Fig. 1
For different models of the stellar evolution grid of Brott et al. (2011a) using LMC metallicity, the surface nitrogen abundance is plotted against the fractional main sequence lifetime. The left panel shows the influence of the initial rotational velocity vZAMS for a given mass of M = 25 M⊙. The right panel depicts the evolution of the surface nitrogen abundance for several masses at vZAMS ≈ 280 km s-1.
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