调频连续波SAR改进的频率尺度变换算法(英文)

本文提出了一种调频连续波SAR改进的频率尺度变换算法。调频连续波SAR在运动过程中持续不断地发射和接收信号,这种运动导致了回波信号的伸缩,对波前重建产生了严重的影响。推导了回波信号模型,给出了信号的距离-多普勒域表达式,分析了由于天线不断运动而导致的相位变化与方位向频率之间的关系。改进的频率尺度变换算法补偿了这种相位变化,实现了目标的精确成像,仿真结果表明了分析的正确性和算法的有效性。     

基于多尺度 3D-2D卷积神经网络的高光谱图像分类

设计提出了 1种针对高光谱图像分类任务的 3D-MSCNN模型。在 PCA降维的基础上,利用 3D空谱特征提 取网络和 2D多尺度特征提取网络实现高光谱图像特征提取,充分发挥高光谱图像空谱信息价值,增强对不同尺度 地表覆盖的表达能力。最后,利用 Softmax分类损失函数实现高光谱图像分类任务。实验结果表明,本文算法在 In. dian Pines和 Pavia University数据集上都取得了较好的分类效果。与 CD-CNN、3D-CNN、SS-Net和 HybirdSN等方法相 比,本文算法能够有效提升总体精度、平均精度和 Kappa系数等客观评价指标。     

角分集ISAR高分辨成像

对不同视角雷达回波进行融合可以形成大的相干积累角,显著增强雷达空间监控能力。给出一种角分集(制)信号融合成像方法,对于角分集(制)回波方位向存在大的间隔,首先将每一距离单元方位向有效稀疏孔径数据排列组合成一Hankel矩阵,由参数化方法估计一维信号参数,再由估计得到的参数对空缺部分预测填补,对每个距离单元横向补全后,压缩得到二维图像。该方法克服了以往预测方法的不足,能有效用于方位向稀疏孔径预测外推,最终仿真与实际数据处理结果证实结论。     

低轨卫星面阵凝视成像技术研究

文章介绍了面阵凝视成像的工作原理及特点，阐述了低轨卫星对地观测凝视成像面临的像移问题及其解决措施，对像移补偿装置与二维指向机构的结合做了初步探讨。     

机载聚束式SAR天线波束指向控制分析

建立波束控制条件下的机载聚束式SAR的天线指向及成像数学模型,证实天线波束指向被控造成回波信号的幅度调制,引起成对回波,从而影响成像质量。此外,分析波束指向控制比率与测绘带方位宽度、图像动态范围的制约关系,提出设计机载聚束式SAR天线波束指向控制比率的基本原则。最后,通过计算机仿真,验证理论分析的正确性。     

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。     

彩色三维激光快速成型技术的研究

目前逆向工程采用线结构激光和一个彩色面阵CCD摄像机构成三维彩色扫描系统,彩色CCD摄像机分两次对被测物体成像,首先摄取物体的彩色图片,然后加用滤光片再摄取激光光平面上的三维信息.最后将两次获取的信息重叠,便可得到三维彩色信息.提出了激光光平面方程式三维测量方法,建立了相应的数学模型.研制成一套适用于彩色逆向工程流程,并进行了实验研究,给出了实验结果.     

调频连续波SAR成像算法研究

机载遥感微波成像雷达在地球观测特别是在城市应用中起着非常重要的作用,现在人们对体积小、重量轻、成本效益高、分辨率高的成像雷达越来越关注。调频连续波(FM-CW)技术和SAR相结合的调频连续波合成孔径雷达应运而生。论文详细分析了FM-CW SAR的成像过程,提出了去除相位残余的算法,并给出仿真结果。通过仿真可以看出,调频连续波合成孔径雷达具有较好的空间分辨力。     

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.     

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。