A fast tearing mode instability driven by agyrotropic electron pressure

The collisionless plasma environment at the current sheet of the Earth’s magnetotail is subjected to fast dynamic evolutions such as tearing instability. By considering agyrotropic pressure for electron and ion components of a collisionless plasma, we analytically investigate the dynamics of tearing mode instability, in which, breaking the frozen-in condition can either be provided by the electron inertia or by agyrotropic electron pressure. A set of linearized Hall-Magnetohydrodynamic (MHD) equations describes the evolution of tearing mode in a sheared force-free field. The presented scaling analysis shows that if the plasma-β$\beta$ exceeds a specified value, then the main mechanism of magnetic reconnection process is the nongyrotropic electron pressure. In this regime, the role played by agyrotropic ion pressure inside the reconnection layer is out of significance. Therefore, the electron-MHD framework, adequately, describes the dynamics of tearing instability with a growth rate which is much faster compared to the cases with a dominated bulk inertia or a gyrotropic plasma pressure.     

Gamma-ray astronomy and cosmic ray origin problem

We analyse the results of the nonlinear kinetic theory of cosmic ray (CR) acceleration in supernova remnants (SNRs) in order to describe their relevant properties: the remnant dynamics and the characteristics of nonthermal emission produced by CRs. It is shown that the theory fits the existing data in a satisfactory way and that the magnetic field in SNRs is significantly amplified due to efficient acceleration of the nuclear CR component. From the fact that magnetic field amplification occurs in all the young SNRs for which relevant data exist, and given the strong theoretical connection between magnetic field amplification and efficiently accelerating the nuclear CRs, we tentatively conclude that the Galactic SNRs are the source population of the Galactic CRs. Due to high interior magnetic fields in young SNRs the π⁰-decay γ-rays generated by the nuclear CR component as a rule dominate over γ-rays generated by the electron CR component, and the calculated γ-ray flux fits existing data.     

Model of the slot region of earth''s electron radiation belt depending on the heliospheric parameters

Relativistic electrons in the slot region of Earth's electron radiation belt are studied using CORONAS-I satellite data obtained in March–May 1994. The strong shifts of the slot latitudinal location (from L≈3 to L≈2) were found. These shifts are associated with the Earth crossing sector boundaries formed by sector corotating structures of the solar wind and interplanetary magnetic field (IMF). The quantitative analysis of the relationship between properties of the slot region and values of the solar wind and IMF parameters was undertaken. The empirical model of the slot region dynamics was developed by means of Artificial Neural Network (ANN).     

存在初始引导场情况下的无碰撞磁场重联

采用二维三分量的全粒子模拟方法研究了不同初始引导场情况下的无碰撞磁场重联及初态为一维的Harris电流片.结果表明,Bz0＞0.5B0的强引导场不仅会显著改变粒子的运动轨迹,而且会改变重联区附近的电场和流场结构,从而影响重联率和电子加速.运用广义欧姆定律解释了不同引导场下电场的结构特征.另外,通过对扩散区附近束流电子的跟踪研究发现,在二维模型中,不论引导场强弱,位于扩散区中心垂直模拟平面的感应电场对电子加速起主要作用,而扩散区外平面电场的贡献很小.      

On the nature of coronal loops above the quiet sun network

The structure and dynamics of a box in a stellar corona can be modeled employing a 3D MHD model for different levels of magnetic activity. Depending on the magnetic flux through the surface the nature of the resulting coronal structures can be quite different. We investigate a model of an active region for two sunspots surrounded by magnetic field patches comparable in magnetic flux to the sunspots. The model results in emission from the model corona being concentrated in loop structures. In Gudiksen and Nordlund (2005) the loops seen in EUV and X-ray emission outline the magnetic field, following the general paradigm. However, in our model, where the magnetic field is far from a force-free state, the loops seen in X-ray emission do not follow the magnetic field lines. This result is of interest especially for loops as found in areas where the magnetic field emerging from active regions interacts with the surrounding network.     

