Ion-acoustic waves in unmagnetized collisionless weakly relativistic plasma of warm-ion and isothermal-electron using time-fractional KdV equation

Collisionless unmagnetized plasma consisting of a mixture of warm ion-fluid and isothermal-electron is considered, assuming that the ion flow velocity has a weak relativistic effect. The reductive perturbation method has been employed to derive the Korteweg–de Vries (KdV) equation for small – but finite-amplitude electrostatic ion-acoustic waves in this plasma. The semi-inverse method and Agrawal’s method lead to the Euler–Lagrange equation that leads to the time fractional KdV equation. The variational-iteration method given by He is used to solve the derived time fractional KdV equation. The calculations show that the fractional order may play the same rule of higher order dissipation in KdV equation to modulate the soliton wave amplitude in the plasma system. The results of the present investigation may be applicable to some plasma environments, such as space-plasmas, laser-plasma interaction, plasma sheet boundary layer of the earth’s magnetosphere, solar atmosphere and interplanetary space.     

高压脉冲电子束的控制及其对焊缝形貌影响

研制出一台150 kV/30 kW高压脉冲电子束焊机,介绍了控制脉冲束流产生的偏压脉冲电源拓扑电路结构及脉冲束流频率、占空比、束流基值、束流峰值的调节控制技术.在0~1 kHz频率范围内,该电源可输出最大幅值200 mA的脉冲电子束束流,且工艺参数调节方便.分别采用脉冲束流与连续束流电子束工艺焊接了1Cr18Ni9Ti奥氏体不锈钢,对不同工艺的焊缝形貌进行了对比分析.与连续束流电子束焊接工艺相比,采用脉冲电子束焊接工艺的焊缝熔深增加,深宽比增大;对于脉冲电子束焊接工艺,占空比给定时,随着束流频率增加,焊接缺陷减少.试验结果表明:脉冲束流频率、占空比是影响焊缝成形的关键工艺参数;脉冲调制方式控制偏压是获得高压脉冲电子束的理想控制技术之一.      

大功率无电极高密度等离子体电磁推进概述

无电极高密度等离子体电磁推进技术已成为未来深空探测、载人航天和货运、太阳能电站以及航天器在轨服务与维护等空间任务中极具竞争力的核心推进技术之一。在梳理不同无电极等离子体电磁加速机制基础上,开展大功率无电极高密度等离子体电磁推进技术性能对比,给出新概念无电极场反构型电磁推进技术向未来超大功率拓展的优势和发展潜力,同步分析了该技术亟需解决的关键基础问题,旨在为中国新概念场反构型电磁推进技术的研发提供理论基础。     

Heliopause stability revisited: dispersion analysis and numerical simulations

The heliopause, a surface separating the tenuous hot heliosheath flow and the dense, strongly magnetized interstellar flow, is subject to instabilities of the Rayleigh–Taylor and Kelvin–Helmholtz types. The dynamic evolution of this discontinuity is of considerable importance for understanding the neutral atom and cosmic-ray filtration at the interface. Here, we investigate the stability of the upwind heliopause in the presence of charge exchange collisions using both an analytic (dispersion relation) approach and a numerical model that includes the interstellar magnetic field. The linear analysis yields a cubic dispersion relation that admits imaginary solutions for the full range of wavenumbers, implying that the stagnation point on the heliopause is unconditionally Rayleigh–Taylor unstable to small perturbations propagating parallel to the discontinuity surface. We confirm this result by following the nonlinear development of the instability with a time-dependent simulation using a four fluid MHD-neutral numerical code. For the typical solar wind and LISM conditions, we obtain cyclical evolution of the upwind heliopause with a period of the order of 100 years. We also identify two areas of space physics where the instability may have important implications.     

