星载平面可展天线支撑桁架的结构效率优化

针对折展结构性能存在多指标且这些指标之间又相互制约的特点,把结构效率引入到可展结构的优化设计中,应用多因素正交试验法对一种空间可展开平板天线支撑桁架的优化问题进行了研究。对其关键几何设计参数进行了分析,建立了桁架结构的优化数学模型,以结构效率最大化作为优化目标,对可展桁架进行了结构优化,得到了支撑桁架各杆件的设计参数。结果表明:结构效率综合考虑了质量和刚度的影响,使结构质量和刚度同时得到优化;长宽比(l/w)是影响可展桁架结构性能的主要因素,对不同优化目标产生影响的次要因素有所不同;截面积对结构效率影响不显著(置信度p=90%),在相同杆长参数配置下,等截面可展桁架的结构效率仅次于变截面方案,但工程经济性最佳。该研究方法有助于在概念设计阶段从系统设计的角度进行空间桁架结构的快速设计与优化。     

多校区高校学生管理分析及管理体系构建

基于当前形势下高校多校区办学现状,针对学生管理过程中出现的问题,以大学生全面发展为目标,以培养大学生自我教育、自我管理的能力为主要途径,结合教育大平台的开发,利用网络资源的优势,依托校园文化的影响,建立起大学生自我教育、自我管理的引导及监控管理体系。     

带校正的机电集成超环面传动最优控制

基于某型机电集成超环面传动的机电耦合动力学模型,得到该传动的速度传递函数,推导了加入校正后系统的状态空间表达.考虑该系统的工程实际要求,建立了最优控制理论模型,求得了最优控制律.解得黎卡提矩阵方程,得到反馈增益矩阵,应用Matlab软件对跟踪响应情况和最优控制输入进行了仿真,明显改善了系统的动态性能,实现了比例积分(PI)控制与最优控制的结合.研究结果对该类型传动的实际应用具有指导意义.      

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.     

航天飞机末端区域能量管理段制导技术概述

末端区域能量管理段主要是控制航天飞机的动能和势能．使航天飞机最终达到进场着陆段的初始要求，以保证其最终成功着陆。在最终制导系统引入一个能量基准剖面，通过调整飞行距离、动压或速度制动使航天飞机达到标准的能量状态。将末端区域能量管理段划分为四个飞行段，并对这四个飞行段的基本设计思想、制导技术及过程进行了研究。经过实际的航天飞机飞行验证．证明这种方案具有良好的制导效果。     

基于状态空间法的低马赫数翼型气动载荷计算

Leishman-Beddoes(L-B)非定常动态失速模型适用于中等马赫数(Ma>0.3),而在低马赫条件(Ma<0.3)下存在与翼型气动试验数据不符合的问题,为此首先研究了低马赫数条件下翼型的非定常动态失速气动特性,其次采用状态空间法从翼型表面气流变化的角度修正了L-B模型,最后通过与翼型气动载荷试验数据的对比表明在低马赫数条件下对L-B模型的修正是正确的,能够准确预测及分析翼型的气动载荷,且该修正模型易于耦合进直升机综合分析代码中.      

自适应增量 Kalman 滤波方法

提出自适应增量Kalman滤波(AIKF)的概念和定义,建立自适应增量Kalman滤波模型及其分析方法,给出主要的计算步骤.传统自适应Kalman滤波(AKF)方法能够对事先未知的系统噪声和量测噪声的统计量进行有效的估计.但是,传统自适应Kalman滤波方法也无法对由于环境因素(如深空探测)的影响、测量设备的不稳定性等原因产生的未知时变测量系统误差进行补偿和校正,从而产生较大的滤波误差,甚至导致发散.提出的自适应增量Kalman滤波方法不但能够对系统噪声和量测噪声的统计量进行估计,而且还能成功消除这种测量系统误差,有效地提高滤波精度.该方法计算简单,便于工程应用.      

风扇转子叶征的非接触振动测量

旋转叶片的振动测量技术主要向非接触测量方向发展,硬件技术基本成熟,国内外主要是研究各种算法。本文对研制的基于叶尖定时原理的非接触振动测量系统的小间距算法进行了简要介绍,并采用该测量系统对某风扇试验件转子叶片的振动频率和幅值进行了测量,对6700r／min附近叶片的共振情况进行了分析。与应变计测量结果和理论计算结果进行的...     

基于泵式流体回路的小卫星姿控/热控一体化执行机构设计

 主要研究了小卫星姿控/热控一体化执行机构的设计问题.首先,根据流体回路中液体流速变化对小卫星产生力矩实现姿态控制、液体流动吸/散废热实现热控制的原理,提出一种姿控/热控一体化执行机构设计方案.然后针对该设计方案,利用以电机转速为变量的流体回路内压强和电磁力矩方程,推导了一体化执行机构姿控力矩模型;利用散热量随流体回路流速的变化,建立了一体化执行机构热控模型.最后,针对某小卫星设计了基于姿控/热控一体化执行机构的闭环控制系统,并针对该一体化执行机构设计了一种姿控/热控解耦算法,对其姿控/热控能力进行数学仿真验证,仿真结果证明了该一体化执行机构的有效性.     

基于提前停止判决的编码软信息辅助载波同步

 针对目前编码辅助载波同步算法中复杂度较高、延时大的问题,提出了引入辅助停止判决机制的编码辅助载波同步算法。在现有的编码辅助载波同步结构基础上,该算法能对环路信噪比(SNR)进行实时判定,在环路SNR满足限定条件后提前停止编码辅助载波同步迭代,而不影响译码性能。采用新的相位估计方式估计含相位噪声的载波相位,提升了该条件下的环路信噪比。仿真采用码率为1/2的低密度奇偶校验(LDPC)码作为编码方式,结果表明:在误码率为10^-5时,该算法减少了约50%的编码辅助载波同步迭代次数;在含相位噪声的信号条件下,与理想解调译码相比,性能损失不超过0.15 dB。