Rotating waves in the Theta model for a ring of synaptically connected neurons
小学上册第十三次英语第5单元真题(有答案)

小学上册英语第5单元真题(有答案)英语试题一、综合题(本题有100小题,每小题1分,共100分.每小题不选、错误,均不给分)1.We eat ______ (snacks) during recess.2.Which animal can swim and fly?A. FishB. BirdC. DuckD. Dog答案:C3.I like to collect ________ (硬币).4.My ________ (玩具名称) brings smiles and laughter.5.The _______ (The Great Awakening) was a series of religious revivals in America.6.Salt forms when an acid reacts with a ________.7.An emulsion is a mixture of two ________ that do not usually mix.8.The stars are ___ (twinkling/shining) in the night.9.The _____ of a planet determines its seasons.10. A __________ is a place of scientific research.11.The Earth's surface is shaped by both human and ______ factors.12.The fountain is _______ (flowing) beautifully.13.The bee is essential for _______ pollination.14.My sister enjoys __________ (参加) school clubs.15.I can ______ (ride) a bicycle.16.My teacher is very ________ (友好) and helps us learn.17.The ________ (花卉) market has many types of flowers.18.The pH scale measures how acidic or ______ a substance is.19.The _______ (The Cold War) shaped the political landscape of the 20th century.20.We have a ______ (丰富的) schedule for learning activities.21. Panther Party was founded to combat ________ (种族不平等). The Bost22.My brother loves to __________ (尝试新事物).23.The chemical formula for silicon dioxide is ______.24.What is the name of the famous artist known for his "The Last Judgment"?A. MichelangeloB. RaphaelC. Leonardo da VinciD. Titian答案: A25.The __________ (二战后的重建) focused on rebuilding Europe.26.The element that makes up most of the human body is _______.27.The starfish can regenerate lost ______ (肢体).28.Astronomy is one of the oldest sciences in ______.29.Catalysts are often used to speed up _____ reactions.30.I enjoy ___ (baking) cookies.31.The dog is _______ (在叫).32.I like to _______ (play) outside.33.The sun is _____ (shining/raining) today.34.I can _____ my shoes by myself. (put on)35.My hamster runs on its ______ (轮子) all night.36. A chemical reaction can change the ______ of a substance.37.My _____ (姐姐) is a great artist.38.The baby is ______ her bottle. (drinking)39.The children are ______ in the swimming pool. (playing)40.The _____ (戏剧) is entertaining.41.I enjoy participating in school events like __________.42.What do we call a house made of ice?A. IglooB. CabinC. CottageD. Mansion答案:A43. A ________ is a large open space in a forest.44.The beauty of flowers can enhance the atmosphere of any ______. (花卉的美丽可以提升任何场合的氛围。
An Analysis of States in the Phase Space From Quantum Mechanics to General Relativity

1
ABSTRACT The paper has euristic character. It exploits basic concepts of quantum physics to infer on a selfconsistent basis the properties of the gravitational field. The only assumption of the theoretical model is the quantum uncertainty: the physical properties of quantum systems depends on the delocalization ranges of the constituent particles and not on their local dynamical variables. The conceptual approach follows the same formalism already described in early non-relativistic papers [S. Tosto, Il Nuovo Cimento B, vol. 111, n.2, (1996) and S. Tosto, Il Nuovo Cimento D, vol. 18, n.12, (1996)]. The paper shows that the extended concept of space time uncertainty is inherently consistent with the postulates of special relativity and that the most significant results of general relativity are achieved as straightforward consequence of the space time delocalization of quantum particles.
大学英语四级模拟试题及答题详解

大学英语四级模拟试题及答题详解Part I Reading Comprehension (Skimming and Scanning) (15 minutes)Directions: In this part, you will have 15 minutes to go over the passage quickly and answer the questions on Answer Sheet 1.For questions 1 - 7, markY (for YES) if the statement agrees with the information given in the passage;N (for NO) if the statement contradicts the information given in the passage;NG (for NOT GIVEN)if the information is not given in the passage.For questions 8 - 10, complete the sentences with the information given in the passage.SleepSleep is one of those funny things about being a human being --- you just have to do it. Have you ever wondered why? And what about the crazy dreams, like the one where a bad person is chasing you and you can’t run or yell. Does that make any sense?Characteristics of SleepWhen we see someone sleeping, we recognize the following characteristics:If possible, the person will lie down to go to sleep.The person’s eyes are closed.The person doesn’t hear anything unless it is a loud noise.The person breathes in a slow, rhythmic pattern.The person’s muscles are completely relaxed. If sitting up, the person may fall out of his or her chair as sleep deepens.During sleep, the person occasionally rolls over or rearranges his or her body. This happens approximately once or twice an hour. This may be the body’s way of making sure that no part of the body or skin has its circulation cut off for too long a period of time.In addition to these outward signs, the heart slows down and the brain does some prettyIn other words, a sleeping person is unconscious to most things happening in the environment. The biggest difference between someone who is asleep and someone who has fainted or gone into a coma is the fact that a sleeping person can be aroused if the stimulus presented by is strong enough. If you shake the person, yell loudly or flash a bright light, a sleeping person will wake up.Who Sleeps?Reptiles(爬行动物), birds and mammals all sleep. That is, they become unconscious to their surroundings for periods of time. Some fish and amphibians (两栖动物)(两栖动物) reduce their awareness but do not ever become unconscious like the higher vertebrates(脊椎动物) do. Insects do not appear to sleep, although they may become inactive in daylight or darkness.By studying brainwaves, it is known that reptiles do not dream. Birds dream a little. Mammals all dream during sleep.Different animals sleep in different ways. Some animals, like humans, prefer to sleep in one long session. Other animals like to sleep in many short bursts. Some sleep at night, while others sleep during the day.Sleep and the BrainIf you attach an electroencephalograph to a person’s head, you can record the person’s brainwave activity. An awake and relaxed person generates alpha waves, which are consistent oscillations at about 10 cycles per second. An alert person generates beta waves, which are about twice as fast.During sleep, two slower patterns called theta waves and delta waves take over. Theta waves have oscillations in the range of 3.5 to 7 cycles per second, and delta waves have oscillations of less than 3.5 cycles per second. As a person falls asleep and sleep deepens, the brainwave patterns slow down. A person deep in delta wave sleep is hardest to wake up.REM SleepAt several points during the night, something unexpected happens -- rapid eye movement (REM) sleep occurs. Most people experience three to five intervals of REM sleep per night, and brainwaves during this period speed up to awake levels. If you ever watch a person or a dog experiencing REM sleep, you will see their eyes flickering back and forth rapidly. In many dogs and some people, arms, legs and facial muscles will twitch during REM sleep. Periods of sleep other than REM sleep are known as NREM (non-REM) sleep.REM sleep is when you dream. If you wake up a person during REM sleep, the person can vividly recall dreams. If you wake up a person during NREM sleep, generally the person will notYou must have both REM and NREM sleep to get a good night ’s sleep. A normal person will spend about 25 percent of the night in REM sleep, and the rest in NREM. A REM session a dream -- lasts five to 30 minutes.When You Miss Some Zzzzs …One way to understand why we sleep is to look at what happens when we don ’t get enough: As you know if you have ever pulled an all-nighter, missing one night of sleep is not fatal. A person will generally be irritable during the next day and will either slow down (become tired easily ) or will be totally wired because of adrenalin (肾上腺素)。
chap7-Waves

(8)
(9)
demonstrating that we do indeed have a solution of the wave equation. This solution is a wave “traveling” in the direction of k in the sense that a point of constant phase, meaning k · x − ωt = constant, moves along this direction with a speed v which is ω/k . Furthermore, we have a plane wave, by which we mean that a surface of constant phase is a plane; in particular, the surfaces of constant phase are just planes perpendicular to k.
