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We have performed ab initio neutrino radiation hydrodynamics simulations inthree and two spatial dimensions (3D and 2D) of core-collapse supernovae fromthe same 15 $M_\odot$ progenitor through 440 ms after core bounce. Both 3D and2D models achieve explosions, however, the onset of explosion (shock revival)is delayed by $\sim$100 ms in 3D relative to the 2D counterpart and the growthof the diagnostic explosion energy is slower. This is consistent withpreviously reported 3D simulations utilizing iron-core progenitors with densemantles. In the $\sim$100 ms before the onset of explosion, diagnostics ofneutrino heating and turbulent kinetic energy favor earlier explosion in 2D.During the delay, the angular scale of convective plumes reaching the shocksurface grows and explosion in 3D is ultimately lead by a single, large-angleplume, giving the expanding shock a directional orientation not dissimilar fromthose imposed by axial symmetry in 2D simulations. We posit that shock revivaland explosion in the 3D simulation may be delayed until sufficiently largeplumes form, whereas such plumes form more rapidly in 2D, permitting earlierexplosions.

Three-dimensional core-collapse supernova simulated using a 15 $M_\odot$ progenitor