假人空投试验六分量天平研究

依据救生伞假人空投试验中六分量应变天平的工作条件与载荷特点,确定了天平的设计载荷并完成了结构设计。针对实际应用中天平各种极限载荷情况,计算了天平各弹性元件的安全系数。对天平应力场进行了有限元分析,获取了天平整体应力分布状况。进一步对传统计算结果进行了验证,为天平结构设计提供了理论依据。     

基于外包合同网的自治电磁探测卫星群任务规划

针对具有星间通信能力的自治电磁探测卫星群任务及载荷特点,建立了基于MAS (Multi\|Agent System)的电磁探测卫星群自主规划模型,提出了基于外包合同网的电磁探 测卫星群自主规划算法。根据模拟的数据进行仿真实验及分析,该方法能有效解决电磁 探测卫星群自主任务规划问题。
     

脉冲发动机陶瓷隔板的设计和试验研究

提出了陶瓷隔板及其组件的设计方法,对陶瓷隔板结构进行应力计算,得到了符合工作要求的陶瓷隔板结构形式。对有无刻痕的2个陶瓷隔板进行了耐压和破碎试验,并对试验结果进行了分析。研究表明,采用可切削加工玻璃陶瓷材料设计的等厚度圆拱形隔板具有凸侧耐压高不易破碎、凹侧耐压低易破碎的特点,满足脉冲发动机隔板使用要求。隔板拱顶和隔板与预紧压盖接触边界附近为应力较大区域。有刻痕隔板虽未完全按刻痕破碎,但刻痕减小了隔板碎片形状和尺寸的随机性,有助于形成规则的破口形状。     

AP/HTPB复合推进剂燃烧的详细化学动力学建模(英文)

采用详细化学动力学机理,为AP/HTPB复合推进剂的燃烧建立了模型。该模型包含2个步骤:前一个是数据准备阶段,后一个是求解阶段。模型中包含了完整的固相、凝相和气相三相反应机理,其中气相反应机理由37个组分和127个反应步组成。为了提高模型的求解效率,用于评估化学反应的先进算法ISAT也被应用。最终,通过与试验结果的比较可看到,所建模型是可靠和精确的,并优于以往模型。     

Dynamics of Planetary Waves in the Ionosphere as Observed from GPS Satellites

The GPS satellite data are used to study the dynamics of the ionospheric total electron content (TEC) over Central Europe in the summer season from June 23 to September 30, 1996. The TEC variations within the range of periods typical of the planetary waves were found to be nearly synchronous with the neutral wind variations in the mesosphere and with the variations in the occurrence of ionospheric sporadic layers. The observed TEC variations were interpreted as the result of penetration of energy carried by nonstationary Rossby waves to the upper atmospheric altitudes.     

内喷管间隙宽度对线性塞式喷管性能的影响

为了了解内喷管间隙宽度对线性塞式喷管性能的影响，提出了对应着同一个内喷管的三种不同间隙宽度的塞锥。采用数值模拟的方法，得到了不同间隙宽度的线性塞式喷管在不同工况下的流场和性能。比较了不同间隙宽度对线性塞式喷管性能的影响，结果表明：增加内喷管间隙会增大线性塞式喷管的面积比和设计压比；内喷管间隙变宽，塞锥表面的压强下降，塞式喷管的性能下降，间隙宽度增大一倍，塞式喷管性能下降1％～3％。另外在计算过程中发现，内喷管的性能是整个线性塞式喷管性能的主要组成部分，占了整个塞式喷管性能的三分之二以上。     

点阵结构空气舵及内部流体热流固耦合研究

开展了钛合金TC4材料激光粉末床熔融(LPBF)工艺研究,在此基础上设计了多孔轻质空气舵模型,并基于有限差分法(FDM),采用三维流固耦合共轭传热数值计算方法,利用流体体积法(VOF)追踪流体自由液面,研究了典型的点阵夹层结构的空气舵内部冷却液动态换热过程的相互影响过程,考虑了冷却液与钛合金材料蒙皮间的耦合传热及湍流换热。结果表明,空气舵的内部流体压强随速度的增加而增加,从而导致流体出口的速度增加。当压强增加到一定程度时,流体的出口以水柱形式喷出。虽然较大的流体速度可以带走较多的热量,但是影响远小于对压强的影响。综合考虑空气舵的服役要求,获得了合适的冷却水入口速度。     

刘家峡右岸水电站模型试验的光路布置

使用二维激光多普勒测速仪（ＬＤＶ）对圆管中水注流进行测速时,对于窗口的设置、利用反射镜前向接收的方法和侧向接收方式等问题,本文进行了探讨,并总结了测量中的一些实际经验。     

灯丝放电磁场约束型原子氧效应地面模拟试验设备

介绍了用于原子氧剥蚀效应研究的灯丝放电磁场约束型地面模拟设备 ( IFM)的构成及工作原理,简单阐述了装置的运行测量结果,分析了等离子体参数随试验条件的变化趋势。并用 IFM设备对 Kapton空间用材料进行了地面模拟试验,试验结果与国外空间飞行暴露试验结果相似     

Far ultraviolet imaging from the IMAGE spacecraft. 2. Wideband FUV imaging

The Far Ultraviolet Wideband Imaging Camera (WIC) complements the magnetospheric images taken by the IMAGE satellite instruments with simultaneous global maps of the terrestrial aurora. Thus, a primary requirement of WIC is to image the total intensity of the aurora in wavelength regions most representative of the auroral source and least contaminated by dayglow, have sufficient field of view to cover the entire polar region from spacecraft apogee and have resolution that is sufficient to resolve auroras on a scale of 1 to 2 latitude degrees. The instrument is sensitive in the spectral region from 140–190 nm. The WIC is mounted on the rotating IMAGE spacecraft viewing radially outward and has a field of view of 17° in the direction parallel to the spacecraft spin axis. Its field of view is 30° in the direction perpendicular to the spin axis, although only a 17°×17° image of the Earth is recorded. The optics was an all-reflective, inverted Cassegrain Burch camera using concentric optics with a small convex primary and a large concave secondary mirror. The mirrors were coated by a special multi-layer coating, which has low reflectivity in the visible and near UV region. The detector consists of a MCP-intensified CCD. The MCP is curved to accommodate the focal surface of the concentric optics. The phosphor of the image intensifier is deposited on a concave fiberoptic window, which is then coupled to the CCD with a fiberoptic taper. The camera head operates in a fast frame transfer mode with the CCD being read approximately 30 full frames (512×256 pixel) per second with an exposure time of 0.033 s. The image motion due to the satellite spin is minimal during such a short exposure. Each image is electronically distortion corrected using the look up table scheme. An offset is added to each memory address that is proportional to the image shift due to satellite rotation, and the charge signal is digitally summed in memory. On orbit, approximately 300 frames will be added to produce one WIC image in memory. The advantage of the electronic motion compensation and distortion correction is that it is extremely flexible, permitting several kinds of corrections including motions parallel and perpendicular to the predicted axis of rotation. The instrument was calibrated by applying ultraviolet light through a vacuum monochromator and measuring the absolute responsivity of the instrument. To obtain the data for the distortion look up table, the camera was turned through various angles and the input angles corresponding to a pixel matrix were recorded. It was found that the spectral response peaked at 150 nm and fell off in either direction. The equivalent aperture of the camera, including mirror reflectivities and effective photocathode quantum efficiency, is about 0.04 cm². Thus, a 100 Rayleigh aurora is expected to produce 23 equivalent counts per pixel per 10 s exposure at the peak of instrument response.