磁云边界层中的复合重联喷流观测分析

太阳风中的磁场重联通常与行星际日冕物质抛射有关.本文分析了1995年10月18日WIND飞船观测到的一例磁云前边界层中的复合重联喷流事件.该复合排空区由相邻两个不同方向的喷流构成，这两个喷流分别经过Walén关系的证认，符合行星际磁场重联排空区等离子体喷流的特征.结果表明，在磁云前端可能存在众多重联点，从而将磁云本体的磁场剥离，形成比单一重联喷流区更复杂的三维边界层结构.磁云边界层中可能发生多点多次重联，从而不表现出单点重联的排空区特征，这可能是行星际磁场重联排空区较少在ICME前端被观测到的原因之一.      

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。     

磁重联区Alfven波及新生离子的加速

利用二维混合数值模拟研究了有速度驱动、低等离子体β值情况下的磁场重联过程，结果表明磁重联过程可以产生Alfven波，该Alfven波动对重新区中的新生离子作用，使得新生离子经历投掷角散射方程，具有球壳分布特征，部分新生离子得到加速，其获得的最大能量约为4（miVA0^2/2)，此加速过程所需的加速时间在100／Ωi量级，是一个极快的加速机制，加速粒子能谱为双幂律谱。     

磁场重联中的哨声波与Hall效应

数值研究Hall电流效应对于重联动力学特征及波动特性的影响.结果表明,具有强Hall效应的算例,重联出流区张角大,重联率高.对于不同Hall效应的算例,应用快速傅里叶变换(FFT),将平面外磁场By分量和(x,z)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,并对电场E采用最小方差分析法,确定波的传播方向与偏振特性.研究发现,在强Hall效应的算例中,磁分界线附近存在具有典型特征的哨声波,Hall效应减弱,则波动信号减弱.上述结果表明,Hall电流效应对重联动力学特征具有重要影响,是产生哨声波和快速重联率的关键因素;此外,对于强Hall效应的算例,磁分界线附近哨声波幅度与平面内场向电流Jp间存在正相关关系,它从另一个侧面展示了哨声波与Hall效应间的重要联系.      

磁云边界层中的重联慢激波观测分析

在Petschek模型中，排空区边界处的一对慢激波是能量耗散的重要机制.已有大量行星际空间的Petschek型磁场重联排空区观测事件被报道，但是只有少量的排空区边界处观测到了慢激波.针对一例位于磁云边界层中的Petschek型磁场重联排空区观测事件，在排空区靠近磁云一侧边界处证认了一例慢激波.激波跃变层两侧的磁场和等离子体参数满足Rankine-Hugoniot关系，且激波上下游的中间马赫数均小于1，上游的慢马赫数为2.94（>1），下游的慢马赫数为0.65（<1），符合慢激波的观测特征.磁云内部的等离子体β值很低，局地阿尔芬速度高，同时磁云边界层中可能发生丰富的磁场重联活动，这可能是磁云前边界处慢激波形成的原因.      

太阳表面水平运动驱动的磁圈与开放磁场重联的模拟研究

太阳大气的诸多观测事件(如耀斑、喷流等)均被归因于磁重联产生的能量转换. 近年来, 关于太阳风起源, 有研究提出了磁重联使闭合磁圈开放为太阳风供应物质的新模式. 在该模式中, 闭合磁圈被光球超米粒组织对流携带, 向超米粒边界运动, 与位于边界的开放磁场相碰撞进而发生磁重联. 该模式中磁重联的驱动及其效应是本文的研究目标. 磁流体力学(MHD)数值模拟是研究太阳大气磁重联物理过程的重要途径. 本文建立了一个二维MHD数值模型, 结合太阳大气温度和密度的分层分布, 在超米粒组织尺度上模拟了水平流动驱动的闭合磁圈与开放磁场的重联过程. 通过对模拟结果的定量分析, 认为磁重联确实能够将闭合磁圈的物质释放, 进而供应给新的开放磁结构并产生向上流动. 该结果为进一步模拟研究太阳风初始外流奠定了基础.      

日冕冲浪形成的磁流体动力学模拟

应用二维时变可压缩磁流体动力学模拟,数值研究了双极-单极磁场中电阻撕裂模不稳定性引起的磁场重联过程,用于模拟日冕冲浪的形成.结果表明,在包含有三区——双极场、电流片和单极场的磁静力平衡初态下,双极场和单极场中的磁力线将会直接重联,磁场演变成鞭状(whip)结构.由弯曲磁力线支撑的等离子体团向上运动到最高位置后,逐渐下落和弥散.等离子体团上升速度可达到0.10v_A(v_A为双极场中的Alfv'én速度).模拟结果证实日冕冲浪的形成可能与双极-单极场中的磁场重联密切相关.      

近地磁尾准无碰撞磁重联事件

综合分析了ClusterⅡ－C1飞船在2001年9月15日飞越地球磁尾等离子体片区的热离子和磁场观测资料。结果表明，约在0340－0440UT时间期间，资料多次呈现出较强的尾向离子流（VXGSM＜0），明显的南向磁场分量（BZGSM＜0），以及明显的晨－昏向磁场分量BYGSM等特征。由此可以推断，在磁尾等离子体片中，在径向方向XGSE＞－18．6Re范围内，可能发生了多次磁重联事件，整个事件持续期约1h。磁重联事件的观测特征与准无（或半）碰撞磁重联理论的基本图像符合一致，因此这些事件应当是准无碰撞磁重联事件。     

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.      

