太阳大气中磁场的扭转储能

本文从完整的磁流体动力学方程组出发, 研究太阳大气中磁力线管根部的扭转储存能量。通过数值方法, 研究了包含太阳表面过渡区在内的非线性无力场的动力学演化。假设初始磁场位形为势场, 根部等离子体运动使活动区磁场扭转。磁能蓬新分布, 在局部区域中储存大量的磁能。计算结果给出非线性无力场的定量关系, 可以解释太阳耀斑的储能过程。      

各向异性等离子体多重电流片的演化

应用二维三维量磁流体动力学方程组模拟，数值研究了压力各向异性等离子体周期多重电流片的演化，发现在β＜＜1时，微弱的各向异性仅仅使电流片中磁场重联的速度加快，而当β≈1（即热压与磁压相当时，微弱的垂直各向异性不仅大大加速了磁场重联的速度，还使重联位置发生显著变化。初始反对称的磁场重联位形逐步转化为对称的磁场位形，进而再演化为与初始反相的反对称磁场位形，场向各向异性和强的垂直各向异性都导致不稳定性增长率成倍增加。但在场各向异下磁场位形基本不变，只在电流片中心出现不规则扰动，同样参数下向向异性等离子体多重电流片中磁场重联形成的磁岛比各向同性多层电流要小。     

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.      

地球磁尾的电场模式

地球磁层中的电场是磁层等离子体运动的主要驱动力。目前常用的磁层电场为均匀晨昏电场和投影电场。本文假定磁力线为电场的等位线，地球电离层电场看做磁层电场沿磁力线在电离层的投影。利用Tsyganenko磁场模式（T89），沿磁力线反电离层电场投影到磁尾，得到了一个新的磁层电场模式。文中对偶极磁场和T89磁场模式下的投影场作了比较，说明本模式突破了偶极磁场的局限，在磁层有更大的适用范围。     

火星空间磁场结构特征

在火星空间模拟的单流体MHD模型的基础上, 研究了火星空间磁场结构及火星表面局部磁异常对磁场结构的影响. 在太阳风与火星相互作用的过程中, 形成弓激波和磁堆积区, 行星际磁场弯曲并向两极移动且被拖拽变形, 大部分磁力线从火星两极绕过, 通过火星之后在磁尾留下V字形结构. 火星表面附近局部磁异常也对火星磁场结构产生不可忽视的影响. 不同位置和强度的磁异常与太阳风相互作用形成结构及形态各异的微磁层, 如被拖拽的微磁层和存在开磁力线的微磁层等. 局部磁异常改变了近火磁场结构, 并可能改变等离子体的分布.      

磁尾等离子体团型结构的数值模拟

考虑横越磁尾不同区域的数密度与离子温度的分布特点,取宁静磁尾温度、密度呈同样形态的非均匀分布,作为模拟计算的初态,对初始By为不同分布的3个算例作模拟计算．数值结果展示了3类磁结构的演化特征．考察磁尾中性片一个给定点的磁场变化,做出3个算例典型事件的磁场矢端图．它们从另一个侧面展示了磁尾通量绳型等离子体团、具有复杂闭合磁力线位形类似于“闭合环”的等离子体团,以及二维“磁岛”型等离子体团的特点．观测表明,多数磁尾等离子体团为具有强核心场的通量绳结构．通过跟踪一个通量绳型等离子体团的发展,作出等离子体团各方向速度与磁场强度随x演化的曲线．其中,vx与磁场强度|B|在近尾至中尾的计算值与Geotail卫星资料统计分析结果大致相符．此外,与Jin等取初始温度为均匀分布的计算结果相比,本文给出的通量绳型等离子体团,其内温度较高、密度较低,与资料分析结果的偏离也随之减小．     

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.      

木星磁层熵参量的计算与分析

空间等离子体熵的不守恒可能来自于磁场位形改变和非绝热过程.熵参量PV~(5/3)被广泛应用于分析地球磁层等离子体片中的输运问题,其中,P为压力,V为单位磁通量管的体积.通过熵参量的分布和变化可以判断磁层的稳定性及揭示磁层中的动力学过程.本文利用地球磁层中熵参量的分析应用,计算了木星稳态磁层模型中磁通量管的熵参量分布.从5R_j(R_j为木星半径)到55_j,熵参量增加了4个量级,55 R)_j之后有所下降,表明所用磁层模型在55R_j之外已经不稳定.同时,假想磁场重联后的单位磁通量管的熵参量分布表明,赤道面中远磁尾的磁场重联是由尾向输运的磁力线管拉伸断裂重联引起的.     

