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Nucleosynthesis in exploding massive Wolf-Rayet stars

Published online by Cambridge University Press:  12 April 2016

M.F. El Eid  and
N. Langer
M.F. El Eid
Affiliation:
Universitäts-Sternwarte Göttingen, Geismarlandstraße 11 D–3400 Göttingen, F.R.G.
N. Langer
Affiliation:
Universitäts-Sternwarte Göttingen, Geismarlandstraße 11 D–3400 Göttingen, F.R.G.

Extract

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Recent observations of the young supernova remnant Cas A (Fesen et al., 1987) suggest an exploding Wolf-Rayet (WR) star of WNL type as a progenitor of this object. The majority of the WR stars seems to originate from massive O-stars of M > 40 M⊙. According to current investigations (Schild and Maeder, 1984; Langer, 1987; cf. also: Langer, this volume) WNL stars rank among the most massive WR stars. Hence, it is possible to assume that the stellar progenitor of Cas A was indeed a very massive star.

As shown by Langer and El Eid (1986), (see also Woosley, 1986) a population I star of initially 100 M⊙ may loose enough mass during its evolution up to core He exhaustion to become a WN star of ∼ 45 M⊙, which then mainly consists of oxygen (more than 80%) synthesized during He burning.

Type
Part III. Chemical and Dynamical Structures of Exploding Stars
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 440 - 441
Copyright
Copyright © Springer-Verlag 1988

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