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

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

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.118..305n&link_type=abstract

(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),

Astronomy and Astrophysics

Astrophysics

2

Carbon Stars, Stellar Mass Accretion, Stellar Models, Supernovae, Visible Spectrum, White Dwarf Stars, Light Curve, Nuclear Fusion, Stellar Composition, Stellar Evolution

Scientific paper

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 0.6 solar mass, Ni-56 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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