考虑局部遮挡的太阳能无人机能源控制

针对太阳能无人机在飞行状态下可能出现的太阳能电池局部遮挡情况,开展相应的太阳能电池最大功率点追踪算法和能源控制研究。通过将发光亮度引入相对吸引力计算过程对萤火虫算法进行改进,实现了局部阴影情况下太阳能电池最大功率点的高效追踪。以此为基础,设计了考虑局部遮挡情况下太阳能无人机的太阳能电池/蓄电池混合能源状态机控制规则。以"蒲公英I"无人机为例,建立了太阳能电池阵列模型,开展了考虑局部遮挡情况下太阳能电池最大功率点追踪仿真实验;基于"蒲公英I"飞行剖面,开展了考虑局部遮挡情况的混合能源控制仿真试验。研究结果表明：改进的萤火虫算法可以实现在局部阴影情况下太阳能电池最大功率点的有效跟踪,与萤火虫算法相比收敛时间更短、且功率波动幅度更小;采用改进萤火虫算法和状态机能源管理策略,在考虑局部遮挡的飞行状态下可以实现太阳能电池/蓄电池之间的合理功率分配与控制。     

ZL104局部阳极氧化工艺研究

研究了铝合金材料阳极氧化理论以及ZL104铝合金材料局部硫酸阳极氧化处理后膜层粘脱现象产生的原因与机理,指出了该现象产生的原因是氧化膜在贮存、水试等环节受到污染而使氧化膜的封孔结构被破坏.根据理论分析和模拟试验结果,提出了局部阳极氧化前增加水封闭处理对氧化膜进行修复的工艺技术.该项技术可有效杜绝氧化膜层粘脱现象.采用该项工艺技术制造的液体火箭发动机已经用于常规运载火箭系统,该运载火箭已经完成飞行任务考核.     

SSPS-OMEGA超大型球形聚光器结构拓扑构型与设计

为同时兼顾千米量级尺度空间太阳能电站聚光系统的在轨发射安装难度、光学收集效率、稳定性及结构工艺等多方面的因素,提出采用基于球面正多面体的经纬线划分法模块化构建球形聚光器。该方法不仅可实现基础划分单元分布均匀、规格种类少,降低在轨构建与运载发射难度。而且只要合理控制弧高等分数和基础划分单元的口径就可以同时保证聚光系统的光学收集效率。理论与仿真结果显示,当弧高等分数为24时,该划分法共有25种基础单元件,整个球面被分成5762块。并且此时模块化构建的实际球形聚光器的光学收集效率与理想球面相比基本保持不变,解决了太阳能电站聚光系统设计中存在的关键问题。     

高温相变单元管蓄热过程数值模拟

对以高温共晶盐 Li F-Ca F2 为相变材料 (PCM)和以干空气为工质的相变蓄热系统 ,采用焓方法建立了以控制体单元为对象的单管相变蓄热模型。在模拟空间站太阳能吸热 /储热器轨道运行参数下进行了数值计算。计算结果与地面模拟试验数据进行了比较 ,吻合良好。     

非线性油膜支承裂纹转子振动特性分析

 以具有无限长轴承和无限短轴承支承的横向裂纹转子为研究对象,分析在非线性油膜力与横向裂纹联合作用时,Jeffcott转子的动力特性,并将其与刚性支承情况进行比较。结果表明轴承油膜力的存在对裂纹转子的振动影响较大,一般将降低转子的振动,这样势必增加转子裂纹故障诊断的难度。所以,在进行裂纹转子的故障诊断时,必须考虑到支承条件的影响,建立合理的动力学模型。     

气膜冷却叶片上扩散型冷却孔对紊流流场的影响

带有护散型冷却孔的气膜冷却叶版是新开发的结构，用于具有很市初始温度（1700℃）的氢气燃气轮机，名古屋工业大学流体机械实验室在日本首次对该结构的流场进行了研究。用垂直型和X型的热线测量了流场，获得了主流方向平均速度，紊流强度和雷诺剪应力，在沿下游方向和展向方向的平面里分别整理了实验数据，证实了扩散冷却孔对改善燃气轮机膜冷却紊流流场的效果。     

