薄壁微三维结构件超精密研抛技术研究

针对影响薄壁微结构件超精密研抛的工艺因素,即单次进给量、研磨轨迹、研磨膏选择和去除量精确控制,通过大量的研抛加工试验,进行研抛工艺研究,得到能实现稳定和理想加工结果的研抛工艺,很好的满足零件性能要求。     

基于Mecanum轮配送车的视觉与磁带双重导引技术研究

针对卫星总装过程中提出的物料配送需求,设计并实现了以Mecanum轮全方位移动平台为基础,可在狭窄配送通道内快速、灵活移动的智能物料配送车。结合总装现场实际环境条件,配送车采用了视觉导引与磁带导引相结合的智能导引策略,有效消除了光照强度变化、地面裂纹、电磁信号干扰等环境因素对车道线采集的影响,最终实现总装物料从库房至多工位的自动配送。     

钛合金TC4的超硬磨料柔性抛光轮数控抛光试验研究

航空发动机叶片钛合金材料在数控磨抛加工中容易发生烧伤及黏附现象,针对常用的TC4材料开展了超硬磨料柔性抛光轮数控抛光试验研究。分析了超硬磨料柔性抛光轮抛光参数中转速、进给速度、预压量及行距对抛光去除深度及抛光后试件表面粗糙度的影响规律并通过正交试验分析了各抛光参数影响的主次关系。确认了钛合金试件抛光表面黏附物质成分,并同时分析了表面黏附物的形成原理。给出了TC4钛合金材料在超硬磨料柔性抛光轮数控抛光过程中工艺参数的选择策略,为TC4材料的航空发动机叶片和整体叶盘在超硬磨料柔性抛光轮数控抛光过程中提供理论依据和技术基础。     

控制飞行器磁特性的方法

由于飞行器结构和功能的需要,任何飞行器都会有一定的磁性。飞行器的磁性会干扰飞行器的姿态和影响磁敏感仪器的性能,因此在飞行器的设计和研制过程中,必须控制飞行器的磁特性。本文简单的介绍了空间环境磁场和飞行器的磁源,着重阐述了控制飞行器磁性的设计原则和试验方法。     

电流片的稳定性问题

本文从理想磁流体力学出发,分析了固结在光球层上的半圆弧形电流片的线性稳定性。主要结论是:当沿电流方向的磁场小于某临界值时,电流片将不稳定,且最先引起不稳定的扰动模沿电流方向的波数近似为电流片圆弧直径的倒数。      

超精密加工中研抛分布力测量方法的探讨

在研磨盘的不同位置打深盲孔,近于贯穿,仅留下薄薄一圆形平膜片,作为抛光法向压力的敏感元件。此圆平膜片半径,厚度由位移敏感元件灵敏度及抛光所容许的外扰（对实际工作状态影响足够小）决定。在此孔中安置光纤位移传感器测量圆平膜片的变形位移,就可解算出抛光时研磨盘的局部压力。信号调制后通过多路遥测装置或电刷滑环等集流器将信号引出。     

Magnetic Field Fluctuations in the Solar Wind, Foreshock and Magnetosheath： Cluster Data Analysis

46 magnetosheath crossing events from the two years (2001.2-2003.1) of Cluster magnetic field measurements are identified and used to investigate the characters of the magnetic field fluctuations in the regions of undisturbed solar wind, foreshock, magnetosheath. The preliminary results indicate the properties of the plasma turbulence in the magnetosheath are strongly controlled by IMF orientation with respect to the bow shock normal. The amplitude of the magnetic field magnitude and direction variations behind quasi-parallel bow shock are larger than those behind quasi-perpendicular bow shock. Almost purely compressional waves are found in quasi-perpendicular magnetosheath.     

Fundamental (f) oscillations in a magnetically coupled solar interior-atmosphere system – An analytical approach

Solar fundamental (f) acoustic mode oscillations are investigated analytically in a magnetohydrodynamic (MHD) model. The model consists of three layers in planar geometry, representing the solar interior, the magnetic atmosphere, and a transitional layer sandwiched between them. Since we focus on the fundamental mode here, we assume the plasma is incompressible. A horizontal, canopy-like, magnetic field is introduced to the atmosphere, in which degenerated slow MHD waves can exist. The global (f-mode) oscillations can couple to local atmospheric Alfvén waves, resulting, e.g., in a frequency shift of the oscillations. The dispersion relation of the global oscillation mode is derived, and is solved analytically for the thin-transitional layer approximation and for the weak-field approximation. Analytical formulae are also provided for the frequency shifts due to the presence of a thin transitional layer and a weak atmospheric magnetic field. The analytical results generally indicate that, compared to the fundamental value ($\omega =\sqrt{\mathit{gk}}$), the mode frequency is reduced by the presence of an atmosphere by a few per cent. A thin transitional layer reduces the eigen-frequencies further by about an additional hundred microhertz. Finally, a weak atmospheric magnetic field can slightly, by a few percent, increase the frequency of the eigen-mode. Stronger magnetic fields, however, can increase the f-mode frequency by even up to ten per cent, which cannot be seen in observed data. The presence of a magnetic atmosphere in the three-layer model also introduces non-permitted propagation windows in the frequency spectrum; here, f-mode oscillations cannot exist with certain values of the harmonic degree. The eigen-frequencies can be sensitive to the background physical parameters, such as an atmospheric density scale-height or the rate of the plasma density drop at the photosphere. Such information, if ever observed with high-resolution instrumentation and inverted, could help to gain further insight into solar magnetic structures by means of solar magneto-seismology, and could provide further insight into the role of magnetism in solar oscillations.     

Kink mode m = 1 in magnetic tube with discontinuous magnetic field

In this paper, we study conditions of realization and stability of kink modes with azimuthal wave numbers $m=\pm 1$ in cylindrical plasma flex with twisted magnetic field and homogeneous current along its axis. We assume permanent axial magnetic field both inside and outside the flex, surrounded by currentless plasma. Azimuthal magnetic field decreases inversely proportional to the distance from the boundary beyond the flex. We derived dispersion equations for stable and unstable modes in approximation of “thin” plasma flex. The analysis of equations has been provided for the case of discontinuous axial magnetic field on flex’s boundary. Conditions of propagation of wave modes have been defined. It was shown, that unstable modes can be implemented in certain interval of longitudinal wavenumbers. Results can be applied for the interpretation of solar magnetic tubes behavior, using measurements, provided by spacecrafts.     

控制力矩陀螺磁悬浮转子的指数趋近积分滑模控制研究

针对微重力、动框架等多源扰动下磁悬浮控制力矩陀螺磁轴承转子系统的强非线性、参数摄动及未建模动态等问题,开展控制力矩陀螺的磁轴承转子鲁棒控制研究。建立了磁轴承转子轴向通道动力学模型与电磁力工作点线性化模型,分析了系统参数摄动及未建模动态,并在此基础上提出了一种非线性系统指数趋近积分滑模控制方法,设计了含有电流及位移的积分滑模平面,采用指数趋近律与饱和函数抑制抖振实现到达阶段滑模控制律。实验结果表明：采用该方法可有效抑制滑模的抖振现象,参数摄动时系统具有较佳动态性能,同时在转子转动、框架工作时保证系统良好鲁棒性。