极区中层夏季回波火箭探空观测的个例分析

利用仅发生极区中层夏季回波 (Polar Mesosphere Summer Echoes, PMSE) 现象时的ECT-02 火箭探空数据, 反演出电子数密度和尘埃电荷数密度. 这些典型的极区中层顶的基本参量为研究PMSE提供了良好的数据基础. 通过分析得出了极区中 层顶区域属于弱电离、弱耦合尘埃等离子体的结论. 根据电子数密度数扰动分析PMSE现象发现, 电子数密度的扰动与PMSE有密切的联系, 扰动强烈的地方回波就强, 扰动弱的地方回波就弱, 或者不发生PMSE 现象.      

高纬极区离子速度分布函数多项式解及非相干散射谱计算

为更准确描述高纬极区电离层离子分布函数, 分别采用弛豫碰撞模型和麦克斯韦分子碰撞模型描述玻耳兹曼方程的碰撞项, 通过求解两种模型下的输运方程, 分别得到两种模型基于麦克斯韦分布下离子分布函数的13矩近似和基于双麦克斯韦分布下离子分布函数的16矩近似. 进一步根据Sheffield理论, 利用两种模型下离子分布函数的13矩和16矩近似, 计算了非相干散射谱, 并对结果进行对比分析. 结果表明, 相对于弛豫碰撞模型, 麦克斯韦分子碰撞模型能更好地描述电离层E层中离子与中性成分的相互作用. 相对于离子分布函数的13矩近似, 16矩近似更适合描述由于电场增加导致的离子温度各向异性特征.      

损失锥电子速度分布激发的哨声波

利用一维粒子模拟方法研究了损失锥电子速度分布激发的哨声波非线性演化过程, 并与双麦克斯韦电子分布激发哨声波的情况进行了比较. 结果表明, 这两种情况下, 在线性增长阶段哨声波的主导频率 (能量最集中的一个频率) 是一样的, 波动的激发使得平行于背景磁场方向的电子温度有所提高. 比较而言,在损失锥分布情况下, 哨声波具有主导频率的波模可较早地被激发, 而在线性增长阶段, 哨声波的能量更倾向于集中在高频(短波长)波段. 部分粒子被散射到损失锥中, 而使损失锥分布得以补充. 本文还研究了不同各向异性分布和磁场强度条件下的激发过程.      

热流效应对场向电流确定的影响

给出了任意速度分布函数条件下复频率的介电函数和色散关系的求解方法. 讨论了16矩近似条件下, 场向热流对电子速度分布函数, 介电函数实部与虚部, 以及离子与电子谐振频率和阻尼率的影响, 并与平衡态时麦克斯韦分布等离子体的计算结果进行了比较. 忽略场向热流效应, 正向电子漂移速度条件下, 上行等离子线探测, 会过高估计场向电流; 负向电子漂移速度条件下, 上行等离子线探测会过低估计场向电流. 对上下行等离子线同时探测情况, 忽略热流效应同样会过高估计场向电流.      

星载大功率复杂微波部件微放电效应数值模拟

随着航天器有效载荷技术向高功率、小型化持续发展,复杂结构微波部件微放电数值模拟与阈值分析成为影响微放电分析的基础瓶颈问题。基于电磁时域有限差分计算方法与粒子模拟技术,结合二次电子发射模拟,提出了微放电电磁粒子联合仿真方法,数值模型中考虑了真实电子间的库仑力以及电子运动产生的电荷和电流变化对电磁场的影响,解决了复杂结构微波部件微放电三维数值模拟技术难题。实现了在统一的三维空间网格与时间步进行电磁场值演变计算、电子运动状态变化推进计算与二次电子产额与能量分布计算,基于得到的二次电子数目随时间变化趋势实现了微放电阈值预判,通过微放电电子随时间演化获得了微放电过程具体物理图像及放电位置,并与实际器件微放电实验进行了对比验证。结果表明,所提出的三维电磁粒子数值模拟方法可对大功率微波部件微放电效应的物理过程与具体放电位置进行三维描述,预测的阈值与微放电实验测量值吻合良好,误差小于1.2dB,验证了该方法的有效性与准确性,对于深入研究微放电效应微观物理机制、提高大功率微波部件微放电设计与分析水平具有重要意义。     

瞬态空气等离子体场的全息术研究

采用双波长双脉冲激光全息术,对有激波存在下的空气放电现象进行了研究。建立了双波长电弧折射率场方程,推导出冲击波区的压强同折射率之间的关系式,得出电弧场的压强分布.曲线及等离子体区的温度分布和电子、离子、原子、分子等粒子的数密度分布。     

大功率无线电波对高电离层的加热

根据动量方程、能量方程和电子的连续性方程，在偶极扩散的假设下，建立了地面入射的大功率无线电波加热高电离层的理论模型．作为应用，对以上方程组数值求解，计算了高电离层(150-400km)电子温度和电子密度随时间的变化．计算结果表明，对于一定参数的发射机，一定的吸收模型，电离层电子温度和密度均有明显的变化．我们发现，应用本文选取的加热参数，在电波反射点附近，电子温度有10％-25％的增加，电子密度有1％-2％左右的减少．电子温度达到稳态的时间要快于电子密度达到稳态的时间．最后，用本文的结果解释了电离层加热实验中的一些观测现象。     