行星际起伏向磁层顶的输运

时间尺度为分钟数量级的太阳风速度和行星际磁场大幅度扰动实际上始终存在于行星际空间的。这些扰动一直传输到紧贴磁层边界面外侧的区域。它们在磁鞘等离子体和磁层顶的相互作用过程中可能起很重要的作用。行星际起伏中的磁场分量在通过地球弓激波时首先经历一次跳跃,然后一部分扰动被带到磁层边界面处。在边界面附近磁场扰动幅度被大大地放大了。弓激波上游的太阳风条件控制了放大因子。本文所作的数值模拟研究结果表明,如果上游有大幅度的扰动,在边界面附近就有大幅度的Alfven起伏的磁场分量。当上游磁场接近垂直于日地联线时,放大因子变得相当大,而且放大因子随上游的等离子体β值和/或Alfven马赫数的增加而增加。上游各向异性对放大因子的影响不大。在磁层边界附近存在大幅度起伏表明这里不存在稳定的片流。      

带电粒子在中性线磁场中运动的解析轨道

本文我们计算了带电粒子在中性线磁场中运动的解析轨道。其结果是:(1)带电粒子在中性片磁场中的运动是粒子在中性线磁场或在具有北向分量的中性片磁场中的第一级近似形式。(2)带电粒子在中性片磁场中的解析轨道的第三级近似形式与电子计算机计算的数值轨道基本相同。它们仅仅在小扰动区与非小扰动区的交界线上出现一些偏差。(3)带电粒子在整个中性片磁场的运动可以分成三种形式。粒子一方面在垂直于磁场的平面上作闭合的周期性轨道运动, 同时闭合轨道的中心还沿着垂直于磁场平行于中性线方向漂移。另一方面粒子还沿磁力线方向做等速运动。(4)在小扰动区中粒子的闭合轨道是一个圆轨道, 但在非小扰动区中却是一个“8”字形轨道, 其漂移速度与小扰动区漂移方向相反, 其大小也比小扰动区漂移大很多。以上结果本文都给出一个完整的解析形式。      

Reconnection in multiple current sheet configurations in the solar corona

We investigate magnetic reconnection in a multiple current sheet configuration by means of three-dimensional resistive MHD simulations. This configuration might be of interest in the solar corona context, e.g. for coronal helmet streamers. We present results of our simulations of the linear and nonlinear development of the tearing mode instability. In particular, we highlight the changes in magnetic topology and the resulting plasma dynamics. Our results indicate that reconnection in complex coronal neighboring magnetic flux systems efficiently converts magnetic field energy into thermal energy and leads to small-scale tongue outflows rather than large-scale coronal mass ejections.     

激波在行星际介质中的能量耗散

导出激波下游介质相对上游介质能流通量增量公式,并由HeliosA,B飞船太阳风观测资料得出不同流速太阳风流中各参量随日心距的幂律变化。以此作为背景值分别计算出磁能、内能、动能和总能在不同日心距离处的能量耗散率。结果指出激波后介质以动能增加为主,内能次之,磁能最少;总能耗率在近日处较大,但下降较快。从0.3-1.0AU,不同强度激波总能耗随初始Alfvén激波数A₁₀增大而增大,对A₁₀从2.0-10.0的计算结果与观测值一致。      

Two energy release processes for CMEs: MHD catastrophe and magnetic reconnection

It remains an open question how magnetic energy is rapidly released in the solar corona so as to create solar explosions such as solar flares and coronal mass ejections (CMEs). Recent studies have confirmed that a system consisting of a flux rope embedded in a background field exhibits a catastrophic behavior, and the energy threshold at the catastrophic point may exceed the associated open field energy. The accumulated free energy in the corona is abruptly released when the catastrophe takes place, and it probably serves as the main means of energy release for CMEs at least in the initial phase. Such a release proceeds via an ideal MHD process in contrast with nonideal ones such as magnetic reconnection. The catastrophe results in a sudden formation of electric current sheets, which naturally provide proper sites for fast magnetic reconnection. The reconnection may be identified with a solar flare associated with the CME on one hand, and produces a further acceleration of the CME on the other. On this basis, several preliminary suggestions are made for future observational investigations, especially with the proposed Kuafa satellites, on the roles of the MHD catastrophe and magnetic reconnection in the magnetic energy release associated with CMEs and flares.     

