酸酐固化剂对硅橡胶低密度烧蚀材料施工期的影响

通过对延长硅橡胶密度烧蚀材料体系施工期的研究，发现酸酐固化剂可以将环氧改性硅橡胶低密度烧蚀材料的施工期延长到24h以上，从而可能实现真空热压罐大面积灌注密度烧蚀材料的成型工艺。通过对固化材料进行红外分析，发现加入酸酐固化剂后并未改变硅橡胶和环氧树脂各自的反应，没有新的反应特征峰出现，说明环氧和硅橡胶之间无反应，只是物理共混，从材料拉伸断面的扫描电镜观察可以证实硅橡胶和环氧树脂以海－岛结构存在。     

轴向密流比对叶栅性能的影响

轴向密流比对叶栅性能有较大的影响,本文对该问题进行理论及实验研究,导出了叶栅主要性能参数与轴向密流比的关联方程,通过压气机叶栅吹风实验,得到了不同轴向密流比条件下的叶栅性能。理论计算与实验结果吻合的程度令人满意,表明文中所得出的理论关联式可以有效地估算轴向密流比对叶栅流动的影响,具有一定的实用价值。     

装备可靠性维修性保障性效能模型及其扩展

在装备效能分析中 ,装备的可靠性 (R)、维修性 (M )及保障性 (S)指标是影响装备效能的重要指标。通过对ADC模型分析的基础上 ,提出了装备的可靠性、维修性及保障性 (RMS)效能的概念 ,并从完成单阶段单任务拓展到多阶段多任务 ,推导出不可修装备RMS效能的综合表达式。从而为完成多阶段多任务的不可修装备的可靠性维修性保障性的效能的定量分析提供了理论依据。     

直升机旋翼试验台数据采集系统的改进与设计

本文详细介绍了直升机旋翼试验台数据采集系统的功能，硬件配置以及软件设计方法。     

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.     

再入弹抛壳气动特性研究

本文用有限差分方法求解再入母弹头与其所抛壳体之间的无粘干扰流场,获得了体—壳的干扰气动力,并在准定常假设的基础上近似模拟了弹体与壳体的分离过程。数值研究的结果表明,体—壳间存在的干扰会导致壳的压心位置急剧变化,危及母弹安全;抛壳速度是体—壳安全分离的关键参数。     

产生标准失真源的方法

介绍了失真的测量原理和产生标准失真源的方法；介绍了失真度测量仪自动测试系统，并对测量装置的误差进行了分析。     

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.     

Robust algorithm for combating look direction error problems

A simple and fast zero tracking algorithm for adaptive arrays with large look direction errors is presented and investigated. Basically, the algorithm is based on adjusting the complex zeroes of a power inversion array in a time-multiplexed manner to track all the sources in the environment. To preserve the desired signal which is supposed to be closest to the look direction of 0°, the algorithm removes the zero with the shortest distance to e^j0 so that the directional response consists of only nulls steered at the jammers. When compared with the least mean square (LMS) algorithm employing zeroth and first-order look direction constraints, the new algorithm has about the same implementation complexity, is considerably faster, and possesses a much better signal-to-noise ratio (SNR) performance when the look direction is erroneous     

基于VXI总线的检测软件设计

基于VXI总线和虚拟仪器技术，研制开发了用于外场的模拟式电子控制器检测软件，并对软件开发的过程和要求进行了分析，重点解决了程序设计中的需求分析和模块化设计问题。