silicon ( _ a_-si ) thin films seems to be good candidates for such a purpose.@xcite an interesting way of studying the _ a_-si thin films magnetic response is to focus on the properties of the neutral dangling - bonds ( d@xmath3 ) present in these materials . neutral dangling - bonds are paramagnetic centers that are excellent probes for the investigation of _ a_-si thin films . moreover , silicon dangling - bonds are charge trapping centers@xcite that are more stable under the diamagnetic d@xmath5 form.@xcite in the present work we have studied the behaviour of the paramagnetic defects d@xmath3 in amorphous silicon nitride thin films doped with various rare - earth elements , _ a_-sin : re ( re = rare - earths : y , la , pr , nd , sm , gd , tb , dy , ho , er , yb , and lu ) . depending on the re dopant , these thin films present a relative strong and narrow light emission , even at room temperature.@xcite,@xcite as a consequence , re - doped _. Please generate the next two sentences of the article

a_-sin thin films are expected to be ideal candidates to develop photonic devices . towards this end

Suppose that you have an abstract for a scientific paper: using the well - known `` displace , cut and reflect '' method used to generate disks from given solutions of einstein field equations , we construct static disks made of perfect fluid based on vacuum schwarzschild s solution in isotropic coordinates . the same method is applied to different exact solutions to the einstein s equations that represent static spheres of perfect fluids . we construct several models of disks with axially symmetric perfect fluid halos . all disks have some common features : surface energy density and pressures decrease monotonically and rapidly with radius . as the `` cut '' parameter @xmath0 decreases , the disks become more relativistic , with surface energy density and pressure more concentrated near the center . also regions of unstable circular orbits are more likely to appear for high relativistic disks . parameters can be chosen so that the sound velocity in the fluid and the tangential velocity of test particles in circular motion are less then the velocity of light . this tangential velocity first increases with radius and reaches a maximum . . And you have already written the first three sentences of the full article: axially symmetric solutions of einstein s field equations corresponding to disklike configurations of matter are of great astrophysical interest , since they can be used as models of galaxies or accretion disks . these solutions can be static or stationary and with or without radial pressure . solutions for static disks without radial pressure were first studied by bonnor and sackfield @xcite , and morgan and morgan @xcite , and with radial pressure by morgan and morgan @xcite .. Please generate the next two sentences of the article

disks with radial tension have been considered in @xcite , and models of disks with electric fields @xcite , magnetic fields @xcite , and both magnetic and electric fields have been introduced recently @xcite . solutions for self - similar static disks were analyzed by lynden - bell and pineault @xcite , and lemos @xcite .

Suppose that you have an abstract for a scientific paper: we investigated a hydrostatic equilibrium model of the milky way following parker ( 1966 ) , to constrain the large scale properties of the interstellar medium . in our approach we found an excellent agreement between our simple hydrostatic equilibrium model of the milky way and the recent all - sky survey data rangeing from the @xmath0-ray to the radio regime . on large scales the galactic disk - halo system is found to be stable against parker - instabilities . pressure support from the galactic disk is essential to stabilise the halo . in particular the diffuse ionised gas layer acts as a disk - halo interface . assuming that the distribution of the soft x - ray emitting plasma traces the gravitational potential , we derived the dark matter content of the milky way to be about @xmath1 . our findings are consistent with the rotation curve of the galaxy . . And you have already written the first three sentences of the full article: since the early fifties it is known from optical polarisation studies , that magnetic fields are constituents of the galactic interstellar medium . the magnetic field strength is about a few @xmath2 g . radio continuum observations clearly indicate synchrotron radiation originating high above the galactic plane .. Please generate the next two sentences of the article

thus , magnetic fields and cosmic rays are obviously constituents of the galactic halo . but what is about the gas within the galactic halo ? already parker ( 1966 ) showed , that magnetic fields are always associated with the gaseous phase .

Suppose that you have an abstract for a scientific paper: from optical photometry the cataclysmic variable rxj0944.5 + 0357 is shown to have a double - peaked pulse profile with a period @xmath0 2160 s. the two peaks vary rapidly in relative amplitude . often most of the optical power is concentrated in the first harmonic of the 2160 s modulation ; rxj0944.5 + 0357 therefore probably belongs to the relatively rare class of two - pole accreting intermediate polars exemplified by yy dra and v405 aur . . And you have already written the first three sentences of the full article: many of the x - ray sources in the rosat all - sky survey have been identified optically in the hamburg objective prism survey ( hagen et al . 1995 ) , among which are several cataclysmic variables ( cvs ) ( jiang et al . the source rxj0944.5 + 0357 (= 1rxsj094432.1 + 035738 ; hereafter rxj0944 ) , in the constellation sextans , was observed spectroscopically by jiang et al . and found to have hi and hei emission lines typical of a cv . further spectroscopic study by mennickent et al .. Please generate the next two sentences of the article

( 2002 ) showed the presence of absorption bands in the red , characteristic of a secondary with a spectral type near m2 . observations by the vsnet group have identified two dwarf nova - like outbursts , in january and june 2001 , during which rxj0944 rose to v @xmath0 13 from its quiescent magnitude of v @xmath0 16.2 .

