Collaborative Research: Turbulence and Particle Acceleration in Solar Flares

本文将研究由磁重联引起的磁流体动力学湍流的演化，并随后用于评估高能粒子在太阳耀斑中的输运和加速。湍流能量从大尺度到小尺度的级联及其通过粒子的加热和加速而产生的耗散阻尼决定了等离子体波动的演化。电子和质子的输运系数从耦合到涨落，进入描述超热粒子能谱和俯仰角分布的Fokker-Planck方程。将这些结果结合到一个耦合且自洽的太阳耀斑模型中，将提供具体的预测，可以针对地面和太空观测进行测试。

The evolution of magnetohydrodynamic turbulence resulting from magnetic reconnection will be investigated, and subsequently employed to evaluate the transport and acceleration of energetic particles in solar flares. The cascade of turbulent energy from large to small scales and its dissipative damping through the heating and acceleration of particles determine the evolution of the plasma fluctuations. The transport coefficients for the electrons and protons follow from the coupling to the fluctuations, and enter into a Fokker-Planck equation describing the energy spectrum and pitch-angle distribution of the superthermal particles. Incorporation of these results into a coupled and self-consistent solar flare model will provide specific predictions that can be tested against ground, and space-based observations.