2012ApJ...759...39H

We systematically explore zero impact parameter collisions of white dwarfs (WDs) with the Eulerian adaptive grid code FLASH for 0.64 + 0.64 M _☉ and 0.81 + 0.81 M_☉mass pairings. Our models span a range of effective linear spatial resolutions from 5.2x10⁷ to 1.2x10⁷ cm. However, even the highest resolution models do not quite achieve strict numerical convergence, due to the challenge of properly resolving small-scale burning and energy transport. The lack of strict numerical convergence from these idealized configurations suggests that quantitative predictions of the ejected elemental abundances that are generated by binary WD collision and merger simulations should be viewed with caution. Nevertheless, the convergence trends do allow some patterns to be discerned. We find that the 0.64 + 0.64 M_☉head-on collision model produces 0.32 M_☉ of ⁵⁶Ni and 0.38 M_☉ of ²⁸Si, while the 0.81 + 0.81 M_☉head-on collision model produces 0.39 M_☉ of ⁵⁶Ni and 0.55 M_☉ of ²⁸Si at the highest spatial resolutions. Both mass pairings produce ∼0.2 M_☉ of unburned ¹²C+¹⁶O. We also find the 0.64 + 0.64 M _☉head-on collision begins carbon burning in the central region of the stalled shock between the two WDs, while the more energetic 0.81 + 0.81 M_☉head-on collision raises the initial post-shock temperature enough to burn the entire stalled shock region to nuclear statistical equilibrium.