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The evolution of Red Supergiants at very low metallicity

Published online by Cambridge University Press:  23 May 2013

J. H. Groh ,
G. Meynet ,
S. Ekström ,
P. Eggenberger ,
C. Georgy ,
A. Granada  and
S. Heap
J. H. Groh
Affiliation:
Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Versoix, Switzerland
G. Meynet
Affiliation:
Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Versoix, Switzerland
S. Ekström
Affiliation:
Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Versoix, Switzerland
P. Eggenberger
Affiliation:
Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Versoix, Switzerland
C. Georgy
Affiliation:
CRAL, ENS-Lyon, 46 allée d’Italie, 69364 Lyon Cedex 07, France
A. Granada
Affiliation:
Geneva Observatory, Geneva University, Chemin des Maillettes 51, 1290 Versoix, Switzerland
S. Heap
Affiliation:
Laboratory of Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
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Abstract

Red supergiants (RSG) are a crucial phase in the evolution of massive stars. At solar metallicity, they represent the stage where substantial amounts of mass and angular momentum are lost. Here we investigate the role of RSGs at very low metallicity. We have computed evolutionary tracks at Z=0.0004 with and without rotation, using the latest version of the Geneva stellar evolution code. Here, we briefly discuss the evolution of RSGs, their lifetimes, mass ranges for forming RSGs, maximum luminosity of RSGs, and how these are affected by rotation.

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