Angular velocity evolution of stellar convective envelope as function of time for fast (up) and slow (down) rotator models in case where Ṁ_acc,init = 10⁻⁹ M_⊙ yr⁻¹. The black and the grey solid lines represent the MEs and APSW processes with Q_acc = 1% and Q_acc = 10%, respectively, and the magnetic field is from the BOREAS routine from Cranmer & Saar (2011). The red and the blue dotted lines represent the models including the MEs and APSW processes with Q_acc = 1% and Q_acc = 10%, respectively, but with the numerically imposed magnetic field B_mod. The free contraction (i.e. without any external interaction) is shown by the magenta long-dashed line. It represents the increase of the rotation rate during a free contraction phase. The angular velocity is scaled to the angular velocity of the present Sun. The blue and the red tilted square and associated error bars represent, respectively, the 90th percentile and the 25th percentile of the rotational distributions of solar-type stars in star-forming regions and young open clusters obtained with a rejection sampling method described in Gallet & Bouvier (2013).