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Magnetic Instabilities in Stellar Atmospheres

Published online by Cambridge University Press:  12 April 2016

E.R. Priest
E.R. Priest*
Affiliation:
Applied Mathematics Department, The University, St.Andrews, Scotland

Abstract.

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The extensive theory for magnetohydrodynamic instability of a flux tube is briefly reviewed, together with its application to tokamaks and solar flares. In a star a single coronal loop whose footprints are anchored in the dense photosphere may become unstable to the kink instability when it is twisted too much. Magnetic arcades may also be subject to an eruptive instability when they are sheared too much. After the eruption the magnetic field closes back down by reconnection and continues to heat the plasma long after the impulsive phase. Global instability of a large part of the coronal magnetic field is also possible when the stored energy is too great.

Type
Session IV: Theoretical Aspects
Information
International Astronomical Union Colloquium , Volume 71: Activity in Red-Dwarf Stars , 1983 , pp. 545 - 558
Copyright
Copyright © Reidel 1983

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