太阳射电微波爆发及其精细结构研究进展  

Progress of Solar Radio Microwave Bursts and Fine Structures

作　　者：李舒浩[1] 王蜀娟[2] 钟晓春[1] 

机构地区：[1]西南交通大学理学院物理系,成都610031 [2]中国科学院国家天文台,北京100012

出　　处：《天文学进展》2005年第4期331-345,共15页Progress In Astronomy

基　　金：国家自然科学基金(10333030;10225313)国家973资助项目(G2000078403)

摘　　要：太阳射电微波爆发携带着爆发源区的物理环境及辐射机制等诸多重要信息。其辐射频段较高，通常来自低日冕磁重联区，尤其是微波爆发的精细结构，持续时间短、变化快、结构复杂，可以反映重联过程复杂的磁场结构、高能粒子运动等许多特征。综述了太阳微波射电爆发分类研究的3个主要阶段，介绍了每一阶段的重要爆发类型、物理机制研究及相应的观测设备，讨论了进一步研究的方向。The complicated radio spectrum detected in solar radio bursts contain a lot of important information on their source regions including physical environment and emission mechanisms. The emission of the microwave bursts is in higher frequency range （GHz） and often came from the magnetic reconnection region in lower corona. Especially, because of their morphologic features of short duration, rapid frequency drift, complicated types and so on, the microwave fine structures could bring out rich information on the source regions such as the complicated configuration of magnetic reconnection, the movement of energetic particle, etc. In this paper, three main stages of researches on the solar microwave bursts and the fine structures are reviewed. The main burst types, the mechanism researches and the observational instrument for each stage are summarized. The future proposals are discussed as well.

关 键 词：天体物理学 微波爆发 综述 太阳耀斑 辐射机制 

分 类 号：P182.24[天文地球—天文学]