Hostname: page-component-745bb68f8f-l4dxg Total loading time: 0 Render date: 2025-01-11T12:02:22.387Z Has data issue: false hasContentIssue false
  • English
  • Français

Spectroscopic Diagnosis of SN1987A and Lesser Lights

Published online by Cambridge University Press:  12 April 2016

J. Craig Wheeler ,
Robert P. Harkness  and
Zalman Barkat
J. Craig Wheeler
Affiliation:
Department of AstronomyUniversity of Texas at Austin
Robert P. Harkness
Affiliation:
Department of AstronomyUniversity of Texas at Austin
Zalman Barkat
Affiliation:
Department of Physics HebrewUniversity of Jerusalem

Abstract

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.

SN 1987A gives a unique chance to study both the precursor star and the subsequent dynamical evolution of the explosion. Comparison of the light curves shows that either H0 ∼ 100 km/s/Mpc, or SN 1987A ejected significantly less 56Ni than ordinary Type II supernovae. Investigation of the stellar structure pertinent to SK -69 202 reveals multiple solutions. For given luminosity, effective temperature, core mass and core radius, there are two families of envelope mass, one with large envelope mass and one with small envelope mass. The small envelope mass solutions can be ruled out by considerations of kinematics and the light curve. Envelopes of moderate mass may avoid each of these problems, but must be helium rich to be structurally self-consistent.

The spectrum in both the optical and the ultraviolet at about two days is fairly well represented by a hydrogen envelope with a power law density profile (ρ∝r-11 ) of one-quarter solar metallicity in LTE. Theoretical spectra at this early epoch tend to favor luminosities on the high side of observational estimates in order to ionize Ca II and prevent excessively strong lines at H and K and the infrared triplet, with some ramifications for distance estimates.

The spectra of SN1987A present an interesting contrast to other SN II events. A McDonald Observatory spectrum of SN 1985H in NGC 3359 of uncertain epoch shows a very close resemblance to that of SN 1987A at about two month’s age, including the strong line at 607 nm attributed by Williams to Barium. SN 1985H may have been of the same class of event as SN 1987A.

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. 305 - 318
Copyright
Copyright © Springer-Verlag 1988

References

Refertences

Arnett, W.D. 1977, Ap. J. Suppl. 35, 145.CrossRefGoogle Scholar
Arnett, W.D. 1987a, Ap. J., 319, 136.CrossRefGoogle Scholar
Arnett, W.D. 1987b, preprint.Google Scholar
Ashoka, B.N., Anupama, G.C., Prabhu, T.P., Giriidhar, S., Ghash, K.K., Jain, S.K., Pati, A.K., and Kameswara Rao, N. 1987, J. Astron. Astr., 8, 195.Google Scholar
Barkat, Z. and Wheeler, J.C.. 1988, in preparation.Google Scholar
Blanco, V.M., et al. 1987, Ap. J., 320, 589.CrossRefGoogle Scholar
Branch, D. 1987a, Ap. J. (Letters), 320, L23.CrossRefGoogle Scholar
Arnett, W.D. 1987b, Ap. J. (Letters), 320, L121.Google Scholar
Cassatella, A., Fransson, C., van Santvoort, J., Gry, C., Talavera, A., Wamsteker, W. and Panagia, N. 1987, Astr. & Ap., 177, L29.Google Scholar
Catchpole, R.M. et al. 1987, M.N.R.A.S., in press.Google Scholar
Chevalier, R.A. and Fransson, C.. 1987, Nature, 328, 44.CrossRefGoogle Scholar
Danziger, I.J., Fosbury, R.A.E., Alloin, D., Cristiani, S., Dachs, J., Gouiffes, C., Jarvis, B., and Sahu, K.C., 1987, Astr. & Ap., 177, L13.Google Scholar
Doggett, J.B., and Branch, D. 1985, Ap. J., 90, 2303.Google Scholar
Dopita, M.A., Achilleos, N., Dawe, J.A., Flynn, C. and Meatheringham, S.J. 1987, preprint.Google Scholar
Fransson, C., Grewing, M., Cassatella, A., Panagia, N. and Wamsteker, W. 1987, Astr. & Ap., 177, L33.Google Scholar
Grassbergh, E.K., Imshennik, V.S., Nadyozhin, D.K., and Utrobin, V.P. 1987, preprint.Google Scholar
Hanuschik, R.W. and Dachs, J. Astr. and Ap., 182, L29.Google Scholar
Harkness, R.P. 1985, in Supernovae as Distance Indicators, ed. Bartel, N. (Berlin: Springer-Verlag), p. 183.CrossRefGoogle Scholar
Harkness, R.P. 1986, in Radiation Hydrodynamics in Stars and Compact Objects, ed. Mihalas, D. and Winkler, K.-H.A. (Berlin: Springer-Verlag), p. 166.CrossRefGoogle Scholar
Harkness, R.P. and Wheeler, J.C. 1988, in preparation.Google Scholar
Hillebrandt, W., Höflich, P., Truran, J.W., and Weiss, A. 1987, Nature, 327, 597.CrossRefGoogle Scholar
Kirshner, R., Sonneborn, G., Crenshaw, D.M., and Nassiopoulos, G.E. 1987, Ap. J., 320, 602.CrossRefGoogle Scholar
Lucy, L.B. 1987, Astr. & Ap., 182, L31.Google Scholar
Maeder, A. 1987, Proceedings of the ESO Conference on SN 1987A, in press.Google Scholar
Menzies, J.W., et al. 1987, M.N.R.A.S., 227, 39pCrossRefGoogle Scholar
Nomoto, K., Shigeyama, T., and Hashimoto, M. 1987, in Proceedings of the ESO Workshop on SN 1987A, in press.Google Scholar
Shigeyama, T., Nomoto, K., Hashimoto, M., and Sugimoto, D. 1987, Nature, 328, 320.CrossRefGoogle Scholar
Tyson, J.A. and Boeshaar, P.C. 1987, preprint.Google Scholar
Walborn, N.R., Lasker, B.M., Laidler, V.G., and Chu, Y.-H. 1987, Ap. J. (Letters), 321, L41.CrossRefGoogle Scholar
Wamsteker, , et al. 1987, Astr. & Ap., 177, L21.Google Scholar
Wheeler, J.C., Harkness, R.P., Barkat, Z. and Swartz, 1986, P.A.S.P., 98, 1018.Google Scholar
Williams, R.E. 1987, Ap. J. (Letters), 320, L117.Google Scholar
Wood, P.R. and Faulkner, D.J. 1987, preprint.Google Scholar
Woosley, S.E., Pinto, P.A., Martin, P.J., and Weaver, T.A. 1987, Ap. J., 318, 664.CrossRefGoogle Scholar
Woosley, S.E., Pinto, P.A., and Ensman, L. 1987, Ap. J., in press.Google Scholar