银河宇宙线在电离层D层中电离的全球分布

本文从带电粒子对D层大气电离出发, 给出了宇宙线相对论粒子、非相对论粒子及低能粒子在地球大气中的电离公式, 从而给出了宇宙线在电离层D层中电子产生率q(h)和电子密度N(h)的全球分布.结果表明, 宇宙线产生的q(h)和N(h)具有明显的纬度效应, 在极区产生的q(h)和N(h)要比低纬高得多, 当截止刚度R_c=10—18GV时, q(h)的变化相差很小.太阳活动11年调制对q(h)的影响是明显的, 但远小于R_c对q(h)的影响.大气密度ρ(h)对q(h)的影响主要是随高度的变化.      

预加热时间对低电离层预加热幅度调制的影响

基于电离层连续方程和能量方程，建立预加热模式下低电离层幅度调制加热理论模型，模拟大功率电波幅度调制电离层电导率和电流随时间的变化，分析预加热时间对幅度调制产生的极低频/甚低频（ELF/VLF）强度的影响.结果表明，低电离层中的电流能够被大功率电波有效调制，可以作为ELF/VLF电波的辐射源.预加热幅度调制模式在预加热时间较长时效果更明显.在考虑能耗的情况下，当有效辐射功率为200MW及高频波的调制频率f_ELF/VLF为1kHz时，预加热幅度调制模式辐射ELF/VLF加热0.1s时效果最好，强度可提高约7.95dB.      

中国空间大功率微波部件微放电抑制表面处理技术最新进展

材料表面的二次电子发射会触发和维持空间高功率射频器件的共振雪崩放电现象,这种现象又被称为微放电效应。微放电效应是限制空间大功率微波部件应用的关键问题之一。从微放电作用的机理出发,首先介绍了两种微放电类型（单表面与双表面）的基本物理机理;然后总结了当前主流的微放电抑制方法并给出各自应用于空间大功率微波部件时的限制。针对空间大功率微波部件微放电抑制的特殊问题,综述了国内近5年来在表面处理法抑制微放电领域的研究成果并预测了微放电抑制技术的发展趋势。     

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。     

Effects of adiabaticity and non-adiabaticity of dust charge fluctuation on the propagation of the dust ion acoustic waves in inhomogeneous dusty plasma

A theoretical investigation has been made for adiabatic positive and negative dust charge fluctuations on the propagation of dust-ion acoustic waves (DIAWs) in a weakly inhomogeneous, collisionless, unmagnetized dusty plasmas consisting of cold positive ions, stationary positively and negatively charged dust particles and isothermal electrons. The reductive perturbation method is employed to reduce the basic set of fluid equations to the variable coefficients Korteweg–de Vries (KdV) equation. Either compressive or rarefactive solitons are shown to exist depending on the critical value of the ion density, which in turn, depends on the inhomogeneous distribution of the ion. The dissipative effects of non-adiabatic dust charge variation has been studied which cause generation of dust ion acoustic shock waves governed by KdV-Burger (KdVB) equation. The results of the present investigation may be applicable to some dusty plasma environments, such as dusty plasma existing in polar mesosphere region.     

Variation of energetic particle precipitation with local magnetic time

The detailed study of the precipitation of magnetospheric particles into the atmosphere is complicated by the rather complex spatial configuration of the precipitation region and its variability with geomagnetic activity. In this paper we will introduce polar oval coordinates and apply them to POES observations of 30 keV to 2.5 MeV electrons and comparable protons to illustrate the dependence of particle precipitation on local time and geomagnetic activity. These coordinates also allow an easy separation of the spatial precipitation patterns of solar and magnetospheric particles. The results indicate that (a) the spatial precipitation pattern of energetic magnetospheric electrons basically follows the pattern of the field parallel Birkeland currents up to MeV energies and (b) at least in the mesosphere the influence of magnetospheric electrons is comparable to the one of solar electrons. Implications for modeling of atmospheric chemistry will be sketched.     

Motion of Microwave Plasma Electrons in the Action of Magnetic Field

对矩形微波谐振腔中的等离子体,在高频电磁场和非均匀稳恒外磁场作用下的电子回旋共振运动进行了讨论.对电子写出了牛顿运动方程,采用数值计算方法,用计算机计算并绘出了电子运动曲线和运动轨迹.对电子的能量也作了计算.从计算结果分析了电子运动的特点和电子的能量吸收.     

