appears, like in the model computed by @FIH90. However, in our computation this convective zone reaches H-rich matter $\approx10\,$yr after the He core flash, whereas in the work by @FIH90 the HEFM occurs immediately after the He-flash ($\approx10^{-3}\,$yr). This difference is due to the much smaller distance between $M(\epsilon^{\rm He}_{\rm max})$ and the outer edge of the H-exhausted region in @FIH90’s [-@FIH90] model compared to our computations.

Fig. \[fig1\] shows the evolution of the energy release produced by H and He burning during the major He core flash for two models: the standard one and a model which does not experience a H-flash (models S1 & S3, see also Fig. \[fig2\]). At the onset of the H-flash, i.e. when the H-burning luminosity exceeds that of He-burning, the outer border of the convective shell has reached a mass shell with $X=0.055$. This value has to be compared with the value of $0.023$ listed by @FII00, which actually belongs to an $0.8\,M_\odot$ model, but which can be extrapolated safely to one with $M=1\,M_\odot$. As soon as H is carried into the interior, it starts to be burnt at an extremely high-rate due to the high temperatures in these regions, and this deeply 