Fig. 4
Thick lines show the acceptable model solutions, i.e. the values of t⋆ and ηwind for which the third generation stars have a solar 26Al abundance. By definition ηwind cannot be larger than 1. The filled circle shows for information the onset of the WR phase. The dotted line shows the 60 M⊙ model with ΔC = 0.5 Myr instead of 0.3 Myr (see text).
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