Abstract
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.
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References
de Loore, C., De Grève, J.P., Lamers, H. (1977), Astron. Astrophys. 61, 251.
de Loore, C., De Grève, J.P., Vanbeveren, D. (1978), Astron. Astrophys. 67, 373.
Vanbeveren, D., Packet, W. (1979), Astron. Astrophys. 80, 242.
Vanbeveren, D., Packet, W. (1979), Astron. Astrophys. 80, 242.
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© 1981 D. Reidel Publishing Company
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Hellings, P., Vanbeveren, D. (1981). Stellar Evolution with SMC Chemical Abundances. In: Chiosi, C., Stalio, R. (eds) Effects of Mass Loss on Stellar Evolution. Astrophysics and Space Science Library, vol 89. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-8500-1_39
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DOI: https://doi.org/10.1007/978-94-009-8500-1_39
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-009-8502-5
Online ISBN: 978-94-009-8500-1
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