Evolution of rotating massive stars with new hydrodynamic wind models

Open Access

Fig. 12.

Variation as a function of time of the total mass (upper red curves), of the mass fraction of ²⁶Al at the centre (bottom cyan curves), and at the surface (grey curves beginning at an ordinate equal to 60) in the 120 M_⊙ rotating models with the old (upper panel) and new (lower panel) mass-loss rates.

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