射电测量卫星及其应用

射电测量卫星，是一种深空探测的有效设备。本文综述了射电测量卫星的新近发展，并对我国如何研发射电测量卫星提出了建议。     

国外空间目标探测与识别系统发展现状研究

介绍了美国、俄罗斯、欧洲的空间目标探测与识别系统发展现状,例如美国地基新型S频段空间篱笆雷达和利用轨道优势进行探测识别的作战响应空间-5(ORS-5)卫星,俄罗斯具有空间目标识别能力的新型高频沃罗涅日(Voronezh)雷达、雷达光学结合探测识别的树冠(Krona)系统,ESA空间碎片望远镜及德国试验监视与跟踪雷达(GESTRA)等。总结分析了国外空间目标探测与识别系统的发展趋势,例如正在发展高频雷达和大口径大面阵光学探测识别设备,建立天基、地基互补探测识别系统,研究雷达与激光、光学相结合的探测识别技术等,可为我国发展空间目标探测与识别系统提供参考。     

天基毫米波空间碎片观测雷达系统分析与设计

介绍了天基毫米波空间碎片观测雷达的难点和关键技术,提出了解决问题的思路。将同时多波束天线引入到高速目标探测中,分析了雷达天线和发射机的形式,采用多频信号处理方法解决多普勒模糊问题。给出了空间站载天基毫米波雷达的系统参数,分析了测距、测角、测速精度。在天球坐标系下建立了雷达平台坐标系,通过速度分解和坐标转换,结合雷达成像的方法分析了雷达和碎片间的相对速度、位置的几何关系,在此基础上对空间站载天基毫米波雷达系统空间碎片轨道预测性能进行了分析。
     

频率分集雷达高灵敏度目标探测技术

本文针对空间非合作目标高灵敏度探测问题,对频率分集抗角闪烁效应进行了试验研究,并在此基础上提出了一种基于分集雷达的高灵敏度目标探测方法,该方法利用高分辨信号的相关性提高检测信噪比,仿真结果表明该方法能有效提升空间非合作目标的高灵敏度探测能力。     

利用“天籁”暗能量观测阵列开展空间目标探测新技术试验

提出一种用于开展空间目标探测的大视场、多波束射电观测手段。通过柱形天线阵列,在特定方向获得大张角均匀巡天视场,实现对大空域范围的连续监视;基于综合孔径天图成像,实现对批量空间目标的实时捕获;利用小口径碟形天线之间的优化干涉组合,通过数字波束合成实现多目标精确跟踪测量。配合软件去噪与阵列定标校准手段,进一步提高微弱目标信号提取认证能力,降低系统功率与增益要求。提出利用具有相似阵列结构的"天籁"暗能量观测系统开展关键技术试验,以缩短研究周期、减少科研成本。从作用距离、信号特征、探测时间等方面对试验可行性进行了分析,结果表明"天籁"阵列具备支撑相关新技术试验的能力。     

天基雷达观测空问碎片的研究现状及关键技术分析

文章针对空间碎片观测中尚未得到确切观测数据的危险碎片的观测需求，综合分析了国内外的研究水平和现状，对天基雷达观测的需求和关键技术开展研究，提出了天基空间碎片观测有三个关键技术需要解决，即如何确定雷达工作体制和平台轨道以提高观测效率，如何有效探测尺度只有几个毫米-几个厘米的细小目标，如何对观测到的空间碎片进行分类和精确定轨。     

多功能相控阵雷达目标监视与气象探测兼容模式设计

对多功能相控阵雷达目标监视与气象探测兼容模式设计进行了研究。针对多功能相控阵低空监视雷达集成气象探测功能的需求,从系统工作兼容性角度出发介绍了一种雷达工作模式折中设计方法。该方法解决了目标监视和气象探测在数据率、波形设计、波束驻留时间分配等的矛盾,实现两种功能的兼容。此外,还对该兼容模式的工程实现进行了探讨。     

