CS-01高空台推力测量和校准装置研制

推力是涡喷涡扇发动机高空模拟试验的重要测量参数之一。CS－01高空台原推力测量采用杠杆、砝码、测力秤系统，现采用原位校准，液压加载、应变式推力传感器来测量和校准，从而消除了“高度差”的影响，降低了稳态推力测量系统的测量不确定度。     

一种模拟喷管二维流场的新方法

采用ＳＩＭＰＬＥ方法对固体火箭发动机喷管进行了纯气相流场的数值模拟。推导了建立在同位网格之上利用协变物理速度分量为计算变量的离散方程，采用协变物理速度分量推导压力修正方程，对密度采用一阶迎风格式插值，将ＳＩＭＰＬＥ方法扩大到计算可压流动。计算结果表明：本方法计算精度高，收敛速度快，程序编写简单。     

CVD过程中温度对SiC涂层沉积速率及组织结构的影响

以CH3SiCl3 H2体系在1000～1300℃沉积了SiC涂层,研究了温度对涂层沉积速率的影响,应用自发形核理论解释了不同沉积温度下CVDSiC涂层的组织结构。结果表明,随着沉积温度的提高,CVDSiC涂层的沉积速率相应增大;1000～1200℃沉积过程为化学动力学控制过程,1200～1300℃沉积过程为质量转移控制,1000℃和1100℃沉积的SiC涂层表面光滑、致密;1200℃和1300℃沉积的SiC涂层表面粗糙、多孔;随着沉积温度的提高,CVDSiC涂层的晶体结构趋于完整,当温度超过1150℃时,涂层中除β SiC外还出现了少量α SiC。     

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.     

二维过渡区喷流干扰流场的DSMC/EPS仿真

应用DSMC／EPS混合算法，数值模拟过渡区有RCS横向喷流干扰的二维有限平板高超声速流场，分析了流场结构、分离形态及物面气动系数分布等特性。结果表明，不同：Knudsen数下，喷流干扰流场存在差异，过渡区中的稀薄气体效应得以体现，证明了DSMC／EPS混合算法是研究稀薄，连续混合区域高超声速流动的有效方法。     

多体运动理论与齿轮测量中心的几何误差建模

本文阐述了多体系统的拓扑结构和低序体阵列,其特征矩阵的基本概念和构建方法,分析了多体系统误差运动的基本规律,结合891E型齿轮测量中心研究了根据特征矩阵得到其空间几何误差的算法,为齿轮测量中心精度分析和几何误差提供了一种理想的建模方法.     

耐高温有机硅树脂的合成及其耐热和固化性能研究

以甲基和苯基氯硅烷为单体,采用水解缩聚的方法合成有机硅树脂,并对影响有机硅树脂合成的有关因素进行了研究。结果表明,当水解温度为70℃,控制水用量n(H2O)／n(c1)在8:1-5:1的范围内时,可合成出易溶于甲苯的有机硅树脂。红外光谱(IR)显示,合成的硅树脂含有端羟基。采用热失重法(TG)、热失重的微分曲线法(DTG)和马弗炉烧蚀试验研究有机硅树脂耐的热性能和室温固化性能,并对KH-CL和三乙醇胺两种室温固化剂对硅树脂的耐热性能的影响进行了对比研究。结果表明,在氩气气氛下,硅树脂具有很高的耐热性能,它的起始分解温度为400℃,热失重主要由400-500℃时"解扣式"降解和500℃之后的"重排"降解引起。但在空气气氛下,由于有机基团的氧化分解,硅树脂的耐热性有所下降。KH-CL可使硅树脂在室温条件下固化,固化后硅树脂的耐热性能提高。     

直升机动力舱高温段流场及温度场的稳态模拟

利用有限体积法,建立了直升机发动机动力舱的有限元模型,并根据舱内实际冷却气体流通情况,分析了在不同的发动机附件散热量边界条件下,动力舱内流场及温度场的分布,以及流场对温度场的影响,为改善动力舱的冷却情况提供了分析依据。     

正弦波模型化测量方法及应用

本文对应用较多的几种正弦波模型化测量方法进行了综述，它们是曲线拟合法、直方图统计分析法、FFT法和拍频法。较详细地介绍了这几种测量方法的典型用途以及特点，通过比较几种方法的优缺点，讨论了它们应用中的局限性。     

求解可压缩N－S方程的无粘－粘性分数步法

用按物理过程作时间分裂的无粘－粘性分数步法求解可压缩Ｎ－Ｓ方程，无粘步用高效欧拉算法解欧拉方程，粘性步用全隐格式解抛物方程；并采取了有效措施消除由分步法产生的时间和空间不相容性，文中给出了轴对称喷管内外流场的数值模拟结果。