烧蚀型脉冲等离子体推力器能量分配机理

脉冲等离子体推力器（以下简称PPT）效率低下的缺点一直为使用者所诟病,但过去对其能量分配机理的研究十分匮乏,难以为高效率PPT的设计提供参考。针对这一现状,本研究以平板式烧蚀型PPT为对象,对推力器在4种不同放电能量（能量比1：2：3：4）下工作的电压、电流和脉冲烧蚀质量进行测量,并根据测量结果估算PPT的元冲量、比冲、效率等推进性能。此外,本研究还建立了能估算PPT推进剂利用率的数值模型,并用该模型分析实验研究结果。研究结果表明,能量利用率和推进剂利用率低下同时导致PPT推力器效率低下,随着放电能量的增加,PPT的能量利用率和推力器效率上升,分别从5.07%和2.88%逐渐提高至16.46%和5.23%,但推进剂利用率反而降低,由56.8%逐渐降低至31.8%。     

Global MHD simulations for southward IMF: a pair of wings in the flanks

Global magnetohydrodynamic (MHD) simulations have shown that for southward interplanetary magnetic field nightside reconnection takes place only in a limited spatial scale in the cross-tail direction. Between the end of the nightside reconnection line and the flank magnetopause are regions of closed magnetic field lines which move relatively slowly tailward, compared with the magnetosheath flow on the far side and the jet flow produced by nightside reconnection on the side closer to the midnight. The magetosphere appears to have a pair of extended wings on the nightside. Further refinement of the simulations shows that the wings are not produced by the numerical effects. Similar features have been observed previously and also shown in different simulation models. The existence of the wings in the simulations indicates that the solar wind momentum is transferred to the closed magnetosphere if the simulations are relevant to reality.     

脉冲射流强化圆柱喷流混合的三维数值模拟

对利用脉冲射流强化圆柱喷流混合的流场进行了数值模拟,这项工作将高频高强度信号射流射入亚音剪切层以强化喷流混合.利用有限体积法和重整化群(RNG)k-ε湍流模型求解N-S方程.分别进行了低亚音马赫数及高亚音马赫数喷流直接排入空气的数值模拟.主要计算3个状态:未受激励的状态,斯德鲁哈尔数St分别为0.2和0.4时的状态.数值模拟结果显示,脉冲激励引起喷流在与激励源平行的平面迅速扩展,在与之垂直的平面收缩,当脉冲射流激励的St在0.2附近时,相关的混合较好,而且少量的射流流量可以极大地增加速度的衰减率.      

Study of three dimensional structure of the fast convection flow in the plasma sheet by MHD simulations on the basis of spontaneous fast reconnection model

Three dimensional structure of the fast convection flow in the plasma sheet is examined using magnetohydrodynamic (MHD) simulations on the basis of spontaneous fast reconnection model. The fast flow observed in the near-Earth magnetotail is one of the key phenomena in order to understand the causal relationship between magnetic substorm and magnetic reconnection. In this paper, we focus on this earthward fast flow in the near-Earth magnetotail. Our previous studies have shown that the fast reconnection produces the Alfvénic fast reconnection outflow and drastic magnetic field dipolarization in the finite extent. In this paper, the results of our simulations are compared with those of the in-situ observations in the geomagnetotail. They have consistent temporal profiles of the plasma quantities. It is suggested that the fast convection flows are caused by spontaneous fast reconnection.     

Comparative study of plasma wave activity in the plasma sheet boundary and near Earth plasma sheet

The general structure of low frequency wave activity in the Earth's plasma sheet and its boundary layer is studied on the basis of the measurements made by ‘Prognoz-8’ satellite in the northern night and morning parts of the magnetotail. Pronounced wave activity is permanently observed in the high latitude parts of the plasma sheet boundary layer. The level of perturbations diminishes when a spacecraft moves towards tail lobes and drops rather sharply when it moves to the central plasma sheet. The peaks near the low hybrid resonance frequency (correlating with the local strength of the magnetic field) are evident in the electric field fluctuations spectra. A plasma instability of low hybrid type driven by transverse current is though to be the possible candidate for the excitation of these waves. Wave activity in tail lobes is related mainly to the isolated hot and cold plasma streams.     

Organic chemistry in Titan's atmosphere: new data from laboratory simulations at low temperature.

