Observed temperature distribution of the WR stars in the SMC (gray area) compared to the time our evolutionary model of the primary (blue) and secondary (orange) are predicted to spend in the different temperature ranges during their WR phase. The observations are shown as Gaussians that have standard deviations corresponding to the observational uncertainties (see Table G.1). We excluded the binary SMC AB5 from this plot, as it has a different evolutionary origin.