Solar Flare Gamma Ray and Neutron Studies

对太阳耀斑的中子和伽马射线线发射的观测为太阳耀斑中的粒子加速和耀斑过程本身提供了重要的新信息。这些伽马射线和中子是由太阳大气中耀斑加速的质子和较重的离子与周围气体的核相互作用直接产生的。因此，它们提供了关于耀斑区域加速离子的总数、能谱、时间依赖性和角度分布的最直接信息，并可以提供关于太阳光球层尺度高度和3He/H比的独特新信息。1973年首次观测到伽玛射线发射，1983年观测到相对论性中子。这些观测刺激了通过耀斑粒子相互作用产生伽马射线线和中子的更广泛的理论计算，耀斑观测与这些计算的比较提供了许多重要的新信息。这项经费将用于研究这些一般的理论目标。特别是，PI将计算伽马射线线发射，以确定耀斑中粒子加速的时间依赖性。所有这些都是为了将理论与观测进行比较，以便缩小太阳耀斑候选模型的范围。

Observations of neutron and gamma-ray-line emission from solar flares are providing important new information on particle acceleration in solar flares and on the flare process itself. These gamma-rays and neutrons are produced directly by nuclear interactions of the flare-accelerated protons and heavier ions with ambient gas in the solar atmosphere. Thus they yield the most direct information available on the total number, energy spectrum, time dependence, and angular distribution of the accelerated ions in the flare region, and they can provide unique new information on both the scale height and the 3He/H ratio in the solar photosphere. Gamma ray line emission was first observed in 1973 and relativistic neutrons were observed in 1983. These observations have stimulated much more extensive theoretical calculations of gamma-ray line and neutron production by flare particle interactions and comparison of the flare observations with these calculations have provided much important new information. This grant will pursue these general theoretical objectives. In particular, the PI will calculate the gamma ray line emission with a view to determining the time dependence of particle acceleration in flares. All of this is with a view to comparing theory with observations in order to narrow the field of candidate models of solar flares.