Many experiments have already been carried out to simulate organic chemistry on Titan, the largest satellite of Saturn. They can provide fruitful information on the nature of minor organic constituents likely to be present in Titan's atmosphere, both in gas and aerosol phases. Indeed, all the organic compounds but one already detected in Titan's atmosphere have been identified in simulation experiments. The exception, C4N2, as well as other compounds expected in Titan from theoretical modeling, such as other N-organics, and polyynes, first of all C6H2, have never been detected in experimental simulation thus far. All these compounds are thermally unstable, and the temperature conditions used during the simulation experiments were not appropriate. We have recently started a new program of simulation experiments with temperature conditions close to that of Titan's environment. It also uses dedicated analytical techniques and procedures compatible with the analysis of organics only stable at low temperatures, as well solid products of low stability in the presence of O2 and H2O. Spark discharge of N2-CH4 gas mixtures was carried out at low temperature in the range 100-150 K. Products were analysed by FTIR, GC and GC-MS techniques. GC-peaks were identified by their mass spectrum, and, in most cases, by comparison of the retention time and mass spectrum with standard ones. We report here the first detection in Titan simulation experiments of C6H2 and HC5N. Their abundance is a few percent relative to C4H2 and HC3N, respectively. Preliminary data on the solid products indicate an elemental composition corresponding to (H11C11N)n. These results open new prospects in the modeling of Titan's haze making.     

A spectroscopic measurement of high velocity spray plasma from an M-class flare and coronal mass ejection

The M1.5-class flare and associated coronal mass ejection (CME) of 16 February 2011 was observed with the Extreme ultraviolet Imaging Spectrometer on board the Hinode spacecraft. Spray plasma associated with the CME is found to exhibit a Doppler blue-shift of 850 km s^?1 – one of the largest values reported from spectroscopy of the solar disk and inner corona. The observation is unusual in that the emission line (Fe xii 193.51 Å) is not observed directly, but the Doppler shift is so large that the blue-shifted component appears in a wavelength window at 192.82 Å, intended to observe lines of O v, Fe xi and Ca xvii. The Fe xii 195.12 Å emission line is used as a proxy for the rest component of 193.51 Å. The observation highlights the risks of using narrow wavelength windows for spectrometer observations when observing highly-dynamic solar phenomena. The consequences of large Doppler shifts for ultraviolet solar spectrometers, including the upcoming Multi-slit Solar Explorer (MUSE) mission, are discussed.     

Electron plasma waves in the solar wind: AMPTE/IRM and UKS observations

Selected events of plasma wave and electromagnetic emissions in the earth's electron fore-shock region have been studied. Strong emissions are observed in the plasma-wave band when the site of the satellite is magnetically connected to the bow shock. These emissions are generally highly fluctuating. Under certain conditions one observes electromagnetic radiation at the second harmonic produced locally. Electromagnetic emission generated at a position far away from the site of the spacecraft is occasionally detected giving rise to remote sensing of the bow shock. These emissions are related to energetic electron fluxes.     

Indo-German low-latitude project deos: plasma bubbles in the post sunset and nighttime sector

Two spread-F flights were performed under equinox conditions in April and September 1998 from the Indian low-latitude station SHAR. Both flights detected plasma bubbles confined to a narrow longitudinal extent. Plasma parameters are measured under two different conditions in the post-sunset ionosphere; when the F-layer is moving upward (19:21 IST launch) and when the F-layer is stationary (20:41 IST launch). Low altitude bubbles during upwelling of the F-region in the prereversal current enhancement phase are characterized by turbulent, non Maxwellian regions. Transitional scale waves with k=−3.6 are observed in the bubbles. This flight also detects strong sharp E-layers during downleg and an intermediate layer at 170km. Nighttime bubbles during almost stationary F-layer conditions show turbulent, Maxwellian features with moderate cooling compared to the undisturbed environment. Transitional scale waves in the bubble region show a spectral index k=−3.1. The spectral power is reduced by around 20dB compared to the sunset flight.     

