The Focusing Optics X-ray Solar Imager (FOXSI)
The Focusing Optics X-ray Solar Imager (FOXSI)
复制标题
聚焦光学 X 射线太阳成像仪 (FOXSI)
DOI：
10.1117/12.895271
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发表时间：
2011
期刊：
影响因子：
--
通讯作者：
et al
中科院分区：
文献类型：
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作者：
S.Krucker;et al
聚焦光学X射线太阳成像仪(FOXSI)是由NASA低成本进入太空计划资助的探空火箭有效载荷，用于测试用于太阳观测的硬X射线(HXR)聚焦光学装置和位置灵敏固态探测器。当今领先的太阳HXR仪器鲁文·拉马蒂高能太阳光谱成像仪(RHESSI)提供了出色的空间(2角秒)和光谱(1keV)分辨率。然而，由于使用了间接成像系统，导出的图像具有低动态范围(通常为<；10)和灵敏度。这些限制使得研究日冕中的微弱X射线源变得困难，而这些X射线源对于理解发生在那里的粒子加速过程至关重要。掠入射X射线聚焦光学与位置灵敏固态探测器相结合可以克服这两个限制，使我们能够在理解太阳上的脉冲能量释放方面取得下一个突破。FOXSI项目由加州大学伯克利分校的空间科学实验室领导。NASA马歇尔太空飞行中心负责GRAGGING入射光学系统，而日本宇宙航空研究开发机构/ISAS的Astro-H团队提供了双面硅条探测器。FOXSI是下一代太阳硬X射线光谱成像仪的探路者。这样的观测站将能够为太阳耀斑加速区内的非热电子成像，追踪它们通过日冕的路径，并提供必要的定量测量，如能谱、密度和加速电子中的能量含量。
The Focusing Optics x-ray Solar Imager (FOXSI) is a sounding rocket payload funded under the NASA Low Cost Access to Space program to test hard x-ray (HXR) focusing optics and position-sensitive solid state detectors for solar observations. Today's leading solar HXR instrument, the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) provides excellent spatial (2 arcseconds) and spectral (1 keV) resolution. Yet, due to its use of an indirect imaging system, the derived images have a low dynamic range (typically <10) and sensitivity. These limitations make it difficult to study faint x-ray sources in the solar corona which are crucial for understanding the particle acceleration processes which occur there. Grazing-incidence x-ray focusing optics combined with position-sensitive solid state detectors can overcome both of these limitations enabling the next breakthrough in understanding impulsive energy release on the Sun. The FOXSI project is led by the Space Sciences Laboratory at the University of California, Berkeley. The NASA Marshall Space Flight Center is responsible for the grazingincidence optics, while the Astro-H team at JAXA/ISAS has provided double-sided silicon strip detectors. FOXSI is a pathfinder for the next generation of solar hard x-ray spectroscopic imagers. Such observatories will be able to image the non-thermal electrons within the solar flare acceleration region, trace their paths through the corona, and provide essential quantitative measurements such as energy spectra, density, and energy content in accelerated electrons.