Magnetism and Activity of the Sun and Stars
J. Arnaud and N. Meunier (eds)
EAS Publications Series, Vol. 9, 2003
DOI: 10.1051/eas:2003103
Stellar prominences and coronal magnetic fields
A.C. Cameron1, M. Jardine1, K. Wood1 and J.-F. Donati2
1
School of Physics and Astronomy,
University of St Andrews,
North Haugh,
St Andrews, Fife,
Scotland KY16 9SS, UK
2
Observatoire Midi-Pyrénées,
14 avenue Edouard Belin, 31400 Toulouse, France
Abstract
Rapidly rotating solar type stars display varying amounts of
chromospheric emission in their Balmer lines. The profiles of these
lines often display rapid variability. Since the mid-1980s,
high-cadence echelle spectroscopy of numerous such stars has revealed
that some of the variability is caused by concentrations of neutral
hydrogen, trapped in the stellar coronal magnetic field at distances
up to a few stellar radii from the rotation axis. In this paper we
review the observations and the tomographic techniques that can be
applied to mapping these "slingshot prominence" systems. We discuss
the possible mechanisms for formation and mechanical support of these
condensations, in the light of recent efforts to map 3-dimensional
stellar coronal magnetic fields and X-ray emission measure
distributions, with the help of Zeeman-Doppler imaging.
© EAS, EDP Sciences 2003
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