Type Ia supernovae are white dwarf stars composed of carbon and oxygen which undergo a thermonuclear explosion, but the nature of the progenitor stars and the mechanism of the explosion is highly debated.
Here we are exploring the double-degenerate channel in which we have two sub-Chandrashekar WDs, each with thin helium shells. During the accretion of He, it detonates on the surface of the primary and wraps around the white dwarf, colliding on the other side. This would lead to the second detonation of carbon, either on the edge or due to shock converge at the core, and thus leading to a Type Ia supernova event.
Late-time light curves are thought to be powered by the radioactive decay of 57Co and provide an independent method to constrain the progenitors of Type Ia supernova. We compared five near-by Type Ias with simulation models of near-Chandrashekar and sub-Chandrashek ar white dwarfs, and see a clear distinction between the two types of progenitors. The red markers are the near-Chandra models while the blue ones are the sub-Chandra models. Color gradients represent the metallicity of the models.
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