Study of solar X-ray albedo by the upper earth atmosphere and fluorescent X-rays using the data obtained by the X-ray astronomy satellite

利用X射线天文卫星获得的数据研究上层地球大气和荧光X射线的太阳X射线反照率

• 批准号: 12640433
• 负责人: ITOH Masayuki
• 金额: $ 0.83万
• 依托单位: Kobe University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (C)
• 财政年份: 2000
• 资助国家: 日本
• 起止时间: 2000 至 2001
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-12640433/
• 关键词: Solar X-ray; The sun; Albedo; 太陽活動周期; 高層大気; 宇宙塵

We studied the earth albedo of the solar X-ray and its long term variation using die data obtained by the Gas Imaging Spectrometer (GIS) on board the X-ray satellite ASCA The X-ray albedo spectra in the energy range of 0.5-5keV were obtained with the resolution that enables detection of K-lines of several elements for almost the full span of solar activity. The spectra can be described with a model that consists of three elements : (a) 2-temperature thermal emission, (b) modification of the thermal emission through the reflection by the earth atmosphere, and (c) additional emission lines. The component (a) is the averaged emission from the solar coronae. The temperatures of the thermal X-ray emission from the sun stayed almost constant within the statistics of the data, and the values of the two components are 〜300MK and 500-1000MK respectively The intensities of the two components showed variation in accordance with the solar activity cycle, of which amplitude was larger for the higher temperature component. The higher temperature component is probably from the X-ray emission of the solar flares, and the lower temperature component is from the non-flaring coronae. The additional emission lines include K-lines of Mg and Si aside from the K-lines from the atmospheric 0 and Ar. The Mg and Si lines have lower energies and higher intensities than those expected from the main component of the thermal emission from the sun. One of the possible explanations is the ionization non-equilibrium eflect in the solar coronal plasma ASTRO-EII that is to be launched in 2005 is expected to enable same line of research with superior energy resolution.

我们研究了太阳能X射线的地球反照率及其长期变化，使用气体成像光谱仪（GIS）在X射线卫星ASCA上获得的模具数据在0.5-5keV的能量范围内获得了X射线卫星ASCA，该分辨率是通过分辨率获得的，该分辨率可检测几乎可以在sol solar of solar的范围内检测几个元素的k线。可以用一个由三个元素组成的模型来描述这些光谱：（a）2-温度的热发射，（b）通过地球大气的反射对热发射进行修饰，以及（c）其他发射线。分量（a）是太阳冠的平均发射。来自太阳的热X射线发射的温度几乎保持在数据的统计数据中，并且两个组件的值分别为〜300MK和500-1000MK，分别是根据太阳能活性周期显示的两个组件的强度，其中较高的温度分数较大。较高的温度成分可能来自太阳耀斑的X射线发射，较低的温度成分来自非晶状冠状动脉。除了大气0和AR的K线外，其他发射线还包括Mg和Si的K线。 MG和SI线具有比主要组成部分预期的能量较低和更高的强度，可能的解释之一是在2005年推出的太阳冠状化等离子体Astro-EII中的电离非平衡有效，预计可以通过卓越的能量分辨率启用相同的研究线。

项目成果

Itoh, M.: "Total Spectrum of the solar X-ray and its long-term variation obtained from earth albedo data of ASCA GIS"The proceedings of the IAU 8-th Asian-Pacific Regional Meeting. Vol.II. 435-436 (2002)

Itoh, M.：“从 ASCA GIS 地球反照率数据获得的太阳 X 射线总光谱及其长期变化”IAU 第 8 届亚太地区会议记录。

Itoh, M. et al.: "Total Spectrum of the solar X-ray and its long-term variation obtained from earth albedo data of ASCA GIS"The Proceedings of the IAU 8th Asian Pacific Regional Meeting. Vol.II. 435-436 (2002)

Itoh, M.等：“从ASCA GIS的地球反照率数据获得的太阳X射线总光谱及其长期变化”IAU第八届亚太地区会议论文集。