赤道面磁层顶位形的磁流体力学模拟研究

磁层顶位置和形状的动态特征描绘是地球物理和空间物理研究的难点之一.文章基于太阳风-磁层-电离层耦合的全球磁流体力学（MHD）数值模拟,运用电流密度极大法确定磁层顶位形,并具体研究两种典型太阳风动压（D_p）和几种不同行星际磁场的z分量（B_z）条件下,地球赤道面上方磁层顶动态特征.模拟结果显示,磁层顶日下点高度r₀主要由D_p控制.随着D_p增加,磁层顶被压缩,r₀显著减小.相同D_p条件下,在B_z由南向（B_z<0）逐渐减小,并转为北向（B_z>0）逐渐增大的过程中,r₀缓慢增大.不同条件下,磁层项张角φ变化较小,反映了赤道面磁层顶结构的相似性.与Shue98低纬磁层顶经验模型比较,MHD模拟能再现磁层顶日下点位置r₀对D_p的响应,而r₀随B_z变化的饱和性仅出现在低速太阳风条件下.MHD模拟和经验模型的磁层项张角φ差别小于2.5°,但模拟显示φ随B_z的变化趋势并非简单线性关系.     

任意多个磁层的层状结构中MSFVW和MSBVW的通用色散方程

本文研究了有限宽度及磁各向异性的多磁层结构内的静磁前向体波(MSFVW)色散方程随磁层增加的变化规律。引进三个自定义函数之后,得到了任意多个磁层的层状结构中的MSFVW通用色散方程。用类似的方法,导出了任意多个磁层的层状结构中的静磁反向体波(MSBVW)的通用色散方程。 关键词：     

月球微磁层的探测

近月空间环境中的等离子体特性是嫦娥一号及二号卫星的重要科学探测目标之一.基于嫦娥卫星上搭载的太阳风离子探测器(SWID)的测量结果,文章作者对月球表面磁异常结构(LMA)与太阳风相互作用这一空间科学中的热点问题进行了探索,并通过质子相空间分布的信息,初步确认了磁异常结构可以对入射原始太阳风起到屏蔽及加热的作用,形成所谓的"微磁层"结构.这是国际上为数不多的微磁层存在证据之一.文章作者期待这一研究(及后续工作)将不仅对月球表面空间风化效应的研究产生推动作用,同时也将有助于百公里尺度上(即质子回旋半径与宏观尺度相当条件下)的磁层物理学研究的发展.     

50年来的中国电离层物理研究

简要叙述了电离层物理这门基础学科的主要研究对象和领域,强调电熟层研究应作为整个日地２环境的一部分,从它与太阳和行星际空间、磁层、热层和中低层大气相互作用角度开展整体的研究,描述了电离层、磁层和中性大气耦合过程的基础图像。对我国电离层研究概况和现状,从探测、形态资料分析、模式建立、物理过程机制研究、新技术应用等几个方面作了介绍,并对某些重要的进展和特色加以简要的评述,同时也特别强调了大力加强我国电离     

磁层顶中的低混杂漂移不稳定性

本文讨论了具有简单结构磁层顶中的低混杂漂移不稳定性,假定在磁层顶中磁场方向是相互平行的,电子与离子的密度处处相等,总压力为一常数,采用1971年Alpers建立的分布函数做为零级分布,计算了下混杂漂移不稳定性的增长率和饱和时相应的反常电阻,计算表明,当磁层顶厚度接近两个质子迴旋半径时,低混杂漂移不稳定性的增长率约为0.26ω_LH(ω_LH为低混杂频率),反常电阻率为10^-5sec,随着磁层顶厚度成倍增加,反常电阻率以指数形式下降。 关键词：     