天基雷达观测空间碎片的研究现状及关键技术分析

文章针对空间碎片观测中尚未得到确切观测数据的危险碎片的观测需求,综合分析了国内外的研究水平和现状,对天基雷达观测的需求和关键技术开展研究,提出了天基空间碎片观测有三个关键技术需要解决,即如何确定雷达工作体制和平台轨道以提高观测效率,如何有效探测尺度只有几个毫米-几个厘米的细小目标,如何对观测到的空间碎片进行分类和精确定轨。     

天基TDM-MIMO雷达空间碎片阵列走动补偿方法研究

天基时分复用多发多收天线(TDM-MIMO)雷达能同时完成较大空域搜索和多目标跟踪任务,有利于实现对多个碎片同时跟踪,且系统架构简单,能够以较小代价获得更多的系统自由度.但由于空间碎片与雷达间的相对高速运动,目标回波信号由窄带阵列信号变成宽带阵列信号,均匀线阵畸变成相对阶梯形阵列,无法实现能量聚焦.为了解决以上问题,提...     

空间目标可见光相机探测能力理论计算方法研究

空间目标可见光相机的探测能力主要与相机自身收集目标信号的能力、相机本身的背景噪声以及探测器组件的噪声水平有关。衡量空间目标可见光相机探测能力的主要技术指标是信噪比。在国内外相关资料比较缺乏的情况下，文章通过原理研究和理论推导，得到了空间目标可见光相机探测能力理论计算公式，并用实例进行了例证，表明该方法正确可取，为空间目标可见光相机设计时对探测能力的分析和预估提供了理论计算方法。     

地基激光测距系统观测空间碎片进展

卫星激光测距作为地基光电望远镜系统重要技术应用,可直接精确测量空间碎片距离,提升碎片目标轨道监测精度。基于上海天文台60 cm口径激光测距望远镜,应用百赫兹重复率高功率激光器、高效率激光信号探测系统等,建立了空间碎片激光测距系统,实现了对距离500~2600 km、截面积0.3~20 m2的碎片目标观测,测距精度优于1 m,具备了碎片目标常规测量与应用能力。此外,开展了空间目标白天监视技术研究,实现了亮于6星等恒星的白天观测,并进行了望远镜局部指向误差模型分析,分析结果可应用于空间碎片白天激光观测的目标监视与引导。     

A space based radar on a micro-satellite for in-situ detection of small orbital debris

The increase in the number of satellites in the Near Earth Orbit is exponential. The consequent increase in pollution of the orbital environment is of growing concern to the international community. There are currently only two observation systems available for measurement of orbital debris. Ground based radar and telescopes can detect objects larger than about 7 cm. Passive space based systems provide an accurate statistical estimation of flux for debris smaller than about 0.1 mm in size. Consequently, there is no way of obtaining information about debris in the millimeter-size range. Considering that the relative speed between objects in space is commonly in the km/s range, millimeter sized debris carry enough energy to be deadly to astronauts or to totally destroy the functioning of any satellite. Then National space agencies have recommended launching orbital spacecraft carrying debris detection experiments for gaining a better understanding of small debris.CNES (the French Space Agency) is developing a new family of micro-satellites, that will make possible to put into orbit a totally new system of radar that could measure in-situ flux of debris. We present results of this system analysis, which would cumulate the advantages of both ground-based radar and in orbit passive experiments.The proposed method for detection is quite original and allows the radar to act like a band-pass filter with respect to the debris diameter. The optimum frequency is shown to be in the Ka-band. Two points are critical in the definition of the radar: the average power available and the false alarm probability in the detection criterion. Therefore, we present a special receiver chain in order to optimize the signal-to-noise ratio. The estimate of the radial velocity through Doppler frequency measurement may be used to discriminate orbital debris from meteoroids. This system could be built today using an existing Continuous Wave amplifier. Several hundreds of objects per year could be detected yielding an accurate statistical estimation.The orbital debris radar would be a major contribution to our knowledge of millimeter sized debris. This experiment would contribute to making the current models more accurate at all inclinations. The micro-satellite concept would make the orbital debris radar mission cheap enough for considering a constellation of such satellites.     

