飞行器振动智能分析与诊断

本文通过综合多个领域知识，引进功能特征描述概念，运用证据理论，提出了对飞行器等复杂系统进行分析诊断的一个新方法并初步完成了专家系统原型，通过具体实例，再现了故障现象     

小波分析和人工神经网络在金属超声无损检测缺陷分类中的应用

基于金属超声检测中的缺陷脉冲回波为非稳态信号的特点，对高温合金材料超声检测信号的小波变换进行了特征分析，提取了各级小波分解信号的能量分布特征，最后将这些特征输入人工神经网络进行训练和分类，实验表明，这种方法具有良好效果。     

人工拉格朗日点附近的被动稳定飞行

利用太阳帆能在三体问题中实现人工拉格朗日点,人工拉格朗日点克服了经典拉格朗日点位置固定的缺点,研究人工拉格朗日点的被动控制对深空探测有重要的意义。理论上人工拉格朗日点都不稳定,研究表明在被动控制下存在某些人工拉格朗日点的稳定特性与稳定平衡点非常接近,在工程上可以认为稳定。被动控制可以通过设计太阳帆来实现,本文给出了被动稳定太阳帆的设计,在该设计下考虑轨道和姿态的耦合动力学方程。基于该耦合方程研究了人工拉格朗日点的稳定性。仿真结果表明被动太阳帆使得人工拉格朗日点稳定。     

大型捆绑运载火箭姿态控制系统

本文介绍了大型捆绑运载火箭姿态控制系统方案、工作原理和首发飞行试验结果,并将部分参数同美国航天飞机进行比较。     

运载火箭控制系统仿真的发展方向

为拓宽仿真系统、仿真计算机、仿真软件和与人工智能相结合等方面的应用范围,本文全面阐述了运载火箭控制系统仿真的发展方向,可供预先研究做选题参考。     

人造地球卫星初轨计算的单位矢量法

本文在建立两组单位矢量系统Ｒ＊，Ｓ＊，φ＊和ρ＊，Ａ＊，ｈ＊的基础上，给出了初轨计算的新的条件方程形式以及对不等精度、不同类型的观测资料的加权处理方法，这对充分发挥高精度测距资料ρ和测速资料ρ·的作用十分有利。实测计算表明，本方法基本解决了初轨计算中轨道半长轴不易定准的困难，并具有定轨精度高、适用范围广、稳定性能好等优点，对静止卫星转移轨道入轨段超短弧段测量资料的初轨计算，作用尤为明显。     

红外型空空导弹智能制导律研究

本文论述了红外型空空导弹应用智能控制的理论基础及结构特点，以多级智能控制的框架和机理设计出以比例导引为主、智能控制为辅的变指令智能制导律，并编制计算机软件以数字仿真的形式验证变指令智能制导规律的有效性和可行性     

无人机涡喷发动机的神经网络自适应PID控制

将基于RBF神经网络的辨识网络与基于BP网络的控制器相结合，组成自适应PID神经网络控制系统。RBF神经网络采用离线学习在线修正权值和阈值，为加快收敛速度，应用带惯性项的梯度下降法。大量仿真结果表明，RBF网络较ELM，标准BP及改进的BP等网络具有明显优点。对某型无人机涡喷发动机控制系统的仿真结果表明此控制方式具有鲁棒性好、响应速度快、稳态误差小等优点。     

固体火箭发动机使用寿命的确定

本文论述了一种新的推进剂老化试验方法:即使用不同年分火药在一种高温下进行加速老化,定期进行发动机试验,用发动机内弹道性能参数和对火药理化性能要求作为失效判定标准,根据不同年分火药和失效时间的关系,可以计算火药的使用寿命.文中提出了一种简便的计算加速因子和火药使用寿命的方法,概括地介绍了有关试验结果.     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.