磁性金属多层膜中的巨磁电阻效应

在许多磁性金属多层膜系统中都存在巨磁电阻效应，这些系统是由厚度为几个纳米的磁层与非磁层交替重叠构成，出现巨磁电阻效应的必要条件是系统的磁化状态能被外加磁场所改变。该效应的物理是传导电子在界面处或磁层内的所谓自旋相关散射，层间耦合随隔离层厚度变化而振荡的现象，在隔离层为非磁过渡金属和贵金属的系统中普遍存在，自旋阀多层结构在信息存储技术中磁电阻“读出”头方面极具应用前景。     

地球等离子体模式及遥感成像技术

地球等离子体层的分布主要受到地球磁层的特性影响。早期对地球磁层的研究,主要是通过采集地磁平静期的观测数据,建立半经验模型和经验模型来研究。随着成像技术的发展,可以通过遥感成像的方式,在全球尺度下获得磁扰期、平静期等不同时刻的地球等离子层分布信息,从而更直观、全面地了解磁层磁场的变化。本文研究了现有的地球等离子体层模型,详细阐述了不同地球等离子层模型的描述形式、应用特性,以及地球等离子体层遥感成像观测的方法和手段。最后,通过计算机模拟了在经验地球等离子层模型输入情况下,极轨道卫星对地球等离子体层分布的成像结果。     

地球磁层将现裂缝太阳风暴乘机袭来

2007年6月,美国发射的THEMIS卫星组就发现太阳喷射的带电粒子湍流凶猛涌入磁层裂缝,速度高达每小时160万千米,裂缝维持了一个多小时。这些高能粒子引起的磁暴,增加电网损耗、影响通讯,甚至导致电网瘫痪、供电中断,严重损毁卫星设备。磁层是地球周围的一个泡状磁场,它保护地球上的一切免受太阳风的侵袭。当地球和太阳磁场方向相反时,磁层就会出现裂缝,大量太阳风粒子乘虚而入,数量将超过平时的20倍。     

磁电子学讲座第三讲 磁性金属多层膜中的巨磁电阻效应

在许多磁性金属多层膜系统中都存在巨磁电阻效应，这些系统是由厚度为几个纳米的磁层与非磁层交替重叠而构成．出现巨磁电阻效应的必要条件是系统的磁化状态能被外加磁场所改变．该效应的物理原因是传导电子在界面处或磁层内的所谓自旋相关散射．层间耦合随隔离层厚度变化而振荡的现象，在隔离层为非磁过渡金属和贵金属的系统中普遍存在．自旋阀多层结构在信息存储技术中磁电阻“读出”头方面极具应用前景．     

短脉冲强激光驱动磁重联过程的靶后电势分布特征

超短超强激光因其极端的物理参数范围以及可用于研究相对论等离子体等特征,成为当前激光驱动磁重联物理的研究热点.通常采用两路激光与平面靶相互作用实现激光驱动磁重联,然而在实验诊断中,由于激光等离子体自身的复杂性导致很难辨别磁重联的物理特征.本文对两路短脉冲激光驱动平面靶磁重联进行了数值模拟,重点分析了靶后电势分布特征和磁重联之间的关系.模拟结果显示,靶后电势分布可以直接影响被加速离子在探测面上的空间分布,因此可用来直接诊断短脉冲激光驱动磁重联实验.     

Ion-pressure equations derived from measurements in space

Cluster measurements at the bow shock, the magnetosheath, and the magnetospheric boundary layer are used to derive ion-pressure equations for hot anisotropic plasmas. It is demonstrated that both perpendicular and parallel ion pressures are well approximated by polybaric expressions is proportional to N(gamma)B(kappa), where N is the plasma density, B is the magnetic field, gamma is in the range 0.5 to 2, and kappa is between -2 and 0. The parameters derived from observations are distinctively different from those predicted by double-adiabatic theory and are shown to hold for pressure variations over 4 orders of magnitude and for a range of plasma beta (ratio of kinetic/magnetic pressures) between 10(-4) and 10. The results are relevant for simulations and theories of astrophysical, solar, interplanetary, and magnetospheric processes based on MHD equations.     

