基于鲁棒曲线匹配的星表特征跟踪方法

针对星际着陆的特征跟踪及障碍识别过程,提出了一种基于尺度不变的曲线描述及匹配方法。该方法利用曲线邻域的梯度信息形成特征描述符,无需知道各点曲率或曲线之间的几何构型,且对旋转、缩放、视角变化及光照影响都具有较强的鲁棒性。仿真实验表明,该算法不仅能够对不同尺度的陨石坑、岩石边缘等障碍或自然陆标进行识别,而且能够实现边缘曲线特征的跟踪,误匹配率低。     

星上数据管理中的实时多任务操作系统设计

参照欧空局的软件工程规范,研制了为星上数据管理任务服务的实时多任务操作系统ＲＴ８６,它的硬件环境是两个互为冷配份的主控单元,通过１５５３Ｂ串行数据总线与多个远置单元联接,完成星上遥测、遥控及星上多项数据库管理任务。文章介绍了其设计要点,做到了系统设计思路简单清晰,程序易于修改维护,可靠性高,它为星上应用软件开发提供了通用设计平台。     

基于ADAMS的行星齿轮系刚柔耦合仿真局部缺陷识别

针对行星齿轮系在工作过程中出现的局部缺陷,将引起齿轮啮合异常,并导致冲击异常,其特征频率就会发生变化。现用ADAMS与ANSYS建立行星齿轮系的刚柔耦合模型,通过快速傅里叶变换（FFT）得到其啮合力的频域曲线,并分析无缺陷行星齿轮系的特征频率、行星轮齿局部缺陷的特征频率、太阳轮齿局部缺陷的特征频率。仿真结果与理论值吻合,说明了所建虚拟样机模型可靠,得到无缺陷行星齿轮系的特征频率是265.34Hz,行星轮齿局部缺陷的特征频率是17.67Hz,太阳轮齿局部缺陷的特征频率是36.13Hz,可用于识别行星齿轮系的行星轮或太阳轮局部缺陷。对行星齿轮系振动特性、可靠性的研究具有一定的指导意义。     

非连续增强镁基复合材料的时效特性

对ＭＢ１５合金和（Ｂ４Ｃｐ＋ＳｉＣｗ）／ＭＢ１５复合材料在１７０℃的时效特性进行了比较研究。ＤＳＣ结果表明,复合材料中时效相的析出过程比基体合金提前,且析出量增加,而析出相的溶解过程推迟。ＴＥＭ观察发现,复合材料中析出物仍为Ｌａｖｅｓ ＭｇＺｎ２＇相,且在ＳｉＣｗ／Ｍｇ与Ｂ４Ｃｐ／Ｍｇ两种界面上和界面反应物ＭｇＢ２上优先析出。维氏硬度测试表明,复合材料有明显的时效加速,达到峰时效只需６ｈ,而基体合     

Effects of Low Energetic Neutral Atoms on Martian and Venusian Dayside Exospheric Temperature Estimations

