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.     

Study of TEC changes during geomagnetic storms occurred near the crest of the equatorial ionospheric ionization anomaly in the Indian sector

GPS satellites data obtained at Bhopal (23.16° N, 77.36° E, geomagnetic latitude 14.23° N) India were analyzed to study the TEC changes during several geomagnetic storms (−300 nT < Dst < −50 nT) occurred in 2005–2007. We had segregated the storms according to the Dst value, i.e. moderate storms (−100 nT < Dst ? −50 nT), strong storms (−150 nT < Dst < −100 nT), and severe storms (Dst less than −150 nT). Total of 21 geomagnetic storms (10 moderate, 9 strong, 2 severe) are considered for the present study. Deviation in vertical total electron content (VTEC) during the main phase of the storm was found to be associated with the prompt penetration of electric field originated due to the under-shielding and over-shielding conditions for almost all geomagnetic storms discussed in this paper. For most of the storms VTEC shows the positive percentage deviation during the main phase while it shows positive as well as the negative deviation during the recovery phase of the storms. The −80% deviation in VTEC was found for geomagnetic storm occurred on July 17, 2005 and the negative trend continued for recovery phase of the storm. This was mainly due to the thermospheric composition changes by Joule heating effect at auroral latitudes that generate electric field disturbance at low latitudes. Traveling ionospheric disturbances (TIDs) were responsible for the formation of wave like nature in VTEC for the storms occurred on May 15, 2005, whereas it was not observed for storm occurred on August 24, 2005.     

Cassini Plasma Spectrometer Investigation

The Cassini Plasma Spectrometer (CAPS) will make comprehensive three-dimensional mass-resolved measurements of the full variety of plasma phenomena found in Saturn’s magnetosphere. Our fundamental scientific goals are to understand the nature of saturnian plasmas primarily their sources of ionization, and the means by which they are accelerated, transported, and lost. In so doing the CAPS investigation will contribute to understanding Saturn’s magnetosphere and its complex interactions with Titan, the icy satellites and rings, Saturn’s ionosphere and aurora, and the solar wind. Our design approach meets these goals by emphasizing two complementary types of measurements: high-time resolution velocity distributions of electrons and all major ion species; and lower-time resolution, high-mass resolution spectra of all ion species. The CAPS instrument is made up of three sensors: the Electron Spectrometer (ELS), the Ion Beam Spectrometer (IBS), and the Ion Mass Spectrometer (IMS). The ELS measures the velocity distribution of electrons from 0.6 eV to 28,250 keV, a range that permits coverage of thermal electrons found at Titan and near the ring plane as well as more energetic trapped electrons and auroral particles. The IBS measures ion velocity distributions with very high angular and energy resolution from 1 eV to 49,800 keV. It is specially designed to measure sharply defined ion beams expected in the solar wind at 9.5 AU, highly directional rammed ion fluxes encountered in Titan’s ionosphere, and anticipated field-aligned auroral fluxes. The IMS is designed to measure the composition of hot, diffuse magnetospheric plasmas and low-concentration ion species 1 eV to 50,280 eV with an atomic resolution M/ΔM ∼70 and, for certain molecules, (such asN ₂ ⁺ and CO⁺), effective resolution as high as ∼2500. The three sensors are mounted on a motor-driven actuator that rotates the entire instrument over approximately one-half of the sky every 3 min.This revised version was published online in July 2005 with a corrected cover date.     

马尔科夫尼可夫规则机理的讨论

不对称烯烃与不对称试剂进行亲电加成反应时,遵守马尔科夫尼可夫规则,本文从生成碳正离子和环状高价正离子的两种反应途径对其反应机理加以讨论,并指出决定两种途径的主要因素.     

IMF Direction Derived from Cycloid-Like Ion Distributions Observed by Mars Express

Although the Mars Express (MEX) does not carry a magnetometer, it is in principle possible to derive the interplanetary magnetic field (IMF) orientation from the three dimensional velocity distribution of pick-up ions measured by the Ion Mass Analyser (IMA) on board MEX because pick-up ions' orbits, in velocity phase space, are expected to gyrate around the IMF when the IMF is relatively uniform on a scale larger than the proton gyroradius. During bow shock outbound crossings, MEX often observed cycloid distributions (two dimensional partial ring distributions in velocity phase space) of protons in a narrow channel of the IMA detector (only one azimuth for many polar angles). We show two such examples. Three different methods are used to derive the IMF orientation from the observed cycloid distributions. One method is intuitive (intuitive method), while the others derive the minimum variance direction of the velocity vectors for the observed ring ions. These velocity vectors are selected either manually (manual method) or automatically using simple filters (automatic method). While the intuitive method and the manual method provide similar IMF orientations by which the observed cycloid distribution is well arranged into a partial circle (representing gyration) and constant parallel velocity, the automatic method failed to arrange the data to the degree of the manual method, yielding about a 30° offset in the estimated IMF direction. The uncertainty of the derived IMF orientation is strongly affected by the instrument resolution. The source population for these ring distributions is most likely newly ionized hydrogen atoms, which are picked up by the solar wind.     

