Federico Rizzuti (Keele)

Our knowledge of stellar evolution is limited by uncertainties arising from complex multi-dimensional processes in stellar interiors, usually reproduced in 1D stellar evolution models with simplified prescriptions. 3D hydrodynamics models can improve these prescriptions by studying realistic multi-D processes, usually for a short timerange (minutes or hours). Recent advances in computing resources are starting to enable longer 3D simulations, more compatible with the evolutionary timescales. In this talk, I will present results coming from a new set of hydrodynamics simulations of a massive-star neon-burning shell, run continuously from early development to fuel exhaustion. I will discuss the implications for convective boundary mixing and entrainment, with the possibility of extracting an entrainment law for 1D models.