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Using MESA code (Modules for Experiments in Stellar Astrophysics, version9575), an evaluation was made of the evolutionary state of the epsilon Aurigaebinary system (HD 31964, F0Iap + disk). We sought to satisfy severalobservational constraints: 1) requiring evolutionary tracks to pass close tothe current temperature and luminosity of the primary star; 2) obtaining aperiod near the observed value of 27.1 years; 3) matching a mass function of3.0; 4) concurrent Roche lobe overflow and mass transfer; 5) an isotopic ratio12 C/ 13 C = 5 and, (6) matching the interferometrically determined angulardiameter. A MESA model starting with binary masses of 9.85 + 4.5 Msun , with a100 day initial period, produces a 1.2 + 10.6 Msun result having a 547 dayperiod, and a single digit 12 C/ 13 C ratio. These values were reached near anage of 20 Myr, when the donor star comes close to the observed luminosity andtemperature for epsilon Aurigae A, as a post-RGB/pre-AGB star.Contemporaneously, the accretor then appears as an upper main sequence, earlyB-type star. This benchmark model can provide a basis for further explorationof this interacting binary, and other long period binary stars.

MESA Models of the Evolutionary State of the Interacting Binary epsilon Aurigae