ZAMS (left) and TAMS (right) profiles of the region containing the inner 40 percent in mass of the three sets of 5 M_⊙ stellar models described in Sect. 2, showing the variation of the MLT variables: convective velocity on the top, mixing length in the middle, and degree of superadiabaticity at the bottom. The solid yellow lines correspond to the non-rotating model, the dashed purple lines correspond to the model with rotation and standard MLT, and the dashed-dotted orange lines correspond to the model with rotation and R-MLT. The vertical dotted line of the corresponding colour in each panel denotes the boundary of the convective core.