Magnetic Reconnection for Coronal Conditions: Reconnection Rates, Secondary Islands and Onset

被引：46
作者：
Cassak, P. A. [1 ]
Shay, M. A. [2 ]
机构：
[1] W Virginia Univ, Dept Phys, Morgantown, WV 26506 USA
[2] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA
来源：
SPACE SCIENCE REVIEWS | 2012年 / 172卷 / 1-4期
基金：
美国国家科学基金会;
关键词：
Magnetic reconnection; Collisionless reconnection; Hall reconnection; Secondary Islands; Plasmoids; Solar corona; THIN CURRENT SHEETS; COLLISIONLESS RECONNECTION; KINK INSTABILITY; HALL CURRENT; EARTHS MAGNETOTAIL; M=1 RECONNECTION; DIFFUSION REGION; X-LINE; SOLAR; ELECTRON;
D O I：
10.1007/s11214-011-9755-2
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Magnetic reconnection may play an important role in heating the corona through a release of magnetic energy. An understanding of how reconnection proceeds can contribute to explaining the observed behavior. Here, recent theoretical work on magnetic reconnection for coronal conditions is reviewed. Topics include the rate that collisionless (Hall) reconnection proceeds, the conditions under which Hall reconnection begins, and the effect of secondary islands (plasmoids) both on the scaling and properties of collisional (Sweet-Parker) reconnection and on the onset of Hall reconnection. Applications to magnetic energy storage and release in the corona are discussed.
引用
收藏
页码：283 / 302
页数：20
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