用于海洋成像仪的离轴三反主光学系统设计

海洋成像仪光学系统要求在宽视场内具有高空间分辨率。该成像仪处于35800km高的静止轨道，在2．46°视场内地面分辨率需要达到250m，光谱覆盖范围为0．4～11．5μm，包括可见光近红外12个通道和远红外两个通道。介绍了满足这些要求的离轴三反射镜主光学系统的设计及结果，像质达到了衍射极限。     

CAD／CAE技术在工艺装备设计中的应用

在镜头的机床定心加工中，过渡环的刚度和质量是影响定心加工精度的主要因素，文章在分析过渡环在加工中的受力情况的基础上，使用Pro／E进行三维造型，使用PATRAN建立有限元模型，使用NASTRAN进行结构静力分析和模态分析，然后根据分析结果优化结构质量。     

空间光学精密展开机构展开方法的初步探讨

文章对空间光学精密展开机构(以下简称展开机构)进行分类,分析了几种典型可展开空间光学系统的展开方法和特点。讨论了展开机构设计需要考虑的主要因素,并给出设计建议。     

空间相机像移补偿方法研究

介绍了空间相机拍照时产生像移的机理及国内外目前较常使用的不同像移补偿方法,并对光、机、电等不同实现方法进行分析比较,得出各种方法的优缺点及适用范围。     

提高航天传输型CCD相机地面像元分辨率方法研究

文章首先对空间传输型遥感相机提高像元分辨率的几种常规和非常规方法做了简介,在分析这些方法的优缺点以及以采样定理为依据分析我国现有CCD相机光学截止频率和CCD采样频率存在的矛盾的基础上探讨了高模式采样技术和超模式采样技术,经过比较这两种采样模式,认为超模式采样技术更具有工程可行性和优越性。然后对超模式采样计算机图像仿真结果进行了分析。     

遥感卫星CCD相机光学系统的热补偿设计

文章对遥感卫星CCD相机光学系统的热补偿设计进行了论述。     

俄罗斯第五代光学侦察卫星

文章主要论述俄罗斯第五代光学侦察卫星(涅曼卫星)的飞行历史,包括发射日期选择,轨道选择和轨道机动、使用和工作寿命等内容。     

应用联合变换相关器的成像制导系统

提出了一种光电混合的成像制导系统，它采用光学联合变换相关器作为其主要的图像识别单元，利用计算机对识别结果进行判决和显示，并发出跟踪信号给导引头，从而实现制导。联合变换相关器是对光学图像信号进行并行处理的器件，实时识别性能强，精度高。此成像制导系统克服了传统的红外制导系统易受外界因素影响，实时处理能力差，误判率较高的缺点，具有并行处理速度快、信息吞吐量大、体积小等优点，应用前景广阔。     

洪都集团企业级信息系统数据备份策略研究

分析了洪都集团当前企业级信息系统数据备份系统中存在的问题,结合目前的主流数据备份策略,提出了基于SAN(存储局域网)的高速、可靠、安全的洪都集团新的企业级信息系统数据备份策略。     

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.