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Chemical composition is an important factor that affects stellar evolution.The element abundance on the stellar surface evolves along the lifetime of thestar because of transport processes, including atomic diffusion. However,models of stars with masses higher than about 1.2Msun predict unrealisticvariations at the stellar surface. This indicates the need for competingtransport processes that are mostly computationally expensive for large gridsof stellar models. The purpose of this study is to implement turbulent mixingin stellar models and assess the possibility of reproducing the effect ofradiative accelerations with turbulent mixing for elements like iron in orderto make the computation of large grids possible. We computed stellar modelswith MESA and assessed the effects of atomic diffusion (with radiativeacceleration) in the presence of turbulent mixing. We parametrised the effectof radiative accelerations on iron with a turbulent diffusion coefficient.Finally, we tested this parametrisation by modelling two F-type stars of theKepler Legacy sample. We found that, for iron, a parametrisation of turbulentmixing that simulates the effect of radiative acceleration is possible. Thisleads to an increase in the efficiency of the turbulent mixing to counteractthe effect of gravitational settling. This approximation does not affectsignificantly the surface abundances of the other elements we studied, exceptfor oxygen and calcium. We demonstrate that this parametrisation has anegligible impact on the accuracy of the seismic properties inferred with thesemodels. Moreover, turbulent mixing makes the computation of realistic F-typestar models including the effect atomic diffusion possible. This leads todifferences of about 10% in the inferred ages compared to results obtained withmodels that neglect these processes.

Atomic diffusion and turbulent mixing in solar-like stars: Impact on the fundamental properties of FG-type stars