v= ω /k
Fig.1: A point of stationary phase moves with velocity |v | = ω/k
1.2
Conditions Imposed by Maxwell’s Equations
Next, let us see how the electromagnetic fields can be described in terms of these scalar plane waves. Let us look for an electric field and a magnetic induction with the forms E(x, t) = E0 ei(k·x−ωt) B(x, t) = B0 ei(k·x−ωt) (10)
The Halo Beaming Model for Gamma-Ray Bursts

a rXiv:as tr o-ph/972182v121Fe b1997The Halo Beaming Model for Gamma-Ray Bursts R.C.Duncan 1&Hui Li 2ReceivedABSTRACTWe consider a model for gamma-ray bursts(GRBs)from high-velocity neutron stars in the galactic halo.In this model,bursters are born in the galactic disk with large recoil velocities V r,and GRBs are beamed to within emission cones of half-angleφb centered on V r.We describe scenarios for magnetically-channeled GRBs that have such beaming characteristics.We then make detailed comparisons of this halo beaming model(HBM)to data from the3rd BATSE Catalog and from the Pioneer Venus Orbiter experiment,for both GRB intensity and angular position distributions.Acceptablefits to observations of over1000bursts are obtained forφb=15◦−30◦and for a BATSE sampling depth of D∼180kpc,which corresponds to a peak burst luminosity of∼1040ergs s−1.Present data favor a truly isotropic(cosmological) model over the HBM,but not by a statistically compelling margin(<∼2σ).The HBM makes the distinctive prediction that the galactocentric quadrupole moment cos2Θ −1/3for bright,nearby GRBs is large,even though the dipole moment cosΘ remains near zero.Bursters born in nearby external galaxies,such as M31,are almost entirely undetectable in the HBM because of misdirected beaming.We analyze several refinements of the basic HBM: gamma-ray intensities that vary with angle from the beam axis;non-standard-candle GRB luminosity functions;and models including a subset of bursters that do not escape from the galaxy.We also discuss the energy budgets for the bursters,the origins of their recoils,and the physics of burst beaming and alignment.One possible physical model is based on the magnetar model of soft gamma repeaters(SGRs).Empirical bounds on the rate of formation and peculiar velocities of SGRs imply that there exist∼104to∼107aged SGRs in the galactic halo within a distance of100kpc.The HBM gives an acceptablefit to observations only if it satisfies some special conditions(φb≈20◦,uniform bursting rate)which are possible,but for which there are no clear and compelling theoretical justifications.The cosmological burst hypothesis is more generic and thus more attractive in this sense.Subject headings:gamma rays:bursts—stars:magneticfields—stars:neutron —galaxy:halo1.IntroductionThe Burst and Transient Source Experiment(BATSE)on the NASA Compton Gamma-Ray Observatory has revealed a nearly isotropic but inhomogeneous sky distribution of gamma-ray bursts(Meegan et al.1992;Meegan et al.1996).An additional major constraint on GRB theories,revealed by the Pioneer Venus Orbiter(PVO)experiment,is that the intensity distribution of bright bursts is consistent with a locally-uniform density of sources in Euclidean space(Fenimore et al.1993).These facts are simply and generically accounted for if the faintest observed GRBs come from cosmological distances(e.g.,Paczy´n ski1995). An alternative possibility,that we will focus on here,is that the bursts come from the extended halo or corona of our galaxy.Galactic halo models for GRBs werefirst considered and tested against data by Fishman et al.(1978)and Jennings&White(1980).Reasons for favoring halo models have been summarized by Lamb(1995).In galactic halo GRB models,it is often supposed that the bursters are neutron stars, since such compact stars are conjectured to be capable of producing intensefluxes of hard, non-thermal photons;while their small size could drive burst variability on submillisecond time scales.Other reasons for favoring neutron stars include observations of spectral lines, which are at present controversial,and a possible connection of classic GRBs with the March5,1979gamma ray burster(e.g.,Duncan&Thompson1992,hereafter DT92)which was localized to an angular position lying within a young supernova remnant(Cline et al.1982;Rothschild,Kulkarni&Lingenfelter1994).The displacement of this burster from the center of the supernova remnant indicates that it acquired a velocity∼1000km s−1at birth(DT92).Neutron stars with such velocities will escape the galactic disk,and move into the halo.Recent analysis of the1979March5th event lends support to its association with classical GRBs(Fenimore,Klebesadel,&Laros1996,hereafter FKL).In addition, many high-velocity radio pulsars(V>500km s−1)have been observed(Lyne&Lorimer1994;Frail1996).For these reasons,we will focus on theories of GRBs from high-velocity neutron stars(HVNSs)born in the galactic disk,asfirst suggested by Shklovskii&Mitrofanov (1985).In particular,we will consider the“halo beaming model”(HBM)proposed earlier (Duncan,Li,&Thompson1993,hereafter DLT;Li,Duncan,&Thompson1994,LDT;Li &Duncan,1996a,1996b;Bulik&Lamb1996).Alternative models for GRBs from HVNSs in the galactic halo invoke a delayed onset of bursting activity at a time∼107years after birth in the disk(Li&Dermer1992,hereafter LD92),which has been applied in several different physical contexts(Colgate&Leonard1994;Lamb,Bulik&Coppi1996;Woosley &Herant1996);and weakly-bound bursters orbiting in a nonspherical galactic potential (Podsiadlowski,Rees&Ruderman1995,hereafter PRR).Models for bursters born in the galactic halo(Eichler&Silk1992;Hartmann1992;Salpeter&Wasserman1993;Wasserman &Salpeter1994),or the Magellanic Clouds(Fabian&Posiadlowski1993),are beyond the scope of this paper.In§2,we will describe our basic model for the galactic population of bursters,and briefly review its physical motivations.In§3we present our basic Monte Carlo model results.We discuss how these results arise,and what they could imply for halo GRB theories.We also explore the model’s sensitivity to different beaming angles.In§4we make detailed quantitative comparisons of the model with BATSE and PVO data.In particular, we study moments of the angular position distribution in bright subsets of observed GRBs, which is potentially a sensitive model discriminant.In§5we estimate the GRB repetition rate and the energy requirements for bursters.We also discuss two candidate power sources that could satisfy these requirements:magnetic energy and accretion energy.Severalrefinements of the basic HBM are investigated in§6,namely:gamma-ray intensities that vary with angular position within the beam,GRB luminosity functions,and models witha significant subset of bursters on bound orbits in the galactic halo.In§7we give our conclusions and outline future observational tests.Note that we consider possible physical mechanisms for halo GRBs,involving neutron stars with unusually strong magneticfields,in§2.3,§2.4,§5,§6.3,and Appendix B.These sections could be read separately from the rest of the paper,since they might apply in a non-beamed model context(cf.§7.2).2.The Halo Beaming Model:Physical Motivations2.1.Model AssumptionsWe will assume that GRBs are emitted by HVNSs,which emanate from the galactic disk like a“wind”extending into the galactic corona(Shklovskii&Mitrofanov1985). The HBM does not require that the bursters or their peculiar velocities have any favored orientation in a galactic coordinate frame,but it does invoke the physically-plausible condition that gamma-rays are produced only within a cone of angular radiusφb about the star’s magnetic axis±−→µ.The magnetic axis is furthermore assumed to be roughly aligned (within∼20◦)with the stellar recoil velocity V r.We discuss the physics of such beaming and alignment in§2.2.The particular version of HBM which we will analyze quantitatively in§3and§4below has the following simple properties:[1]bursters are born at positions distributed like young Pop.I stars in the galactic disk;[2]with randomly directed recoils V r=1000km s−1;[3] they emit GRBs at a constant rate,with[4]constant luminosity,and[5]the gamma ray emission is beamed parallel and anti-parallel to V r,within an angular radiusφb that we will vary.GRB beaming in a direction correlated with V r makes the observable burst distributioncomply with the BATSE dipole isotropy and the PVO brightness–distribution constraints, for the following reasons(see Figure1).Since the HVNSs are freely–streaming out