Fig. 1.
Surface nitrogen abundances as a function of stellar age for extreme values of αov and M⊙. The blue lines represent rotating 40 M⊙ models with an initial rotation rate of 200 km s−1, αov = 0.1 (dash-dotted), and αov = 0.5 (solid). The red lines show the corresponding non-rotating models for the same mass and values of αov respectively.
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