国外航天侦察相机和测绘相机发展概况

航天侦察和测绘是战略武装必不可少的组成部分,航天侦察和测绘相机是对地观测卫星的有效载荷。 该文将简要介绍国外航天侦察和测绘相机发展概况、水平和发展趋势。     

一种用于测量高层大气风场的新型地基Fabry-Perot干涉仪

地表海拔大约250\,km高度处大气非常稀薄,目前被动光学观测是该层风场探测最有效手段.Fabry-Perot干涉仪(FPI)由于具有较高能量利用率及光谱分辨率等特点,是该层大气最有效的地基风场探测仪器之一.基于采用光路缩束系统及滤光片后置(标准具之后)方法研制的小型化FPI,2014年分别在河北廊坊(39.40°N,116.65°E)和山西岢岚(38.71°N,111.58°E)进行了地基观测试验,将观测数据与反演算法相结合得到高层大气风场数据,并将数据结果与美国大气研究中心两台FPI的风场数据进行了比较研究,在气辉整体辐射较弱的情况下得到岢岚站的风速平均反演偏差为11.8 m·s^-1.     

Recent Advances in Chinese Meridian Project

To develop an understanding of near-Earth space's response to solar activities and the coupling among different layers in geospace, China has initiated a ground base program to monitor China's geospace environment called the Meridian Space Weather Monitoring Project (Chinese Meridian Project). The effort consists of a chain of 15 ground-based observatories located roughly along 120°E longitude and 30°N latitude. Each observatory is equipped with multiple instruments to measure key parameters such as the baseline and time-varying geomagnetic field, as well as the middle and upper atmosphere and ionosphere from about 20 to 1000 kilometers. This project started collecting data in 2012. We will give a brief introduction to the Chinese Meridian Project, and present recent scientific results mainly in ionospheric and atmospheric studies.     

RN-FD型固体氡气源的稳定性及应用分析

对测氡仪器进行精确校准是氡测量工作中的重要环节,固体氡气源的稳定性、可靠性在校准中则显得至关重要。本文通过分析RN-FD型固体氡气源对闪烁室K值的稳定性实验结果,认为:RN-FD型固体氡气源标称的浓度值与实际浓度值不一致,标称浓度值只是理论浓度值而不是实际浓度值,需重新刻度才能使用;RN-FD型固体氡气源抽气循环时间不同则浓度不同,但抽气循环时间固定,观测结果比较稳定;对于没有α检查源的台站,RN-FD型固体氡气源可用于氡观测仪器坪区检查。     

大型真空热试验中的摄像观察技术

为完成在大型真空热试验中对飞船表面及舷窗的摄像观察提出了实施方案,分析并解决了普通摄像设备在真空—低温下使用的关键的技术问题,满足了试验要求.     

电子干扰对低可观测飞行器飞行路径规划的影响

为了提高巡航导弹的低空突防能力,在分析电子干扰对雷达网威胁区域的影响后认为:在多重干扰条件下,雷达探测空间会顺着干扰方向产生内凹和偏移,因此,建立了新的雷达探测空间模型.采用空间对象间拓扑关系推理方法建立了飞行器飞行路径规划目标函数中雷达威胁指数模型,然后改进了飞行器飞行路径规划模型,并在此基础上进行了巡航导弹飞行路径规划的软件仿真.仿真结果表明:考虑电子干扰对雷达威胁区域的影响情况下规划的飞行路径能够回避雷达威胁,有效提高飞行器低空突防能力.     

用于荧光细胞观察的制冷CCD成像系统

细胞成像技术是研究细胞运动、分裂和凋亡的必要手段,所以荧光条件下的细胞成像技术显得尤为重要。为满足荧光细胞观察对微弱光信号的检测和成像的要求,文章通过结构和电路设计,研制了一种用于荧光细胞观察的制冷CCD成像系统。通过分析各组件的技术特点,设计了高效制冷结构,提高了细胞荧光观察输出图像质量。     

