Mass-loss rate Ṁ as a function of T_eff(τ_crit) for our model sequences. For comparison, a set of empirically inferred temperatures T_* for different types of WR stars is shown as well (gray symbols), illustrating the well-known “WR radius problem.” Since the empirical values are inferred from models without dynamical consistency, the values of T_* defined at a Rosseland optical depth of τ_R,cont = 20, are shown. For our model sequences, the values of T_* and T_eff(τ_crit) align very closely except for the highest mass-loss rates. A direct comparison with T_* from the dynamically-consistent models is provided in Fig. E.1.