太阳大气的波动加热
Wave heating of the solar atmosphere.
作者信息
Arregui Iñigo
机构信息
Instituto de Astrofísica de Canarias, Vía Lactea s/n, La Laguna E-38205, Spain Departamento de Astrofísica, Universidad de La Laguna, La Laguna E-38206, Spain
出版信息
Philos Trans A Math Phys Eng Sci. 2015 May 28;373(2042). doi: 10.1098/rsta.2014.0261.
Magnetic waves are a relevant component in the dynamics of the solar atmosphere. Their significance has increased because of their potential as a remote diagnostic tool and their presumed contribution to plasma heating processes. We discuss our current understanding of coronal heating by magnetic waves, based on recent observational evidence and theoretical advances. The discussion starts with a selection of observational discoveries that have brought magnetic waves to the forefront of the coronal heating discussion. Then, our theoretical understanding of the nature and properties of the observed waves and the physical processes that have been proposed to explain observations are described. Particular attention is given to the sequence of processes that link observed wave characteristics with concealed energy transport, dissipation and heat conversion. We conclude with a commentary on how the combination of theory and observations should help us to understand and quantify magnetic wave heating of the solar atmosphere.
磁波是太阳大气动力学中的一个重要组成部分。由于其作为一种远程诊断工具的潜力以及对等离子体加热过程的假定贡献，其重要性日益增加。基于最近的观测证据和理论进展，我们讨论了目前对磁波日冕加热的理解。讨论首先从一系列观测发现开始，这些发现使磁波成为日冕加热讨论的前沿。然后，描述了我们对观测到的波的性质和特性以及为解释观测结果而提出的物理过程的理论理解。特别关注将观测到的波的特征与隐藏的能量传输、耗散和热转换联系起来的过程序列。最后，我们评论了理论与观测的结合应如何帮助我们理解和量化太阳大气的磁波加热。
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