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Magnetic activity, high-energy radiation and variability: from young solar analogs to low-mass objects

Published online by Cambridge University Press:  26 February 2010

Manuel Güdel
Manuel Güdel*
Affiliation:
Institute of Astronomy, ETH Zurich, 8093 Zurich, Switzerland email: guedel@pastro.phys.ethz.ch
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Abstract

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Magnetic activity on cool stars expresses itself in a bewildering variety of radiative and particle output originating from magnetic regions between the photosphere and the corona. Given its origin in evolving magnetic fields, most of this output is variable in time. Radiation in the ultraviolet, the extreme ultraviolet, and the X-ray ranges are important for heating and ionizing upper planetary atmospheres and thus driving atmospheric evaporation. Additionally, stellar winds interact with the upper atmospheres and may lead to further erosion. The stellar high-energy output is therefore a prime factor in determining habitability of planets. We summarize our knowledge of magnetic activity in young solar analogs and lower-mass stars and show how the stellar output changes on evolutionary timescales.

Keywords

Sun: evolutionstars: activitystars: evolutionstars: flarestars: rotationstars: magnetic fieldsstars: windsastrobiology
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S264: Solar and Stellar Variability: Impact on Earth and Planets , August 2009 , pp. 375 - 384
Copyright
Copyright © International Astronomical Union 2010

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