of the galaxy,their mean density diminishes with distance from the galactic center as n∼r−2. However,the fraction of escaping bursters that are potentially detectable at Earth increases in proportion to the transverse area of their beaming cones,∼r2.These two trends cancell, making the effective number of bursters increase linearly with the sampled volume(i.e.,an apparent“constant density”of detectable stars)within a“core radius”R c∼R o/φb,where R o∼8.5kpc is a galactic disk dimension.In the HBM,this produces the the observed “homogeneous”distribution of bright GRBs found by the PVO experiment.Furthermore, since most bursters are undetectable when they are at small r,the observable dipole anisotropy of GRB positions in the direction of the galactic center is greatly reduced.At distances larger than R c,all bursters are detectable at Earth(or nearly all;see exceptions discussed in§3),and the n∝r−2free-streaming fall-offof burster density prevails, accounting for the“boundedness”( V/V max <0.5)found by BATSE.A more detailed illustration of the geometrical effect of burst beaming is given in Figure2.To understand thisfigure,consider for a moment an idealized model in which all stars are born precisely at the galactic center(GC),and move out in random directions on straight–line trajectories,each emitting GRBs into a cone of half-opening angleφb around its velocity vector.Bursters lying outside the circles in Figure2,or within the lens-shaped intersection of circles between the GC and Earth,are then the only ones that can be detected at Earth.There is a large“zone of avoidance”(ZOA),within which all bursters are invisible.Figure2actually shows only the2-D cross-section of this ZOA.The true ZOA is the volume of revolution of the pictured shape about the line between Earth and the galactic center.The boundary in Figure2at which stars just become observable(edge of the ZOA)is part of a circle with radius D sun/sinφb,where D sun=8.5kpc is the distance from Sun to the galactic center.In the realistic situation,bursters are born throughout the galactic disk,with a peak birth rate at∼4–5kpc from the center,where the greatest concentration of Population I stars are located(van der Kruit1987).Each birthplace in the disk then has its own ZOA, scaling up or down in linear size with the distance between the birthplace and Earth.One must add the weighted distributions of detectable bursts together to get the total observable GRB distribution.There is no simple,analytic way to do this,so in what follows we will use Monte Carlo methods.We will also calculate realistic trajectories in the galactic potential, rather than assuming straight lines.2.2.Physics of Beaming and AlignmentGamma-ray bursts from high-B environments tend to be beamed alongfield lines because of the transverse pair-creation opacity(e.g.,Riffert,M´e sz´a ros&Bagoly1989; Ho,Epstein&Fenimore1990)and because gamma rays produced by such mechanisms as curvature radiation and Compton upscattering are strongly beamed alongfield lines (e.g.,Sturrock1986;Dermer1990and references therein).Even locally–isotropic emissions are strongly beamed when they occur in a relativistic outflow channeled by a magneticfield(e.g.,Yi1993).Gamma emissions induced by sheared Alfv´e n waves in a neutron star magnetosphere can also be highly beamed(Melia&Fatuzzo1991;Fatuzzo&Melia 1993).Beaming obviates theγ–γopacity limit for GRBs(Krolik&Pier1991;Baring1993; Fenimore Epstein&Ho1993).The HBM invokes the additional(assumed)property that burster recoil velocities areapproximately aligned with magnetic dipole—and hence burst beaming—axi:−→V r −→µ.This requires that the rotation axis −→Ωis also roughly aligned with−→µ,at least to within theburst opening angleφb.Is −→V r −→µa plausible assumption?Any recoil mechanism which imparts impulses to the stellar surface with a coherence time longer than the rotation period of the star willtend to make −→V r ±−→Ωbecause of “rotational averaging.”One such recoil mechanism isanisotropic neutrino emission during the first ∼10s after formation (§2.4below).If itis also true that −→µ ±−→Ω(at least to within the beaming angle φb )then the alignmentcondition of the HBM is satisfied.Such near–alignment between −→µand ±−→Ωis expected if the neutron star magnetic fieldis generated by large-scale dynamo action,as in familiar stellar and planetary dynamos.The “magnetar”model,described below (§2.3),is one scenario involving such a dynamo.Vacuum magnetic torques increase alignment (Michel &Goldwire 1970;Davis &Goldstein 1970)after the star spins down past the “death line”at which magnetospheric currents are quenched,at age t D ∼105(B dipole /1014G)−1yrs (Chen &Ruderman 1993).Before this point is reached,currents might exert counter-aligning torques of comparable strength (e.g.,McKinnon 1993and references therein).Note that the GRB beaming angle φb is the sum of the intrinsic beaming angle due to gamma-ray opacity and radiative effects,and the r.m.s.scatter in the angle between −→Ωand −→µ.Gamma production mechanisms such as curvature radiation and Compton upscattering could operate at significant altitudes in the magnetosphere,where field linesare tilted with respect to −→µ,yielding larger values of φb than one would estimate under theassumption of near-polar gamma emission (as adopted by Riffert,M´e sz´a ros &Bagoly 1989;Ho,Epstein &Fenimore 1990).Values as large as φb ∼20◦are possible.2.3.Magnetically-powered Bursts?The HBM might apply in a variety of different physical contexts.Here we will briefly discuss the“magnetar”model for GRBs(DT92).The magnetar idea has previously been invoked in models of soft gamma repeater bursts(Thompson&Duncan1995,hereafter TD95)as well as in models of continuous X-ray emissions from SGRs and from anomalous X-ray pulsars like1E2259+586(Thompson&Duncan1996,TD96).Magnetars are hypothetical neutron stars which are born with dipolefields in excess of B Q≡me2c3/e¯h=4.4×1013G.How might such stars form?Neutron stars are hot and convective during thefirst∼10seconds after they form.They also undergo strong differential rotation(TD93).Large-scale dynamo action might operate efficiently during this time for neutron stars with mean rotation periods below a threshold comparable to the convective overturn time,as predicted byα–Ωdynamo theory.There is evidence for such a threshold in magnetically-active main-sequence stars(e.g.,Simon1990).This threshold effect could give rise to a bimodal population of neutron stars(“pulsars and magnetars”) with a factor>∼102difference infield strength(DT92).A more detailed explanation of this magnetar formation hypothesis is given by Duncan&Thompson(1996,DT96).Seven distinct estimates of thefield in the bursting neutron star SGR0526−66seem to indicate B>1014G(TD95).3Magnetars spin down too rapidly to be observed as radio pulsars.DT92conjectured that GRBs areflare-like reconnection events in a galactic halo population of such strongly-magnetized neutron stars.We will show in§4.5that the available magnetic energy is sufficient to power observed GRBs,in the context of the HBM(see also PRR).Magnetic reconnection is a theoretically advantageous energy source for GRBs,for several reasons.Gravitational and nuclear energy releases generally occur in bulk baryonic matter,which has many degrees of freedom into which energy can thermalized and degraded via adiabatic expansion(e.g.,Piran&Shemi1993).Flares in a neutron star magnetosphere, on the other hand,can be“clean,”exciting only photon and pair degrees of freedom to a first rge scale electromotive forces induced by reconnection will generally accelerate pairs,and may produce hard,non-thermal spectra via Compton upscattering, synchrotron emission,and curvature radiation(Sturrock1986).Indeed,GRBs have many qualitative similarities to stellarflares.Both are transient energy releases,with chaotic variability over a wide range of time scales;and both have spectrally-hard non-thermal components(e.g.,Murphy et al.1993;Ramaty&Mandzhavidze1993).The similarities are so strong that a minor fraction of bursts in the BATSE catalog might actually be intense events from nearby,non-neutron,flare stars(Liang&Li1993).Stochastic avalanche models give a goodfit to GRB time profiles(Stern&Svensson1996)and to many properties of solarflares(Lu et al.1993).If the V r–B dipole correlation observed in some samples of radiopulsars(e.g.,Cordes 1986;Stollman&van den Heuvel1986)is applicable