电离层对单频卫星导航系统伪距差分定位的影响

用计算机仿真方法 ,给出了单频卫星导航系统伪距差分后 ,定位误差受电离层影响的一些结果。伪距差分定位能够校正电离层时延误差 ,但校正精度随用户与基准站到同一颗卫星倾斜因子的不同而不同。为此 ,提出了一种改进的伪距差分方法。仿真结果表明 ,改进后有明显效果     

TD-SCDMA 中外环功率控制的研究

CDMA系统是干扰受限的系统,降低干扰可以提高系统的容量.TD-SCDMA系统的功率控制就是在保证用户的QoS前提下,降低发射功率,减少系统干扰从而增大系统的容量.本文介绍了TD-SCDMA中外环空率控制的算法,并且分析了功率控制参数对系统性能的影响.     

超短波电台自动检测与故障诊断系统设计

介绍了超短波电台自动检测系统与故障诊断系统的功能,并根据功能要求进行了硬件电路的设计,采取面向信号的ATLAS语言进行软件设计和建立在专家知识输入故障推理模型.该系统经使用证明,检测结果精确,检测效率较高.     

诱饵诱偏无人机截获系统的仿真分析

诱偏技术是电子对抗中自我保护的有效方法.在分析电扫恒差比幅测向原理的基础上,讨论了设置诱饵情况下无人机截获系统测向的误差;在射频仿真系统中,对诱饵、雷达与无人机的相对位置关系进行了研究,给出了算法,最后通过仿真对其进行了验证.这对电子对抗中武器系统诱偏技术的应用、射频仿真系统功能完善以及武器系统作战效能评估等研究都具有一定的参考价值.     

EUV and Radio Observations of an Equatorial Coronal Hole

An equatorial coronal hole has been observed on 18 and 19 October 1996 with SOHO-CDS and with the Nancąy Radioheliograph (RH). The CDS EUV line intensities are used to determine the coronal hole Differential Emission Measure (DEM); in turn this is used to compute the radio brightness temperature T_b at the observed frequencies, leaving the coronal electron temperature and density as free parameters. EUV line intensities, calculated from the derived models, show a good agreement with EUV observations. This revised version was published online in June 2006 with corrections to the Cover Date.     

基于DRFM技术的雷达标校器设计与实现

建立了基于数字射频存储器技术构建雷达标校器的方法.该雷达标校器可灵活实现目标运动模拟、多普勒频率加载、目标RCS模拟、多目标模拟等功能,较传统的基于光纤延迟实现的雷达标校器更具有应用价值.针对实际应用需求提出了解决频率捷变的方案,给出了典型模拟策略所需数学模型.应用研究表明,基于数字射频存储器技术的雷达标校器具有较强的...     

基于软件无线电的机会信号实时盲分离系统

在复杂的电磁环境中,往往存在多种频率交叠的机会信号,为利用机会信号进行定位增加了难度。针对这个问题,提出了一种基于软件无线电的机会信号实时盲分离系统。系统的硬件部分是在FPGA中实现等变自适应盲分离算法的,实现了AD采集后的复数域混合信号的分离。分离后的信号通过USB3.0数据线上传到上位机中进行存储、识别和实时显示。算法的FPGA实现采用流水线架构和浮点运算设计来提高信号的实时处理能力和数据计算精度。实测结果表明,该系统能够实时分离多路复数域混合机会信号。     

Variability of the upper troposphere and lower stratosphere observed with GPS radio occultation bending angles and temperatures

Recently, Lewis (2009) introduced a new method for the identification of tropopause heights (TPHs) from GPS radio occultation (RO) bending angles (α)$(\alpha )$. The method uses a covariance transform to identify transitions in a ln(α)$\mathit{ln}(\alpha )$ profile. Lewis validates the results with lapse rate tropopause (LRT) heights from one year of FORMOSAT-3/COSMIC data and radiosondes. In this study we apply the new method to the RO data sets from CHAMP/GRACE (2001–2009) and FORMOSAT-3/COSMIC (2006–2009). These results are the basis for TPH trend estimations for the time period between May 2001 and August 2009 (100 months) based on zonal monthly mean GPS RO data from CHAMP (2001–2008), GRACE (since 2006) and FORMOSAT-3/COSMIC (since 2006). Further, we compare the α$\alpha$ based TPH trends with LRT height trends and discuss the differences, which are largest in the subtropical regions (20°–40°) on both the northern and southern hemisphere. A global increase of the TPH between 5 and 9 m/yr is found for both methods and different data sets (CHAMP/GRACE alone and CHAMP/GRACE plus FORMOSAT-3/COSMIC). The results for the TPH trends are linked with bending angle and temperature trends in the upper troposphere and lower stratosphere region. Generally, an upper tropospheric warming (bending angle decrease) and a lower stratospheric cooling (bending angle increase) is noted.     

Solar energetic particle events during the rise phases of solar cycles 23 and 24

We present a comparative study of the properties of coronal mass ejections (CMEs) and flares associated with the solar energetic particle (SEP) events in the rising phases of solar cycles (SC) 23 (1996–1998) (22 events) and 24 (2009–2011) (20 events), which are associated with type II radio bursts. Based on the SEP intensity, we divided the events into three categories, i.e. weak (intensity < 1 pfu), minor (1 pfu < intensity < 10 pfu) and major (intensity ? 10 pfu) events. We used the GOES data for the minor and major SEP events and SOHO/ERNE data for the weak SEP event. We examine the correlation of SEP intensity with flare size and CME properties. We find that most of the major SEP events are associated with halo or partial halo CMEs originating close to the sun center and western-hemisphere. The fraction of halo CMEs in SC 24 is larger than the SC 23. For the minor SEP events one event in SC23 and one event in SC24 have widths < 120° and all other events are associated with halo or partial halo CMEs as in the case of major SEP events. In case of weak SEP events, majority (more than 60%) of events are associated with CME width < 120°. For both the SC the average CMEs speeds are similar. For major SEP events, average CME speeds are higher in comparison to minor and weak events. The SEP event intensity and GOES X-ray flare size are poorly correlated. During the rise phase of solar cycle 23 and 24, we find north–south asymmetry in the SEP event source locations: in cycle 23 most sources are located in the south, whereas during cycle 24 most sources are located in the north. This result is consistent with the asymmetry found with sunspot area and intense flares.     

月球轨道编队超长波天文观测微卫星任务

月球背面能够有效屏蔽来自地球并同时遮挡来自太阳的射电信号干扰,拥有太阳系中近乎最安静的电磁环境,是开展空间超长波天文观测的最佳选择区域。在立足完成空间干涉实验的基本任务目标基础、并力争实现重大科学发现的研究思路基础上,研制并发射两颗微卫星,搭载"嫦娥4号"任务进入地月转移轨道,自主完成地月转移、近月制动,在有效燃料约束下形成环月大椭圆轨道编队,构建环月超长波天文干涉仪。说明了系统的工作模式,对数据处理与科学分析方法进行了论述,包括数据预处理、干涉成像与全天功率谱获取角度,进而从支持服务模块和科学载荷模型两个方面对微卫星方案进行了简要概述,凝练了项目任务解决的关键科学与技术问题。月球轨道编队超长波天文观测微卫星的实施将通过全球首个绕月近距编队飞行系统,构建全球首个星–星干涉射电天文观测系统,进而打开人类认识宇宙的新窗口。