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Fig. 2.
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Teff versus time for 90 M⊙ stars with [Fe/H]=0.0 and v/vcrit = 0.0, with WR winds modeled with three different atmosphere morphologies. We divided the time axis into two equal halves, one from 0 − 3 Myr and another from 3 − 3.5 Myr, using different stretches in order to zoom-in on the evolution of Teff after 3 Myr.
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