圆极化天线旋向的差错问题

以实例说明了左右圆极化天线经常发生旋向差错的原因 ;论述了圆极化波和天线的基本概念和定义 ;为防止在今后卫星工程和协调中再出现类似差错 ,建议采取两项技术措施 ,可确保星 -地圆极化天线旋向的匹配 ,避免对卫星系统工作造成重大损失     

SMESE: A SMall Explorer for Solar Eruptions

The SMall Explorer for Solar Eruptions (SMESE) mission is a microsatellite proposed by France and China. The payload of SMESE consists of three packages: LYOT (a Lyman imager and a Lyman coronagraph), DESIR (an Infra-Red Telescope working at 35–80 and 100–250 μm), and HEBS (a High-Energy Burst Spectrometer working in X- and γ-rays).

The status of research on flares and coronal mass ejections is briefly reviewed in the context of on-going missions such as SOHO, TRACE and RHESSI. The scientific objectives and the profile of the mission are described. With a launch around 2012–2013, SMESE will provide a unique tool for detecting and understanding eruptions (flares and coronal mass ejections) close to the maximum phase of activity.     

Ka波段高增益圆极化机载微带天线阵的设计与实现

设计、分析、制作了一种工作在Ka波段的4单元高增益、圆极化机载微带天线阵列。利用顺序旋转阵列和串并馈方式的微带线网络馈电,显著改善了天线的轴比带宽和驻波带宽,减少了馈线损耗,实现了高增益。采用L型微带调配枝节对贴片单元进行匹配,便于组阵,解决了阵列空间布局不合理的难题;馈电网络和天线单元集成在同一介质基板上,易于加工和制作。测试结果表明:该天线阵具有高增益和良好的圆极化特性,从而证实了该方法的正确性和实用性。本文所设计的天线由于具有体积小、质量轻、结构紧凑、易于集成等优点,在机载相控阵雷达以及卫星通信系统中具有很好的应用前景。     

基于RGB亮度分级的图像预处理研究

利用一种基于RGB亮度分级的图像预处理方法,在源图像的R、G、B三个分量上对图像进行亮度分级合并,以减少自然场景图像的颜色数目,在不破坏源图像结构的前提下降低图像的复杂度,同时又保证了较好的通用性。     

光源光谱对干涉式光纤陀螺零漂的影响

以采用Y波导集成光学调制器的保偏型干涉式光纤陀螺(IFOG,Interference Fiber Optic Gyroscopes)为研究对象,根据各光学元器件的参数,建立了各器件的琼斯矩阵以及光路传输模型,在此基础上进行了光路偏振误差的理论分析.通过推导,得到了保偏型干涉式光纤陀螺的偏振误差表达式.首次借助光源偏振度的改变,分析了不同形状的光源光谱对偏振模式耦合误差引起的陀螺零漂的影响.通过计算得出,当光源的偏振度在0~3%之间呈线性变化以及光路中其它参数不变时,谱宽较窄的光谱引起的零漂较大,谱宽较宽的光谱引起的零漂较小.仿真结果给光纤陀螺光源光谱的选择提供了理论依据.      

冕洞区SiⅡ辐射线源区的相关高度

SiⅡ辐射线源区的高度表征了太阳大气过渡区的底层高度．通过对超紫外线的辐射强度结构和无力场外推所得的三维磁场结构作相关分析来求相关高度是一种研究超紫外辐射线源区高度的新方法．有研究发现,该方法得到的冕洞区SiⅡ辐射线源区的高度比传统观点所认为的高．由于目前运用该方法的数据分析有限,需要用更多的数据进一步验证这一结果．运用该方法分析了SOHO/SUMER观测到的位于太阳南极冕洞之下的日面区域SiⅡ辐射线数据和美国National Solar Observatory/Kitt Peak(NSO/KP)测量的磁场数据,得到冕洞区SiⅡ辐射线源区的相关高度约为5．0Mm．该结果支持了冕洞区的过渡区底层高度比宁静区的要高的结论．同时发现了新的现象,并对其原因进行推测．     

Particle Acceleration at Interplanetary Shocks

This paper briefly reviews proton acceleration at interplanetary shocks. This is key to describing the acceleration of heavy ions at interplanetary shocks because wave excitation—and hence particle scattering—at oblique shocks is controlled by the protons and not the heavy ions. Heavy ions behave as test particles, and their acceleration characteristics are controlled by the properties of proton-excited turbulence. As a result, the resonance condition for heavy ions introduces distinctly different signatures in abundance, spectra, and intensity profiles, depending on ion mass and charge. Self-consistent models of heavy-ion acceleration and the resulting fractionation are discussed. This includes discussion of the injection problem and the acceleration characteristics of quasi-parallel and quasi-perpendicular shocks.     

ICME期间磁暴的太阳风参数和极光沉降能量

基于1995-2004年ICME驱动的强烈磁暴(SA型)、强磁暴(SB型)和延迟型主相暴(SC型)三种磁暴类型,对1AU处太阳风动压、太阳风速度、行星际磁场、EK-L电场以及极光沉降能量进行时序叠加分析,并分别与-vBz耦合函数和Newell耦合函数进行对比.结果表明,三种磁暴在ICME到达前期的太阳风动压较稳定,背景太阳风、极光沉降能量、行星际磁场和磁层存在相对平静期. ICME到达前期SA型磁暴的背景太阳风速度、行星际磁场南向分量以及极光沉降能量的均值高于另外两种磁暴类型,这说明大型日冕物质抛射在ICME到达前就对行星际磁场、背景太阳风和HP产生了影响.磁暴急始后,SC型磁暴的EK-L电场斜率小,峰值延后且行星际磁场北向分量增强,这些都是磁暴主相延迟的表现,极光沉降能量随着行星际磁场转为南向而增加.     

频率选择表面(FSS)在天线隐身技术中的应用

本文简要叙述了飞行器隐身技术中通常采用的三种方法。飞行器采取上述隐身技术措施后,机载雷达天线对电磁波的散射成为飞行器的主要散射源。因此,天线隐身技术的研究就显得十分重要。本文介绍的频率选择表面(FSS)是一种由无源谐振单元,按一定排列方式组成的准二维平面周期结构,利用其对电磁波具有频率及极化的双重滤波的概念,以达到降低天线雷达截面积(RCS)的效果。文中用谱域分析法对十字形振子阵FSS的特性进行了分析计算,并应用于天线罩或低RCS反射面天线中。对已加工出的面积为42×42cm~2,在聚四氟乙烯玻璃纤维布上的十字形振子阵FSS样品进行了性能测试,从测试曲线看出方法是有效的。     

Coronal mass ejections in the heliosphere

With the advent of the NASA STEREO mission, we are in a position to perform unique investigations of the evolution of coronal mass ejections (CMEs) as they propagate through the heliosphere, and thus can investigate the relationship between CMEs and their interplanetary counterparts, so-called interplanetary CMEs (ICMEs). ICME studies have been principally limited to single-point, in-situ observations; interpretation of the in-situ characteristics of ICMEs has been used to derive a range of ICME properties which we can now confirm or refute using the STEREO imaging data. This paper is a review of early STEREO CME observations and how they relate to our currently understanding of ICMEs based on in-situ observations. In that sense, it is a first glance at the applications of the new data-sets to this topic and provides pointers to more detailed analyses. We find good agreement with in-situ-based interpretations, but this in turn leads to an anomaly regarding the final stages of a CME event that we investigate briefly to identify directions for future study.