色球和冕层加热机制

The Heating Mechanisms in Chromosphere and Corona

简要回顾了近年来恒星色球和恒星冕层加热机制研究的一些重要成果和进展。恒星高层大气具有多种加热方式,在非磁区域和磁性区域的加热机制有所不同。主要讨论了稳定的恒星色球和冕层加热机制,包括传统的非磁区域的声波加热,磁性作用下的快慢磁声波加热,阿尔芬波加热,磁重联加热以及费米加热等。

The important achievements and progress of the heating mechanisms of the star chromospheres and coronae in recent years are briefly reviewed in this paper. Various kinds of mechanisms have been proposed to accomplish the heating processes in the start atmosphere, and there are different mechanisms in the regions with or without magnetic field. In the region without magnetic field, the main heating mecnanism is shock dissipationm from acoustic waves which generated by the motion of turbulent in photosphere. The energy carried by the slow and fast magnetoacoustic waves, Alfven wave is dissipated into heat in the region with magnetic field. The other heating mechanisms in the magnetic field region are magnetic reconnection which occurred with complex magnetic field structure, and the Fermi acceleration which heat the atmosphere in the low-beta coronal hole.