Gamma ray lines from solar flares
Gamma ray lines from solar flares
复制标题
太阳耀斑的伽马射线线
DOI：
10.1007/978-94-010-1802-9_34
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发表时间：
1975
期刊：
影响因子：
--
通讯作者：
R. Lingenfelter
中科院分区：
文献类型：
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作者：
R. Ramaty;R. Lingenfelter
我们详细地讨论了太阳耀斑中伽马射线线产生的理论。理论预测和观测检测到的最强线在2.2 MeV，是由于光球中的质子捕获中子。中子是在耀斑加速粒子的核反应中产生的，这些粒子也会产生正电子并产生核伽马射线。从4.4或6.1 MeV谱线与2.2 MeV谱线的观测和计算强度比较，可以推断出耀斑区域加速核的谱；从这些谱线的绝对强度可以推算出太阳上加速原子核的总数。2.2 MeV线的研究也提供了光球中He3含量的信息。由正电子湮灭产生的0.51 MeV线的研究补充了从其他线获得的数据；此外，它还提供了湮灭区内的温度和密度以及产生能量大于约1兆电子伏特的连续伽马射线的加速电子束的各向异性的信息。
We have treated in detail the theory of gamma-ray line production in solar flares. The strongest line, both predicted theoretically and detected observationally at 2.2 MeV, is due to neutron capture by protons in the photosphere. The neutrons are produced in nuclear reactions of flare accelerated particles which also produce positrons and prompt nuclear gamma rays. From the comparison of the observed and calculated intensities of the lines at 4.4 or 6.1 MeV to that of the 2.2 MeV line it is possible to deduce the spectrum of accelerated nuclei in the flare region; and from the absolute intensities of these lines it is possible to obtain the total number of accelerated nuclei at the Sun. The study of the 2.2 MeV line also gives information on the amount of He3 in the photosphere. The study of the line at 0.51 MeV resulting from positron annihilation complements the data obtained from the other lines; in addition it gives information on the temperature and density in the annihilation region and on the anisotropy of the accelerated electron beam which produces continuum gamma rays at energies greater than about 1 MeV.