等离子体湍动对准垂直激波中粒子加速的影响

本文利用试验粒子方法研究了在考虑等离子体湍动的情况下带电粒子在准垂直激波中的加速, 在计算中, 我们采用组合模型来拟合等离子体湍动. 计算结果表明, 在存在等离子体湍动的情况下, 粒子可横越背景磁场运动, 从而被激波反射的上游粒子在到达下游后可被等离子体湍动散射回到上游, 并再次被激波反射并加速, 这样的过程可重复很多次, 因而粒子可被加速到很高的能量. 我们还研究了激波角, 粒子的初始能量和等离子体湍动的强度, 以及相干长度和两种湍动组分强度比与加速粒子的能谱之间的关系.     

基于测试粒子模拟的垂直无碰撞激波对离子的加速研究

本文利用测试粒子模拟的方法研究离子在通过垂直无碰撞激波结构时的加速.我们首先探究了在理想激波条件下,离子通过激波结构后的能量增益与其初始参数(包括回旋相位角、初始位置和上游平均能量)的关系;然后进一步探索了离子通过由自洽的一维混合模拟给出的更接近真实的激波结构时获得的加速,研究了激波内部的电场和磁场结构对离子能量增益的...     

太阳风湍流和磁层亚暴的一种机制

太阳风的动量涨落将通过磁层边界在磁尾激发磁流体力学波。快磁声波携带扰动能量传到等离子体片中,发展为激波,或者通过激波的相互作用而耗散能量,使等离子体加热。等离子体片中的随机费米加速机制,使麦克斯韦分布尾巴部分的高能量粒子被加速到更高能。在宁静态时,加热、加速与耗散过程平衡。当太阳风的动量或者其涨落较大时,整个加热和加速过程加剧,更多的高能粒子产生,并从等离子体片中逃逸,形成高速的等离子体流注入近地轨道和极区,表现为磁层亚暴过程。利用这种机制,可以解释地球磁层亚暴的定性特征。     

磁场偶极化过程中磁尾离子加速:Ⅱ上行离子速度和能量的变化

根据采用动力学方程对亚暴期间磁尾磁场向偶极形弛豫过程中离子分布函数的模拟结果 ,研究了磁尾来自电离层的O+,H+和He+离子的速度及能量随时间的变化 .主要结果为 :（1 ）离子的加速及能量变化主要发生在磁场偶极化过程的中期 ,对应的地心距离位于- 1 2RE到 - 8RE 之间 ;（2 ）垂直于磁场方向上离子加速及能量变化较快 ,平行方向上较慢 ;（3）轻离子较重离子加速及能量变化快 ,磁场偶极化终结 ,3种离子的能量均可增加 2 0 0倍左右 ;（4）初始能量较高时 ,离子加速及能量变化较快 ,离子最终获得的能量较大 .理论计算的磁尾离子能量在磁场偶极化过程终了可达 1 0 2 keV的量级 ,这与观测结果一致 .     

磁场重联中电子加速问题的物理分析和数值研究

观测表明耀斑中电子加速发生在软X射线耀斑环上方的磁重联区域.在重联电流片中被super Dreicer电场直接加速似乎是产生能量在10keV～10MeV之间高能电子的最直接的方式.本文的结果证明纵向电磁场可以有效地将电子“锁”在重联电流片上，使得横向电场得以直接加速电子.对于解释产生相对论性粒子的脉冲式耀斑，这可能是一个有效的机制.     

日冕物质抛射与太阳粒子事件

本文介绍了２０多年来对日冕物质抛射与太阳粒子事件的关系和太阳粒子事件的源等方面的研究成果和进展。大量的研究表明，太阳粒子事件源于日冕物质抛射并被日冕和行星际激波加速和控制。在无耀斑源的日冕和行星际激波加速和控制。只有极少数产生太阳粒子事件，并且这些事件中多数为低能粒子事件。这些相关日冕物质抛射的共同特征是：无相关的强Ｘ射线爆发，产生的行星际激波速度较快，无激波加速，无Ⅱ和Ⅳ米波爆发。几乎所有的产生     

Alfven行波涌浪携带的场向电场──极光粒子加速机制

提出一个剪切Ａｌｆｖｅｎ波加速极光粒子的新模式。频率远小于离子回旋频率的Ａｌｆｖｅｎ波由磁层向电离层传播会演化成孤波，当场向电流超过离子声不稳定性的临界电流时，激发离子声不稳定性，波与粒子的相互作用产生反常阻尼使Ａｌｆｖｅｎ波演化成行波涌浪。它携带一个方向向上的平行电场，加速极光电子形成分立极光。对等离子体密度、电场及其对应的电势进行了数值计算，结果发现满足磁层加速区条件形成Ａｌｆｖｎ行波涌浪，提供足够强的加速粒子的电场。     

