The past and future evolution of a star like Betelgeuse (original) (raw)

Issue EAS Publications Series Volume 60, 2013 Betelgeuse Workshop 2012 The Physics of Red Supergiants: Recent Advances and Open Questions
Page(s) 17 - 28
Section Introduction
DOI https://doi.org/10.1051/eas/1360002
Published online 23 May 2013

Betelgeuse Workshop 2012
P. Kervella, T. Le Bertre and G. Perrin (eds)
EAS Publications Series, 60 (2013) 17-28

1 Geneva Observatory, University of Geneva, 1290 Versoix, Switzerland
2 ENS, Lyon, France

Abstract

We discuss the physics and the evolution of a typical massive star passing through an evolutionary stage similar to that of Betelgeuse. After a brief introduction recalling various observed parameters of Betelgeuse, we discuss the Pre-Main-Sequence phase (PMS), the Main-Sequence (MS) phase, the physics governing the duration of the first crossing of the HR diagram, the red supergiant stage (RSG), the post-red supergiant phases and the final fate of solar metallicity stars with masses between 9 and 25 _M_⊙. We examine the impact of different initial rotation and of various prescriptions for the mass loss rates during the red supergiant phase. We show that, whatever the initial rotation rate (chosen between 0 and 0.7 × _υ_crit, _υ_crit being the surface equatorial velocity producing a centrifugal acceleration balancing exactly the gravity) and the mass loss rates during the RSG stage (varied between a standard value and 25 times that value), a 15 _M_⊙ star always ends its lifetime as a RSG and explodes as a type II-P or II-L supernova.

© EAS, EDP Sciences 2013

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