Hostname: page-component-cd9895bd7-jkksz Total loading time: 0 Render date: 2024-12-27T11:47:49.567Z Has data issue: false hasContentIssue false
  • English
  • Français

Stellar prominences and coronal magnetic fields

Published online by Cambridge University Press:  17 November 2003

J. Arnaud ,
N. Meunier ,
A. C. Cameron ,
M. Jardine ,
K. Wood  and
J.-F. Donati
A. C. Cameron
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife, Scotland KY16 9SS, UK
M. Jardine
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife, Scotland KY16 9SS, UK
K. Wood
Affiliation:
School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife, Scotland KY16 9SS, UK
J.-F. Donati
Affiliation:
Observatoire Midi-Pyrénées, 14 avenue Edouard Belin, 31400 Toulouse, France
Get access

Abstract

Rapidly rotating solar type stars display varying amounts ofchromospheric emission in their Balmer lines. The profiles of theselines often display rapid variability. Since the mid-1980s,high-cadence echelle spectroscopy of numerous such stars has revealedthat some of the variability is caused by concentrations of neutralhydrogen, trapped in the stellar coronal magnetic field at distancesup to a few stellar radii from the rotation axis. In this paper wereview the observations and the tomographic techniques that can beapplied to mapping these "slingshot prominence" systems. We discussthe possible mechanisms for formation and mechanical support of thesecondensations, in the light of recent efforts to map 3-dimensionalstellar coronal magnetic fields and X-ray emission measuredistributions, with the help of Zeeman-Doppler imaging.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 9: Magnetism and Activity of the Sun and Stars , 2003 , pp. 217
Copyright
© EAS, EDP Sciences, 2003

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)