for all neutron stars,then the mean magnetar recoil velocity would be>∼10times larger than the mean for radiopulsars(but see Lorimer,Lyne and Anderson1995).Several mechanisms predict unusually large recoils for magnetars,sufficient to propel them into the galactic halo,as explained in§2.4below.Because of the dynamo origins of magnetarfields,one expects that initially −→Ω,±−→V rand±−→µare roughly aligned in magnetars.4As the star spins down,magnetospheric currents might drive some degree of misalignment;however,once the star spins down past the“death line”at time∼105(B dipole/1014G)−1yrs(Chen&Ruderman1993),further spindown certainly enforces alignment(Michel&Goldwire1970;Davis&Goldstein1970), since the magnetostatic stellar distortion in magnetars is large enough to damp nutations of −→Ωabout−→µ(Goldreich1970,DLT).Incidentally,this is probably not true in old,spun-down(P rot>4s)radiopulsars.We conclude that −→V r is likely to be roughly aligned with±−→µinold magnetars,where±−→µis also the axis of beamed gamma emissions(DLT).5 This scenario for classic GRBs assumes that magnetars retain strong dipole magnetic firge-scale magnetic instabilities that reduce B dipole(Flowers&Ruderman1979) might be suppressed by toroidalfield components in the stellar interior,as expected for fields generated viaα–Ωdynamos,or perhaps by other mechanisms(TD93§14.2).Note that a dipolefield anchored in the stably–stratified liquid interior of a magnetar cannot be greatly distorted by spindown-induced crustal tectonic drift(Ruderman1991)because magnetic stresses dominate tensile stresses in the crust.This might differ markedly from the circumstance in ordinary radiopulsars(Ruderman1991).The interactions of vortexlines in the neutron superfluid with superconductingflux tubes are also probably irrelevant for young magnetars,because the interiorfield is probably strong enough to suppress superconductivity.A young magnetar’sfield evolves predominantly via ambipolar diffusion in the interior and Hall fracturing in the crust(TD96).As the interiorfield decays, superconductivity will appear in the mantle and perhaps the core;but this probably happens only after rapid spindown has driven most superfluid vortex lines out of the interior.Further discussion of magnetar evolution is given by PRR.2.4.Neutrino Magnetic RecoilsA dipole anisotropy of only∼0.03in the neutrino emission from a young,hot neutron star would impart a recoil velocity∼1000km s−1to the star(Chugai1984).Here we briefly review mechanisms whereby neutrino anisotropies could be magnetically induced. Purely hydrodynamic(non-magnetic)mechanisms for producing neutron star recoils have been proposed by Janka&M¨u ller(1994),Shimizu,Yamada&Sato(1994),Burrows& Hayes(1996),and in references quoted therein.A strong magneticfield affects neutrino emissions from the beta processes n→p+e−νand p+e−→n¯ν,as calculated by Dorofeev,Rodionov&Ternov(1985),and from neutrino scattering processes as calculated by Vilenkin(1995).Dorofeev et al.and Vilenkin furthermore estimated the neutron star recoils resulting from these processes,in the uniform-field idealization.This is a macroscopic manifestion of parity-nonconservation in the weak interactions.6In a realistically non-uniform magneticfield,the back-reaction of magnetic stresses on convective energyflow,along with the neutrino opacity variations outlined above,would give rise to“neutrino starspots,”analogous to sunspots,and thus produce neutron star recoils of a magnitude estimated in DT92and§13of TD93.These calculations are based on standard Weinberg-Salam weak interaction theory. If neutrinos have mass,on the other hand,a strong magneticfield will shift resonantflavor-changing(MSW)oscillations,thereby also inducing an anisotropy in the emergent neutrinoflux from a nascent neutron star(Kusenko&Segr`e1996).All of these mechanisms produce recoils which vary directly—usually linearly—with the mean magneticfield strength:V r∝B.Thus if any of these mechanisms dominate, one would expect much larger recoils for magnetars than for pulsars.Several non-neutrino recoil mechanisms which also might operate more efficiently in magnetars than in pulsars were discussed by DT92.7To estimate neutrino magnetic recoils realistically,one must know the strength,coherence length and coherence time of the magneticfield during the epoch of maximum neutrino luminosity.This is not possible at present.However,if the magneticfield approaches equipartition with the free energy of differential rotation and/or the convective fluid mixing—which is strongly in the MHD limit—then B>∼1016G at the neutrinosphere (TD93).Such strongfields could be present when most of the neutrino energy is radiated away,even if the surface dipolefield,which is frozen-in tens of seconds later by the onset of stable stratification in the liquid interior(Goldreich&Reisenegger1992),is smaller by a factor of∼10or∼30.Recoils V r>∼103km s−1are plausible.3.Galactic Halo Model ResultsBy integrating a large number(∼106)of neutron star trajectories in a realistic galactic potential,we have derived the sky distribution of HVNSs.In the model described here(§3 and§4),all stars have|V r|=1000km s−1;thus they move in nearly straight lines and eventually escape from the galaxy(but see§6.3).We used a Monte Carlo code developed by Li&Dermer(1992),which in turn follows many of the prescriptions of Paczy´n ski(1990)and Hartmann,Epstein&Woosley(1990). In particular,we adopt van der Kruit’s(1987)model for the spatial distribution of young Pop.I stars which spawn neutron stars in the galactic disk.The trajectories of∼106 neutron stars were numerically integrated in a realistic galactic potential(Miyamoto& Nagai1975)8including a dark halo cutoffat radius R H=70kpc.The escape velocity fromthe center of this model potential is V esc∼600km s−1.This increases only logarithmically with R H,reaching800km s−1for R H=200kpc,thus our results are probably insensitive to R H over its plausible range(LD92).Deviations from sphericity in the dark halo were neglected(but see PRR).We also do not include the potential of M31since stars withV r∼103km s−1are negligibly perturbed by M31within the BATSE sampling depth we found of<200kpc(§4.1).In Figure3we show HBM numerical results for several angular statistics,plotted as functions of sampling depth D about the Earth.That is,thefigure shows cumulative angular statistics for all detectable bursters at distances from Earth that are less than or equal to the value of D on the horizontal axis.The topmost plot of Figure3shows the galactocentric dipole moment cosΘ ,whereΘis the angle between a burst and the galactic center.The second plot shows the disk-like quadrupole, sin2b −1/3,where b is galactic latitude; sin2b <1/3implies that sources are concentrated toward the disk.The third plot shows the galactocentric quadrupole, cos2Θ −1/3.The bottom plot of Figure3 shows V/V max ,a statistic which is related to the slope of the cumulative log N—log P brightness distribution,as explained below.Within each subplot of Figure3,the various lines correspond to different beaming anglesφb as described in thefigure caption.We have cut offtheφb=10◦and5◦curves for D≤10kpc because our Monte Carlo sampling statistics at smaller D are too poor.For example,the number of detectable stars at D≤3kpc in our Monte Carlo model is only ∼55forφb=5◦,whereas it is∼104for in the unbeamed case(φb=90◦).Increasing the sampling depth D(moving to the right in Figure3)is tantamount to including fainter and fainter bursts.Eventually the BATSE sampling depth is reached;atthis point,if the model is tofit observations,all the plotted statistics must simultaneously match BATSE values to within observational uncertainty.The most recent published BATSE results9are plotted in Figure3at a value D=180kpc.Before discussing these results,we must explain the significance of V/V max .The V/V max statistic was invented for the study of the quasars(Schmidt1968),and wasfirst applied to GRBs by Schmidt,Higdon&Hueter(1988).For scintillation counter experiments, V/V max is the average of(C/C min)−3/2over all bursts,where C is the peak counts(in a set time interval)and C min is the threshold for detection.C min can vary with background noise and other effects(e.g.,“overwrites”);however,for a source population that is uniformly distributed in static Euclidean space, V/V max is equal to0.5 regardless of how the threshold varies;and V/V max <0.5indicates that the density of bursters diminishes with distance,for standard-candle sources.Because C min is variable, the V/V max statistic is useful in the study of inhomogeneous data sets only when trying to answer the yes/no question:“Is the observed brightness distribution consistent witha uniform density of sources distributed in Euclidean space?”