Competing mechanisms of plasma transport in inhomogeneous configurations with velocity shear: the solar-wind interaction with earth's magnetosphere

Two-dimensional simulations of the Kelvin-Helmholtz instability in an inhomogeneous compressible plasma with a density gradient show that, in a transverse magnetic field configuration, the vortex pairing process and the Rayleigh-Taylor secondary instability compete during the nonlinear evolution of the vortices. Two different regimes exist depending on the value of the density jump across the velocity shear layer. These regimes have different physical signatures that can be crucial for the interpretation of satellite data of the interaction of the solar wind with the magnetospheric plasma.     

Dynamics of the Magnetospheric Cyclotron ELF/VLF Maser in the Backward-Wave-Oscillator Regime. I. Basic Equations and Results in the Case of a Uniform Magnetic Field

We consider the nonlinear dynamics of absolute instability of whistler-mode waves in the Earth's magnetosphere in the presence of a step-like deformation in the distribution function of energetic electrons. Development of this instability, implying the transition of the magnetospheric cyclotron maser to the regime of a backward-wave oscillator (BWO), was proposed earlier as a generation mechanism of magnetospheric chorus emissions. We derive simplified nonlinear equations describing the dynamics of the magnetospheric BWO in the case of low efficiency of wave-particle interactions. Numerical simulations of these equations confirm qualitative similarity of the laboratory and magnetospheric BWOs and justify quantitative estimates of parameters of chorus emissions. __________ Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 48, No. 9, pp. 719–729, September 2005.     

First and second order non-equilibrium phase transition and evidence for non-extensive Tsallis statistics in Earth’s magnetosphere

In this paper strong evidence is provided for significant far from equilibrium phase transition processes in the Earth’s magnetosphere as revealed by the nonlinear analysis of in situ observations. These results constitute the solid base for the solution of the durable controversy about the chaotic or non-chaotic character of the magnetospheric dynamics. During the last two decades the concept of low dimensional chaos was supported by theoretical and experimental methods by our group in Thrace and others scientists, as an explicative paradigm of the magnetospheric dynamics including substorm processes. In parallel, the concept of self-organized criticality (SOC) and space-time intermittency was introduced as new and opposing to low dimensional chaos concepts for modeling the magnetospheric dynamics. Novel results concerning the nonlinear analysis of in situ space plasma data (magnetic-electric field, energetic particles and bulk plasma flow time series) obtained by the Geotail spacecraft presented in this paper for the first time reveal the following: (a) Coexistence of SOC and chaos states in the magnetospheric system and global phase transition from one state to the other during substorms. (b) Strong intermittent turbulent character of the magnetospheric system at the SOC or the low dimensional chaos states. (c) Clear indications for non-extensivity and q-Gaussian statistics during periods of low dimensional and chaotic dynamics of the magnetosphere. (d) Low dimensional and nonlinear space plasma dynamics in the day side magnetopause and bow shock dynamics. The dual character of the magnetospheric dynamics including low dimensional chaotic (coherent) and high dimensional turbulent states, as supported in this paper, is in agreement and verifies previous theoretical and experimental studies.     

Strong cosmic ray cutoff rigidity decreases during great magnetospheric disturbances

The theoretical and experimental cosmic ray cutoff rigidities during great magnetospheric disturbances in November 2004 and May 2005 have been determined. The theoretical geomagnetic cutoffs were calculated by the trajectory tracing method in the magnetic field of Tsyganenko’s magnetospheric model T03, which describes great magnetospheric disturbances (at Dst < 65 nT). The experimental geomagnetic cutoffs were determined by the spectrographic global survey method on the basis of the world network data. The cutoff rigidity decreases at Dst minima can reach 70–80% for theoretical cutoffs and ～40% for experimental cutoffs at mid latitudes.     

