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We study the impact of large-scale perturbations from convective shellburning on the core-collapse supernova explosion mechanism usingthree-dimensional (3D) multi-group neutrino hydrodynamics simulations of an 18solar mass progenitor. Seed asphericities in the O shell, obtained from arecent 3D model of O shell burning, help trigger a neutrino-driven explosion330ms after bounce whereas the shock is not revived in a model based on aspherically symmetric progenitor for at least another 300ms. We tentativelyinfer a reduction of the critical luminosity for shock revival by ~20% due topre-collapse perturbations. This indicates that convective seed perturbationsplay an important role in the explosion mechanism in some progenitors. Wefollow the evolution of the 18 solar mass model into the explosion phase formore than 2s and find that the cycle of accretion and mass ejection is stillongoing at this stage. With a preliminary value of 0.77 Bethe for thediagnostic explosion energy, a baryonic neutron star mass of 1.85 solar masses,a neutron star kick of ~600km/s and a neutron star spin period of ~20ms at theend of the simulation, the explosion and remnant properties are slightlyatypical, but still lie comfortably within the observed distribution. Althoughmore refined simulations and a larger survey of progenitors are still calledfor, this suggests that a solution to the problem of shock revival andexplosion energies in the ballpark of observations are within reach forneutrino-driven explosions in 3D.

Supernova Simulations from a 3D Progenitor Model -- Impact of Perturbations and Evolution of Explosion Properties