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Observations of stellar coronae and prominences

Published online by Cambridge University Press:  06 January 2014

Gaitee A. J. Hussain
Gaitee A. J. Hussain*
Affiliation:
ESO, Karl-Schwarzschild-Strasse 2, D-85748, Garching bei MünchenGermany email: ghussain@eso.org
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Abstract

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X-ray and EUV observations of young cool stars have shown that their coronae are extremely pressured environments with temperatures and densities that are up to two orders of magnitudes larger than those observed in the solar corona. At the same time rapidly transiting absorption features in optical and UV spectra reveal the presence of large cool, prominence-type complexes that can extend several stellar radii. I will give an overview of our current understanding of coronal structures in cool stars from multi-wavelength observations, detailing their properties and apparent dependence on spectral type. I will also outline future prospects in this field, particularly from observations of stellar coronal environments at radio and sub-mm wavelengths.

Keywords

stars: activitystars: coronaestars: circumstellar matterstars: magnetic fieldsX-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 309 - 317
Copyright
Copyright © International Astronomical Union 2013 

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