非均匀磁等离子体中电磁波和电声波耦合传播理论

我们从磁流体力学基本方程出发,给出了计及外加常数磁场情况下规则非均匀等离子体中电磁波和电声波的耦合传播方程。在选用的电子密度剖面下,求解了该方程组的边界值问题,得到了|P_1|和|H_x|的数值解,进而证明了在此基础上我们得到的电磁波和电声波传播的简单近似耦合方程组是可用的。 最后,我们计算了Debye长度和等离子体波长,指出在等离子体鞘套中等离子体波不能辐射出去的主要原因是在鞘套外边界严重的Landau阻尼造成的,并非在激波线强间断处的多次反射结果。 同时,也对所得到的传播耦合方程的普遍性进行了讨论。     

基于JUNO卫星WAVES仪器波动数据的木星磁层哨声波分析研究

等离子体波的空间分布在木星磁层高能电子动力学过程中起着重要的作用.现有大多数对木星磁层哨声波的观测仅限于|λ|≤15°的磁纬范围内,但是最新的JUNO卫星WAVES仪器提供的波动数据使得更高纬度、更广区域范围内的等离子体波动分布研究成为可能.本文通过对JUNO卫星WAVES仪器数据进行分析处理,详细研究了木星磁层哨声波的空间分布特性.观测表明,存在位于高LJ、高磁纬的木星磁层哨声波,它们广泛分布于距木星中心距离35～75个木星半径、磁纬为|λ|≤30°的空间区域.分析研究发现,WAVES仪器观测的木星磁层哨声波幅度一般为几个pT,远小于地球磁层哨声波的强度.木星磁层哨声波幅会随着LJ的增大缓慢增加,也会随着磁纬的减小趋向平缓变化.基于以上观测事实,本文利用指数幂函数分别拟合得到木星磁层哨声波幅随LJ和磁纬变化的经验模型.该模型将有助于精确理解哨声波对木星磁层高能电子动力学过程的重要影响.     

磁层亚暴扩展相的数值模拟

本文用多步隐格式方法,求解包含电阻的磁流体力学方程组,对磁层亚暴扩展相作数值模拟.计算结果展现了亚暴扩展相期间磁尾变化的主要特征.它表明,球向和尾向等离子体流与准稳态重联有关.等离子体团的尾向喷发,致使中性线尾侧电流片内的密度降低,等离子体片变薄.中性线近地侧的等离子体团朝着地球运动,并合并于地球附近的重联区内.     

太阳风湍流和磁层亚暴的一种机制

太阳风的动量涨落将通过磁层边界在磁尾激发磁流体力学波。快磁声波携带扰动能量传到等离子体片中,发展为激波,或者通过激波的相互作用而耗散能量,使等离子体加热。等离子体片中的随机费米加速机制,使麦克斯韦分布尾巴部分的高能量粒子被加速到更高能。在宁静态时,加热、加速与耗散过程平衡。当太阳风的动量或者其涨落较大时,整个加热和加速过程加剧,更多的高能粒子产生,并从等离子体片中逃逸,形成高速的等离子体流注入近地轨道和极区,表现为磁层亚暴过程。利用这种机制,可以解释地球磁层亚暴的定性特征。     

地核中MHD波的惯性模

地球外核处于高温、高压、高密度的等离子体状态,可以支持多种磁流体波的激发和传播。在地核中存在强的环型磁场,沿磁力传播的MHD波受到地球旋转的影响,分成东行的惯性模和西行的磁模,这两种波模具有高度色散的特点。其中西行磁模波与地磁场长期变化和西漂有关。东行惯性模波具有数天到数百天的周期,其磁效应被导电地幔所屏蔽,传不到地表,但它与下地幔物质可能发生力学耦合,在地幔中产生周期变化的力学过程,这种影响可能达及地表并在地表的地球物理现象中表现出来,它可能是某些周期性或韵律性地球物理现象的原因之一。     

太阳等离子体和磁场输出源表面结构的一种MHD模型

以观测到的光球视向磁场、Ｋ－日冕亮度作为输入,以相应的统计结果为约束条件,利用磁流体力学方程组,给出了等离子体及磁场各参数在源表面上的二维分布．其结果与同期的卫星观测数据和已有的统计结果相比较,显示出相当程度的一致性．     

太阳风动量涨落激发磁层亚暴的机制

本文将太阳风涨落传输能量产生磁层亚暴的机制推广到无碰撞等离子体过程。太阳风的涨落在磁层顶激发压缩阿尔文波,并在磁尾的无碰撞等离子体中传播。尾瓣中满足条件β?1,而等离子体片中β≥1,其中β为等离子体压力与磁压之比。这样,快磁声波在尾瓣中几乎不衰减,而在等离子体片中很快衰减,将波动能量耗散在等离子体片中使等离子体加热或者粒子加速。这种机制还表明,磁尾等离子体片中的高能粒子可以由太阳风涨落动能耗散而被加速,不一定是直接源于太阳。     

