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Magnetic helicity of solar active regions

Published online by Cambridge University Press:  01 September 2008

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 is a quantity that describes the linkage and twistedness/shear in the magnetic field. It has the unique feature that it is probably the only physical quantity which is approximately conserved even in resistive MHD. This makes magnetic helicity an ideal tool for the exploration of the physics of eruptive events. The concept of magnetic helicity can be used to monitor the whole history of a CME event from the emergence of twisted magnetic flux from the convective zone to the eruption and propagation of the CME into interplanetary space. In this article, I discuss the sources of the magnetic helicity injected into active regions and the role of magnetic helicity in the initiation of solar eruptions.

Keywords

Sun: activitySun: magnetic fieldsSun: coronal mass ejections (CMEs)Sun: flares
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 133 - 143
Copyright
Copyright © International Astronomical Union 2009

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