Particle acceleration and transport in the inner heliosphere

作     者：LI Gang 

作者机构：School of Geophysics and Information Technology China University of Geosciences (Beijing) Department of Space Science and CSPAR University of Alabama in Huntsville 

出 版 物：《Science China Earth Sciences》 (中国科学（地球科学英文版）)

年 卷 期：2017年第60卷第8期

页      面：1440-1465页

核心收录：

学科分类：07[理学] 0708[理学-地球物理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：supported in part by a guest professorship grant from the School of Geophysics and Information Technology  China University of Geosciences (Beijing) 

主　　题：粒子加速器 运输问题 日光层 日冕物质抛射 太阳耀斑 高能粒子 太阳风 冲击加速度 

摘      要：In the solar system, our Sun is Nature s most efficient particle accelerator. In large solar flares and fast coronal mass ejections(CMEs), protons and heavy ions can be accelerated to over ~GeV/nucleon. Large flares and fast CMEs often occur together. However there are clues that different acceleration mechanisms exist in these two processes. In solar flares, particles are accelerated at magnetic reconnection sites and stochastic acceleration likely dominates. In comparison, at CME-driven shocks,diffusive shock acceleration dominates. Besides solar flares and CMEs, which are transient events, acceleration of particles has also been observed in other places in the solar system, including the solar wind termination shock, planetary bow shocks, and shocks bounding the Corotation Interaction Regions(CIRs). Understanding how particles are accelerated in these places has been a central topic of space physics. However, because observations of energetic particles are often made at spacecraft near the Earth,propagation of energetic particles in the solar wind smears out many distinct features of the acceleration process. The propagation of a charged particle in the solar wind closely relates to the turbulent electric field and magnetic field of the solar wind through particle-wave interaction. A correct interpretation of the observations therefore requires a thorough understanding of the solar wind turbulence. Conversely, one can deduce properties of the solar wind turbulence from energetic particle observations. In this article I briefly review some of the current state of knowledge of particle acceleration and transport in the inner heliosphere and discuss a few topics which may bear the key features to further understand the problem of particle acceleration and transport.