近地轨道集群航天器电磁编队飞行非线性反馈控制方法

针对近地轨道集群航天器电磁编队飞行的动力学和控制问题, 提出了一种非线性反馈控制方法. 基于电磁力模型和地磁场模型, 分析了地磁场对近地轨道电磁编队的影响; 建立了集群航天器电磁编队高精度相对轨道动力学模型; 基于Lyapunov稳定性理论设计了一种非线性反馈控制律, 利用该方法对两星电磁编队维持控制进行了仿真验证. 仿真结果表明, 地磁场引起的电磁干扰力可以忽略, 但是电磁干扰力矩的影响必须考虑; 近地轨道集群航天器电磁编队是可控的, 所设计的控制方法是可行的.      

电磁航天器编队位置跟踪自适应协同控制

通过引入一致性理论针对电磁航天器编队相对位置协同控制问题设计了自适应协同控制器。分析了电磁航天器编队的基本原理,建立了电磁航天器编队相对运动精确的非线性动力学方程。基于电磁力远场计算模型的不确定性,对相对运动动力学模型进行了修正。在电磁力计算模型不确定和航天器间存在通信时延的条件下,对位置跟踪控制的目标设计了自适应协同控制器。考虑到电磁航天器磁矩产生能力的不同,给出了通过优化进行磁矩分配的方案。通过仿真表明:所设计的自适应协同控制器不仅实现了对期望轨迹的准确跟踪,而且相比人工势函数法,暂态维持编队构型的能力提高了4.9倍,并且所给出的磁矩分配方案实现了磁矩的合理分配。     

Wobble of a spin stabilized satellite with cross products of inertia and magnetic attitude control

Asymmetrical spin stabilized satellite dynamics in the vicinity of the required motion is considered. The principal axis of the maximum moment of inertia slightly deviates from its assumed direction in the satellite reference frame. This is formalized in the cross products of inertia. This inertial uncertainty results in a wobble, that is undesired angular velocity components perpendicular to the rotation axis, and oscillations of this axis near the required direction. The torque-free motion is investigated first. Expressions that explicitly relate satellite inertia parameters to wobble are provided. Wobble evolution under the action of magnetic damping control is analyzed next. Its amplitude approximate exponential decay behavior and residual unavoidable wobble level are derived. These expressions are compared with numerical simulation results of nonlinear equations of motion including various disturbance sources.     

Nonlinear quantum ion acoustic shock wave dynamics with exchange-correlation effects

The dynamics of linear and nonlinear electrostatic shock excitations is studied in homogeneous, unmagnetized, unbounded and dissipative quantum plasma consisting of electrons and ions. The dissipation in the system is taken into account by incorporating the ion kinematic viscosity. The system is modelled using the quantum hydrodynamic equations in which the electrons are significantly affected by the quantum forces, viz., the quantum statistical pressure, the quantum Bohm potential and electron exchange-correlations due to electron spin. In the weakly nonlinear limit, using reductive perturbation method deformed Korteweg-de Vries Burgers’s (KdVB) equation, which elegantly combines the effects of nonlinearity, dispersion and dissipation is derived. It is found that the present model predicts the existence of both nonlinear oscillatory and monotonic shock structures. The temporal evolution, stability and phase-space dynamics of nonlinear ion acoustic shocks are investigated numerically to elucidate the effects of quantum diffraction, electron exchange correlation and ion kinematic viscosity.     

Electrostatic Structure of the Electron Phase-space Holes Generated by the Electron Two-stream Instability with a Finite Width

Space satellite observations in an electron phase-space hole (electron hole) have shown that bipolar structures are discovered at the parallel cut of parallel electric field, while unipolar structures spring from the parallel cut of perpendicular electric field. Particle-in-cell (PIC) simulations have demonstrated that the electron bi-stream instability induces several electron holes during its nonlinear evolution. However, how the unipolar structure of the parallel cut of the perpendicular electric field formed in these electron holes is still an unsolved problem, especially in a strongly magnetized plasma (Ω_e > ω_pe, where Ω_e is defined as electron gyrofrequency and ω_pe is defined as plasma frequency, respectively). In this paper, with two-dimensional (2D) electrostatic PIC simulations, the evolution of the electron two-stream instability with a finite width in strongly magnetized plasma is investigated. Initially, those conditions lead to monochromatic electrostatic waves, and these waves coalesce with each other during their nonlinear evolution. At last, a solitary electrostatic structure is formed. In such an electron hole, a bipolar structure is formed in the parallel cut of parallel electric field, while a unipolar structure presents in the parallel cut of perpendicular electric field.      

