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Rapid rotation and mixing in active OB stars – Physical processes

Published online by Cambridge University Press:  12 July 2011

Jean-Paul Zahn
Jean-Paul Zahn*
Affiliation:
LUTH, Observatoire de Paris, CNRS UMR 8102, Université Paris Diderot 5 place Jules Janssen, 92195 Meudon, France email: [email protected]
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Abstract

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In the standard description of stellar interiors, O and B stars possess a thoroughly mixed convective core surrounded by a stable radiative envelope in which no mixing occurs. But as is well known, this model disagrees strongly with the spectroscopic diagnostic of these stars, which reveals the presence at their surface of chemical elements that have been synthesized in the core. Hence the radiation zone must be the seat of some mild mixing mechanisms. The most likely to operate there are linked with the rotation: these are the shear instabilites triggered by the differential rotation, and the meridional circulation caused by the changes in the rotation profile accompanying the non-homologous evolution of the star. In addition to these hydrodynamical processes, magnetic stresses may play an important role in active stars, which host a magnetic field. These physical processes will be critically examined, together with some others that have been suggested.

Keywords

stars: early-typestars: interiorsstars: magnetic fieldsstars: rotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 14 - 25
Copyright
Copyright © International Astronomical Union 2011

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