Improving stellar evolution models with atomic diffusion from asteroseismology of intermediate-mass stars

One of the biggest enigmas of stellar evolution concerns the transport of chemical elements. As this process is already ill-constrained during the core-hydrogen burning phase, the uncertainties that are introduced propagate into models of more evolved stars. The current state-of-the-art models are not able to predict the observed oscillation frequencies in intermediate-mass stars with their uncertainties. In this talk, we discuss the effect of atomic diffusion (including radiative levitation) on the frequencies of gravity modes and its implications for forward seismic modelling of intermediate-mass stars. Our results show significant differences in frequencies when including atomic diffusion, resulting in different derived masses, ages and metallicities. We will present our findings of our improved forward modelling scheme applied to a slowly rotating pulsator.