Same as Fig. 9 for models computed without additional viscosity during the main sequence. The black line corresponds to a model with an initial velocity on the ZAMS of 8 km s^-1, an additional viscosity during the post-main sequence of 1.1 × 10⁴ cm² s^-1, and without braking of the surface by magnetized winds. Blue, red, and green lines indicate models that include a solar-calibrated braking of the stellar surface and an additional viscosity during the post-main sequence of 1.1 × 10⁴, 1.2 × 10⁴, and 1.3 × 10⁴ cm² s^-1, respectively. They are computed for an initial velocity of 20 km s^-1 on the ZAMS.