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Testing convective mixing in massive stars

Published online by Cambridge University Press:  26 May 2016

Mounib F. El Eid  and
Philip J. Flower
Mounib F. El Eid
Affiliation:
Department of Physics, American University of Beirut, P.O. Box 11-236, Beirut, Lebanon
Philip J. Flower
Affiliation:
Department of Physics and Astronomy, Clemson University, Clemson, SC 29634-1911, USA

Abstract

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Stellar evolution sequences are presented for stars in the mass range 5-21 M⊙ with initial metallicity Z = 0.002 and initial helium abundance Y = 0.25 resembling average composition of the Small Magellanic Cloud. The stellar models are calculated with different treatment of convective mixing in regions of varying molecular weight gradient. The stellar sequences are used to study the morphology of the well-observed star cluster NGC 330 in the SMC. We argue that convective mixing should be inhibited in inhomogeneous stellar regions in order to understand the morphology of NGC 330. In other words, our contribution emphasizes the important role of semi-convection in the evolution of massive stars.

Type
Part 2. Interiors of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 291 - 295
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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