Abstract

Motivated by recent results in stellar evolution predicting hybrid white dwarf (WD) stars with a C, O core inside an O, Ne shell, we simulate thermonuclear (Type Ia) supernovae from these hybrids using a multidimensional deflagration to detonation transition (DDT) paradigm implemented in the FLASH code. Using a hybrid WD model including the effects of the Urca process produced by the stellar evolution code MESA, we map the progenitor to the FLASH grid preserving hydrostatic equilibrium. We then perform a suite of DDT simulations over a range of ignition conditions consistent with the progenitor's thermal and convective structure. To compare Type Ia supernovae from these hybrid WD stars to previous results for C, O white dwarfs, we construct a set of C, O WD models and simulate their explosions as Type Ia supernovae using randomized ignition conditions but the same central density and DDT density as the hybrid progenitor. We find that despite the individual variability within the suites of hybrid models and C, O models, trends distinguishing their Type Ia supernovae are apparent in their Ni-56 yields and the kinetic properties of their ejecta, leading us to suggest observational signatures of the hybrid C, O, Ne white dwarfs.