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Connecting a Star’s Convection Zone with its Corona

Published online by Cambridge University Press:  25 April 2016

D. J. Galloway  and
C. A. Jones
D. J. Galloway
Affiliation:
School of Mathematics and Statistics, University of Sydney, NSW 2006, Australia. galloway_d@maths.usyd.edu.au
C. A. Jones
Affiliation:
Department of Mathematics, University of Exeter, EX4 4QE, UK
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Abstract

This paper discusses problems which have as their uniting theme the need to understand the coupling between a stellar convection zone and a magnetically dominated corona above it. Interest is concentrated on how the convection drives the atmosphere above, loading it with the currents that give rise to flares and other forms of coronal activity. The role of boundary conditions appears to be crucial, suggesting that a global understanding of the magnetic field system is necessary to explain what is observed in the corona. Calculations are presented which suggest that currents flowing up a flux rope return not in the immediate vicinity of the rope but rather in an alternative flux concentration located some distance away.

Keywords

convection — magnetic fields — starscoronae — Sunsunspots — flares
Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 12 , Issue 2 , August 1995 , pp. 180 - 185
Copyright
Copyright © Astronomical Society of Australia 1995

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