位标器陀螺转子的动平衡

阐述了具有阿基米德螺旋线图案的位标器的基本原理及其运动规律，并说明这种陀螺转子的振动与绕动的平衡原理与方法。     

航电系统的处理机重构算法与实现

主要阐述了满足新一代航空电子系统中核心数据综合处理要求的实时操作系统 ;概述了系统软件的三个主要层次的总体结构 ;着重论述了重构处理机的问题 ;并详细讨论了处理机容错重构处理的实施过程。     

中、高密度Nomex蜂窝力学性能研究

研究了航空用三种中、高密度Nomex蜂窝的力学性能 ,并讨论了纸的厚度、浸渍溶液浓度、环境湿度和渗透剂对Nomex蜂窝力学性能的影响。结果表明 ,选择厚度合适的Nomex纸 ,严格控制湿度 ,并在浓度为 35 %～5 0 %范围内浸渍胶液中加入适量的渗透剂可以制作出与国外同类产品性能相当的高性能中、高密度Nomex蜂窝     

多孔层板换热特性实验研究

本实验选取了一种典型结构的多孔层板作为研究对象 ,进行了换热特性实验研究。研究了改变冷热气流吹风比对该型层板冷却效果的影响。另外 ,对该型多孔层板的冷却效果沿中轴线顺气流方向的变化规律也作了深入的研究。并给出了层板局部 N ux 和冷却效果 E关于局部 Rex 及冷热气流吹风比 M的数学拟合表达式。     

高温相变单元管蓄热过程数值模拟

对以高温共晶盐 Li F-Ca F2 为相变材料 (PCM)和以干空气为工质的相变蓄热系统 ,采用焓方法建立了以控制体单元为对象的单管相变蓄热模型。在模拟空间站太阳能吸热 /储热器轨道运行参数下进行了数值计算。计算结果与地面模拟试验数据进行了比较 ,吻合良好。     

塞式喷管底部二次流的数值模拟研究

从 N-S方程出发 ,采用二阶精度的 NND格式对塞式喷管的流场进行了数值模拟 ,重点研究了一线性塞式喷管底部二次流在低中高空的特性。研究表明 ,塞式喷管底部回流区的消失不仅与二次流流量大小有关 ,而且与底部压强有关 ;加入二次流会使塞式喷管的推力上升 ,但在大多数情况下其比冲会下降 ,只有特定压强比条件下 ,加入少量的二次流比冲才会上升     

发动机孔探图像三维测量与立体重建的实现

作为一种新兴的可视探测技术，孔探成像分析在现代发动机故障诊断中一直发挥着重要的作用。研制和开发基于孔探图像的三维测量与立体重建系统对提高故障诊断水平和预测准确度，降低工作中的人力物力投入，节约维护成本都有着重要的现实意义。本文以整体系统的构架为线索，阐述了系统的图像采集，摄像机标定，图像预处理，立体匹配，3D计算以及深度重建等功能模块的研制思路和基本算法，并给出部分研制结果。本系统的开发为基于也探图像的发动机故障监测与诊断系统的奠定了重要的基础。     

基于CCD的底片判读仪透射屏厚度精确测量

提出了一种利用线阵CCD传感器作为接收装置，以8253编程芯片实现自动测量并实时显示测量结果的底片判读仪透射屏厚度测量系统。文中主要论述了该系统的工作原理和软硬件的实现途径，并分析了系统的测量误差；文章最后列出了实测数据，证明了系统的可行性和先进性。     

The Cassini Cosmic Dust Analyzer

The Cassini-Huygens Cosmic Dust Analyzer (CDA) is intended to provide direct observations of dust grains with masses between 10⁻¹⁹ and 10⁻⁹ kg in interplanetary space and in the jovian and saturnian systems, to investigate their physical, chemical and dynamical properties as functions of the distances to the Sun, to Jupiter and to Saturn and its satellites and rings, to study their interaction with the saturnian rings, satellites and magnetosphere. Chemical composition of interplanetary meteoroids will be compared with asteroidal and cometary dust, as well as with Saturn dust, ejecta from rings and satellites. Ring and satellites phenomena which might be effects of meteoroid impacts will be compared with the interplanetary dust environment. Electrical charges of particulate matter in the magnetosphere and its consequences will be studied, e.g. the effects of the ambient plasma and the magnetic field on the trajectories of dust particles as well as fragmentation of particles due to electrostatic disruption.The investigation will be performed with an instrument that measures the mass, composition, electric charge, speed, and flight direction of individual dust particles. It is a highly reliable and versatile instrument with a mass sensitivity 10⁶ times higher than that of the Pioneer 10 and 11 dust detectors which measured dust in the saturnian system. The Cosmic Dust Analyzer has significant inheritance from former space instrumentation developed for the VEGA, Giotto, Galileo, and Ulysses missions. It will reliably measure impacts from as low as 1 impact per month up to 10⁴ impacts per second. The instrument weighs 17 kg and consumes 12 W, the integrated time-of-flight mass spectrometer has a mass resolution of up to 50. The nominal data transmission rate is 524 bits/s and varies between 50 and 4192 bps.This revised version was published online in July 2005 with a corrected cover date.     

2001 Mars Odyssey Mission Summary

The 2001 Mars Odyssey spacecraft, now in orbit at Mars, will observe the Martian surface at infrared and visible wavelengths to determine surface mineralogy and morphology, acquire global gamma ray and neutron observations for a full Martian year, and study the Mars radiation environment from orbit. The science objectives of this mission are to: (1) globally map the elemental composition of the surface, (2) determine the abundance of hydrogen in the shallow subsurface, (3) acquire high spatial and spectral resolution images of the surface mineralogy, (4) provide information on the morphology of the surface, and (5) characterize the Martian near-space radiation environment as related to radiation-induced risk to human explorers. To accomplish these objectives, the 2001 Mars Odyssey science payload includes a Gamma Ray Spectrometer (GRS), a multi-spectral Thermal Emission Imaging System (THEMIS), and a radiation detector, the Martian Radiation Environment Experiment (MARIE). THEMIS and MARIE are mounted on the spacecraft with THEMIS pointed at nadir. GRS is a suite of three instruments: a Gamma Subsystem (GSS), a Neutron Spectrometer (NS) and a High-Energy Neutron Detector (HEND). The HEND and NS instruments are mounted on the spacecraft body while the GSS is on a 6-m boom. Some science data were collected during the cruise and aerobraking phases of the mission before the prime mission started. THEMIS acquired infrared and visible images of the Earth-Moon system and of the southern hemisphere of Mars. MARIE monitored the radiation environment during cruise. The GRS collected calibration data during cruise and aerobraking. Early GRS observations in Mars orbit indicated a hydrogen-rich layer in the upper meter of the subsurface in the Southern Hemisphere. Also, atmospheric densities, scale heights, temperatures, and pressures were observed by spacecraft accelerometers during aerobraking as the spacecraft skimmed the upper portions of the Martian atmosphere. This provided the first in-situ evidence of winter polar warming in the Mars upper atmosphere. The prime mission for 2001 Mars Odyssey began in February 2002 and will continue until August 2004. During this prime mission, the 2001 Mars Odyssey spacecraft will also provide radio relays for the National Aeronautics and Space Administration (NASA) and European landers in early 2004. Science data from 2001 Mars Odyssey instruments will be provided to the science community via NASA’s Planetary Data System (PDS). The first PDS release of Odyssey data was in October 2002; subsequent releases occur every 3 months.