梯度加权局部分析解差分格式及其应用

提出了一种新的针对Ｎａｖｉｅｒ－Ｓｔｏｋｅｓ方程符合含有梯度项的对流扩散方程的梯度加权局部分析解的有限差分格式，且给出了通用的系数表达式。ＧＷ－ＬＡＤ格式是基于积分型的有限体积法并且通过附加源项的方法来实现。能够适用于粘性和无粘性及不可压缩和可压缩的压力驱动流动。通过对叶栅流道中二维湍流流的计算表明ＧＷＬＡＤ格式与ＥＤ格式相比，具有较高的精度和很快的收敛速度并且得到更好的压力场和速度场。     

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。     

随机声载荷时域信号仿真模型研究

利用航空发动机环行燃烧室噪声测试数据，采用时间序列自回归分析方法得到了燃烧室噪声及动压仿真模型ARMA（17，16），并用其对噪声时间历程数据进行了最佳预测。     

轴流压缩机粘性尾迹噪声研究

本文研究了微弯机翼在正弦阵风作用下的脉动升力,并导出计算公式,分析了动、静叶栅几何及气动参数对转子脉动升力及噪声级的影响。     

两相湍流的非线性k-ε-kp模型

由两相湍流的代数应力模型，提出一种两相湍流的非线性k-ε-kp模型，可以合理地模拟各向异性较强的旋流，浮力流等两相流动，具备二阶矩模型的优点，又比二阶矩模型简单。文中推导出气相、颗粒相的雷诺应力和两相脉动速度关联的非线性应力应变关系式。这些代数式和两相各自的湍动能k，kp以及两相脉动关联湍动能kpg的方程联立，就构成非线性k-ε-kp模型。本文将该模型用于模拟突扩湍流两相流动，给出两相时均速度场及雷诺应力各分量，并且将模拟结果和PDPA实验数据以及二阶矩模型的模拟结果对照。结果表明，该模型预报各向异性两相湍流的能力和二阶矩模型的能力接近，但是计算量比二阶矩模型的小得多。     

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。     

风对建筑绕流流动的数值方法

本文利用k-ε湍流模型及SIMPLE方法,在二维条件下,就风对建筑绕流流动进行了数值模拟,建筑及地面的边界条件采用以低Re数k-ε湍流模型中导出的壁函数处理近壁湍流。自由边界采用外推格式。对于计算域中的建筑物则利用控制粘性系数的方法处理。并对计算结果和风洞实验进行了比较。 为了研究建筑物之间的气流及压力分布,本文还对并列两栋建筑的不同情况进行了数值计算和分析。     

非参量量化秩检测器的性能研究

 许多作者讨论过非参量秩检测器在雷达信号处理中的应用。秩检测器首先把接收波形样本转换为秩。如果检验单元和参考单元的噪声样本独立和分布,则无信号时检验单元的秩具有离散均匀分布,与输入噪声的分布无关。所以秩检测器可能提供分布自由的恒虚警率性能。量化秩检测器（QRD）只对二进量化秩进行积累,所以它实现起来很经济。本文分析QRD的检测性能。证明QRD有一最佳秩量化门限（ORQT）。确定高斯和韦伯噪声中的ORQT。另外,把QRD同高斯噪声中的局部最佳秩检测器和最佳参量检测器进行比较。     

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.