A determination of the (He-3)/H ratio in the solar photosphere from flare gamma-ray line observations
A determination of the (He-3)/H ratio in the solar photosphere from flare gamma-ray line observations
复制标题
根据耀斑伽马射线线观测确定太阳光球层中的 (He-3)/H 比
DOI：
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发表时间：
1987
期刊：
影响因子：
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通讯作者：
R. Lingenfelter
中科院分区：
文献类型：
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作者：
X. Hua;R. Lingenfelter
2.223 MeV的伽马射线线发射的时间依赖性，从捕获耀斑产生的中子在太阳光球提供了一个灵敏的措施，He-3丰度。Monte Carlo计算已经取得了这种时间依赖性作为一个函数的He-3丰度和观测角度的厚靶相互作用的耀斑加速离子的入射能谱和角分布的范围内产生的中子。假设镜像分布，建议由其他观测，它被发现，太阳极大使命测量的时间依赖性的2.223 MeV线发射的太阳耀斑的1982年6月3日，意味着太阳光球（He-3）/H比为（2.3 +或-1.2）× 10-5在90%的置信水平。44篇参考文献。
The time dependence of the 2.223 MeV gamma-ray line emission from the capture of flare-produced neutrons in the solar photosphere provides a sensitive measure of the He-3 abundance there. Monte Carlo calculations have been made of this time dependence as a function of both He-3 abundance and observing angle for neutrons produced by thick-target interactions of flare-accelerated ions with a range of incident energy spectra and angular distributions. Assuming a mirroring distribution, suggested by other observations, it is found that the Solar Maximum Mission measurements of the time dependence of the 2.223 MeV line emission from the solar flare of June 3, 1982, imply a solar photospheric (He-3)/H ratio of (2.3 + or - 1.2) x 10 to the -5th at the 90 percent confidence level. 44 references.