航天器大型网状天线透光性遮挡的精确计算方法

针对航天器太阳电池阵的设计和仿真中需要考虑大型网状天线造成的透光性遮挡的问题,提出一种精确计算透光性遮挡的方法。该方法以最小重复单元对金属网布进行三维建模,求取不同光照下金属网布透光率并存为表格;计算含金属网布构件造成的透光性遮挡图形时,用三角面片对构件进行三维建模,先计算出三角面片与入射光线的位置关系,查表得到该三角面片的透光率后将其投影区域的光照强度相应减少。径向肋天线算例表明,该方法快速准确,能正确生成透光性遮挡图形,为太阳电池阵仿真分析奠定了基础。     

基于脉冲子结构的探测器结构动力学优化设计

针对传统结构优化设计中,精细化模型求解复杂结构动响应过于耗时的问题,引入保精度、高效的脉冲子结构方法,提出一种考虑结构动力学响应的优化设计流程,并对月球探测器太阳翼结构进行优化分析,获得了太阳翼结构设计参数,有效地提高了太阳翼动力学特性指标,改善了月球探测器关键位置处的动力学环境。结果表明,脉冲子结构方法可以有效应用于航天器结构动力学优化设计,提高优化设计效率,所得优化结果对实际结构设计具有一定指导意义。     

微光视觉CCD在卫星云图观测中的应用

为满足气象云图观测对电荷耦合器件(CCD)的量子效率、器件规模、像素尺寸和动态范围等提出的更高要求,可选用超低噪声和高量子效率的微光视觉电荷耦合器件(L3VisionCCD)。分析了该种器件的电子倍增工作原理和性能特点,并给出CCD97器件的部分参数。讨论了L3VisionCCD器件用于云图观测时的增益选择与控制、动态范围控制,以及器件规模与实现等关键技术。分析表明,L3VisionCCD器件尤其适用于可见光云图观测,可进一步增大云图的动态范围。     

“风云一号”气象卫星

本文叙述了中国第一颗气象卫星“风云一号”。这是一颗试验气象卫星,重750公斤,其主体为1.40米×1.40米×1.20米的六面体,连同太阳电池阵共展宽8.60米,高1.76米。运行在太阳同步轨道,高度900公里,倾角99°,每天绕地球运行14圈。地面接收到高质量的图象资料和轨道空间的辐射环境资料。     

太阳电池对平流层飞艇热特性的影响分析

研究太阳电池对平流层飞艇驻空阶段热特性的影响。建立了太阳电池热模型、平流层飞艇热分析模型,包括热平衡方程、太阳直射辐射、天空散射辐射、地面反射辐射、大气长波辐射、地球长波辐射、蒙皮长波辐射、对流换热等;采用多节点模型,对平流层飞艇在驻空期间太阳电池、蒙皮与艇内氦气温度变化过程进行了数值模拟,得到了温度昼夜变化规律;分析了太阳电池（含隔热结构）的等效面积热阻、转换效率、铺装面积对平流层飞艇热特性的影响,得到了其温度昼夜变化规律。本文为平流层飞艇热性能分析和热控系统设计提供依据。     

空间碎片自然衰减和太阳活动

分析研究了空间碎片数随太阳辐射流量Ｆ１０．７的变化;给出预报Ｆ１０．７长期变化的计算方法和预测空间碎片数的数学模型。结果显示：①强太阳活动造成空间碎片年增长率下降;②空间碎片数与太阳活动１１年变化密切相关,相关数为０．９;③空间碎片增长率约为发射率的两倍;④若发射率保持不变,则到２０２０年,大于１０ｃｍ的碎片数将达到１４５００;⑤若小碎片的增长为大碎片增长的两倍,则到２０２０年,大于１ｃｍ的碎片数可达１２５０００。     

X射线耀斑的强度指标

本文利用GOES-7卫星的1分钟记录资料研究了1991年3月和6月期间6个大X耀斑伴随的软X射线爆发特性和源强度的关系。结果指出：对X射线耀斑，其射线辐射流量上升快的在日冕中激起的激波速度也较快．数值模拟研究指出，这可能反映爆发能量释放速率是源强度的主要指标．     

高频大功率GXN—50型霓虹灯电子电源的研制

ＧＸＮ－５０型霓虹灯电子电源是为负载提供高频交流电压电流的电源设备，是一种专用大功率霓虹灯电源。该产品采用先进的电子技术，节能效率高，带负载能力强（比传统电源高４倍以上），并采用超音技术，用特制的电子开关代替价格昂贵的机械继电器，因而无任何噪声，灯光变化采用程序控制，变换方式灵活，工作稳定可靠。该电源体积小、重量轻，并设计了过压过流保护电路，具有抗干扰能力强等特点。     

O2 evolution and cyclic electron flow around photosystem I in long-term ground batch culture of Euglena gracilis

Based on the purpose of better exploring the function of green producers in the closed aquatic biological life support system, the condition of dynamic O₂ evolution and performance of cyclic electron flow around photosystem I (CEF-PSI) in long-term ground batch culture of Euglena gracilis were studied, the relationship between linear electron flow (LEF) and CEF-PSI was revealed, the function of CEF-PSI was investigated. Excellent consistency in O₂ evolution pattern was observed in cultures grown in both closed and open containers, O₂ evolution was strictly suppressed in phase 1, but the rate of it increased significantly in phase 2. CEF-PSI was proposed to be active during the whole course of cultivation, even in the declining phase 3, it still operated at the extent of 47–55%. It is suggested that the relationship between LEF and CEF-PSI is not only competition but also reciprocity. CEF-PSI was proposed to contribute to the considerable growth in phase 1; it was also suggested to play an important protective role against photosystem II (PSII) photoinhibition at the greatly enhanced level (approximately 80–95%) on the 2nd day. Our results in this research suggest that E. gracilis had very particular photosynthetic characteristics, the strict O₂ evolution suppression in the initial culture phase might be a special light acclimation behavior, and CEF-PSI could be an important mechanism involved in this kind of adaptation to the changeable light environment.     

CMEs and active regions on the sun

The relationship between active regions (ARs) and coronal mass ejections (CMEs) is studied. For this purpose a statistical analysis of 694 CMEs associated with ARs was carried out. We considered the relationship between properties of the CMEs and ARs characterized using the McIntosh classification. We demonstrated that CMEs are likely to be launched from ARs in the mature phase of their evolution when they have complex magnetic field. The fastest and halo CMEs can be ejected only from the most complex ARs (when an AR is a bipolar group of spots with large asymmetric penumbras around the main spot with many smaller spots in the group). We also showed that the wider events have a tendency to originate from uncomplicated magnetic structures. This tendency was used for estimation of the real angular widths of the halo CMEs. The probability of launching of fast CMEs increases together with increase of the complexity and size of ARs. The widest, but slow, CMEs originate from the simplest magnetic structure which are still able to produce CMEs. Our results could be useful for forecasting of space weather.