Fig. 6.
Binding energy of the envelope of a 30 M⊙ post main-sequence star as a function of radius. Tracks are shown for our default set of physical assumptions, as well as for a model with increased overshooting and one with increased mass loss rates. For each model, we also show the binding energy resulting from the fits of Xu & Li (2010) and Claeys et al. (2014).
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