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The stellar magnetic dynamo during the evolution across the main sequence

Published online by Cambridge University Press:  26 February 2010

Swetlana Hubrig
Swetlana Hubrig*
Affiliation:
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany email: shubrig@aip.de
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Abstract

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In comparison with stellar magnetic field studies in the eighties and nineties, where most effort was focused on A, B, and active solar-type stars, magnetic fields are currently directly measured in massive early B and O stars with radiative envelopes, as well as in the lower mass tail consisting of fully convective late-M dwarfs. Knowledge of the magnetic field topology of stars of different mass and at different evolutionary stages is important to understand the underlying magnetic field generation mechanisms. I review the present status of magnetic field studies along with the results of theoretical modeling.

Keywords

MHDinstabilitiestechniques: polarimetricbinaries: spectroscopicstars: chemically peculiarstars: evolutionstars: formationstars: magnetic fieldsstars: pre–main-sequencestars: spots
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. 171 - 180
Copyright
Copyright © International Astronomical Union 2010

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