反导相控阵雷达注入式半实物仿真方法研究

对反导系统中的多功能相控阵雷达进行建模与仿真,是准确评估其反导防御能力的重要基础.以导弹突防为背景,基于射频注入式仿真技术,针对典型反导相控阵雷达,研究了半实物仿真平台的总体结构和工作流程,阐述了主要分系统的实现方案.采用该方法建立的半实物仿真平台可用来研究运用多种电子对抗突防措施下的相控阵雷达系统的防御能力,为科学决策提供技术支撑.     

基于远程预警雷达的临近空间无源相干定位系统

针对空中高价值隐身目标的探测问题,研究了基于远程预警雷达的临近空间无源相干定位技术。对目标探测距离进行了简单分析计算,给出了系统工作信号处理流程,对其中的主要关键技术进行了梳理。该技术可应用于无线电静默状态下的非协同探测定位系统项目,通过与电子侦察系统多传感器融合可以进一步完善防空体系无源探测网,完成对侦察目标在电子静默情况下的态势判断。     

超视距雷达探测高超声速飞行器可行性分析

在前期开展再入飞行器RCS（雷达散射截面）特性试验和理论研究的基础上，对典型临近空间高超声速飞行器RCS特性开展了研究，分析了绕流和尾迹对飞行器本体RCS特性的影响。研究表明等离子体流场在头身部绕流、近尾尾迹和部分远尾尾迹的最大电子密度将远高于电离层最高电子密度，更高于典型天波超视距雷达工作频段对应的临界电子密度。因而等离子体尾迹将会对3~30 MHz频段电磁波产生较强的散射，使得等离子体尾迹的RCS远远大于飞行器本体的RCS。利用临近空间高超声速飞行器尾迹RCS的这一特点，有可能实现对临近空间高超声速飞行器的超视距探测。     

A search for narrow band signals with SERENDIP II: a progress report

Commensal programs for the Search for Extraterrestrial Intelligence (SETI), carried out concurrently with conventional radio astronomical observing programs, can be an attractive and cost-effective means of exploring the large multidimensional search space intrinsic to this effort. Our automated commensal system, SERENDIP II, is a high resolution 131,072 channel spectrometer. It searches for 0.49 Hz signals in sequential 64,700 Hz bands of the IF signal from a radio telescope being used for an astronomical observation. Upon detection of a narrow band signal with power above a preset threshold, the frequency, power, time, and telescope direction are recorded for later study. The system has been tested at the Hat Creek Radio Astronomy Observatory 85 ft telescope and the NASA-JPL Deep Space Station (DSS 14) 64 m telescope. It is currently collecting data at the National Radio Astronomy Observatory 300 ft telescope.     

Frequency management and SETI: threats to SETI observations in the 1–3 GHz band

The nature of a SETI search makes observations uniquely vulnerable to radio frequency interference because the frequency of a possible ETI signal is unknown. Sensitive radio telescopes, sophisticated software and enhanced signal detection equipment are employed to detect faint signals in the 1–3 GHz frequency range. Frequency management at SETI occurs within a policy environment of the ITU spectrum allocation process. Increased demand by commercial satellite services for access to spectrum adjacent to bandwidth allocated to radio astronomy creates severe international and domestic pressures on SETI observations. Strategies for addressing the RFI problem at the international level will be discussed that include a contingency ITU allocation plan for exclusive use of a particular frequency range by SETI in the event a signal is detected. The lunar farside is, by international agreement, a radio quiet zone for use by radio astronomers. Protected from most human-generated emissions, a SETI radio telescope array on the lunar farside would provide reliable data with minimum interference.