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Type Ia supernovae (SNe Ia) are likely the thermonuclear explosions ofcarbon-oxygen (CO) white-dwarf (WD) stars, but their progenitor systems remainelusive. Recent studies have suggested that a propagating detonation within athin helium shell surrounding a sub-Chandrasekhar mass CO core can subsequentlytrigger a detonation within the core (the double-detonation model, DDM). Theoutcome of this explosion is similar to a central ignition of asub-Chandrasekhar mass CO WD (SCD). While SCD is consistent with someobservational properties of SNe Ia, several computational challenges prohibit arobust comparison to the observations. We focus on the observed$t_0-M_\text{Ni56}$ relation, where $t_0$ (the $\gamma$-rays' escape time fromthe ejecta) is positively correlated with $M_\text{Ni56}$ (the synthesized$^{56}$Ni mass). We apply our recently developed numerical scheme to calculateSCD and show that the calculated $t_0-M_\text{Ni56}$ relation, which does notrequire radiation transfer calculations, converges to an accuracy of a fewpercent. We find a clear tension between our calculations and the observed$t_0-M_\text{Ni56}$ relation. SCD predicts an anti-correlation between $t_0$and $M_\text{Ni56}$, with $t_0\approx30\,\textrm{day}$ for luminous($M_\text{Ni56}\gtrsim0.5\,M_{\odot}$) SNe Ia, while the observed $t_0$ is inthe range of $35-45\,\textrm{day}$. We show that this tension is larger thanthe uncertainty of the results, and that it exists in all previous studies ofthe problem. Our results hint that more complicated models are required, but weargue that DDM is unlikely to resolve the tension with the observations.

Sub-Chandrasekhar-mass detonations are in tension with the observed $t_0-M_\text{Ni56}$ relation of type Ia supernovae