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Abundance Anomalies and Rotation in Main Sequence OB Stars

Published online by Cambridge University Press:  26 May 2016

A. Herrero  and
D. J. Lennon
A. Herrero
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain Universidad de La Laguna, Departamento de Astrofísica, Avda. Astrofísico Francisco Sánchez, s/n, E-38071 La Laguna, Spain
D. J. Lennon
Affiliation:
Isaac Newton Group of Telescopes, Apartado de correos 321, E-38700, Santa Cruz de La Palma, Spain

Abstract

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We review the present status of our knowledge about observational evidence of the influence of rotation on the evolution and chemical surface enrichment of OB Main Sequence stars. We pay special attention to the CNO elements and show that luminosity class IV-V OB stars provide a good reference point for abundance analyses.

While there is clear evidence of rotationally induced mixing in OB stars, we show that fast rotation is not a guarantee of enrichment. A comparison of observed data with present evolutionary models indicates that the observed facts can be explained assuming that the stars are born with a distribution of rotational velocities, and that depending on the stellar mass the surface abundance changes will be dominated by rotation or mass loss. Only the existence of a large number of B supergiants beyond the Main Sequence cannot be explained in this scenario. We show that current evolutionary models including rotation do not adequately account for the transfer of angular momentum from the interior to the surface.

We point out that the difficulty in determining He abundances and in knowing the present or past binary status of many stars leads us to consider the above conclusions as preliminary.

Type
Session 2 Rotation in Relation with Abundances and Magnetic Fields
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 209 - 217
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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