结合小波变换的Jacquin分形图像编码

提出了一种将分形与小波变换紧密结合起来的图像压缩方法;改进了目前虽简单易行,但编码时间过长的分形图像编码,而且Domain块的采样方式也存在缺陷。针对这些问题,利用小波分解的特性构造了一种基于小波分解的分形图像编码算法;对输入图像进行小波变换,将变换后的低频部分作为Jacquin分形编码方法的搜索区域。实验表明重构图像的质量得到了较大的提高。     

利用栅网控制空间等离子体环境效应模拟中的等离子体参数

通常采用ECR等离子体源产生的等离子体的温度和密度都比较大，通过附加适当目数的栅网，并在栅网上加一定的偏置电位来对等离子体参数，尤其是温度，密度进行调整，满足空间等离子体环境模拟要求，本文利用14目，25目的栅网，对已有的地面实验室空间等离子体环境进行了改进，得到了更加接近空间等离子体参数的一个地面模拟环境。     

空间站废水的处理及管理

长期载入飞行的空间站需要大量的用水，为解决由此引起的巨大的维持飞行的运行费用，需要实现水的再生与闭路循环，如何针对空间站废水的特征，解决废水的处理与利用问题，并建立合理的水循环体系是这一工作的关键，文中分析，比较了空间站废水的处理方法，设计了空间站水管理整合方案，并多方面探讨和验证这一方案的合理性和可行性。     

光波纳米推进技术中的表面等离激元增益光镊作用机理

为研究天线不同结构对表面等离激元（SPP）增益光镊作用的影响,建立天线-基底的电磁波传输耦合激元电场触发光梯度力的数值模型,并利用数值模型分析天线不同结构对SPP电场的影响规律,同时,这种电场变化规律对光镊增益有直接的数学关系,基于上述物理机制,获得不同天线结构对光梯度力产生的优化策略。为验证上述物理机制与优化策略的有效性,开展纳米颗粒的粒子图像测速（PIV）试验,天线材料为银,基底为二氧化硅,纳米颗粒为银,试验能够完好地观测到纳米颗粒在天线通道的运动情况。结果表明,光梯度力的增益机制在于激元电场强度和梯度两方面因素,前者随天线不对称性增强而先增大后减小,后者呈现一直增大趋势;纳米颗粒推动作用力的计算误差约为5.5%~13.8%,且试验值与计算值的趋势相符,一方面验证本文研究机理及优化策略的有效性,另一方面证明PFP技术的原理可行。     

Interplanetary shocks and sudden impulses during solar maximum (2000) and solar minimum (1995–1996)

In this work a study is performed on the correlation between fast forward interplanetary shock parameters at 1 Astronomical Unit and sudden impulse (SI) amplitudes in the H-component of the geomagnetic field, for periods of solar activity maximum (year 2000) and minimum (year 1995–1996). Solar wind temperature, density and speed, and total magnetic field, were taken to calculate the static pressures (thermal and magnetic) both in the upstream and downstream sides of the shocks. The variations of the solar wind parameters and pressures were then correlated with SI amplitudes. The solar wind speed variations presented good correlations with sudden impulses, with correlation coefficients larger than 0.70 both in solar maximum and solar minimum, whereas the solar wind density presented very low correlation. The parameter better correlated with SI was the square root dynamic pressure variation, showing a larger correlation during solar maximum (r = 0.82) than during solar minimum (r = 0.77). The correlations of SI with square root thermal and magnetic pressure were smaller than with the dynamic pressure, but they also present a good correlation, with r > 0.70 during both solar maximum and minimum. Multiple linear correlation analysis of SI in terms of the three pressure terms have shown that 78% and 85% of the variance in SI during solar maximum and minimum, respectively, are explained by the three pressure variations. Average sudden impulse amplitude was 25 nT during solar maximum and 21 nT during solar minimum, while average square root dynamic pressure variation is 1.20 and 0.86 nPa^1/2 during solar maximum and minimum, respectively. Thus on average, fast forward interplanetary shocks are 33% stronger during solar maximum than during solar minimum, and the magnetospheric SI response has amplitude 20% higher during solar maximum than during solar minimum. A comparison with theoretical predictions (Tsyganenko’s model corrected by Earth’s induced currents) of the coefficient of sudden impulse change with solar wind dynamic pressure variation showed excellent agreement, with values around 17 nT/nPa^1/2.     

