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Stellar models rely on a number of free parameters. High-quality observationsof eclipsing binary stars observed by Kepler offer a great opportunity tocalibrate model parameters for evolved stars. Our study focuses on six Keplerred giants with the goal of calibrating the mixing-length parameter ofconvection as well as the asteroseismic surface term in models. We introduce anew method to improve the identification of oscillation modes which exploitstheoretical frequencies to guide the mode identification ('peak-bagging') stageof the data analysis. Our results indicate that the convective mixing-lengthparameter (alpha) is about 14% larger for red giants than for the Sun, inagreement with recent results from modelling the APOGEE stars. We found thatthe asteroseismic surface term (i.e. the frequency offset between the observedand predicted modes) correlates with stellar parameters (Teff, log g) and themixing-length parameter. This frequency offset generally decreases as giantsevolve. The two coefficients a_-1 and a_3 for the inverse and cubic terms thathave been used to describe the surface term correction are found to correlatelinearly. The effect of the surface term is also seen in the p-g mixed modes,however, established methods for correcting the effect are not able to properlycorrect the g-dominated modes in late evolved stars.

Modelling Kepler Red Giants in Eclipsing Binaries:Calibrating the Mixing Length Parameter with Asteroseismology