涡轮泵转子工作转速的模糊可靠性确定方法及其应用

针对涡轮泵转子共振失效的特点,分析了转子工作状态超界的隶属函数,详细讨论了隶属函数中有关参数的确定方法,建立了转子工作转速模糊可靠性计算模型,推导出工作转速的计算公式,并与常规的工作转速确定法进行了比较。     

1991年太阳L260°活动概况及其射电的特征

本文介绍了太阳L260°活动概况,并计算了黑子群的位置漂移及对应的射电缓变源.北京天文台2.84GHz射电望远镜在该活动区观测到8次特大的射电爆发(流量超过1000s.f.u.),其中4次(1991年5月16日,6月9日,6月11日,8月25日)射电爆发时变曲线十分相似而且这些微波爆发都与Ⅱ型Ⅲ型Ⅳ型米波爆发有良好的对应.可能说明该活动区所对应的日冕在长时间内存在一种磁场位形结构,这种磁场位形结构容易产生日冕物质抛射.      

轨道参数对阿尔法磁谱仪太阳辐射热流的影响

为探明阿尔法磁谱仪（AMS）的温度变化规律,并为制定AMS的热控制方案提供指导和依据,推导了AMS重要区域（AMS前方、后方、顶部和左舷）的太阳辐射热流计算公式,分析了这些区域太阳辐射热流随轨道参数的变化,解释了AMS顶部的温度变化和太阳辐射热流变化规律在热控方案中的应用。分析表明在国际空间站（ISS）正常飞行姿态下,AMS前、后方和左舷的太阳辐射热流受太阳光与ISS轨道面的夹角（β角）、ISS与会日点的角距（θ角）和地球阴影区的影响,AMS顶部太阳辐射热流受β角和θ角的影响。得出结论：β角、θ角和地球阴影区均是影响AMS温度的主要因素,各区域的太阳辐射热流变化规律可以作为设计AMS温度控制方案的主要依据之一。     

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.     

Structure of the Program of Short-term Prediction of Powerful Solar Flares

Input data of the system are two-dimensional images and one-dimensional distributions of total and polarized solar emission at 5.2 cm wavelength obtained with SSRT. Together with photoheliograms, magnetograms, Hα-filtergrams and characteristics of active regions received from other sources, they form the initial database. The first stage includes superimposing the images, identifying microwave sources with active regions, assigning NOAA numbers to the sources, and determining for each active region the heliolatitude, extent, and inclination angle of the group's axis to the equator. These data are used to calculate the boundaries of longitude zones for each active region. A next stage involves determining the brightness temperatures of microwave sources less than the polarization distribution, the degree of polarization, and microwave emission flux, as well as calculating the parameters of microwave sources. Each parameter is assigned its own value of the weight factor, and the sum of values is used to draw the conclusion about the flare occurrence probability in each active region and on the Sun in general.      

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.     

Observation of a 27-day solar signature in noctilucent cloud altitude

Previous studies have identified solar 27-day signatures in several parameters in the Mesosphere/Lower thermosphere region, including temperature and Noctilucent cloud (NLC) occurrence frequency. In this study we report on a solar 27-day signature in NLC altitude with peak-to-peak variations of about 400?m. We use SCIAMACHY limb-scatter observations from 2002 to 2012 to detect NLCs. The superposed epoch analysis method is applied to extract solar 27-day signatures. A 27-day signature in NLC altitude can be identified in both hemispheres in the SCIAMACHY dataset, but the signature is more pronounced in the northern hemisphere. The solar signature in NLC altitude is found to be in phase with solar activity and temperature for latitudes $?70°$N. We provide a qualitative explanation for the positive correlation between solar activity and NLC altitude based on published model simulations.     

一种空间超大型可展开柔性聚光器

面向空间太阳能电站（SSPS）对大口径太阳能聚光器的应用需求,提出一种超大型、轻量化、高精度的空间可展开柔性聚光器的新构型。采取理论建模、计算仿真、优化设计相结合的方法对其抛物面构型原理、展开机构折展原理、展开态结构稳定性、动态聚焦精度等问题进行研究,并完成大口径可展开柔性聚光器的设计。提出了基于多层弹性花瓣镜体复合结构的大口径柔性聚光器优化创新设计方法。由于采用薄板柔索结构,本聚光器具有精度高、展收体积比大、质量轻、在线控制简单等优点,为空间太阳能电站千米级聚光器提供一种创新设计方法。     

基于超椭圆方程和序列响应面法的回转壳开孔形状优化

含有多种功能开孔的轻质回转壳结构是航空航天结构系统内的常用支撑构件,其开孔形状直接影响结构的静动态性能。以回转壳结构为对象,基于超椭圆方程和坐标映射变换推导了回转壳开孔边界的参数化表达,开展了开孔形状动力学优化研究。为提高结构优化计算的精度、效率和收敛性,提出了准等弧长方法和基于均匀设计的序列响应面近似建模方法(SRSM),以分别实现空间超椭圆曲线的精确逼近、减少结构有限元分析成本和加快迭代收敛。以非支配排序遗传算法Ⅱ(NSGA-Ⅱ)作为响应面模型求解算法,结合有限元分析构建了回转壳开孔形状优化设计流程,开展了最大化结构一二阶频率带隙的典型回转壳结构开孔形状优化设计。结果表明,基于超椭圆方程和序列响应面法的开孔优化方法获得了有效改进结构动态特性的回转壳开孔形状,对开展计算耗时工程结构形状优化设计具有一定应用价值。