From solar and stellar flares to coronal heating: Theory and observations of how magnetic reconnection regulates coronal conditions

被引：43

作者：

Cassak, P. A. ^{[1
]}

Mullan, D. J. ^{[1
]}

Shay, M. A. ^{[1
]}

机构：

[1] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2008年 / 676卷 / 01期

关键词：

stars : activity; stars : coronae; stars : flare; Sun : activity; Sun : corona; Sun : flares;

D O I：

10.1086/587055

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

There is currently no explanation of why the corona has the temperature and density it has. We present a model that explains how the dynamics of magnetic reconnection regulates the conditions in the corona. A bifurcation in magnetic reconnection at a critical state enforces an upper bound on the coronal temperature for a given density. We present observational evidence from 107 flares in 37 Sun-like stars that stellar coronae are near this critical state. The model may be important to self-organized criticality models of the solar corona.

引用

页码：L69 / L72

页数：4