等离子体彗尾动力学的数值研究

本文基于可压缩磁流体动力学模型,数值研究了尾瓣巾具有超Alfven速流动的等离子体彗尾的动力学特征。结果表明,等离子体片和尾瓣之间的剪切等离子体流动将会激发流动撕裂模不稳定性,引起彗尾等离子体片中发生磁场重联,形成磁岛和高密度的等离子体团。进而模拟了太阳风引起的局部驱动力对等离子体彗尾中磁场重联的影响,其特征时间远大于流动撕裂模。我们认为一些观测到的等离子体彗尾中的四块和彗尾截断事件可能主要与彗尾中剪切等离子体流动所引起的流动撕裂模不稳定性有关。      

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.     

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.     

太阳风向磁层输入电磁能量研究

利用全球磁流体力学（MHD）模拟结果,通过确立包含磁层顶的太阳风流线内边界来识别三维磁层顶位形,并以极尖区位置作为磁层顶日侧与夜侧的分界线,在此基础上定量研究了不同条件下穿过磁层顶向磁层内输入的电磁能量. 研究发现,磁层顶的能量传输与太阳风条件密切相关,磁重联是控制电磁能量传输的重要机制. 结果表明,当IMF（行星际磁场）南向时,极尖区后方的磁尾附近存在电磁能输入最大值,当IMF北向时,电磁能输入最大值发生在极尖区附近;南向IMF条件下,在IMF强度增大或太阳风密度增大时,磁层顶电磁能传输的电磁能量比北向IMF条件时增加更显著. 太阳风通过调节磁层顶面积间接影响到磁层顶能量传输大小. 研究还发现,北向IMF与南向IMF条件下穿过磁层顶的电磁能输入的比值范围约为10%～30%,此比值一定程度上反映了北、南方向IMF与地磁场磁重联效率的比值.      

Global Hybrid Simulation of Magnetic Reconnection in the Magnetosheath

A three-dimensional (3-D) global hybrid simulation is carried out for the generation and structure of magnetic reconnection in the magnetosheath due to interaction of an interplanetary Tangential Discontinuity (TD) with the bow shock and magnetosphere. Runs are performed for solar wind TDs possessing different initial half-widths. As the TD propagates through the bow shock toward the magnetopause, it is greatly narrowed by a two-step compression processes, a "shock compression' followed by a subsequent ``convective compression'. In cases with a relatively thin solar wind TD, 3-D patchy reconnection is initiated in the transmitted TD, forming magnetosheath flux ropes. Multiple components of ion particles are present in the velocity distribution in the magnetosheath merging, accompanied by ion heating. For cases with a relatively wide initial TD, a dominant single X-line appears in the subsolar magnetosheath after the transmitted TD is narrowed. A shock analysis is performed for the detailed structure of magnetic reconnection in the magnetosheath. Rotational Discontinuity (RD)/Time-Dependent Intermediate Shock (TDIS) are found to dominate the reconnection layer, which and some weak slow shocks are responsible for the ion heating and acceleration.      

Solar wind interaction with lunar crustal magnetic anomalies

Using Lunar Prospector data, we review the magnetic field and electron signatures of solar wind interaction with lunar crustal magnetic sources. Magnetic field amplifications, too large to represent direct measurements of crustal fields, appear in the solar wind over strong crustal sources, with the chance of observing these amplifications depending on upstream solar wind parameters. We often observe increases in low-energy (?100 eV) electron energy fluxes simultaneously with large magnetic field amplifications, consistent with an increase in plasma density across a shock surface. We also often observe low frequency wave activity in the magnetic field data (both broadband turbulence and monochromatic waves), often associated with electron energization, sometimes up to keV energies. Electron energization appears to be correlated more closely with wave activity than with magnetic amplifications. Detailed studies of the interaction region will be necessary in order to understand the physics of the Moon–solar wind interaction. At present, the Moon represents the only natural laboratory available to us to study solar wind interaction with small-scale crustal magnetic fields, though simulation results and theoretical work can also help us understand the physical processes at work.     

Solar wind governing the response of Venusian atmosphere and ionosphere

The ionosphere of Venus is primarily formed by photoionization of a gaseous blanket around Venus. The impact ionization by energetic solar charged particles also plays an important role in the variability of Venusian ionospheric ion, electron density and their temperature profiles. The microscopic variations in the solar wind velocity, particle flux and orientations of frozen-in interplanetary magnetic field determine the solar wind interaction with the Venusian ionosphere. The ion and electron density profiles obtained by Pioneer Venus Orbiter and Pioneer Venus Entry Probes have been analysed in the light of simultaneous solar wind velocity and particle flux. Marked changes in height profiles of ion, electron densities and their temperatures have been found to correlate with the simultaneous changes in the solar wind velocity and particle flux. It is shown that the solar wind plays a more important role in controlling the physical properties and behavior of daytime as well as nighttime ionosphere of Venus, whereas the solar xuv sustains the primary ionization process.     

Plasma flow across the cusp-magnetosheath boundary under northward IMF

In this paper, we have used two closely spaced (INTERBALL-1 and MAGION-4) satellites orbiting in the region adjacent to the magnetopause with motivation to determine the structure of the cusp-magnetosheath boundary under steady solar wind conditions and under the northward interplanetary magnetic field (IMF). Two-point observations reveal that a steady reconnection takes place tailward of the cusp and the position of the reconnection site moves in accordance with the actual IMF direction. Reconnection produces a latitudinally dispersed cusp precipitation with highest energies in the cusp poleward edge. The reconnection site is widely spread in local time and thus changes of the IMF By component only slightly modulate observed patterns. The change of the plasma flow direction suggests the presence of the vortex-like structure in the exterior cusp.