Atomic Diffusion and Turbulent Mixing in Solar-Like Stars: Impact on the Fundamental Properties of FG-Type Stars

Chemical transport mechanisms are a key ingredient in stellar modelling. One of the most important is atomic diffusion, which has proven to be very successful in modelling the Sun and solar-like stars. However, for stars more massive than 1.2 𝑀⊙, it predicts over-variation of surface abundances that are not observed in real stars. It is then necessary to take into account the other mechanisms in competition with atomic diffusion in stellar models. One possibility is the implementation of a turbulent mixing coefficient that is parameterized in order to reproduce the effect of other physical processes inside the star, by homogenizing part of the radiative region. In this work, we studied the effects of atomic diffusion considering gravitational settling and radiative accelerations (with and without) to explore the effects on the surface evolution of iron content and metallicity. We investigated the potential of using turbulent mixing to avoid the surface over-variations in the chemical abundances and reproduce the effects of radiative acceleration.