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11.
文中就中分辨率成像光谱仪的焦平面设计进行了分析,根据中分辨率成像光谱仪的谱段配置、微型组合滤光片研制难度、辐照分辨率、空间分辨率等具体情况,提出了详细的焦平面设想:在可见光波段焦平面(VIS FPA)采用镶嵌蓝光增强PIN二极管列阵,近红外焦平面(NIR FPA)采用红外增强PIN二极管列阵,读出采用CMOS多路读出及源跟随器输出结构,以相关双取样电路消除背景噪声、复位噪声和热噪声,每列探测器对应一路前置放大器;短波红外焦平面(SWIR FPA),探测器采用光伏HgCdTe器件,采用直接注入多路读出电路;长波红外焦平面(LWIR FPA),探测器采用光导HgCdTe器件,读出电路为与光敏元一一对应的前置放大器,主放大器,然后以模拟开关变为串行输出,文中还就各FPA的信噪比、量子效率、串音等进行了分析,提出了各焦平面的最佳工作温度、响应率和一致性等要求。 相似文献
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燃气蒸汽式发射系统内弹道若干问题研究 总被引:3,自引:0,他引:3
通过对燃气蒸汽式发射动力系统的研究,总结出影响内弹道计算精度的若干因素,并就其中几个影响较大的问题进行了详细的分析,开发研制出了一套用于预估内弹道性能的系统化程序。通过实验数据的比较,验证了适用于内弹道计算的数学物理模型,为燃气蒸汽式发射系统设计提供参考依据。 相似文献
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制造误差对气体静压轴承涡流力矩影响分析方法研究 总被引:5,自引:0,他引:5
采用有限元方法研究了制造误差对狭缝节流气体静压轴颈—止推轴承的涡流力矩的影响。对于轴颈—止推相连结构的气体轴承,通过相容变换进行统一编程计算;在离散化过程中,利用加权余量法将二阶偏微分方程降低一阶,放松了对插值函数连续度的要求,便于借助有限元技术分析狭缝节流气体静压轴承的流场参数。分析了狭缝气膜宽度误差和轴颈圆度误差对涡流力矩的影响,以及轴颈的不同安装角度、偏心等因素对涡流力矩的影响。经对比验证,有限元计算结果与实测结果基本一致,研究结果对于气体静压轴颈—止推轴承的设计、装配优化和性能预测有重要指导意义。 相似文献
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S. M. Krimigis D. G. Mitchell D. C. Hamilton S. Livi J. Dandouras S. Jaskulek T. P. Armstrong J. D. Boldt A. F. Cheng G. Gloeckler J. R. Hayes K. C. Hsieh W.-H. Ip E. P. Keath E. Kirsch N. Krupp L. J. Lanzerotti R. Lundgren B. H. Mauk R. W. McEntire E. C. Roelof C. E. Schlemm B. E. Tossman B. Wilken D. J. Williams 《Space Science Reviews》2004,114(1-4):233-329
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. 相似文献