街道峡谷湍流流动的风洞试验与数值计算

在１：２５０的风洞模型上,测量街道峡谷的平均流速,湍流度等参数,分析了街道峡谷内的湍流流动状态,探讨了屋顶来流风在街道峡谷内产生复杂流场的主要特征,并用三维湍流流模型对风洞试验模型进行了数值计算,试验和计算结果为研究街道峡谷风环境以及街道峡谷的传热传质过程提供了基础。     

钛合金近β锻造研究

 提出钛合金塑性变形中一种新的热加工方法——钛合金近β锻造。试验和生产实践表明,它能在不影响合金塑性、不降低热稳定性的条件下,显著地提高合金的高温性能、低周疲劳性能和断裂韧性、使钛锻件具有最好的塑性、热强性和断裂韧性的综合。新工艺适用于（α+β）型合金,可应用于α型和近α型合金。     

叶片失速颤振发作机理的探讨

 本文对于现有的叶片失速颤振计算模型进行了一些改进,以期使其更接近于真实物理图画。计算结果表明,就槽道激波以及物面气流分离对于叶片气动弹性稳定性所起的作用来看,在单自由度纯弯振荡和双自由度弯曲主导振荡两种情况之下是具有实质性差别的。在文中对于一个实际转子的失速颤振边界进行了数值预测,并与相应的实验结果进行了对比。     

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。     

基于8098单片机的飞行指引系统综合测试装置

介绍一种基于8098单片机的飞行指引系统综合测试装置，给出了飞行指引系统综合测试装置的用途。主要硬件组成和软件设计方法。     

两级固体火箭联合动力装置的参数优化

本文针对某型导弹由两级固体火箭发动机组成的联合动力装置进行九变量寻优计算.通过采用二维抛物线插值方法及合理组织迭代的技巧,解决了庞大的目标函数计算子程序耗时太多的问题;经大量调试,协调寻优步长、罚因子、收敛精度,最后成功地完成了本文的九维寻优计算,得到了能稳定收敛的最优解.所得最优方案比原参考方案的发动机总重减轻7.03kg(约占总重的2%).     

Silicon Solar Cell Performance at High Intensities

The theoretical and experimental work performed since 1960 in the area of high-intensity and high-temperature operation of silicon and gallium arsenide photovoltaic devices is reviewed. Test results for conventional 5-grid silicon cells, for specially designed 13-grid silicon cells, and for a GaAs cell are presented parametrically for the illumination intensity range from 0.07 to 2.8 W/cm2 and the temperature range from 30 to 1 50°C. The data cover the 3 points on the currentvoltage characteristic required to reconstruct the full characteristic in the power-generating quadrant. The 13-grid silicon cells showed much better performance than the GaAs cell.     

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.     

某型涡喷发动机的可靠性增长分析

针对某型涡喷发动机的一组含零故障的多台不同步截尾故障数据。给出了趋势检验、AMSAA模型的拟合优度检验及模型参数的极大似然估计方法。分析表明，该型发动机有显著的可靠性增长，且可用AMSAA模型拟合其故障数据，在考虑零故障后，其参数及MTBF的极大似然估计（MLE）更为可信。     

Huygens Probe Aerosol Collector Pyrolyser Experiment

ACP's main objective is the chemical analysis of the aerosols in Titan's atmosphere. For this purpose, it will sample the aerosols during descent and prepare the collected matter (by evaporation, pyrolysis and gas products transfer) for analysis by the Huygens Gas Chromatograph Mass Spectrometer (GCMS). A sampling system is required for sampling the aerosols in the 135'32 km and 22'17 km altitude regions of Titan's atmosphere. A pump unit is used to force the gas flow through a filter. In its sampling position, the filter front face extends a few mm beyond the inlet tube. The oven is a pyrolysis furnace where a heating element can heat the filter and hence the sampled aerosols to 250 °C or 600 °C. The oven contains the filter, which has a thimble-like shape (height 28 mm). For transferring effluent gas and pyrolysis products to GCMS, the carrier gas is a labeled nitrogen ¹⁵N₂, to avoid unwanted secondary reactions with Titan's atmospheric nitrogen. Aeraulic tests under cold temperature conditions were conducted by using a cold gas test system developed by ONERA. The objective of the test was to demonstrate the functional ability of the instrument during the descent of the probe and to understand its thermal behavior, that is to test the performance of all its components, pump unit and mechanisms. In order to validate ACP's scientific performance, pyrolysis tests were conducted at LISA on solid phase material synthesized from experimental simulation. The chromatogram obtained by GCMS analysis shows many organic compounds. Some GC peaks appear clearly from the total mass spectra, with specific ions well identified thanks to the very high sensitivity of the mass spectrometer. The program selected for calibrating the flight model is directly linked to the GCMS calibration plan. In order not to pollute the two flight models with products of solid samples such as tholins, we excluded any direct pyrolysis tests through the ACP oven during the first phase of the calibration. Post probe descent simulation of flight results are planned, using the much representative GCMS and ACP spare models. This revised version was published online in August 2006 with corrections to the Cover Date.