(e.g.,Band1992;Petrosian 1993).In Figure3,we use V/V max in a purely illustrative way.Our model values of V/V max are ideal values that would be found by an instrument with a uniform detection threshold, i.e.,no variations in the noise or the threshold settings.Since the C min values in the BATSE catalog are not highly variable(Meegan et al.1996)preliminary comparisons with BATSE,as in the bottom panel of Figure3,will not lead us astray.However,the most accurate way to compare burst observations with theory is tofit the observed distribution of peak photonfluxes to Monte Carlo models which have been realisticallyfiltered for detection incompleteness(e.g.,Lubin&Wijers1993).This is what we do in our actual statistical comparisons of the HBM with the BATSE catalog(§4).Note that the model curves for angular statistics in Figure3implicitly assume a detector with uniform sky coverage;i.e.,we have idealized that the detector is equally capable of detecting bursts from any location on the celestial sphere.We have corrected for the imperfect sky coverage of BATSE by shifting the data points in Figure3appropriately (see footnote9).In§4we will take the opposite approach:using the raw BATSE data and filtering the Monte Carlo model to take into account BATSE’s imperfect sky coverage.What can be learned from Figure3?Beaming evidently increases V/V max to nearly 0.5for nearby bursters,D∼30kpc.This can make the model satisfy PVO constraints,as we show quantitatively below.Beaming also evidently reduces cosΘ .Theφb=20◦case fits BATSE observations over an appreciable range of sampling depths D>100kpc.Note that the largest deviations from isotropy in Figure3occur for bright(i.e., small-D)subsets of the observable bursts.A distinctive signature of the HBM is thatcos2Θ −1/3is positive for bright bursts.This can be understood as follows.The(bright) bursters which become visible at Earth before reaching the remote galactic halo are the oneswhich happen to be born with beaming axis−→µ(and hence,with −→V r)pointed approximatelytoward or away from Earth(to within∼φb).Because most bursters are born within the Solar circle in the galactic disk,the brightest ones tend to be seen in that direction and toward the galactic anticenter,if they have already moved past the Earth on their way out of the galaxy.Thus cos2Θ >1/3for bright bursts,while the dipole moment cosΘ remains small.。
英语专业四级听写训练20:Waves

英语专业四级听写训练 20:WavesWavesHow does light get from the sun to the earth? How does music get from the stage to the audience? They move the same way-----in waves! Light and sound are fomp3s of energy. All waves carry energy, but they may carry it differently.Light and sound travel through different kinds of matter.For example, light waves cannot move through walls, but sound waves can. That is why you can hear people talking in another room even though you cannot see them. The energy of some waves is destructive.An earthquake produces seismic waves. Catch a wave. Ask a friend to stand a few feet away from you. Stretch a spring between you. Shake the spring to transfer energy to it. What happens? The spring bounces up and down in waves. When the waves reach your friend, they bounce back to you!Light waves travel 300,000 kilometers (186,000 miles) per second! They can also travel through a vacuum. That is why light from the sun and distant stars can travel through space to the earth!Useful Words and Expressions ;1. destructive 破坏的2. seismic 地震的3. vacuum 真空。
Gravitational waves from hot young rapidly rotating neutron stars
The r-modes of rotating Newtonian stars are generally defined to be solutions of the perturbed fluid equations having (Eulerian) velocity perturbations of the form
ω=−
(l − 1)(l + 2) Ω. l+1
(2.3)
˜ is related to the imaginary Thus the time derivative of E part of the frequБайду номын сангаасncy 1/τ by ˜ ˜ 2E dE =− . dt τ (2.7)
These modes represent large scale oscillating currents that move (approximately) along the equipotential surfaces of the rotating star. The restoring force for these oscillations is the Coriolis force; hence the frequencies of these modes are low compared to the usual f and p−modes in slowly rotating stars. These expressions for δv and ω are the lowest order terms in an expansion in terms of the angular velocity Ω. The exact expressions contain additional terms of order Ω3 . There may exist other modes of rotating barotropic stellar models with properties similar to these classical r-modes; however, our discussion here is limited to the properties of these classical r-modes. The density perturbation associated with the r-modes can be deduced by evaluating the inner product of v (the unperturbed fluid velocity) with the perturbed Euler equation, and the equation for the perturbed gravitational potential [10]: dρ 2l δρ= αR2 Ω2 ρ dp 2l + 1 r l l+1 R
武汉2024年07版小学3年级上册第9次英语第四单元自测题[含答案]
武汉2024年07版小学3年级上册英语第四单元自测题[含答案]考试时间:80分钟(总分:140)B卷考试人:_________题号一二三四五总分得分一、综合题(共计100题)1、填空题:The ancient Romans created a complex system of ________ (法律).2、Who is the main character in "Harry Potter"?A. FrodoB. HarryC. PercyD. Luke3、What is the name of the action where you move your body rhythmically?A. DancingB. SingingC. ActingD. Playing答案: A4、听力题:My aunt enjoys baking ____ (pies).5、听力题:The element with the symbol F is __________.6、填空题:The ocean waves are _______ (汹涌).7、填空题:My favorite thing about nature is ______.8、听力题:The __________ is part of the brain that controls movement.9、填空题:My cousin is very __________ (勤奋).10、What is the capital of New Zealand?A. AucklandB. WellingtonC. ChristchurchD. Hamilton答案:B11、填空题:The tortoise slowly makes its way through the ______ (草地).12、听力题:My dad helps me with my ____ (projects) for school.13、听力题:The car is ___. (parked)14、听力题:I like to _____ with my friends. (hang out)15、听力题:The Earth's crust is constantly being ______ and recycled.16、填空题:The rabbit's hearing is very ______ (灵敏).17、听力题:I see a _____ (工人) fixing the road.18、What is the main purpose of a garden?A. To grow foodB. To decorateC. To relaxD. To entertain答案:A19、听力题:The ______ is a talented musician.20、What is the capital of Brazil?A. BrasíliaB. São PauloC. Rio de JaneiroD. Salvador答案:A21、ers open up in the morning and ______ at night.(有些花在早晨开放,晚上闭合。
theta翻译
theta翻译英文单词:theta中文翻译:Theta (音译,代表希腊字母Θ,表示角度,在数学和物理中常用)使用场景:1. 数学和物理中表示角度的符号。
2. 统计学中用来代表变量的位置参数,通常也称为“中位数”,是一种描述特定数据集的一种常用度量。
3. 在神经科学和心理学中,Theta是脑电波的一种频率范围,通常在4-8 Hz之间。
双语例句:1. In mathematics, theta is commonly used to denote angles, arcs and functions that change by a specific angle.在数学中,theta通常用于表示角度,弧和随着特定角度变化的函数。
2. The median is a type of theta value that is commonly used in statistical analysis.中位数是统计分析中常用的theta值类型。
3. Theta waves are commonly observed in the brain during relaxation, meditation and sleep.Theta波通常在放松、冥想和睡眠期间观察到。
4. The theta rhythm is a well-known phenomenon in neurophysiology.Theta节律是神经物理学中一个广为人知的现象。
5. The theta state of consciousness is associated with deep relaxation and increased creativity.Theta意识状态与深度放松和增强创造力有关。
6. In physics, theta is commonly used to represent the inclination of an object or surface.在物理学中,theta通常用来表示物体或表面的倾角。
Waves,LightandSoundUnitTestWhichofthe…
Use the diagram below to answer questions #8-9:
8. Which Interval represents one full wavelength? a. Point A to Point C b. Point B to Point D c. Point C to Point G d. Point A to Point G
9. Point D represents the ________________ of a transverse wave. a. crest b. trough c. amplitude d. normal
10. The highest parts of a transverse wave are called a. crests. b. troughs. c. amplitudes. d. wavelengths.
1. Which of the following illustrates the particle arrangement of a block of wood? a. Diagram 3 b. Diagram 2 c. Diagram 1 d. None of the above
2. Which of the following illustrates the particle arrangement of oxygen? a. Diagram 3 b. Diagram 2 c. Diagram 1 d. None of the above
Use the diagrams A and B to help you answer questions #16-17:
16. Wave B, when compared to wave A, can be described as having a. high amplitude, low frequency. b. high amplitude, high frequency. c. low amplitude, low frequency. d. low amplitude, high frequency.
