Fig. 13
Evolution of the surface rotation rate as a function of time for the models computed with IGW. Stellar masses are indicated on the tracks. In the left panel, the theoretical predictions for the 0.9, 1, and 1.2 M⊙ models are compared with the observed rotational distribution for stars with estimated masses between ~0.9 and 1.1 M⊙ in young open clusters from Gallet & Bouvier (2013).
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