Surface rotational velocity as a function of buoyancy radius. The lines correspond to our models with different initial masses, computed at three different initial rotation rates for each initial mass. Left: driven by hydrodynamical processes alone. Right: same, but including internal magnetic fields. The data points correspond to γ Dor stars for which surface velocities are available from the literature (see Sect. 2); buoyancy radii are taken from Li et al. (2020). The surface velocity of the models is multiplied by π/4 to average over the unknown inclination angles of the stars.