Current collection through the transport of electrons across magnetic field lines

Collection of electrons by a long conducting cylinder in a flowing plasma is studied by means of numerical simulations. The plasma flow simulates the relative motion between a spacecraft and plasma. The sheath structures and the levels of electron current collections for the cases with and without an ambient magnetic field ( ) are studied. It is found that for the flow perpendicular to the magnetic field, the current is considerably enhanced depending on the relative drift velocity. In the case of a non-zero magnetic field perpendicular to the cylinder axis, the potential structure is a two-dimensional double layer with dimensions L L_|, where L and L_| are the dimensions perpendicular and parallel to , respectively. L is found to be the current limiting radius given by the Parker-Murphy model. For the flow along , the electron current is found to be smaller than that for the flow perpendicular to . This is explained in terms of the potential structures.     

Electron acoustic solitary waves in the Earth’s magnetotail region

Satellite observations have revealed solitary potential structures in the Earth’s magnetotail region. These structures have both positive (compressive) and negative (rarefactive) electrostatic potentials. In this paper we study the electron-acoustic solitary waves (EASWs) in an unmagnetized plasma consisting of cold plasma electrons and isothermal ions with two different temperatures. Using the reductive perturbation method, the nonlinear evolution of such structures is studied. The numerical computations are performed to study the role of two temperature ions in the generation of EASWs. In this case, the model supports the existence of both positive and negative electrostatic potentials with bipolar pulses. The electric field associated with these positive and negative solitary structures are numerically computed. The present study could be useful to construe the compressive and rarefactive electric field bipolar pulses associated with the BEN type emissions in the magnetospheric regions where the electron beams are not present.     

Solar wind-driven electron radiation belt response functions at 100-min time scales

We present a simple yet numerically robust technique, using autoregressive linear filters, to remove unwanted “colored noise” from solar wind and radiation belt electron data at sub-daily resolution. The remaining signal is then studied using finite impulse response linear prediction filters to represent the driven portion of the linear dynamics that describe the coupling between solar wind speed and electron flux. Sub-daily resolution response profiles covering magnetic L-shells between 1.1 and 8.0 R_E are presented which are consistent with daily resolution response functions. Namely, while there is strong global coherence governing electron flux dynamics, there are at least two distinct responses. The first response is an immediate dropout of electrons between L = 4 and L = 7 that is at least a partly adiabatic effect associated with enhancements in the ring current. This is followed by a 1–2 day delayed enhancement across the same L-shells that is likely a result of increased radial diffusion. The second response is an immediate enhancement seen between L = 3 and L = 4 with a typical duration of less than one day. Plausible explanations for this second response are briefly discussed, but neither empirical nor theoretical evidence can establish conclusively a definite physical cause. Finally, the response profiles show significant solar cycle and seasonal dependencies, indicating that better model output might be achieved with: (1) additional simultaneous solar wind inputs; (2) more sophisticated dynamical model structures capable of incorporating non-linear feedback; and/or (3) time-adaptive linear filters that can track non-stationary dynamics in time.     

太阳米波噪暴：哨声模式

本文以日冕活动区磁结构演化为噪暴现象的驱动力,并假定日冕活动区在磁学上是不均匀的——存在强磁场纤维,提出了太阳米波噪暴的哨声模式.活动区磁结构的演化将在冕弧中产生弱激波.当弱激波通过强磁场纤维时,加热部分电子,被加热的电子在强磁场纤维中形成损失锥分布.在日冕的噪暴区域中,快速电子的损失锥分布将产生高亮度的哨声波和朗缪尔波.通过感应散射,朗缪尔波滑向低波区域时将与哨声波发生强烈的互作用而产生窄束电磁辐射(Ⅰ型爆发).强磁场纤维及相应的场位形决定了Ⅰ型爆发的频宽和持续时间.而噪暴连续谱则采用通常认为的各同向电子产生的朗缪尔波与低频波耦合的产物.     

