Time evolution of the stellar convective envelope mass obtained from models by Hoppe et al. (2020) for various [Fe/H] (left panel) and M_⋆ (right panel), indicated by a change in line color. The ordinate shows 1 – M_CE/M_⋆, so that if the star has a more massive convective zone, a lower value is shown, to indicate that the convective zone abundances adapt to the composition of the accretion flux more slowly.