Evolution of electron energy spectrum during solar flares

Particle acceleration by direct current electric field in the current sheet has been extensively studied, in which an electric and a magnetic field are generally prescribed, and a power law distribution of the electron energy is obtained. Based on MHD numerical simulations of flares, this paper aims at investigating the time evolution of the electron energy spectrum during solar flares. It turns out that the model reproduces the soft–hard–hard spectral feature which was observed in some flares.     

Acceleration of charged particles by fluctuating and steady electric fields in a X-type magnetic field

Release of stored magnetic energy via particle acceleration is a characteristic feature of astrophysical plasmas. Magnetic reconnection is one of the mechanisms for releasing energy from magnetized plasmas. Collisionless magnetic reconnection could provide both the energy release mechanism and the particle accelerator in space plasmas. Here we studied particle acceleration when fluctuating (in-time) electric fields are superposed on an static X-type magnetic field in collisionless hot solar plasma. This system is chosen to mimic the reconnective dissipation of a linear MHD disturbance. Our results are compared to particle acceleration from constant electric field superposed on an X-type magnetic field. The constant electric field configuration represents the effects of steady state magnetic reconnection. Time evolution of ion and electron distributions are obtained by numerically integrating particle trajectories. The frequencies of the electric field represent a turbulent range of waves. Depending on the frequency and amplitude of the electric field, electrons and ions are accelerated to different degrees and have energy distributions of bimodal form consisting of a lower energy part and a high energy tail. For frequencies (ω in dimensioless units) in the range 0.5 ? ω ? 1.0 a substantial fraction (20%–30%) of the proton distribution is accelerated to gamma-ray producing energies. For frequencies in the range 1 ? ω ? 100.0 the bulk of the electron distribution is accelerated to hard X-ray producing energies. The acceleration mechanism is important for solar flares and solar noise storms but it could be applicable to all collisionless astrophysical plasmas.     

日球基本参数的冕洞周变化与冕洞大气

本文利用MHD波与日冕大气耦合的磁流体动力学方程组,计算得到冕洞内的日冕大气的温度T、密度N和流速V的分布.根据这些量的分布特点,认为日球基本参数T、N和V的冕洞周变化,可以用冕洞磁场的非径向因子a值,随黑子活动的下降而变小来解释.      

The accuracy of present models of the high altitude polar magnetosphere

The Polar satellite has explored the high-latitude, high-latitude magnetosphere out to 9 Earth radii (Re). The magnetic field data returned from this mission can be used both to provide data for new empirical models and to test existing models. Tests include comparing the observed location of the polar cusp with its position in the empirical models and comparing the strength of the magnetic field in the surrounding region. Near the cusp the magnetosphere is quite sensitive to solar wind conditions. In particular the energy density of the cusp plasma depends on the pressure of the solar wind applied to the interface of the cusp and the sheath. The applied pressure in turn depends on the shape of the magnetopause and the orientation of that interface, both controlled by the direction of the interplanetary magnetic field. Magnetohydrodynamic (MHD) models provide a coarse picture of the magnetosphere at high latitudes. While generally quite realistic, these too require testing against observations because even the MHD models must make some simplifying assumptions.     

A transient MHD model applicable for the source of solar cosmic ray acceleration

A two-dimensional, time-dependent magnetohydrodynamic (MHD) model is used to describe the possible mechanisms for the source of solar cosmic ray acceleration following a solar flare. The hypothesis is based on the propagation of fast mode MHD shocks following a sudden release of energy. This model has already been used with some success for simulation of some major features of type II shocks and white light coronal transients. In this presentation, we have studied the effects of initial magnetic topology and strength on the formation of MHD shocks. We consider the plasma beta (thermal pressure/magnetic pressure) as a measure of the $\text{initial}$, relative strength of the field. During dynamic mass motion, the Alfvén Mach number is the more appropriate measure of the magnetic field's ability to control the outward motion. We suggest that this model (computed self-consistently) provides the shock wave and the disturbed mass motion behind it as likely sources for solar cosmic ray acceleration.