Mini-magnetosphere: Laboratory experiment,physical model and Hall MHD simulation

Magnetosphere with a size comparable to the ion kinetic scales is investigated by means of laboratory experiment, analytical analysis and Hall MHD simulation. In experiment a specific magnetic field was observed which is non-coplanar to dipole field, does not change sign at dipole moment inversion and could be generated only via the quadratic Hall term. Magnetopause position and plasma stand off distance were found to be profoundly different between the experimental regimes with small and large ion inertia length. In the previous studies of a mini-magnetosphere by kinetic codes such novel features were observed as absence of the bow shock and plasma stopping at the Stoermer particle limit instead of the pressure balance distance. Proposed analytical model explains these features by Hall currents which tend to cancel magnetic field convection by ions. Performed numerical simulation shows a good agreement with experiment and analytical model. It gives detailed spatial structure of the Hall field and reveals that while ions penetrate deep inside mini-magnetosphere electrons overflow around it along magnetopause boundary.     

轴对称磁静平衡态Ⅰ.微变换方法

轴对称磁静平衡态被广泛用来描述不同尺度的恒星大气结构。对这类平衡态,可引入所谓磁通量函数来描述磁场,它满足一变系数、非线性椭圆型方程。迄今为止,人们只就线性情况的某些特例给出该方程的解析解;对较为复杂的情况,特别是非线性情况,还未找到有效的办法进行解析处理。本文将应用微变换方法求上述变系数、非线性方程的相似解,并给出普遍结果。有关特解的具体形式及对太阳大气的应用将在本系列的下几篇论文中另作讨论。      

太阳大气中有限振幅磁场扰动的动力学过程

本文从完整的磁流体动力学方程组出发,通过太阳大气中磁力线管根部有限振幅磁场的扰动,研究了非线性磁场的动力学演化。假设初始磁场位形足β<<1的势场,根部磁力线管磁场扰动,驱动等离子体运动,一部分磁能转换为等离子体动能。等离子体压缩运动具有快磁声波的特性。计算结果给出非线性磁场演化的定量关系,可以解释太阳大气中日冕活动过程。也可用于模拟实验室里高β实验装置中的等离子体的持性。      

多刚体卫星转动惯量在轨辨识

惯量辨识需要精确的动力学特性,针对动力学特性不可忽略太阳电池阵转动这一状况,提出一种惯量辨识方法,用于卫星本体惯量和太阳电池阵惯量的联合辨识.在建立多刚体姿态动力学基础上,针对辨识变量的耦合特性,推导带约束的优化辨识模型,再利用约束最小二乘算法求解.最后通过仿真计算验证了辨识方法的可行性.     

Small amplitude ion acoustic solitons in a weakly magnetized plasma with anisotropic ion pressure and kappa distributed electrons

The Zakharov–Kuznetzov (ZK) equation is derived for nonlinear electrostatic waves in a weakly magnetized plasma in the presence of anisotropic ion pressure and superthermal electrons. The anisotropic ion pressure is defined using Chew–Goldberger–Low (CGL) while a generalized Lorentzian (kappa) distribution is assumed for the non-thermal electrons. The standard reductive perturbation method (RPM) is employed to derive the two dimensional ZK equation for the dynamics of obliquely propagating low frequency ion acoustic wave. The influence of spectral index (kappa) of non-thermal electron on the soliton is discussed in the presence of anisotropic ion pressure in plasmas. It is found that ion pressure anisotropy and superthermality of electrons affect both the width and amplitude of the solitary waves. On the other hand the magnetic field is found to alter the dispersive property of the plasma only, and hence the width of the solitons is affected while the amplitude of the solitary waves is independent of external magnetic field. The numerical results are also presented for illustrations.     

Investigation of impulsive soft X-ray brightening in solar flares

Four multi-loops or arcade flares showing strong impulsive soft X-ray brightenings on Yohkoh/SXT frames have been selected. By inspection of light curves of individual pixels, the areas of brightening have been localised. Evidences that non-thermal electron beams easily penetrate through whole flaring structures have been found. In some footpoints of the flaring structures during the impulsive phase the evidence of the chromospheric evaporation driven by non-thermal electron beams has been detected. The velocities of the upflowing plasma have been estimated. Derived values are in a wide range among 220 and 750 km/s. The SXT images of the investigated flares have been compared with the Yohkoh/HXT images. Generally good spatial and temporal coincidence between soft and hard X-ray emission from footpoints of flaring structures during the impulsive phase have been found but some exceptions occur. An explanation of the reported exceptions based on the magnetic field configuration has been proposed.