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Effects of rotation and magnetic fields on the structure and surface abundances of solar-type stars

Published online by Cambridge University Press:  23 April 2010

P. Eggenberger ,
A. Maeder  and
G. Meynet
P. Eggenberger
Affiliation:
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, CH-1290 Versoix, Suisse email: patrick.eggenberger@unige.ch; andre.maeder@unige.ch; georges.meynet@unige.ch
A. Maeder
Affiliation:
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, CH-1290 Versoix, Suisse email: patrick.eggenberger@unige.ch; andre.maeder@unige.ch; georges.meynet@unige.ch
G. Meynet
Affiliation:
Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, CH-1290 Versoix, Suisse email: patrick.eggenberger@unige.ch; andre.maeder@unige.ch; georges.meynet@unige.ch
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Abstract

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The effects of shellular rotation on the modelling of solar-type stars (in particular internal structure, evolutionary tracks in the HR diagram, lifetimes and surface abundances) are first examined. Then the effects of a dynamo possibly occuring in the internal stellar radiative zone by imposing nearly solid body rotation are studied. These results are finally discussed in the context of the rotational history of exoplanet host stars and the link between lithium depletion and the presence of exoplanets.

Keywords

Stars: rotationmagnetic fieldsinteriorsabundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 381 - 386
Copyright
Copyright © International Astronomical Union 2010

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