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Suppose that you have an abstract for a scientific paper: the dual - kinetic - balance ( dkb ) finite basis set method for solving the dirac equation for hydrogen - like ions [ v. m. shabaev _ et al .
_ , phys .
rev .
lett . * 93 * , 130405 ( 2004 ) ] is extended to problems with a non - local spherically - symmetric dirac - hartree - fock potential .
we implement the dkb method using b - spline basis sets and compare its performance with the widely - employed approach of notre dame ( nd ) group [ w.r .
johnson and j. sapirstein , phys .
rev .
lett . * 57 * , 1126 ( 1986 ) ] .
we compare the performance of the nd and dkb methods by computing various properties of cs atom : energies , hyperfine integrals , the parity - non - conserving amplitude of the @xmath0 transition , and the second - order many - body correction to the removal energy of the valence electrons .
we find that for a comparable size of the basis set the accuracy of both methods is similar for matrix elements accumulated far from the nuclear region .
however , for atomic properties determined by small distances , the dkb method outperforms the nd approach .
in addition , we present a strategy for optimizing the size of the basis sets by choosing progressively smaller number of basis functions for increasingly higher partial waves .
this strategy exploits suppression of contributions of high partial waves to typical many - body correlation corrections . .
And you have already written the first three sentences of the full article: applications of perturbation theory in quantum mechanics require summations over a complete set of states of the lowest - order hamiltonian .
usually , the relevant spectrum is innumerable . in practical applications such eigenspectra
are often modeled using finite basis sets , chosen to be numerically complete . since the sets are finite , the otherwise infinite summations become amendable to numerical evaluations ..
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the use of a finite basis set composed of piecewise polynomials , so - called b - splines @xcite , has proven to be particularly advantageous in atomic physics and quantum chemistry applications @xcite . in this approach ,
an atom is placed in a sufficiently large cavity and the atomic wavefunctions are expanded in terms of the underlying b - spline set .
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11,301 |
Suppose that you have an abstract for a scientific paper: we classify noninvertible , holomorphic selfmaps of the projective plane that preserve an algebraic web . in doing so
, we obtain interesting examples of critically finite maps . .
And you have already written the first three sentences of the full article: in this paper we classify holomorphic selfmaps of the complex projective plane @xmath0 that are integrable in the quite specific sense that they preserve an algebraic web .
recall that an _ algebraic web _ is given by a reduced curve @xmath1 , where @xmath2 is the dual projective plane consisting of lines in @xmath0 .
we say that the web is irreducible if @xmath3 is an irreducible curve ..
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the web is _ invariant _ for a holomorphic mapping @xmath4 if every line in @xmath0 belonging to @xmath3 is mapped to another such line .
see sections [ sec : webs ] and [ sec : invariance ] for details .
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11,302 |
Suppose that you have an abstract for a scientific paper: elemental and isotopic abundances are the fossils of galactic archaeology . the observed [ x / fe]-[fe / h ] relations in the galactic bulge and disk and the mass - metallicity relation of galaxies are roughly reproduced with chemodynamical simulations of galaxies under the standard @xmath0-cdm picture and standard stellar physics .
the isotopic ratios such as @xmath1o and @xmath2 mg may require a refinement of modelling of supernova and asymptotic giant branch stars .
the recent observation of the carbon - rich damped lyman @xmath3 system can be reproduced only with faint core - collapse supernovae .
this suggests that chemical enrichment by the first stars in the first galaxies is driven not by pair - instability supernovae but by core - collapse supernovae ( @xmath4 ) .
the observed f abundances can be reproduced with the neutrino processes of core - collapse supernovae . as in f ,
the observations of elemental abundances in small systems may requires further complications of chemical enrichment . in globular clusters
the relative contribution from low - mass supernovae is likely to be smaller than in the field , while the contribution from massive supernovae seems smaller in dwarf spheroidal galaxies than in the solar neighborhood . .
And you have already written the first three sentences of the full article: elemental and isotopic abundances are the fossils of galactic archaeology . different elements are produced from stars on different timescales , therefore elemental and isotopic abundance ratios provide independent information on the `` age '' of a system and can be used as a form of `` cosmic clock '' .
the formation and evolutionary history of galaxies can be constrained in theoretical models by using the observed abundances of stars .
the space astrometry missions ( e.g. , gaia ) and large - scale surveys ( e.g. , hermes on the aat ) will produce unprecedented information on the chemodynamical structure of the milky way galaxy . theoretically @xcite succeeded in reproducing the average evolution of major elements ( except for ti ) in the solar neighbourhood including normal type ii supernovae ( sne ii ) and hypernovae ( hne ) . in this paper.
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we extend the discussion to isotope ratios ( 2 ) and more realistic chemodynamical simulations ( 3 ) . from the observed abundances ,
we discuss the possibility of non - standard chemical enrichment in the very metal - poor damped lyman @xmath3 system ( dla , 4 ) , globular clusters ( gcs , 5 ) , and dwarf spheroidal galaxies ( dsphs , 6 ) .
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11,303 |
Suppose that you have an abstract for a scientific paper: we present the two - loop virtual qed corrections to @xmath0 and bhabha scattering in dimensional regularization .
the results are expressed in terms of polylogarithms .
the form of the infrared divergences agrees with previous expectations .
these results are a crucial ingredient in the complete next - to - next - to - leading order qed corrections to these processes
. a future application will be to reduce theoretical uncertainties associated with luminosity measurements at @xmath1 colliders .
the calculation also tests methods that may be applied to analogous qcd processes .
hep - ph/0010075 slac pub8655 + ucla/00/tep/26 + october , 2000 * two - loop correction to bhabha scattering * 1.5 cm z. bern@xmath2 + _ department of physics and astronomy + ucla , los angeles , ca 90095 - 1547 _ 0.7 cm l. dixon@xmath3 + _ stanford linear accelerator center + stanford university + stanford , ca 94309 _ 0.6 cm and 0.4 cm a. ghinculov@xmath2 + _ department of physics and astronomy + ucla , los angeles , ca 90095 - 1547 _ 2 cm _ submitted to physical review d _ ' '' '' width 3.6 in @xmath4research supported by the us department of energy under grant de - fg03 - 91er40662.@xmath5research supported by the us department of energy under grant de - ac03 - 76sf00515 . .
And you have already written the first three sentences of the full article: bhabha scattering is an important process for extracting physics from experiments at electron - positron colliders primarily because it provides an effective means for determining luminosity .
these measurements depend on having precise theoretical predictions for the bhabha scattering cross sections . as yet , the complete next - to - next - to - leading order ( nnlo ) qed corrections needed for reducing theoretical uncertainties have not been computed . in this paper
we present the complete two - loop matrix elements that would enter into such a computation ..
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this calculation also provides a means for validating techniques that can be applied to physically important but more intricate qcd calculations .
it also provides an additional explicit verification of a general formula due to catani @xcite for the structure of two - loop infrared divergences , and allows us to determine the process - dependent terms for the processes at hand .
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11,304 |
Suppose that you have an abstract for a scientific paper: the similarity between observed velocity structures of al iii and singly ionised species in damped ly@xmath0 systems ( dlas ) suggests the presence of ionised gas in the regions where most metal absorption lines are formed . to explore the possible implications of ionisation effects we construct a simplified two - region model for dlas consisting of an ionisation bounded region with an internal radiation field and a neutral region with a lower metal content . within this framework
we find that ionisation effects are important . if taken into account , the element abundance ratios in dlas are quite consistent with those observed in milky way stars and in metal - poor h ii regions in blue compact dwarf galaxies
. in particular we can not exclude the same primary n origin in both dlas and metal - poor galaxies . from our models no dust depletion of heavy elements needs to be invoked ; little depletion is however not excluded . .
And you have already written the first three sentences of the full article: the study of damped lyman @xmath0 systems ( dlas ) is of great interest for numerous fields in astrophysics ( cf .
petitjean , these proceedings ) , including nucleosynthesis and the chemical evolution of galaxies and the universe at large .
in addition to investigations on the metallicity evolution with redshift ( e.g. pettini et al ..
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1994 , 1997 ) , spectroscopic studies with 10 m class telescopes have opened the opportunity to study ly@xmath0 absorption lines for a large number of elements including n , o , mg , al , si , s , cr , mn , fe , ni and zn . two main interpretations of the abundance ratios in dlas exist currently in the literature both suffering from several inconsistencies .
* 1 ) * lu et al . ( 1996 ) , prochaska & wolfe ( 1999 ) , outram et al . ( 1999 ) , and pettini et al . ( 2000 ) found that the relative abundance patterns indicate that the bulk of heavy elements in these high - redshift objects were produced by type ii supernovae .
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11,305 |
Suppose that you have an abstract for a scientific paper: we review recent advances in the field of full counting statistics ( fcs ) of charge transfer through impurities imbedded into strongly correlated one - dimensional metallic systems , modelled by tomonaga - luttinger liquids ( tlls ) .
we concentrate on the exact analytic solutions for the cumulant generating function ( cgf ) , which became available recently and apply these methods in order to obtain the fcs of a non - trivial contact between two crossed tll . .
And you have already written the first three sentences of the full article: the relative abundance of exactly solvable models makes the one - dimensional ( 1d ) systems a unique testing ground for new concepts in condensed matter physics . however , during the last two decades the purely academical purpose of 1d studies transformed into an applied science as such extremely reliable 1d metallic materials as single wall carbon nanotubes ( swnts ) became widespread in laboratories @xcite .
the surging interest in low - dimensional materials is motivated by the rapidly shrinking lateral sizes of the microelectronic circuitry , which is soon expected to arrive at device dimensions at which any wire is truly one - dimensional from the point of view of current carrying electrons .
the most fundamental difference between the 1d metals and their higher - dimensional counterparts is the role of interactions ..
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while ( at least in clean systems ) the full perturbative expansion in correlation strength is controllable and even convergent in 3d and leads only to insignificant renormalization of parameters ( landau s fermi liquid theory ) , it diverges for one - dimensional systems . this is a clear indication of a new universality class the so - called tomonaga - luttinger liquid ( tll ) . in its simplest form it has first been discussed by tomonaga in @xcite .
a slight generalization was offered by luttinger @xcite . finally , an extremely convenient field theoretical reformulation has been presented by haldane @xcite .
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11,306 |
Suppose that you have an abstract for a scientific paper: it is well known that the forgetful functor from symmetric operads to nonsymmetric operads has a left adjoint @xmath0 given by product with the symmetric group operad .
it is also well known that this functor does not affect the category of algebras of the operad . from the point of view of the author s theory of higher operads , the nonsymmmetric operads are @xmath1-operads and
@xmath0 is the first term of the infinite series of left adjoint functors @xmath2 called symmetrisation functors , from @xmath3-operads to symmetric operads with the property that the category of one object , one arrow , . .
, one @xmath4-arrow algebras of an @xmath3-operad @xmath5 is isomorphic to the category of algebras of @xmath6 .
in this paper we consider some geometrical and homotopical aspects of the symmetrisation of @xmath3-operads .
we follow getzler and jones and consider their decomposition of the fulton - macpherson operad of compactified real configuration spaces .
we construct an @xmath3-operadic counterpart of this compactification which we call the getzler - jones operad .
we study the properties of getzler - jones operad and find that it is contractible and cofibrant in an appropriate model category .
the symmetrisation of the getzler - jones operad turns out to be exactly the operad of fulton and macpherson .
these results should be considered as an extension of stasheff s theory of @xmath1-fold loop spaces to @xmath3-fold loop spaces @xmath7 we also show that a space @xmath8 with an action of a contractible @xmath3-operad has a natural structure of an algebra over an operad weakly equivalent to the little @xmath3-disks operad .
a similar result holds for chain operads .
these results generalise the classical eckman - hilton argument to arbitrary dimension .
finally , we apply the techniques to the swiss cheese type operads introduced by voronov and prove analogous results in this case . 1991 math .
subj . class .
18d05 , 18d50 , 55p48 .
And you have already written the first three sentences of the full article: this is the second paper in a sequence of papers devoted to the relations between higher categories and @xmath3-fold loop space theory . in the first paper
@xcite we developed the necessary categorical techniques which allow us to go back and forth between @xmath3-operads and classical symmetric operads .
the main goal of this paper is to clarify the geometric and homotopy theoretic aspects of this theory . to do this we restrict ourselves to a class of so called pruned @xmath9terminal @xmath10operads ..
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this is a slightly smaller category of @xmath3-operads than we considered in @xcite but it is big enough to include most applications we have in mind .
the reason is that the functor of desymmetrisation from symmetric operads to @xmath3-operads @xcite can be factorised through the category of pruned @xmath3-operads .
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11,307 |
Suppose that you have an abstract for a scientific paper: we investigate the response of the star formation efficiency ( sfe ) to the main parameters of simulations of molecular cloud formation by the collision of warm diffuse medium ( wnm ) cylindrical streams , neglecting stellar feedback and magnetic fields .
the parameters we vary are the mach number of the inflow velocity of the streams , @xmath0 , the rms mach number , @xmath1 of the initial background turbulence in the wnm , and the total mass contained in the colliding gas streams , @xmath2 .
because the sfe is a function of time , we define two estimators for it , the `` absolute '' sfe , measured at @xmath3 myr into the simulation s evolution ( sfe@xmath4 ) , and the `` relative '' sfe , measured 5 myr after the onset of star formation in each simulation ( sfe@xmath5 ) . the latter is close to the `` star formation rate per free - fall time '' for gas at @xmath6 .
we find that both estimators decrease with increasing @xmath2 , although by no more than a factor of 2 as @xmath0 increases from 1.25 to 3.5 .
increasing levels of background turbulence ( injected at scales comparable to the streams transverse radius ) similarly reduce the sfe , because the turbulence disrupts the coherence of the colliding streams , fragmenting the cloud , and producing small - scale clumps scattered through the numerical box , which have low sfes .
finally , the sfe is very sensitive to the mass of the inflows ( at roughly constant density and temperature ) , with sfe@xmath5 decreasing from @xmath7 to @xmath8 as the mass in the colliding streams decreases from @xmath9 to @xmath10 or , equivalently , the virial parameter @xmath11 increases from @xmath12 to @xmath13 .
this trend is in partial agreement with the prediction by @xcite , since the latter lies within the same range as the observed efficiencies , but with a significantly shallower slope .
we conclude that the observed variability of the sfe is a highly sensitive function of the parameters of the cloud formation process , and may be the cause of....
And you have already written the first three sentences of the full article: the control of the star formation efficiency ( sfe ) by turbulence is a central issue in our present understanding of star formation , and currently a topic of intense study ( see , e.g. , the reviews by * ? ? ?
* ; * ? ? ?
in recent years , several groups have studied the sfe of molecular clouds ( mcs ) using numerical simulations of isothermal turbulence , in which the entire numerical box represents the interior of a molecular cloud ( see , e.g. , the reviews by * ? ? ? * ; * ? ? ? * ; * ? ? ? * ) ..
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one confusing issue is that simulations of _ driven _ turbulence seem to indicate that the sfe _ decreases _ as the turbulent rms mach number @xmath14 increases ( e.g. , * ? ? ?
* ; * ? ? ?
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11,308 |
Suppose that you have an abstract for a scientific paper: we explore the possibility that the dynamics of the universe can be reproduced choosing appropriately the initial global topology of the universe . in this work
we start with two concentric spherical three - dimensional branes @xmath0 , with radius @xmath1 immersed in a five - dimensional space - time .
the novel feature of this model is that in the interior brane there exist only spin - zero fundamental fields ( scalar fields ) , while in the exterior one there exist only spin - one fundamental interactions . as usual ,
the bulk of the universe is dominated by gravitational interactions . in this model , like in the ekpyrotic one , the big bang is consequence of the collision of the branes and causes the existence of the particles predicted by the standard model in the exterior brane ( our universe ) .
the scalar fields on the interior brane interact with the spin - one fields on the exterior one only through gravitation , they induce the effect of scalar field dark matter with an ultra - light mass on the exterior one .
we discuss two different regimes where the energy density and the brane tension are compared , with the aim to obtain the observed dynamics of the universe after the collision of the branes . .
And you have already written the first three sentences of the full article: in the last part of the twentieth century , cosmology became a precision science getting observational data with an accuracy comparable with the data obtained through the standard model .
the last data arising from observations confirm that our universe is accelerating due to the existence of some unknown type of energy and also requires the existence of an unknown field that permeates the universe and dictates the formation and evolution of the structures at large scales .
both dark components of the universe are not predicted by the standard model or by the general theory of relativity either ..
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this opens the possibility to extend these theories to limits beyond the current ones and to formulate new paradigms that predict new physics , under the condition that in the appropriated limits these new theories reproduce the current standard observations .
so far the best accepted candidate to be the dark energy of the universe is the cosmological constant @xmath2 .
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11,309 |
Suppose that you have an abstract for a scientific paper: we carry out numerical investigations of the perturbations in nflation models where the mass spectrum is generated by random matrix theory .
the tensor - to - scalar ratio and non - gaussianity are already known to take the single - field values , and so the density perturbation spectral index is the main parameter of interest .
we study several types of random field initial conditions , and compute the spectral index as a function of mass spectrum parameters .
comparison with microwave anisotropy data from the wilkinson microwave anisotropy probe shows that the model is currently viable in the majority of its parameter space . .
And you have already written the first three sentences of the full article: the nflation model of dimopoulos et al .
@xcite corresponds to a collection of uncoupled massive fields which drive inflation via the assisted inflation mechanism @xcite .
the existence of multiple fields is motivated by the axions of string theory , and their presence enables sufficient inflation to be obtained without using super - planckian field values ..
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models of this type had first been considered by kanti and olive @xcite and then kaloper and liddle @xcite in the context of kaluza klein models .
they showed the massive fields evolve faster to the minima of their own potential and light ones later .
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11,310 |
Suppose that you have an abstract for a scientific paper: we have selected the seven most well - defined wr ring nebulae in the lmc ( br 2 , br 10 , br 13 , br 40a , br 48 , br 52 , and br 100 ) to study their physical nature and evolutionary stages .
new ccd imaging and echelle observations have been obtained for five of these nebulae ; previous photographic imaging and echelle observations are available for the remaining two nebulae . using the nebular dynamics and abundances
, we find that the br 13 nebula is a circumstellar bubble , and that the br 2 nebula may represent a circumstellar bubble merging with a fossil main - sequence interstellar bubble .
the nebulae around br 10 , br 52 , and br 100 all show influence of the ambient interstellar medium .
their regular expansion patterns suggest that they still contain significant amounts of circumstellar material .
their nebular abundances would be extremely interesting , as their central stars are wc5 and wn3 - 4 stars whose nebular abundances have not been derived previously .
intriguing and tantalizing implications are obtained from comparisons of the lmc wr ring nebulae with ring nebulae around galactic wr stars , galactic lbvs , lmc lbvs , and lmc bsgs ; however , these implications may be limited by small - number statistics . a snr candidate close to br 2
is diagnosed by its large expansion velocity and nonthermal radio emission .
there is no indication that br 2 s ring nebula interacts dynamically with this snr candidate .
-0.5 in 6.5 in .
And you have already written the first three sentences of the full article: wolf - rayet ( wr ) stars are characterized by broad emission lines that are indicative of fast stellar winds and high mass loss rates .
the fast stellar wind sweeps up the ambient medium into a dense expanding shell , called a wind - blown bubble .
wind - blown bubbles in a homogeneous medium have been modeled by , for example , castor , mccray , & weaver ( 1975 ) , steigman , strittmatter , & williams ( 1975 ) , and weaver et al ..
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however , these models can not be readily applied to bubbles blown by wr stars because wr stars are evolved massive stars and their progenitors mass loss has drastically modified their gaseous surroundings .
the physical conditions of a wr star s ambient medium are highly dependent on the star s evolutionary history and mass loss history .
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11,311 |
Suppose that you have an abstract for a scientific paper: for every @xmath0 , we construct a regular and continuous specification ( @xmath1-function ) , which has a variation sequence that is in @xmath2 and which admits multiple gibbs measures . combined with a result of johansson and berg , @xcite
, this determines the optimal modulus of continuity for a specification which admits multiple gibbs measures . .
And you have already written the first three sentences of the full article: for a finite set @xmath3 let @xmath4 be the set of probability distributions on @xmath3 .
a _ specification g _
( also commonly known as a @xmath1-function ) is a measurable function from @xmath5 to @xmath4 ..
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a specification @xmath1 is _ regular _ if there exists @xmath6 such that for every sequence @xmath7 and every @xmath8 we have that @xmath9 .
we focus on specifications that are regular and continuous with respect to the product topology .
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11,312 |
Suppose that you have an abstract for a scientific paper: in a recent preprint , @xcite , we showed that for the dirichlet laplacian @xmath0 on the unit disk , the wave trace @xmath1 , which has complicated singularities on @xmath2 , is , on the interval @xmath3 , the restriction to this interval of a @xmath4 function on its closure . in this paper
we prove the analogue of this somewhat counter - intuitive result for the friedlander model .
the proof for the friedlander model is simpler and more transparent than in the case of the unit disk . .
And you have already written the first three sentences of the full article: let @xmath5 be a smooth bounded strictly convex region in the plane , and let @xmath6 be the eigenvalues , with multiplicity , of the dirichlet problem for the laplacian on @xmath5 : @xmath7 in the spirit of @xcite ) we will define the _ wave trace _ of the dirichlet laplacian @xmath0 to be the sum @xmath8 by a theorem of andersson and melrose @xcite , @xmath9 is a tempered distribution whose singular support in @xmath10 is the closure of the set @xmath11 where @xmath12 is the set of critical values of the length function given by @xmath13
@xmath14 are distinct boundary points .
each critical point of the length function defines a polygonal trajectory consisting of the line segments joining @xmath15 to @xmath16 and @xmath14 to @xmath17 ..
