On magnetic reconnection and flux rope topology in solar flux emergence

Mactaggart, D. and Haynes, A. L. (2014) On magnetic reconnection and flux rope topology in solar flux emergence. Monthly Notices of the Royal Astronomical Society, 438(2), pp. 1500-1506. (doi: 10.1093/mnras/stt2285)

Full text not currently available from Enlighten.

Publisher's URL: http://dx.doi.org/10.1093/mnras/stt2285


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.

Item Type:Articles
Glasgow Author(s) Enlighten ID:Mactaggart, Dr David
Authors: Mactaggart, D., and Haynes, A. L.
College/School:College of Science and Engineering > School of Mathematics and Statistics > Mathematics
Journal Name:Monthly Notices of the Royal Astronomical Society
Publisher:Wiley-Blackwell Publishing Ltd.
ISSN (Online):1365-2966
Related URLs:

University Staff: Request a correction | Enlighten Editors: Update this record