气、液组合膜流对壁面冷却效果的理论及试验研究

本文针对液膜及气膜组合流动的特点,提出了组合薄膜流动的“四层式流场物理模型”.根据所做简化、假设,对液膜区流场结构及冷却效果进行了理论计算,并通过分析方法,对其紧接的气膜段流动及冷却效果进行了理论预估.试验的结果表明:液膜段的理论计算与试验数据基本相符.并从试验中发现了液膜蒸干后气膜段冷却的一些特点.这对研究液体冷却时液膜及气膜组合流动的冷却效果提出了可行的途径.     

航空燃气涡轮冷气掺混流动损失的数值研究

采用理论分析的研究方法,对不同冷气掺混形式造成的涡轮气动性能的变化进行了数值计算研究。针对气膜冷却所造成的流动损失,采用修正的Ito等压混合模型;而针对尾缘冷气喷射所造成的流动损失,则采用了修正的Schoberi流动损失模型。对于不同的冷却方式,假定它们之间对主流造成的流动损失是相互独立。以某高压涡轮导向器作为研究对象,分析了各种冷气参数和几何参数对冷气掺混过程的影响规律。研究结果表明,涡轮叶片气冷过程引起的叶栅总压损失随冷气入射角度、吹气比、混合层厚度的变化而显著变化,通过优化设计可以使气冷过程造成的流动损失最小。     

Solar Irradiance Variability Since 1978

Since November 1978 a set of total solar irradiance (TSI) measurements from space is available, yielding a time series of more than 25 years. Presently, there are three TSI composites available, called PMOD, ACRIM and IRMB, which are all constructed from the same original data, but use different procedures to correct for sensitivity changes. The PMOD composite is the only one which also corrects the early HF data for degradation. The results from the detailed analysis of the VIRGO radiometry allow a good understanding of the effects influencing the long-term behaviour of classical radiometers in space. Thus, a re-analysis of the behaviour of HF/NIMBUS-7 and ACRIM-I/SMM was indicated. For the former the situation is complicated by the fact that there are no in-flight means to determine changes due to exposure to solar radiation by comparison with a less exposed radiometer on the same spacecraft. The geometry and optical property of the cavity of HF is, however, very similar to the PMO6-type radiometers, so the behaviour of the PMO6V radiometers on VIRGO can be used as a model. ACRIM-I had to be revised mainly due to a henceforth undetected early increase and a more detailed analysis of its degradation. The results are not only important for solar radiometry from space, but they also provide a more reliable TSI during cycle 21. The differences between the revised PMOD composite and the ACRIM and IRMB are discussed by comparison with a TSI reconstruction from Kitt-Peak magnetograms. As the PMOD composite is the only one which has reliable data for cycle 21, the behaviour of the three solar cycles can now be compared and the similarities and differences discussed.     

Global Response of Martian Plasma Environment to an Interplanetary Structure: From Ena and Plasma Observations at Mars

As a part of the global plasma environment study of Mars and its response to the solar wind, we have analyzed a peculiar case of the subsolar energetic neutral atom (ENA) jet observed on June 7, 2004 by the Neutral Particle Detector (NPD) on board the Mars Express satellite. The “subsolar ENA jet” is generated by the interaction between the solar wind and the Martian exosphere, and is one of the most intense sources of ENA flux observed in the vicinity of Mars. On June 7, 2004 (orbit 485 of Mars Express), the NPD observed a very intense subsolar ENA jet, which then abruptly decreased within ∼10 sec followed by quasi-periodic (∼1 min) flux variations. Simultaneously, the plasma sensors detected a solar wind structure, which was most likely an interplanetary shock surface. The abrupt decrease of the ENA flux and the quasi-periodic flux variations can be understood in the framework of the global response of the Martian plasma obstacle to the interplanetary shock. The generation region of the subsolar ENA jet was pushed towards the planet by the interplanetary shock; and therefore, Mars Express went out of the ENA jet region. Associated global vibrations of the Martian plasma obstacle may have been the cause of the quasi-periodic flux variations of the ENA flux at the spacecraft location.