Solar Flare Gamma Ray and Neutron Studies

太阳中子和γ射线谱线发射的观测 耀斑提供了关于粒子的重要新信息 加速太阳耀斑和耀斑过程本身。 这些 伽马射线和中子是由核相互作用直接产生的 耀斑加速的质子和较重的离子与周围的气体， 太阳大气层。 因此，它们提供了最直接的信息 可用的总数，能谱，时间依赖性，和 耀斑区域中加速离子的角分布，以及 它们可以提供有关刻度高度和 太阳光球层中的3 He/H比值。 伽马射线线发射在1973年首次被观测到， 相对论中子在1983年被观测到。 这些观测 激发了更广泛的伽马射线理论计算 耀斑粒子相互作用产生的中子和中子， 将耀斑观测结果与这些计算结果进行了比较， 提供了许多重要的新信息。 这项赠款将追求这些一般的理论目标。 在 特别是，PI将计算伽马射线线发射， 考虑到确定粒子加速度的时间依赖性， 照明弹 所有这些都是为了将理论与 为了缩小候选模型的领域， 太阳耀斑

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.