Dependencia entre la mezcla en los bordes de regiones convectivas y la masa estelar

Convective mixing in stellar interiors is one of the most misunderstood processes, although it is fundamental to build theoretical models. Convective overshooting (OV) is a process that extends the mixing beyond the convective boundaries imposed by the classical Schwarzschild criterion. In the diffusive approximation, this process depends on a free parameter ($f_{\rm ov}$) which measures its efficiency. The value of $f_{\rm ov}$ adopted in models can affect important parameters, such as the inferred age of stellar clusters. In this work we study the relationship between OV strength and stellar mass. We take into account additional mixing processes, such as semi-convection and thermohaline mixing. We use our stellar evolution code to compute models and compare them to measured and accurate properties of stars in order to infer values of $f_{\rm ov}$. We find that OV strength increases with stellar mass up to $\sim 2.5~\rm{M_{\odot}}$ and then remains approximately constant.