3D hydrodynamic simulations of neon burning

The evolution of massive stars is deeply affected by uncertainties connected with the convective boundary mixing (CBM). Only recently, theoretical works are starting to improve 1D stellar evolution codes with the help of 3D hydrodynamic models, which can reproduce, on a shorter timescale, more realistic 3D processes (e.g. convection, rotation, magnetic activity). In order to better understand and constrain some of the CBM uncertainties, we computed a series of 3D hydrodynamical simulations of turbulent convection during neon burning in massive stars with the PROMPI code (using different boosting factors of the driving luminosity: 1, 10 and 100 times the standard energy generation rate). In this talk, I will present preliminary results from these 3D simulations including kinetic behaviour of the fluid elements within the convective region, entrainment rates, and shape of the boundaries estimated from the composition profiles.