E10.7指数在软X射线谱段的修正应用

表征EUV辐射通量的E10.7指数在越来越多的研究和应用中被用来代替传统的F10.7指数.X射线对地球D层和E层的电离起着重要作用,但由于D层观测数据的不足和E层电离源的多样性,难以被用来考虑X射线对电离层的影响.火星电离层下层的电离源几乎是单一的软X射线,这为研究X射线对电离层的作用提供了可能性.通过研究火星电离层下层的峰值电子浓度对E10.7的依赖关系,发现即便经过必要的修正,这种关系对不同的观测时段并不具备一致性.通过理论推导和数据分析,得到了一种特别用于描述太阳软X射线辐射通量的新指数,即Xs指数,用来替代E10.7指数.Xs指数在描述火星电离层下层对太阳辐射的依赖关系时,不同的观测时段有很好的一致性,表明Xs指数在表征太阳软X射线辐射强度方面比E10.7指数更加合适.      

FY-2C卫星太阳X射线探测器性能定标

通过具体的实验对FY-2C太阳X射线探测器进行了详细的定标.太阳X射线探测器的传感器采用充Ar气的正比计数器.主要探测能量大于4 KeV的太阳X射线流量.在坪特性、效率、正比性、能道划分、能量分辨率和时间分辨率等6个方面详细介绍了定标的方法及结果.定标结果表明,FY-2C卫星的太阳X射线探测器在各个方面都具有很好的性能.最后对FY-2C的在轨探测数据与GOES卫星进行了比较.GOES卫星的太阳X射线传感器采用电离室.FY-2C的探测结果与GOES的探测结果非常吻合.结果表明,FY-2C太阳X射线探测器可以很好地监测太阳X射线的流量变化,为空间环境监测提供有效的服务.      

ASO-S卫星HXI调制定标装置设计与验证

先进天基太阳天文台卫星（ASO-S）是中国首颗综合性太阳观测任务，太阳硬X射线成像仪（HXI）是ASO-S卫星三大载荷之一，主要负责太阳耀斑观测。HXI采用阵列空间调制间接成像方法，包含91个子准直器单元。发射前，在地面对HXI进行调制参数定标非常必要，但由于没有平行的X射线源而十分困难。本文根据HXI的基本原理与设计方案，提出了基于地面调制功能定标的设备与HXI调制定标的需求。根据所述需求，介绍了研制的X射线束流调制定标装置；利用该装置对HXI飞行件上所有子准直器完成地面调制功能定标。标定试验结果与预期相符，充分证明了准直器与X射线束流定标装置性能优良，该装置还可用于后续类似载荷的定标。     

太阳耀斑显著的热和非热事件的统计特征

本文利用GOES卫星和SMM卫星软、硬X射线耀斑观测资料,分析耀斑中软、硬X射线辐射流量的分布,发现太阳耀斑存在着显著的热事件(PT事件)和显著的非热事件(PNT事件),它们主要特征是:(1)PT事件为缓变型耀斑,PNT事件为脉冲型耀斑;(2)PT事件的硬X射线谱较软,PNT事件能谱较硬;(3)PNT事件非热能量释放速率比PT事件快3—10倍;(4)耀斑发展趋缓慢,PT事件中软X射线峰值流量越大;(5)耀斑中PNT事件约占60％,PT事件约占40％.最后定性讨论了产生PT和PNT事件的可能机制.      

应用BP神经网络针对高通量质子事件的通量数值预报

质子事件的爆发与太阳软X射线辐射有着很强的相关性,利用GOES卫星的1～8 (A)波段和0.5～4 (A)波段的软X射线数据,选取一些特征参量验证该相关性并应用到质子事件短期预报中.在当前质子事件传输物理机制不完全明确的情况下,在现有的预报质子事件有无的模型基础上,利用BP神经网络,根据软X射线通量水平等预测事件质子峰值通量水平,再对训练后的网络进行检验,检验预测所得结果与实际探测值误差小于一个量级,具备一定实用意义.      

太阳耀斑硬X射线能谱演变特征

太阳硬X射线是耀斑高能电子束流与太阳大气相互作用产生的韧致辐射,根据简单的太阳耀斑环物理模型,假定具有流量与能谱同步变化的高能电子束流从耀斑环顶部注入,计算了硬X射线辐射在不同的靶物质密度区的能谱演变特征。结果表明:硬X射线辐射在低大气密度靶区呈现软一硬一硬的能谱演变特征,在高密度靶区硬X射线能谱则具有软一硬一软的变化特征。高能电子束流持续时间影响谱型转变区域在耀斑环中的高度。      

发展中的X射线空间望远镜

<正>由于天体发射出的X射线在穿过大气层时大部分会被吸收,因此使用空间望远镜,在大气层以外对天体辐射的X射线进行观测,是X射线天文学的主要观测方式。从20世纪70年代至今,不少X射线空间望远镜被发射升空,为我们揭示了肉眼看不到的宇宙秘密。     

