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Fig. 1


Duration of the different evolution phases up to the end of central helium burning for the 0.75 M models as a function of initial helium enrichment for the four different values of [Fe/H] (see colours and symbols in inset; MS = main sequence; SGB = subgiant branch; RGB = red giant branch; HB = horizontal branch). The abscissa ΔYini is the difference between the initial helium mass fraction of a given model and that of 1P stars at the considered metallicity

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