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

Understanding the physical process responsible for the transport of energy in the core of $\ alpha$ CentauriA is of the utmost importance if this star is to be used in the calibration of stellarmodel physics. Adoption of different parallaxmeasurements available in the literature results in differences in the interferometric radius constraints used in stellarmodelling. Further, this is at the origin of the different dynamical mass measurements reported for this star. With the goal of reproducing the revised dynamical mass derived by y Pourbaix & Boffin, we modelled the star using two stellargrids varying in the adopted nuclear reactionrates. Asteroseismic and spectroscopic observables were complemented with different interferometric radius constraints during the optimisation procedure. Our findings show that best- fit modelsreproducing the revised dynamical mass favour the existence of a convective core ($\gtrsim$ 70% of best- fit models), a result that is robust against changes to the model physics. If this mass is accurate, then $\ alpha$ CentauriA may be used to calibrate stellarmodel parameters in the presence of a convective core.