Effective temperature and evolution time as a function of initial mass at the point of WR formation; i.e., at the first computational time-step where each model fulfills our evolutionary criteria for WR stars. The colors and shapes indicate the chosen OB mass-loss prescription as either Vin01 (yellow squares) or Bes20 (red circles). The results are shown in separate panels depending on metallicity: solar (left) and LMC (right). The y-axis of the bottom plots refers to the time-span elapsed since the ZAMS at the moment of WR formation, normalized by the time spent on the MS by each model. The purple dotted line represents the separation of the models into two evolution scenarios, described in the text: the early-formed and late-formed WR stars are below and above this line, respectively.