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Paper: Evolution of Rotating Massive Stars into the Wolf--Rayet Phase at Solar Metallicity
Volume: 211, Massive Stellar Clusters
Page: 105
Authors: Meynet, G.
Abstract: In this work we study the impact of rotational mixing on the WR star formation process and derive some consequences for the WR populations expected at solar metallicity. More precisely we obtain that : * The rotating models with initial masses superior to about 60 M_sun reach the break-up limit when the core contracts at the beginning of the He-burning phase, reinforcing the possible link between the Luminous Blue Variable (LBV) phenomenon and the approach of the break-up limit (Langer 1998; Maeder 1999). * With respect to non-rotating models, models with mean rotational velocities on the Main Sequence comparable to the observed ones, have a WR lifetime increased by about a factor 2.5 - 3.5 at solar metallicity. * The minimum initial mass for stars going through a WR phase is decreased by rotation. * The observed number ratio of WR to O-type stars in the solar neighbourhood is much better accounted for by the rotating models than by the non-rotating ones. The number ratio of WC to WN stars is decreased by rotation.
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