基于特征点运动矢量估计的动态序列图像运动目标跟踪

提出了一种改进的特征点运动矢量估计方法,用于动态序列图像中的运动目标跟踪。首先利用改进的最小亮度变化算法提取特征点;然后通过自适应的十字模式搜索法确定这些特征点的匹配点。在RANSAC方法的基础上,利用运动背景的仿射变换参数实现运动背景的补偿。最后利用合理的形态滤波技术,运动目标将完整地从背景中提取出来并实现准确跟踪。实验结果表明,改进的方法可以成功完成运动背景的补偿,并为动态序列图像的运动目标跟踪提供了保证。     

旋转惯导系统中的圆锥误差分析及其补偿

圆锥误差是由转动不可交换性误差引起的,存在于惯导系统导航解算的一种误差形式。由于基于旋转调制方式的惯导系统运动模式与传统捷联惯导系统不同,因此圆锥误差的表现形式也会发生相应变化。首先建立了旋转调制惯导系统的圆锥运动模型,对其不可交换性误差进行了推导。在此基础上分析了基于等效旋转矢量的多子样算法在旋转惯导系统圆锥误差补偿中的应用效果以及旋转方案对圆锥误差补偿的影响,最终通过仿真对理论分析进行了验证。仿真结果表明,圆锥误差对于旋转惯导系统的影响要大于传统惯导系统,但可以通过改变旋转方式来对圆锥误差进行抑制。     

压缩逆合成孔径雷达中的相位自聚焦算法(英文)

与常规逆合成孔径雷达(Inverse syntheticaperture radar,ISAR)相同,压缩ISAR也需要进行基于回波信号的运动补偿,其中包括距离对准和相位补偿。本文提出了一种适用于压缩ISAR成像处理的相位自聚焦算法。该算法采用特征向量法解决稀疏ISAR信号的相位补偿问题。试验结果证明了该算法的有效性。     

基于PSPICE高温度稳定性基准电压源的设计

Psp ice是一个功能强大的模拟电路系统设计和分析的EDA工具。用此工具可方便精确地分析计算基准电压源设计中的温度特性及电源电压抑制比等参数,大大提高设计效率。温度曲率补偿型CMOS带隙基准电压源电路采用了有效的曲率补偿技术,温度稳定性高,结构简单。     

惯性仪表误差补偿技术在提高战略导弹精度中的应用

本文对有关战略导弹惯性仪表主要误差源的分类及对精度的影响；惯性仪表误差补偿的各种方法及其优缺点等内容作了介绍，对美国洲际导弹误差补偿方法也作了介绍，最后对惯性仪表误差的几种补偿方案作了分析。     

基于液晶偏转系统的卫星平台振动补偿方法研究

针对卫星平台振动严重影响空间光通信跟瞄精度的问题,提出了基于液晶偏转控制系统的扰动补偿方案。建立了液晶偏转控制系统的数学模型,为了提高收敛速度,设计了基于后验估计误差RLS格型滤波算法的自适应控制器。引入了变阶算法,不但实现了快速、高精度的扰动补偿,而且在没有增加计算量的情况下,消除了高定阶RLS自适应算法中大的暂态响应,改善了控制系统性能。实验结果表明补偿后的扰动残差在10-6rad量级,验证了该控制方案的有效性和可行性。     

矢量信号调制质量分析方法研究与实现

采用矢量信号分析技术通过分析已调信号的特性，能够快速发现引起信号失真的原因，定位系统设计中的错误，该技术在信号分析仪器、数字通信等领域应用广泛。本文在深入研究矢量分析技术的基础上，建立了矢量信号分析模型，并对矢量信号分析中对结果影响较大的最佳判决未知和幅相补偿模块进行了详细分析。利用软件实现了矢量信号调制质量分析，能够快速的对EVM等指标进行计算，且易于嵌入其它系统和设备，使用方便。     

舰载机着舰舰面效应及其补偿方法研究

根据舰面效应的作用机理,分析了舰面效应对舰载机着舰的影响,总结了舰载机在不同着舰模式下的舰面效应补偿方法.针对舰载机自动着舰模式,通过分析舰面效应所产生的附加升力造成的着舰偏差,提出了引导信号指令修正的舰面效应补偿方法,并给出了舰面效应自动补偿方法的具体流程,分析了自动补偿方法的特性及其应用面临的关键问题.     

Ionospheric responses to the 21 August 2017 great American solar eclipse – A multi-instrument study

Herein, we report on the ionospheric responses to a total solar eclipse that occurred on 21 August 2017 over the US region. Ground-based GPS total electron content (TEC) data along with ground-based measurements (Millstone Hill Observatory (MHO) and digital ionosondes) and space-based measurements (COSMIC radio occultation (RO) technique) allowed us to identify eclipse-associated ionospheric responses. TEC data at ~20°, ~30°, and ~40°N latitudes from the west to east longitudes show not only considerable depression but also wave-like characteristics in TEC both in the path of totality and away from it, exclusively on the day of eclipse. Interestingly, the observed depressions are associated with lesser (higher) magnitudes at stations over which the solar obscuration percentage was meager (significant), a clear indication of bow-wave-like features. The MHO observes a 30% reduction in F₂-layer electron densities between 180 and 220 km on eclipse day. Ionosonde-scaled parameters over Boulder (40.4°N, 100°E) and Austin (30.4°N, 94.4°E) show a significant decrease in critical frequencies while an altitude elevation is seen in the virtual heights of the F-layer only during the eclipse day and that decreases are associated with wave-like signatures, which could be attributed to eclipse-generated waves. The estimated vertical electron density profile from the COSMIC RO-based technique shows a maximum depletion of 40%. Relatively intense and moderate depths of TEC depression, considerable reductions in the F₂-layer electron densities measured by the MHO and COSMIC RO-measured densities at the F₂-layer peak, and elevations in virtual heights and reduction in the critical frequencies measured by ionosondes during the eclipse day could be due to the eclipse-induced dynamical effects such as gravity waves (GWs) and their associated electro-dynamical effects (modification of ionospheric electric fields due to GWs).     

Gravity field models from kinematic orbits of CHAMP,GRACE and GOCE satellites

The aim of our work is to generate Earth’s gravity field models from GPS positions of low Earth orbiters. Our inversion method is based on Newton’s second law, which relates the observed acceleration of the satellite with forces acting on it. The observed acceleration is obtained as numerical second derivative of kinematic positions. Observation equations are formulated using the gradient of the spherical harmonic expansion of the geopotential. Other forces are either modelled (lunisolar perturbations, tides) or provided by onboard measurements (nongravitational perturbations). From this linear regression model the geopotential harmonic coefficients are obtained.