HXMT的空间环境本底计算

硬X射线调制望远镜(HXMT)是一颗宽波段X射线(1～250 keV)天文卫星,其核心载荷高能X射线望远镜(HE)工作于硬X射线能区(20～250 keV),致力于实现硬X射线的高灵敏度巡天观测,描绘硬X射线天图,并对特殊天体作高灵敏度定点观测.为了获得高灵敏度,必须有效地抑制本底.本底主要是由轨道环境中的粒子(γ射线、质子、电子、中子)与探测器相互作用产生的.本文结合大量的描述近地空间本底的文献和最新的实测数据,整理出一套自洽的近地空间本底粒子的数据和公式,便于应用.并通过Geant 4软件模拟计算给出了HXMT的本底及本底随时间和轨道的变化.      

空间光通信激光相干组束技术研究

介绍多种在输出功率得以提高的同时保持好的光束质量的激光相干组束技术原理.综合分析并评述激光相干组束技术研究状况,对主动相位控制和被动相位控制两种技术方案进行比较,基于主振荡放大的主动相位控制方案可以获得接近衍射极限、稳定、远场高亮度的光束,可为构建高效、可靠的长距离、高速率空间光通信系统提供技术支撑,对认识激光相干组束技术的发展趋势,研究空间激光通信系统具有一定的参考价值.     

大口径积分球辐射定标光源辐射性能研究

目前,我国空间光学遥感器正向着大型化、高精度的方向发展,辐射定标装置也随之发展进步。本文系统地介绍了大口径空间相机用积分球辐射定标装置辐射性能的测试方法。研制出一套积分球辐射性能测试装置,用于测试大口径积分球的均匀性、余弦特性和稳定性,并给出了积分球辐射定标光源的输出不确定度。文中检测的积分球辐射定标光源内径为3 000mm,出光面直径为1 000mm,得到该积分球辐射定标光源的均匀性为0.11%,在±20°范围内余弦特性最大偏移为1.1%,整个系统的输出不确定度为5.94%。     

单色仪输出波长准确度校准技术研究

利用激光器产生单色光光源,解决了红外探测器相对光谱响应（单色仪）的溯源。根据单缝衍射和多光束干涉的原理,将光垂直入射到光栅面上,经会聚镜会聚其焦平面上形成一系列对称排列的明条纹,通过旋转光栅,在输出端得到以单色光波长倍数递增的、信噪比足够大的光源。这样,只要选择合适的激光器,就可解决单色仪整个波段的溯源性。     

AXAF,a permanent orbiting X-ray observatory: Telescope and instrumentation plans

The Advanced X-ray Astrophysics Facility (AXAF) now under study is to be a long-lived X-ray observatory in space. It is to be launched by the Space Shuttle, maintainable on-orbit, and retrievable for ground re-furbishment. The AXAF is conceived as an X-ray telescope with 6 nested grazing incidence X-ray mirrors (with a maximum aperture of 1.2 m) and interchangeable and replaceable focal plane instruments. The optics will provide 0.5 arcsecond imagery over a several arcminute field and somewhat reduced resolution over 1 degree in the X-ray band from 0.1 to 10 keV (1.2 to 120 A). The characteristics and expected performance of the observatory are described.     

U.S. planetary protection program: Implementation highlights

The implementation of planetary protection in the United States space program has reflected the trend in policy from an absolute to a probabilistic prohibition of the contamination of the celestial bodies of the solar system. The early emphasis on spacecraft sterilization (e.g. Ranger) was replaced by the imposition of contamination control procedures on later missions such as Pioneer, Viking, and Voyager. Similarly, analytical and laboratory techniques were developed to demonstrate compliance with probabilistic requirements. Microbial burden reduction methods that are not hazardous for spacecraft reliability supplanted the abstract concept of sterilization. The United States implementation of planetary protection has been completely successful. In an exploration program that has included Mercury, Venus, Mars, the Jovian system, and the Saturnian system, there have been no accidental impacts or detection of false positives (terrestrial microbes). Further, the contamination control and microbial burden procedures have proved beneficial to spacecraft systems and on-board science instruments. We review in this paper the implementation of planetary protection procedures by the Pioneer (10 and 11), Viking and Voyager projects.     

热离子质谱分析仪的研制及定标

热离子质谱分析是空间等离子体探测的核心技术之一.热离子质谱分析仪采用了半球形静电分析器结合基于碳膜的飞行时间系统方案，是目前应用最广泛、最成熟的空间热离子质谱分析技术.热离子质谱分析仪解决了三项关键技术，即5mV高分辨扫描高压，10~20nm超薄碳膜处理以及30kV超高加速电压.分析仪原理样机在瑞士伯尔尼大学完成了定标试验，实现指标参数如下:能量范围为0.499eV~29.94keV，能量分辨率为10.5%；能够实现离子成分H+，He+，O+的分辨；视场范围为360°×8.4°，角度分辨率为22.5°×8.4°.基于热离子质谱分析仪的研制基础，可以进一步开发出更高质谱分辨、更大探测视场以及小型化的等离子体探测载荷.      

