Surface rotational velocity as a function of time for stellar model sequences with four different initial masses (as indicated), and for three initial surface rotational velocities. The rapid decrease in rotation rate seen for ν_i ≃ 50,200 km s^-1 is caused by the enhanced mass loss at the bi-stability jump, whereas the steep decline of the rotation velocity for the fast rotators (ν_i ≃ 500 km s^-1) is a consequence of Wolf-Rayet type mass loss.