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these are , by definition , the _ closed geodesics _ on @xmath5 , and @xmath18 is the set of lengths of these geodesics , i.e. the _ length spectrum _ of @xmath5 .
each set @xmath12 is closed , but there are limiting geodesics as @xmath19 .
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11,313 |
Suppose that you have an abstract for a scientific paper: typically , there is no guarantee that a numerical approximation obtained using standard nonlinear equation solvers is indeed an actual solution , meaning that it lies in the quadratic convergence basin .
instead , it may lie only in the linear convergence basin , or even in a chaotic region , and hence not converge to the corresponding stationary point when further optimization is attempted . in some cases
, these non - solutions could be misleading .
proving that a numerical approximation will quadratically converge to a stationary point is termed _
certification_. in this report , we provide details of how smale s @xmath0-theory can be used to certify numerically obtained stationary points of a potential energy landscape , providing a _ mathematical proof _ that the numerical approximation does indeed correspond to an actual stationary point , independent of the precision employed . .
And you have already written the first three sentences of the full article: given a potential @xmath1 , with @xmath2 , the surface defined by @xmath1 is called the potential energy landscape ( pel ) of the given system @xcite .
the special points of a pel , defined by the solutions of the equations @xmath3 for @xmath4 , provide important information about the pel .
these special points , called critical points or stationary points ( sps ) of the pel , can be further classified according to the number of negative eigenvalues of the hessian matrix , @xmath5 ..
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the sps at which @xmath6 is positive ( negative ) definite are called minima ( maxima ) of the pel and the sps at which @xmath6 has exactly @xmath7 negative eigenvalue are called saddles of index @xmath7 .
sps at which @xmath6 has at least one zero eigenvalue , after removing the global symmetries from the system corresponding to overall translation and rotation , are called singular sps or non - morse points .
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11,314 |
Suppose that you have an abstract for a scientific paper: in this talk the methods and computer tools which were used in our recent calculation of the three - loop standard model renormalization group coefficients are discussed .
a brief review of the techniques based on special features of dimensional regularization and minimal subtraction schemes is given .
our treatment of @xmath0 is presented in some details .
in addition , for a reasonable set of initial parameters the numerical estimates of the obtained three - loop contributions are presented .
the renormalization group ( rg ) proves to be a useful and powerful tool in studying high - energy behavior of the standard model . before the discovery of the higgs boson rg equations ( rge ) were used , among other things , to bound the value of the higgs self - coupling .
however , the bounds significantly depends on the scale at which one expects the appearance of new physics .
the observation of the higgs boson in 2012 @xcite in some sense finalizes the sm since the information about the values of all the sm couplings become available from experiments . due to this fact
, the interest to rg studies of the standard model arises again , but at a new level of precision .
one- and two - loop results for sm beta - functions have been known for quite a long time @xcite and are summarized in @xcite . the first paper with full three - loop calculation of gauge coupling beta - functions within the sm was published in ref .
@xcite .
the next step was carried out by another group from karlsruhe @xcite , which considered , in the specific limit , the three - loop beta - functions for the top quark yukawa coupling , the higgs self - coupling and mass parameter . at this state of things
our group entered the game .
we not only confirmed the results of refs .
@xcite but also provided the three - loop expressions for beta - functions of all the yukawa couplings @xcite corresponding to the fermions of third generation .
contrary to chetyrkin and zoller , we include the dependence on....
And you have already written the first three sentences of the full article: 10 url # 1#1urlprefix[2][]#2 aad g _
et al . _ ( atlas collaboration ) 2012 _ phys.lett . _ * b716 * 129 ( _ preprint _ ).
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11,315 |
Suppose that you have an abstract for a scientific paper: a number of recent experiments have suggested the presence of either real or complex components in the gap symmetry of high-@xmath0 superconductors ( htsc ) . in this paper
we introduce a novel approach to study the competition of such complex order parameter mixtures by varying the position of the two - body attractive potential in a two dimensional extended hubbard hamiltonian .
we show that this procedure explain a number of experimental results and on the theoretical side , it may be related with certain htsc microscopic models like the spin fluctuation theory . following current trends we concentrate on the study of @xmath1 order parameter with a component of the type @xmath2 or a s - wave like @xmath3 and @xmath4 symmetry .
we show that the position of the optimal s - component peak changes with the position parameter @xmath5 while the d - component occurs always in the optimally region around hole content @xmath6 . these studies may be useful to interpret some experimental data and to explain why similar experiments yield different gap symmetries . 2 .
And you have already written the first three sentences of the full article: in order to understand the fundamental mechanism for high-@xmath0 superconductors ( htsc ) , many experiments have attempted to find out the properties of the superconductors pair wave function . notwithstanding this effort
the nature of the orbital order parameter symmetry ( or energy gap ) has not yet been settled , despite increasing evidences toward a major @xmath1 symmetry as it explains a number of different experimental results@xcite .
furthermore the d - wave state has also theoretical support from weak and strong - coupling approaches@xcite and from monte carlo and numerical studies on a two dimensional hubbard model@xcite . on the other hand several experiments.
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have also suggested the presence of real or complex mixture of order parameters .
for instance , c - axis josephson tunneling data between twinned ybco and a s - wave superconductor were interpreted by a condensate containing a mixture of @xmath1 and @xmath7 order parameter@xcite .
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11,316 |
Suppose that you have an abstract for a scientific paper: the hard state of x - ray binaries ( xrbs ) is characterized by a power law spectrum in the x - ray band , and a flat / inverted radio / ir spectrum associated with occasionally imaged compact jets .
it has generally been thought that the hard x - rays result from compton upscattering of thermal accretion disk photons by a hot , coronal plasma whose properties are inferred via spectral fitting .
interestingly , these properties especially those from certain magnetized corona models
are very similar to the derived plasma conditions at the jet footpoints . here we explore the question of whether the ` corona ' and ` jet base ' are in fact related , starting by testing the strongest premise that they are synonymous .
in such models , the radio through the soft x - rays are dominated by synchrotron emission , while the hard x - rays are dominated by inverse compton at the jet base with both disk and synchrotron photons acting as seed photons .
the conditions at the jet base fix the conditions along the rest of the jet , thus creating a direct link between the x - ray and radio emission .
we also add to this model a simple iron line and convolve the spectrum with neutral reflection .
after forward - folding the predicted spectra through the detector response functions , we compare the results to simultaneous radio / x - ray data obtained from the hard states of the galactic xrbs gx 339@xmath04 and cygnus x-1 .
results from simple compton corona model fits are also presented for comparison .
we demonstrate that the jet model fits are statistically as good as the single - component corona model x - ray fits , yet are also able to address the simultaneous radio data . .
And you have already written the first three sentences of the full article: bipolar plasma outflows , loosely termed jets , are a feature common to a variety of different astrophysical objects .
jets are observed in accreting compact objects of all scales , as well as at stellar birth and death .
they seem equally able to form out of massive accretion disks as well as from quasi - spherically collapsing plasma , which suggests that their creation is a basic byproduct of some routinely occurring ingredients ..
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these necessary inputs seem to be rotation , collapsing or infalling / accreting plasma , and magnetic fields .
jets likely are formed at least in part from a necessity to shed the system of excess angular momentum ( e.g. , * ? ? ?
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Suppose that you have an abstract for a scientific paper: we present new near - infrared and optical spectroscopic observations which confirm the redshift of the @xmath0 extremely red object ero j164502 + 4626.4 ( object # 10 of hu & ridgway 1994 ; formerly known as ` hr 10 ' or ` [ hr94 ] 10 ' ) and a _ hubble space telescope _ image which reveals a reflected - s shaped morphology at ( rest frame ) near - ultraviolet wavelengths .
the contrast between the rest frame far - red ( @xmath1 ) and near - uv ( @xmath2 ) morphologies suggests that the central regions of the galaxy are heavily obscured by dust and that the galaxy is most likely an interacting or disturbed system .
we also present new photometry of this object at 450 , 850 and 1350 obtained using the scuba submillimeter camera on the james clerk maxwell telescope .
our sub - mm data are extremely sensitive to emission from cold dust at high redshift . the rest
frame spectral energy distribution of ero j164502 + 4626.4 is best understood in terms of a highly reddened stellar population with ongoing star formation , as originally suggested by graham & dey ( 1996 ) .
the new submillimeter data presented here indicate that the remarkable similarity to ultraluminous infrared galaxies ( ulirgs ) such as arp 220 and mrk 231 extends into the rest - frame far - infrared which bears the signature of thermal emission from dust , presumably heated by young stars .
ero j164502 + 4626.4 is extremely luminous ( @xmath3 ) and dusty ( @xmath4 ) .
if its luminosity is powered by young hot stars , then ero j164502 + 4626.4 is forming stars at the prodigious rate of @xmath5 . we conclude that ero j164502 + 4626.4 is a distant analogue of the nearby ulirg population , the more distant or less luminous counterparts of which may be missed by even the deepest existing optical surveys .
the sub - mm emitters recently discovered by deep scuba surveys may be galaxies similar to ero j164502 + 4626.4 ( but perhaps more distant ) .
this population of extremely dusty galaxies may also contribute....
And you have already written the first three sentences of the full article: near infrared ( near ir ) imaging surveys have resulted in the discovery of a population of infrared bright , extremely red objects ( ` eros ' ) , which may be of significance to studies of galaxy evolution .
eros , which we define in this paper as having observed optical near - ir colors @xmath10 , have been identified both in the field , and around high - redshift radio galaxies and quasars ( elston , rieke , & rieke 1988 , 1989 , 1991 ; mccarthy , persson , & west 1992 ; eisenhardt & dickinson 1992 ; graham et al .
1994 ; hu & ridgway 1994 ; dey , spinrad , & dickinson 1995 ) ..
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images of eros from ground based telescopes show that they are spatially extended on scales of @xmath11 .
this suggests that eros are probably galaxies rather than stellar objects ( e.g. , brown dwarfs ) .
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Suppose that you have an abstract for a scientific paper: the heavy sfermion scenario is naturally realized when supersymmetry breaking fields are charged under some symmetry or are composite fields . there , scalar partners of standard model fermions and the gravitino are as heavy as @xmath0 tev while gauginos are as heavy as @xmath1 tev .
the scenario is not only consistent with the observed higgs mass , but also is free from cosmological problems such as the polonyi problem and the gravitino problem . in the scenario ,
gauginos are primary targets of experimental searches . in this thesis
, we discuss gaugino masses in the heavy sfermion scenario .
first , we derive the so - called anomaly mediated gaugino mass in the superspace formalism of supergravity with a wilsonian effective action
. then we calculate gaugino masses generated through other possible one - loop corrections by extra light matter fields and the qcd axion .
finally , we consider the case where some gauginos are degenerated in their masses with each other , because the thermal relic abundance of the lightest supersymmetric particle as well as the the strategy to search gauginos drastically change in this case . after calculating the thermal relic abundance of the lightest supersymmetric particle for the degenerated case
, we discuss the phenomenology of gauginos at the large hadron collider and cosmic ray experiments .
.
And you have already written the first three sentences of the full article: supersymmetry ( susy ) has been intensively studied as a fundamental law of nature for following reasons : susy reduces degrees of divergences in quantum field theories @xcite , and hence stabilizes the vast separation between the electroweak scale and the planck scale or the grand unification scale @xcite .
if susy is broken by some strong gauge dynamics , the smallness of the electroweak scale is explained by dimensional transmutation . in the minimal susy extension of the standard model ( mssm ) ,
three gauge coupling constants unify , which is consistent with the prediction of the simplest grand unified theory ( gut ) , namely the @xmath2 gut @xcite . with an @xmath3 parity preserved ,.
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the lightest susy particle ( lsp ) is a good candidate of dark matter @xcite . the discovery of the standard - model - like higgs as heavy as @xmath4 gev @xcite strongly constrains the mass spectrum of mssm particles . in the mssm ,
quartic couplings of higgs fields are given by @xmath5 term potentials of standard model gauge interactions in the susy limit .
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Suppose that you have an abstract for a scientific paper: we report the discovery of two new dwarf galaxies , lacerta i / andromeda xxxi ( lac i / and xxxi ) and cassiopeia iii / andromeda xxxii ( cas iii / and xxxii ) , in stacked pan - starrs1 @xmath0- and @xmath1-band imaging data . both are luminous systems ( @xmath2 ) located at projected distances of @xmath3 and @xmath4 from m31 .
lac i and cas iii are likely satellites of the andromeda galaxy with heliocentric distances of @xmath5 and @xmath6 , respectively , and corresponding m31-centric distances of @xmath7 and @xmath8 .
the brightest of recent local group member discoveries , these two new dwarf galaxies owe their late discovery to their large sizes ( @xmath9arcmin or @xmath10 for lac i ; @xmath11arcmin or @xmath12 for cas iii ) , and consequently low surface brightness ( @xmath13 mag / arcsec@xmath14 ) , as well as to the lack of a systematic survey of regions at large radii from m31 , close to the galactic plane .
this latter limitation is now alleviated by the @xmath15 pan - starrs1 survey , which could lead to the discovery of other distant andromeda satellite dwarf galaxies . .
And you have already written the first three sentences of the full article: the salience of satellite dwarf galaxies for understanding galaxy formation in a cosmological context has been made all the more evident in the past decade with the discovery of numerous faint local group galaxies .
these faint systems are not only important to understand the faint end of galaxy formation ( e.g. @xcite ) but also their distribution around their host can test the hierarchical formation induced by the favored cosmological paradigm ( e.g. @xcite ) .
the andromeda satellite system is arguably the ideal system to study in order to tackle these questions as its proximity renders it easily observable , while our outsider s perspective facilitates its complete mapping , provided one has access to high - quality , multi - color , and wide - field photometry ..
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the number of known andromeda satellite dwarf galaxies has soared over the last decade , thanks mainly to two large photometric surveys of this region of the sky .
the sloan digital sky survey ( sdss ) enabled the discovery of a handful of relatively bright ( @xmath16 ) systems , initially from a dedicated stripe along the major axis of the andromeda galaxy ( and ix , and x ; @xcite ) , which was later complemented by a more systematic coverage of parts of the region around m31 in data release 8 ( and xxviii , and xxix ; @xcite ) . the pan - andromeda archaeological survey ( pandas )
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Suppose that you have an abstract for a scientific paper: we argue that the results for the vacuum forces on a slab and on an atom embedded in a magnetodielectric medium near a mirror , obtained using a recently suggested lorentz - force approach to the casimir effect , are equivalent to the corresponding results obtained in a traditional way .
we also derive a general expression for the atom - atom force in a medium and extend a few classical results concerning this force in vacuum and dielectrics to magnetodielectric systems .
this , for example , reveals that the ( repulsive ) interaction between atoms of different polarizability type is at small distances unaffected by a ( weakly polarizable ) medium .
although modifications of the casimir and van der waals forces due to the presence of a medium between the interacting objects were the subject of interest for a long time @xcite , this issue is still of great importance owing to the dominant role of these forces at small distances and to the rapid progress in micro and nanotechnologies .
a common way of extending the lifshitz theory @xcite of the casimir effect @xcite to material cavities is to ( eventually ) employ the minkovski stress tensor @xmath0 when calculating the force @xcite .
recently , however , a lorentz - force approach to the casimir effect was suggested @xcite ( see also @xcite ) in which the relevant stress tensor is of the form ( brackets denote the average with respect to fluctuations and we use the standard notation for the macroscopic field operators ) @xmath1 in this work , we reinterpret the results for the vacuum forces on a slab and on an atom embedded in a semi - infinite magnetodielectric cavity ( see figure 1 ) as recently obtained using @xmath2 @xcite and argue their equivalence to the corresponding results obtained using @xmath3 . also , we derive a general expression for the atom - atom force in a medium and extend a few well - known results for this force to magnetodielectric systems . when calculating @xmath2 for planar geometry @xcite , the zero - temperature....
And you have already written the first three sentences of the full article: .
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Suppose that you have an abstract for a scientific paper: strong frequency dependence is unlikely in diffusive or over - damped systems .
when exceptions do occur , such as in the case of stochastic resonance , it signals an interesting underlying phenomenon .
we find that such a case appears in the motion of a particle in a diffusive environment under the effect of periodically oscillating retarded force emanating from the boundaries .
the amplitude for the expectation value of position has an oscillating frequency dependence , quite unlike a typical resonance .
we first present an analysis of the associated fokker - planck equation , then report the results of a monte carlo simulation of the effect of a periodic perturbation on a totally asymmetric simple exclusion process ( tasep ) model with single species .
this model is known to exhibit a randomly moving shock profile , dynamics of which is a discrete realization of the fokker - planck equation .
comparison of relevant quantities from the two analyses indicate that the same phenomenon is apparent in both systems . .
And you have already written the first three sentences of the full article: diffusive systems can not support resonances in the usual sense , a periodic force can not build oscillations that grow with each cycle .
the frequency response of systems vary monotonously .
we present an over - damped system which has an oscillating frequency response due to the presence of a position dependent effective force ..
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such conditions arise for objects under the influence of retarded effects from boundaries an example of which we also provide .
the fokker - planck ( fp ) equation @xcite describes the time dependence of the probability distribution @xmath0 of the position of a particle in a diffusive environment : @xmath1 \label{fp}\ ] ] where @xmath2 is the drift constant relating velocity to force and @xmath3 is the coefficient of the diffusion term .
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Suppose that you have an abstract for a scientific paper: high - resolution spectroscopy is a very important tool for studying stellar physics , perhaps , particularly so for such enigmatic objects like the r coronae borealis and related hydrogen deficient stars that produce carbon dust in addition to their peculiar abundances .
examples of how high - resolution spectroscopy is used in the study of these stars to address the two major puzzles are presented : ( i ) how are such rare h - deficient stars created ? and ( ii ) how and where are the obscuring soot clouds produced around the r coronae borealis stars ? = 1 .
And you have already written the first three sentences of the full article: we congratulate the organizers for arranging and conducting this conference , celebrating the 150 years of the discovery by ( gustav robert ) kirchoff and ( robert wilhelm eberhard ) bunsen that various gases can be easily and positively identified by a detailed study of the light they emit and absorb . as paul merrill ( @xcite ) noted , a new era in astronomy began when bunsen saw ` in yellow flame of an ordinary alcohol lamp whose wick was sprinkled with salt , and possibilities of the chemical analysis of the most distant stars ' .
thus began the era of astronomical spectroscopy .
merrill s own contributions to our discipline are legendary with his discovery of tci lines in the spectra of s stars signaling that element synthesis in stars was a continuing phenomena ( @xcite ).
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. a few historical remarks might be appropriate .
astronomical spectroscopy in india started during the famous total solar eclipse that occurred on 1868 august 18 in which a spectroscope was first used to study the nature of solar prominences leading to the discovery of helium .
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Suppose that you have an abstract for a scientific paper: using the hugenholtz - van hove theorem , we derive analytical expressions for the nuclear symmetry energy @xmath0 and its density slope @xmath1 in terms of the lorentz covariant nucleon self - energies in isospin asymmetric nuclear matter .
these general expressions are useful for determining the density dependence of the symmetry energy and understanding the lorentz structure and the microscopic origin of the symmetry energy in relativistic covariant formulism . as an example
, we analyze the lorentz covariant nucleon self - energy decomposition of @xmath0 and @xmath1 and derive the corresponding analytical expressions within the nonlinear @xmath2-@xmath3-@xmath4-@xmath5 relativistic mean field model . .
And you have already written the first three sentences of the full article: in the current research of nuclear physics and astrophysics , there is of great interest to study the density dependence of the nuclear symmetry energy @xmath0 that essentially characterizes the isospin dependent part of the equation of state ( eos ) of asymmetric nuclear matter .
the exact knowledge on the symmetry energy is important for understanding not only many problems in nuclear physics , but also many critical topics in astrophysics @xcite as well as some interesting issues regarding possible new physics beyond the standard model @xcite . during the last decade , although significant progress has been made both experimentally and theoretically on constraining the density dependence of the symmetry energy @xcite ( see , e.g. , refs .
@xcite for review of recent progress ) , large uncertainties on @xmath0 still exist , especially its super - normal density behavior remains elusive and largely controversial @xcite ..
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to reduce the uncertainties of the constraints on @xmath0 is thus of critical importance and remains a big challenge in the community , and this provides a strong motivation for studying isospin nuclear physics in radioactive nuclei at the new / planning rare isotope beam facilities around the world , such as csr / lanzhou and brif - ii / beijing in china , ribf / riken in japan , spiral2/ganil in france , fair / gsi in germany , frib / nscl in usa , spes / lnl in italy , and koria in korea .
theoretically , the uncertainties of the constraints on @xmath6 are mainly due to the lack of knowledge about the isospin dependence of in - medium nuclear effective interactions and the limitations in the techniques for solving the nuclear many body problem .
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Suppose that you have an abstract for a scientific paper: we report on a highly efficient waveguide resonator device for the production of 775 nm light using a titanium indiffused linbo@xmath0 waveguide resonator .
the device stably produces up to 110mw of second harmonic power with 140mw _ incident _ on the device - an external conversion efficiency of 75% .
the cavity length is also locked , using a pound - drever - hall type locking scheme , via one of two methods involving feedback to either the cavity temperature or the laser frequency .
both locking schemes result in a stable output power of at least 10mw over one hour . .
