Hostname: page-component-848d4c4894-wg55d Total loading time: 0 Render date: 2024-05-17T14:10:31.260Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution of the Precursor of SN1987A

Published online by Cambridge University Press:  12 April 2016

P.R. Wood  and
D.J. Faulkner
P.R. Wood
Affiliation:
Mount Stromlo and Siding Spring Observatories Private Bag, Woden P.O., A.C.T. 2606Australia
D.J. Faulkner
Affiliation:
Mount Stromlo and Siding Spring Observatories Private Bag, Woden P.O., A.C.T. 2606Australia

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.

The evolution of a 17.5 M⊙ star, chosen to be similar to the precursor of SN1987A, has been studied using the input physics described in Wood and Faulkner (1987). The calculations: use opacities from the Astrophysical Opacity Library of Huebner et al (1977) with H, He, C, N, O and other metals in LMC ratios; treat semi-convection in the manner of Lamb, Iben and Howard (1976); and assume the mass loss rate to be the minimum of (a) α times the rate give in Waldron (1985) (this rate applied in the blue part of the HR diagram), and (b) L/(cv) (this rate applied in the red), where v is the stellar wind expansion velocity which was taken to be 12 km s−1.

Typical evolutionary tracks resulting from these calculations are shown in Figure 1. The track shown as a continuous line is the one shown in Wood and Faulkner (1987) and corresponds to α = 2.5, while the track shown as a dotted line results from a slightly different treatment of semi-convection on the main-sequence and to α = 1.

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. 410 - 411
Copyright
Copyright © Springer-Verlag 1988

References

Huebner, W.F., Merts, A.L., Magee, N.H. and Argo, M.F. 1977, Astrophysical Opacity Library, Los Alamos Scientific Laboratory, La-6760-M.Google Scholar
Lamb, S.A., Iben, I., and Howard, W.M. 1976, Ap. J., 207, 209.Google Scholar
Waldron, W.L. 1985, The Origin ofNonradiative Heating/Momentum in Hot Stars, Underbill, A.B. and Michelitsianos, A.G. (eds.), NASA Conf. Publ. CP-2358, p. 95.Google Scholar
Wood, P.R. and Faulkner, D.I. 1987, Proc. Astr. Soc. of Australia, in press.Google Scholar