Suppose that you have an abstract for a scientific paper: homology theories for associative algebraic structures are well established and have been studied for a long time . more recently , homology theories for self - distributive algebraic structures motivated by knot theory , such as quandles and their relatives , have been developed and investigated . in this paper , we study associative self - distributive algebraic structures and their one - term and two - term ( rack ) homology groups . . ] in may of 2015 , during a discussion of the origin of the word ` quandle ' on the _ n - category caf _ ( https://golem.ph.utexas.edu/category/ ) , sam c. remarked that unital shelves are associative and provided an elegant short proof . the work herein was inspired by this post . in section [ intro ] , we provide definitions and discuss some elementary propositions . the first two of these propositions were proven by sam c. ( @xcite ) . the latter propositions lay the pathway for the subsequent sections . following this , we discuss a way to construct families of algebraic structures , in particular associative shelves and spindles . section [ finitelygen ] addresses finitely generated associative shelves , their cardinalities and generating functions . following this , finitely generated proto - unital shelves , pre - unital shelves , and unital shelves are discussed . while some of the observations in this section are new , others are stated for completeness ( @xcite , @xcite and @xcite ) . in section [ homologyassoc ] , the two well - known homology theories for self - distributive algebraic structures , namely one - term distributive homology and two - term ( rack ) homology are defined and the main results concerning the homology groups of a special class of associative shelves are proven . in particular , we compute one - term and two - term ( rack ) homology of unital shelves . the main theorem concerning two - term homology of shelves with right fixed elements extends to the two - term ( rack ) homology groups of laver.... And you have already written the first three sentences of the full article: [ 1.1 ] a * quandle * @xmath0 is a magma satisfying the following properties : 1 . * ( idempotence ) * @xmath1 for all @xmath2 , 2 . * ( inverse ) * there exists @xmath3 such that @xmath4 for all @xmath5 , and 3 . *. Please generate the next two sentences of the article

( self - distributivity ) * @xmath6 for all @xmath7 . the primordial example of a quandle arises when starting with a group @xmath8 and defining the quandle operation as @xmath9 for all @xmath10 .

Suppose that you have an abstract for a scientific paper: starting with far field data of time - harmonic acoustic or electromagnetic waves radiated by a collection of compactly supported sources in two - dimensional free space , we develop criteria and algorithms for the recovery of the far field components radiated by each of the individual sources , and the simultaneous restoration of missing data segments . although both parts of this inverse problem are severely ill - conditioned in general , we give precise conditions relating the wavelength , the diameters of the supports of the individual source components and the distances between them , and the size of the missing data segments , which guarantee that stable recovery in presence of noise is possible . the only additional requirement is that a priori information on the approximate location of the individual sources is available . we give analytic and numerical examples to confirm the sharpness of our results and to illustrate the performance of corresponding reconstruction algorithms , and we discuss consequences for stability and resolution in inverse source and inverse scattering problems . mathematics subject classifications ( msc2010 ) : 35r30 , ( 65n21 ) + keywords : inverse source problem , helmholtz equation , uncertainty principles , far field splitting , data completion , stable recovery + short title : uncertainty principles for inverse source problems . And you have already written the first three sentences of the full article: in signal processing , a classical uncertainty principle limits the time - bandwidth product @xmath0 of a signal , where @xmath1 is the measure of the support of the signal @xmath2 , and @xmath3 is the measure of the support of its fourier transform @xmath4 ( cf . , e.g. , @xcite ) . a very elementary formulation of that principle is @xmath5 whenever @xmath6 and @xmath7 . in the inverse source problem ,. Please generate the next two sentences of the article

the far field radiated by a source @xmath8 is its _ restricted _ ( to the unit sphere ) _ fourier transform _ , and the operator that maps the restricted fourier transform of @xmath9 to the restricted fourier transform of its translate @xmath10 is called the _ far field translation operator_. we will prove an uncertainty principle analogous to , where the role of the fourier transform is replaced by the far field translation operator . combining this principle with a _ regularized picard criterion _ , which characterizes the non - evanescent ( i.e. , detectable ) far fields radiated by a ( limited power ) source supported in a ball provides simple proofs and extensions of several results about locating the support of a source and about splitting a far field radiated by well - separated sources into the far fields radiated by each source component .