具有不同等离子体β值的Hall MHD重联中的低频波研究

数值研究具有不同等离子体β值(等离子体热压与磁压之比)的Hall MHD重联过程.对于β值在0.5≤β≤6.5的算例,稳态重联率(6)A/(6)t|st为0.15≥(6)A/(6)t|st≥0.095.本文研究β值在上述范围内的Hall MHD重联中的波动.通过快速傅里叶变换(FFT),将平面外磁场By分量和xz平面内的速度分量vx,vz位于给定点的时间序列转换为功率谱.结果表明,By,vx,vz功率谱的频率范围为Ωci＜ω＜8Ωci,其中Ωci为离子回旋频率.随着β值增大,功率谱峰值能量降低,并且朝着低频端移动.对于电场E采用最小方差分析法(MVA)可以确定波的传播方向k,波矢k与局地磁场B之间的夹角α随β值增大而增大.对于β值最大的算例3(β=6.5),α＜28°.上述结果表明,k准平行于B.为了研究波的偏振特征,在垂直于k的平面内画出E的矢端图.三个算例的矢端图均表明,波动具有右旋偏振特征,在算例1(β=0.5)中矢端图为右旋椭圆偏振,而在算例2(β=2.5)和算例3(β=6.5)中矢端图变成复杂的右旋偏振图形,这些均为哨声波的典型特征.本文的研究为快速磁重联与哨声波之间提供了一种可能的联系.      

太阳风中磁场重联离子扩散区的大尺度特征

利用ACE和WIND卫星2007年1月6日的联合探测, 在1AU附近发现了一个等离子体密度极低的Petschek-like重联喷流区. 该喷流区内部出现了非常明显的Hall双极磁场、等离子体密度下降区以及与Hall电流相符的低能段电子投掷角分布. 这些特征与重联离子扩散区的Hall效应非常吻合, 说明很可能在太阳风中观测到了一个离子扩散区. 分析表明, 与之相关的磁场重联为准稳态快速完全反向重联, 其扩散区以一对慢模波为边界, 空间尺度达到80个离子惯性长度, 表现出了大尺度重联的特征.      

磁场重联的二维粒子模拟研究

利用二维全粒子模拟方法研究了无碰撞等离子体中的磁场重联过程，得到了不同区域的离子和电子速度分布．计算结果表明，电子和离子在扩散区中的不同动力学特性产生的Hall电流使磁场的y分量By呈现四极形分布．离子和电子的速度分布偏离了初态时的Maxwell分布，呈现非局域的多重分布．同时由于磁场重联而产生的电场使电子在X点附近得到加速和加热，因而在电子的能谱分布中形成-高能尾。     

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.      

行星际磁云与日球电流片相互作用的实例分析

基于1995-2007年Wind飞船观测到的105个磁云事件, 按照磁云在地球附近是否与日球电流片发生碰撞, 将其分为碰撞和未碰撞两类, 得到初步分析结果. ①可能与日球电流片发生碰撞的磁云事件有51例, 约占事件总数的49%; ②发生碰撞时, 磁云与日球电流片之间的相互作用区内呈现动力学相互作用增强的趋势, 例如多呈现局部的磁场方向间断结构(或称局域电流片结构), 伴随磁场强度下降、质子温度升高、部分质子速度分量出现跃变, Langmuir波或100~250,kHz的离子声波出现增强,这些现象可能与碰撞相互作用区域内发生的磁重联有关; 没有碰撞时这些特征一般不明显; ③至少有15个事例中, 磁云前后背景磁场的极性相反, 或磁场极性反转的位置位于磁云内部, 显示磁云可能正在跨越电流片运动; ④在几个磁云事件中发现磁云的亮环和亮核纤维结构. 这些极为初步的分析结果有利于了解磁云与日球电流片之间的相互作用过程.      

2.5维自适应磁场重联MHD模式

磁雷诺数(R_m)是影响磁场重联的重要因素. 真实的物理环境中R_m往往很高, 例如, 在行星际空间和太阳日冕中R_m通常大于104量级. 高R_m条件下的磁重联表现出很多异常特性, 然而高R_m条件下的磁场重联数值模拟需要很高的时空分辨率, 否则很难分辨出重联过程中形成的薄电流片. 本文基于自适应软件包PARAMESH将并行自适应网格技术引入磁场重联数值模拟, 建立了一个2.5维自适应磁场重联MHD模式, 研究高磁雷诺数条件下重联的动态演化过程, 进而将不同磁雷诺数的参数进行对比研究. 结果表明, 该模式可以自动捕捉到磁场重联产生的奇性电流片, 高磁雷诺数条件下产生的慢激波结构可提供一种快速磁能释放机制.      

