Predicted time a model spends in the different WR phases τ_WR as a function of luminosity for different initial parameters. The tracks taken from literature cover initial masses M_i = 30 M_⊙, 40 M_⊙, 60 M_⊙, and 80 M_⊙ (or 85 M_⊙ for the Geneva models). Due to the logarithmic spacing of our initial masses our models cover initial masses M_i = 32 M_⊙, 39.2 M_⊙, 63.1 M_⊙, and 79.4 M_⊙. The tail of each track is labeled with its initial mass. The tracks are colored in orange, green, and blue according to their surface abundances which are used in the later analysis to respectively differentiate the H-poor WN, H-free WN, and WC phase. In panel a and d the nonrotating and rotating Geneva tracks at galactic (dashed) and SMC (dotted) metallicity are compared to our model tracks (solid). Panels b and e show the nonrotating and rotating stellar evolution MIST tracks at galactic (dashed) and LMC (dotted) metallicity, in comparison to our tracks (solid). The last two panels c and f emphasize the differences of the galactic (dashed) and SMC (dotted) of the FRANEC models to our LMC models (solid).