A DYNAMIC MODEL OF THE SOLAR-POWERED SOLID ABSORPTION REFRIGERATION SYSTEM

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Particle Acceleration by the Sun: Electrons, Hard X-rays/Gamma-rays

Observations of hard X-ray (HXR)/γ-ray continuum and γ-ray lines produced by energetic electrons and ions, respectively, colliding with the solar atmosphere, have shown that large solar flares can accelerate ions up to many GeV and electrons up to hundreds of MeV. Solar energetic particles (SEPs) are observed by spacecraft near 1 AU and by ground-based instrumentation to extend up to similar energies, but it appears that a different acceleration process, one associated with fast Coronal Mass Ejections (CMEs) is responsible. Much weaker SEP events are observed that are generally rich in electrons, ³He, and heavy elements. The energetic particles in these events appear to be similar to those accelerated in flares. The Ramaty High Energy Solar Spectroscopic Imager (RHESSI) mission provides high-resolution spectroscopy and imaging of flare HXRs and γ-rays. The observations of the location, energy spectra, and composition of the flare accelerated energetic particles at the Sun strongly imply that the acceleration is closely related to the magnetic reconnection that releases the energy in solar flares. Here preliminary comparisons of the RHESSI observations with observations of both energetic electrons and ions near 1 AU are reviewed, and the implications for the particle acceleration and escape processes are discussed.     

光学太阳反射镜抗静电薄膜的设计原则

对氧化铟锡（ITO）薄膜在光学太阳反射镜（OSR）抗静电放电设计中的应用进行了研究，采用Drude理论分析了ITO薄膜的表面方阻等对OSR的太阳光谱吸收比的影响，测试了光学太阳反射镜充电电位，讨论了薄膜接地状况对OSR表面充放电性能的影响，结果表明，ITO薄膜应用于OSR表面防静电放电时，需合理设计表面方阻和接地方式。     

折叠状航天器太阳电池阵在轨热分析(Ⅱ)--计算结果和分析

采用 SIP算法 ,对高 H =2 0 0 km的在轨航天器折叠状太阳电池阵的三维不稳定温度分布做了数值分析。计算时仔细考虑了不同时刻电池阵不同的热输入。计算网格 N =N1 × N2 × N3=14× 2 2× 2 2 =6776,初始温度T0 =2 78K。获得了抛罩 -展开Δ t=3 2 5 4 s间隔内 4块折叠状太阳电池阵三维不稳定温度场响应特点。比较了考虑和不考虑地球入射辐射对电池阵温度分布的影响。本文分析对航天器发射进而对折叠状太阳电池阵展开时刻的认定有重要参考价值     

Study of Micrometeoroid and Orbital Debris Effects on the Solar Panels Retrieved from the Space Station “MIR”

A study of micrometeoroid and orbital debris (MMOD) long-term effects on solar cell samples of solar panels returned from the space station MIR has been carried out. Five samples from the solar array, which spent over 10 years in space, have been studied with the help of optical microscopes with magnification up to 1000. Craters with dimensions as small as 1m were registered. Additional large impact features were investigated by observing a large number of cells (150) with an optical microscope of small magnification. The aim of the study was to define morphological and statistical characteristics of samples surface damages as well as the extent of surface erosion caused by MMOD impacts. The results of statistical analysis of the data obtained in this study are shown to correlate with the experimental data obtained in the Hubble Telescope solar panel return experiment, and MMOD flux estimations are in good agreement with modern MMOD models. The relative surface area damaged by impacts of small size (1–100m) MMOD particles is estimated to be 0.01%, while the relative surface area of large impact features (greater than 0.1mm) is estimated to be 0.045%.     

折叠状航天器太阳电池阵在轨热分析(Ⅰ)——计算模型

将太阳电池板蜂窝芯子、面板和硅电池片中发生的辐射－传导复合传热过程等效为一个无内热源的三维瞬态热传导问题。根据电池板的材料、尺寸及结构形态导出太阳电池板的三维等效导热系数。针对任意两相邻电池板表面间的热辐射交换规律，构造适用于这表面内节点温度的离散方程系数。研究折叠状态太阳电池阵边界节点的热特点时，仔细考虑了地球红外辐照、地球的太阳反照、太阳辐射加热、航天器舱体几何遮挡、深冷环境散热、飞行轨道高度及航天器在太阳－地球系中不同位置等造成的影响。利用本文给出的方程，可以求出展开前在轨折叠状太阳电池阵三瞬态不稳定温度场。     

中国空间探索的切入点——"地月日大系统研究"的观念

探讨了地月系统、地日系统,并在此基础上提出了"地月日大系统"的研究思路。将地、月、日三者关联起来,从系统的角度和多时空尺度研究地、月、日三者之间的内在关联和相互影响,从中找出未来空间探索的主题和科学研究的目标,同时还要围绕这一主题和目标,用系统、整体、历史的观点筹划未来空间活动的开展。     

同步卫星姿态控制系统稳定性分析

本文介绍苏联“萤光屏”系列地球同步卫星的姿态控制系统以及在稳态运行时姿态控制系统俯仰通道的稳定性分析,分析中考虑了太阳帆板的挠性。飞行实验表明,文中所介绍的方法在工程设计中是简单可行的。     

Spatial fragmentation of solar flare plasma and beams

The observational and theoretical arguments for spatial fragmentation of the bulk of the thermal and non-thermal components of solar flare plasma are summarised. Observational aspects considered include XUV filling factors, EUV centre to limb variations, andH impact polarisation. Theoretical points addressed are the high flare inductance and beam/return current closure at the acceleration site.A high degree of beam/plasma filamentation implies strong transverse temperature gradients so that cross-field conduction must be included in energy transport modelling. Preliminary results are described for a simple two-component model.     

The acceleration of pickup ions

The well-established association of pickup ions with anomalous cosmic rays shows that acceleration of pickup ions to energies above 1 GeV occurs. At present, diffusive shock acceleration of the pickup ions at the termination shock of the solar wind seems to be the best candidate for acceleration to the high energies of anomalous cosmic rays, accounting well for many of their observed properties. However, it is shown that acceleration of pickup ions from their initial energies by this process appears to be difficult at very strong, nearly perpendicular shocks such as the termination shock. This injection problem remains without a clear solution. A number of alternatives have been proposed for the initial acceleration of pickup ions to the point where diffusive acceleration at the termination shock can take over, but none of these processes has yet emerged as a clear favorite.