And you have already written the first three sentences of the full article: integrated optical waveguide technologies offer improvements in size , scalability , integrability and nonlinear interaction strength over their bulk counterparts .
these properties have been used to create a myriad of impressive devices , such as high - speed switches @xcite , optical parametric oscillators @xcite and frequency conversion devices @xcite .
frequency conversion is often used to produce laser fields at wavelengths inaccessible to current materials @xcite , but can also be used to interface individual parts of a network @xcite or to transfer information from one field to another at a different wavelength @xcite . traditionally , the main advantage of waveguide devices has been very high nonlinear interaction strengths , allowing for relatively high conversion efficiencies at low input and low output powers ..
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however , for many applications both high conversion efficiency and high output powers are desired .
this is where the performance of waveguides has traditionally been limited , due to a number of factors such as large waveguide losses , poor mode shape profile and high power effects such as photorefraction .
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Suppose that you have an abstract for a scientific paper: solid state actuators ( piezoelectric , ferroelectric , ... ) deform under an external field , and have found many applications .
they respond fast , but their mechanical deformations are very small .
there is a need for soft actuators , giving larger responses , but necessarily less fast .
this paper describes the early attempts by katchalsky and others , and the problems which showed up -related to time constants , and , most importantly , to fatigue .
two current attempts are reviewed .
_ key words _ : actuators , artificial muscles , nematic polymers , electro osmosis .
_ pacs numbers _ : 64.70 md , 65.70 + y , 66.30 qa . .
And you have already written the first three sentences of the full article: as soon as kuhn understood the flexibility of polymer chains , and the origin of rubber elasticity , his student a. katchalsky thought about the possibility of transforming chemical energy into mechanical energy , using gels swollen by water .
his first idea is explained on fig.[fig1 ] .
starting from chains which carry acid groups @xmath0 and adding @xmath1 ions , one obtains a charged network @xmath2 where the chains stretch by electrostatic repulsions ..
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if one then adds @xmath3 , the system returns to neutral , and the gel contracts .
[ h ] pgg1nov.eps this system , however , does not allow for many cycles .
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Suppose that you have an abstract for a scientific paper: this paper presents a simple , one - dimensional model of a randomly advected passive scalar .
the model exhibits anomalous inertial range scaling for the structure functions constructed from scalar differences .
the model provides a simple computational test for recent ideas regarding closure and scaling for randomly advected passive scalars .
results suggest that high order structure function scaling depends on the largest velocity eddy size , and hence scaling exponents may be geometry - dependent and non - universal .
_ pacss : _ 47.27.gs
; 05.40.+j _ keywords : _ isotropic turbulence ; random processes ; passive scalars .
And you have already written the first three sentences of the full article: passive scalars are ` tracer particles ' which are advected by the flow of another fluid .
a typical example might be ink mixed by flowing water .
the mixing of a scalar field @xmath0 in a velocity field @xmath1 is governed by the advection - diffusion equation , @xmath2 in which @xmath3 is a diffusion constant and @xmath4 is an external source of scalar ..
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the velocity field is determined independently of the scalar field ( hence the adjective _ passive _ ) and ( in this discussion ) is incompressible ( @xmath5 ) .
the incompressible flow simply transports the scalar , without changing any of the scalar s values .
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Suppose that you have an abstract for a scientific paper: we present here a small anomalous radial velocity ( rv ) signal expected to be present in rv curves measured during planetary transits .
this signal is induced by the convective blueshift ( cb ) effect a net blueshift emanating from the stellar surface , resulting from a larger contribution of rising hot and bright gas relative to the colder and darker sinking gas .
since the cb radial component varies across the stellar surface , the light blocked by the planet during a transit will have a varying rv component , resulting in a small shift of the measured rvs .
the cb - induced anomalous rv curve is different than , and independent of , the well known rossiter - mclaughlin ( rm ) effect , where the latter is used for determining the sky - projected angle between the host star rotation axis and the planet s orbital angular momentum axis .
the observed rv curve is the sum of the cb and rm signals , and they are both superposed on the orbital keplerian curve . if not accounted for , the presence of the cb rv signal in the spectroscopic transit rv curve may bias the estimate of the spin - orbit angle .
in addition , future very high precision rvs will allow the use of transiting planets to study the cb of their host stars . .
And you have already written the first three sentences of the full article: radial velocity ( rv ) measurements of sun - like stars are now reaching the 1 m s@xmath0 accuracy milestone and are expected to become more accurate in the future ( e.g. , * ? ? ?
* ; * ? ? ?
* ; * ? ? ?.
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* ; * ? ? ?
naturally , the increased sensitivity allows to identify more and more low amplitude effects that need to be accounted for when modeling the measured rv curves .
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Suppose that you have an abstract for a scientific paper: we present a systematic study of the morphology of homoepitaxial inp films grown by metalorganic vapor - phase epitaxy which are imaged with _
ex situ _ atomic force microscopy .
these films show a dramatic range of different surface morphologies as a function of the growth conditions and substrate ( growth temperature , v / iii ratio , and miscut angle @xmath0 and orientation toward a or b sites ) , ranging from stable step flow to previously unreported strong step bunching , over 10 nm in height .
these observations suggest a window of growth parameters for optimal quality epitaxial layers .
we also present a theoretical model for these growth modes that takes account of deposition , diffusion , and dissociation of molecular precursors , and the diffusion and step incorporation of atoms released by the precursors .
the experimental conditions for step flow and step bunching are reproduced by this model , with the step bunching instability caused by the difference in molecular dissociation from above and below step edges , as was discussed previously for gaas ( 001 ) . .
And you have already written the first three sentences of the full article: homoepitaxial films of inp are commonly grown as buffer and cladding / waveguiding layers , setting the base for numerous types of semiconductor devices.@xcite the morphology of these films can have a crucial impact on the quality of the overgrown material .
for example , poor quality buffers could result in structural defects propagating to the device layers , reducing the carrier mobility or affecting optical properties , and thereby degrading the performance of the device.@xcite in general , an epitaxial process is required to fabricate materials with reproducible properties of the highest quality in terms of crystal structure , purity , alloy composition , surface morphology , etc . in most cases , material quality is controlled by the adjustment of the growth conditions , such as substrate temperature , gas / molecular flow and their ratios which , in metalorganic vapor - phase epitaxy ( movpe ) , will affect precursors diffusion , surface decomposition processes , nucleation , diffusion of adatoms and their insertion at specific crystallographic sites and steps.@xcite for molecular - beam epitaxy , a well - founded conceptual and computational framework has emerged @xcite since the pioneering work of burton , cabrera , and frank ( bcf).@xcite systematic studies based on surface diffraction measurements and scanning tunneling microscopy , in conjunction with extensive computational modeling have identified and characterized many of the atomistic processes , even in the complex setting of iii - v systems.@xcite the corresponding development for movpe has been comparatively slow , due in part to the limited availability of _ in situ _
measurements.@xcite nevertheless , systematic _ ex situ _ measurements of growth morphologies , again in conjunction with theoretical modeling , have revealed the importance of precursor diffusion and decomposition at step edges in determining the nature and scale of surface morphologies.@xcite epitaxy - ready substrates are prepared by cutting individual slices out of....
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epitaxial overgrowth on such substrates may then proceed ( when truly `` epitaxial '' ) in one of three basic growth modes : step flow , where the overgrowing layer is advancing each exposed step at the same rate , creating an exact copy of the underlying surface ; step bunching , where terrace formation is observed due to clustering of individual steps ; or island formation , when the growth of new layer is initiated only at the step edges , but also between steps , in which case no long range order is observed .
if the growth conditions are not optimal , due to defect formation , the surface morphology can be corrupted and will not resemble any of the three main modes . for most applications ,
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Suppose that you have an abstract for a scientific paper: molecular dynamics computer simulations of a binary lennard - jones glass under shear are presented .
the mechanical response of glassy states having different thermal histories is investigated by imposing a wide range of external shear rates , at different temperatures .
the stress - strain relations exhibit an overshoot at a strain of around 0.1 , marking the yielding of the glass sample and the onset of plastic flow .
the amplitude of the overshoot shows a logarithmic behavior with respect to a dimensionless variable , given by the age of the sample times the shear rate .
dynamical heterogeneities having finite lifetimes , in the form of shear bands , are observed as the glass deforms under shear . by quantifying the spatial fluctuations of particle mobility ,
we demonstrate that such shearbanding occurs only under specific combinations of imposed shear - rate , age of glass and ambient temperature . .
And you have already written the first three sentences of the full article: the mechanical properties of amorphous solids have been harnessed extensively in designing materials which are ubiquitous in our everyday life . however , a complete microscopic understanding of the mechanisms leading to the macroscopic response of these materials is still missing . in order to develop materials with specific functions ,
it is necessary to have an improved knowledge of these underlying processes .
this remains a challenging task ..
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it is known that the material properties of amorphous solids , such as colloidal or metallic glasses , depend on their history of production , e.g. the cooling rate by which they were quenched from a fluid phase @xcite .
this dependence on the history , i.e. the age of the amorphous solid , is an important issue in computer simulations of glasses , especially because the accessible cooling rates in simulations are many orders of magnitudes larger than those accessible in experiments of real systems . with respect to the comparison between simulation and experiment
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Suppose that you have an abstract for a scientific paper: we numerically determine the very rich phase diagram of mass - imbalanced binary mixtures of hardcore bosons ( or equivalently fermions , or hardcore - bose / fermi mixtures ) loaded in one - dimensional optical lattices .
focusing on commensurate fillings away from half filling , we find a strong asymmetry between attractive and repulsive interactions .
attraction is found to always lead to pairing , associated with a spin gap , and to pair crystallization for very strong mass imbalance . in the repulsive case
the two atomic components remain instead fully gapless over a large parameter range ; only a very strong mass imbalance leads to the opening of a spin gap .
the spin - gap phase is the precursor of a crystalline phase occurring for an even stronger mass imbalance .
the fundamental asymmetry of the phase diagram is at odds with recent theoretical predictions , and can be tested directly via time - of - flight experiments on trapped cold atoms .
one - dimensional quantum liquids occupy a special place in the context of quantum many - body systems : indeed interactions of any strength lead to quantum fluctuations as strong as to discard bose condensation for bosons and the fermi liquid picture for fermions down to zero temperature . for sufficiently weak interactions
a new unifying paradigm of the so - called tomonaga - luttinger liquids ( tll ) emerges @xcite , characterized by the fact that all elementary excitations are gapless , and both diagonal and off - diagonal correlations decay algebraically with the distance .
recent advances in the trapping of ultracold atoms in optical lattices allow to realize one - dimensional quantum liquids in a highly flexible way , with the possibility of fully controlling the statistics and the interaction strength @xcite .
a series of recent experiments has demonstrated the physics of one - dimensional bose gases with strong interactions up to the hardcore ( or tonks - girardeau ) limit @xcite . a special role in the context of one - dimensional....
And you have already written the first three sentences of the full article: in this section we focus on the attractive case @xmath7 . the transition from the psf phase to the cdw phase , obtained for decreasing hopping ratio @xmath82 , is characterized by an inversion of the hierarchy between the pairing correlations , @xmath111 , and the density - density correlations @xmath112 . in the psf phase @xmath113 , while in the cdw phase @xmath114 .
the @xmath31 exponent , extracted from the low-@xmath74 behavior of the density structure factor as discussed in the text , is shown in fig . [ f.psf-cdw ] as a function of @xmath82 for various system sizes .
a finite - size extrapolation allows to identify the critical @xmath82 value at which @xmath31 traverses the critical value @xmath115 ..
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the composite @xmath2-@xmath3 pairs form therefore a tll with effective exponent @xmath116 . in the cdw phase
, we obtain a tll with @xmath117 , which is quite remarkable in a system with on - site interactions only .
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Suppose that you have an abstract for a scientific paper: we show that anderson localization in quasi - one dimensional conductors with ballistic electron dynamics , such as an array of ballistic chaotic cavities connected via ballistic contacts , can be understood in terms of classical electron trajectories only . at large length scales ,
an exponential proliferation of trajectories of nearly identical classical action generates an abundance of interference terms , which eventually leads to a suppression of transport coefficients .
we quantitatively describe this mechanism in two different ways : the explicit description of transition probabilities in terms of interfering trajectories , and an hierarchical integration over fluctuations in the classical phase space of the array cavities . .
And you have already written the first three sentences of the full article: the interplay of quantum phase coherence and repeated random scattering is at the origin of many effects in mesoscopic physics.@xcite these effects include weak localization and universal conductance fluctuations , both of which are small but fundamental corrections with respect to the conductance obtained from drude - boltzmann theory .
they culminate in anderson localization , the phenomenon that the resistance of a one or two - dimensional electron gas grows exponentially with system size if the system size is sufficiently large.@xcite originally , anderson localization and other mesoscopic effects were discovered in the context of disordered metals , in which electrons scatter off impurities with a size comparable to their wavelength .
theoretically , quantum effects in disordered metals are described using the ` disorder average ' which deals with an ensemble of macroscopically equivalent but microscopically different impurity configurations ..
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the presence of impurities is not essential for the existence of quantum effects , however .
the same effects , with the same statistical properties , have been found to appear if the electron motion is ballistic and chaotic , the only source of scattering of electrons being specular reflection off the sample boundaries.@xcite besides being of theoretical interest for understanding the quantum properties of systems with chaotic classical dynamics,@xcite the case of ballistic electron motion is relevant experimentally for very clean artificially structured two - dimensional electron gases in semiconductor heterostructures , such as quantum dots or antidot lattices.@xcite unlike disordered metals , in which impurities scatter diffractively , electrons in ballistic conductors have a well - defined classical dynamics .
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Suppose that you have an abstract for a scientific paper: the morphologies of wide - angle tailed ( wat ) radio sources ( edge - darkened , c - shaped , fr i radio sources ) are the result of confinement and distortion of the radio lobes by the dense x - ray - emitting gas in clusters or groups of galaxies .
these radio sources are easily seen at high redshifts ( @xmath0 ) in short - exposure images from the faint images of the radio sky at twenty - cm ( first ) survey . using a sample of approximately 400 wat sources from the first survey
, we have discovered a number of high-@xmath1 clusters . here
, we present the highest-@xmath1 cluster found so far using this method : 1137 + 3000 at @xmath2 .
we include photometric and spectroscopic results .
ten galaxies are confirmed at the cluster redshift , with a line - of - sight velocity dispersion of @xmath3 km s@xmath4 , typical of an abell richness class 0 cluster .
[ 1996/06/01 ] a&a .
And you have already written the first three sentences of the full article: wide - angle tailed ( wat ) radio sources were first defined as a class by owen & rudnick ( 1976 ) who described them as a sub - class of head - tail radio sources .
head - tail sources include a radio core and tails of radio emission trailing from the core as the host galaxy moves through the dense gas of a cluster s intracluster medium ( icm ) .
head - tail galaxies also include narrow - angle tails ( nats ) , which are generally associated with galaxies with large peculiar velocities in the outer parts of clusters ; the ram pressure from the interaction with the icm bends the radio lobes to create the nat structure ..
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owen & rudnick found that wats , however , are most often associated with bright elliptical or cd galaxies in the cores of clusters , and surmised that their smaller peculiar velocities would therefore produce smaller bends in the radio lobes , resulting in a wide - angle , rather than a narrow - angle , tailed morphology .
later work , by e.g. eilek et al .
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Suppose that you have an abstract for a scientific paper: i review some of the recent progress in string / m - theory epsf = 0 = 0 = 0 = 0 # 1 # 2 # 3=#1 = # 2 # 1 # 2 # 3=#1 = # 2 by - by - # 1 = cmbx12 = cmbx12 scaled 1 = cmbx12 scaled 2 amssym.def amssym.tex .
And you have already written the first three sentences of the full article: when i was asked to give this plenary lecture in place of ashoke sen , i had some considerable misgivings that i would be able to do the subject the justice that he would undoubtedly have .
however i had no doubts about what i should speak .
the subject formerly known as string theory , and increasingly frequently being referred to as m - theory , has made some stunning advances since gr14 ..
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hence my title .
i should perhaps apologize , especially in india , for its wording .
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Suppose that you have an abstract for a scientific paper: the lorenz 1963 dynamical system is known to reduce in the steady state to a one - dimensional motion of a classical particle subjected to viscous damping in a past history - dependent potential field .
if the potential field is substituted by a periodic function of the position , the resulting system shows a rich dynamics where ( standard ) diffusive behaviours , ballistc motions and trapping take place by varying the model control parameters .
this system permits to highlight the intimate relation between chaos and long - time deterministic diffusion . .
And you have already written the first three sentences of the full article: chaotic dynamical systems are known to exhibit typical random processes behaviour due to their strong sensitivity to initial conditions .
deterministic diffusion arises from the chaotic motion of systems whose dynamics is specified , and it should be distinguished from noise induced diffusion where the evolution is governed by probabilistic laws .
diffusive ( standard and anomalous ) behaviours have been observed in periodic chaotic maps ( see , _.
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e.g. _ , refs .
@xcite and references therein ) and in continuous time dynamical systems @xcite .
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Suppose that you have an abstract for a scientific paper: we study the ground - state properties of spin-1/2 fermionic atoms confined in a one - dimensional optical superlattice with harmonic confinement by using the density matrix renormalization group method . for this purpose
, we consider an ionic hubbard model that has superlattice potentials with 2-site periodicity .
we find that several different types of insulating regimes coexist even if the number of atoms at each site is not an integer , but its average within the unit cell is an integer or half integer .
this is contrasted to the coexisting phase of the metallic and mott - insulating regimes known for the ordinary hubbard model in an optical lattice .
the phase characteristics are elucidated by investigating the profiles of the atom density , the local density / spin fluctuations , the double occupation probability and the spin correlations in detail . .
And you have already written the first three sentences of the full article: experimental techniques for manipulating ultracold atoms have made great progress since the successful realization of atomic bose - einstein condensates ( becs ) @xcite .
optical lattices , formed by a standing wave of laser light , are providing the ideal stages for an experimental investigation of the fundamental many - body problems in condensed matter physics via ultracold atomic gases @xcite .
a recent series of experimental studies on bosonic mott - insulators @xcite have clearly demonstrated this feature , namely the realization of quantum simulators ..
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a noteworthy advantage of atomic gases over condensed matter such as solids or liquids is that their experimental parameters are highly controllable .
both density and temperature of atomic gases are fully controlled in the process of evaporative cooling @xcite .
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Suppose that you have an abstract for a scientific paper: we establish several analogues of the classical lidskii theorem for some special classes of singular traces ( dixmier traces and connes - dixmier traces ) used in noncommutative geometry . .
And you have already written the first three sentences of the full article: an important role in noncommutative geometry @xcite is played by the set of compact operators whose partial sums of singular values are logarithmically divergent .
this set can be adequately described using the terminology of marcinkiewicz spaces .
consider the marcinkiewicz sequence space @xmath0 where we set @xmath1 here , @xmath2 is the sequence @xmath3 rearranged in nonincreasing order ..
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fix an infinite - dimensional separable complex hilbert space @xmath4 and consider the set @xmath5 of all compact operators @xmath6 on @xmath4 such that the sequence of its singular values @xmath7 falls into the space @xmath8 ( recall that the singular values of a compact operator @xmath9 are the eigenvalues of the operator @xmath10 ) .
we set @xmath11 it is well known that the ideal of compact operators @xmath5 equipped with the norm @xmath12 is a banach space .
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Suppose that you have an abstract for a scientific paper: we study theoretical and empirical aspects of the mean exit time of financial time series .
the theoretical modeling is done within the framework of continuous time random walk .
we empirically verify that the mean exit time follows a quadratic scaling law and it has associated a pre - factor which is specific to the analyzed stock .
we perform a series of statistical tests to determine which kind of correlation are responsible for this specificity .
the main contribution is associated with the autocorrelation property of stock returns .
we introduce and solve analytically both a two - state and a three - state markov chain models .
the analytical results obtained with the two - state markov chain model allows us to obtain a data collapse of the 20 measured met profiles in a single master curve . .
And you have already written the first three sentences of the full article: the continuous time random walk ( ctrw ) formalism introduced four decades ago by montroll and weiss @xcite has been successfully applied to a wide and diverse variety of physical phenomena over the years @xcite but only recently to finance @xcite . in this latter context , the efforts have been mostly focused on the statistical properties of the waiting time between successive transactions and the asset return at each transaction .
different studies in different markets are conceiving the idea that the empirical distributions of both random variables are compatible with an asymptotic fat tail behavior @xcite . within the ctrw formalism
some of us have recently investigated the mean exit time ( met ) of asset prices out of a given interval of size @xmath0 for financial time series @xcite ..
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this study shows that the met follows a quadratic growth in terms of @xmath0 for small interval lengths @xmath0 . in the same study ,
this functional form was observed for a specific time series of the foreign exchange ( fx ) market , which is the u.s .
