Notes. Values of the Bonn models were chosen to best represent the typical vsin i of our sample stars, i.e. ~300 km s^-1, at the middle of the MS phase. In this context, we assume i = 70° as, being fast rotators, our targets are preferentially seen close to equator on (see Appendix B and discussion in Sect. 3 for the inclination values found by BONNSAI; we also note that Zorec et al. 2002, obtained an average value of 68 ± 18° for a sample of Be stars). We emphasise that another slightly different choice would not affect our conclusions. Geneva models have systematically greater initial rotational velocities than the Bonn models. This is due to the different treatment of rotation within the star: Geneva models assume a less strong coupling between the core and the envelope and the surface spin-down by stellar winds is more efficient than in Bonn models. Higher initial rotational velocities are therefore needed to reach fast rotation during the MS phase.