Hostname: page-component-745bb68f8f-v2bm5 Total loading time: 0 Render date: 2025-01-13T05:42:45.076Z Has data issue: false hasContentIssue false
  • English
  • Français

Stellar evolution with SMC chemical abundances

Published online by Cambridge University Press:  12 April 2016

P. Hellings  and
D. Vanbeveren
P. Hellings
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, Belgium
D. Vanbeveren
Affiliation:
Astrophysical Institute, Vrije Universiteit Brussel, Belgium

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Evolutionary computations are presented for massive stars between 20 Mo and 100 Mo with chemical abundances holding for the Small Magellanic Cloud, i.e. X = .76 and Z = .003. Mass loss by stellar wind is taken into account during core hydrogen burning. After core hydrogen burning some models are considered as members of close binary systems and are followed during their Roche lobe overflow stage according an early case B of mass transfer. During the core helium burning stage of the RL0F remnants mass loss rates comparable to WR stars are included in order to study the formation and the evolution of WR stars. Comparison with similar galactic computations (Vanbeveren, Packet, 1978) is made.

Type
Session V - Mass Loss and Stellar Evolution: Massive Stars
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 279 - 282
Copyright
Copyright © Reidel 1981

References

de Loore, C., De Grève, J.P., Lamers, H. (1977), Astron. Astrophys. 61, 251.Google Scholar
de Loore, C., De Grève, J.P., Vanbeveren, D. (1978), Astron. Astrophys. 67, 373.Google Scholar
Vanbeveren, D., Packet, W. (1979), Astron. Astrophys. 80, 242.Google Scholar
Vanbeveren, D., De Grève, J.P. (1979), Astron. Astrophys. 77, 295.Google Scholar