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Suppose that you have an abstract for a scientific paper: high - contrast imaging from space must overcome two major noise sources to successfully detect a terrestrial planet angularly close to its parent star : photon noise from diffracted star light , and speckle noise from star light scattered by instrumentally - generated wavefront perturbation .
coronagraphs tackle only the photon noise contribution by reducing diffracted star light at the location of a planet .
speckle noise should be addressed with adaptative - optics systems . following the tracks of @xcite
, we develop in this paper two analytical methods for wavefront sensing and control that aims at creating _ dark holes _ , i.e. areas of the image plane cleared out of speckles , assuming an ideal coronagraph and small aberrations .
the first method , _ speckle field nulling _ , is a fast fft - based algorithm that requires the deformable - mirror influence functions to have identical shapes .
the second method , _ speckle energy minimization _
, is more general and provides the optimal deformable mirror shape via matrix inversion . with a @xmath0 deformable mirror ,
the size of matrix to be inverted is either @xmath1 in the general case , or only @xmath0 if influence functions can be written as the tensor product of two one - dimensional functions .
moreover , speckle energy minimization makes it possible to trade off some of the dark hole area against an improved contrast . for both methods , complex wavefront aberrations ( amplitude and phase )
are measured using just three images taken with the science camera ( no dedicated wavefront sensing channel is used ) , therefore there are no non - common path errors .
we assess the theoretical performance of both methods with numerical simulations including realistic speckle noise and experimental influence functions .
we find that these speckle nulling techniques should be able to improve the contrast by several orders of magnitude . .
And you have already written the first three sentences of the full article: the field of extrasolar planet research has recently made a leap forward with the direct detection of extrasolar giant planets ( egps ) . using spitzer space telescope ,
@xcite and @xcite have detected infrared photons from two transiting planets , tres-1b and hd209458b , respectively .
@xcite have reported the infrared imaging of an egp orbiting the nearby young brown dwarf 2m1207 with vlt / naco , whereas @xcite have collected evidence for an egp companion to the t - tauri star gq lup using vlt / naco as well ..
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although there are claims that the direct detection of terrestrial planets could be performed from the ground with yet to come extremely large telescopes @xcite , it is widely believed that success will be more likely in space .
direct detection is the key to spectroscopy of planetary atmospheres and discovery of biomarkers , namely indirect evidence of life developed at the planetary scale ( e.g. * ? ? ?
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Suppose that you have an abstract for a scientific paper: dynamics of deterministic systems perturbed by random additive noise is characterized quantitatively . since for such systems the kolmogorov - sinai ( ks )
entropy diverges if the diameter of the partition tends to zero , we analyze the difference between the total entropy of a noisy system and the entropy of the noise itself . we show that this quantity is finite and non negative and call it the dynamical entropy of the noisy system . in the weak noise limit
this quantity is conjectured to tend to the ks - entropy of the deterministic system . in particular , we consider one - dimensional systems with noise described by a finite - dimensional kernel for which the frobenius - perron operator can be represented by a finite matrix . .
And you have already written the first three sentences of the full article: stochastic perturbations are typical for any physical realization of a given dynamical system .
also round - off errors , inevitable in numerical investigation of any dynamics , may be considered as a random noise .
quantitative characterization of dynamical systems with external stochastic noise is a subject of several recent studies @xcite . on the other hand ,.
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the influence of noise on various low dimensional dynamical systems and the properties of random dynamical systems have been extensively studied for many years @xcite .
consider a discrete dynamical system generated by @xmath0 , where @xmath1 is a subset of @xmath2 , in the presence of an additive noise @xmath3 where @xmath4 are independent random vectors fulfilling @xmath5 and @xmath6 .
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Suppose that you have an abstract for a scientific paper: we report on the first high - resolution spectroscopic analysis of , a bright ( @xmath0 ) , ultra metal - poor ( @xmath1 $ ] = @xmath24.1 ) , carbon - enhanced ( @xmath3 $ ] = @xmath41.7 ) star selected from the hamburg / eso survey .
this star exhibits low abundances of neutron - capture elements ( @xmath5 $ ] = @xmath6 ) , and an absolute carbon abundance @xmath7(c ) = 6.1 ; based on either criterion , is sub - classified as a cemp - no star .
we show that the light - element abundance pattern of is consistent with predicted yields from a massive ( m = @xmath8 ) , primordial composition , supernova ( sn ) progenitor .
we also compare the abundance patterns of other ultra metal - poor stars from the literature with available measures of c , n , na , mg , and fe abundances with an extensive grid of sn models ( covering the mass range @xmath9 ) , in order to probe the nature of their likely stellar progenitors .
our results suggest that at least two classes of progenitors are required at @xmath1 $ ] @xmath10 , as the abundance patterns for more than half of the sample studied in this work ( 7 out of 12 stars ) can not be easily reproduced by the predicted yields . .
And you have already written the first three sentences of the full article: observational evidence has emerged over the past few decades indicating that carbon is ubiquitous in the early universe . the class of carbon - enhanced metal - poor ( cemp ; @xmath3$]@xmath11 , e.g. , * ? ? ?
* ; * ? ? ?
* ) stars are found with increasing fractions at lower metallicities , and account for at least 80% of all ultra metal - poor ( ump ; [ fe / h]$ ] = @xmath12 , where @xmath13 is the number density of atoms of elements @xmath14 and @xmath15 in the star ( @xmath16 ) and the sun ( @xmath17 ) , respectively . ].
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@xmath18 ) stars observed to date @xcite .
in particular , the so - called cemp - no stars ( which exhibit sub - solar abundances of neutron - capture elements ; e.g. , @xmath5 $ ] @xmath19 0.0 ) are believed to be direct descendants from the very first stellar generations formed after the big bang @xcite .
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Suppose that you have an abstract for a scientific paper: we show that long period dwarf novae offer a promising route for making type ia supernovae . for typical dwarf
nova duty cycles @xmath0 , mass is accreted by the white dwarf mainly during dwarf nova outbursts at rates allowing steady nuclear burning of most of the accreted matter .
mass gains up to @xmath1 are possible in this way .
although these are too small to allow a @xmath2 wd to reach the chandrasekhar mass , they are sufficient if the wd grew to @xmath3 in a previous episode of thermal timescale mass transfer , i.e. for those long period dwarf novae which descend from supersoft binaries .
a further advantage of this picture is that the supernova always occurs in a binary of small secondary / primary mass ratio , with the secondary having very little remaining hydrogen .
both features greatly reduce the possibility of hydrogen contamination of the supernova ejecta . accretion , accretion discs binaries : general x rays : binaries stars : dwarf novae
supernovae : general galaxies : stellar content cosmology : distance scale .
And you have already written the first three sentences of the full article: it is now generally agreed that type ia supernovae originate from accreting white dwarfs , and widely accepted that their occurrence signals arrival at the chandrasekhar mass @xmath4 .
however there is no consensus as to how the white dwarf gains mass ( see e.g. livio , 2001 , for a review ) .
two possibilities are currently discussed . in the first.
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, two white dwarfs merge as their relative orbit shrinks under gravitational radiation ( the double degenerate scenario ) . in the second possibility
, a white dwarf accretes from a non degenerate companion ( the single degenerate scenario ) .
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Suppose that you have an abstract for a scientific paper: we use the microlensing variability observed for nine gravitationally lensed quasars to show that the accretion disk size at 2500 is related to the black hole mass by @xmath0@xmath1m@xmath2 .
this scaling is consistent with the expectation from thin disk theory ( @xmath3 ) , but it implies that black holes radiate with relatively low efficiency , @xmath4 where @xmath5 .
these sizes are also larger , by a factor of @xmath6 , than the size needed to produce the observed @xmath7 quasar flux by thermal radiation from a thin disk with the same @xmath8 temperature profile .
more sophisticated disk models are clearly required , particularly as our continuing observations improve the precision of the measurements and yield estimates of the scaling with wavelength and accretion rate . .
And you have already written the first three sentences of the full article: despite nearly 40 years of work on accretion disk physics , the simple @xcite thin disk model and its relativistic cousins ( e.g. * ? ? ?
* ; * ? ? ?
* ; * ? ? ?.
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* ) remain the standard model despite many theoretical alternatives ( e.g. * ? ? ?
* ; * ? ? ?
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Suppose that you have an abstract for a scientific paper: recent observational studies of intermediate- and high - mass star - forming regions at submillimeter and infrared wavelengths are reviewed , and chemical diagnostics of the different physical components associated with young stellar objects are summarized .
procedures for determining the temperature , density and abundance profiles in the envelopes are outlined .
a detailed study of a set of infrared - bright massive young stars reveals systematic increases in the gas / solid ratios , the abundances of evaporated molecules , and the fraction of heated ices with increasing temperature .
since these diverse phenomena involve a range of temperatures from @xmath0k to 1000 k , the enhanced temperatures must be communicated to both the inner and outer parts of the envelopes .
this ` global heating ' plausibly results from the gradual dispersion of the envelopes with time .
similarities and differences with low - mass ysos are discussed .
the availability of accurate physical models will allow chemical models of ice evaporation followed by ` hot core ' chemistry to be tested in detail . .
And you have already written the first three sentences of the full article: massive star - forming regions have traditionally been prime targets for astrochemistry owing to their bright molecular lines ( e.g. , johansson et al .
1984 , cummins et al .
1986 , irvine et al . 1987 , ohishi 1997 ).
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. massive young stellar objects ( ysos ) have luminosities of @xmath1 l@xmath2 and involve young o- and b - type stars . because their formation proceeds more rapidly than that of low - mass stars and involves ionizing radiation , substantial chemical differences may be expected .
the formation of high mass stars is much less well understood than that of low - mass stars .
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Suppose that you have an abstract for a scientific paper: a simple spatial computer simulation model was recently introduced to study the evolution of the linguistic diversity @xcite .
the model considers processes of selective geographic colonization , linguistic anomalous diffusion and mutation . in the approach , we ascribe to each language a fitness function which depends on the number of people that speak that language . here
we extend the aforementioned model to examine the role of saturation of the fitness on the language dynamics .
we found that the dependence of the linguistic diversity on the area after colonization displays a power law regime with a nontrivial exponent in very good agreement with the measured exponent associated with the actual distribution of languages on the earth .
@xmath0departamento de fsica , universidade federal de pernambuco , 50670 - 901 , recife , pe , brazil + @xmath1departamento de fsica e matemtica , universidade federal rural de pernambuco 52171 - 900 , dois irmos , recife - pe , brazil + @xmath2centro de informtica , universidade federal de pernambuco , 50670 - 901 , recife , pe , brazil .
And you have already written the first three sentences of the full article: the research in language dynamics has arose an increasing interest of the complex systems community in the last years .
most of the researchers focus their investigations on issues like rise , competition , extinction risk and death of languages @xcite .
furthermore , recent advances in archeology , genetics and linguistics have provided relevant contributions to a better comprehension of the linguistic diversification @xcite ..
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some investigations have demonstrated that distinct causes have greatly affected the evolution of the linguistic diversity . among the main elements are geographic factors , economic features , complexity of the language , to cite just a few .
for instance , sutherland @xcite has shown that beside country area , forest area and maximum altitude contribute to increase diversity , whereas the diversity decreases for a larger latitude . according to bellwood @xcite and renfrew @xcite
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Suppose that you have an abstract for a scientific paper: we formulate the first order fermi acceleration in shock waves in terms of the random walk theory .
the formulation is applicable to any value of the shock speed and the particle speed , in particular , to the acceleration in relativistic shocks and to the injection problem , where the particle speed is comparable to the fluid speed , as long as large angle scattering is suitable for the scattering process of particles .
we first show that the trajectory of a particle suffering from large angle scattering can be treated as a random walk in a moving medium with an absorbing boundary ( e.g. , the shock front ) .
we derive an integral equation to determine the density of scattering points of the random walk , and by solving it approximately we obtain approximate solutions of the probability density of pitch angle at and the return probability after the shock crossing in analytic form .
these approximate solutions include corrections of several non - diffusive effects to the conventional diffusion approximation and we show that they agree well with the monte carlo results for isotropic scattering model for any shock speed and particle speed . when we neglect effects of ` a few step return ' , we obtain ` the multi - step approximation ' which includes only the effect of finite mean free path and which is equivalent to ` the relativistic diffusion approximation ' used by peacock ( 1981 ) if the correct diffusion length is used in his expression .
we find that the multi - step approximation is not appropriate to describe the probability densities of individual particles for relativistic shocks , but that the pitch angle distribution at the shock front in steady state is in practice quite well approximated by that given by the multi - step approximation because the effects of finite mean free path and a few step return compensate each other when averaged over pitch angle distribution .
finally , we give an analytical expression of the spectral index of accelerated particles in parallel shocks valid for....
And you have already written the first three sentences of the full article: it is now widely accepted that the first order fermi acceleration , which is driven in various astrophysical shocks , provides a factory of non - thermal energetic particles .
for example , recent observations discovered synchrotron x - rays from energetic electrons with energies above @xmath0ev in the shell of the supernova remnant 1006 @xcite . since the basic theory was proposed more than 20 years ago by 78 , krymski ( 1977 ) , axford et al .
( 1977 ) , and blandford and ostriker ( 1978 ) , many papers have dealt with fundamental mechanisms of shock acceleration ..
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the mechanism has been applied to many situations ranging from interplanetary shocks to relativistic shocks in active galactic nuclei or gamma - ray bursts ( see for review blandford & eichler 1987 and kirk & duffy 1999 ) .
although most of the recent theoretical interests have been concentrated on non - linear problems where the shock structure is modified by accelerated particles ( ellison , baring & jones 1996 , berezhko & ellison 1999 ) , some of the linear problems in the test particle approximation still remain to be clarified and need more close examinations , especially for relativistic shocks , oblique shocks and injection of seed particles .
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Suppose that you have an abstract for a scientific paper: in the framework of the spatial coherence wavelets , different features of the first - order spatial coherence ( young s interference ) are analyzed by calculating the corresponding marginal power spectrum , a close related quantity to the classical wigner distribution function ( wdf ) of the optical field .
the consideration of the radiant and virtual point sources evidences some effects , conventionally attributed to non - classical correlations of light , although such type of the correlations are not explicitly included in the model .
specifically , a light state is produced that has similar morphology to the wdf of the well - known quantum schdinger cat state . .
And you have already written the first three sentences of the full article: the advances on cavity quantum electrodynamics ( cqed ) and on semi - conductor quantum electrodynamics ( scqed ) , reached in the last three decades , allowed developing devices that approach the predictions of the quantum theory of the matter - radiation interaction to the experimental results . in this context , the manipulation of the quantum states of light is a subject of growing interest , with topics as the production of only - one photon sources @xcite , the analysis of the quantum interference mechanisms like the schrdinger cat states of light @xcite and those derived from the matter - radiation interaction @xcite for instance .
they are promising topics for technological applications in quantum computation and information processing @xcite , quantum teleportation @xcite and quantum opto - electronic system @xcite-@xcite .
+ in spite of the accepted quantum nature of topics as the schrdinger cat states , a classical approach to them seems to be possible by adding novel considerations to the phase - space representation of the optical wave - field , like the spatial coherence wavelets emitted by both radiant and virtual point sources @xcite ..
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it could revaluate the actual limits of the classical theories and the real grounds of the physical behavior of light .
for instance , the analysis presented in this paper suggest that the schrdinger cat states are actually originated by the spatial coherence state of the light .
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Suppose that you have an abstract for a scientific paper: we present a new approach to calculate real - time quantum dynamics in complex systems .
the formalism is based on the partitioning of a system s environment into `` core '' and `` reservoir '' modes , with the former to be treated quantum mechanically and the latter classically .
the presented method only requires the calculation of the system s reduced density matrix averaged over the quantum core degrees of freedom which is then coupled to a classically evolved reservoir to treat the remaining modes .
we demonstrate our approach by applying it to the spin - boson problem using the noninteracting blip approximation to treat the system and core , and ehrenfest dynamics to treat the reservoir .
the resulting hybrid methodology is accurate for both fast and slow baths , since it naturally reduces to its composite methods in their respective regimes of validity .
in addition , our combined method is shown to yield good results in intermediate regimes where neither approximation alone is accurate and to perform equally well for both strong and weak system - bath coupling .
our approach therefore provides an accurate and efficient methodology for calculating quantum dynamics in complex systems . .
And you have already written the first three sentences of the full article: the calculation of real - time quantum dynamics for large molecular systems is a longstanding problem in chemical physics . of particular interest
is the case of a small subsystem embedded in a surrounding thermal bath , which forms the basis for the investigation of condensed phase energy and electron transfer as well as spin and charge transport in nanoscale devices@xcite . in such situations ,
one is typically interested in the calculation of the system s _ reduced _ dynamics , averaged over the bath degrees of freedom ..
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due to the importance of these problems and the absence of a general solution , a variety of methods have been developed which vary as to the regimes in which they are accurate and their applicability to large systems .
many of these approaches rely on either averaging over semi - classical trajectories of bath degrees of freedom or propagating the system s reduced density matrix ( rdm ) directly without explicit treatment of the bath , for example by master equations or path integral techniques .
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Suppose that you have an abstract for a scientific paper: in this work , we establish the response of scalar systems with multiple discrete delays based on the laplace transform . the time response function is expressed as the sum of infinite series of exponentials acting on eigenvalues inside countable branches of the lambert w functions .
eigenvalues in each branch of lambert w function are computed by a numerical iteration .
numerical examples are presented to illustrate the results obtained .
delay system , lambert w function , multiply delays , time response , 34a45 , 34k06 , 34k07 , 34k35 , 44a10 .
And you have already written the first three sentences of the full article: dynamical systems with delays play an important role in modeling natural processes which include the influence of past effects for a better description of the evolution . in classical physics , life sciences , physiology , engineering system , neural networks , epidemiology , and economics
, realistic models must take in account the time - delays due to the finite propagation speed to determine the future evolution .
many examples of real phenomena with delay effects can be found in @xcite ..
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furthermore of importance in applications , the delay system is , in general , described by delay differential equations which have several distinct mathematical properties of ordinary and partial differential equations , and also provides them with a purely mathematical interest . in this work , we consider the differential equation with discrete delays .
let @xmath0 , @xmath1 , not all zero @xmath2 , @xmath3 , and @xmath4 is a continuous preshape function defined on @xmath5 $ ] .
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Suppose that you have an abstract for a scientific paper: the tolerance of bacterial populations to biocidal or antibiotic treatment has been well documented in both biofilm and planktonic settings . however , there is still very little known about the mechanisms that produce this tolerance .
evidence that small , non - mutant subpopulations of bacteria are not affected by antibiotic challenge has been accumulating and provides an attractive explanation for the failure of typical dosing protocols .
although a dosing challenge can kill all the susceptible bacteria , the remaining persister cells can serve as a source of population regrowth .
we give a robust condition for the failure of a periodic dosing protocol for a general chemostat model , which supports the mathematical conclusions and simulations of an earlier , more specialized batch model .
our condition implies that the treatment protocol fails globally , in the sense that a mixed bacterial population will ultimately persist above a level that is independent of the initial composition of the population .
we also give a sufficient condition for treatment success , at least for initial population compositions near the steady state of interest , corresponding to bacterial washout .
finally , we investigate how the speed at which the bacteria are wiped out depends on the duration of administration of the antibiotic .
we find that this dependence is not necessarily monotone , implying that optimal dosing does not necessarily correspond to continuous administration of the antibiotic .
thus , genuine periodic protocols can be more advantageous in treating a wide variety of bacterial infections . * keywords : persister , biofilm , model , chemostat , tolerance * .
And you have already written the first three sentences of the full article: the failure of antibiotic treatments to eliminate bacterial infections has become both more evident and better understood in the past several decades . although there is evidence that the over use of antibiotics has amplified the number of chromosomal - resistant bacteria @xcite , it is becoming increasingly clear that there are other mechanisms that protect populations of bacteria
. many of these mechanisms depend on whether the bacteria exist in a biofilm or not @xcite .
in particular , the notion that small sub - populations of bacteria may display innate tolerance to various biocides has been proposed as a possible reason for the failure of treatment for bacterial infections @xcite ..
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bacteria within a biofilm are enmeshed in a physical gel that provides a secondary boundary that may allow small numbers of bacteria to evade the antibiotic ; therefore , the failure to eliminate the entire population can allow the population to regrow . it should be noted that populations of planktonic bacteria also contain these highly tolerant or persister cells @xcite . thus understanding the process of persister formation and the response of the population to biocidal application is fundamental to developing dosing protocols and treatments in both batch culture and biofilm populations . as in many areas of biology
, mathematical modeling has been used as a counterpart to experimental observations . because there are several hypotheses regarding the mechanism of persister formation
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Suppose that you have an abstract for a scientific paper: ultra high energy neutrinos are produced by the interaction of hadronic cosmic rays with the cosmic radiation background .
more exotic scenarios like _ topological defects _ or _ new hadrons _ predict even larger fluxes .
in particular , earth skimming tau neutrinos could be detected by the fluorescence detector ( fd ) of pierre auger observatory .
a detailed evaluation of the expected number of events has been performed for a wide class of neutrino flux models .
an updated computation of the neutrino nucleon cross section and of the tau energy losses has been carried out . for the most optimistic theoretical models , about one earth skimming neutrino event is expected in several years at fd .
* earth skimming uhe tau neutrinos at the fluorescence detector of pierre auger observatory * * c. aramo*@xmath0 , * a. insolia*@xmath1 , * a. leonardi*@xmath1 , * g. miele*@xmath0 , * l. perrone*@xmath2 , * o. pisanti*@xmath0 , * d.v .
semikoz*@xmath3 _ @xmath0 dipartimento di scienze fisiche , universit di napoli `` federico ii '' and istituto nazionale di fisica nucleare sezione di napoli , complesso universitario di monte s. angelo , via cinthia , i-80126 napoli , italy .
