  Forward asteroseismic modelling plays an important role towards a complete
understanding of the physics taking place in deep stellar interiors. With a
dynamical mass in the range over which models develop convective cores while in
the main sequence, the solar-like oscillator $\alpha$ Centauri A presents
itself as an interesting case study. We address the impact of varying the
metallicity mixture on the determination of the energy transport process at
work in the core of $\alpha$ Centauri A. We find that $\gtrsim$ 70$\%$ of
models reproducing the revised dynamical mass of $\alpha$ Centauri A have
convective cores, regardless of the metallicity mixture adopted. This is
consistent with the findings of Nsamba et al., where nuclear reaction rates
were varied instead. Given these results, we propose that $\alpha$ Centauri A
be adopted in the calibration of stellar model parameters when modelling
solar-like stars with convective cores.
