Effect of turbulence on the evolution of a) carbon and b) iron mass fractions, and c) the HRD of a 0.75 M_⊙ star accreting 0.1 M_⊙ of material from a 1 M_⊙ primary. Large abundance variations are expected after accretion in absence of turbulence (black and red dashes). Inclusion of turbulence as in Eq. (7)erases all abundance signatures of atomic diffusion on the post-mass-transfer main sequence (dark blue), even for small turbulent diffusion coefficients (orange). Only when the temperature parameter is reduced to log T₀ ≲ 5.5 do the abundance variations start to reappear (light blue and magenta). The thermohaline-mixing-only model (solid grey) is hotter than the models with turbulence, because in the latter diffusion still modifies the layers with T ≳ T₀, and thermohaline mixing is not as deep. For clarity, the HRD only shows the post-mass-transfer part of the evolutionary tracks.