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Mergers of carbon-oxygen (CO) white dwarfs (WDs) are considered as one of thepotential progenitors of type Ia supernovae (SNe Ia). Recent hydrodynamicalsimulations showed that the less massive (secondary) WD violently accretes ontothe more massive (primary) one, carbon detonation occurs, the detonation wavepropagates through the primary, and the primary finally explodes as asub-Chandrasekhar mass SN Ia. Such an explosion mechanism is called the violentmerger scenario. Based on the smoothed particle hydrodynamics (SPH) simulationsof merging CO WDs, we derived more stringent critical mass ratio (qcr) leadingto the violent merger scenario than the previous results. We conclude that thisdifference mainly comes from the differences in the initial condition,synchronously spinning of WDs or not. Using our new results, we estimated thebrightness distribution of SNe Ia in the violent merger scenario and comparedit with previous studies. We found that our new qcr does not significantlyaffect the brightness distribution. We present the direct outcome immediatelyfollowing CO WD mergers for various primary masses and mass ratios. We alsodiscussed the final fate of the central system of the bipolar planetary nebulaHenize 2-428, which was recently suggested to be a double CO WD system whosetotal mass exceeds the Chandrasekhar-limiting mass, merging within the Hubbletime. Even considering the uncertainties in the proposed binary parameters, weconcluded that the final fate of this system is almost certainly asub-Chandrasekhar mass SN Ia in the violent merger scenario.

The critical mass ratio of double white dwarf binaries for violent merger-induced Type Ia supernova explosions