期刊文献+

色球和冕层加热机制 被引量:1

The Heating Mechanisms in Chromosphere and Corona
下载PDF
导出
摘要 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.
出处 《天文学进展》 CSCD 北大核心 2011年第3期241-259,243-259,共19页 Progress In Astronomy
关键词 声波 磁声波 阿尔芬波 磁重联 费米加热 acoustic wave magnetoacoustic wave alfven wave reconnection fermi acceleration
  • 相关文献

参考文献1

二级参考文献2

  • 1涂传诒,Sol Phys,1997年
  • 2涂传诒,Observations Theor,1995年,1页

共引文献1

同被引文献1

引证文献1

二级引证文献1

相关作者

内容加载中请稍等...

相关机构

内容加载中请稍等...

相关主题

内容加载中请稍等...

浏览历史

内容加载中请稍等...
;
使用帮助 返回顶部