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Carbon deflagration models for type-I supernovae and theoretical optical spectra

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Abstract

A carbon deflagration model in the accreting C+O white dwarf is presented as a plausible model for type-I supernovae (SN I). The evolution of the white dwarf is calculated from the beginning of accretion through complete disruption. The propagation of a carbon deflagration wave from center to the surface and associated nucleosynthesis are calculated. About 0.6M ⊙ 56Ni and substantial amounts of Ca, Ar, S, Si, Mg, and O are synthesized.

The synthetic spectrum at maximum light for this carbon deflagration model is calculated and compared to the observed spectrum of SN 1981b in NGC 4536 at maximum light. If the radial stratification of composition in the outer layers of the model is removed by mixing, the theoretical spectrum is in good agreement with the observed spectrum.

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Authors and Affiliations

  1. Dept of Earth Science and Astronomy, University of Tokyo, Japan

    Ken'Ichi Nomoto

  2. Institut für Astrophysik, Max-Planck-Institut für Physik und Astrophysik, Garching, F.R.G.

    Friedrich-K. Thielemann

  3. Institut für Kernphysik III, Karlsruhe, F.R.G.

    Koichi Yokoi

  4. Dept of Physics and Astronomy, University of Oklahoma, Norman, OK, U.S.A.

    David Branch

Authors
  1. Ken'Ichi Nomoto
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  2. Friedrich-K. Thielemann
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  3. Koichi Yokoi
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  4. David Branch
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Nomoto, K., Thielemann, FK., Yokoi, K. et al. Carbon deflagration models for type-I supernovae and theoretical optical spectra. Astrophys Space Sci 118, 305–309 (1986). https://doi.org/10.1007/BF00651141

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  • DOI: https://doi.org/10.1007/BF00651141

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