Particle Acceleration in Solar Flares

该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 其他粒子在几分钟内被加速到几十MeV， 脉冲射线发射证实了这一点。这个过程是 称为第一阶段离子加速。最广泛接受的 解释这种加速度的模型是冲击加速度， 阿尔文波或磁声波的随机加速。都不 这些模型是自洽开发的，或者直接 观测验证这个项目检查了一致的 一个单圈Manetohydrodynamic（MHD）波的发展 随机加速度模型一个半循环分为2个 日冕切片连接到一个模型色球和光球。 日冕部分包括源， 包括波粒和波波相互作用的加速度 发生，并且质子在其中传播的传输部分 扩散。与以前的工作不同，它将是一个完整的模型， 包括核相互作用的非相对论能量 计算.因此，将有可能研究 改变源中湍流的频谱和/或功率， 循环大小等，在整个循环中。简而言之， 能够把随机加速度模型， test.瞬发>-射线发射的观测结果来自于 计算的核相互作用部分。这些结果将 增加我们对太阳能这一重要领域的了解 research. #

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. #