Fig. 5

Download original image
Mass-loss rate Ṁ as a function of Teff(τcrit) 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 τR,cont = 20, are shown. For our model sequences, the values of T* and Teff(τcrit) 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.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.