+ @xmath1 dipartimento di fisica e astronomia , universit di catania and istituto nazionale di fisica nucleare sezione di catania , via s. sofia 64 , i-95123 catania , italy .
+ @xmath2 fachbereich c , sektion physik , universitt wuppertal , d-42097 wuppertal , germany .
+ @xmath4 department of physics and astronomy , ucla , los angeles , ca 90095 - 1547 usa .
+ @xmath5 inr ras , 60th october anniversary prospect 7a , 117312 moscow , russia . _ _ pacs numbers : 95.85.ry , 13.15.+g , 96.40.tv , 95.55.vj , 13.35.dx;_ = .8 cm .
And you have already written the first three sentences of the full article: the measurement of ultra high energy cosmic rays ( uhecr ) flux is the goal of a wide class of past , present and future detectors @xcite-@xcite .
uhe neutrinos are expected to be produced by the interaction of hadronic matter with the surrounding radiation / matter . a search for this signal is currently performed by several neutrino telescopes @xcite-@xcite .
neutrinos with energy above @xmath6 ev are expected to originate from the interaction of uhe cosmic rays with the cosmic microwave background ( cmb ) _ via _ the @xmath7-photoproduction , @xmath8 , the so - called _ cosmogenic neutrinos _.
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the prediction for such a flux is however affected by several uncertain physical quantities , namely the spatial distribution of astrophysical sources , the ejected proton fluxes ( if proton ) and the way of modelling the diffuse extragalactic electromagnetic background in the different frequency regions .
one can assume a reasonable ansatz for all these quantities combined with the measurement of the diffuse photon flux in the gev region by egret @xcite , and the agasa / hires data .
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Suppose that you have an abstract for a scientific paper: it is known that the gauge field and its composite operators evolved by the yang
mills gradient flow are ultraviolet ( uv ) finite without any multiplicative wave function renormalization . in this paper , we prove that the gradient flow in the 2d @xmath0 non - linear sigma model possesses a similar property : the flowed @xmath1-vector field and its composite operators are uv finite without multiplicative wave function renormalization .
our proof in all orders of perturbation theory uses a @xmath2-dimensional field theoretical representation of the gradient flow , which possesses local gauge invariance without gauge field . as application of the uv finiteness of the gradient flow
, we construct the energy
momentum tensor in the lattice formulation of the @xmath0 non - linear sigma model that automatically restores the correct normalization and the conservation law in the continuum limit . .
And you have already written the first three sentences of the full article: the yang mills gradient flow or the wilson flow @xcite has attracted much attention in recent years in the context of lattice gauge theory .
its known applications include , scale setting @xcite , definition of the topological charge @xcite , definition of non - perturbative gauge coupling @xcite , chiral condensation @xcite , improvement of step scaling @xcite , etc .
even its application to supersymmetric theory @xcite and to the operator product expansion @xcite is considered ..
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reference @xcite is a review of this notion and further related works can be found in a review @xcite and in a most recent paper on the non - perturbative beta function @xcite . a crucial property of the yang
mills gradient flow , underlying the above applications , is its `` ultraviolet ( uv ) finiteness '' @xcite . the gradient flow is a one - parameter ( called the flow - time ) evolution of the gauge field , according to a `` heat diffusion equation '' ( called the flow equation ) . a remarkable fact that can be rigorously proven @xcite in all orders of perturbation theory
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Suppose that you have an abstract for a scientific paper: we study the cosmological evolution of massless single - field scalar - tensor theories of gravitation from the time before the onset of @xmath0 annihilation and nucleosynthesis up to the present . the cosmological evolution together with the observational bounds on the abundances of the lightest elements ( those mostly produced in the early universe ) place constraints on the coefficients of the taylor series expansion of @xmath1 , which specifies the coupling of the scalar field to matter and is the only free function in the theory . in the case when @xmath1 has a minimum ( i.e. , when the theory evolves towards general relativity ) these constraints translate into a stronger limit on the post - newtonian parameters @xmath2 and @xmath3 than any other observational test .
moreover , our bounds imply that , even at the epoch of annihilation and nucleosynthesis , the evolution of the universe must be very close to that predicted by general relativity if we do not want to over- or underproduce @xmath4he .
thus the amount of scalar field contribution to gravity is very small even at such an early epoch . # .
And you have already written the first three sentences of the full article: scalar - tensor ( st ) theories of gravitation have a long history . the first ones to appear were those of jordan@xcite , fierz@xcite , and brans - dicke@xcite .
these are the simplest theories in the sense that they consist of just one massless scalar field and its coupling strength to matter is constant .
later bergmann@xcite , nordtvedt@xcite , and wagoner@xcite generalized the theory . in their versions.
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the scalar field has a dynamic ( scalar field dependant ) coupling to matter and/or an arbitrary self - interaction .
more recently , in a very comprehensive work , damour and esposito - farse@xcite considered the theory with multiple scalar fields .
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Suppose that you have an abstract for a scientific paper: sgr a east is a very prominent elongated shell structure surrounding ( though off - centered from ) the galactic nucleus .
its energetics ( @xmath0 ergs ) , based on the power required to carve out the radio synchrotron remnant within the surrounding dense molecular cloud , appear to be extreme compared to the total energy ( @xmath1 ergs ) released in a typical supernova ( sn ) explosion .
yet it shares several characteristics in common with sn remnants ( snrs ) , the most significant of which is the @xmath2 gev @xmath3-ray spectrum measured by egret , if we associate the galactic center source 2egj1746 - 2852 with this nonthermal shell . we here show that the highest - energy component in sgr a east s spectrum , like that of snrs , can be fitted with the @xmath3-rays produced in @xmath4 decays .
further , we demonstrate in a self - consistent manner that the leptons released in the associated @xmath5 decays produce an @xmath6 distribution that can mimic a power - law with index @xmath7 , like that inferred from the vla data for this source .
these relativistic electrons and positrons also radiate by bremsstrahlung , and inverse compton scattering with the intense ir and uv fields from the nucleus .
we show that the overall emissivity calculated in this way may account for sgr a east s broadband spectrum ranging from ghz frequencies all the way to tev energies , where whipple has thus far set an upper limit to the flux corresponding to a @xmath8 signal above the noise .
3gcm^-3 3cm^-3 # 1#1 #1#2#3#1 , a&a , * # 2 * , # 3 .
# 1#2#3#1 , a&a _ ( letters ) _ , * # 2 * , # 3 .
# 1#2#3#1 , a&as , # 2 , # 3 # 1#2#3#1 , aj , # 2 , # 3 # 1#2#3#1 , _ apj _ , * # 2 * , # 3 .
# 1#2#3#1 , _ apj ( letters ) _ , * # 2 * , # 3 .
# 1#2#3#1 , apjs , # 2 , # 3 # 1#2#3#1 , ara&a , # 2 , # 3 # 1#2#3#1 , baas , # 2 , # 3 # 1#2#3#1 , icarus , # 2 , # 3 # 1#2#3#1 , _ mnras _ , * # 2 * , # 3 .
# 1#2#3#1 , _ nature _ , * # 2 * , # 3 .
# 1#2#3#1 , pasj , # 2 , # 3 # 1#2#3#1 , pasp , # 2 , # 3 # 1#2#3#1 ,....
And you have already written the first three sentences of the full article: sgr a east is an elliptical shell structure elongated along the galactic plane with a major axis of length @xmath9 pc and a center displaced from the apparent dynamical nucleus , sgr a west , by @xmath10 pc in projection toward negative galactic latitudes .
the latter is a ( @xmath11 pc ) three - arm spiral configuration of ionized gas ( ekers et al . 1983 ; lo & claussen 1983 ) that engulfs a compact nonthermal radio source , sgr a * , having a dimension between 1.1 au and 0.1 au ( morris & serabyn 1996 ) .
the bulk of the thermally emitting sgr a west appears to be located in front of sgr a east ( yusef - zadeh & morris 1987 ; pedlar et al . 1989 ) , whose exact distance behind the nucleus is not known , but a number of arguments suggest that it is positioned very close to the galactic center ( e.g. , gsten & downes 1980 ; goss et al ..
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1989 ; yusef - zadeh et al . 1998 ) .
thus , if present , the massive black hole ( presumably associated with sgr a * ) lies within the sgr a east shell , but at one extreme end of its elongated structure .
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Suppose that you have an abstract for a scientific paper: many immunization strategies have been proposed to prevent infectious viruses from spreading through a network . in this work ,
we study efficient immunization strategies to prevent a default contagion that might occur in a financial network .
an essential difference from the previous studies on immunization strategy is that we take into account the possibility of serious side effects . _ uniform immunization _ refers to a situation in which banks are vaccinated with a common low - risk asset .
the riskiness of immunized banks will decrease significantly , but the level of systemic risk may increase due to the de - diversification effect . to overcome this side effect
, we propose another immunization strategy , called _ counteractive immunization _ , which prevents pairs of banks from failing simultaneously .
we find that counteractive immunization can efficiently reduce systemic risk without altering the riskiness of individual banks . since the global financial crisis of 2007 - 2009
, many researchers in various fields of natural and social sciences , such as physicists , ecologists and economists , have been tackling the question of how to reduce financial systemic risk.@xcite many of those studies are based on network theory , which has been used extensively to explore complex systems since the early 2000s .
percolation is one of the most frequently used concepts in thinking about the fragility of networks .
percolation theory provides a way to reveal the threshold of the number of removed nodes above which the giant component disintegrates.@xcite applying this theory , researchers examined the fragility of various types of actual complex networks , such as the internet , road networks , and power grids.@xcite percolation theory also gives us some useful insights into the question of how to control the way in which infectious viruses spread through a network .
many studies proposed various immunization strategies to make the percolation threshold as small as possible.@xcite ....
And you have already written the first three sentences of the full article: following gai and kapadia@xcite , a _ financial crisis _ is defined as a situation in which at least 5% of banks go bankrupt .
fig.1 illustrates the frequency and the conditional average of the size of crises .
some interesting properties are observed ..
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first , fig.1a reveals that the uniform immunization strategy based on pagerank is most successful in terms of reducing the frequency of crises .
the least efficient one is random immunization .
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Suppose that you have an abstract for a scientific paper: electron capture and emission by coulomb scattering in self - assembled quantum dot ( qd ) devices is studied theoretically . while the dependence of the coulomb scattering ( auger ) rates on the local wetting layer electron density has been a topic of intense research , we put special interest on the remote scattering between qd electrons and continuum electrons originating from a quantum well , doped bulk layers or metal contacts .
numerical effort is made to include all microscopic transitions between the fermi distributed continuum states .
the remote coulomb scattering is investigated as a function of the electron density , the distance from the qds and the temperature .
our results are compared with experimental observations , considering lifetime limitations in qd memory structures as well as the electron emission in pn - diodes . .
And you have already written the first three sentences of the full article: the controversial discussions about the nature of the electron dynamics in quantum dots @xcite ( qds ) show that this topic is still not fully understood .
different electron - phonon coupling regimes leading to a multi - phonon process @xcite or a polaron decay @xcite have been proposed . especially for a multi - phonon process a so - called bottleneck effect @xcite is expected due to the discrete qd density of states . on the other hand it has been shown theoretically @xcite as well as experimentally @xcite that electron capture and relaxation by coulomb scattering ( auger effect ) with electrons in the wetting layer can be very efficient for large enough densities .
furthermore , an auger - type process can overcome the bottleneck due to the continuous energy dispersion in the wetting layer ..
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the depletion of the wetting layer density by an electric field @xcite has been shown to reduce the relaxation rates .
similarly , the electron density in the vicinity of the qds is reduced in a pn diode by the depletion layer within a dlts experiment @xcite .
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Suppose that you have an abstract for a scientific paper: various @xmath0-penalised estimation methods such as graphical lasso and clime are widely used for sparse precision matrix estimation .
many of these methods have been shown to be consistent under various quantitative assumptions about the underlying true covariance matrix .
intuitively , these conditions are related to situations where the penalty term will dominate the optimisation . in this paper
, we explore the consistency of @xmath0-based methods for a class of sparse latent variable -like models , which are strongly motivated by several types of applications .
we show that all @xmath0-based methods fail dramatically for models with nearly linear dependencies between the variables .
we also study the consistency on models derived from real gene expression data and note that the assumptions needed for consistency never hold even for modest sized gene networks and @xmath0-based methods also become unreliable in practice for larger networks . .
And you have already written the first three sentences of the full article: estimating the sparse precision matrix , i.e. the inverse covariance matrix , from data is a very widely used method for exploring the dependence structure of continuous variables .
the motivation for the approach stems from the fact that for a gaussian markov random field model , zeros in the precision matrix translate exactly to absent edges in the corresponding undirected gaussian graphical model , thus being informative about the marginal and conditional independence relationships among the variables .
the full @xmath1-dimensional covariance matrix contains @xmath2 parameters , making its accurate estimation from limited data difficult ..
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additionally , the structure learning requires the inverse of the covariance , and matrix inversion is in general a very fragile operation . to make the problem tractable
, some form of regularisation is typically needed .
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Suppose that you have an abstract for a scientific paper: we present new measurements of the time variability of intensity , doppler and non - thermal velocities in moss in an active region core observed by the euv imaging spectrometer on hinode in 2007 , june .
the measurements are derived from spectral profiles of the 195 line . using the 2@xmath0 slit
, we repeatedly scanned 150@xmath0 by 150@xmath0 in a few mins .
this is the first time it has been possible to make such velocity measurements in the moss , and the data presented are the highest cadence spatially resolved maps of moss doppler and non - thermal velocities ever obtained in the corona .
the observed active region produced numerous c- and m- class flares with several occurring in the core close to the moss .
the magnetic field was therefore clearly changing in the active region core , so we ought to be able to detect dynamic signatures in the moss if they exist . our measurements of moss intensities agree with previous studies in that a less than 15% variability is seen over a period of 16 hours .
our new measurements of doppler and non - thermal velocities reveal no strong flows or motions in the moss , nor any significant variability in these quantities .
the results confirm that moss at the bases of high temperature coronal loops is heated quasi - steadily .
they also show that quasi - steady heating can contribute significantly even in the core of a flare productive active region .
such heating may be impulsive at high frequency , but if so it does not give rise to large flows or motions . .
And you have already written the first three sentences of the full article: one of the most important unsolved problems in astrophysics is the question of how the solar corona is heated .
directly related to this problem is understanding the evolution of the emission in active regions , particularly in the core .
recent observations from _ hinode _ @xcite are providing a comprehensive view of active regions . they appear to be composed of at least two dominant loop populations : core loops that are seen evolving at multi - temperatures , and peripheral cool loops that develop downflows @xcite . the former appear to be rooted in unipolar magnetic concentrations @xcite ..
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the latter are seen extending to great heights and appear to be associated with coronal rain .
fan structures around the edges of active regions show strong outflows @xcite that may be significant sources of the slow solar wind ( @xcite ) . a key question is what is the time - scale of heating in the cores of active regions ?
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Suppose that you have an abstract for a scientific paper: we have used magneto - photoluminescence measurements to establish that inp / gaas quantum dots have a type - ii ( staggered ) band alignment . the average excitonic bohr radius and the binding energy
are estimated to be 15 nm and 1.5 mev respectively . when compared to bulk inp ,
the excitonic binding is weaker due to the repulsive ( type - ii ) potential at the hetero - interface .
the measurements are extended to over almost six orders of magnitude of laser excitation powers and to magnetic fields of up to 50 tesla .
it is shown that the excitation power can be used to tune the average hole occupancy of the quantum dots , and hence the strength of the electron - hole binding .
the diamagnetic shift coefficient is observed to drastically reduce as the quantum dot ensemble makes a gradual transition from a regime where the emission is from ( hydrogen - like ) two - particle excitonic states to a regime where the emission from ( helium - like ) four - particle biexcitonic states also become significant . .
And you have already written the first three sentences of the full article: until recently but for a few exceptions the study of quantum dot ( qd ) heterostructures with the staggered ( type - ii ) band alignment had been largely ignored because of the absence of confinement of one of the two types of carriers and their presumed poor radiative efficiency . however , it has come to be recognized that these structures are interesting , especially for their rich physics of excitons.@xcite in contrast to the usual type - i qds ( e.g. inas / gaas ) where the confinement energy scale is far greater than the energy of the coulomb interaction , the role of confinement in type - ii qds is largely limited to defining the geometry of the system .
this in itself has interesting consequences .
the multiply - connected topology can give rise to an oscillatory ground state energy for the magneto - excitons.@xcite secondly , type - ii qds also act as nanocapacitors@xcite which selectively accommodate only one type of particles ; but once charged they can bind the complementary particle to form an exciton . the strength of the coulomb interaction can be modified by screening or magnetic field.@xcite at higher excitation powers , they can be doubly - charged and form four - particle bound states ( biexcitons ) ..
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the biexcitons in a type - ii qd system are very unlike their counterparts@xcite in type - i qds and quantum wells .
they always have negative ` binding energy'.@xcite in the atomic physics language , while the usual biexciton is structurally analogous to a hydrogen molecule , the biexciton@xcite in type - ii qds is more like a helium atom.@xcite in this article we have probed the nature of the ensemble photoluminescence ( pl ) emission from a sample with inp qds in a gaas matrix . although the band offsets@xcite of _ bulk _ inp and gaas and some previous studies suggest that this material combination forms type - ii structures with electrons localized within the inp quantum dots and free holes in the gaas matrix , the energy gap of inp and gaas is within @xmath0mev of each other , and the conduction band offset is relatively small.@xcite thus alloying and anisotropic strain within the qds,@xcite can modify the energy gap and the relative offsets in way that is dependent on the details of the size and shape of the qds . for example , a comprehensive k.p calculation @xcite does not find a type - ii alignment in this system .
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Suppose that you have an abstract for a scientific paper: the ly@xmath0 absorption spectrum of the highest redshift quasars indicates that they are surrounded by giant regions , a few mpc in size .
the neutral gas around these regions should emit 21 cm radiation in excess of the cosmic microwave background , and enable future radio telescopes to measure the transverse extent of these regions . at early times , the regions expand with a relativistic speed .
consequently , their measured sizes along the line - of - sight ( via ly@xmath0 absorption ) and transverse to it ( via 21 cm emission ) should have different observed values due to relativistic time - delay .
we show that the combined measurement of these sizes would directly constrain the neutral fraction of the surrounding intergalactic medium ( igm ) as well as the quasar lifetime .
based on current number counts of luminous quasars at @xmath1 , an instrument like _ lofar _ should detect @xmath2 redshifted 21 cm shells per field ( with a radius of @xmath3 ) around active quasars as bright as those already discovered by sdss , and @xmath4 relic shells of inactive quasars per field .
we show that ly@xmath0 photons from the quasar are unable to heat the igm or to couple the spin and kinetic temperatures of atomic hydrogen beyond the edge of the region .
the detection of the igm in 21 cm emission around high redshift quasars would therefore gauge the presence of a cosmic ly@xmath0 background during the reionization epoch . .
And you have already written the first three sentences of the full article: the recent discovery of quasars at @xmath5 ( fan et al
. 2001 ; fan et al .
2003 ) and the subsequent observation of two gunn - peterson ( 1965 ) troughs ( djorgovski et al ..
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2003 ; white et al . 2003 ) established a new era in studies of the end of the reionization epoch .
the absorption of ly@xmath0 photons from these quasars probes the ionization state of the hydrogen in the intergalactic medium ( igm ) near the quasar redshift and has revealed giant ionized regions ( cen & haiman 2000 ; madau & rees 2000 ) .
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Suppose that you have an abstract for a scientific paper: quantum gases of atoms and exciton - polaritons are nowadays a well established theoretical and experimental tool for fundamental studies of quantum many - body physics and suggest promising applications to quantum computing . given their technological complexity
, it is of paramount interest to devise other systems where such quantum many - body physics can be investigated at a lesser technological expense .
here we examine a relatively well - known system of laser light propagating through thermo - optical defocusing media : based on a hydrodynamical description of light as a quantum fluid of interacting photons , we investigate such systems as a valid , room temperature alternative to atomic or exciton - polariton condensates for studies of many - body physics .
first , we show that by using a technique traditionally used in oceanography , it is possible to perform a direct measurement of the single - particle part of the dispersion relation of the elementary excitations on top of the photon fluid and to detect its global flow .
then , using a pump - and - probe set - up , we investigate the collective nature of low - wavevector sound modes of the fluid and observe signatures of superfluid behaviour . .
And you have already written the first three sentences of the full article: quantum gases , i.e. systems in which the thermal de broglie wavelength is larger than the average particle distance are an ever increasingly important area of theoretical and experimental study with applications as diverse as quantum computing and quantum simulation of general relativity models .
the most important example of such physics is the bose - einstein condensate where a macroscopic number of bosonic particles at low temperature share the same wavefunction .
after early work on liquid helium , the physics of condensates has been experimentally studied in ultracold atomic gases and , more recently , in exciton - polariton fluids in semiconductor microcavities ..
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building on these latter studies , an ever growing community is now active on the study of the so - called quantum fluids of light , where the many - photons forming the beam are seen as a gas of interacting particles via the optical nonlinearity of the medium @xcite . among the many hydrodynamic effects that are presently being studied in such fluids of light , we can mention turbulence @xcite , where the general physical processes found in a fluid or superfluid can be found in many other systems such as plasmas or in astrophysical systems .
another intriguing direction is so called `` analogue gravity '' where flowing fluids are used to model gravitational spacetime geometries @xcite .
