基于Bootstrap方法的捷联惯组历次测试数据验前分布研究

针对捷联惯性测量组合（捷联惯组）历次测试数据小样本的特点，在总体分布参数形式未知的情况下，根据已有的先验信息，提出了通过Bootstrap重采样技术，获得捷联惯组历次测试数据总体参数的验前分布。结合当前样本信息，给出捷联惯组历次测试数据的验后分布。将统计推断建立在验后分布基础之上，可以减小小样本情况下的统计分析误差。     

用于微小卫星推进装置的脉冲等离子体推力器

论述了脉冲等离子体推力器(PPT)的工作原理和研究状况。在分析其主要优缺点的基础上，讨论了PPT技术的发展方向，并就PPT的应用前景作了展望。分析认为PPT是一种先进的小推力动力装置，特别适合于微小卫星的轨道转移、姿态控制、位置保持以及星座编队飞行。     

国外军用小卫星的发展及测控技术

介绍了国外现代军用小卫星的应用情况及发展计划，分析了小卫星的未来发展方向，论述了军用小卫星发展所需的新型测控体制及相应的关键技术。最后，就我国小卫星技术的发展提出了建议。     

基于模糊神经网络的小卫星任务自主调度设计

为了提高小卫星星务软件的自主化、智能化水平，提出一种基于模糊神经网络的小卫星任务自主调度的设计方法。该方法根据小卫星有效载荷和任务的需求，将小卫星的星务软件分解为若干个任务模块。同时，考虑到一些任务执行的紧前关系要求，将若干有紧前关系的任务模块划分为一个任务流程。以任务流程为单位，利用模糊神经网络构建任务流程自主调度决策系统。仿真实验结果表明，该决策系统能够根据小卫星的监测数据，以任务流程的自主调度为基础，最终实现对任务模块的动态自主调度。     

应用于小卫星平台的中分辨率成像光谱仪

文章简要介绍了中分辨率成像光谱仪（CMODIS）的组成、原理及系统设计。     

Globalstar星座与意大利的小卫星中心

介绍了意大利 Alenia 航空航天公司为生产 Globalstar 卫星而建立的小卫星中心及其环境试验概况。     

某微小型卫星姿轨控计算机系统的设计

为实现卫星姿轨控计算机小型化，采用TI公司的数字处理器(DSP)TMS320F206芯片作为CPU，其他逻辑采用现场可编程逻辑门阵列(FPGA)实现，并以此为基础，将姿轨控系统其他有关仪器设备集成到计算机中，形成一台复合控制设备。研究表明，DsP可用于实现姿轨控计算机的小型化，以及今后复合控制系统的设计。     

承载紧固孔边应力强度因子

 <正> 1.孔边穿透裂纹应力强度因子 采用宽度修正系数FB(c/W),可得紧固件孔边裂纹的SIF式中f_1(α/R)、钉载作用时的FB(c/W)以及未开裂应力σ_Y(X)。对双向载荷下的宽度修正系数,采用文献的数据最小二乘拟合,得     

编队飞行小卫星空间状态测量方法研究

介绍了编队飞行小卫星特点，提出了小卫星空间状态测量方案。着重论述了星间相对状态自主测量方法，计算了伪码和载波相位跟踪环路、时钟基准频差以及测量设备延迟带来的星间相对距离测量误差，讨论了降低误差的方法。在对误差项进行综合分析后，得出相对距离测量误差可达到厘米级的结论。     

Working Group 3 Report: Coronal Hole Boundaries and Interactions with Adjacent Regions

Summarized below are the discussions of working group 3 on "Coronal hole boundaries and interactions with adjacent regions" which took place at the 7th SOHO workshop in Northeast Harbor, Maine, USA, 28 September to 1 October 1998. A number of recent observational and theoretical results were presented during the discussions to shed light on different aspects of coronal hole boundaries. The working group also included presentations on streamers and coronal holes to emphasis the difference between the plasma properties in these regions, and to serve as guidelines for the definition of the boundaries. Observations, particularly white light observations, show that multiple streamers are present close to the solar limb at all times. At some distance from the sun, typically below 2 R, these streamers merge into a relatively narrow sheet as seen, for example, in LASCO and UVCS images. The presence of multiple current sheets in interplanetary space was also briefly addressed. Coronal hole boundaries were defined as the abrupt transition from the bright appearing plasma sheet to the dark coronal hole regions. Observations in the inner corona seem to indicate a transition of typically 10 to 20 degrees, whereas observations in interplanetary space, carried out from Ulysses, show on one hand an even faster transition of less than 2 degrees which is in agreement with earlier Helios results. On the other hand, these observations also show that the transition happens on different scales, some of which are significantly larger. The slow solar wind is connected to the streamer belt/plasma sheet, even though the discussions were still not conclusive on the point where exactly the slow solar wind originates. Considered the high variability of plasma characteristics in slow wind streams, it seems most likely that several types of coronal regions produce slow solar wind, such as streamer stalks, streamer legs and open field regions between active regions, and maybe even regions just inside of the coronal holes. Observational and theoretical studies presented during the discussions show evidence that each of these regions may indeed contribute to the solar slow wind. This revised version was published online in June 2006 with corrections to the Cover Date.