Status of the Hard X-ray Modulation Telescope (Insight-HXMT) Project

The Hard X-ray Modulation Telescope (HXMT) was launched at Jiuquan Satellite Launch Center on June 15, 2017, and was named as Insight-HXMT after the launch. Now all the instruments work properly in space, dozens of sources have been observed, and some early scientific results have been published. The nominal lifetime of Insight-HXMT is 4 years.      

Measuring the economic benefits of a national planetary protection policy to regulate future private space activities between Earth and Mars: Results of a contingent valuation survey in Greece

The emergence of private space actors may soon enable the growth of the novel market segments of space research and exploration, space resources utilization, and human access to space. The interdisciplinary field of Planetary Protection has to keep up with these advances. Planetary Protection is defined as a set of guidelines that aim to prevent the forward contamination of celestial bodies with biological material from Earth and the backward contamination of the terrestrial biosphere with extraterrestrial biological material. As space entrepreneurs acquire and develop the resources and competencies for commercial access to space, significant questions are expected to be raised in the future with respect to potential forward and backward contamination issues, particularly with respect to activities between Earth and Mars. Although such private activities do not seem to pose a serious Planetary Protection threat at the moment, certain preparatory steps need to be taken in order to prudently inform the relevant policy-making procedures. This work describes the application of the Contingent Valuation Method, a useful tool of the environmental economics discipline, with the aim of demonstrating a novel approach to estimate the economic valuation of the external benefits of preventing forward and backward contamination between Earth and Mars. Particularly, via a survey specifically developed for this purpose, a set of questions are used to elicit the perceived economic value that respondents place on the prevention of forward and backward contamination; the survey is administered to a national probability sample in Greece, and the generated data is processed through statistical analysis. The Contingent Valuation Method is a popular and well-established stated preference valuation technique; these techniques are often the more suitable choice for ex-ante valuations of future changes, and are currently the only known approach to capture all the aspects of the economic value of non-market goods. Through an initial proof-of-concept in Greece, the goal of this work is to provide useful insights on the expected external benefits of a national Planetary Protection policy to regulate future private space activities between Earth and Mars, and to encourage a larger-scale application of this tool in other countries around the world.     

The ROSAT mission

A primary scientific objective of the ROSAT mission is to perform the first all-sky survey with an imaging X-ray telescope leading to an improvement in sensitivity by several orders of magnitude compared with previous surveys. A large number of new sources (? 10⁵) will be discovered and located with an accuracy of 1 arcmin or better. These will comprise almost all astronomical objects from nearby normal stars to distant quasistellar objects. After completion of the survey which will take half a year the instrument will be used for detailed observations of selected sources with respect to spatial structure, spectra and time variability. In this mode which will be open for guest observers ROSAT will provide substantial improvement over the imaging instruments of the Einstein observatory.The main ROSAT telescope consists of a fourfold nested mirror system with 83 cm aperture having three focal plane instruments. Two of them will be imaging proportional counters (0.1 – 2 keV) providing a field of view of 2°, an angular resolution of ≈ 30″ in the pointing mode and a spectral resolution ^ΔE/E ≈ 45% FWHM at 1 keV. The third focal instrument will be a high resolution imager (≈ 3″). The main ROSAT telescope will be complemented by a parallel looking Wide Field camera which extend the spectral coverage into the XUV band.     

层板式喷注器在空间飞行器发动机中的应用综述

综述了层板式喷注器在空间飞行器液体火箭发动机中的应用。着重举例分析了层板式喷注器应用于航天飞机轨道机动发动机、小推力姿控发动机、燃气发生器中所获得的优于传统喷注器的良好性能和效益;分析了层板式喷注器在小推力＿液体火箭发动机稳态和脉冲方式工作时对抑制排气羽流污染的有效作用;最后提出了研制层板式喷注器所需进一步做的工作。     

Progress of Solar Wind Magnetosphere Ionosphere Link Explorer(SMILE) Mission

SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) mission is a joint ESA-CAS space science project. The working orbit is a 19 R_e 5000 km HEO with 4 scientific instruments:Soft X-ray Imager(SXI), Ultra-Violet Imager (UVI), Magnetometer (MAG) and Light Ion Analyzer (LIA). SMILE aims to understand the interaction between the solar wind and the Earth's magnetosphere through the images of SXI and UVI and in-situ measurement from LIA and MAG. After the kick-off in 2016, the SMILE project went to Phase A study. The mission adoption is scheduled for November 2018, with a target launch date in 2022-2023. In this paper, the background of the mission, scientific objectives, the design and characteristics of scientific instruments and the mission outline will be introduced in details.