Abstract
Abstract SNe Ia are likely the thermonuclear explosions of carbon–oxygen white-dwarf stars, but their progenitor systems remain elusive. A few theoretical scenarios for the progenitor systems have been suggested, which have been shown to agree with some observational properties of SNe Ia. However, several computational challenges prohibit a robust comparison to the observations. We focus on the observed t 0 – M N I 56 relation, where t 0 (the γ-rays’ escape time from the ejecta) is positively correlated with M N I 56 (the synthesized 56Ni mass). Comparing to the t 0 – M N I 56 relation bypasses the need for radiation transfer calculations, as the value of t 0 can be directly inferred from the ejecta. We show that all known SNe Ia models fail to reproduce the observed t 0 – M N I 56 correlation.
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