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We present evolutionary models for solar-like stars with an improvedtreatment of convection that results in a more accurate estimate of the radiusand effective temperature. This is achieved by improving the calibration of themixing-length parameter, which sets the length scale in the 1D convection modelimplemented in the stellar evolution code. Our calibration relies on theresults of 2D and 3D radiation hydrodynamics simulations of convection tospecify the value of the adiabatic specific entropy at the bottom of theconvective envelope in stars as a function of their effective temperature,surface gravity and metallicity. For the first time, this calibration is fullyintegrated within the flow of a stellar evolution code, with the mixing-lengthparameter being continuously updated at run-time. This approach replaces themore common, but questionable, procedure of calibrating the length scaleparameter on the Sun, and then applying the solar-calibrated value in modelingother stars, regardless of their mass, composition and evolutionary status. Theinternal consistency of our current implementation makes it suitable forapplication to evolved stars, in particular to red giants. We show that theentropy calibrated models yield a revised position of the red giant branch thatis in better agreement with observational constraints than that of standardmodels.

Stellar evolution models with entropy-calibrated mixing-length parameter: application to red giants