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Convective zones in the envelope of massive stars

Published online by Cambridge University Press:  26 May 2016

Frank M. Alberts
Frank M. Alberts*
Affiliation:
Astronomical Institute ‘Anton Pannekoek’ and Center for High Energy Astrophysics University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, Netherlands

Extract

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In the calculation of stellar models with the Cox–Stewart opacities no convective zones in the outer layers of massive stars appear. The new OPAL opacities (Rogers & Iglesias, 1992) show a significant bump in the opacity near temperatures of log T = 5.2. This opacity effect results in a small convective zone in the envelope of stars with mass ranging from 15 M⊙ to 150 M⊙, apart from possible convective zones caused by ionization. This was also briefly mentioned by Glatzel & Kiriakidis (1993). For stars on the main sequence this zone is small, about 1% of its radius on the zero age main sequence up to 7% at the onset of the core helium burning and contains a negligible amount of mass. For helium burning stars, however, this convective zone moves inward, keeping the same size but containing more and more mass.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 67 - 68
Copyright
Copyright © Kluwer 1994 

References

Eggleton, P.P., 1971, MNRAS, 151, 351 CrossRefGoogle Scholar
Glatzel, W. and Kiriakidis, M., 1993, MNRAS, 262, 85 CrossRefGoogle Scholar
Rogers, F.J. and Iglesias, C.A., 1992, ApJS, 79, 507 CrossRefGoogle Scholar