排序方式: 共有53条查询结果,搜索用时 31 毫秒
31.
Giuseppe Nisticò Gaetano Zimbardo 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
Recently a new model for explaining the observations of preferential heating of heavy ions in the polar solar corona was proposed ( and ). In that model the ion energization mechanism is the ion reflection off supercritical quasi-perpendicular collisionless shocks in the corona and the subsequent acceleration by the motional electric field E = −V × B/c. The mechanism of heavy ion reflection is based on ion gyration in the magnetic overshoot of the shock. The acceleration due to the motional electric field is perpendicular to the magnetic field, giving rise to large temperature anisotropy with T⊥ ? T∥, in agreement with SoHO observations. Such a model is tested here by means of a one dimensional test particle simulation where ions are launched toward electric and magnetic profiles representing the shock transition. We study the dynamics of O5+, as representative of coronal heavy ions for Alfvénic Mach numbers of 2–4, as appropriate to solar corona. It is found that O5+ ions are easily reflected and gain more than mass proportional energy with respect to protons. 相似文献
32.
根据磁层粒子动力学理论, 通过偶极磁场模型验证利用三维试验粒子轨道方法模拟近地球区(r < 8Re)带电粒子运动特征的可靠性. 在此基础上, 以太阳风和磁层相互作用的全球MHD模拟结果为背景, 利用三维试验粒子轨道方法, 对非磁暴期间南向行星际磁场背景下太阳风离子注入磁层的情形进行数值模拟, 并对北向行星际磁场背景下太阳风离子注入极尖区以及内磁层的几种不同情形进行了单粒子模拟. 模拟结果反映了南向和北向行星际磁场离子向磁层的几种典型输入过程, 揭示出行星际磁场南向时太阳风粒子在磁层内密度分布的晨昏不对称性以及其在磁鞘和磁层内的大致分布, 并得出统计规律. 模拟结果与理论预测和观测结论相一致, 且通过数值模拟发现, 行星际磁场北向时靠近极尖区附近形成的非典型磁镜结构对于能量粒子经由极尖区注入环电流区域过程有重要的影响和作用. 相似文献
33.
34.
铁电材料研究进展及其在飞行器上的应用 总被引:4,自引:0,他引:4
铁电材料是具有驱动和传感 2种功能的机敏材料,可以块材、膜材 (薄膜和厚膜 )和复合材料等多种形式应用,在微电子机械和智能材料与结构系统中具有广阔的潜在应用市场。近年来铁电陶瓷材料获得很大发展,例如弛豫型铁电陶瓷,反铁电 -铁电相变型铁电陶瓷都取得了实际应用。铁电材料中大应变弛豫型铁电单晶材料研制成功,是近 50年来取得的突破性进展。主要介绍了智能材料与结构相关的铁电材料特点及其在飞行器上的应用前景 相似文献
35.
《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2020,65(1):129-137
The nature of ionospheric losses from Venus is of essential importance for understanding the ionosphere dynamics of this unmagnetized planet. A plausible mechanism that can explain the escape of charged particles involves the solar wind interaction with the upper atmospheric layers of Venus. The hydrodynamic approach proposed for plasma expansion in the present study comprises two populations of positive ions and the neutralizing electrons, which interact with the solar wind electrons and protons. The fluid equations describing the plasma are solved numerically using a self-similar approach. The behavior of plasma density, velocity, and electric potential, as well as their reliance upon solar wind parameters have been examined. It is found that for noon midnight sites, the oxygen ion-to-electron relative density may be the main factor to enhance the ionic loss. However, the other parameters, like hydrogen density and solar wind density and velocity seem to do not stimulate the runaway ions. For lower dawn-dusk region, the plasma are composed of hydrogen and oxygen ions as well as electrons, but for higher altitudes only hydrogen ions and electrons are encountered. All ionic densities play an important role either to reduce or boost the ionic loss. The streaming solar wind velocity has no effect on the plasma escaping for lower altitudes, but it reduces the expansion at higher altitudes. 相似文献
36.
37.
S.A. Elwakil E.M. Abulwafa E.K. El-Shewy H.M. Abd-El-Hamid 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
A theoretical investigation has been made for electron acoustic waves propagating in a system of unmagnetized collisionless plasma consists of a cold electron fluid and ions with two different temperatures in which the hot ions obey the non-thermal distribution. The reductive perturbation method has been employed to derive the Korteweg–de Vries equation for small but finite amplitude electrostatic waves. It is found that the presence of the energetic population of non-thermal hot ions δ, initial normalized equilibrium density of low temperature ions μ and the ratio of temperatures of low temperature ions to high temperature ions β do not only significantly modify the basic properties of solitary structure, but also change the polarity of the solitary profiles. At the critical hot ions density, the KdV equation is not appropriate for describing the system. Hence, a new set of stretched coordinates is considered to derive the modified KdV equation. In the vicinity of the critical hot ions density, neither KdV nor modified KdV equation is appropriate for describing the electron acoustic waves. Therefore, a further modified KdV equation is derived. An algebraic method with computerized symbolic computation, which greatly exceeds the applicability of the existing tanh, extended tanh methods in obtaining a series of exact solutions of the various KdV-type equations, is used here. Numerical studies have been reveals different solutions e.g., bell-shaped solitary pulses, singular solitary “blowup” solutions, Jacobi elliptic doubly periodic wave, Weierstrass elliptic doubly periodic type solutions, in addition to explosive pulses. The results of the present investigation may be applicable to some plasma environments, such as Earth’s magnetotail region. 相似文献
38.
