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Table 1: Characteristics of the stellar models (with $[{\rm Fe/H}]=-2$ ) on the ZAMS and at 10 Gyr: effective temperature, luminosity, thickness of the external convective zone in stellar mass and radius, largest convective scale $\ell _{\rm c}$ , characteristic convective frequency $\nu _{\rm c}$ , and thermal diffusivity below the convective envelope $K_{\rm T}$ . $\nu _{\rm max}$ is the maximum frequency required to capture the wave - mean flow interaction.