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On magnetic reconnection and flux rope topology in solar flux emergence View all abstracts by submitter

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 fi eld, 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 diff erent evolution resulting in di fferent 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

Publication Status: MNRAS, Submitted
Last Modified: 2013-11-26 05:41
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