基于黏弹滑移界面理论揭示套管中模式波的传播特征

目前固井质量评价主要是利用套管中模式波的幅度或衰减变化判断套管与水泥间的胶结状况.在超声测量频段（70~500 kHz）,现有声波测井仪器工作时在套管中激发的模式波类似薄板中的对称兰姆波（拉伸波）或反对称兰姆波（弯曲型兰姆波）.本文将黏弹滑移界面理论应用到套管和水泥的耦合界面,探讨了套管中的准兰姆波（包括拉伸波和弯曲型兰姆波）与套管后物质的耦合方式,拉伸波与套后物质主要以剪切刚度耦合,即便是0.01 mm的微环也会使得拉伸波的衰减明显降低,接近套后是流体时的响应特征;而弯曲型兰姆波与套管后物质主要以法向刚度耦合,这使得在套后胶结轻质水泥时弯曲型兰姆波对微环不敏感,在套后耦合常规水泥时微环的存在又会使得弯曲型兰姆波的衰减明显增强,衰减的增加说明其与套后物质的声耦合更紧密,也表明微环与常规水泥的等效声阻抗适当降低,更有利于弯曲型兰姆波传播时与套后介质实现法向刚度的匹配.拉伸波和弯曲型兰姆波对同一胶结状况的不同响应特征也为固井质量综合评价时区分不同的水泥胶结状况提供了可能.     

基于黏弹滑移界面理论揭示套管中模式波的传播特征

目前固井质量评价主要是利用套管中模式波的幅度或衰减变化判断套管与水泥间的胶结状况.在超声测量频段(70～500 kHz),现有声波测井仪器工作时在套管中激发的模式波类似薄板中的对称兰姆波(拉伸波)或反对称兰姆波(弯曲型兰姆波).本文将黏弹滑移界面理论应用到套管和水泥的耦合界面,探讨了套管中的准兰姆波(包括拉伸波和弯曲型兰姆波)与套管后物质的耦合方式,拉伸波与套后物质主要以剪切刚度耦合,即便是0.01 mm的微环也会使得拉伸波的衰减明显降低,接近套后是流体时的响应特征;而弯曲型兰姆波与套管后物质主要以法向刚度耦合,这使得在套后胶结轻质水泥时弯曲型兰姆波对微环不敏感,在套后耦合常规水泥时微环的存在又会使得弯曲型兰姆波的衰减明显增强,衰减的增加说明其与套后物质的声耦合更紧密,也表明微环与常规水泥的等效声阻抗适当降低,更有利于弯曲型兰姆波传播时与套后介质实现法向刚度的匹配.拉伸波和弯曲型兰姆波对同一胶结状况的不同响应特征也为固井质量综合评价时区分不同的水泥胶结状况提供了可能.     

不同类型日冕物质抛射事件的比较

依据二维磁流体力学方程组 ,在子午面内分别数值模拟了与动量扰动和温度扰动相关的日冕物质抛射事件 （CME） ,并将二者结果进行对比 .结果认为 :二者在事件的空间结构 ,前沿激波的演化 ,暗腔的形成及作用 ,扰动后近日面新喷发物质的特征等方面是相似的 ;但在前沿激波的传播速度 ,强度和径向演化进程 ,暗腔的行为和磁感应强度以及后随等离子体团的密度等方面却不相同 .     

Propagation of normal modes due to impulsive loading to 3-D medium on a rigid basement

Generally, waves in layered media include several surface wave modes showing dispersive properties. These properties often complicate the understanding of the propagation characteristics of elastic waves. In this paper, not only a method for decomposing transient elastic waves into normal modes is presented but also investigations are applied to decomposed normal modes. This method is developed by means of DWFE and the modal superposition method. In the formulation process, transfer functions describing the relationship between the amplitude of normal modes and that of force density are defined. It was found that the propagation properties of the normal modes were well explained by the dispersion curves and transfer functions. From investigations of the normal mode propagation, properties of each normal mode can be discussed.     

Interchange instability as a mechanism of magnetotail current disruption at the magnetic storm recovery phase

The theory of relaxation of geomagnetic depression observed during magnetic storm has been proposed based on the knowledge of the interaction between the Dst index and the magnetotail current. It has been indicated that the disruption of the tail current that was enhanced during the storm main phase can be caused by the interchange instability, which develops in the boundary plasma sheet due to the sheet curvature in the near to the Earth region and due to a sharp, directed toward the curvature center, plasma pressure gradient at the boundary between the plasma sheet and the tail lobe. The dispersion equation and expression for the instability growth rate have been obtained. The theoretically predicted characteristic time of storm depression relaxation τ is ～10 h and is in good agreement with the experimental estimate.     

