Convective overshooting from stellar cores: 3D simulation and Reynold's stress models

Convection in the central regions of stars is very important in determining how stars evolve since convection is very efficient at mixing the chemical elements produced by nuclear reactions in the centre Convection generated in an unstable core will penetrate beyond the boundary of the unstable region affecting both the structure of the star and enlarging the mass that is mixed in the core. This changes the evolution of the star, with consequences for estimating the age of stellar systems, and the late stages of evolution up to supernovae. I propose to undertake full 3-dimensional numerical simulations of convection in stellar interiors and also to develop so called Reynold's stress models to understand this phenomenon for a range of stellar conditions, including rotation and magnetic fields.