Abstract We calculated a grid of evolutionary tracks of rotating models with masses between 1.0 and 3.0 M⊙ and resolution δM≤0.02 M⊙, which can be used to study the effects of rotation on stellar evolution and on the characteristics of star clusters. The value of ~2.05 M⊙ is a critical mass for the effects of rotation on stellar structure and evolution. For stars with M>2.05 M⊙, rotation leads to an increase in the convective core and prolongs their lifetime on the main sequence (MS); rotating models evolve more slowly than non-rotating ones; the effects of rotation on the evolution of these stars are similar to those of convective core overshooting. However for stars with 1.1
Keywords stars: evolution — stars: rotation — stars: interiors
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