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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.
K. Nomoto (1982) studied this question.