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Four open questions in massive star evolution

Published online by Cambridge University Press:  19 December 2013

G. Meynet ,
P. Eggenberger ,
S. Ekström ,
C. Georgy ,
J. Groh ,
A. Maeder ,
H. Saio  and
T. Moriya
G. Meynet
Affiliation:
Geneva Observatory, University of Geneva, 1290 Versoix, Switzerland
P. Eggenberger
Affiliation:
Geneva Observatory, University of Geneva, 1290 Versoix, Switzerland
S. Ekström
Affiliation:
Geneva Observatory, University of Geneva, 1290 Versoix, Switzerland
C. Georgy
Affiliation:
Astrophysics group, Lennard-Jones Laboratories, EPSAM, Keele University, Staffordshire, ST5 5BG, UK
J. Groh
Affiliation:
Geneva Observatory, University of Geneva, 1290 Versoix, Switzerland
A. Maeder
Affiliation:
Geneva Observatory, University of Geneva, 1290 Versoix, Switzerland
H. Saio
Affiliation:
Astronomical Institute, Graduate School of Science, Tohoku University, Sendai, Japan
T. Moriya
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, University of Tokyo, Kashiwanoha 5-1-5, Kashiwa, Chiba 277-8583, Japan
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Abstract

We discuss four questions dealing with massive star evolution. The first one is about the origin of slowly rotating, non-evolved, nitrogen rich stars. We propose that these stars may originate from initially fast rotating stars whose surface has been braked down. The second question is about the evolutionary status of α-Cygni variables. According to their pulsation properties, these stars should be post red supergiant stars. However, some stars at least present surface abundances indicating that they should be pre red supergiant stars. How to reconcile these two contradictory requirements? The third one concerns the various supernova types which are the end point of the evolution of stars with initial masses between 18 and 30M⊙, i.e. the most massive stars which go through a red supergiant phase during their lifetime. Do they produce types IIP, IIL, IIn, IIb or Ib supernovae or do they end without producing any SN event? Finally, we shall discuss reasons why so few progenitors of type Ibc supernovae have yet been detected?

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 63: New Advances in Stellar Physics: From Microscopic to Macroscopic Processes , 2013 , pp. 373 - 383
Copyright
© EAS, EDP Sciences, 2013

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