Evolution of the surface rotation periods as a function of time during core hydrogen burning for our 1.5 M_⊙ models. Models with B_p, ini = 10, 100, 1000, and 10 000 G are shown by red solid, dashed, dotted, and dash-dotted lines, respectively. Models with P_rot, ini = 1000, 100, 10, and 1 d are shown in the top-left, top-right, bottom-left, and bottom-right panels, respectively. The solid black lines correspond to models without stellar wind mass loss and with B_p, ini = 10 G for each initial rotation period.