Comparison of methods for the determination of key reactions in chemical systems: Application to Titan’s atmosphere

A new paradigm is emerging in the field of photochemistry modeling in giant planets and Titan atmospheres. The emphasis is placed on the accurate predictions of the models and the quantification of their uncertainties. In order to improve photochemical models predictions, it is necessary to identify in chemical schemes the key reactions that should be studied in priority at conditions relevant to planetary atmospheres.     

涡轮叶片与涡轮盘热弹塑性蠕变接触分析

利用大型通用结构分析程序APOLANS对某型航空发动机高压涡轮盘与叶片进行了热弹塑性蠕变接触分析, 并与轮盘热弹塑性蠕变分析结果进行了比较, 得出了一些有益的结论, 为涡轮盘、叶片的应力应变分析提供了一种较为准确的方法。      

Surface-Exosphere-Magnetosphere System Of Mercury

Mercury is a poorly known planet, since the only space-based information comes from the three fly-bys performed in 1974 by the Mariner 10 spacecraft. Ground-based observations also provided some interesting results, but they are particularly difficult to obtain due to the planet’s proximity to the Sun. Nevertheless, the fact that the planet’s orbit is so close to the Sun makes Mercury a particularly interesting subject for extreme environmental conditions. Among a number of crucial scientific topics to be addressed, Mercury’s exosphere, its interaction with the solar wind and its origin from the surface of the planet, can provide important clues about planetary evolution. In fact, the Hermean exosphere is continuously eroded and refilled by these interactions, so that it would be more proper to consider the Hermean environment as a single, unified system – surface-exosphere-magnetosphere. These three parts are indeed strongly linked to each other. In recent years, the two missions scheduled to explore the iron planet, the NASA MESSENGER mission (launched in March 2004) and the ESA cornerstone mission (jointly with JAXA) BepiColombo (to be launched in 2012), have stimulated new interest in the many unresolved mysteries related to it. New ground-based observations, made possible by new technologies, have been obtained, and new simulation studies have been performed. In this paper some old as well as the very latest observations and studies related to the surface-exosphere-magnetosphere system are reviewed, outlining the investigations achievable by the planned space-based observations. This review intends to support the studies, in preparation of future data, and the definition of specific instrumentation.     

基于格林函数法的板翅式冷板瞬态热分析(英文)

在航空电子电路设计和温度监控过程中,为保证电子元件安装部位的温度不超过允许值,需要对板翅热沉温度进行准确分析。而在发热元件为非均匀热源作用下的冷板表面温度显式解析解,可提供电子元件发热量与航空电子设备各点温升的直观了解。本文建立了板翅式冷板的三维瞬态传热模型,提出了板翅式冷板的热模拟解析求解方法,通过算例计算了板翅式冷板在非均匀热流密度下电子元件不同安装位置的瞬态温升。分析解结果与试验测量结果误差不超过3K。     

一种简易的双星定位系统定位解算方法

双星导航定位系统采用双星定位体制,其定位基本原理为三球交会测量原理,其中2颗量测量与用户到2颗卫星的距离有关,与用户高程有关的第3个量测量是决定系统定位精度的关键因素.为此,为了简化定位算法,文章根据地球椭球几何及大地纬度的相关知识,推导了与用户高程有关的第3个量测量的精确模型,进而建立了用户的定位算法.该算法具有简单...     

深空天文测角测速组合自主导航可观测性分析方法

导航系统的性能与其可观测性密切相关,而可观测矩阵是分析导航系统可观测性能的重要依据。本文基于分段线性定常系统(PWCS)方法给出导航系统的可观测矩阵,进而针对测角测速组合导航系统开展可观测性分析。通过分析测角测速组合导航系统可观测矩阵的秩和条件数,得到导航系统的可观测性和整体可观测度,并研究导航系统的可观测阶数对导航系统的影响;同时基于奇异值分解(SVD)方法给出测角测速组合导航系统各个状态分量的可观测性分析方法。最后,以小行星探测工程任务巡航段为背景,系统地给出了不同量测模型的导航系统可观测性结果,分析了不同可观测性分析方法对导航系统可观测性刻画的适用性。本文所提出的可观测性分析方法,对导航系统可观测性分析具有很好的参考性,可为组合导航系统量测模型的优选提供参考,具有良好的理论和应用价值。     

“天宫一号”目标飞行器结构模态试验方法

“天宫一号”目标飞行器结构初样模态试验的激励方式、模态参数的识别方法及试验结果的评估等都有其独到的地方。多点激励模态试验的关键在于激励位置的选择及考核输入激励力的相关性,识别耦合紧密的模态结果重点在于参数识别算法。文章从模态试验原理出发,对多点激励在“天宫一号”目标飞行器结构初样模态试验中的应用及耦合紧密的模态试验结果的识别方法进行了探讨和分析。     

航天器相对运动的两点边界值问题解析解

针对无摄椭圆轨道,推导了表示真实相对位置速度的状态转移矩阵,进而推导出了相对运动两点边界值问题的一阶解析解。所得结果不仅可指定转移时间、还可在时间范围内进行全局的燃料优化或在时间和燃料两者间折中;对于周期和非周期的相对运动均适用。仿真结果表明此解的归一化精度达到10^－6。进一步的仿真发现相对转移过程的燃料消耗会随目标轨道偏心率的增加而增加;随长半轴的增加而减少;随初始真近点角的增加呈现周期性变化;随着转移时间增加,燃料消耗的总趋势是减少的。     

考虑地球扁率修正的基于日地月方位信息的地球卫星自主导航

给出了基于地球球形假设的双圆锥地心方位确定算法,研究了考虑地球扁率的地心方位精确确定算法,给出了基于扁率修正的日地月自主导航算法。蒙特卡洛仿真表明,对于500km高度,对地定向三轴稳定的姿态运行模式的卫星,在地球敏感器噪声为0.1°(3σ),日、月敏感器噪声为0.05°(3σ)的情况下,导航位置精度能达到800m(3σ),速度精度能达到2.4m/s(3σ)。     

无穷维情形下的Rolle定理

设Ω是自反的实Banach空间X中的有界开凸集,Y为一实赋范线性空间。证明了一个无穷维情形下的Rolle定理：如果算子A∶Ω→Y在Ω上强连续,在Ω内Frèchet可微,并且存在Y上的非0连续线性泛函f,使得f（Ax）=0对一切x∈Ω成立,则至少存在一点∈Ω,使对一切u∈X,都成立f（A′（x）u）=0。