直接的矩阵分裂计算跨音速喷管流场

给出了分离系数矩阵求解欧拉方程组时系数矩阵的直接分离公式，减少和简化了应用该方法时的矩阵运算，参照Ｂｅａｍ－Ｗａｒｍｉｎｇ显式格式构造与ＳＣＭ方法一致的内点差分格式，并分析了它的数值特性，对有斜激波的跨音速内流场进行了数值仿真。计算中采用变系数的当地时间步长，加快了流场达到的收敛速度，计算无需引入任何人工参数，计算值与实验结果吻合。     

燃气轮机分布式控制系统设计

阐述了燃气轮机分布式控制系统的技术方案,详细介绍了该系统的硬件电路设计、软件设计和控制模块机箱设计,为配合动力控制系统的发展提供了新的思路。     

汽车尾气分析仪中的大气压力补偿技术

控制汽车尾气量的增加,是减少汽车废气污染改善人类生活环境的重要措施。汽车尾气分析仪主要是通过检测汽车尾气中不同气体的含量,以达到合理控制的目的。在对气体浓度的检测中,大气压力的影响不能忽视。本文围绕这个问题,详细讨论了大气压力影响的补偿方法。     

直升机飞行控制系统的快速原型设计

针对直升机飞行控制的特点，结合国际直升机界的研究热点，提出了直升机飞行控制的快速原型设计方法，该方法分利用当今计算机领域的最新技术，在不牺牲系统性能的前提下，以最低的成本，最快的速度，构建最小规模的实时系统和直观的控制系统设计界面，并提供完整的验证手段。     

虚构解方法程序验证

对求解偏微分方程问题的程序的严格验证,一直以来由于其精确解有限,较难进行,针对这种情况,本文给出了一种新的程序验证方法,虚构解方法,该方法旨在解决大型科学计算程序如何较严格地进行程序验证这一问题;该方法通过构造虚构解,修改原控制方程,然后通过对计算结果的分析处理达到对程序的精确验证;文中给出了一组通用的虚构解的选取办法,解决了虚构解方法验证过程中确定虚构解的问题;同时还给出了运用该方法对非结构二维Euler计算程序进行验证的具体例子,网格收敛分析结果表明该方法是一种有效的程序验证方法,并且具有较好的通用性。     

线性有延迟的微分方程的解

在解决一些有关生物数学的问题时，经常会遇到求解具有延迟的微分方程。到目前为止，还没有非常有效的方法求解这类方程，只是对于一小部分具有特殊形式可以求解。介绍一种此类方程的解法，其主要思想是把微分方程转化为一般的代数方程求解，然后研究解的稳定性，技巧性很强。     

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。     

喷管流场和羽流场的N－S数值模拟

利用时间推进的方法，通过求解可压缩的、雷诺平均的Ｎ－Ｓ方程，并利用Ｂａｌｄｗｉｎ－Ｌｏｍａｘ两层代数滴流模型和Ｐｒａｎｄｔｌ混合长度模型，数值模拟了飞机和火箭发动机喷管的内流和羽流，获得了喷管内流场和羽流场的参数分布，计算结果与试验结果及国外研究成果一致。网格划分采和了自适应网格技术。     

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。