等离子体片中能量离子的空间分布--Cluster/RAPID观测数据分析

本文根据Cluster卫星上的粒子成像质谱仪（RAPID）探测器在穿越地球等离子体片过程中的观测数据,统计研究了等离子体片中能量离子能量密度的空间分布（氢离子能量范围从40keV到1500keV,氦离子和氧离子从10keV到1500keV）,并且给出了离子能量密度在不同地磁活动时期随GSE Z向分布的剖面.研究表明能量离子的能量密度以及能量密度的梯度与地磁活动指数Kp之间存在近似线性的关系.观测结果表明形成这种分布变化的主要原因是在地磁活动期间在电流片附近离子能量密度的增加,特别是其中的重离子成分增加更为显著.本文通过一个简化的电流片模型的数值计算,定性地研究了形成能量离子空间分布的机理.计算表明重离子在电流片中可以获得更多的能量,电流片加速可能是形成能量密度分布变化的一种可能的机制.     

磁场重联中的电子加速机制的数值模拟研究

在应用2.5维混合模拟方法研究Petschek模型磁场重联的基础上,考察了试验电子被加速的特征. 模拟结果表明,稳态的低频重联场能将少量试验电子加速到高能,电子的能谱为幂律谱,但总体分布函数未发生显著变化. 电子在整个加速过程中被束缚在低磁场的加速区内,由重联产生的感应电场Ey分量对其直接加速,根据加速时间和加速区域可以将这些电子分为两种情况：初始位于加速区和漂移到加速区被加速.     

地球弓激波前的低频磁流体波

一、引言 在地球弓激波前存在着低频磁流体波。这种低频磁流体波是太阳风在地球弓激波上的反射粒子和太阳风粒子之间相互作用产生的。根据人造卫星的观测资料可以得到,在地球弓激波前,Pc3-4脉动频率范围内的低频磁流体波的主频率和行星际磁场强度     

Particle acceleration and transport in the inner heliosphere

In the solar system, our Sun is Nature’s most efficient particle accelerator. In large solar flares and fast coronal mass ejections (CMEs), protons and heavy ions can be accelerated to over ~GeV/nucleon. Large flares and fast CMEs often occur together. However there are clues that different acceleration mechanisms exist in these two processes. In solar flares, particles are accelerated at magnetic reconnection sites and stochastic acceleration likely dominates. In comparison, at CME-driven shocks, diffusive shock acceleration dominates. Besides solar flares and CMEs, which are transient events, acceleration of particles has also been observed in other places in the solar system, including the solar wind termination shock, planetary bow shocks, and shocks bounding the Corotation Interaction Regions (CIRs). Understanding how particles are accelerated in these places has been a central topic of space physics. However, because observations of energetic particles are often made at spacecraft near the Earth, propagation of energetic particles in the solar wind smears out many distinct features of the acceleration process. The propagation of a charged particle in the solar wind closely relates to the turbulent electric field and magnetic field of the solar wind through particle-wave interaction. A correct interpretation of the observations therefore requires a thorough understanding of the solar wind turbulence. Conversely, one can deduce properties of the solar wind turbulence from energetic particle observations. In this article I briefly review some of the current state of knowledge of particle acceleration and transport in the inner heliosphere and discuss a few topics which may bear the key features to further understand the problem of particle acceleration and transport.     

Injection and acceleration of H+ and He2+ at Earth’s bow shock

We have performed a number of one-dimensional hybrid simulations (particle ions, massless electron fluid) of quasi-parallel collisionless shocks in order to investigate the injection and subsequent acceleration of part of the solar wind ions at the Earth’s bow shock. The shocks propagate into a medium containing magnetic fluctuations, which are initially superimposed on the background field, as well as generated or enhanced by the electromagnetic ion/ion beam instability between the solar wind and backstreaming ions. In order to study the mass (M) and charge (Q) dependence of the acceleration process He²⁺ is included self-consistently. The upstream differential intensity spectra of H⁺ and He²⁺ can be well represented by exponentials in energy. The e-folding energy E_c is a function of time: E_c increases with time. Furthermore the e-folding energy (normalized to the shock ramming energy E_p) increases with increasing Alfvén Mach number of the shock and with increasing fluctuation level of the initially superimposed turbulence. When backstreaming ions leave the shock after their first encounter they exhibit already a spectrum which extends to more than ten times the shock ramming energy and which is ordered in energy per charge. From the injection spectrum it is concluded that leakage of heated downstream particles does not contribute to ion injection. Acceleration models that permit thermal particles to scatter like the non-thermal population do not describe the correct physics.     