引导场对无碰撞电流片低频电磁不稳定性的影响

通过数值求解无碰撞电流片中可压缩磁流体力学模型下得到的一般形式的色散关系,讨论了无碰撞电流片中引导场对低频电磁波不稳定性的影响.结果表明,平衡态磁场中的引导场,对于三维扰动传播的波不稳定性有很强的影响.(1)在电流片中间平面上(z=0),无引导场时,没有不稳定性发生,但若存在引导场,不稳定性便发生,并随着引导场的增强,不稳定性明显增强,不稳定的波模可能是低混杂模.(2)在中间平面附近(z=0.2),电流片是不稳定的.随着引导场的增强,不稳定性增长率明显地增强,不稳定的波模从平行和反平行两个方向传播变为反平行方向一个方向传播,并且是斜传播的,具有低频哨声模或低混杂模的特征.(3)在电流片边缘附近(z=0.8),引导场对不稳定的波模和增长率没有明显影响,不稳定的波模都是准平行的哨声波.      

TC-1和Cluster对向阳侧磁层顶通量传输事件的联合观测研究

2004年2至4月期间,探测一号(TC-1)卫星和Cluster卫星有25次同时处在向阳侧磁层顶附近的磁鞘内,TC-1卫星在低纬区,Cluster卫星在中高纬区.利用这一期间两卫星探测到的27个通量传输事件(FTE),分析行星际磁场(IMF)横向分量BT={By,Bz}对磁层顶重联发生位置的影响,以及分量重联的观测事实,得到如下主要结果.(1)当IMF南向分量Bz占优势(|Bz|＞|By|)时,FTE大多(约占87.5%)能在低纬观测到,而当IMF By分量占优势(|Bz|＜|By|)时,则FTE大部分能在中高纬观测到(占84.2%);(2)很少观测到相关联的事件(关联事件指在低纬生成的FTE,向高纬运动中先后被TC-1卫星和Cluster卫星探测到的事件),表明在低纬形成的FTE可能大多沿磁层顶两侧滑向磁尾,只有少数可能运动到高纬地区;(3)中纬地区探测到的FTE大多是以分量重联方式产生于该区,而非来自磁赤道附近成对形成的FTE.      

电流片的自发重联与无力场──磁岛的形成

采用二维三分量磁流体力学数值模拟方法,研究了线性无力场对电流片的自发重联的影响。结果表明:电流片的背景场(无力场)对重联的拓扑位形有重要的影响,当无力场因子达到一定值时,在模拟区域内出现大范围的磁岛,磁岛厚度随时间的发展而增加,而无力场因子较小时则没有磁岛形成。当无力场因子为零时,即回到普通的位场情形的单x线重联,位场情形磁场拓扑位形与Scholar的结果一致。      

利用Cluster卫星磁尾单事例研究具有复杂核心磁场结构的磁通量绳

2002年8月28日09:50UT-10:50UT,Cluster卫星在地球磁尾观测到一次导向场磁场重联事件.卫星观测到磁场重联扩散区附近清晰的霍尔（Hall）四极型磁结构.由于导向场的存在,该四极型结构被扭曲变形.在该磁场重联事件中,卫星观测到多个磁通量绳,大部分磁通量绳的核心场极性与导向场极性一致.但是,其中一例磁通量绳的核心场结构极性较复杂.该例磁通量绳中心区域核心场强度出现峰值,核心场极性和导向场极性一致;中心以外区域的核心场极性和导向场极性相反.这种复杂核心场结构以前未见报道.通过最小方向导数法,发现该磁通量绳的轴向是弯曲的.C1和C3卫星穿越了磁通量绳弯曲部分,探测到核心场极性变化;C2和C4卫星位于C1和C3卫星的北侧,仅穿越了磁通量绳弯曲处的一部分,故核心场具有单极性.      

Theoretical model of steady-state magnetic reconnection in collisionless incompressible plasma based on the Grad–Shafranov equation solution

The problem of steady-state magnetic reconnection in an infinite current layer in collisionless, incompressible, nonresistive plasma, except of the electron diffusion region, is examined analytically using the electron Hall magnetohydrodynamics approach. It is found that this approach allows reducing the problem to the magnetic field potential finding, while last one has to satisfy the Grad–Shafranov equation. The obtained solution demonstrates all essential Hall reconnection features, namely proton acceleration up to Alfvén velocities, the forming of Hall current systems and the magnetic field structure expected. It turns out that the necessary condition of steady-state reconnection to exist is an electric field potential jump across the electron diffusion region and the separatrices. Besides, the powerful mechanism of electron acceleration in X-line direction is required. It must accelerate electrons up to the electron Alfvén velocity inside the diffusion region and on the separatrixes. This is a necessary condition for steady-state reconnection as well.     

