发表机构
NASA Goddard Space Flight Center; SUPA School of Physics and Astronomy, University of Glasgow; Department of Physics, Catholic University of America; Department of Physics, American University; Astronomy Department, University of Maryland; Institute for Research in Electronics and Applied Physics, University of Maryland; Heliophysics and Planetary Science Branch, NASA Marshall Space Flight Center（美国国家航空航天局戈达德太空飞行中心; 苏格兰大学物理与天文学学院，格拉斯哥大学; 天主教大学物理系; 美国大学物理系; 马里兰大学天文系; 马里兰大学电子与应用物理研究所; 美国国家航空航天局马歇尔太空飞行中心日地物理学与行星科学处）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出一个连接ARMS、kglobal和RADYN+FP三个模型的综合框架，用于模拟太阳耀斑从触发、粒子加速到大气加热的全过程，并首次在同一环中追踪非热电子和质子，为构建全三维耀斑模型奠定基础。
AI 中文摘要
太阳耀斑中的物理过程跨越了时空尺度上的多个数量级，因此，一个能够解释所有相关过程的统一模型在计算上仍然难以实现。相反，人们开发了专门的代码，针对特定领域来解决太阳耀斑问题的特定方面。在此，我们提出了一个综合框架，该框架将三个模型联系起来，以捕捉耀斑的触发和能量释放、随后的粒子加速、这些粒子的传播和热化，以及最终对太阳低层大气的加热。我们使用2.5D ARMS磁流体动力学（MHD）代码来模拟活动区中磁场的应力积累、电流片的形成、磁重联以及新形成的耀斑环的演化。我们利用ARMS电流片中的条件来初始化kglobal模型，该模型预测随时间变化的非热电子和质子分布。最后，我们使用RADYN+FP将这些分布注入到新重连的ARMS环中，并计算随后的粒子输运、大气加热和辐射发射。这是首次详细介绍在同一环中追踪非热电子和质子的RADYN+FP模拟。除了讨论其中发生的有趣物理过程外，我们还注意到这如何导致与观测一致的耀斑白光发射高度。这项工作朝着构建完全三维的耀斑建模框架迈出了第一步。
英文摘要
Physical processes in solar flares span many orders of magnitude in spatiotemporal scales, so a single unified model accounting for all relevant processes remains computationally intractable. Instead, specialized codes have been developed, targeting specific domains that tackle specific aspects of the solar flare problem. Here, we present a comprehensive framework that links three models to capture flare initiation and energy release, the subsequent particle acceleration, the propagation and thermalization of those particles, and ultimately the heating of the lower solar atmosphere. We use the 2.5D ARMS magnetohydrodynamics (MHD) code to model stressing of the magnetic field in a simulated active region, the formation of a current sheet, magnetic reconnection, and the evolution of newly formed flare loops. We use the conditions in the ARMS' current sheet to initialize the kglobal model, which predicts time-dependent nonthermal electron and proton distributions. Finally, we use RADYN+FP to inject these distributions into a newly reconnected ARMS loop and compute subsequent particle transport, atmospheric heating, and radiative emissions. This is the first detailed presentation of a RADYN+FP simulation tracking nonthermal electrons and protons in the same loop. As well as discussing the interesting physics that takes place, we note how this results in white-light flare emission height consistent with observations. This work is a first step toward building a fully 3D flare modeling framework.
Comments21 pages, 12 figures, accepted for publication by Astrophysical Journal