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Suppose that you have an abstract for a scientific paper: we consider the gaussian free field on @xmath0 , @xmath1 , and prove that the critical density for percolation of its level sets behaves like @xmath2 as @xmath3 tends to infinity .
our proof gives the principal asymptotic behavior of the corresponding critical level @xmath4 .
moreover , it shows that a related parameter @xmath5 introduced by rodriguez and sznitman in @xcite is in fact asymptotically equivalent to @xmath4 .
alexander drewitz and pierre - franois rodriguez .
And you have already written the first three sentences of the full article: when studying the statistical mechanics of random interfaces which typically arise between coexisting phases of a ( @xmath6-dimensional ) physical system in equilibrium , one often considers so - called _ effective _ models , which aim at describing the @xmath3-dimensional surface _ itself _ , free from its surroundings .
arguably the most notorious example in this class is the massless harmonic crystal , or gaussian free field ( precise definitions will follow , see below ) .
a natural approach in trying to gain some insight into the geometry of this field is to inquire about its level sets , say , above a given height @xmath7 . in case.
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the underlying space is the cubic lattice @xmath0 , with @xmath1 , and due to the presence of strong correlations ( the susceptibility is infinite ) , this gives rise to an interesting percolation model , which was originally introduced by lebowitz and saleur in @xcite , and has since then been investigated in @xcite , @xcite , @xcite , @xcite , @xcite and @xcite , see also @xcite , @xcite for related results .
only recently has it been shown in @xcite that the associated phase transition is non - trivial in _ all _ dimensions @xmath1 ( partial results were already obtained in @xcite and @xcite ) .
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Suppose that you have an abstract for a scientific paper: we have performed fully 3-d simulations of the collapse of molecular cloud cores which obey the logatropic equation of state . by following the collapse of these cores from states of near hydrodynamic equilibrium
, we are able to produce accretion histories which closely resemble those of observed cores .
the accretion proceeds in four distinct stages : an initial period of very slow accretion ; a period of vigorous accretion following the development of a central density singularity , with @xmath0 , as predicted by self - similar models ; a period of relatively stable , vigorous accretion ; and finally a gradual decrease in the accretion rate once about 50% of the available mass of the molecular cloud core has been accreted .
these results may explain the accretion histories of cores as they pass through the pre - protostellar , class 0 , and class i stages . .
And you have already written the first three sentences of the full article: mounting evidence indicates that massive molecular cloud cores possess properties which are not adequately explained by models employing an isothermal equation of state . for example , surveys of prestellar cores in a variety of star - forming complexes show that intermediate and high mass cores have nonthermal line widths which are significantly greater than their thermal line widths ( @xcite ) .
models of the collapse of isothermal molecular cloud cores exhibit a number of features which are not borne out by observations , such as a time - invariant rate of accretion onto the central object ( @xcite ) and highly supersonic infall ( @xcite ) . to address some of the shortcomings of isothermal models
, @xcite advanced a model for molecular cloud core collapse which accounts for some degree of turbulent support via a phenomenological equation of state ..
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this logatropic equation of state reads + @xmath1 where the subscript `` c '' denotes `` central '' values .
the constant @xmath2 is an adjustable parameter whose value for a range of molecular cloud core masses was determined empirically by @xcite to be @xmath3 .
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Suppose that you have an abstract for a scientific paper: we report on our analysis of a 300 ks observation of the vela pulsar with the rossi x - ray timing explorer ( rxte ) .
the double - peaked , pulsed emission at 2 - 30 kev , which we had previously detected during a 93 ks observation , is confirmed with much improved statistics .
there is now clear evidence , both in the spectrum and the light curve , that the emission in the rxte band is a blend of two separate components .
the spectrum of the harder component connects smoothly with the osse , comptel and egret spectrum and the peaks in the light curve are in phase coincidence with those of the high - energy light curve .
the spectrum of the softer component is consistent with an extrapolation to the pulsed optical flux , and the second rxte pulse is in phase coincidence with the second optical peak .
in addition , we see a peak in the 2 - 8 kev rxte pulse profile at the radio phase . # 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: the vela pulsar ( psr b0833 - 45 ) is the strongest @xmath0-ray source in the sky , but it is one of the most difficult pulsars to detect at x - ray energies .
this is in part because it is embedded in a very bright x - ray synchrotron nebula providing a large unpulsed background , but also because its pulsed x - ray emission is comparatively weak .
the first detection of pulsed emission at x - ray energies was made by rosat in the 0.1 - 2 kev band ( ogelman 1993 ) , and the spectrum is consistent with a blackbody ..
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we detected the pulsar for the first time in hard x - rays ( 2 - 30 kev ) during a 93 ks rxte cycle 1 observation ( strickman , harding & de jager 1999 [ shd99 ] ) and the pulse profile shows two peaks .
the first rxte peak is closely aligned with the first egret @xmath0-ray peak , but the second peak has an energy - dependent phase and is aligned with the second egret peak only at the highest energy ( 16 - 30 kev ) . in our lowest energy rxte band
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Suppose that you have an abstract for a scientific paper: we apply the lindstedt method to the one dimensional fermi - pasta - ulam @xmath0 lattice to find fully general solutions to the complete set of equations of motion .
the pertubative scheme employed uses @xmath1 as the expansion parameter , where @xmath1 is the coefficient of the quartic coupling between nearest neighbors . we compare our non - secular perturbative solutions to numerical solutions and find striking agreement . .
And you have already written the first three sentences of the full article: no known solution for a coupled set of duffing oscillators exists , with the exception of specific cases .
the duffing lattice is perhaps more well known as the fpu @xmath0-system , one of the systems studied by fermi , pasta , and ulam in the @xmath2 @xcite to numerically investigate the approach to thermal equilibrium in nonlinear systems .
fpu found that the expected equipartition of energy among the linear normal modes did not occur , and that periodic , non - ergodic motion persisted even in the presence of the nonlinear mixing terms ..
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subsequent investigations , both numerical and analytic , have shown that different parameter regions specified by the total energy and the strength of the nonlinear terms as specified by the parameter @xmath1 lead to markedly different types of behaviour @xcite , with the expected ergodicity emerging with increasing energy and @xmath1 .
but the observation of the periodic motion in the orginal fpu @xmath0-system computer experiments lends credence to the possibility of finding acceptable pertubative solutions in certain parameter regions . that no exact solution exsists for a large @xmath3 - body lattice modulo some exceptional cases @xcite motivates us to develop pertubative solutions to systems of duffing oscillators .
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Suppose that you have an abstract for a scientific paper: dynamics of thin films of poly(vinyl acetate ) ( pvac ) and poly(methyl methacrylate ) ( pmma ) have been investigated by dielectric relaxation spectroscopy in the frequency range from 0.1hz to 1mhz at temperatures from 263k to 423k .
the @xmath0-process , the key process of glass transition , is observed for thin films of pvac and pmma as a dielectric loss peak at a temperature @xmath1 in temperature domain with a fixed frequency . for pmma
the @xmath2-process is also observed at a temperature @xmath3 . for pvac , @xmath1 decreases gradually with decreasing thickness , and the thickness dependence of @xmath1 is almost independent of the molecular weight ( @xmath42.4@xmath510@xmath6 ) . for pmma
, @xmath1 remains almost constant as thickness decreases down to a critical thickness @xmath7 , at which point it begins to decrease with decreasing thickness .
contrastingly , @xmath3 decreases gradually as thickness decreases to @xmath7 , and below @xmath7 it decreases drastically . for both pvac and pmma ,
the broadening of the distribution of the relaxation times in thinner films is observed and this broadening is more pronounced for the @xmath0-process than for the @xmath2-process .
it is also observed that the relaxation strength is depressed as the thickness decreases for both the polymers . 2 .
And you have already written the first three sentences of the full article: recent progress in theoretical and experimental studies has clarified many properties of glass transitions @xcite .
however , the mechanism of the glass transition has not yet been fully understood @xcite .
the major issue is the experimental approach to the investigation of the length scale of the glass transition and dynamics of the @xmath0-process such as dynamical heterogeneity @xcite . according to the adam and gibbs theory ,.
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the dynamics of glass transitions are associated with cooperative motions which are characterized by a so - called _ cooperatively rearranging region _ ( crr ) , in which molecules move cooperatively with each other @xcite .
the size of the crr is assumed to increase as temperature decreases to the glass transition temperature @xmath8 .
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11,366 |
Suppose that you have an abstract for a scientific paper: few high - redshift , radio - loud quasars are known to date .
the extremely luminous , radio - bright quasar , sdss [email protected] was recently discovered at a redshift of @xmath1 .
we observed the source with high resolution very long baseline interferometry ( vlbi ) at 1.7ghz with the european vlbi network ( evn ) and found a single compact radio component .
we estimated a lower limit to the brightness temperature of the detected radio component , @xmath2k .
additionaly , when compared to archival radio data , the source showed significant flux density variation .
these two findings are indicative of the blazar nature of the source .
[ firstpage ] techniques : interferometric galaxies : active quasars : individual : sdss [email protected] galaxies : high - redshift .
And you have already written the first three sentences of the full article: high - redshift ( @xmath3 ) quasars are of major importance since they can provide information on the growth of the supermassive black holes and the evolution of active galactic nuclei ( agn ) in the early universe .
the mere existence of black holes with a few million solar masses ( or more ) at @xmath4 constrains the black hole growth and the accretion process ( e.g. * ? ? ?
* and references therein ) . among the high - redshift quasars ,.
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the radio - loud ones constitute a very attractive subsample , since their radio jets can be studied with the highest angular resolution , via very long baseline interferometry ( vlbi ) technique .
typically , radio - loud agn contain a flat - spectrum core and a steep - spectrum jet .
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Suppose that you have an abstract for a scientific paper: we generalize our analytic approach ( berent m and parzyski r 2009 _ phys .
rev . _ a * 80 * 033834 ) to include the effect of strong depopulation of the initial state when considering the multiphoton population transfer and scattering of low - frequency light by a 3-level system in the lambda - type configuration .
we discuss the quality of the approximations made , i.e. , the adiabatic and generalized rotating - wave approximations . .
And you have already written the first three sentences of the full article: in an analytic approach @xcite , we have recently described the spectrum of light scattered by a three - level lambda - type system under two conditions .
one condition was that the incident - light frequency was much lower than the separation frequencies between the states situated in the ends of the arms of lambda configuration ( figure [ fig : lambda ] ) .
thus , the transitions in the arms had multiphoton character ..
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the other condition was that of weak depopulation of the initial state placed at the bottom of one arm ( the black dot in figure [ fig : lambda ] ) .
as long as the latter condition was fulfilled , our analytic approach succeeded in explaining all details of the spectra found by numerical integration of the schrdinger equation ( number of peaks , their internal structures , positions , relative heights and sensitivity to the light - pulse shape and strength ) .
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Suppose that you have an abstract for a scientific paper: the implementation of the kinetic diffuse boundary condition with the characteristic streaming - collision mechanism is studied for the high - order lattice boltzmann ( lb ) models .
the obtained formulation is also tested and validated numerically for three high - order lb models for both isothermal and thermal couette flows .
the streaming - collision mechanism ensures that high - order lb models can retain particle feature while go beyond the navier - stokes hydrodynamics . .
And you have already written the first three sentences of the full article: high - order models have recently attracted considerable interests in the lattice boltzmann ( lb ) community . for these models ,
high - order terms in the expanded distribution function are retained , thus multi - speed lattices have to be used . by doing so , we have a few benefits , e.g. consistent description of thermal flows , the galilean invariance of the transport coefficients , improved model capability for compressible and rarefied flows@xcite .
meanwhile , high - order models can still preserve the simplicity of the standard lb model ..
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high - order lb models are tererfore often applied to thermal flows , compressible flows , and rarefied flows @xcite . due to their kinetic origin ,
high - order lb models have shown to be able to approach the boltzmann model equation such as the bhatnagar - gross - krook ( bgk ) equation by increasing the expansion and quadrature order@xcite .
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Suppose that you have an abstract for a scientific paper: we report the discovery of a system of unusual filaments which appear to be associated with molecular clouds in the perseus spiral arm of our galaxy .
we investigate the hypothesis that this system is the result of a directed flow of dissociated gas from clouds trapped within an extended wind flow from massive stars .
the wolf - rayet star wr 5 and the oib(f ) star hd 17603 are identified as candidate driving sources .
however , an examination of this hypothesis within the context of the theory of mass - loaded winds shows that these two stars alone can not account for the energetics and kinematics of the required spherically symmetric wind flow . unless the apparent association between , molecular gas , and stars is an accidental one
, we suggest that other as - yet unidentified stars must have contributed to driving the filaments . .
And you have already written the first three sentences of the full article: massive o - type stars , including the progenitors of wolf - rayet stars , inject enormous quantities of energy into the interstellar medium ( ism ) in the form of dissociating and ionizing radiation and winds .
the radiation fields create circumstellar / interstellar and regions into which winds blow , creating large - scale swept - up expanding shells of gas known as stellar wind bubbles @xcite .
there are numerous analytical and numerical studies of the formation , structure , and evolution of stellar wind bubbles ( swbs ) , but there are few convincing observations of bubbles around wolf - rayet stars and massive o - stars ..
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the viith catalogue of galactic wolf - rayet stars indicates that only @xmath0 are associated with bubbles @xcite .
surveys are incomplete , but many of these proposed bubbles are not securely established . the interstellar environment of massive stars is observed to be extremely complex and is likely to be the combined result of inhomogeneous initial conditions and the influence of the stars .
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Suppose that you have an abstract for a scientific paper: we present three - dimensional simulations of the dynamical bar - mode instability in magnetized and differentially rotating stars in full general relativity .
our focus is on the effects that magnetic fields have on the dynamics and the onset of the instability . in particular , we perform ideal - magnetohydrodynamics simulations of neutron stars that are known to be either stable or unstable against the purely hydrodynamical instability , but to which a poloidal magnetic field in the range of @xmath0@xmath1 g is superimposed initially . as expected , the differential rotation is responsible for the shearing of the poloidal field and the consequent linear growth in time of the toroidal magnetic field .
the latter rapidly exceeds in strength the original poloidal one , leading to a magnetic - field amplification in the the stars .
weak initial magnetic fields , i.e. , @xmath2 g , have negligible effects on the development of the dynamical bar - mode instability , simply braking the stellar configuration via magnetic - field shearing , and over a timescale for which we derived a simple algebraic expression . on the other hand , strong magnetic fields , i.e. , @xmath3 g , can suppress the instability completely , with the precise threshold being dependent also on the amount of rotation . as a result ,
it is unlikely that very highly magnetized neutron stars can be considered as sources of gravitational waves via the dynamical bar - mode instability . .
And you have already written the first three sentences of the full article: main - sequence stars with masses greater than about @xmath4 follow two evolutionary paths ; either they form a degenerate core of o / ne / mg , or a degenerate fe core , which , after undergoing a type ii supernova core collapse , forms a proto - neutron star @xcite .
neutron stars ( nss ) are also expected to form through the accretion - induced collapse of a white dwarf @xcite . at birth
, nss are rapidly and differentially rotating , which makes them subject to various types of instabilities . among these ,.
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the dynamical bar - mode instability and the shear - instability are particularly interesting because of their potential role as sources of gravitational waves ( gws ) . indeed
, a newly born ns may develop a dynamical bar - mode instability when the rotation parameter @xmath5 , with @xmath6 the rotational kinetic energy and @xmath7 the gravitational binding energy , exceeds a critical value @xmath8 ( see , for instance , @xcite for some reviews ) . under these conditions ,
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Suppose that you have an abstract for a scientific paper: we explore the evolution of thermonuclear supernova explosions when the progenitor white dwarf star ignites asymmetrically off - center .
several numerical simulations are carried out in two and three dimensions to test the consequences of different initial flame configurations such as spherical bubbles displaced from the center , more complex deformed configurations , and teardrop - shaped ignitions .
the burning bubbles float towards the surface while releasing energy due to the nuclear reactions .
if the energy release is too small to gravitationally unbind the star , the ash sweeps around it , once the burning bubble approaches the surface .
collisions in the fuel on the opposite side increase its temperature and density and may in some cases initiate a detonation wave which will then propagate inward burning the core of the star and leading to a strong explosion .
however , for initial setups in two dimensions that seem realistic from pre - ignition evolution , as well as for all three - dimensional simulations the collimation of the surface material is found to be too weak to trigger a detonation . .
And you have already written the first three sentences of the full article: type ia supernovae are generally associated with the thermonuclear explosion of earth - sized white dwarf ( wd ) stars the final stages of the evolution of small and intermediate - mass stars .
these dense objects consist of carbon and oxygen and their pressure is dominated by degenerate electrons . in a binary system , the wd can gain mass from its companion by accretion .
however , there exists a fundamental limit , the chandrasekhar mass , beyond which the star is unstable against gravitational collapse . before reaching this stage , the density at the center of the wd reaches values at which nuclear reactions from carbon to heavier elements.
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this establishes a stage of convective carbon burning which is finally terminated when a thermonuclear runaway forms a flame .
the thermonuclear flame propagates outward and may give rise to an explosion of the star @xcite .
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Suppose that you have an abstract for a scientific paper: we obtain phase diagrams of regular and irregular finite connectivity spin - glasses .
contact is firstly established between properties of the phase diagram and the performances of low density parity check codes ( ldpc ) within the replica symmetric ( rs ) anstz .
we then study the location of the dynamical and critical transition of these systems within the one step replica symmetry breaking theory ( rsb ) , extending similar calculations that have been performed in the past for the bethe spin - glass problem .
we observe that , away from the nishimori line , in the low temperature region , the location of the dynamical transition line @xmath0 change within the rsb theory , in comparison with the ( rs ) case . for ldpc decoding over the binary erasure channel we find , at zero temperature and rate @xmath1 an rs critical transition point located at @xmath2
while the critical rsb transition point is located at @xmath3 , to be compared with the corresponding shannon bound @xmath4 . for the binary symmetric channel ( bsc )
we show that the low temperature reentrant behavior of the dynamical transition line , observed within the rs anstz , changes within the rsb theory ; the location of the dynamical transition point occurring at higher values of the channel noise .
possible practical implications to improve the performances of the state - of - the - art error correcting codes are discussed .
+ pacs numbers : 89.90+n , 89.70+c,05.50+q + .
And you have already written the first three sentences of the full article: the survival of ferromagnetic ordering under the disruption of frozen random fields @xcite and the onset of spin - glass ( sg ) order in systems characterized by random competing interactions @xcite are two central problems in the statistical mechanics of systems with quenched randomness . when properly rephrased , these two problems turn out to relate to core problems in other , quite different disciplines .
insight into these two closely related problems in any given system is obtained from the corresponding phase diagram as a function of the physical parameters , such as temperature and disorder strength .
finite - connectivity mean - field sg models @xcite and their _.
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p_-spin counterpart @xcite are important for two distinct reasons .
firstly , despite being mean - field in nature , they are believed to share common properties with finite - dimensional spin - glass systems @xcite .
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Suppose that you have an abstract for a scientific paper: a hydrodynamic formulation of the evolution of large - scale structure in the universe is presented .
it relies on the spatially coarse - grained description of the dynamical evolution of a many - body gravitating system .
because of the assumed irrelevance of short - range ( `` collisional '' ) interactions , the way to tackle the hydrodynamic equations is essentially different from the usual case .
the main assumption is that the influence of the small scales over the large - scale evolution is weak : this idea is implemented in the form of a _ large - scale expansion _ for the coarse - grained equations .
this expansion builds a framework in which to _ derive _ in a controlled manner the popular `` dust '' model ( as the lowest - order term ) and the `` adhesion '' model ( as the first - order correction ) .
it provides a clear physical interpretation of the assumptions involved in these models and also the possibility to improve over them .
phys .
rev .
d ; submitted : may 18 , 2000 ; accepted : july 18 , 2000 .
And you have already written the first three sentences of the full article: the standard model to understand the large - scale features of the matter distribution in the universe after decoupling from radiation can be hardly simpler : a collection of many identical point particles interacting with each other via the newtonian gravitational force in an expanding spatial background @xcite .
structure arises as a consequence of the gravitational instability of initially tiny density perturbations .
this model neglects relativistic effects , which become important only at scales of the order of the horizon and beyond , or when dealing with relativistic velocities ..
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the model also excludes nongravitational interactions , which are assumed to be relevant only at small enough scales .
the general solution to the dynamical evolution of this model is unknown due to the mathematical difficulties .
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Suppose that you have an abstract for a scientific paper: we are undertaking an extensive x - ray monitoring campaign of the two crab - like pulsars in the large magellanic clouds , psr b0540 - 69 and psr j0537 - 6910 .
we present our current phase - connected timing analysis derived from a set of 50 pointed x - ray observations spanning several years . from our initial 1.2 yr monitoring program of the young 50 ms pulsar psr b0540 - 69 , we find the first compelling evidence for a glitch in its rotation .
this glitch is characterized by @xmath0 and @xmath1 .
taking into account the glitch event , we derive a braking index of @xmath2 , significantly lower than previous reported .
for the 16 ms pulsar , psr j0537 - 6910 , we recorded 6 large glitch events during a period of nearly 3 years , the highest rate of all known crab - like systems . despite the extreme timing activity
, the long term spin - down of this pulsar continues to average @xmath3 hz / s
. 73 # 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: a characteristic signature of young rotation - powered pulsars is the phenomena of `` glitches '' , sudden discontinuous changes in their spin periods ( e.g. , see lyne & graham - smith 1998 ) .
the physical causes of these glitches are not understood .
suggestions include sudden changes in the neutron star ( ns ) crust configuration ( `` starquakes '' ) , abrupt reconfiguration of the magnetic field , or perhaps to the sudden unpinning of vortices in the superfluid neutrons in the inner part of the ns crust . for the latter , the amplitude of the glitch provides an estimate of the fractional part of the moment of inertia carried by superfluid neutrons ( lyne et al ..