Coupling plasma plume of a low-power magnetically shielded Hall thruster with a hollow cathode

The coupling region of a Hall thruster with a hollow cathode is the region between the cathode and the thruster plume. The characteristics of plasma in that region are complicated and strongly associated with the thruster working conditions and the cathode position. In this paper, a laboratory 100 W class magnetically shielded Hall thruster was coupled with a hollow cathode. Optical imaging and electrostatic probe were employed to monitor and scan the plasma plume. Plume characteristics in the coupling region in non-self-sustained mode and self-sustained mode were compared. Evolution of the coupling plume with the cathode position was studied. Experiments show that, when turning the thruster into self-sustained mode or moving the cathode further away axially, the discharge current can be reduced by 6.4–10.6% restraining the electron current and improving ionization. In particular, when the cathode is moved further, the electron conduction near the channel walls is suppressed. The electron current is reduced by 27.4% and the ion beam current is increased by 7%. Overall, this work shows that the working mode of the thruster and the position of the cathode greatly affect the coupling plasma plume. Both play an important role in improving the utilizations of propellant and current.     

阳极层霍尔推力器内轮辐效应不稳定性研究

为研究圆柱形阳极层霍尔推力器内轮辐效应的不稳定性,利用高速相机和静电探针得到1-2-1模式、1-2-3-1模式和1-2-3-2-1模式的轮辐分裂与合并现象。随着磁感应强度由205Gs增加到225Gs,轮辐个数m由1增加到3。轮辐的分裂与合并模式增多,且轮辐的旋转频率随之由25kHz提高到40kHz～50kHz。轮辐效应的存在是电子密度分布函数的宏观体现,动理论方程中力F的波动引起了轮辐的分裂,随着轮辐个数m的增加,电子分布的低频大幅度波动逐渐演变为小幅度高频率的波动。电子密度分布函数的波动引起的轮辐效应产生了角向分布的电场强度与磁场共同作用,增强了电子轴向漂移运动。     

毛细管放电型脉冲等离子体推力器输出特性分析

为了研究毛细管放电型脉冲等离子体推力器输出特性,借助电学诊断手段展开实验研究,获得了推力器典型放电波形,系统研究了不同毛细管内径和施加电压对等离子体等效阻抗、沉积能量效率的影响规律。利用微冲量测量台架,测试了不同参数下毛细管推力器输出元冲量,并通过计算获得了推力器比冲、总体效率的变化规律。实验结果表明,当毛细管内径不断增大时,能量沉积效率不断下降,元冲量下降,比冲降低。主电容电压增大时,放电能量不断增大,能量沉积效率降低,元冲量和单次等效烧蚀质量不断增大,但推力器比冲和总体效率均先增加并趋于稳定。当毛细管腔体长度为16mm,内径3mm,主电容2.5μF,充电电压为2kV时,输出元冲量350.79±7.50μN?s,比冲531s,总体效率可达18.3%。     

霍尔推力器不同壁面侵蚀对低频振荡特性影响研究

基于霍尔推力器一维准中性流体模型,对放电壁面侵蚀对低频振荡特性的影响进行了数值模拟研究。通过改变霍尔推力器放电通道的横截面积,研究了霍尔推力器寿命期内通道受离子溅射后,放电电流振荡特性变化。研究结果显示,横截面积从25cm2增大到37cm2时,放电电流振荡幅值增加,振荡频率基本不变;继续增加横截面积,放电电流振荡幅值减小,振荡频率增加。理论分析表明:通道侵蚀面积增大,导致离子碰撞频率变化,进而引起振荡特性变化。     

面向立方星变轨任务的机动控制策略

为了实现立方星在轨飞行与变轨,基于模块化推进器系统提出混合控制策略实现微小卫星轨道持续变化任务需求。首先,针对多单元立方星单一主推进器的结构部署,基于高斯变分方程采用连续低推进力实现轨道机动变化。为了实现对立方星主推进器的指向调整,基于姿态动力学模型利用PD连续姿态控制求得所需扭矩,实现对立方星的指向角和指向角速度调节。针对配置的微脉冲等离子推进器(μ-PPT)不连续的特点,通过搜寻μ PPT最优脉冲序列组合获得实际扭矩,满足对外部干扰的持续补偿以及立方星的姿态稳定和指向调整操作需求。此外,引入姿态误差敏感度阈值,使姿态控制器在能够提高系统鲁棒性的同时减少μ-PPT消耗。最后,通过对3U立方星在轨飞行与变轨的具体案例分析,表明所提出的基于微推进器系统的混合控制策略能够实现立方星轨道机动变化需求。