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The bright, nearby binary $\alpha$ Centauri provides an excellent laboratoryfor testing stellar evolution models, as it is one of the few stellar systemsfor which we have high-precision classical (mass, radius, luminosity) andasteroseismic ($p$-mode) observations. Stellar models are created and fit tothe classical and seismic observations of both stars by allowing for the freevariation of convective mixing length parameter $\alpha_{\text{MLT}}$. Thissystem is modeled using five different sets of assumptions about the physicsgoverning the stellar models. There are 31 pairs of tracks (out of ${\sim}150,000$ generated) which fit the classical, binary, and seismic observationalconstraints of the system within $3\,\sigma$. Models with each tested choice ofinput physics are found to be viable, but the optimal mixing lengths for Cen Aand Cen B remain the same regardless of the physical prescription. The optimalmixing lengths are $\alpha_{\text{MLT,A}} /\alpha_{\odot}= 0.932$ and$\alpha_{\text{MLT,B}}/\alpha_{\odot} = 1.095$. That Cen A and Cen B requiresub- and super-solar mixing lengths, respectively, to fit the observations is atrend consistent with recent findings, such as in Kervella et al. (2017), Joyceand Chaboyer (2018), and Viani et al. (2018). The optimal models find an agefor $\alpha$ Centauri of $5.3 \pm 0.3$ Gyr.

Classically and Asteroseismically constrained 1D Stellar Evolution Models of $\alpha$ Centauri A and B using Empirical Mixing Length Calibrations