共查询到19条相似文献,搜索用时 140 毫秒
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围绕国际一流科学目标,发展顶级探测设备是中国太阳物理位列国际先进行列的立足点。70多年的空间太阳探测历程中,极紫外波段探测发挥了极其重要的作用,极紫外观测设备也几乎成为了太阳探测卫星的必备载荷之一。中国在极紫外探测,尤其是光谱探测方面的基础非常薄弱,导致相关科学研究几乎全部依赖国外数据,从而严重制约了中国太阳物理学科的发展。本文根据太阳极紫外探测的特点,系统分析了国外光谱探测的历史、现状以及未来发展趋势,并归纳了三类主要探测方式,即全日面积分光谱探测、低速光谱成像探测、快速光谱成像探测的当前水平,包括其技术方案及取得的部分科学成果。在此基础上,提出中国太阳极紫外光谱探测“三步走”的发展思路,并对每一步的科学目标、指标需求和候选探测方案提出建议。同时,展望了在太阳极紫外成像探测方面开展创新性尝试的思路。 相似文献
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太阳X-EUV成像望远镜波长选择装置 总被引:1,自引:1,他引:0
太阳X射线-极紫外射线(X-EUV,X rays-Extreme Ultraviolet)成像望远镜是我国专门服务于空间天气预报研究的太阳短波成像监测仪器,望远镜工作在0.4~10 nm的X射线波段和19.5 nm的极紫外谱段,能够提供全日面、高分辨率的成像观测.波长选择装置是该望远镜的一个重要子系统,可以增强望远镜动态响应范围,有助于获取更多的反演日冕等离子体参数,这些参数可用来诊断日冕活动.该装置的运动控制具有低功耗的特点,能够满足空间应用环境的特殊要求.其中,步进电机精位置控制是设计的重点,有2种光电编码矩阵可以用于位置检测,从工程可实现角度优选出其中一种,并且从工程可靠性角度分析了该光电编码矩阵的故障模式,提出了在轨故障处理的预案. 相似文献
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采用红外传感器观测海面,若观测天顶角较大,则视场中会同时出现海面与天空背景.通过计算传感器每一像素单元接收的辐射强度,可以得到海天背景多谱段光学图像.为了计算假定海况条件下海面随观测方向变化的反射辐射,基于几何光学原理修正了传统海面辐射特性模型.由于路径长度随传感器垂直视场变化,此时大气对辐射传输的影响十分显著.天光及水平路径辐射采用改进的大气辐射传输模型计算.该模型具有更高的光谱分辨率,适用于多谱段成像仿真.基于给出的海面辐射特性模型和大气辐射传输模型,分别仿真了不同时刻不同观测角下可见光、中波红外和长波红外的海天背景辐射图像.仿真结果符合物理原理,与实测图像的对比验证了新模型的可靠性. 相似文献
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在历时20余年的立项和研制进程后,2020年2月10日由欧空局(ESA)主导、美国参加的太阳轨道探测器任务在美国发射升空,这是人类首个对太阳极区成像的空间太阳物理任务。太阳轨道探测器将用约3年时间在水星轨道以内的大椭圆日心轨道开展近距离太阳观测,用7年(包括3年延寿期)时间在黄道面外开展太阳极区高分辨率成像及探测。该任务有望进一步揭示太阳磁场,太阳活动爆发,太阳风起源、加速及其行星际传播和对地球空间天气的驱动等重要前沿问题的本质,加深对太阳活动周以及日地联系的理解。该任务启示中国空间科学要重视太阳深空观测任务的前瞻布局与立项实施。 相似文献
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为了对"高分五号"卫星全谱段光谱成像仪的太阳反射谱段辐射性进行长期监测与校正,并针对其谱段范围宽、精度要求高、口径大、使用寿命长等特点与要求,优化设计了可展开的漫反射板进行全光路全视场的辐射定标。定标漫反射板安装在相机光学系统的前端侧面,不影响相机正常成像,在定标时通过驱动机构展开漫反射板到相机前端,根据"高分五号"卫星轨道特点、定标能量要求及相机安装矩阵等设计定标漫反射板展开角度为39°。研制了430 mm×430 mm大尺寸聚四氟乙烯漫反射板组件以保证在展开时满足全光路全视场的定标,漫反射板在420~2 400 nm光谱范围内半球反射率高于95%,在相机观测方向BRDF变化优于2.5%。同时,设计了漫反射板稳定性监视辐射计用于监测漫反射板在轨性能衰减,监测精度1.5%。在轨定标精度分析为4.76%,满足指标要求。 相似文献
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Recent advances in observations and modeling of the solar ultraviolet and X-ray spectral irradiance 总被引:1,自引:0,他引:1
Thomas N. Woods 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
There have been significant, recent advances in understanding the solar ultraviolet (UV) and X-ray spectral irradiance from several different satellite missions and from new efforts in modeling the variations of the solar spectral irradiance. The recent satellite missions with solar UV and X-ray spectral irradiance observations include the X-ray Sensor (XRS) aboard the series of NOAA GOES spacecraft, the Upper Atmosphere Research Satellite (UARS), the SOHO Solar EUV Monitor (SEM), the Solar XUV Photometers (SXP) on the Student Nitric Oxide Explorer (SNOE), the Solar EUV Experiment (SEE) aboard the Thermosphere, Ionosphere, Mesosphere, Dynamics, and Energetics (TIMED) satellite, and the Solar Radiation and Climate Experiment (SORCE) satellite. The combination of these measurements is providing new results on the variability of the solar ultraviolet irradiance throughout the ultraviolet range shortward of 200 nm and over a wide range of time scales ranging from years to seconds. The solar UV variations of flares are especially important for space weather applications and upper atmosphere research, and the period of intense solar storms in October–November 2003 has provided a wealth of new information about solar flares. The new efforts in modeling these solar UV spectral irradiance variations range from simple empirical models that use solar proxies to more complicated physics-based models that use emission measure techniques. These new models provide better understanding and insight into why the solar UV irradiance varies, and they can be used at times when solar observations are not available for atmospheric studies. 相似文献
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L. Qian S.C. Solomon R.G. Roble B.R. Bowman F.A. Marcos 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