一种天基光学GEO目标定位方法及初轨算法观测几何评价

提出一种基于天基光学短弧观测数据对GEO区目标进行定位的方法,以GEO区目标半径、偏心率为几何约束,通过最小二乘法估计目标位置、速度,估计结果可作为初轨算法的输入,也可以为初值预测轨道,引导其它平台对目标观测。利用广义Laplace初轨算法对多平台多观测弧段处理,为表征观测几何对定轨性能的影响,将几何精度因子(GOP)扩展到多平台多观测弧段,并引入几何精度因子的误差灵敏度(ESGOP)表征测量误差对观测几何的影响,仿真结果表明:对GEO目标而言,当GOP不小于0.03、ESGOP不大于0.005时,对目标的初轨精度可控制在50km之内。     

利用微波探测仪(ATMS)对在轨微波辐射计观测精度的模拟分析

微波辐射计的观测精度及其对数值模式同化应用的影响评估是微波辐射计观测指标设计的重要参考。基于微波探测仪(ATMS)资料,利用三维变分同化系统模拟分析在轨微波辐射计的观测精度指标。针对ATMS观测误差特征,在其观测基础上增加均值为零、标准偏差分别为0.5,1.0,1.5,2.0K的正态随机扰动,进而获得不同精度的观测模拟值序列,然后利用Harris和Kelley的辐射资料偏差订正经验方法订正不同精度的观测资料。偏差订正后,利用三维变分同化模式(WRFDA)直接同化ATMS资料。通过2016年6月6h预报场的同化试验,评估了不同观测精度的模拟资料对数值模式的同化影响。     

Feasibility of performing space surveillance tasks with a proposed space-based optical architecture

Under ESA contract an industrial consortium including Aboa Space Research Oy (ASRO), the Astronomical Institute of the University of Bern (AIUB), and the Dutch National Aerospace Laboratory (NLR), proposed the observation concept, developed a suitable sensor architecture, and assessed the performance of a space-based optical (SBO) telescope in 2005. The goal of the SBO study was to analyse how the existing knowledge gap in the space debris population in the millimetre and centimetre regime may be closed by means of a passive optical instrument. The SBO instrument was requested to provide statistical information on the space debris population in terms of number of objects and size distribution. The SBO instrument was considered to be a cost-efficient with 20 cm aperture and 6° field-of-view and having flexible integration requirements. It should be possible to integrate the SBO instrument easily as a secondary payload on satellites launched into low-Earth orbits (LEO), or into geostationary orbit (GEO). Thus the selected mission concept only allowed for fix-mounted telescopes, and the pointing direction could be requested freely. Since 2007 ESA focuses space surveillance and tracking activities in the Space Situational Awareness (SSA) preparatory program. Ground-based radars and optical telescopes are studied for the build-up and maintenance of a catalogue of objects. In this paper we analyse how the proposed SBO architecture could contribute to the space surveillance tasks survey and tracking. We assume that the SBO instrumentation is placed into a circular sun-synchronous orbit at 800 km altitude. We discuss the observation conditions of objects at higher altitude, and select an orbit close to the terminator plane. A pointing of the sensor orthogonal to the orbital plane with optimal elevation slightly in positive direction (0° and +5°) is found optimal for accessing the entire GEO regime within one day, implying a very good coverage of controlled objects in GEO, too. Simulations using ESA’s Program for Radar and Optical Observation Forecasting (PROOF) in the version 2005 and a GEO reference population extracted from DISCOS revealed that the proposed pointing scenario provides low phase angles together with low angular velocities of the objects crossing the field-of-view. Radiometric simulations show that the optimal exposure time is 1–2 s, and that spherical objects in GEO with a diameter of below 1 m can be detected. The GEO population can be covered under proper illumination nearly completely, but seasonal drops of the coverage are possible. Subsequent observations of objects are on average at least every 1.5 days, not exceeding 3 days at maximum. A single observation arc spans 3° to 5° on average. Using a simulation environment that connects PROOF to AIUB’s program system CelMech we verify the consistency of the initial orbit determination for five selected test objects on subsequent days as a function of realistic astrometric noise levels. The initial orbit determination is possible. We define requirements for a correlator process essential for catalogue build-up and maintenance. Each single observation should provide an astrometric accuracy of at least 1”–1.5” so that the initially determined orbits are consistent within a few hundred kilometres for the semi-major axis, 0.01 for the eccentricity, and 0.1° for the inclination.