微小卫星的在轨推进技术

简述了微小卫星对在轨推进(控制)技术提出的新要求,分析和比较了几种不同的在轨推进技术,着重介绍了脉冲等离子体推力器的应用和发展情况。     

大气等离子喷涂纳米ZrO2涂层工艺与性能研究

以结合强度为测试指标进行正交试验,优化出纳米ZrO2热障涂层喷涂的最佳工艺参数,并对该涂层的结合强度、抗热震性能及隔热性能进行了试验研究。试验结果表明,经优化工艺喷涂的涂层结合强度可达33 MPa;抗热震性能好,1050℃水冷试验中,涂层可经历22次左右的热震循环;隔热效果明显,火焰与涂层表面以及涂层表面和试样背面随着火焰温度不同,分别具有300~600℃和100~200℃左右的温差。     

空间环境对无线电波传播的影响综述

文章研究了空间环境对无线电通信的影响,主要体现在多种因素制约下的等离子体环境对电波传播的影响。首先介绍了几种典型的电离层模型,接着详细讲述了工程实用电离层模型;随后给出了电磁波在等离子体环境中的传播路径和等离子体介质在磁场环境下对电磁波影响的定量分析,并建议将空间等离子体环境（包括星际等离子体环境和电离层等离子体环境等）作为一个整体进行研究,来考虑地磁场对等离子体电磁特性的影响;最后基于目前理论的不足与实际需求的矛盾,探讨未来的研究方向。     

空间等离子体源与测试系统设计

文章介绍了空间等离子体源与测试系统的设计方法。为了实现具有较高能量的低密度等离子体环境,首先在源入口处设计水平与垂直两种微波输入模式,提高电子的密度和温度,然后在源出口处设计装有几何调节栅和电位调节网的扩散杯,调节电子密度和温度。     

板料n,r值对钣金零件成型工艺的影响

本文详细论述了板料成型性能指数ｎ，ｒ值的物理意义及其对各种钣金元件成型工艺性的影响，结合典型成型工艺，利用钣金冷压成型原理，对ｎ，ｒ值的具体影响进行了分析研究腹出了一些针对具体成型工艺的一般规律性的结论。将本文的一些概念和分析研究的结果同具体的生产实践相结合，则会对促进生产和提高成型件的质量有一定的指导意义。     

不同主流速度下障碍涡脱落冷流实验研究

采用冷流试验系统研究了不同主流速度对压强振荡的影响,并通过在流场中加入示踪粒子,且运用连续片光流动显示技术和高速数字摄像技术获得了试验器中流场的旋涡运动情况.实验结果表明,随着主流速度的增加,旋涡脱落的频率相应升高.同时,对比压强测试结果与高速摄影结果,发现当旋涡脱落的频率接近实验器声场的某一阶固有频率时,就可能引起压...     

Relativistic waves raised by explosions in space as sources of ultra-high-energy cosmic rays

The paper discusses the possibility of particle acceleration up to high energies in relativistic waves generated by various explosive processes in the interstellar medium. We propose to use the surfatron mechanism of acceleration (surfing) of charged particles trapped in the front of relativistic waves as a generator of high-energy cosmic rays (CRs). Conditions under which surfing in the waves under consideration can be made are studied thoroughly. Ultra-high-energy CRs (up to 10²⁰ eV) are shown to be obtained due to the surfing in relativistic plane and spherical waves. Surfing is supposed to take place in nonlinear Langmuir waves excited by powerful electromagnetic radiation or relativistic beams of charged particles, as well as in strong shock waves generated by relativistic jets or spherical formations that expand fast (fireballs).     

Specific features of the high-speed plasma stream cycles

The high-speed plasma streams in the solar wind are investigated during the solar cycles nos. 20–22 (1964–1996), separately on the two types of streams according to their solar origin: the HSPS produced by coronal holes (co-rotating) and the flare-generated, in keeping with the classification made in different catalogues. The analysis is performed taking into account the following high-speed stream parameters: the durations (in days), the maximum velocities, the velocity gradients and, the importance of the streams. The time variation of these parameters and the high-speed plasma streams occurrence rate show an 11-year periodicity with some differences between the solar cycles considered. A detailed analysis of the high-speed stream 11-year cycles is made by comparison with the “standard” cycles of the sunspot relative number (Wolf number). The different behaviour of the high-speed stream parameters between even and odd solar cycles could be due to the 22-year solar magnetic cycle. The increased activity of the high-speed plasma streams on the descendant phases of the cycles, regardless of their solar sources, proves the existence of some special local conditions of the solar plasma and the magnetic field on a large scale that allow the ejection of the high energy plasma streams. This fact has led us to the analysis the stream parameters during the different phases of the solar cycles (minimum, ascendant, maximum and, descendant) as well as during the polar magnetic field reversal intervals. The differences between the phases considered are pointed out. The solar cycles 20 and 22 reveal very similar dynamics of the flare-generated and also co-rotating stream parameters during the maximum, descendant and reversal intervals. This fact could be due to their position in a Hale Cycle (the first component of the 22-year solar magnetic cycle). The 21st solar cycle dominance of all co-rotating stream parameters against the 20th and 22nd solar cycle ones, during almost all phases, could be due to the same structure of a Hale Cycle – solar cycle 21 is the second component in a 22-year SC. During the reversal intervals, all high-speed stream parameters have comparable values with the ones of the maximum phases of the cycles even if this interval contains a small part of the descendant branch (solar cycles 20 and 22).     

Recent Developments in Magnetospheric Diagnostics Using ULF Waves

One of the most ubiquitous indicators of the state and topology of the magnetosphere are ultra-low frequency (ULF) waves. These may be continuously and inexpensively monitored from the ground using networks of magnetometers. The most robust measurable quantity provided by magnetometer networks is signal phase and this paper emphasizes the usefulness of this parameter in a variety of ULF wave diagnostic processes ranging from equatorial to high latitudes. This revised version was published online in August 2006 with corrections to the Cover Date.     

The Strength and Structure of the Coronal Magnetic Field

I discuss a method for determining the strength and spatial structure of the coronal magnetic field by observations of the Faraday rotation of a radio galaxy which is in conjunction with the Sun. Given a knowledge of the plasma density in the outer corona, and the magnetic field sector structure (both independently available), the strength of the coronal field can be determined, as well as the magnitude of spatial variations on scales of 1000 km to several solar radii. Such knowledge is crucial for testing computational models of the solar corona, which are prominently featured in this meeting. Results are presented from observations with the Very Large Array radio telescope of the radio galaxy 3C228 on August 16, 2003, when the line of sight to the source was at heliocentic distances of 7.1−6.2R _⊙. The observations are consistent with a coronal magnetic field which is proportional to the inverse square of the distance in the range 6 ≤ r ≤ 10R _⊙, and has a value of 39 mG at 6.2R _⊙. The Faraday rotation is uniform across the source, indicating an absence of strong plasma inhomogeneity on spatial scales up to 35,000 km.