Top: Li surface abundance versus T_eff in the Hyades (filled squares) and Praesepe (open squares) from Cummings et al. (2017); downward triangles are for upper limits. Comparison to the predictions at 0.75 Gyr (diamonds) of models with [Fe/H] = +0.15 computed under several assumptions: classical models (C; dashed black line) and complete models (cyan, blue, and violet diamonds for slow, median, and fast initial rotation velocities, respectively) and (light green, green, and dark green diamonds for slow, median, and fast initial rotation velocities, respectively). Bottom: V sin i versus T_eff in the Hyades (filled squares) and Praesepe (open squares) from Cummings et al. (2017). Comparison to the surface rotation velocity predictions of model at 0.75 Gyr. Insert: Zoom on the cool side of the Kraft rotation break including model predictions for 0.8–1.2 M_⊙ stars.