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Stellar mass ejections

Published online by Cambridge University Press:  01 September 2008

Moira Jardine ,
Jean-Francois Donati  and
Scott G. Gregory
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
Scott G. Gregory
Affiliation:
SUPA, School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, UK email: sg64@st-andrews.ac.uk
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Abstract

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It has been known for some time now that rapidly-rotating solar-like stars possess the stellar equivalent of solar prominences. These may be three orders of magnitude more massive than their solar counterparts, and their ejection from the star may form a significant contribution to the loss of angular momentum and mass in the stellar wind. In addition, their number and distribution provide valuable clues as to the structure of the stellar corona and hence to the nature of magnetic activity in other stars.

Until recently, these “slingshot prominences” had only been observed in mature stars, but their recent detection in an extremely young star suggests that they may be more widespread than previously thought. In this review we will summarise our current understanding of these stellar prominences, their ejection from their stars and their role in elucidating the (sometimes very non-solar) behaviour of stellar magnetic fields.

Keywords

stars:magnetic fieldsstars:coronaestars:imagingstars:spots
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 201 - 210
Copyright
Copyright © International Astronomical Union 2009

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