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a r X i v:n lin/04529v3[nli n.PS]3J un24ROTATING W A VES IN THE THETA MODEL FOR A RING OF SYNAPTICALLY CONNECTED NEURONS GUY KATRIEL Abstract.We study rotating waves in the Theta model for a ring of synaptically-interacting neurons.We prove that when the neurons are oscillatory,at least one rotating wave always exists.In the case of excitable neurons,we prove that no travelling waves exist when the synaptic coupling is weak,and at least two rotating waves,a ‘fast’one and a ‘slow’one,exist when the synaptic coupling is sufficiently strong.We derive explicit upper and lower bounds for the ‘critical’coupling strength as well as for the wave velocities.We also study the special case of uniform coupling,for which complete analytical results on the rotating waves can be achieved.1.introduction In this work we study rotating waves in rings of neurons described by the Theta model.The Theta model [2,3,5,6],which is derived as a canonical model for neurons near a ‘saddle-node on a limit cycle’bifurcation,assumes the state of the neuron is given by an angle θ,with θ=(2l +1)π,l ∈Z corresponding to the ‘firing’state,and the dynamics described by (1)dθ∂t =1−cos(θ(x,t ))+(1+cos(θ(x,t ))) β+g ΩJ (x −y )s (y,t )dy,(3)∂s (x,t )Partially supported by the Edmund Landau Center for Research in Mathematical Anal-ysis and Related Areas,sponsored by the Minerva Foundation (Germany).12GUY KATRIELwhere J is a positive function and P is defined by∞ l=−∞δ(θ−(2l+1)π).(4)P(θ)=Here s(x,t)(x∈Ω,t∈R)measures the synaptic transmission from the neuron located at x,and according to(3),(4)it decays exponentially,except when the neuronfires(i.e.whenθ(x,t)=(2l+1)π,l∈Z),when it experiences a jump.(2)says that the neurons are modelled as Theta-neurons,where the input I(x,t)to the neuron at x,as in(1),is given byI(x,t)=g ΩJ(x−y)s(y,t)dy.J(x−y)(here assumed to be positive)describes the relative strength of the synaptic coupling from the neuron at x to the neuron at y,while g>0is a parameter measuring the overall coupling strength.The above model,in the case c>0,is the one presented in[2,7].In the case c=0this model is the one presented in[6](Remark2)and[9].We always assume c≥0.When the geometry is linear,Ω=R,it is natural to seek travelling waves of activity along the line in which each neuron makes one or more oscillations and then approaches rest.In[8]it was proven that for sufficiently strong synaptic coupling g,at least two such waves,a slow and a fast one,exist,and also that they always involve each neuronfiring more than one time before it approaches rest,while for sufficiently small g such waves do not exist.It was not determined how many times each neuronfires before coming to rest,and it may even be that each neuronfires infinitely many times.Some numerical results in the case of a one and a two-dimensional geometry were obtained in [7].In this work we consider a different possibility for the spacial geometry:Ω=S1,so the neurons are placed on a ring and our equations are(3)and∂θ(x,t)(5)ROTATING WA VES IN THETA NEURONS3(10)s(x+2π,t)=s(x,t)∀x,t∈RThe integer m(the‘winding number’)is determined by the initial condition θ(x,0),and will be preserved as long as the solution remains continuous.In this geometry,a different kind of wave of activity is possible:a wave that rotates around the ring repeatedly.Such waves,that is solutions of the form:(11)θ(x,t)=φ(x+vt)(12)s(x,t)=r(x+vt)where v is the wave velocity,are the focus of our investigation.In section2we show that in the case that the winding number m=0, there can exist only trivial rotating waves.Thus the interesting cases are when m>0.Here we study the case m=1,the case m>1being beyond our reach.Thus,this work concentrates on thefirst non-trivial case.Our central results about existence,nonexistence and multiplicity of ro-tating waves can be summarized as follows(seefigures1,2for the simplest diagrams consistent with these results):Theorem 1.Consider the equations(5),(3)with conditions(9),(10),and m=1.(I)In the oscillatory caseβ>0:for all g>0there exists a rotating wave, with velocity going to+∞as g→+∞.(II)In the excitable caseβ<0:(i)For g>0sufficiently small there exist no rotating waves.(ii)for g sufficiently large there exist at least two rotating waves,a‘fast’and a ‘slow’one,in the sense that their velocities approach+∞and0,respectively, as g→+∞.Therefore our results bear resemblance to those obtained in[8]for the case of a linear geometry.We note that although for the rotating waves found here each neuronfires infinitely many times,the reason for this is that it is re-excited each time,because of the periodic geometry.During each revolution of the rotating wave,each neuronfires once,so naively one could think that the analogous phenomenon in a linear geometry would be a travelling wave with each neuronfiring once-but this was shown to be impossible in[8]. It is interesting to note that while in[8]some restrictions were made on the coupling function J,like being decreasing with distance,here no such restrictions are imposed beyond(7),(8).We would expect however that some restriction would need to be imposed on J in order to obtain stability of travelling waves.The whole issue of stability remains quite open and awaits future investigation.In the caseΩ=R,both numerical evidence in[7,8]4GUY KATRIELand results obtained in other models[1]indicate that the fast wave is stable while the slow wave is unstable,so we might conjecture that this is true for the case investigated here as well-at least under some natural assumptions on J.Some analytical progress on the stability question in the caseΩ=R has recently been achieved in[9].Let us note that the model considered here,in the caseβ<0,describes waves in an excitable medium,about which an extensive literature exists(see [10]and references therein).However,most models consider diffusive rather than synaptic coupling.In the case of the Theta model on a ring,with diffusive coupling,and m=1,it is proven in[4]that a rotating wave exists regardless of the strength of coupling(i.e.the diffusion coefficient),so that our results highlight the difference between diffusive and synaptic coupling.In section3we reduce the study of rotating waves to the investigation of the zeroes of a function of one variable.In section4we investigate the special case in which the coupling is uniform(J(x)is a constant function), which,although artificial from a biological point of view,allows us to obtain closed analytic expressions for the wave-velocity vs.coupling-strength curves in an elementary fashion.We can thus gain some intuition for the general case,and obtain information which is unavailable in the case of general J, like precise multiplicity results.It is interesting to investigate to what extent the more precise results obtained in the uniform-coupling case extend to the general case,and we shall indicate several questions,which remain open,in this direction.In section5we turn to the case of general coupling functions J,and prove the results of theorem1above,obtaining also some quantitative estimates:lower and upper bounds for the critical values of synaptic coupling coupling strength g,as well as for the wave velocities.2.preliminariesWe begin with an elementary calculus lemma which is useful in several of our arguments below.Lemma2.Let f:R→R be a differentiable function,and let b,c∈R,b=0, be constants such that we have the following property:(13)f(z)=c⇒f′(z)=b.Then the equation f(z)=c has at most one solution.proof:Assume by way of contradiction that the equation f(z)=c has at least two solutions z0<z1.Define S⊂R byS={z>z0|f(z)=c}.S is nonempty because