Solar Atmospheric Abundances and Energy Content in Flare-accelerated Ions from Gamma-Ray Spectroscopy
Solar Atmospheric Abundances and Energy Content in Flare-accelerated Ions from Gamma-Ray Spectroscopy
复制标题
来自伽马射线光谱的太阳大气丰度和耀斑加速离子的能量含量
DOI：
10.1086/309841
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发表时间：
1995
期刊：
影响因子：
--
通讯作者：
R. Murphy
中科院分区：
文献类型：
--
作者：
R. Ramaty;N. Mandzhavidze;B. Kozlovsky;R. Murphy
我们使用SMM伽马射线数据从19个太阳耀斑研究太阳大气中的环境元素丰度。我们发现，丰度比低FIP（第一电离势），高FIP元素的增强相对于光球丰度，但这些比率的变化，从耀斑到耀斑是有限的，比从EUV和X射线观测推断的范围较窄。γ射线源Mg/O（低FIP与高FIP元素丰度比）的平均值为冠状，个别值总是高于光球Mg/O。Ne/O的值（~0.25）高于从太阳高能粒子数据中获得的日冕值0.15，但与一些EUV和X射线测定结果并不矛盾。为了避免Ne/O高于0.3，需要向下延伸到约1 MeV/核子的陡峭加速粒子能谱。这意味着大部分可用的耀斑能量包含在加速的离子中。
We used SMM gamma-ray data from 19 solar flares to study ambient elemental abundances in the solar atmosphere. We found that the abundance ratios of low FIP (first ionization potential) to high FIP elements are enhanced relative to photospheric abundances, but that the variability of these ratios from flare to flare is limited to a narrower range than that inferred from EUV and X-ray observations. The mean of the gamma-ray derived Mg/O (a low FIP to high FIP element abundance ratio) is coronal and the individual values are always higher than the photospheric Mg/O. The value of Ne/O (~0.25) is higher than the coronal value of 0.15 obtained from solar energetic particle data, but not inconsistent with some EUV and X-ray determinations. To avoid Ne/O higher than 0.3 a steep accelerated particle energy spectrum extending down to about 1 MeV per nucleon is needed. This implies that a large fraction of the available flare energy is contained in accelerated ions.