Left panel: distribution of He-burning stars in terms of ν_max. In blue we show the number of low-mass He-burning stars (M ≤ 1.2 M_⊙), and in green we show the number of high-mass He-burning stars (M ≥ 1.2 M_⊙). The colour bar indicates the location in ν_max where we expect the AGB bump for a given mass following Eq. (19) and adopting T_eff = 4800(ν_max/40.0)^0.06 (Mosser et al. 2010). The blue and green arrows roughly indicate the location of the AGB bump for low-mass and high-mass stars, respectively, which is characterised by a local excess of stars. Right panel: Evolution speed dν_max/dτ, where τ is the stellar age, as a function of ν_max for different stellar masses. The models computed with MESA start from the end of the clump phase, which is marked by a diamond. The start and the end of the AGB bump are marked by a circle and a star, respectively.