z1∈S.Let z)=c.We have either z=z0,and we shall show that both ofROTATING WA VES IN THETA NEURONS5 these possibilities lead to contradictions.If z)=csign(f′(z0))=sign(f′(z)with f(z2)=c,contradicting the definition of z=z0then z0is a limit-point of S,which implies that f′(z0)=0,contradicting(13).These contradictions conclude our proof.Turning now to our investigation,we note a few properties of the functions h(θ)and w(θ)defined by(6)which will be used often in our arguments: (14)h((2l+1)π)=2∀l∈Z,(15)h(2lπ)=2β,∀l∈Z,(16)w((2l+1)π)=0∀l∈Z,(17)w(2lπ)=2∀l∈Z,Plugging(11),(12)into(5),(3),and setting z=x+vt we obtain the following equations forφ(z),r(z):(18)vφ′(z)=h(φ(z))+gw(φ(z)) π−πJ(z−y)r(y)dy,(19)vr′(z)+r(z)=P(φ(z))(1−cr(z)).In order to satisfy the boundary conditions(9),(10),φand r have to satisfy(20)φ(z+2π)=φ(z)+2πm∀z∈R,(21)r(z+2π)=r(z)∀z∈R.Let usfirst dispose of the case of zero-velocity waves,v=0.We get the equations(22)h(φ(z))+gw(φ(z)) π−πJ(z−y)r(y)dy=0,(23)r(z)=P(φ(z))(1−cr(z)).If there exists some z0∈R withφ(z0)=(2l+1)π,l∈Z,then,substituting z=z0into(22)and using(14),(16),we obtain2=0,a contradiction.Hence we must have(24)φ(z)=(2l+1)π∀z∈R,l∈Z6GUY KATRIELwhich implies that P(φ(z))≡0,so that(23)gives r(z)≡0,and(22)reduces to h(φ(z))≡0,and thusφ(z)is a constant function,the constant being a root of h(θ).This implies,first of all,that the winding number m is0,since a constantφ(z)cannot satisfy(20)otherwise.In addition the function h(θ) must vanish somewhere,which is equivalent to the conditionβ≤0.We have thus provenLemma3.Zero-velocity waves exist if and only if m=0andβ≤0,and in this case they are just the stationary solutionsr(z)≡0φ(z)≡±cos−1 β+1.vThus the assumptions of lemma2,with f=φ,c=(2l+1)π,b=2ROTATING WA VES IN THETA NEURONS7 Having found all possible rotating waves in the case m=0,we can now turn to the case m>0.In fact,as was mentioned in the introduction,we shall treat the case m=1,the cases m>1being harder.By lemma3we know that there are no zero-velocity waves,so we can assume v=0and define1(27)λ=8GUY KATRIELBy lemma2,(35)implies that the equationφ(z)=2l+1has at most one solution for each l∈Z.In particular,sinceφ(0)=π,φ(2π)=3πwe have φ(z)=π,3πfor z∈(0,2π),and by continuity ofφ(z)this implies(33).Let us note that if we knew that for rotating waves the functionφ(z)must be monotone,then lemma5would follow immediately from(32).Question6.Is it true in general that rotating wave solutions are monotone (for m¿0)?Lemma7.Assume(λ,φ,r)satisfy(28),(29)with conditions(30),(31),(32). Thenλ>0.In other words,v>0for all rotating waves with m=1,so the waves rotate clockwise.Of course in the symmetric case m=−1the waves will rotate counter-clockwise.proof:By(32)and(35)we haveφ′(0)=2λ.We have already noted that λ=0.Ifλwere negative,thenφwould be decreasing near z=0,so for small z>0we would haveφ(z)<0,contradicting(33).Our next step is to solve(29),(31)for r(z),in terms ofφ(z).We will use the following important consequence of lemma5:Lemma8.P(φ(z))|(−2π,2π)=12λδ(z).Letχ(z)∈C∞0(R)be a test ing lemma5again we have (37) π−πχ(u)δ(φ(u)−π)du= ǫ−ǫχ(u)δ(φ(u)−π)du,whereǫ>0is arbitrary.In particular,sinceφ′(0)=2λ>0,we may choose ǫ>0sufficiently small so thatφ′(z)>0for z∈(−ǫ,ǫ),so that we can make a change of variablesϕ=φ(u),obtainingǫ−ǫχ(u)δ(φ(u)−π)du= φ(ǫ)φ(−ǫ)χ(φ−1(ϕ))δ(ϕ−π)dϕφ′(φ−1(π))=χ(0)2λ.(38)ROTATING WA VES IN THETA NEURONS9 This proves(36),completing the proof of the lemma.By lemma8we can rewrite equation(29)on the interval(−2π,2π)as(39)r′(z)+(λ+c2δ(z),The solution of which is given by(40)r(z)= 12H(z)),where H is the Heaviside function:H(z)=0for z<0,H(z)=1for z>0. Substituting z=πinto(40)and using(31),we obtain an equation for r(−π)whose solution isr(−π)=12−e−πλ)−1,and substituting this back into(40),we obtain that the solution of(29),(31) which we denote by rλ(z)in order to emphasize the dependence on the pa-rameterλ,is given on the interval(−2π,2π)by(41)rλ(z)=12H(z)) H(z)+(e2πλ+c2λρc(λ),whereρc(λ)=e2πλ−12−1.We note that(43)ρ0(λ)≡1,A fact that considerably simplifies the formulas in the case c=0.The rotating waves correspond to solutions(λ,φ)of the equation (44)φ′(z)=λh(φ(z))+λgw(φ(z)) π−πJ(z−y)rλ(y)dy,withφ(z)satisfying(32)and(45)φ(π)=φ(−π)+2π.To simplify notation,we define(46)Rλ(z)= π−πJ(z−y)rλ(y)dy,10GUY KATRIELso that (44)is rewritten as (47)φ′(z)=λh (φ(z ))+λgR λ(z )w (φ(z )).We note that (47)is a nonautonomous differential equation for φ(z ),and since the nonlinearities are bounded and Lipschitzian,the initial value problem(47),(32)has a unique solution,which we denote by φλ.Rotating waves thus correspond to solutions λ>0of the equation(48)φλ(π)−φλ(−π)=2π.Rewriting (47)and (50)we have(49)φ′λ(z )=λh (φλ(z ))+λgR λ(z )w (φλ(z )),(50)φλ(0)=π,and defining(51)Ψ(λ)=12λρc (λ),so that (49)reduces to(53)φ′λ(z )=λh (φλ(z ))+g 2ππ−πφ′(z )dz 2ρc (λ)w (φ(z ))=1λh (ϕ)+g 2π π−πdϕ2ρc (λ)w (ϕ).(55)ROTATING WA VES IN THETA NEURONS11 Substituting the explicit expressions for h and w from(6),and using the formula(56)1A+Bcos(φ)=1A2−B2(|A|>|B|),(55)becomes(57)1=14λ2β+2gλρc(λ),so that rotating waves correspond to solutions of(57),with their velocities given by v=12λρc(λ).In the following lemma we collect some properties of the functions f c,β(λ), which are obtained by elementary calculus:Lemma9.(i)Whenβ<0,f c,βis positive and convex on(0,∞),and (60)limλ→0f c,β(λ)=∞,(61)limλ→∞f c,β(λ)=∞.(ii)Whenβ≥0,f c,βis decreasing on(0,∞),and(60)holds.Ifβ>0it has a zero atλ=1β,ifβ=0it is positive on(0,∞)and limλ→∞f c,0(λ)=0.From lemma9we conclude that whenβ<0(58)has exactly two solutions if g>Ω(c,β),where(62)Ω(c,β)=minλ>0f c,β(λ),which we will denote byλλc,β(g),no solution if g<Ω(c,β),and a unique solution when g=Ω(c,β).Whenβ≥0,part(ii)of lemma9implies that(58)has a unique solution for any g>0,which we denote byλc,β(g).An elementary asymptotic analysis of the equation(58)yieldsLemma10.(i)Whenβ<0we have the following asymptotics as g→∞(63)2g as g→∞.12GUY KATRIELFor λc,β(g )=112−1)1g +O10,β(g )=1g+O1c,β(g ),given in (64)for c >0and (65)for c =0.We thus obtainTheorem 11.When J ≡1:(I)In the excitable case β<0:(i)If g >Ω(g,c )there exist two rotating waves with velocities given by (66)vv c,β(g )=1c,β(g ),and we have,for the slow wave (67)v21g 3as g →∞,for the fast wave when c >0:(68)π2−1√v 0,β(g )=2g +O1c,β(g )=λc,β(g ),and for large g it has the same asymptotics as in (68),(69)in the cases c >0,c =0,respectively.In the excitable case we thus have two rotating waves born at a supercritical saddle-node bifurcation as the coupling strength g crosses Ω(c,β).ROTATING WA VES IN THETA NEURONS 13246810v12345678gFigure 1.Velocity of waves (v )vs.coupling strength (g )for the case J ≡1,c =0,β=−0.5.We now note that in the special case c =0(the model introduced in [6])we can obtain more explicit ing (43)we havef 0,β(λ)=1−4βλ2|β|.We can also solve (58)explicitly,and obtain the velocities of the rotating waves.When β<0,g >Ω(0,β)vg 2+4β,g 2+4β.When β≥0,for all g >0v 0,β(g )=14GUY KATRIEL246810v12345678gFigure 2.Velocity of waves (v )vs.coupling strength (g )for the case J ≡1,c =0,β=0.5.246810v12345678gFigure 3.Velocity of waves (v )vs.coupling strength (g )for the case J ≡1,c =1,β=−0.5.ROTATING WA VES IN THETA NEURONS 15246810v12345678gFigure 4.Velocity of waves (v )vs.coupling strength (g )for the case J ≡1,c =1,β=0.5.5.The general caseWe now return to the case when J is a general continuous positive 2π-periodic function,and prove that several of the results about rotating waves obtained above for the special case J ≡1remain valid,though the proofs are necessarily less direct.Lemma 12.lim λ→0Ψ(λ)=0.proof:We shall prove that (72)φλ(z )=π+O (λ)as λ→0uniformly in z ∈[−π,π].The lemma follows immediately from this and from (51).When c >0,the claim (72)is immediate,since,using (41),lim λ→0r λ(z )=12H (z ) (e c16GUY KATRIELFor c=0,rλ(z)becomes singular asλ→0,so we need a more refined argument.Forλrλ(z)we have(74)λrλ(z)=12J=1J2λρc(λ)minx∈RJ(x)≤Rλ(z)≤1ρc(λ)≥gρc(λ)≥gROTATING WA VES IN THETA NEURONS17(79)φλ(z)>0∀z∈[−π,0].Together with(51),these imply the result of our lemma.To prove our claim we note that,using(49),(15),(17),part(ii)of lemma13(which is why we need the assumption that J is non-constant)and(77)φλ(z)=0or2π⇒φ′λ(z)=2λβ+2λgRλ(z)<2λβ+gρc(λ)maxx∈R J(x)≤2λβ+2λ|β|=0.