On the coalescence of twisted flux tubes

Abstract

We study the problem of the coalescence of twisted flux tubes by assuming that the azimuthal field lines reconnect at a current sheet during the coalescence process and everywhere else the magnetic field is frozen in the fluid. We derive relations connecting the topology of the coalesced flux tube with the topologies of the initial flux tubes, and then obtain a structure equation for calculating the field configuration of the coalesced flux tube from the given topology. Some solutions for the two extreme cases of low-β plasma and high-β plasma are discussed. The coalesced flux tube has less twist than the initial flux tube. Magnetic helicity is found to be exactly conserved during the coalescence, but the assumptions in the model put a constraint on the energy dissipation so that we do not get a relaxation to the minimum-energy Taylor state in the low-β case. It is pointed out that the structure equation connecting the topology and the equilibrium configuration is quite general and can be of use in many two-dimensional flux tube problems.     

阿尔文涨落与地球磁层亚暴

本文讨论了一种地球磁层的亚暴机制。当行星际磁场有大的南向分量时,磁层的位形可由基本闭式转变为开式。磁鞘中的阿尔文波可以携带超过10~(18)尔格/秒的能流传入磁层尾部,并将能量耗散于等离子体片中。等离子体片中的粒子被加热和加速后,注入近地空间,产生环电流和极区亚暴。计算了剪切流场中阿尔文波的传播过程,以及磁层中阿尔文波的耗散。将本文的结算与[4]中的结果合在一起,可以说明当行星际磁场转向南时,容易发生地球磁层亚暴,但这两者并非一一对应的关系,行星际磁场没有南向分量时也可以发生地球磁层亚暴。     

ELF plasma waves in hot and cold plasma fluxes observed by Prognoz-8 in the magnetospheric tail

We present Prognoz-8 observations of low-frequency plasma waves (2-105 Hz) associated with plasma fluxes near the outer boundary of the plasma sheet. These plasma fluxes were different from the regular plasma sheet boundary layer and consisted of tailward flowing warm proton and cold oxygen beams accompanied by rather cold electrons (T _e less than 100 eV). Observed plasma characteristics were used in the numerical solution of the dispersion relation for the ion-beam acoustic instability. Detailed analysis shows that this instability can be a source of observed emissions at frequencies up to 25 Hz.     

On the influence of the horizontal component of the earth's rotation on long period waves

Abstract

A general linearized wave equation for a stratified rotating fluid is derived and applied to obtain a dispersion relation for waves of short latitudinal extent in a thin shell of fluid. Long period wave solutions in three ocean models are compared: (1) for a stratified ocean with both components of the rotation vector; (2) for a stratified ocean without the horizontal component of rotation, and finally, (3) for a homogeneous ocean without horizontal rotation. The inclusion of the horizontal component of the Earth's rotation is found to have no noticeable effect on the dispersion relation of long period waves; its only influence is the introduction of a vertical phase shift in the motions. The origin of this phase shift is found in the tendency of the motions to satisfy the Taylor-Proudman theorem. The phase shift is of possible oceanographic relevance only for bottom-trapped buoyancy waves in a relatively weak stratification. The differences between the three ocean models are also discussed with the help of graphs of the numerically integrated dispersion relations. The relative influences of shell thinness and stratification in inhibiting the influence of the horizontal component of the earth's rotation are also briefly discussed.     

Sausage mode instability of thin current sheets as a cause of magnetospheric substorms

Observations have shown that, prior to substorm explosions, thin current sheets are formed in the plasma sheet of the Earth’s magnetotail. This provokes the question, to what extent current-sheet thinning and substorm onsets are physically, maybe even causally, related. To answer this question, one has to understand the plasma stability of thin current sheets. Kinetic effects must be taken into account since particle scales are reached in the course of tail current-sheet thinning. We present the results of theoretical investigations of the stability of thin current sheets and about the most unstable mode of their decay. Our conclusions are based upon a non-local linear dispersion analysis of a cross-magnetic field instability of Harris-type current sheets. We found that a sausage-mode bulk current instability starts after a sheet has thinned down to the ion inertial length. We also present the results of three-dimensional electromagnetic PIC-code simulations carried out for mass ratios up to M_i/m_e = 64. They verify the linearly predicted properties of the sausage mode decay of thin current sheets in the parameter range of interest.     

Acoustic gravity wave growth and damping in convecting plasma

The propagation of acoustic gravity waves through steadily convecting plasma in the thermosphere has been analysed theoretically. The growth and damping rates of internal gravity waves due to the feedback effects of wave-modulated Joule heating and Laplace forcing have been calculated. It is found that large convection flow velocities lead to the growth of large-scale internal gravity waves, whilst small- and medium-scale waves are heavily damped, under similar conditions. It has also been shown that wave growth is favoured for waves travelling against the plasma flow direction. The effects of critical coupling when wave phase speeds match the plasma flow speed have also been investigated. The results of these calculations are discussed in the context of the atmospheric energy budget and thermosphere-ionosphere coupling.