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Magnetic helicity ejections and coronal activity

Published online by Cambridge University Press:  18 July 2013

A. Nindos
A. Nindos*
Affiliation:
Section of Astrogeophysics, Physics Department, University of Ioannina, Ioannina GR-45110, Greece email: anindos@cc.uoi.gr
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Abstract

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Magnetic helicity quantifies the degree of linkage and/or twistedness in the magnetic field. It is probably the only physical quantity which is approximately conserved even in resistive MHD. This makes it an ideal tool for the exploration of the physics of solar eruptions. In this article, I discuss the sources of magnetic helicity injected into active regions and I point out that coronal mass ejections (CMEs) are probably necessary to remove at least part of the excess helicity produced in the Sun. I also discuss the importance of magnetic helicity in the overall coronal evolution that may lead to eruptions.

Keywords

Sun: activitySun: magnetic fieldsSun: coronal mass ejections (CMEs)Sun: flares
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S294: Solar and Astrophysical Dynamos and Magnetic Activity , August 2012 , pp. 519 - 530
Copyright
Copyright © International Astronomical Union 2013 

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