Hostname: page-component-8448b6f56d-qsmjn Total loading time: 0 Render date: 2024-04-23T08:06:48.080Z Has data issue: false hasContentIssue false
  • English
  • Français

SN 1987a: Theoretical Considerations

Published online by Cambridge University Press:  12 April 2016

S. E. Woosley
S. E. Woosley*
Affiliation:
Board of Studies in Astronomy and Astrophysics Lick Observatory, University of Californiaat Santa Cruz Santa Cruz CA 95064

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.

There is now general agreement that the presupernova star for 1987a was indeed SK-69-202, a star that had visual magnitude 12.36 (Walborn et al. 1987), bolometric correction 1.15m (Humphreys and McElroy 1984), and extinction 0.5m (Woosley et al. 1987). The distance modulus to the LMC is presently controversial, but most astronomers prefer a value near 18.5 (e.g., Walker 1985; Chiosi and Pigatto 1986) with an uncertainty of perhaps 0.2m. Putting it together, one arrives at a bolometric magnitude for SK-69-202 of −7.8 with a probable range −7.5 to −8.2, or a luminosity of 4 × 1038 erg s−1 with a range of 3 to 6 × 1038 erg s−1. At the time of the supernova the hydrogen burning shell contributes negligible energy generation so the critical quantity determining the luminosity is the helium core mass. Inspection of a variety of current stellar models indicates that SK-69-202 had a helium core mass of 6 ± 1 M⊙ from which we may infer that, on the main sequence, it had a mass of 19 ± 3 M⊙. A B3-I supergiant has a surface temperature of ∼16,000 K (Humphreys and McElroy 1984). For the above range of luminosities and assuming a temperature in the range 15,000 to 18,000 K one obtains a radius for SK-202-69 of 3 ± 1 × 1012 cm.

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. 361 - 374
Copyright
Copyright © Springer-Verlag 1988

References

Arnett, W.D. 1987, Ap. J., 319, 136.Google Scholar
Burrows, A., and Woosley, S.E. 1986, Ap. J., 308, 680.Google Scholar
Catchpole, R.M., Menzies, J.W., Monk, A.S., Wargau, W.F. and 16 others. 1987, preprint, South Africa Observatory.Google Scholar
Chevalier, R., and Klein, R.I. 1978, Ap. J., 219, 994.CrossRefGoogle Scholar
Chiosi, A., and Maeder, A. 1986, Ann. Rev. Astron. and Ap., 24, 329.CrossRefGoogle Scholar
Chiosi, C., and Pigatto, L. 1986, Ap. J., 308, 1.Google Scholar
Elias, , and Gregory, 1987, in preparation for Ap. J. Google Scholar
Hamuy, M., Suntzeff, N.B., Gonzalez, R., and Martin, G. 1987, NOAO Preprint No. 102, submitted to Ap. J. Google Scholar
Humphreys, R.M. 1984, in Observational Tests of Stellar Evolution Theory, IAU Symposium 105, ed. Maeder, A. and Renzini, A., (D. Reidel: Dordrecht), p. 279.Google Scholar
Humphreys, R.M., and McElroy, D.B. 1984, Ap. J., 284, 565.Google Scholar
Karp, A.H., Lasher, G., Chan, K.L., and Salpeter, E.E. 1977, Ap. J., 214, 161.Google Scholar
Maeder, A. 1987, preprint to appear in Proc. of ESO Workshop on SN1987a, ed. Danziger, J., in press.Google Scholar
Manchester, R.N., and Taylor, J.H. 1977, Pulsars, (Freeman: San Francisco).Google Scholar
Mayle, R.W., and Wilson, J.R. 1987, preprint, submitted to Ap. J. Google Scholar
Nomoto, K., Shigeyama, T., and Hashimoto, K. 1987, in Proc. ESO Workshop, on SN1987a, ed. Danziger, J., in press.Google Scholar
Ostriker, J.P., and Gunn, J.E. 1969, Ap. J., 157, 1395.Google Scholar
Pinto, P.A., and Woosley, S.E. 1987, submitted to Ap. J.Google Scholar
Shigeyama, T., Nomoto, K., Hashimoto, K., and Sugimoto, D. 1987, Nature, 328, 320.CrossRefGoogle Scholar
Taylor, J. 1986 in The Origin and Evolution of Neutron Stars, ed. Helfand, D.J. and Huang, J.-H., (D. Reidel: Dordrecht), p. 383.Google Scholar
Truran, J.W., and Weiss, A. 1987, Max Planck Inst. for Ap. preprint No. 303. To appear in Proc. of 4th Workshop on Nuclear Astrophysics.Google Scholar
Walborn, N.R., Lasker, B.M., Laidler, V.G., and Chu, Y.-H. 1987, Ap. J. Lettr., in press.Google Scholar
Walker, A.R. 1985, MNRAS, 212, 343.CrossRefGoogle Scholar
Wood, P.R., and Faulkner, D.J. 1987, Proc. Astron. Soc. Australia, in press.Google Scholar
Woosley, S.E. 1987, submitted to Ap. J. Google Scholar
Woosley, S.E., Pinto, P.A., Martin, P., and Weaver, T.A. 1987, Ap. J., 318, 664.Google Scholar
Woosley, S.E., Pinto, P.A., and Ensman, L. 1988, Ap. J., 324, 000.Google Scholar
Woosley, S.E., and Weaver, T.A. 1987, Physics Reports, Proc. Bethe Birthday Workshop, submitted.Google Scholar
Woosley, S.E., and Weaver, T.A. 1986, in Radiation Hydrodynamics in Stars and Compact Objects, ed. Mihalas, D. and Winkler, K.-H. A., (Springer Verlag: Berlin), p. 91.CrossRefGoogle Scholar