Energetic particle investigation using the ERNE instrument

During solar flares and coronal mass ejections, nuclei and electrons accelerated to high energies are injected into interplanetary space. These accelerated particles can be detected at the SOHO satellite by the ERNE instrument. From the data produced by the instrument, it is possible to identify the particles and to calculate their energy and direction of propagation. Depending on variable coronal/interplanetary conditions, different kinds of effects on the energetic particle transport can be predicted. The problems of interest include, for example, the effects of particle properties (mass, charge, energy, and propagation direction) on the particle transport, the particle energy changes in the transport process, and the effects the energetic particles have on the solar-wind plasma. The evolution of the distribution function of the energetic particles can be measured with ERNE to a better accuracy than ever before. This gives us the opportunity to contribute significantly to the modeling of interplanetary transport and acceleration. Once the acceleration/transport bias has been removed, the acceleration-site abundance of elements and their isotopes can be studied in detail and compared with spectroscopic observations.     

Ion dynamics associated with substorm dipolarization fronts

We report where and how ions are accelerated in the proximity of earthward propagating dipolarization fronts(DFs) in the magnetotail during a magnetospheric substorm on February 15, 2008. Two DFs were observed by multiple THEMIS spacecraft in the near-Earth magnetotail(~?10 Re). We studied the ion dynamics associated with these DFs by comparing observed results with large scale kinetic(LSK) simulation results. The LSK simulation reproduced the sudden ion energy flux enhancement concurrent with the arrival of the DF at the satellite locations. We found that ions can be accelerated to more than 100 keV energy at the DF. These ions were initially non-adiabatically accelerated near magnetic reconnection site and then still non-adiabatically accelerated at the DF structure.     

Arrival of the first relativistic solar protons and conditions in the solar corona

When solar cosmic rays (SCRs) can be observed with ground-based equipment (ground-level enhancements, GLEs), events are often characterized by a rapid increase in the relativistic proton intensity during the initial phase, which makes it possible to estimate the time of particle escape from the solar corona. This phase attracts attention of researchers owing to its closeness in time to the instant of particle acceleration. It is known that the observed SCR characteristics bear traces of many physical processes, including different acceleration mechanisms the relative role of which is still unclear. Flare processes and acceleration by a shock, related to coronal mass ejection (CME), are the main pretenders to the role of SCR accelerator. Several powerful solar proton events during cycle 23 are considered in the work, and the release time of the first particles from the corona and the dynamics of CMEs have been estimated. The time series of the X-ray and radio bursts, close in time to particle escape, are analyzed. The conclusion have been drawn that the first relativistic particles were most probably accelerated during flare processes.     

Magnetotail dipolarization fronts and particle acceleration: A review

In this paper, the particle acceleration processes around magnetotail dipolarization fronts(DFs) were reviewed. We summarize the spacecraft observations(including Cluster, THEMIS, MMS) and numerical simulations(including MHD, testparticle, hybrid, LSK, PIC) of these processes. Specifically, we(1) introduce the properties of DFs at MHD scale, ion scale, and electron scale,(2) review the properties of suprathermal electrons with particular focus on the pitch-angle distributions,(3)define the particle-acceleration process and distinguish it from the particle-heating process,(4) identify the particle-acceleration process from spacecraft measurements of energy fluxes, and(5) quantify the acceleration efficiency and compare it with other processes in the magnetosphere(e.g., magnetic reconnection and radiation-belt acceleration processes). We focus on both the acceleration of electrons and ions(including light ions and heavy ions). Regarding electron acceleration, we introduce Fermi,betatron, and non-adiabatic acceleration mechanisms;regarding ion acceleration, we present Fermi, betatron, reflection, resonance, and non-adiabatic acceleration mechanisms. We also discuss the unsolved problems and open questions relevant to this topic, and suggest directions for future studies.     

Long-duration high-energy proton events observed by GOES in October 1989

We consider the prolonged injection of the high-energy (> 10 MeV) protons during the three successive events observed by GOES in October 1989. We apply a solar-rotation-stereoscopy approach to study the injection of the accelerated particles from the CME-driven interplanetary shock waves in order to find out how the effectiveness of the particle acceleration and/or escape depends on the angular distance from the shock axis. We use an empirical model for the proton injection at the shock and a standard model of the interplanetary transport. The model can reproduce rather well the observed intensity-time profiles of the October 1989 events. The deduced proton injection rate is highest at the nose of the shock; the injection spectrum is always harder near the Sun. The results seem to be consistent with the scheme that the CME-driven interplanetary shock waves accelerate a seed particle population of coronal origin.