银河系凸出的X射线光晕——6.7 keV线映射

Back to the Galaxy Pub Date : 2008-05-29 DOI:10.1063/1.44016

K. Koyama, S. Yamauchi

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引用次数: 0

摘要

6.7 keV谱线是类氦铁(FeXXV)的K壳共振跃迁，是温度在107至108 K之间的光学薄宇宙等离子体中最强烈的谱线。因此，可以用6.7 keV谱线来选择银河系中的光学薄热等离子体。本文报道了6.7 keV的谱图，并讨论了银河系中热气体组分的性质。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

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X‐ray halo from the Galactic bulge ‐The 6.7 keV line mapping

The 6.7 keV line is the K‐shell resonance transition from a Helium like iron (FeXXV) and is the most intense line in an optically thin cosmic plasma with a temperature ranging from 107 to 108 K. Therefore optically thin hot plasma in our Galaxy can be selected by the 6.7 keV line. This paper report on the 6.7 keV line map and discuss on the nature of the hot gas components in our Galaxy.

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Back to the Galaxy

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