平面运动激波在定常超音速劈表面马赫反射的研究

本文介绍了在电控双驱动激波风洞中进行的平面运动激波在有定常超音速绕流的尖劈表面马赫反射的实验。这种反射现象属于准定常的,在实验中观察到了四种反射(RR,SMR,CMR和DMR)。本文还计算了三波点Τ的迹线及弯折点Κ的迹线分别和劈面的夹角χ和χ',以及各种反射相互转变的边界。发现运动激波波前定常超音速气流马赫数Μ_0会影响χ和χ'角,使(θ_ω+χ,Μ_s)平面上各种反射的转变边界发生变化,但不影响(θ_w,Μ_s)平面上的各条转变边界线。     

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。     

一个基于WINDOWS环境的网络连接服务

该文介绍了在校园网环境及WINDOWS平台，采用TCP/IP协议设计并开发PING网络连接服务和客户机/服务器功能的VC^ 程序。     

机翼/外挂系统的颤振主动抑制研究

 本文对颤振主动抑制控制律进行了研究。研究对象为一小展弦比带外侧导弹的机翼颤振模型,模型具有外侧后缘控制面。依据该模型的全部动力特性和刚度特性,以最优控制为基础,采用动态补偿器方法,设计了两阶控制律。对该控制律进行了风洞实验验证。实验结果表明:颤振临界速度提高了14％以上。理论计算结果与实验结果一致。     

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。     

网上考试系统的设计与实现

本文讨论了一种新的考试方法———网上考试 ,并讨论了一种基于B/S系统实现网上考试的思路和设计方法 ,并对实现网上考试系统的部分关键技术进行了分析     

民机数据总线信号综合测试仪

介绍的民机数据总线信号测试仪综合了当前民机上主要采用的ARINC429、ARINC419、CSDB和RS232等数字式航空数据总线规范的接口，具有和这些总线接口设备通讯的能力，可以灵活方便地应用于机载设备检测，装机交联实验当中。     

TiAl合金不同钛铝比层片组织的稳定性

对钛铝比为１．１７４、１．１０５和１．０４１的（ＴｉＡｌ）－２．５Ｖ－１Ｃｒ（ａｔ％）合金层片组织在１３２３Ｋ热暴露中的组织变化进行了观察和分析。发现钛铝比对ＴｉＡｌ合金层片组织的稳定性和失稳分解机理有重要影响，钦铝比适当大于１：１（如１．１０５）的合金可以得到稳定性更好的层片组织。     

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。     

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.