Particle Acceleration in Solar Flares

这个项目将研究太阳耀斑中的粒子加速。太阳耀斑物理学中的一个关键问题是质子和其他粒子在几秒钟内被加速到几十兆电子伏的方式，这是脉冲>射线发射所证明的。这个过程被称为第一相离子加速。在解释这种加速度时，最广泛接受的模型是激波加速度和阿尔芬波或磁声波的随机加速度。这两种模型都不是自洽的，也没有直接的观测验证。本项目探讨了单环大气水动力（MHD）波浪随机加速模型的一致性发展。半环被分成两个日冕部分，分别与色球球和光球球模型相连。日冕部分包括时间相关加速（包括波粒和波波相互作用）发生的源，以及质子扩散传播的输运部分。与以前的工作不同，它将是一个完整的非相对论能量模型，包括核相互作用的计算。因此，将有可能研究在整个环路中改变源中湍流的频谱和/或功率、环路尺寸等的影响。简而言之，我们将能够对随机加速度模型进行非常彻底的测试。即时>射线发射的观测结果来自计算的核相互作用部分。这些结果将增加我们对太阳研究这一重要领域的了解。＃

This project will study particle acceleration in solar flares. A key problem in solar flare physics is the manner in which protons and other particles are accelerated to several tens of MeV in a few seconds as evidenced by impulsive >-ray emission. This process is called first-phase ion acceleration. The most widely accepted models in explaining this acceleration are shock acceleration and stochastic acceleration by Alfven or magnetosonic waves. Neither of these models has been developed self-consistently or has direct observational verification. This project examines the consistent development of a single-loop manetohydrodynamic (MHD) wave stochastic acceleration model. A half-loop is divided into 2 coronal sections attached to a model chromosphere and photosphere. The coronal sections include the source where time-dependent acceleration including wave-particle and wave-wave interactions occurs, and a transport section in which protons propagate diffusively. Unlike previous work, it will be a complete model for nonrelativistic energies including a nuclear interaction calculation. Thus, it will be possible to study the effect of changing the spectrum and/or power of turbulence in the source, the loop size, etc., throughout the whole loop. In short, we shall be able to put the stochastic acceleration model to a very thorough test. Observational consequences in prompt >-ray emission come from the nuclear interaction part of the calculation. These results will increase our understanding in this important area of solar research. #