Mass-loss rate of our MESA models as function of time, from the ZAMS until the end of core He burning. The models adopt the winds by Sabhahit et al. (2023). From top to bottom: Z = 0.008, 0.004, 0.001, and 0.0008. The solid lines correspond to the evolutionary phase in which the stellar models are in the optically thick regime (Γ_Edd > Γ_Edd,tr), while the dashed lines mark the optically thin regime.