The heating of the upper atmospheres and the formation of the ionospheres on Venus and Mars are mainly controlled by the solar X-ray and extreme ultraviolet (EUV) radiation (λ = 0.1–102.7 nm and can be characterized by the 10.7 cm solar radio flux). Previous estimations of the average Martian dayside exospheric temperature inferred from topside plasma scale heights, UV airglow and Lyman-α dayglow observations of up to ∼500 K imply a stronger dependence on solar activity than that found on Venus by the Pioneer Venus Orbiter (PVO) and Magellan spacecraft. However, this dependence appears to be inconsistent with exospheric temperatures (<250 K) inferred from aerobraking maneuvers of recent spacecraft like Mars Pathfinder, Mars Global Surveyor and Mars Odyssey during different solar activity periods and at different orbital locations of the planet. In a similar way, early Lyman-α dayglow and UV airglow observations by Venera 4, Mariner 5 and 10, and Venera 9–12 at Venus also suggested much higher exospheric temperatures of up to 1000 K as compared with the average dayside exospheric temperature of about 270 K inferred from neutral gas mass spectrometry data obtained by PVO. In order to compare Venus and Mars, we estimated the dayside exobase temperature of Venus by using electron density profiles obtained from the PVO radio science experiment during the solar cycle and found the Venusian temperature to vary between 250–300 K, being in reasonable agreement with the exospheric temperatures inferred from Magellan aerobraking data and PVO mass spectrometer measurements. The same method has been applied to Mars by studying the solar cycle variation of the ionospheric peak plasma density observed by Mars Global Surveyor during both solar minimum and maximum conditions, yielding a temperature range between 190–220 K. This result clearly indicates that the average Martian dayside temperature at the exobase does not exceed a value of about 240 K during high solar activity conditions and that the response of the upper atmosphere temperature on Mars to solar activity near the ionization maximum is essentially the same as on Venus. The reason for this discrepancy between exospheric temperature determinations from topside plasma scale heights and electron distributions near the ionospheric maximum seems to lie in the fact that thermal and photochemical equilibrium applies only at altitudes below 170 km, whereas topside scale heights are derived for much higher altitudes where they are modified by transport processes and where local thermodynamic equilibrium (LTE) conditions are violated. Moreover, from simulating the energy density distribution of photochemically produced moderately energetic H, C and O atoms, as well as CO molecules, we argue that exospheric temperatures inferred from Lyman-α dayglow and UV airglow observations result in too high values, because these particles, as well as energetic neutral atoms, transformed from solar wind protons into hydrogen atoms via charge exchange, may contribute to the observed planetary hot neutral gas coronae. Because the low exospheric temperatures inferred from neutral gas mass spectrometer and aerobraking data, as well as from CO⁺ ₂ UV doublet emissions near 180–260 nm obtained from the Mars Express SPICAM UV spectrograph suggest rather low heating efficiencies, some hitherto unidentified additional IR-cooling mechanism in the thermospheres of both Venus and Mars is likely to exist. An erratum to this article can be found at     

多级涡轮多目标气动优化设计流程

在准三维设计基础上,采用多目标优化设计方法,给出一个多级涡轮气动优化设计流程,优化联合采用人工神经网络和遗传算法,流场计算采用全三维粘性流N-S方程求解。此优化设计流程有三个特点:针对每列叶栅的气动特性进行局部优化;各列叶栅反复多次优化;粗细网格交替使用。并采用此设计流程对一三级涡轮进行优化设计,效率提高1%,说明此方法可以有效的用于多级涡轮气动优化设计。     

关于BP网络算法的输电线速断保护

建立人工神经网络BP算法，利用计算运行方式的变化改进传统的电力输电线系统的保护措施，可以实时跟踪故障点并同步实施控制。利用人工神经网络技术的快速性、自适应性和容错性，在一个周期内准确地定位区内、区外故障点，实现对输电线的速断保护。     

C/E复合材料声发射信号小波分析及人工神经网络模式识别

以复合材料为对象，以宽频带传感器及线阵列方式对各类模式试样采集了波形及信号参数，比较波形、信号参数、频谱及小波谱的特征，筛选出六类1300个样本，采用多分辨小波变换提取了5个特征向量，实现了特征空间的降维处理，采用B—P型反向传播神经网络构成了智能化模式分类器，研究了网络模型的学习效果和对与复合材料主要损伤机制有关的六类声发射信号的识别能力。试验结果表明，神经网络对六类信号的平均正确识别率达到90.4%。最佳识别率为97.2%。该方法成功用于90°、0°光滑和0°缺口三种试样的破坏过程分析，获得了满意的效果。     

一种火箭推进系统非线性动态神经网络模型

为了获得实时、准确、可靠的液体火箭推进系统非线性动态模型，使其适用于控制系统的设计和故障检测与诊断，基于RBF（Radial Basis Function）神经网络理论和系统工作机理，综合考虑了系统的动态信息，适当选择了输入输出参数，建立了一种多输入多输出的液体火箭推进系统非线性动态模型。模型的输出与实际试车结果的对比分析表明，模型的计算时间短、实时性强、精度高，可用于液体火箭推进系统的实时状态监控、故障诊断及控制系统设计等。     

基于神经网络的冷却剂热物性拟合方法

基于径向基函数神经网络（RBFN）和广义回归神经网络（GRNN）对火箭发动机冷却热物性进行拟合，并与BP网络进行了比较，结果表明，采用RBFN和GRNN进行物性拟合具有网络结构简单，计算精度高，训练速度快的优点，可方便地引入液体火箭发动机传热计算程序中。