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We present results from high-resolution semi-global simulations ofneutrino-driven convection in core-collapse supernovae. We employ an idealizedsetup with parametrized neutrino heating/cooling and nuclear dissociation atthe shock front. We study the internal dynamics of neutrino-driven convectionand its role in re-distributing energy and momentum through the gain region. Wefind that even if buoyant plumes are able to locally transfer heat up to theshock, convection is not able to create a net positive energy flux and overcomethe downwards transport of energy from the accretion flow. Turbulent convectiondoes, however, provide a significant effective pressure support to theaccretion flow as it favors the accumulation of energy, mass and momentum inthe gain region. We derive an approximate equation that is able to explain andpredict the shock evolution in terms of integrals of quantities such as theturbulent pressure in the gain region or the effects of non-radial motion ofthe fluid. We use this relation as a way to quantify the role of turbulence inthe dynamics of the accretion shock. Finally, we investigate the effects ofgrid resolution, which we change by a factor 20 between the lowest and highestresolution. Our results show that the shallow slopes of the turbulent kineticenergy spectra reported in previous studies are a numerical artefact.Kolmogorov scaling is progressively recovered as the resolution is increased.

Neutrino-Driven Convection in Core-Collapse Supernovae: High-Resolution Simulations