Research on a complex CME event including Hα, LASCO, radio and MDI observations

We present our research on a fast and decelerating partial halo coronal mass ejection (CME) event detected in multi-wavelengths in the chromosphere and the corona on 14 October, 1999. The event involved a whole complex active area which spanned more than 40° of heliolongitude. It included a strong solar flare (XI/1N) and a complex eruptive filament within an active region of the entire complex. Especially, several radio sources were detected in the decimetric range prior to the CME by the Nançay Radioheliograph (NRH). A linear force-free field extrapolation of the Michelson Doppler Imager (MDI) magnetogram was performed to calculate the magnetic topology of the complex prior to the triggering of the event. The presence of a coronal null point combined with the occurrence of two distant and nearly simultaneous radio sources put strong arguments in favor of the generalized breakout model for the triggering of the eruption. The analysis of the subsequent development of the event suggests that large interconnecting loops were ejected together with the CME.     

基于GPS遥感的延迟映射接收机关键技术

全球卫星定位系统GPS(Global Positioning System)广泛应用于定位和导航,还可利用海面对GPS信号产生的散射效应进行微波遥感,是一种新型微波遥感手段.首先介绍了GPS海洋遥感测风技术产生背景及特点,给出了GPS散射信号测量技术理论基础,重点分析了延迟映射接收机设计中提高采样信号信噪比、双射频前端电路设计、计算反射点延迟、接收机工作模式、内嵌软件处理等5项关键技术.设计的延迟映射接收机样机在天津近海完成了首次搭载飞行试验,试验结果表明,延迟映射接收机可同时接收直射和海面散射卫星信号并输出导航定位解,正确计算镜面散射点码延迟,准确接收海面散射的GPS卫星信号,且散射信号信噪比达到了14.9 dB以上,接收机输出为反演海面风场提供了准确的基础数据,这种方式可推广到遥感探测陆地土壤湿度、海冰厚度、海浪高度等领域.      

基于模式特征的图像压缩算法

从人眼视觉特征与空域模式特征的角度出发,提出了一种基于模式特征的图像压缩算法。经过对一组遥感图像的对比试验,可以看出本算法在对纹理信息丰富的遥感图像进行压缩时明显优于SPIHT算法。     

基于DEM的星载SAR图像模拟以及用于图像精校正

根据星载SAR的距离-多普勒成像原理对DEM的三维位置点进行成像几何位置的计算,然后根据经验公式给出了雷达后向散射系数的模拟方法。针对DEM格网间隔和SAR图像分辨率的不同,以及由于侧视成像雷达的特点而导致山区的迎坡和背坡模拟图像点密度不均匀等问题,采用了基于DEM格网点内插的算法。最后应用模拟的SAR图像和真实图像匹配来实现星载SAR图像的几何精校正处理。通过采用RADARSAT的实际图像进行了图像的模拟和几何校正,证明了方法的可行性。     

一种基于窄带雷达的低轨空间目标识别方法

通过分析低轨空间目标的姿态运动对窄带回波脉冲数据的调制,表明低轨空间目标窄带回波脉冲数据信号的相位比幅度包含了更多的目标特征信息。采用小波分析从实测窄带相参回波特性数据的相位中,估计低轨空间目标的整体运动趋势,判别低轨空间目标的粗略类型,并通过大量实测数据的实验结果验证了该方法判别低轨空间目标粗略类型的有效性。