单星-星光制导方案

从原理上论述星跟踪器捷联安装的单星－星光制导原理，推导利用星光信息来修正导弹团初始定位定向误差引起落点偏差的数据处理方法、公式，对两种主要的误差源进行了数学仿真计算，结合仿真试验分析了单星方案的可行性。     

一种新的导航星选取算法研究

在导航星表的建立过程中，由于恒星的数量太多，往往要进行筛选，通常这种选择复杂费时，而结果往往并不是最优的。本文引入了动态星等阈值分布函数，将传统星等阈值过滤算法中的静态阈值用动态星等阈值代替，建立了一种新的动态星等阈值过滤选择模式。而基于统计学习理论的支持向量机方法为求解高维非线性动态星等阈值分布函数提供了新的途径。本文讨论了这种基于支持向量机的导航星自动选择算法——回归选取算法。实验表明，用该算法所选取的导航星表，导航星数量少、分布均匀性好。同时它还能适应多种任务的导航星选取要求，具有很强的通用性。     

捷联星光制导仿真方法研究

捷联星光制导方案是把星跟踪器安装在平台基座上，利用星跟踪器和平台框架角的测量信息解算出因初始定位定向误差引起导弹的落点偏差，由末助推控制系统完成弹道修正。有关捷联星光制导方案的地面仿真原理、方法、组成，选星及大气修正计算原则、地球旋转影响在本文中作了论述，并给出仿真原理框图、硬件设备组成和功能、接口要求以及系统工作程序框图。     

Modeling Pulsar Wind Nebulae

In the last few years, new observations by CHANDRA and XMM have shown that Pulsar Wind Nebulae present complex but similar inner features, with the presence of axisymmetric rings and jets, which are generally referred to as a jet-torus structure. Due to the rapid growth in accuracy and robustness of numerical schemes for relativistic fluid-dynamics, it is now possible to model the flow and magnetic structure of the relativistic plasma responsible for the emission. Recent results have clarified how the jet and rings are formed, suggesting that the morphology is strongly related to the wind properties, so that, in principle, it is possible to infer the conditions in the unshocked wind from the nebular emission. I will review here the current status in the modeling of Pulsar Wind Nebulae, and, in particular, how numerical simulations have increased our understanding of the flow structure, observed emission, polarization and spectral properties. I will also point to possible future developments of the present models.     

星孔装药燃面退移图象显示中的特殊问题

介绍了采用双三次均匀B样条曲面法构造星孔装药燃面退移图象中，夹直纹面的曲面；具有脊线曲面的反算拟合；燃面拟合的边界条件及曲面加密网格的求解等特殊问题。     

药柱通用坐标计算法计算结果跳动的原因分析及解决途径

对药柱通用坐标计算法计算结果跳动的原因进行了分析,提出了解决途径和方法,并对提高计算准确度的问题也进行了讨论。经实例计算证明解决途径和方法是有效的,与解析法计算结果比较误差不大于0.85％。     

捷联惯导/星敏感器组合系统的在轨自标定方法研究

研究了捷联惯导/星敏感器组合系统中对陀螺仪和星敏感器进行在轨自标定的方法。分析捷联惯导系统和星敏感器的误差源,对陀螺仪随机漂移和星敏感器安装误差进行建模并列入系统状态,建立系统状态方程;利用捷联惯导输出的载体位置、姿态与星敏感器输出的姿态矩阵来构造量测,建立量测方程。设计卡尔曼滤波算法,经过滤波计算获得陀螺仪随机常值漂移和星敏感器安装误差的估计值,从而实现组合系统的在轨自标定。仿真结果表明,基于卡尔曼滤波的在轨自标定方法能够标定出85%以上的陀螺仪随机常值漂移和95%以上的星敏感器安装误差。     

一个基于CMOS器件的新型嵌入式星敏感器设计

CMOS图像敏感器应用于星敏感器设计是当前国内外研究的热点。本文采用CMOS图像敏感器STAR2 5 0结合当前先进的ARM (RISC)技术 ,设计了具有自主性的轻型嵌入式星敏感器 ,具有抗辐射、体积小、质量轻、低功耗、可靠性高等特点     

星敏感器用典型CCD探测器电离总剂量效应研究

用自建的工程单机对星敏感器用核心器件CCD的电离总剂量效应进行了研究,给出了不同辐照剂量下辐照前后图像灰度、标准差等反映CCD拍摄图像质量的参数变化。研究表明：CCD对电离总剂量效应较敏感,辐照会引起输出图像灰度和标准差变大,导致图像质量下降、信噪比降低,最终影响探测器的成像效果。     

Systematic centroid error compensation for the simple Gaussian PSF in an electronic star map simulator

Simulated star maps serve as convenient inputs for the test of a star sensor, whose standardability mostly depends on the centroid precision of the simulated star image, so it is necessary to accomplish systematic error compensation for the simple Gaussian PSF（or SPSF, in which PSF denotes point spread function）. Firstly, the error mechanism of the SPSF is described, the reason of centroid deviations of the simulated star images based on SPSF lies in the unreasonable sampling positions（the centers of the covered pixels） of the Gaussian probability density function. Then in reference to the IPSF simulated star image spots regarded as ideal ones, and by means of normalization and numerical fitting, the pixel center offset function expressions are got, so the systematic centroid error compensation can be executed simply by substituting the pixel central position with the offset position in the SPSF. Finally, the centroid precision tests are conducted for the three big error cases of Gaussian radius r = 0.5, 0.6, 0.671 pixel, and the centroid accuracy with the compensated SPSF（when r = 0.5） is improved to 2.83 times that of the primitive SPSF, reaching a 0.008 pixel error, an equivalent level of the IPSF. Besides its simplicity, the compensated SPSF further increases both the shape similarity and the centroid precision of simulated star images, which helps to improve the image quality and the standardability of the outputs of an electronic star map simulator（ESS）.