Mixing coefficient (black) and Brunt–Väisälä frequency (blue) for the same region and stellar models as shown in Fig. 2. Profiles near the ZAMS are on the left-hand side, with the non-rotating model on the top, the model with rotation and standard MLT in the middle, and the model with rotation and R-MLT at the bottom. The corresponding profiles at the TAMS are displayed in the right-hand panels. Background shading indicates the dominant mixing mechanism in different stellar layers: grey for convection, purple for overshoot, green for the radiative envelope, and orange for the envelope with rotational mixing.