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Normal type Ia supernovae (SNe) are thought to arise from the thermonuclearexplosion of massive ($>0.8$ M$_\odot$) carbon-oxygen white dwarfs (WDs),although the exact mechanism is debated. In some models helium accretion onto acarbon-oxygen (CO) WD from a companion was suggested to dynamically trigger adetonation of the accreted helium shell. The helium detonation then produces ashock that after converging on itself close to the core of the CO-WD, triggersa secondary carbon detonation and gives rise to an energetic explosion.However, most studies of such scenarios have been done in one or twodimensions, and/or did not consider self-consistent models for the accretionand the He-donor. Here we make use of detailed 3D simulation to study theinteraction of a He-rich hybrid $0.69\,\mathrm{M_\odot}$ HeCO WD with a moremassive $0.8\,\mathrm{M_\odot}$ CO~WD. We find that accretion from the hybridWD onto the CO~WD gives rise to a helium detonation. However, the heliumdetonation does not trigger a carbon detonation in the CO~WD. Instead, thehelium detonation burns through the accretion stream to also burn the heliumshell of the donor hybrid HeCO-WD. The detonation of its massive helium shellthen compresses its CO core, and triggers its detonation and full destruction.The explosion gives rise to a faint, likely highly reddened transient,potentially observable by the Vera Rubin survey, and the high-velocity ($\sim1000\,\mathrm{km s^{-1}}$) ejection of the heated surviving CO~WD companion.Pending on uncertainties in stellar evolution we estimate the rate of suchtransient to be up to $\sim10\%$ of the rate of type Ia SNe.

Thermonuclear explosion of a massive hybrid HeCO white-dwarf triggered by a He-detonation on a companion