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Magnetic coronae of active main-sequence stars

Published online by Cambridge University Press:  01 November 2008

Moira Jardine  and
Jean-Francois Donati
Moira Jardine
Affiliation:
SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, UK email: mmj@st-andrews.ac.uk
Jean-Francois Donati
Affiliation:
LATT, CNRS–UMR 5572, Obs. Midi-Pyrénées, 14 Av. E. Belin, F-31400 Toulouse, France email: donati@ast.obs-mip.fr
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Abstract

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The coronal structure of main sequence stars continues to puzzle us. While the solar corona is relatively well understood, it has become clear that even stars of the same mass as the Sun can display very non-solar coronal behaviour, particularly if they are rapid rotators or in a binary system. At masses greater than and also less than that of the Sun, the non-solar internal structure appears to affect both the geometry and dynamics of the stellar corona and the nature of the X-ray and radio emission. In this talk I will describe some recent advances in our understanding of the structure of the coronae of some of the most active (and interesting) main sequence stars.

Keywords

Stars: magnetic fields – stars: coronae – stars: imaging – stars: spots
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S259: Cosmic Magnetic Fields: From Planets, to Stars and Galaxies , November 2008 , pp. 357 - 362
Copyright
Copyright © International Astronomical Union 2009

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