Where will efficient energy release occur in 3-D magnetic configurations?

The energy needed to power flares is thought to be stored in the coronal magnetic field. However, the energy release is efficient only at very small scales. Magnetic configurations with a complex topology, i.e. with separatrices, are the most obvious configurations where current sheets can form, and then, reconnection can efficiently occur. This has been confirmed for several flares computing the coronal field and comparing the locations of the flare loops and ribbons to the deduced 3-D magnetic topology. However, this view is too restrictive taking into account the variety of observed solar flaring configurations. Indeed, “Quasi-Separatrix Layers” (QSLs), which are regions where there is a drastic change in field-line linkage, generalize the definition of separatrices. They let us understand where reconnection occurs in a broader variety of flares than separatrices do. The strongest electric field and current are generated at, or close to where the QSLs are thinnest. This defines the region where particle acceleration can efficiently occur. A new feature of 3-D reconnection is the natural presence of fast field-line slippage along the QSLs, a process called “slip-running reconnection”. This is a plausible origin for the motions of the X-ray sources along flare ribbons.     

Linear theory of steady X-point magnetic reconnection

Slow magnetic reconnection at a neutral X-point of a two-dimensional magnetic field is studied in an incompressible viscous resistive fluid. It is shown analytically that the combined effect of viscosity and resistivity resolves the current singularity appearing in both the ideal and resistive magnetohydrodynamic approximations at the X-point and along the separatrices when the flow is allowed to cross them. A previous attempt had retained a weak singularity at third order. A two-parameter family of exact solutions describing the structure of the flow and current density distribution is found for the corresponding basic equations.     

Particle simulation study of substrom triggering with a southward IMF

This paper reports the spatial and temporal development of bursty bulk flows (BBFs) created by reconnection as well as current disruptions (CDs) in the near-Earth tail using our 3-D global electromagnetic (EM) particle simulation with a southward turning interplanetary magnetic field (IMF) in the context of the substorm onset. Recently, observations show that BBFs are often accompanied by current disruptions for triggering substorms. We have examined the dynamics of BBFs and CDs in order to understand the timing and triggering mechanism of substorms. As the solar wind with the southward IMF advances over the Earth, the near-Earth tail thins and the sheet current intensifies. Before the peak of the current density becomes maximum, reconnection takes place, which ejects particles from the reconnection region. Because of earthward flows the peak of the current density moves toward Earth. The characteristics of the earthward flows depend on the ions and electrons. Electrons flow back into the inflow region (the center of reconnection region), which provides current closure. Therefore the structure of electron flows near the reconnection region is rather complicated. In contrast, the ion earthward flows are generated far from the reconnection region. These earthward flows pile up near the Earth. The ions mainly drift toward the duskside. The electrons are diverted toward the dawnside. Due to the pile-up, dawnward current is generated near Earth. This dawnward current dissipates rapidly with the sheet current because of the opposite current direction, which coincides with the dipolarization in the near-Earth tail. At this time the wedge current may be created in our simulation model. This simulation study shows the sequence of the substorm dynamics in the near-Earth tail, which is similar to the features obtained by multisatellite observations. Identification of the timing and mechanism of triggering substorm onset requires further studies in conjunction with observations.     

Modeling large solar flares

The basic ideas to model the large solar flares are reviewed and illustrated. Some fundamental properties of potential and non-potential fields in the solar atmosphere are recalled. In particular, we consider a classification of the non-potential fields or, more exactly, related electric currents, including reconnecting current layers. The so-called ‘rainbow reconnection’ model is presented with its properties and predictions. This model allows us to understand main features of large flares in terms of reconnection. We assume that in the two-ribbon flares, like the Bastille-day flare, the magnetic separatrices are involved in a large-scale shear photospheric flow in the presence of reconnecting current layers generated by a converging flow.     

Numerical study of magnetic reconnection possibly occurring near heliospheric current sheet

The third-order accurate upwind compact difference scheme has been applied for the numerical study of the magnetic reconnection driven by a plasma blob impacting the heliospheric current sheet, under the framework of the two-dimensional compressible magnetohydrodynamics. The results show that the driven reconnection near the current sheet could occur in about 10–30 min for the interplanetary high magnetic Reynolds number, R_M = 2000–10,000, a stable magnetic reconnection structure can be formed in hour order of magnitude, and there appear some basic properties such as the multiple X-line reconnections, vortex structures, filament current systems, splitting and collapse of the high-density plasma blob. These results are helpful in understanding and identifying the magnetic reconnection phenomena possibly occurring near the heliospheric current sheets.