Solar Flare Gamma-Ray and Neutron Studies

对太阳大气中加速离子相互作用产生的伽马射线和中子辐射的大范围观测与详细的理论计算进行了比较，极大地促进了我们对太阳耀斑加速、传播和相互作用的理解。这些比较得出了加速离子在太阳大气中相互作用的总数、能谱和角分布、它们的逃逸概率、元素丰度等。这些计算是通过开发一个复杂的蒙特卡罗程序计算机代码进行的。这些计算现在将扩展到包括随机加速，这将允许研究离子加速和在太阳耀斑中传播的依赖时间的性质，以及MHD湍流在这些过程中的作用。

Comparisons of wide ranging observations of gamma-ray line and neutron emission with detailed theoretical calculations of their expected production by accelerated ion interactions in the solar atmosphere has greatly advanced our understanding of solar flare acceleration, propagation and interaction. These comparisons produced the total number, energy spectrum and angular distribution of accelerated ions interacting in the solar atmosphere, their probability of escape, elemental abundances, etc. These calculations have been performed by developing a complex computer code of Monte Carlo programs. These calculations will now be expanded to include stochastic acceleration, which will permit study of the time dependent nature of ion acceleration and propagation in solar flares and the role of MHD turbulence in such processes.*** //