Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...280..282s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 280, May 1, 1984, p. 282-297. Research supported by the Natural Sciences an
Astronomy and Astrophysics
Astrophysics
126
Light Curve, Nuclear Fusion, Stellar Cores, Stellar Models, Supernovae, White Dwarf Stars, Abundance, Carbon Stars, Radioactive Decay, Stellar Mass Accretion, Taylor Instability, Thermonuclear Reactions
Scientific paper
White dwarf models are calculated for the explosions and light curves of Type I supernovae using full hydrodynamics and radiative diffusion. Comparison is made to recent observations. The models are based on the instantaneous thermonuclear burning of part or all of a degenerate carbon/oxygen/helium core. The Rayleigh-Taylor instability at the points of density/composition discontinuity is explored. The effects of radioactive decay of 56Ni and 56Co are incorporated by means of an absorption treatment of γ-rays. It is concluded that despite the qualitative appeal of the picture in which binary mass accretion raises a carbon-oxygen white dwarf to the Chandrasekhar limit, the demand to produce supernovae of the observed characteristics is not easily reconciled quantitatively with current calculations of hydrogen accretion.
Sutherland Peter G.
Wheeler Justin C.
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