Fig. 14
Luminosity of the RGB bump as a function of initial stellar mass and Yini for those stars that undergo the bump before 14 Gyr (see ages given in Gyr along the dotted-line isochrones). The white area corresponds to the (M; Y) domain where stars do not undergo the RGB bump (this is also the case for models with an initial mass lower than 0.75 M⊙).
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