固体推进剂燃烧中凝相粒子的激光全息测试

概述了测试凝相粒子尺寸的基本方法，较详细地阐述了研究燃烧场凝相粒子尺寸分布的激光全息测量方法和测试结果。     

高分辨率星载聚束式SAR改进的ECS成像算法

提出一种适用于高星载聚束式合成孔径雷达（SAR）的改进Extended Chirp Scaling（ECS）算法。基于斜视距离等效模型，推导出改进的ECS算法，给出改进的方位Scaling因了以及算法的实现步骤。在斜视情况下改进的方法Scaling因子可以减小算法所需要的方位时间展宽，提高方位处理效率。为解决高分辨率星载聚束式SAR脉冲重复频率（PRF）过高等问题，在算法中结合了子孔径处理，并分析了采用子孔径处理的必要性及其实现方法。最后，通过计算机仿真，验证了算法的有效性。     

N2O-C2H2火焰原子吸收光谱法测定纯镍中硅含量

为简化纯镍中硅含量的测定过程,提高测量精度,研究了一种N2O-C2H2火焰原子吸收光谱法用于检测。介绍了方法的原理、工作参数和测定条件,并确定最佳工作条件,讨论了燃烧温度、共存离子等干扰因素的影响。实验结果表明,该法的灵敏度高、干扰小、选择性和重现性好,操作简单,分析周期短。其测定结果的相对标准偏差均小于1.0%,标准加入回收率大于97.0%(样本数n=6),可满足实验室仪器分析质量与控制的要求。     

画幅式层析成像光谱系统设计和实验研究

文章介绍一种无需时间或空间扫描的新型成像光谱仪—利用位相光栅作为分束器件的计算层析成像光谱仪 (CTIS)。重点介绍了各个系统的设计原则和位相光栅的设计 ,并给出了光栅的设计结果。详细介绍系统矩阵的实验定标方法和过程。叙述了自然光照明条件下真实物体组成的靶标的光谱成像实验 ,对目标实验采样的数据进行重构处理 ,给出了实验结果。     

几种新型的星载多光谱和成像光谱仪

近几年出现了几种新型的星载多光谱和成像光谱仪,例如:Landsat-7卫星的有效载荷增强型主题测绘仪+（ETM+）;EOS AM-1卫星的有效载荷多角度成像光谱仪（MISR）和先进空间热发射和反射辐射计（ASTER）;特殊探测器紫外成像光谱仪（SSUSI）。文章从结构、性能参数等方面综述了这几种星载成像光谱仪。     

稀疏孔径成像系统发展概况

介绍了稀疏孔径成像系统的发展现状。重点介绍了系统的成像原理和种类，国外的研究进展以及系统实现的关键技术和应用前景。     

成像光谱仪编程选择波段数据采集系统的研究

随着成像光谱仪的发展,遥感数据量越来越大,这对电子学系统中的数据采集、传输和处理带来了一定的困难。基于目前技术和数据的实用性两方面考虑,采用编程选择波段的方法能够很好地解决数据量日益增大的问题,国内外的一些方案中已经对此有了一定的设想,即通过遥控指令改变波段数目、光谱取样间隔或波段的重组,这一切都要求有一个灵活性强、通用性好的数据采集系统,能够对不同的选择情况正确地收集用户所需的数据。文中对数据采集的可行性进行了研究,并提出了一个较为容易实现的方案。     

中分辨率成像光谱仪焦平面设计方案设想

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。     

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.     

论在X射线探伤中曝光时间与管电压的关系

本文针对X射线探伤中曝光时间与管电压的关系以及曝光时间在探伤中的实际意义做了详尽分析，并提出了对于不同厚度的零件如何选择曝光时间的原则。