Astronomy and Astrophysics – Astrophysics
Scientific paper
Jun 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...257..780n&link_type=abstract
Astrophysical Journal, Part 1, vol. 257, June 15, 1982, p. 780-792.
Astronomy and Astrophysics
Astrophysics
133
Detonation Waves, Shock Wave Propagation, Stellar Mass Accretion, Stellar Models, Supernovae, White Dwarf Stars, Density Distribution, Hydrodynamics, Light Curve, Nuclear Fusion, Supernova Remnants, Temperature Profiles
Scientific paper
The hydrodynamical behavior of supernova models based on accreting carbon-oxygen white dwarfs is computed through the explosion for three cases with different accretion rates. For intermediate accretion rates, the helium flash is so strong that it produces a helium detonation wave propagating outward and a carbon detonation wave propagating inward, which results in most of the star's material being converted into N-56 and the star itself being completely disrupted. For the case with a slower accretion rate, the helium flash is only strong enough to form a single detonation wave propagating outward, leaving behind either a white dwarf remnant or disrupting the star completely, depending on conditions in the white dwarf. The ejecta of double detonation supernovae is composed mostly of N-56, while the single detonation ejects a small amount of N-56 or N-56, C, and O in the case of total disruption. These models are compared with observed features of type I supernovae.
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