Shape of the overall internal mixing profile in our stellar models. The green zone on the left is the fully mixed convective core, the dark blue zone indicates the convective overshoot zone, and the light blue area is the radiative envelope where mixing takes place through IGWs. The size of the overshoot zone is determined by α_ov, and the starting height of the envelope mixing is determined by log(D_env/cm² s⁻¹). This figure is inspired by Figure 3 from Pedersen et al. (2021).