Une nouvelle approche pour les sous-orages magnétosphériques

In a previous report we had started a systematic study of the ballooning modes as the natural waves of the magnetospheric turbulence, substorm and reconnection. After many new results following from the very high mirror ratio of the magnetospheric plasma, summarized in this note, we explain the fundamental role of ion cyclotron instabilities generated by the closure of confinement currents, by field-aligned currents in a three-dimensional (3D) configurations resulting from the growth phase and (or) ballooning modes. These instabilities destroy the current system, dipolarize the magnetic field and are consequently the non linear missing piece of substorm phenomenology. An indirect proof of this theory (apart from observational evidence) is found in the fast heating of electrons, the so-called `dispersionless injection' and a smaller effect on the proton population (diffusion coefficients are in the minutes time scale for protons and seconds for electrons!). This magnetospheric mechanism is very likely operating in solar flares and is in fact an added stone to a 3D time-dependent reconnection and acceleration.     

Numerical evidence of undriven, fast reconnection in the solar-wind interaction with earth's magnetosphere: formation of electromagnetic coherent structures

We give evidence for the first time of the onset of undriven fast, collisionless magnetic reconnection during the evolution of an initially homogeneous magnetic field advected in a sheared velocity field. We consider the interaction of the solar wind with the magnetospheric plasma at low latitude and show that reconnection takes place in the layer between adjacent vortices generated by the Kelvin-Helmholtz instability. This process generates coherent magnetic structures with a size comparable to the ion inertial scale, much smaller than the system dimensions but much larger than the electron inertial scale. These magnetic structures are further advected in the plasma in a complex pattern but remain stable over a time interval much longer than their formation time. These results can be crucial for the interpretation of satellite data showing coherent magnetic structures in the Earth's magnetosheath or the magnetotail.     

Global magnetohydrodynamic simulations of the magnetosphere

The authors demonstrate the use of a global MHD (magnetohydrodynamic) simulations to study the magnetospheric configuration by reviewing some of the results obtained from the Ogino model. The authors start by considering the steady-state configuration of the magnetosphere in the absence of an IMF (interplanetary magnetic field), and then demonstrate how that configuration is changed when a northward or southward IMF is introduced. It is noted that the magnetosphere is very dynamic and since global MHD simulations are intrinsically time-dependent, they offer the possibility of modeling the time-sequence of events in the magnetosphere. Finally results of a calculation in which a magnetospheric substorm is modeled are presented     

Magnetospheric dynamics during the storm of February 14, 2009

The structure of the magnetic field in the magnetospheric during the storm of February 14, 2009 is studied. The model parameters that characterize the magnetospheric magnetic field are calculated every hour on the basis of solar wind data and the evolution of the magnetic field during the storm is reproduced using the A2000 model of the Earth’s magnetosphere. It is shown that extremely quiet geomagnetic conditions in 2009 promoted the expansion of the magnetosphere and were favorable for the formation of magnetic-island-like structures (plasmoids) in the geomagnetic tail. It is ascertained that negative variations in the B_z component could occur in the nightside magnetosphere in situations where the magnetic flux through the tail lobes exceeded certain thresholds, which depend on the parameters of the magnetospheric current systems. It is shown that the formation of magnetic islands decreases the magnetic flux through the tail lobes and prevents excessively strong development of the magnetic field in the tail.     

Electrodynamics of solar wind-magnetosphere-ionosphere interactions

The authors present a coherent picture of fundamental physical processes in three basic elements of the SW-I (solar wind-magnetosphere-ionosphere) coupling system: (i) the field-aligned potential structure which leads to the formation of auroral arcs; (ii) the magnetosphere coupling which leads to the onset of magnetospheric substorms; and (iii) the solar wind-magnetosphere dynamo which supplies the power for driving various magnetospheric processes. The field-aligned potential structure on auroral lines is forced into existence by the loss-cone constriction effect when the upward field-aligned current density exceeds the loss-cone thermal flux limit. The substorm onset occurs when the ionosphere responds fully to the enhanced magnetospheric convection driven by the solar wind. The energy is transferred from the solar wind to the magnetosphere by a dynamo process primarily on open field lines