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Consequences of Rotational Mixing in late Type Massive Stars

Published online by Cambridge University Press:  04 August 2017

S.R. Sreenivasan  and
W.J.F. Wilson
S.R. Sreenivasan
Affiliation:
Department of Physics, The University of Calgary Calgary, Alberta, Canada T2N 1N4
W.J.F. Wilson
Affiliation:
Department of Physics, The University of Calgary Calgary, Alberta, Canada T2N 1N4

Extract

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We have examined further the consequences of mixing induced by rotation in massive stars (Pop I composition: X = 0.7; Y = 0.27) in the mass range 40–100 M⊙. The basic physics and a detailed examination for a 60 M⊙ model has recently been published (Sreenivasan and Wilson 1985b), as has a detailed examination of supergiants without such mixing (Sreenivasan and Wilson 1985a). We shall therefore not go into the background of our computation here, but merely summarize our present findings.

Information

Type
Poster Papers 3
Information
Symposium - International Astronomical Union , Volume 116: Luminous Stars and Associations in Galaxies , 1986 , pp. 385 - 387
Copyright
Copyright © Reidel 1986 

References

Humphreys, R.M., and McElroy, D.B. 1984, Ap. J. 284, 565–577.Google Scholar
Sreenivasan, S.R., and Wilson, W.J.F. 1982, Ap. J. 254, 287–296.Google Scholar
Sreenivasan, S.R., and Wilson, W.J.F. 1985a, Ap. J. 290, 653–659.Google Scholar
Sreenivasan, S.R., and Wilson, W.J.F. 1985b, Ap. J. 292, 000.Google Scholar