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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 

References

Alef, W., Benz, A. O., & Güdel, M. 1997, A&A, 317, 707Google Scholar
Barnes, J. R., Collier Cameron, A., Unruh, Y. C., Donati, J. F., & Hussain, G. A. J. 1998, MNRAS, 299, 904Google Scholar
Brickhouse, N. S., Dupree, A. K., & Young, P. R. 2001, ApJ, 562, L75CrossRefGoogle Scholar
Byrne, P. B., Eibe, M. T., & Rolleston, W. R. J. 1996, A&A, 311, 651Google Scholar
Collier Cameron, A. & Robinson, R. D. 1989, MNRAS, 236, 57Google Scholar
Donati, J.-F. & Collier Cameron, A. 1997, MNRAS, 291, 658CrossRefGoogle Scholar
Donati, J.-F., Collier Cameron, A., Hussain, G. A. J., & Semel, M. 1999, MNRAS, 302, 437Google Scholar
Dunstone, N. J. 2008, PhD thesis, University of St Andrews, UKGoogle Scholar
Dunstone, N. J., Collier Cameron, A., Barnes, J. R., & Jardine, M. 2006, MNRAS, 373, 1308CrossRefGoogle Scholar
Gabriel, A. H. & Jordan, C. 1969, MNRAS, 145, 241Google Scholar
Huenemoerder, D. P., Testa, P., & Buzasi, D. L. 2006, 650, 1119Google Scholar
Hussain, G. A. J., Donati, J.-F., Collier Cameron, A., & Barnes, J. R. 2000, MNRAS, 318, 961Google Scholar
Hussain, G. A. J., Jardine, M., Donati, J.-F., Brickhouse, N. S., Dunstone, N. J., Wood, K., Dupree, A. K., Collier Cameron, A., & Favata, F. 2007, MNRAS, 377, 1488Google Scholar
Jardine, M. & van Ballegooijen, A. A. 2005, MNRAS, 361, 1173Google Scholar
Jeffries, R. D. 1993, MNRAS, 262, 369CrossRefGoogle Scholar
Kochukhov, O., Mantere, M. J., Hackman, T., & Ilyin, I. 2013, A&A, 550, 84Google Scholar
Leitzinger, M., Odert, P., Ribas, I., Hanslmeier, A., Lammer, H., Khodachenko, M. L., Zaqarashvalli, T. V., & Rucker, H. O. 2011, A&A, 536, A62Google Scholar
Maehara, H., Shibayama, T., Notsu, S., Notsu, Y., Nagao, T., Kusaba, S., Honda, S., & Nogami, D., Shibata, K. 2012, Nature, 485, 478Google Scholar
Mullan, D. J., Mathioudakis, M., Bloomfield, D. S., & Christian, D. J. 2006, ApJS, 164, 173Google Scholar
Ness, J.-U., Güdel, M., Schmitt, J. H. M. M., Audard, M., & Telleschi, A. 2004, A&A, 427, 667Google Scholar
Semel, M. 1989, A&A, 225, 456Google Scholar
Schmitt, J. H. M. M. & Favata, F. 1999, Nature, 401, 44Google Scholar
Testa, P., Drake, J. J., & Peres, G. 2004, ApJ, 617, 508Google Scholar
Walter, F. M. 2004, AN, 325, 241Google Scholar