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Thermal instability of hydrogen burning shells in very massive stars

Published online by Cambridge University Press:  12 April 2016

Y. Tanaka ,
N. Arimoto  and
M. Takeuti
Y. Tanaka
Affiliation:
Faculty of Education, Ibaraki University, Mito 310, Japan
N. Arimoto
Affiliation:
Department of Astronomy, Tohoku University, Sendai 980, Japan
M. Takeuti
Affiliation:
Department of Astronomy, Tohoku University, Sendai 980, Japan

Extract

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Stothers and Chin (1972) examined numerically thermal instability of H burning shells in very massive stars. They reported the discovery of the thermal pulses in the shell on a stage of the contracting core just after the core exhaustion. Their results, however, are inconsequential because the pulses are very feeble and the mechanism of such feeble pulses is not well known at the shell burning phases. In this note, we summarize our analytical method and the results on the possibility of such feeble pulses in H burning shells, of which detailed procedure is described in another paper(Tanaka et al., 1980).

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. 289 - 292
Copyright
Copyright © Reidel 1981

References

Baker, N.:1966, in “Stellar Evolution”, ed. R.F.Stein and A.G.W.Cameron (Plenum Press, New York), p.333.Google Scholar
Sackmann, I.J.:1977, Astrophys.J., 212, pp.159–170.CrossRefGoogle Scholar
Stothers, R. and Chin, C.-w.:1972, Astrophys.J., 177. pp.155–160.Google Scholar
Tanaka, Y. Arimoto, N., and Takeuti, M.:1980, Submitted to Publ.Astron. Soc. Japan. Google Scholar