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Table 1

Assumed initial rotational velocities for Geneva and Bonn models.

Geneva Bonn
M (M) vZAMS (km s-1) M (M) vZAMS (km s-1)

15 400 15 329
20 421 20 324
25 441 25 374
32 614 30 372
40 647 40 417
60 714 60 455

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.

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