Impulsive magnetic reconnection in the earth's magnetotail and the solar corona

被引：112
|
作者：
Bhattacharjee, A [1 ]
机构：
[1] Univ New Hampshire, Inst Study Earth Ocean & Space, Ctr Magnet Reconnect Studies, Durham, NH 03824 USA
来源：
ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS | 2004年 / 42卷
关键词：
forced reconnection; resistive NM; Hall MHD; magnetotail substorms; solar flares;
D O I：
10.1146/annurev.astro.42.053102.134039
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Impulsive reconnection dynamics is characterized not only by fast growth but also by a sudden change in the time derivative of the growth rate. I review recent developments in the theory and simulation of forced impulsive reconnection based on the equations of resistive and Hall magnetohydrodynamics (MHD). Impulsive reconnection can be realized in resistive as well as Hall MHD by the imposition of suitable boundary conditions. However, compared with resistive MHD, Hall MHD reconnection is distinguished by qualitatively different magnetic field and electron and ion signatures in the reconnection layer. Furthermore, nonlinear reconnection rates in Hall MHD are weakly dependent on the Lundquist number. I discuss applications of the physics of impulsive reconnection to substorms in the Earth's magnetotail and solar flares.
引用
收藏
页码：365 / 384
页数：26
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