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On the Origin of Supernovae of Type Ib

Published online by Cambridge University Press:  12 April 2016

David Branch
David Branch*
Affiliation:
Department of Physics and Astronomy, University of Oklahoma Norman, Oklahoma 73019, U.S.A.

Extract

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The issue I want to discuss is this: supernovae observed during their photospheric phases display three distinct kinds of spectra - but there are four distinct chemical compositions that should be considered for the outer layers of exploding stars. What is the correspondence between the observed supernova type and the chemical composition?

The three kinds of observed spectra are Type II, which by definition shows optical hydrogen lines, Type Ia, which has neither hydrogen nor helium lines, and Type Ib, which has helium but not hydrogen.

The compositions to be considered are hydrogen-rich, or, speaking loosely, “solar”; helium-rich, or, loosely, “Wolf-Rayet”; deflagration - initially a mixture of heavy elements from carbon to radioactive nickel, which decays through cobalt to iron; and detonation - initially a mixture of just helium and radioactive nickel.

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. 281 - 287
Copyright
Copyright © Springer-Verlag 1988

References

Abbott, D., Beiging, J.H., Churchwell, E., and Torres, A. 1986, Ap. J., 303, 239 Google Scholar
Begelman, M.C., and Sarzin, C.L. 1986, Ap. J. (Lett.), 302, 59.CrossRefGoogle Scholar
Branch, D., and Nomoto, K. 1986, Astr. Ap., 164, L13.Google Scholar
Chevalier, R.A. 1984a, Ap. J. (Lett.), 285, L63.Google Scholar
Chevalier, R.A. 1984b, Ann. N. Y. Acad. Sci., 422, 215.Google Scholar
Chevalier, R.A. 1986, Highlights Astron., 7, 599.Google Scholar
Elias, J.H., Mathews, K., Neugebauer, G., and Persson, S.E. 1986, Ap. J., 296, 379.Google Scholar
Filippenko, A.V., and Sargent, W.L.W. 1986, A. J., 91, 691.Google Scholar
Gaskell, C.M., Capellaro, E., Dinerstein, H., Garnett, D., Harkness, R.P., and Wheeler, J.C. 1986, Ap. J. (Lett.), 306, 77.Google Scholar
Graham, J.R. 1987, Ap. J., 315, 588.Google Scholar
Harkness, R.P., Wheeler, J.C., Margon, B., Downes, R.A., Kirshner, R.P., Uomoto, A., Barker, E.S., Cochran, A.L., Dinerstein, H.L., Granett, D.R., and Levreault, R.M. 1987, Ap. J., 317, 355.Google Scholar
Huang, Y.-L. 1987, P.A.S.P., 99, 461.Google Scholar
Iben, I Jr., Nomoto, K., Tornambe, A., and Tutukov, A.V. 1987, Ap. J., 317, 717 Google Scholar
Khokhlov, A.M., and Ergma, E.V. 1986, Sov. Astr. Lett., 12, 152 Google Scholar
Nomoto, K. 1987, in Proc. 13th Texas Symp. Rel. Ap., ed. Ulmer, M.P. (World Scientific Press, Singapore), in press.Google Scholar
Panagia, N., Sramek, R.A., and Weiler, K.W. 1986, Ap. J. (Lett.), 300, 55.Google Scholar
Porter, A.C., and Filippenko, A.V. 1987, A. J., 93, 1372.Google Scholar
Rust, B.W. 1974, Oak Ridge Nat. Lab., Rept. 4953.Google Scholar
Schaeffer, R., Casse, M., and Cahen, S. 1987, Ap. J. (Lett.), 316, 31.Google Scholar
Sramek, R.A., Panagia, N., and Weiler, K.W. 1984, Ap. J. (Lett.), 285, 59.Google Scholar
Wheeler, J.C.., and Levreault, R. 1985, Ap. J. (Lett.), 294, 17.Google Scholar
Woosley, S.E., Taam, R.E., and Weaver, T.A. 1986, Ap. J., 301, 601 Google Scholar
Woosley, S.E., and Weaver, T.A. 1986, Ann. Rev. Astr. Ap., 24, 205.Google Scholar