虚拟装配技术在发动机漏油箱设计中的应用

以航空发动机漏油箱的改进设计为例，介绍了利用UG的特征和装配模块展开其成员组件的装配环境设计和修改工作，以便使其能够最大限度满足类似漏油箱一类具有修配性质的结构件的设计安装要求。通过示例可以看出，该设计方法对外部配置变化具有较主动的适应能力，从而能明显减少人工反复时产生的非一致错误。     

叉流管－管型换热器二维温度场的数值分析

建立并导出叉流管－管型换热器传热过程的二维数学模型及相应的差分格式，对比实验数据和性能计算结果，表明数值方法是有效可行的。据此编制的计算机程序已成功地用于组合发动机空气预冷换热器工作过程的预测。     

复合材料板壳在过屈曲下最佳铺层设计的工程方法

 本文基于相同边界条件下铺层构成对失稳后的变形形态影响不大的基本假设,根据理论和实践经验得到的准最佳铺层失稳后的位移场为基础,给出了确定最佳铺层参数的工程方法。计算表明,其基本假设和解题思路是正确的。由于本方法最后归结为解一个一元三次方程,使计算大为简化,可降低设计成本和周期,在工程设计中具有实际意义。     

用于棘轮变形预测的棘轮演化统一模型研究

 在大量单轴棘轮实验基础上,研究了均值、幅值、峰值和谷值应力对 304不锈钢的饱和棘轮应变的影响规律,首次提出了棘轮应力σ_r和棘轮门槛值σ_rth 的概念,建立了基于单参数控制的、用于饱和棘轮应变预测的 SRM饱和棘轮本构模型和用于独立循环应力工况下棘轮应变演化预测的 REM棘轮演化模型,并由此发展了全面描述任意循环应力工况下棘轮应变演化规律的 URM棘轮演化统一模型。抛物律模型 SRM和幂律模型 REM对实验数据拟合的相关系数均超过 0.98。URM建模容易,只需 4～ 6个试样的单轴棘轮实验数据。此外还讨论了获得 SRM本构模型的单试样实验法。     

基于CMMI的软件测试项目过程管理

针对独立的第三方软件测试项目特点,运用基于CMM I的软件项目管理方法,将需求管理、测试项目策划、项目监督与控制、质量保证和配置管理要求贯彻在软件测试过程中,给出了软件测试项目过程管理解决方案。该方案保证了软件测试项目的质量,提高了测试项目的技术水平和管理水平。     

非刚性基准浮动工件宽度的在线测量

介绍１种用标准长度作基准，以自扫描光电二极管列阵作光电传换器，微型计算机进行数据处理，对基准浮动的非刚性工件宽度进行在线测量的测量装置。     

液氮纯度分析的偏差及修正

液氮纯度是液氮产品非常关键的一个技术指标.液氮纯度的在线跟踪测量是通过测量液氮中的氧含量来实现的.在多年来的液氮在线分析及液氮出库分析过程中,发现氧含量测量结果普遍偏低.本文通过理论分析及大量的实验数据,找到了数据产生偏差的原因,并给出了科学的修正办法,为以后液氮生产过程中更加有效地控制产品质量打下了基础.     

钼-铌合金原料品质对单晶制备的影响

主要讨论了钼-铌合金原料品质,包括烧结条的制备、原料的化学成分、原料棒的尺寸规格等对单晶制备的影响。结果表明:高温真空烧结钼-铌合金烧结条由于C、O等杂质含量过高,在20 kW电子束悬浮区域熔炼炉上区域熔炼时未能直接生长制备出单晶,但其经过两次电子束熔炼获得的Ф(12~17)mm原料棒C元素质量分数降为6.3×10-3%、O元素质量分数降低了近2个数量级,仅为1.4×10-3%,能稳定地生长制备出Ф31 mm×735 mm的大尺寸钼-铌合金单晶,而直径超过Ф18 mm或小于Ф11 mm原料棒在区域熔炼时未能获得钼-铌合金单晶。     

钝锥有攻角分离流动的数值模拟及其分析

本文定性分析了开式分离的性状,并对钝锥有攻角超声速绕流的开式分离作了数值模拟。分析指出,开式分离可能存在两种形态,第一种分离线的起点为正常点,第二种分离线的起始为鞍、结点(包括螺旋点)的组合。对于第一种形态,分离线的起点是横向分离的起始点,除分离线外,分离面上的流线不是从分离线的起点发出的。对文中计算的情况,流动属第一种开式分离。计算证实了定性分析的结论。计算和分析均指出,对第一种开式分离,在分离的起始区域,分离流面尚未卷曲,但在下游,则变成卷曲面。文中还研究了围绕物体的流管在分离诱导下的变形情况。     

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.