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We perform two- (2D) and three-dimensional (3D) hydrodynamics simulations ofconvective oxygen shell-burning that takes place deep inside a massiveprogenitor star of a core-collapse supernova. Using one dimensional (1D)stellar evolution code, we first calculate the evolution of massive stars withan initial mass of 9-40 $M_\odot$. Four different overshoot parameters areapplied, and CO core mass trend similar to previous works is obtained in the 1Dmodels. Selecting eleven 1D models that have a silicon and oxygen coexistinglayer, we perform 2D hydrodynamics simulations of the evolution $\sim$100 suntil the onset of core-collapse. We find that convection with large-scaleeddies and the turbulent Mach number $\sim$0.1 is obtained in the models havinga Si/O layer with a scale of 10$^8$ cm, whereas most models that have anextended O/Si layer up to a few $\times 10^9$ cm exhibit lower turbulentvelocity. Our results indicate that the supernova progenitors that possess athick Si/O layer could provide a preferable condition for perturbation-aidedexplosions. We perform 3D simulation of a 25 $M_\odot$ model, which exhibitslarge-scale convection in the 2D models. The 3D model develops large ($\ell =2$) convection similar to the 2D model, however, the turbulent velocity islower. By estimating the neutrino emission properties of the 3D model, we pointout that a time modulation of the event rates, if observed in KamLAND andHyper-Kamiokande, would provide an important information about structuralchanges in the presupernova convective layer.

One-, Two-, and Three-dimensional Simulations of Oxygen Shell Burning Just Before the Core-Collapse of Massive Stars