(80)We now show that(80)implies(78).If(78)fails to hold,then we setz0=min{z∈[0,π]|φλ(z)=2π}.This number is well-defined by continuity and by the fact thatφλ(0)=π, which implies also that z0>0.By(80)we haveφ′λ(z0)<0,but this implies thatφλ(z)is decreasing in a neighborhood of z0,and in particular that there exist z∈(0,z0)satisfyingφλ(z)=2π.But this contradicts the definition of z0,and this contradiction proves(78).Similarly,assuming(79)does not hold and definingz1=max{z∈[−π,0]|φλ(z)=0},we conclude that z1<0andφ′λ(z1)<0,so thatφλ(z)is decreasing in a neighborhood of z1,and this implies a contradiction to the definition of z1 and proves that(79)holds.This concludes the proof of the lemma.Sincelimλ→∞ρc(λ)=e−c2∀λ>0,we conclude from lemma14thatLemma15.In the excitable caseβ<0,we haveλ≥ge−c2|β|maxx∈RJ(x)⇒Ψ(λ)<1,Let us note that sinceΨ(λ)<1implies that(52)doesn’t hold,and since v=12g.18GUY KATRIELThe following theorem shows that,in the excitable case and for sufficiently weak synaptic coupling,there are no rotating waves(so it implies part(II)(i) of theorem1).Theorem17.In the excitable caseβ<0,if g∈(0,g0),whereg0=Ω(c,β)2|β|ρc(λ)maxx∈RJ(x).We defineµ=β+g2λρc(λ)maxx∈RJ(x) (1+cos(φλ(z)))=λ[(µ+1)+(µ−1)cos(φλ(z))].(85)which implies(note that the integral below is well-defined because of(84))π−πφ′λ(z)dz(µ+1)+(µ−1)cos(ϕ)≤2πλ.If we assume,by way of contradiction,that(82)does not hold,i.e.that φλ(π)−φλ(−π)≥2π,then,using(56),φλ(π)φλ(−π)dϕ(µ+1)+(µ−1)cos(ϕ)=πµ,ROTATING WA VES IN THETA NEURONS19so together with(86)we obtain1µ≤2λ,which is equivalent tog≥12λρc(λ),which contradicts g<g0.This contradiction proves(82),concluding the proof of the theorem.We now proceed to prove that in the excitable case when the synaptic coupling is sufficiently large we have at least two rotating waves(see theorem 20below).Lemma18.In the excitable caseβ<0,if there exists someλ0>0withΨ(λ0)>1,then there exist at least two solutionsλ1,λ2of(52)with0<λ2<λ0<λ1, hence two rotating waves,with velocities satisfyingv1=1λ0<12λfor allλ≥λ′1,and in particular it follows thatλ′1>λ0.Wethus haveλ′2<λ0<λ′1withΨ(λ′2)<1,Ψ(λ0)>1,Ψ(λ′1)<1.Thus by the intermediate value theorem,the equation(52)has a solution λ2∈(λ′2,λ0)and a solutionλ1∈(λ0,λ′1),corresponding to two rotating waves.The following lemma is valid for all values ofβ:Lemma19.Assume thatλ>0satisfies the inequality(87)f c,β(λ)<g minx∈RJ(x),where f c,βis defined by(59).ThenΨ(λ)>1.20GUY KATRIELproof:By(51),our claim is equivalent to(88)φλ(π)−φλ(−π)>2π.We definegη=β+.4λ2Using(49)and lemma13we haveφ′λ(z)=λ[h(φλ(z))+gRλ(z)w(φλ(z))]≥λ 1−cos(φλ(x))+ β+g(η+1)+(η−1)cos(φλ(z))≥2πλ.Making the change of variablesϕ=φλ(z),we obtain (91) φλ(π)φλ(−π)dϕ2π0dϕ√(η+1)+(η−1)cos(ϕ)≤√,min x∈R J(x)whereΩ(c,β)is defined by(62).Then when g>g1,there exist at least two rotating waves.In fact,we have a‘slow’wave with velocity v s bounded from above by(93)v s≤vROTATING WA VES IN THETA NEURONS21 and a‘fast wave’with velocity v f bounded from below by(94)v f≥c,β,2g+O 1πmin x∈R J(x)2−1√g as g→∞.proof:g>g1and(62)imply the existence ofλ>0satisfying(87),hence by lemma19Ψ(λ)>1,so that lemma18implies the existence of two rotating waves.To prove(93),(94),we note that,assuming g>g1,the range of values of λ0for which(87)holds is the intervalλλc,β(g minx∈RJ(x)),where the functionsλλc,βare defined in section4.Thus,applying lemma 18withλ0=λc,β(g min x∈R J(x))−ǫ.Sinceǫ>0is arbitrary,we have a solutionλof(52)withλ≥c,β(g min x∈R J(x))+ǫ,we obtain the existence of a wave with velocity v fsatisfying(94).The estimates(95)-(97)follow from(93),(94)and lemma10.We note that along with the upper bound(95),we have a lower bound for the velocity of the slow wave,given by lemma16.Question21.Derive an upper bound for the velocities of the fast waves(note that(94)gives a lower bound).Question22.Theorems17and20show that several of the qualitative features that we saw explicitly in the case of uniform coupling(section4)remain valid in the general case.It is natural to ask whether more can be said,e.g.,whether22GUY KATRIELthe following conjecture,or some weakened form of it,is true:for any J,there exists a value g crit such that:(i)For g<g crit there exist no travelling waves.(ii)For g=g crit there exists a unique travelling wave.(iii)For g>g crit there exist precisely two travelling waves.The next theorem deals with the oscillatory caseβ>0,as well as the borderline caseβ=0,and in particular proves part(I)of theorem1. Theorem23.Ifβ≥0,there exists a rotating wave solution for any value of g>0,with velocity v bounded from below byJ(x)),(98)v≥v(g minx∈Rwhere v is the function defined by(71),and the asymptotic formulas(96),(97) hold with v f replaced by v.proof:Ifβ>0,then for any g>0the equationJ(x)f c,β(λ)=g minx∈Rhas the unique solutionλc,β(g min x∈R J(x)).Hence,anyJ(x))λ0>λc,β(g minx∈Rsatisfies(87),so that by lemma19Ψ(λ0)>1.On the other hand forλsufficiently small we have,by lemma12,Ψ(λ)<1.Hence there exists a solutionλ∈(0,λ0)of(52).Sinceλ0>λc,β(g min x∈R J(x))is arbitrary,we conclude that there exists a solutionλ≤λc,β(g min x∈R J(x))of(52).Hence a rotating wave with velocity satisfying(98).Question24.Is it true that in the oscillatory caseβ≥0the rotating wave is always unique?We saw that this is the case when J≡1.Finally,we stress the important question of stability of the rotating waves, which remains open:Question25.Investigate the question of stability of the rotating waves,i.e., do arbitrary solutions of(5),(3)approach one of the rotating waves in large time?We conjecture that,at least under some restrictions on J,the rotating wave is stable in the caseβ>0,while in the caseβ<0the fast rotating wave is stable and the slow one is unstable.References[1]P.C.Bressloff,Travelling waves and pulses in a one-dimensional network of excitableintegrate-and-fire neurons,J.Math.Biol.40(2000),169-198.[2]G.B.Ermentrout,Type I membranes,phase resetting curves and synchrony,NeuralComput.8(1996),979-1001.[3]G.B.Ermentrout&N.Kopell,Parabolic bursting in an excitable system coupled witha slow oscillation,SIAM J.Appl.Math.46(1986),233-253.ROTATING WA VES IN THETA NEURONS23 [4]G.B.Ermentrout&J.Rinzel,Waves in a simple,excitable or oscillatory,reaction-diffusion model,J.Math.Biology11(1981),269-294.[5]F.C.Hoppensteadt&E.M.Izhikevich,‘Weakly Connected Neural Networks’,Springer-Verlag(New-York),1997.[6]E.M.Izhikevich,Class1neural excitability,conventional synapses,weakly connectednetworks,and mathematical foundations of pulse-coupled models,IEEE Trans.Neural Networks10(1999),499-507.[7]R.Osan&B.Ermentrout,Two dimensional synaptically generated travelling waves ina theta-neuron neuronal network,Neurocomputing38-40(2001),789-795.[8]R.Osan,J.Rubin&B.Ermentrout,Regular travelling waves in a network of Thetaneurons,SIAM J.Appl.Math.62(2002),1197-1221.[9]J.E.Rubin,A nonlocal eigenvalue problem for the stability of a travelling wave in aneuronal medium,Discrete&Continuous Dynamical Systems10,(2004),925-940.[10]A.T.Winfree,‘The Geometry of Biological Time’,Springer-Verlag(New-York),2001.Einstein Institute of Mathematics,The Hebrew University of Jerusalem,Jerusalem, 91904,IsraelE-mail address:haggaik@。