六类高超声速激波-激波干扰的数值模拟研究

基于粘性全N-S方程，利用有限体积法进行数值离散，对Ⅰ到Ⅵ六种类型的激波一激波干扰现象进行了数值模拟，其中采用了二阶Harten-TVD格式，LU隐式算法以及Baldwin-Lomax代数湍流模型。每种类型都得到了清晰的干扰流场结构，其中Ⅳ型干扰的模拟结果与实验结果进行了比较，符合较好。数值模拟结果的对比指出，由入射位置差异引起的不同类型激波-激波干扰结构有很大不同，对壁面压强分布的影响也存在较大差异。     

基于SIMULINK的超声速进气道仿真方法

将进气道一维流动的偏微分方程离散为一系列可积分的线性常微分方程,基于此创建了超声速进气道仿真模型,提出了一种基于SIMULINK的进气道仿真方法,模拟了来流参数和燃烧室反压扰动时流场内各个参数的变化规律。对一个一维变几何超声速进气道进行仿真,获得了结尾正激波的稳态特性及动态特性。该模型定义并输出了激波位置,有效地将一维超声速进气道的分布参数问题转换为零维问题,解决了系统分析与控制系统设计中无法实现集总参数的困难。     

三维管道超声速气固两相流动的CFD/DSMC仿真

采用NND格式求解气相N-S方程，采用DSMC方法模拟固相颗粒运动，数值模拟了三维管道超声速气固两相流场，分析了固体颗粒对流场结构产生的影响。计算结果表明，将DSMC方法与CFD方法相结合是解决气固两相流动问题的一种有效途径。     

动静圆柱坐标系下N-S方程的分区算法及子域干涉处理研究

耦合了相对和绝对圆柱坐标系下三维Navier-Stokes方程,统一了动子域和静子域的控制方程;在子域计算中,采用高分辨率的三阶ENN格式及LU-SGS隐式解法;在子域干涉处理中,研究并对比了动静子域干涉面的重合处理与重叠处理;最终发展了一种新的既高效又准确的分区算法。通过对某带进口导叶的三级跨声速轴流压气机叶栅内三维紊流流场的数值模拟,验证了该分区算法的有效性,计算结果与实验数据吻合较好。     

单晶高温合金接近使用条件下的寿命估算与损伤分析

针对发动机热端部件承受的典型载荷谱，发展了一种通用的寿命预测方程和损伤分析方法。这个方法是在疲劳蠕变交互作用断裂特征图及其最大应力修正的寿命方程基础上建立的。根据ＤＤ３单晶合金的疲劳蠕变交互作用断裂特征图及其最大应力修正的寿命方程，验证了本方法是切实可行的。预测精度是符合要求的。     

航空制件超声检测中的声场特性分析

 针对航空制件超声检测中影响缺陷定量准确性的声场问题进行了深入讨论, 研究了脉冲波声场的计算方法, 设计了相应的计算软件并绘制出实用换能器声轴线上的声压分布曲线, 分析了不同材料和厚度的采样回波对频谱的影响, 比较了连续波声场和脉冲波声场的分布特性及异同点。研究结果为提高超声检测中缺陷定量的准确性和科学性提供了依据。     

薄膜材料和纤维材料的热扩散率测量

介绍了激光热波技术用于测量薄膜材料和纤维材料热扩散率的测试系统，测试温度范围为２０－５００℃。讨论了测量中的各种试验条件、基本公式和误差分析。在理论上此系统可以应用于任何厚度样品面向热扩散率的测量。     

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.     

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。     

旋转爆轰流场的数值模拟

基于带化学反应的二维Euler方程,采用氢气-空气的9组分19步基元反应简化模型,对充有当量比的氢气-空气预混气和空气的环形旋转爆轰流场,从点火燃烧到发展成旋转爆轰的过程进行了数值模拟。根据数值结果分析了波后流场中爆轰产物受激波、高温和离心力等作用而挤向外壁,形成有利于充入燃料,实现持续稳定旋转爆轰的流场特征。还讨论流场中爆轰波、激波与间断面和内外壁面反射或折射,从而形成多个激波相交的波系特征。为认识和理解旋转爆轰流场,开展旋转爆轰的实验研究等具有现实的指导意义。