Modeling the meteoric dust effect on the equatorial electrojet

Dust particles of meteoric origin in the lower E-region can affect the conductivity parameters by varying the effective collision frequency and by causing electron bite outs through the capture of ambient electrons. In magnetized plasma, neutral dust particles can alter the effective collision frequency parameters and thus affect the Pedersen and Hall conductivities in the electrojet region. The Cowling conductivity profile is determined by the height profiles of the Hall and Pedersen conductivities. The collision parameters altered by the neutral dust particles can be considerably different from those estimated from atmospheric models, in the lower E-region heights where dust particles of meteoric origin are known to exist in large numbers. A significant fraction of these dust particles may capture free electrons from the ambient medium and get charged negatively. This can result in reduction in the number density of free electrons especially below the electrojet peak where the dust particles can be present in large numbers, at least on days of large meteor showers. This, in turn, can once again alter the vertical profile of the east–west Hall current driven by the vertical Hall polarization field and under favorable conditions, can even account for the reversal of the electrojet currents below the current peak. Assuming a realistic model for the distribution of neutral dust particles, the conductivity parameters are estimated here. Conditions under which the dust particles can cause partial reversals in the electrojet currents are critically examined here.     

Cosmic dust measurements in lunar orbit

On 15th February 1992, ISAS space engineering satellite HITEN was successfully inserted into an elliptical orbit around the moon with perilune between some 100 km and 8000 km and apolune of about 50.000 km. On board was a small scientific experiment designed to detect cosmic dust particles, MDC - Munich Dust Counter. During a period of more than one year, until Hiten's hard landing on the moon surface at 10th of April 1993 (UTC), measurements of impact velocity, mass and crude flight direction of micrometeoroid particles have been performed. In total 150 cosmic dust impacts were detected and evaluated. From these measurements, the impact rate versus time and the dust flux versus distance from the moon are derived. The evidence of moon ejecta and some indications of particles which are orbiting the moon will be discussed. The spatial distribution of the measured particles is shown in lunarcentric as well as in heliocentric coordinate systems. The directional distribution is also given, showing the different populations of cosmic dust particles. Finally, the gathered data will be compared with previous results from measurements in the vicinity of the Earth and in the geomagnetic tail region.     

Experimental investigation on silica dust lofting due to charging within micro-cavities and surface electric field in the vacuum chamber

The charged dust particles can be mobilized electrostatically by the repulsion between the adjacent grains and the surface electric field due to the incoming electron current and the charge accumulation within the micro-cavities. In this study, the experimental results of the initial vertical launching velocities and the maximum dust heights are compared with the estimated values for the lofted spherical dust grains by the patch surface charging equations. Silica particles with the sizes between <6 and 45?µm in radius are loaded on a graphite plate, and they are exposed to the electron beam with 450?eV energy under 4?×?10^?3?Pa vacuum chamber pressure. During the first set of the experiments, the dust samples are tested without an initial compression process and an additional horizontal electric field. Second, the dust samples are compressed by two different weights in order to increase the packing density under approximately 780.7?Pa and 3780?Pa. Finally, the dust grains are placed between the two parallel aluminum plates to apply approximately 2000?V/m and 4800?V/m horizontal electric field. A high-speed camera is used to record the transportation of the dust grains together with a microscopic telescope, and the results point out that the patch surface dust-charging model estimations are in agreement with the first experiments. On the other hand, the dust particles from the compressed samples are lofted with higher velocities than the estimations, and the number of the dust lofting observations decreases significantly, which demonstrates the importance of the micro-cavities and the increased charging requirement to overcome the contact forces. When the horizontal electric field is present, the initial vertical launching velocities are measured to be lower than the other experiments, which can be attributed to the decreased charging requirement for the dust lofting as a result of inter-particle collisions and rolling motion. According to the experimental results, the electrostatic dust transportation can be controlled not only by the ambient plasma and the solar irradiation on the airless planetary bodies, but also by the surface properties such as the contact surfaces between the dust grains, the number of the micro-cavities related to the packing density, and the presence of the horizontal electric field contributing to the external forces by other particle motions.     

On the effects of electron-cyclotron masers during flares

First recognized by Wu and Lee (Ap. J. 230, 621, 1979), electron-cyclotron masers can be activated under very mild conditions. Large growth rates can occur even for relatively mild anisotropies in the electron velocity distribution, e.g., the one-sided loss cones that commonly occur when electrons with small pitch angles precipitate into high density regions at the footpoints of flaring loops while others are reflected in the converging field in the corona. Maser action can plausibly occur at the second harmonic of the local gyrofrequency and so explain certain very bright (? 10¹⁰ K) microwave bursts from the sun and other stars. However, the preponderance of the energy is at the first harmonic.We suggest that masers operating at the local gyrofrequency in a flaring loop generate radiation at decimeter wavelengths that is a significant fraction of the total energy of the flare, in fact (and not coincidentally) comparable with the energy in electrons associated with hard X-ray bursts. Essentially all of the radio energy is trapped in the corona and serves to produce localized heating in a volume large compared with the energy release region. Thus it can transfer energy by radiation from one magnetic loop to another, possibly inducing further instabilities, and spreading the course of the flare. Eventually the energy probably escapes the corona as soft X-rays. The electron-cyclotron maser saturates by extracting the perpendicular energy of the electrons, thereby diffusing them into the loss cone at the maximum possible rate; the enhanced precipitation into the footpoints can produce bright emission in hard X-rays, EUV and Hα and remove any necessity for directive acceleration in the energy release region.Details of the proposed mechanism and effects are contained in two papers by Melrose and Dulk (Ap. J. 259, 1982).This work was sponsored by NASA under grants NAGW-91 and NSG-7287 to the University of Colorado.