On magnetic reconnection and flux rope topology in solar flux emergence |
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David MacTaggart Submitted: 2013-11-26 05:39
We present an analysis of the formation of atmospheric
flux ropes in a magnetohydro-dynamic (MHD) 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 (CME), we discuss the implications of our ndings for solar
eruptions.
Authors: D. MacTaggart, A.L. Haynes
Projects: None
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Publication Status: MNRAS, Submitted
Last Modified: 2013-11-26 05:41
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