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1996 ) .
the largest glitches have relative amplitudes ( @xmath4 ) of several parts per million , but the range of amplitudes covers many orders of magnitude . often there is a partial recovery back toward the pre - glitch rotation rate on a time scale of @xmath5 days , however , the spin - down rate may be permanently altered .
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11,375 |
Suppose that you have an abstract for a scientific paper: the sine - gordon equation is a nonlinear partial differential equation .
it is known that the sine - gordon has soliton solutions in the 1d and 2d cases , but such solutions are not known to exist in the 3d case .
several numerical solutions to the 1d , 2d , and 3d sine - gordon equation are presented and comments are given on the nature of the solutions . .
And you have already written the first three sentences of the full article: many problems in science and engineering can be expressed as a partial differential equation ( pde ) .
finding accurate numerical solutions is often important for these applications , but there are many challenges associated with computing these solutions .
nonlinear pdes can cause numerical methods to destabilize@xcite . finding accurate solutions can require high resolution , large amounts of memory , small time - steps , and a lot of computation time ..
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numerical methods that compute solutions for pdes must approximate derivatives .
one way to achieve this is with a finite difference ; one of the simplest such methods is the forward difference given by @xmath0 ( * ? ? ?
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11,376 |
Suppose that you have an abstract for a scientific paper: we study quantum quenches in the two - dimensional kitaev toric code model and compute exactly the time - dependent entanglement entropy of the non - equilibrium wave - function evolving from a paramagnetic initial state with the toric code hamiltonian .
we find that the area law survives at all times . adding disorder to the toric code couplings
makes the entanglement entropy per unit boundary length saturate to disorder - independent values at long times and in the thermodynamic limit .
there are order - one corrections to the area law from the corners in the subsystem boundary but the topological entropy remains zero at all times .
we argue that breaking the integrability with a small magnetic field could change the area law to a volume scaling as expected of thermalized states but is not sufficient for forming topological entanglement due to the presence of an excess energy and a finite density of defects . .
And you have already written the first three sentences of the full article: cold atomic systems have provided an ideal playground for the experimental studies of the unitary evolution of thermally isolated quantum systems .
@xcite apart from the experimental interest , studies of quantum evolution have shed light on some fundamental questions such as thermalization .
@xcite a widely - studied scenario is the unitary evolution of a quantum state when the hamiltonian is suddenly changed a `` quantum quench '' , @xcite which has been the subject of many recent studies ( see refs ..
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[ ] for a few examples ) . a challenging question , which has been addressed theoretically in one dimensional systems , is the evolution of the entanglement entropy following the quench .
@xcite more generally , such studies are concerned with the fate of an out - of - equilibrium quantum state with a hamiltonian that changes with some time - dependent protocol .
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Suppose that you have an abstract for a scientific paper: in open quantum systems , entanglement can vanish faster than coherence .
this phenomenon is usually called sudden death of entanglement . in this paper sudden death of entanglement
is discussed from a geometrical point of view , in the context of two qubits .
a classification of possible scenarios is presented , with important known examples classified .
sugestions of theoretical and experimental examples are given as well as large dimensional and multipartite versions of the effect are briefly discussed . .
And you have already written the first three sentences of the full article: coherence is a central theme in quantum physics . in feynman s
words on quantum theory @xcite , it is _ the only mystery_. a good definition of coherence depends on two things @xcite : the state of the system , @xmath0 , and the alternatives under consideration , usually attached to different eigenvalues of an observable @xmath1 . whenever @xmath0 is written in a basis ,
the non - diagonal elements of @xmath0 are called _ coherences _ ( with respect to that basis ) since they can originate the oscillating patterns which characterize interference ..
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curiously , measurements of @xmath1 can not show the effects of such coherences .
the mean value of @xmath1 is simply the wheighted sum of its proper values .
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Suppose that you have an abstract for a scientific paper: we describe a general procedure for using number counts of any object to constrain the probability distribution of the primordial fluctuations , allowing for generic weak non - gaussianity .
we apply this procedure to use limits on the abundance of primordial black holes and dark matter ultracompact minihalos ( ucmhs ) to characterize the allowed statistics of primordial fluctuations on very small scales .
we present constraints on the power spectrum and the amplitude of the skewness for two different families of non - gaussian distributions , distinguished by the relative importance of higher moments .
although primordial black holes probe the smallest scales , ultracompact minihalos provide significantly stronger constraints on the power spectrum and so are more likely to eventually provide small - scale constraints on non - gaussianity . .
And you have already written the first three sentences of the full article: the power spectrum of primordial fluctuations is well measured on cosmological scales using the cosmic microwave background ( cmb ) and large scale structure @xcite .
these observations provide compelling evidence that the fluctuations originated in an era of inflation .
however , there is a great deal of new information waiting to be accessed in small - scale fluctuations and in higher - order statistics ( non - gaussianity ) . in this paper.
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we explore both new regimes by examining how object number counts constrain the probability distribution of primordial fluctuations . by looking at very small objects ( primordial black holes and ultracompact minihalos ) ,
we constrain the power in fluctuations on smaller scales than the cmb and large scale structure currently probe , @xmath0 mpc@xmath1 .
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Suppose that you have an abstract for a scientific paper: we show that by switching on a spin - orbit interaction in a cold - atom system , experiencing a zeeman - like coupling to an external field , e.g. , in a bose - einstein condensate , one can simulate a quantum measurement on a precessing spin . depending on the realization ,
the measurement can access both the ergodic and the zeno regimes , while the time dependence of the spin s decoherence may vary from a gaussian to an inverse fractional power law .
back action of the measurement forms time- and coordinate - dependent profiles of the atoms density , resulting in its translation , spin - dependent fragmentation , and appearance of interference patterns . u .
And you have already written the first three sentences of the full article: recent advances in producing synthetic spin - orbit coupling fields in cold atoms , both bosonic @xcite and fermionic , @xcite opened a new field of research in cold matter physics reviewed in refs .
spin - orbit coupling of the rashba and dresselhaus forms , as well as effective magnetic fields leading to the zeeman - like splitting for the corresponding pseudospin , can be designed there by optical means . in these systems
the pseudospin is formed by coupling hyperfine atomic levels with highly coherent resonant laser radiation . since this.
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coupling strongly depends on the detuning of the laser frequency from the resonance , the movement of an atom also modifies its interaction with light via the doppler shift linear in the atom velocity .
this effect is seen as the effective spin - orbit coupling .
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11,380 |
Suppose that you have an abstract for a scientific paper: spherical dust collapse generally forms a shell focusing naked singularity at the symmetric center .
this naked singularity is massless . further the newtonian gravitational potential and speed of the dust fluid elements are everywhere much smaller than unity until the central shell focusing naked singularity formation if an appropriate initial condition is set up .
although such a situation is highly relativistic , the analysis by the newtonian approximation scheme is available even in the vicinity of the space - time singularity .
this remarkable feature makes the analysis of such singularity formation very easy .
we investigate non - spherical even - parity matter perturbations in this scheme by complementary using numerical and semi - analytical approaches , and estimate linear gravitational waves generated in the neighborhood of the naked singularity by the quadrupole formula .
the result shows good agreement with the relativistic perturbation analysis recently performed by iguchi et al .
the energy flux of the gravitational waves is finite but the space - time curvature carried by them diverges . 0.5 cm pacs number(s ) : 04.25.nx,04.30.db,04.20.dw @ @.2326ex # 1^to-1.4@-@@ ken - ichi nakao@xmath0 , hideo iguchi@xmath1 and tomohiro harada@xmath2 + _ @xmath0department of physics , osaka city university _
+ _ osaka 558 - 8585 , japan _
+ _ @xmath1department of earth and space science , graduate school of science , osaka university
_ + _ toyonaka , osaka 560 - 0043 , japan _ + _ @xmath2department of physics , waseda university _
+ _ oh - kubo , shinjuku - ku , tokyo 169 - 8555 , japan _ + .
And you have already written the first three sentences of the full article: general relativity predicts that gravitational collapse of massive objects leads to space - time singularities in rather general circumstances in our universe@xcite and such singularities might be accompanied with the blow up of physical quantities ( energy density , pressure and curvature of space - time , etc ) . the known physical laws including general relativity itself will break down in the neighborhood of the space - time singularity and hence the quantum theory of gravity is believed to be necessary to describe the physical phenomena in such a region .
one of the important issues is whether the space - time singularities formed in our universe are visible or not for the observer ( us ) far from the region where the gravitational collapse occurs .
the cosmic censorship conjecture proposed by penrose gave a strong motivation to investigate this problem@xcite ..
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roughly speaking , this conjecture states that the singularity is not visible for any observer if it is resulted from physically reasonable initial conditions .
however , this conjecture has not yet been proven .
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Suppose that you have an abstract for a scientific paper: the independent predictions of edge ferromagnetism and the quantum spin hall phase in graphene have inspired the quest of other two dimensional honeycomb systems , such as silicene , germanene , stanene , iridiates , and organometallic lattices , as well as artificial superlattices , all of them with electronic properties analogous to those of graphene , but much larger spin - orbit coupling .
here we study the interplay of ferromagnetic order and spin - orbit interactions at the zigzag edges of these graphene - like systems .
we find an in - plane magnetic anisotropy that opens a gap in the otherwise conducting edge channels , that should result in large changes of electronic properties upon rotation of the magnetization .
magnetic anisotropy , a technologically crucial property , is driven by spin - orbit interaction , which is normally the underdog in the competition with the other two terms that control ferromagnetism , namely , kinetic and coulomb energy@xcite . as a result ,
magnetic anisotropy energy in conventional ferromagnets is at least 2 orders of magnitude smaller than the curie temperature and the fermi energies ( or the band - gap , in the case of insulators ) . for the same reason ,
transport properties in ferromagnetic metals are only weakly dependent on the magnetic orientation , and typical values for the anisotropic magnetoresistance ( amr ) are below 3 percent@xcite . here
we study magnetic anisotropy in a class of systems for which the balance between these three energy scales is very different from the usual , which leads to two dramatic consequences , very different from conventional ferromagnetism .
first , the conducting properties change from metal to insulator , depending on the magnetization orientation , an effect that , to the best of our knowledge , has never been reported .
second , the magnetic moment magnitude depends strongly on the magnetic orientation , and it can change even vanish in some directions , a phenomenon dubbed colossal magnetic....
And you have already written the first three sentences of the full article: upon a rotation of angle @xmath12 of the spin quantization axis in the @xmath66 plane , the rotated of up and down density operators take the following form in the basis of the z - axis eigenstates .
@xmath67 @xmath68 thus , these are the local mean field operators in a collineal calculation only allowing the development of magnetism along this particular quantization axis .
this choice of mean field operators restrics the avaible hilbert space to the collinear solutions , whereas the inclusion of the exchange term will lead to the full non - collinear solutions ..
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even though the anisosotrpy calculations were performed on a zigzag edge , localized edge states also appear on chiral nanoribbons @xcite .
thus , this anisotropy effect will appear as well in chiral ( n , m ) nanoribbons due to the local lattice imbalance . as a particular example
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Suppose that you have an abstract for a scientific paper: recently , for spin @xmath0 impurities quite different size dependence of the kondo contribution to the resistivity was found experimentally than for @xmath1 . therefore previous calculation about the effect of the spin - orbit - induced magnetic anisotropy on the kondo amplitude of the resistivity
is extended to the case of @xmath0 impurity spin which differs from the integer spin case as the ground state is degenerated . in this case
the kondo contribution remains finite when the sample size goes to zero and the thickness dependence in the kondo resistivity is much weaker for cu(mn ) .
the behavior of the kondo coefficient as a function of the thickness depends on the kondo temperature , that is somewhat stronger for larger @xmath2 . comparing our results with a recent experiment in thin cu(mn ) films , we find a good agreement . .
And you have already written the first three sentences of the full article: the kondo effect @xcite in samples with reduced dimensions ( thin films , narrow wires ) is one of the most challenging problems in the field .
most of the experiments @xcite have shown that the kondo contribution to the resistivity is suppressed when the sample size is reduced or the disorder in the sample is increased .
in addition the different thermopowers of samples with different thickness gave further evidences for the existence of size dependence @xcite ..
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the previously examined samples were au(fe ) , cu(fe ) , and cu(cr ) alloys , i.e. , alloys with integer spin impurities .
surprisingly , however , very weak size dependence has been found recently in cu(mn ) alloys @xcite . the first possible explanation related to the size of the kondo screening cloud @xcite
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11,383 |
Suppose that you have an abstract for a scientific paper: we present an exact mathematical description of josephson vortices and of the meissner effect in periodic thin - layer superconductor / insulator structures with an arbitrary number of identical junctions @xmath0
( @xmath1 , where @xmath2 is the number of superconducting layers ) in terms of localized solutions to a system of differential equations for phase differences . we establish a general criterion of the existence of localized solutions .
we show that meissner solutions are characterized by several josephson lengths @xmath3 ( @xmath4 lengths for even @xmath2 , and @xmath5 lengths for odd @xmath2 ) .
we derive an exact expression for the superheating field of the meissner state , @xmath6 , as an explicit function of @xmath7 . for josephson vortices , we find two basically different types of topological solutions : vortex - plane solutions and incoherent vortex solutions .
thermodynamically stable vortex - plane
solutions represent a chain of @xmath0 vortices ( one vortex per each insulating layer ) .
they are characterized by the same set of @xmath8@xmath9 as the meissner solutions .
we obtain exact analytical expressions for their self - energy and for the lower critical field @xmath10 .
incoherent vortex solutions comprise solutions with @xmath11 vortices and different vortex - antivortex configurations .
in contrast to the vortex - plane solutions , they prove to be thermodynamically unstable , and their spatial dependence is characterized , in general , by @xmath0 length scales . as an illustration , we analyze 1 - 4-josephson - junction stacks and investigate a transition to the layered superconductor limit ( @xmath12 ) . .
And you have already written the first three sentences of the full article: we present a rigorous mathematical examination of the problem of josephson vortices and of the meissner effect in thin - layer josephson - junction stacks and layered superconductors , with a static external magnetic field @xmath13 applied parallel to the layers ( along the @xmath14 axis , see fig . 1 . )
we consider periodic systems composed of an arbitrary number @xmath0 of identical superconductor / insulator ( s / i ) junctions ( @xmath15 , where @xmath2 is the number of s - layers , with @xmath16 being the layering axis ) .
our starting point is the microscopic gibbs free - energy functional derived in ref . ..
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mathematical structure of this functional is analogous to that of the phenomenological lawrence - doniach model .
@xcite thus , the treatment of our paper fully applies to the latter model as well .
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Suppose that you have an abstract for a scientific paper: we relate the @xmath0-truncated kronecker products of symmetric functions to the semi - invariant rings of a family of quiver representations .
we find cluster algebra structures for these semi - invariant rings when @xmath1 .
each @xmath2-vector cone @xmath3 of these cluster algebras controls the @xmath4-truncated kronecker products for all symmetric functions of degree no greater than @xmath5 . as a consequence , each relevant kronecker coefficient is the difference of the number of the lattice points inside two rational polytopes .
we also give explicit description of all @xmath3 s . as an application
, we compute some invariant rings . [ multiblock footnote omitted ] .
And you have already written the first three sentences of the full article: given a partition @xmath6 of @xmath7 , let @xmath8 be the associated irreducible complex representation of the symmetric group @xmath9 .
the _ kronecker coefficients _
@xmath10 are the tensor product multiplicities : @xmath11 to determine these coefficients and understand their properties has been one of the major problems in combinatorics and representation theory for nearly a century ..
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people are particularly interested in finding combinatorial interpretation for these coefficients .
they hope that kronecker coefficients count some combinatorial objects , eg .
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Suppose that you have an abstract for a scientific paper: we measured the low - temperature thermal conductivity of a new layered superconductor with quasi - one - dimensional characteristics , the ternary telluride ta@xmath0pd@xmath1te@xmath2 with transition temperature @xmath3 4.3 k. the significant residual linear term of thermal conductivity in zero magnetic field and its rapid field dependence provide evidences for nodes in the superconducting gap . by measuring resistivity under pressures ,
we reveal a superconducting dome in the temperature - pressure phase diagram .
the existence of gap nodes and superconducting dome suggests unconventional superconductivity in ta@xmath0pd@xmath1te@xmath2 , which may relate to a charge - density wave instability in this low - dimensional compound . .
And you have already written the first three sentences of the full article: finding unconventional superconductors and understanding their superconducting mechanism is one of the main themes in condensed matter physics @xcite .
the term unconventional " firstly means the superconducting pairing mechanism is not phonon - mediated .
this usually manifests as a superconducting dome neighbouring a magnetic order in the phase diagram , and spin fluctuations are considered as the major pairing glue @xcite ..
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secondly , the term unconventional " means the wave function of cooper pairs is not @xmath4-wave .
symmetry imposed nodes ( gap zeros ) are often observed , such as in @xmath5-wave cuprate superconductors and heavy - fermion superconductor cecoin@xmath6 @xcite , and in @xmath7-wave superconductor sr@xmath8ruo@xmath0 @xcite .
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Suppose that you have an abstract for a scientific paper: we investigate the mixed state properties in a type ii multiband superconductor with uniaxial anisotropy under the pauli paramagnetic effects .
eilenberger theory extended to a multiband superconductor is utilized to describe the detailed vortex lattice properties , such as the flux line form factors , the vortex lattice anisotropy and magnetic torques .
we apply this theory to sr@xmath0ruo@xmath1 to analyze those physical quantities obtained experimentally , focusing on the interplay between the strong two - dimensional anisotropy and the pauli paramagnetic effects .
this study allows us to understand the origin of the disparity between the vortex lattice anisotropy ( @xmath260 ) and the @xmath3 anisotropy ( @xmath220 ) . among the three bands
; @xmath4 with the effective mass anisotropy @xmath2180 , @xmath5 with @xmath2120 , and @xmath6 with @xmath260 , the last one is found to be the major band , responsible for various magnetic responses while the minor @xmath4 band plays an important role in the vortex formation .
namely , in a field orientation slightly tilted away from the two dimensional basal plane those two bands cooperatively form the optimal vortex anisotropy which exceeds that given by the effective mass formula with infinite anisotropy .
this is observed by small angle neutron scattering experiments on sr@xmath0ruo@xmath1 .
the pairing symmetry of sr@xmath0ruo@xmath1 realized is either spin singlet or spin triplet with the d - vector strongly locked in the basal plane .
the gap structure is that the major @xmath6 band has a full gap and the minor @xmath4 band has a @xmath7 like gap . .
And you have already written the first three sentences of the full article: it is now widely recognized that multiband superconductors are omnipresent @xcite .
this recognition may be triggered by mgb@xmath0 @xcite where there exist distinctive two bands ; the 3d @xmath8-band and 2d like @xmath9-band@xcite .
they play different role in forming superconductivity , in particular in magnetic properties under an applied field , such as symmetry of vortex lattices@xcite or the form factors probed by small angle neutron scattering ( sans ) experiments@xcite . to understand its detailed magnetic response , a two band model is indispensable ..
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in fact different dimensionality of the band structures between the @xmath8-band and @xmath9-band gives rise to rotation of the triangular vortex lattice under varying field@xcite .
the form factors of sans experiments clearly demonstrate a gradual change of the two components of the @xmath8-band and @xmath9-band as field varies@xcite .
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Suppose that you have an abstract for a scientific paper: spatio - temporal bifurcations and complex dynamics in globally coupled intrinsically bistable electrochemical systems with an s - shaped current - voltage characteristic under galvanostatic control are studied theoretically on a one - dimensional domain .
the results are compared with the dynamics and the bifurcation scenarios occurring in a closely related model which describes pattern formation in semiconductors . under galvanostatic control
both systems are unstable with respect to the formation of stationary large amplitude current domains .
the current domains as well as the homogeneous steady state exhibit oscillatory instabilities for slow dynamics of the potential drop across the double layer , or across the semiconductor device , respectively .
the interplay of the different instabilities leads to complex spatio - temporal behavior .
we find breathing current domains and chaotic spatio - temporal dynamics in the electrochemical system . comparing these findings with the results obtained earlier for the semiconductor system , we outline bifurcation scenarios leading to complex dynamics in globally coupled bistable systems with subcritical spatial bifurcations . .
And you have already written the first three sentences of the full article: the focus of research in nonlinear dynamics has evolved from temporal instabilities over simple spatial patterns to complex spatio - temporal behavior and the control or synchronization of such dynamics .
complex spatio - temporal behavior in reaction - diffusion equations , which is in a wider sense the class of equations dealt with also in electrochemistry , might be found when instabilities breaking time and space symmetries interact .
a generic case is the interaction of turing @xcite and hopf bifurcation in a two component activator - inhibitor system in which the involved species diffuse ..