2D and 3D MHD simulations of disk accretion by rotating magnetized stars: Search for variability

We performed 2D and full 3D magnetohydrodynamic simulations of disk accretion to a rotating star with an aligned or misaligned dipole magnetic field. We investigated the rotational equilibrium state and derived from simulations the ratio between two main frequencies: the spin frequency of the star and the orbital frequency at the inner radius of the disk. In 3D simulations we observed different features related to the non-axisymmetry of the magnetospheric flow. These features may be responsible for high-frequency quasi-periodic oscillations (QPOs). Variability at much lower frequencies may be connected with restructuring of the magnetic flux threading the inner regions of the disk. Such variability is specifically strong at the propeller stage of evolution.     

Meteoroids and space debris hypervelocity impact penetrations in LDEF MAP foils compared with hydrocode simulations

The continued analyses of penetrating impacts on MAP foils of Aluminium and Brass have produced data for several LDEF faces, i.e., Space, West, and East. These data have immediate bearing on the interpretation and design of devices to detect the penetration of a thin metallic film by a dust grain which have been tested both in the laboratory and in space. A crucial component of the analysis has been the theoretical calculation utilizing CTH, a Sandia National Laboratory Hydrodynamic computer code /1/ to assess the parameters of the hypervelocity penetration event. In particular theoretical hydrodynamic calculations have been conducted to simulate the hypervelocity impact event where various cosmic dust grain candidates, e.g., density = 0.998, 2.700, 7.870 (gm/cm³), and velocities, i.e., 7 - 16 km/s, have been utilized to reproduce the events. Theoretical analyses of hypervelocity impact events will be reported which span an extensive matrix of values for velocity, density and size. Through a comparison between LDEF MAP foil measurements and CTH hydrocode calculations these analyses will provide an interpretation of the most critical parameters measured for space returned materials, i.e., for thin films, the diameter of the penetration hole, D_h, and for semi-infinite targets, the depth-to-diameter ratio of craters, . An immediate consequence of a comparison of CTH calculations with space exposed materials will be an enhancement of the coherent model developed by UKC-USS researchers to describe penetration dynamics associated with LDEF MAP foils.     

Boost电路开关瞬间电压尖峰产生机理及抑制方法

Boost变换器常用作两级式逆变器的前级升压电路,由于电路中寄生参数的存在,开关瞬间输出电压叠加有瞬态尖峰,降低了波形质量,甚至影响逆变器的正常工作。为了抑制直流环节电压尖峰,研究了Boost电路开关瞬态过程,针对瞬态电路开关特性和开关器件工作状态,建立了基于金属氧化物半导体场效应晶体管（MOSFET）和肖特基二极管（SBD）的换流单元的解析模型,进一步分析了不同寄生参数对开关瞬态电流特性的影响,以及导致电压尖峰的机理等。仿真分析了寄生参数与输出电压尖峰大小的关系,提出了“减缓开关速度”和“降低输出端寄生电感”2种从源头抑制输出电压尖峰的方法。仿真和实验表明,这2种抑制方法能够有效减小电压尖峰,提高Boost电路的输出电压性能。      

旋转状态下涡轮叶片前缘的流动与换热

用数值模拟的方法对旋转状态下涡轮叶片前缘冷却结构进行了数值研究,该结构由进气腔、叶片尾缘块和前缘块构成,对此结构不同的旋转速度情况进行了计算,根据计算结果分析了旋转对涡轮叶片前缘流动与换热的影响.计算结果表明,旋转状态下带气膜出流的冲击流动中,前尾缘冲击面的换热随着转速的增加而减小,且尾缘冲击面的换热比前缘冲击面的换热要好;同时前尾缘冲击面换热的差别随着转速的增加将越来越小.     

Cosmic ray measurements in High Tatra mountains: 1957–2007

Lomnický Štít (LS, situated at High Tatra mountain, 2634 m above sea level, in the direction of 49.40°N, 20.22°E; geomagnetic vertical cut-off rigidity for cosmic rays ∼4 GV) is a relevant place for cosmic ray studies. After a brief review of the LS research history we present a selection of the results based on the measurements performed by the neutron monitor located at that site. In particular, the characteristics of quasi-periodicities and the diurnal variability amplitude and phase obtained from those data are discussed.