挠性空间结构的H∞辨识

重点研究挠性空间结构的Ｈ∞辨识，研究表明：依据系统的输入输出空间，对系统的未知动力学参数估计和对高维数截断的适当操作，将导致适合于控制的低维数学模型。模型维数确定时，系统模型与实际系统的距离在Ｈ∞范数的意义下几乎为最小，模型维数足够大时，系统模型与实际系统的距离可任意小，这是文下间提出了挠性空间结构Ｈ∞辨识的基本思想，为此，以带挠性梁的卫星系统为背景，首先分析了系统的动力学特性，引入了挠性系统Ｈ∞     

SDF方法在目标图像处理中的应用

利用综合函数判断法（ＳＤＦ）对目标图像进行识别，能有效识别真目标的各种畸变图像及受过训练的假目标图像如干扰和背景等，并提出ＳＤＦ实时光学识别图像的可能。     

职务分析在高职院校人力资源管理中的应用

职务分析是人力资源管理的基础，是一种重要的人力资源管理技术，只有作好了职务分析工作，其它的人力资源管理工作才能顺利地开展。论文分析了高职院校进行职务分析的必要性，较全面地阐述了在高职院校进行职务分析的实施过程，并提出了进行职务分析时应注意的问题。     

改进体育课堂教学质量的几点思考

本文对现在体育教学方法提出了几点改进意见。目的是为了提高体育课的教学质量，增强学生的身体健康。     

Kinetic cyclotron and synchrotron maser instabilities: Radio emission processes by direct amplification of radiation

This article reviews the theory of the kinetic (cyclotron an synchroton) maser instabilities. The subject has been extensively developed in recent years by many authors, who have been incited by the research of the auroral kilometric radiation and other applications. The maser mechanism is appealing because it is simple and efficient, and can lead to direct amplification of radiation. Two types of electron distribution functions have been investigated so far. These are the loss-cone and hollow-beam distributions which may exist pervasively in many regions within and beyond the solar system. It is likely that the maser instabilities can have many potentially important applications to numerous radio emission processes observed in astrophysical research.     

我国超精密加工廉价化对策

提出了通过降低设备造价等技术措施和集中应用等管理措施来实现超精密加工的廉价化，以适应我国高技术发展需要     

计算机多媒体辅助教学软件设计思想

本文根据几年来制作多媒体课件的实践，详细，系统地阐述了多媒体辅助教学软件开发的总体设计思想。     

星载嵌入式处理器软件在轨重配置技术研究

文章主要介绍了星载嵌入式处理器软件在轨重配置技术,给出了在轨重配置的基本原理、方法及处理流程。     

某型水陆两栖飞机主结构铝合金材料选用分析

材料选用是飞机研制过程中的一项重要内容,选用材料的好坏直接影响飞机性能的优劣,飞机选材需要考虑多个因素。某型水陆两栖飞机按照疲劳、损伤容限设计原则进行结构设计。通过对某型水陆两栖飞机载荷工况和服役环境的分析,结合飞机基本选材原则和某型水陆两栖飞机结构设计对材料的静强度性能,疲劳、损伤容限性能,耐腐蚀性能等的要求,综合考虑铝合金材料特点、适航性、成本及供货等因素,最终提出某型水陆两栖飞机结构的铝合金材料选材方案。     

The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.