On magnetic reconnection and flux rope topology in solar flux emergence

被引：24

作者：

MacTaggart, D. ^{[1
]}

Haynes, A. L. ^{[2
]}

机构：

[1] Univ Abertay Dundee, Dundee DD1 1HG, Scotland

[2] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2014年 / 438卷 / 02期

关键词：

magnetic fields; magnetic reconnection; MHD; Sun: coronal mass ejections (CMEs); Sun: magnetic topology; CORONAL MASS EJECTIONS; MODEL; SIMULATIONS; MECHANISM; ERUPTIONS; INSTABILITY; ATMOSPHERE; HELICITY; BREAKOUT; ENERGY;

D O I：

10.1093/mnras/stt2285

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present an analysis of the formation of atmospheric flux ropes in a magnetohydrodynamic solar flux emergence simulation. The simulation domain ranges from the top of the solar interior to the low corona. A twisted magnetic flux tube emerges from the solar interior and into the atmosphere where it interacts with the ambient magnetic field. By studying the connectivity of the evolving magnetic field, we are able to better understand the process of flux rope formation in the solar atmosphere. In the simulation, two flux ropes are produced as a result of flux emergence. Each has a different evolution resulting in different topological structures. These are determined by plasma flows and magnetic reconnection. As the flux rope is the basic structure of the coronal mass ejection, we discuss the implications of our findings for solar eruptions.

引用

页码：1500 / 1506

页数：7

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