Recent measurements by the Solar EUV (Extreme Ultra Violet) Experiment (SEE) aboard the Thermosphere–Ionosphere–Mesosphere Energetics and Dynamics satellite (TIMED) provide solar EUV spectral irradiance with adequate spectral and temporal resolution, and thus the opportunity to use solar measurements directly in upper atmospheric general circulation models. Thermospheric neutral density is simulated with the NCAR Thermosphere–Ionosphere–Electrodynamic General Circulation Model (TIEGCM) using TIMED/SEE measurements and using the EUVAC solar proxy model. Neutral density is also calculated using the NRLMSISE-00 empirical model. These modeled densities are then compared to density measurements derived from satellite drag data. It is found that using measured solar irradiance in the general circulation model can improve density calculations compared to using the solar proxy model. It is also found that the general circulation model can improve upon the empirical model in simulating geomagnetic storm effects and the solar cycle variation of neutral density. 相似文献
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Alan Title 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,4(8):67-74
Solar physics is about to undergo a revolution in the amount and quality of undistorted high resolution filter-grams and spectra available for study. Spacelab 2 will obtain UV and visible data comparable to the best obtained on Earth, but free of both blurring and image distortion. The goals of the Spacelab 2 flight are to collect data on the evolution of the solar magnetic and velocity fields on time scales of seconds to days. In the first part of the next decade, the 1.3 meter aperture Solar Optical Telescope will have sufficient spatial resolution to collect data on the scale of the solar density scale height [~ 100 km] which should be sufficient to study the basic physical processes in the solar atmosphere. 相似文献
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《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2005,35(3):384-387
The hydrogen Lyman (Lyα, 121.267 nm and Lyβ, 102.572 nm) lines are important contributors to the solar extreme ultra violet (EUV) flux which illuminates the upper Earth’s atmosphere. From high resolution spectral observations performed with the solar ultraviolet measurement of emitted radiations (SUMER) spectrometer on the Solar and Heliospheric Observatory (SOHO), the detailed profiles of these two lines have been obtained. Some insights into the variation of the shape of the profiles, sampled throughout the present solar cycle 23, are given and discussed. 相似文献
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R. Devaraj K. Sankarasubramanian Surekha Kamath 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2013
Multi-slit spectropolarimeter is a next-generation spectropolarimeter to obtain vector magnetic field information at high spatial, spectral, and temporal resolution for studying the magnetic structures on the Sun. Once developed, it can be used as ground based instrument at solar observatories, also as a space payload for various solar missions. A high spectral resolution is invariably an important parameter for accurate vector magnetic field measurements and faster cadence is required for the study of dynamical evolution of structures (e.g., solar flares, sunspots etc.) on the Sun and hence better understanding on the physics behind their evolution. 相似文献
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A. Coradini M. C. De Sanctis F. Capaccioni G. Piccioni A. Romoli E. Suetta C. Giunti M. Barilli 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,33(12):2189-2194
The BepiColombo mission to Mercury is devoted to the thorough exploration of Mercury and its environment, with the aim to understand the processes of planetary formation and evolution in the hottest part of the protoplanetary nebula. This mission represents an unique opportunity for the European community to extend the understanding of the Solar Nebula evolution from its outer edge – ideally represented by comets – to its inner and warmer edge. Obviously this exploration asks for a detailed knowledge of the main constituents of the matter present in the different Solar System areas. Spectroscopy is a powerful tool to acquire this knowledge. We have participated with a large consortium of European researchers to the development of the Rosetta imaging spectrometer. We propose here to use our experience to develop a newly designed spectrometer to investigate the mineralogical composition of the Mercurial surface. Given the particular thermodynamical situation of the Mercurial surface, we have developed a concept that combines a medium IR low spectral resolution imager with a moderate spectral resolution NIR point spectrometer. The main goal of METHIS is to provide the mineralogical characterisation of the surface with sufficient spectral resolution in a scientifically diagnostic spectral range. 相似文献