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Understanding the physical process responsible for the transport of energy inthe core of $\alpha$ Centauri A is of the utmost importance if this star is tobe used in the calibration of stellar model physics. Adoption of differentparallax measurements available in the literature results in differences in theinterferometric radius constraints used in stellar modelling. Further, this isat the origin of the different dynamical mass measurements reported for thisstar. With the goal of reproducing the revised dynamical mass derived byPourbaix & Boffin, we modelled the star using two stellar grids varying in theadopted nuclear reaction rates. Asteroseismic and spectroscopic observableswere complemented with different interferometric radius constraints during theoptimisation procedure. Our findings show that best-fit models reproducing therevised dynamical mass favour the existence of a convective core ($\gtrsim$ 70%of best-fit models), a result that is robust against changes to the modelphysics. If this mass is accurate, then $\alpha$ Centauri A may be used tocalibrate stellar model parameters in the presence of a convective core.

$\alpha$ Centauri A as a potential stellar model calibrator: establishing the nature of its core