Models which are able to achieve the best fit for each individual Wolf–Rayet star.
|SMC||M0||vrot ,0||T*||log L||XH||vsini; vrot||Pinc|
|AB||[ M⊙]||[km s−1]||[kK]||[L⊙]||[km s−1]|
Notes. For each object we display the initial mass and initial rotation velocity of the best-fitting models and we compare the observed values (Hainich et al. 2015) of the fit parameters to their model values at the momentthe best fit is achieved. Next, we display the observed upper limit on the rotational velocity v sin i and the model vrot at the moment the best fit is achieved. For models where vrot exceeds the observedupper limit on vsini we calculate Pinc, i.e., the chance that vsini does not exceed the upper limit due to a low inclination of the rotational axis. is the lowest χ2 value achieved with our three fit parameters T*, log L and XH . In this table, only single stars are considered and compared to models that are core hydrogen burning.
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