Particle Acceleration by Magnetic Reconnection in Impulsive and Gradual Solar Flares

研究人员将确定在各种磁场重联几何结构中加速的测试粒子的能量分布。这将通过将粒子运动方程积分到特定的磁流体动力学方程的解析和数值解中来实现。根据这些详细的计算，将得出太阳高能粒子(SEP)事件的标度定律，并随后与高能太阳光谱成像仪(HESI)卫星的观测结果进行比较。这项工作的主要目标是开发一个可测试的模型，能够解释不同的重联配置如何以及为什么产生不同的加速机制，从瞬发电子加速到伽马射线能量，从质子加速到大型渐变耀斑中的GeV能量。这项工作承诺为SEP事件提供关键的新见解，SEP事件是空间天气的一个重要组成部分。

The investigators will determine the energy distribution of test particles accelerated in various magnetic field reconnection geometries. This will be achieved by integrating the particle equations of motion in specified analytic and numerical solutions of the magnetohydrodynamic equations. From these detailed computations, scaling laws for solar energetic particle (SEP) events will be derived, and subsequently compared with observations from the High Energy Solar Spectroscopic Imager (HESSI) satellite. The major goal of this effort is to develop a testable model capable of explaining how and why different reconnection configurations produce different acceleration regimes, ranging from prompt electron acceleration to gamma-ray energies to proton acceleration to GeV energies in large gradual flares. This work promises to provide critical new insight on to SEP events, which are a prominent component of Space Weather.