This review is devoted to ponderomotive forces and their importance for the acceleration of charged particles by electromagnetic
waves in space plasmas. Ponderomotive forces constitute time-averaged nonlinear forces acting on a media in the presence of
oscillating electromagnetic fields. Ponderomotive forces represent a useful analytical tool to describe plasma acceleration.
Oscillating electromagnetic fields are also related with dissipative processes, such as heating of particles. Dissipative
processes are, however, left outside these discussions. The focus will be entirely on the (conservative) ponderomotive forces
acting in space plasmas.
The review consists of seven sections. In Section 1, we explain the rational for using the auxiliary ponderomotive forces
instead of the fundamental Lorentz force for the study of particle motions in oscillating fields. In Section 2, we present
the Abraham, Miller, Lundin–Hultqvist and Barlow ponderomotive forces, and the Bolotovsky–Serov ponderomotive drift. The hydrodynamic,
quasi-hydrodynamic, and ‘`test-particle’' approaches are used for the study of ponderomotive wave-particle interaction. The
problems of self-consistency and regularization are discussed in Section 3. The model of static balance of forces (Section
4) exemplifies the interplay between thermal, gravitational and ponderomotive forces, but it also introduces a set of useful
definitions, dimensionless parameters, etc. We analyze the Alfvén and ion cyclotron waves in static limit with emphasis on
the specific distinction between traveling and standing waves. Particular attention has been given to the impact of traveling
Alfvén waves on the steady state anabatic wind that blows over the polar regions (Section~5). We demonstrate the existence
of a wave-induced cold anabatic wind. We also show that, at a critical point, the ponderomotive acceleration of the wind is
a factor of 3 greater than the thermal acceleration. Section 6 demonstrates various manifestations of ponderomotive forces
in the Earth's magnetosphere, for instance the ionospheric plasma acceleration and outflow. The polar wind and the auroral
density cavities are considered in relation to results from the Freja and Viking satellites. The high-altitude energization
and escape of ions is discussed. The ponderomotive anharmonicity of standing Alfvén waves is analyzed from ground based ULF
wave measurements. The complexity of the many challenging problems related with plasma processes near the magnetospheric boundaries
is discussed in the light of recent Cluster observations. At the end of Section 6, we consider the application of ponderomotive
forces to the diversity of phenomena on the Sun, in the interstellar environment, on newborn stars, pulsars and active galaxies.
We emphasize the role of forcing of magnetized plasmas in general and ponderomotive forcing in particular, presenting some
simple conceivable scenarios for massive outflow and jets from astrophysical objects. 相似文献
39.
Jian He Qingguo Zhang 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
In this paper, using the intensity ratio of carbon ions emission lines, we determined the optical depths at the line center of the CI at about 165.7 nm, CII at about 133.5 nm, CIII at about 117.5 nm and CIV at about 154.9 nm emission lines by escape factor treatment. For CI and CII emission lines, we discuss the intensity ratio of two lines arising from the common upper levels; while for CIII and CIV emission lines, we discuss the intensity ratio of two lines arising from the common lower levels. By introducing the measured abundance of carbon and the results of ionization balance calculations, we make an estimate of the line-of-sight physical thickness of the regions of carbon ions. This discussion will provide some results in the discussion of opacity on the solar ultraviolet (UV) or extreme-ultraviolet (EUV) spectrum. 相似文献
40.
电荷交换离子对栅极系统束流影响的数值研究 总被引:2,自引:0,他引:2
采用二维网格质点法(PIC)计算离子在离子发动机栅极系统中的运动, 通过在模型中添加离子和中性粒子电荷交换的Monte Carlo碰撞模块, 得到了电荷交换离子在栅极周围的分布及电荷交换离子的运动规律.计算结果表明:考虑电荷交换离子后, 屏栅极电流较不考虑电荷交换离子情况时增大了1.42%, 所受影响不大, 加速栅极电流由0增大到主束流电流的1.41%.模拟结果表明:加速栅极下游较远处产生的电荷交换离子, 是造成加速栅极下游面腐蚀及加速栅极电流的主要原因. 相似文献