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complex spatio - temporal dynamics has been found near this codimension - two point theoretically @xcite as well as experimentally @xcite . in electrochemical systems that can be described by a two component model one variable typically is of electrical nature and the associated transport mechanism is migration rather than diffusion @xcite .
the decisive variable for the dynamics of the electric circuit is the double layer potential @xmath0 , measuring the voltage drop across the interface between the working electrode and the electrolyte solution @xcite .
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Suppose that you have an abstract for a scientific paper: we propose a scheme for implementing a controlled unitary gate between two distant atoms directly communicating through a quantum transmission line . to achieve our goal ,
only a series of several coherent pulses are applied to the atoms .
our scheme thus requires no ancilla atomic qubit .
the simplicity of our scheme may significantly improve the scalability of quantum computers based on trapped neutral atoms or ions . .
And you have already written the first three sentences of the full article: a quantum optical system utilizing trapped neutral atoms or ions for qubits is one of promising candidates for implementing a quantum computer @xcite .
actually , there have been numerous theoretical @xcite and experimental @xcite achievements showing the positive prospects for it .
the number of qubits in such a system is , however , obviously limited by the size of the trapping structure , while one of the essential factors for a useful quantum computer is the scalability ..
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this difficulty could be overcome by connecting partially implemented quantum computation nodes to form a quantum network . for any unitary operation for the whole quantum network to be possible , controlled unitary operations between two nodes
should be performed as well as local unitary operations at each node @xcite .
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11,389 |
Suppose that you have an abstract for a scientific paper: the contribution of the quiet sun to solar irradiance variability , due either to changes of the solar effective temperature or to the presence of unresolved magnetic field , is still poorly understood . in this study
we investigate spectral line diagnostics that are sensitive to both temperature variations and the presence of small scale unresolved magnetic features in these areas of the solar atmosphere .
specifically we study the dependence on the magnetic flux density of three parameters describing the shape of two magnetically sensitive lines , at 630.2 nm and 617.3 nm , namely the line core intensity ( ic ) , full width at half maximum ( fwhm ) , and the equivalent width ( eqw ) . to this aim
we analyze observations of active region noaa 11172 , acquired with ibis at the dunn solar telescope , as well as results from numerical synthesis .
our results show that ic is sensitive to both temperature and magnetic flux density variations , fwhm is mostly affected by magnetic field changes , and eqw is mostly sensitive to temperature .
variations of a few percent of the measured line parameters are found in observational data that was spatially degraded to represent quiet - sun , disk - centre , medium resolution observations .
it is therefore possible to disentangle magnetic from pure thermodynamic effects by comparison of temporal variations of the eqw and the fwhm of either the two lines . .
And you have already written the first three sentences of the full article: it is well established that both the total and spectral solar irradiance ( si , henceforth ) are modulated by the emergence and evolution of the magnetic field in the solar atmosphere . in particular , si variations measured on time scales from days to several solar rotations can be explained by accounting for the radiative effect of the presence of magnetic flux in sunspots , faculae , and network regions ( e.g. * ? ? ?
. however , there is still uncertainty in measurements of si variations on time scales of the activity cycle and longer ( e.g. * ? ? ?
* ; * ? ? ?.
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* ) , as well as in the determination of individual contributions of different magnetic features to the measured variations ( e.g. * ? ? ?
* ; * ? ? ?
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Suppose that you have an abstract for a scientific paper: we present results of numerical studies of the landau - ginzburg dynamics of the order parameter in one - dimensional models inspired by the condensed matter analogues of cosmological phase transitions .
the main goal of our work is to show that , as proposed by one of us @xcite , the density of the frozen - out topological defects is set by the competition between the quench rate the rate at which the phase transition is taking place and the relaxation rate of the order parameter .
in other words , the characteristic domain size , which determines the typical separation of topological defects in the new broken symmetry phase , is of the order of the correlation length at the instant at which the relaxation timescale of the order parameter equals the time remaining to the phase transition
. in estimating the size of topological domains , this scenario shares with the original kibble mechanism the idea that topological defects will form along the boundaries of independently selected regions of the new broken symmetry vacuum .
however , it derives the size of such domains from non - equilibrium aspects of the transition ( quench rate ) , as opposed to kibble s original proposal in which their size was estimated from the ginzburg temperature above which thermally activated symmetry restoration can occur . .
And you have already written the first three sentences of the full article: the expansion of the universe inevitably leads to a drop of the temperature of the primordial fireball .
this cooling provides natural conditions that are believed to precipitate a series of phase transitions in which `` false '' symmetric , high temperature phases are transformed into low temperature broken symmetry `` true '' vacuum . as the universe undergoes such phase transitions , the selection of the low - temperature , broken symmetry phase can only occur locally , within the causally correlated regions .
kibble @xcite first noted that this symmetry breaking process may leave relics of the high energy phase which will be trapped by the topologically stable configurations of the broken symmetry phase . in principle , such topological defects could be massive enough to leave an observational imprint in the cosmic microwave background and perhaps also produce the seeds needed for matter structure formation @xcite ..
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there are three principal types of topological defects @xcite .
they differ by their dimensionality .
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11,391 |
Suppose that you have an abstract for a scientific paper: we have used the sinfoni integral field spectrograph to map the near - infrared k - band emission lines of molecular and ionised hydrogen in the central regions of two cool core galaxy clusters , abell 2597 and sersic 159 - 03 .
gas is detected out to 20 @xmath0 from the nuclei of the brightest cluster galaxies and found to be distributed in clumps and filaments around it .
the ionised and molecular gas phases trace each other closely in extent and dynamical state .
both gas phases show signs of interaction with the active nucleus . within the nuclear regions the kinetic luminosity of this gas
is found to be somewhat smaller than the current radio luminosity . outside the nuclear region
the gas has a low velocity dispersion and shows smooth velocity gradients .
there is no strong correlation between the intensity of the molecular and ionised gas emission and either the radio or x - ray emission . the molecular gas in abell 2597 and sersic 159 - 03 is well described by a gas in local thermal equilibrium ( lte ) with a single excitation temperature @xmath1 @xmath2 2300 @xmath3 .
the emission line ratios do not vary strongly as function of position , with the exception of the nuclear regions where the ionised to molecular gas ratio is found decrease .
these constant line ratios imply a single source of heating and excitation for both gas phases .
[ firstpage ] galaxies : clusters : individual : abell 2597 galaxies : clusters : individual : sersic 159 - 03 cooling flows infrared : ism . .
And you have already written the first three sentences of the full article: cool cores are regions at the centre of rich clusters where the hot thermal x - ray emitting gas ( @xmath4 @xmath2 10@xmath5 @xmath3 ) is dense enough to cool radiatively within a hubble time ( see * ? ? ?
* ; * ? ? ?
* for reviews ) ..
Please generate the next two sentences of the article
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cooling rates of the order of 100 @xmath6 @xmath7 and up to 1000 @xmath6 @xmath7 have been estimated for this hot x - ray gas ( e.g. , * ? ? ?
. however , recent _ chandra _ and _ xmm - newton _ x - ray spectra show that little or no x - ray emitting gas ( @xmath810% ) cools below one third of the virial temperature ( e.g. , * ? ? ?
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11,392 |
Suppose that you have an abstract for a scientific paper: in this talk , we discuss some general properties of particle production in a field theory coupled to strong time dependent sources , and techniques to compute the spectrum of the produced particles in such theories .
we also discuss the application of these results to the description of hadron or heavy ion collisions in the color glass condensate framework . 1
. service de physique thorique ( ura 2306 du cnrs ) + cea / dsm / saclay , 91191 , gif - sur - yvette cedex , france 2 . nuclear theory , physics department + brookhaven national laboratory , upton , ny 11973 , usa .
And you have already written the first three sentences of the full article: at high energy , all the internal timescales of a hadron are time dilated .
therefore , more and more soft fluctuations carrying a smaller and smaller fraction @xmath0 of the hadron momentum become long - lived and become relevant in interactions with another hadron . on the contrary , on the timescales relevant for such an interaction process
, the large @xmath0 partons can be seen as completely frozen degrees of freedom , whose only role is to act as sources that radiate more small @xmath0 gluons ..
Please generate the next two sentences of the article
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moreover , the small @xmath0 modes will eventually have an occupation number larger than unity , and undergo recombinations
a process known as _ saturation _
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11,393 |
Suppose that you have an abstract for a scientific paper: we study the cosmology of a generalized galileon field @xmath0 with five covariant lagrangians in which @xmath0 is replaced by general scalar functions @xmath1 ( @xmath2 ) . for these theories ,
the equations of motion remain at second - order in time derivatives .
we restrict the functional forms of @xmath1 from the demand to obtain de sitter solutions responsible for dark energy .
there are two possible choices for power - law functions @xmath1 , depending on whether the coupling @xmath3 with the ricci scalar @xmath4 is independent of @xmath0 or depends on @xmath0 .
the former corresponds to the covariant galileon theory that respects the galilean symmetry in the minkowski space - time . for generalized galileon theories
we derive the conditions for the avoidance of ghosts and laplacian instabilities associated with scalar and tensor perturbations as well as the condition for the stability of de sitter solutions .
we also carry out detailed analytic and numerical study for the cosmological dynamics in those theories . .
And you have already written the first three sentences of the full article: the @xmath5-cold - dark - matter ( @xmath5cdm ) model has been consistent with observational data , but the energy scale of dark energy is too low to be compatible with the cosmological constant originated from the vacuum energy in quantum field theory @xcite . since the observations allow the variation of the dark energy equation of state @xcite , many models have been proposed to explain the present accelerated expansion of the universe @xcite . for example , a light scalar field with a slowly varying potential , called quintessence , was introduced as an alternative to the cosmological constant @xcite . in general , however , it is not easy to construct viable particle physics models of quintessence because of an extremely light mass required for the cosmic acceleration today @xcite .
another approach for addressing the dark energy problem is to modify the law of gravity from general relativity at large distances @xcite . in this approach
there have been two main streams ..
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the first consists of introducing a lagrangian for gravity built up out of the ricci , riemann , and metric tensors , which generally leads to 4-th order differential equations .
the @xmath6 gravity @xcite and the gauss - bonnet gravity @xcite belong to this class .
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11,394 |
Suppose that you have an abstract for a scientific paper: power consumption is a critical consideration in high performance computing systems and it is becoming the limiting factor to build and operate petascale and exascale systems .
when studying the power consumption of existing systems running hpc workloads , we find that power , energy and performance are closely related which leads to the possibility to optimize energy consumption without sacrificing ( much or at all ) the performance . in this paper , we propose a hpc system running with a gnu / linux os and a real time resource manager ( rtrm ) that is aware and monitors the healthy of the platform . on the system ,
an application for disaster management runs .
the application can run with different qos depending on the situation .
we defined two main situations .
normal execution , when there is no risk of a disaster , even though we still have to run the system to look ahead in the near future if the situation changes suddenly . in the second scenario ,
the possibilities for a disaster are very high .
then the allocation of more resources for improving the precision and the human decision has to be taken into account .
the paper shows that at design time , it is possible to describe different optimal points that are going to be used at runtime by the rtrm with the application .
this environment helps to the system that must run 24/7 in saving energy with the trade - off of losing precision .
the paper shows a model execution which can improve the precision of results by 65% in average by increasing the number of iterations from 10 ^ 3^ to 10 ^ 4^. this also produces one order of magnitude longer execution time which leads to the need to use a multi - node solution . the optimal trade - off between precision vs. execution time
is computed by the rtrm with the time overhead less than 10% against a native execution .
[ pacs : 89.20.ff , 47.50.cd , 92.40.-t , 07.05.bx , 07.05.tp , 89.20.ff ] .
And you have already written the first three sentences of the full article: application requirements , power , and technological constraints are driving the architectural convergence of future processors towards heterogeneous many - cores .
this development is confronted with variability challenges , mainly the susceptibility to time - dependent variations in silicon devices .
increasing guard - bands to battle variations is not scalable , due to too large worst - case cost impact for technology nodes around 10 nm ..
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the goal of next generation firmware is to enable next - generation embedded and high - performance heterogeneous many - cores to cost - effectively confront variations by providing dependable - performance : correct functionality and timing guarantees throughout the expected lifetime of a platform under thermal , power , and energy constraints .
an optimal solution should employ a cross - layer approach .
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11,395 |
Suppose that you have an abstract for a scientific paper: one of the major challenges about cyber physical systems is how to prevent cyber attacks to ensure system integrity .
there has been a large number of different types of attacks discussed in the modern control and computer science communities . in this paper
we aim to investigate one special type of attacks in the discrete - event system framework , where an attacker can arbitrarily alter sensor readings after intercepting them from a target system in order to trick a given supervisor to issue control commands improperly , driving the system to an undesirable state .
we first consider the cyber attack problem from an attacker point of view , and formulate an attack with bounded sensor reading alterations ( absra ) problem .
we then show that the supremal ( or least restrictive ) absra exists and can be synthesized , as long as the plant model and the supervisor model are regular , i.e. , representable by finite - state automata . upon the synthesis of the supremal absra , we present a synthesis algorithm , which ensures that a computed supervisor will be absra - robust ,
i.e. , either an absra will be detectable or will not lead the system to an undesirable state .
discrete - event systems , supervisory control , cyber security , attack under bounded sensor reading alterations , partial observation , controllability .
And you have already written the first three sentences of the full article: a cyber - physical system ( cps ) is a mechanism controlled or monitored by computer - based algorithms
. examples of cps include smart grid , autonomous automobile systems , medical monitoring , process control systems , distributed robotics , and automatic pilot avionics , etc .
the connection between the cyber part and the physical part heavily relies on communication networks , which has been raising a major security concern , as different types of cyber attacks can tamper the data collection processes and interfere safety critical decision making processes , which may cause irreparable damadges to the physical systems being controlled and to people who depend on those systems ..
Please generate the next two sentences of the article
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+ there has been a growing number of publications addressing the cyber security issues from both the computer science community , which focuses on the computer computation related issues , and the systems control community , which focuses on issues related to the system dynamics affected by cyber attacks .
recently , more and more efforts have been made in classifying different types of malicious attacks , assuming that the attackers are sufficiently intelligent @xcite @xcite , instead of merely just generating random failures , which is well studied in the fields of reliability and fault tolerant control .
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11,396 |
Suppose that you have an abstract for a scientific paper: our main result is that the image of the quantum representation of a central extension of the mapping class group of the genus @xmath0 closed orientable surface at a prime @xmath1 is a zariski dense discrete subgroup of some higher rank algebraic semi - simple lie group @xmath2 defined over @xmath3 . as an application we find that , for any prime @xmath1 a central extension of the genus @xmath4 mapping class group surjects onto the finite groups @xmath5 , for all but finitely many primes @xmath6 .
this method provides infinitely many finite quotients of a given mapping class group outside the realm of symplectic groups .
+ 2000 msc classification : 57 m 07 , 20 f 36 , 20 g 20 , 22 e 40 .
+ keywords : mapping class group , dehn twist , braid group , burau representation , quantum representation , discrete subgroup of semi - simple lie groups , finite quotient . .
And you have already written the first three sentences of the full article: the aim of the this paper is to obtain a largeness result for the images of quantum representations of mapping class groups in genus at least @xmath7 .
the main motivation is the construction of large families of finite quotients of ( central extensions of the ) mapping class groups by using the strong approximation theorem .
this method furnishes a large supply of finite quotients of mapping class groups outside the realm of symplectic groups ..
Please generate the next two sentences of the article
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similar results were obtained independently by masbaum and reid in @xcite .
earlier , looijenga has proved in @xcite that the images of prym representations ( associated to finite abelian groups ) of suitable finite index subgroups of mapping class groups and of subgroups from the johnson filtration are arithmetic groups .
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11,397 |
Suppose that you have an abstract for a scientific paper: the classical drift diffusion ( dd ) model of spin transport treats spin relaxation via an empirical parameter known as the `` spin diffusion length '' . according to this model ,
the ensemble averaged spin of electrons drifting and diffusing in a solid decays exponentially with distance due to spin dephasing interactions .
the characteristic length scale associated with this decay is the spin diffusion length .
the dd model also predicts that this length is different for `` upstream '' electrons traveling in a decelerating electric field than for `` downstream '' electrons traveling in an accelerating field .
however this picture ignores energy quantization in confined systems ( e.g. quantum wires ) and therefore fails to capture the non - trivial influence of subband structure on spin relaxation .
here we highlight this influence by simulating upstream spin transport in a multi - subband quantum wire , in the presence of dyakonov - perel spin relaxation , using a semi - classical model that accounts for the subband structure rigorously .
we find that upstream spin transport has a complex dynamics that defies the simplistic definition of a `` spin diffusion length '' .
in fact , spin does not decay exponentially or even monotonically with distance , and the drift diffusion picture fails to explain the qualitative behavior , let alone predict quantitative features accurately .
unrelated to spin transport , we also find that upstream electrons undergo a `` population inversion '' as a consequence of the energy dependence of the density of states in a quasi one - dimensional structure . .
And you have already written the first three sentences of the full article: spin transport in semiconductor structures is a subject of much interest from the perspective of both fundamental physics and device applications .
a number of different formalisms have been used to study this problem , primary among which are a classical drift diffusion approach @xcite , a kinetic theory approach @xcite , and a microscopic semiclassical approach @xcite .
the central result of the drift diffusion approach is a differential equation that describes the spatial and temporal evolution of carriers with a certain spin polarization @xmath0 ..
Please generate the next two sentences of the article
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@xcite derived this equation for a number of special cases starting from the wigner distribution function . in a coordinate system where the x - axis coincides with the direction of electric field driving transport , this equation is of the form : @xmath1 where @xmath2 @xmath3 is the diffusion coefficient , and @xmath4 and @xmath5 are dyadics ( 9-component tensors ) that depend on @xmath3 , the mobility @xmath6 and the spin orbit interaction strength in the material
. solutions of equation ( [ spin ] ) , with appropriate boundary conditions , predict that the ensemble averaged spin @xmath7 = @xmath8 should decay exponentially with @xmath9 according to : @xmath10 where @xmath11 here @xmath12 is the strength of the driving electric field and @xmath13 is a parameter related to the spin orbit interaction strength . the quantity
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11,398 |
Suppose that you have an abstract for a scientific paper: we explore set - stabilizability by constrained controls , and both controllability and stabilizability can be regarded as the special case of set - stabilizability .
we not only clarify how to define equilibrium points of schr@xmath0dinger equations , but also establish the necessary and sufficient conditions for stabilizability of quantum systems .
unfortunately , it is revealed that the necessary conditions are quite strict for stabilizability of some concrete quantum systems like nuclear spin systems , and this further justifies the introduction of set - stabilizability notion .
it is also exemplified that set - stabilizability can be used for investigating quantum information processing problems including quantum information storage and entangled states generation . , , quantum systems , controllability , stabilizability .
And you have already written the first three sentences of the full article: the concepts of controllability and observability are important contribution of control theorists to the science , technology , and engineering domain . with the introduction of these structural concepts , we begin to deeply understand the relationship between the input - output description and state - space description .
the concept of controllability was first proposed for linear systems by r. e. kalman in his remarkable paper@xcite in 1960s .
controllability of nonlinear systems was further investigated by h. j. sussmann and v. jurdjevic@xcite and r. hermann and a. j. krener@xcite in 1970s ..
Please generate the next two sentences of the article
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quantum control theory has been developed ever since last century@xcite .
recently , quantum information and quantum computation is the focus of reseach@xcite .
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11,399 |
Suppose that you have an abstract for a scientific paper: an understanding of how individuals shape and impact the evolution of society is vastly limited due to the unavailability of large - scale reliable datasets , that can simultaneously capture information regarding individual movements as well as social interactions .
we believe that the popular indian film industry , ` bollywood ' , can provide a social network apt for such a study .
bollywood provides massive amounts of real , unbiased data that spans over 100 years and hence this network has been used as a model for the present paper .
it is seen that the nodes which maintain a moderate degree or widely cooperate with the other nodes of the network , tend to be more fit ( measured as the success of the node in the industry ) in comparison to the other nodes .
the analysis carried forth in the current work , using a conjoined framework of complex network theory and random matrix theory , aims to quantify the elements that determine the fitness of an individual node and the factors that contribute to the robustness of a network .
the authors of this paper believe that the method of study used in the current paper can be extended to study various other industries and organizations . * uncovering randomness and success in society * + * sarika jalan@xmath0 , camellia sarkar@xmath1 , anagha madhusudanan@xmath2 , sanjiv kumar dwivedi@xmath2 + _ @xmath3 complex systems lab , physics discipline , indian institute of technology indore , m - block , iet - davv campus , khandwa road , indore 452017 , india + _ @xmath4 complex systems lab , center for biosciences and biomedical engineering , indian institute of technology indore , m - block , iet - davv campus , khandwa road , indore 452017 , india + @xmath5 e - mail : [email protected]__ * .
And you have already written the first three sentences of the full article: the field of network analysis helps us to look at the study of an individual component as a part of a complex social structure and its interactions @xcite .
it explains various phenomena in a wide variety of disciplines ranging from physics to psychology to economics .
the theory is adept at finding the causal relationships between network attributes such as the position of a node and the specific ties associated with it , and the fitness of the said node @xcite ..
Please generate the next two sentences of the article
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such relationships , that seemed thoroughly random to the eyes of a researcher only about a decade before , have now been vastly studied and documented @xcite .
we aim to further investigate the very interesting idea that human behavior is predictable to a fair degree @xcite using the bollywood network as a model for this purpose . making nearly one thousand feature films and fifteen hundred short films per year ,
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