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The rotation of very low-mass stars and brown dwarfs

Published online by Cambridge University Press:  01 May 2007

Jochen Eislöffel  and
Alexander Scholz
Jochen Eislöffel
Affiliation:
Thüringer Landessternwarte, Sternwarte 5, D-07778 Tautenburg, Germany
Alexander Scholz
Affiliation:
SUPA, School of Physics & Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, United Kingdom
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Abstract

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The evolution of angular momentum is a key to our understanding of star formation and stellar evolution. The rotational evolution of solar-mass stars is mostly controlled by magnetic interaction with the circumstellar disc and angular momentum loss through stellar winds. Major differences in the internal structure of very low-mass stars and brown dwarfs – they are believed to be fully convective throughout their lives, and thus should not operate a solar-type dynamo – may lead to major differences in the rotation and activity of these objects. Here, we report on observational studies to understand the rotational evolution of the very low-mass stars and brown dwarfs.

Keywords

Stars: activitystars: evolutionstars: formationstars: low-massbrown dwarfsstars: magnetic fieldsstars: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 241 - 248
Copyright
Copyright © International Astronomical Union 2007

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