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Stellar evolution codes play a major role in present-day astrophysics, yetthey share common simplifications related to the outer layers of stars. We seekto improve on this by the use of results from realistic and highly detailed 3Dhydrodynamics simulations of stellar convection. We implement a temperaturestratification extracted directly from the 3D simulations into two stellarevolution codes to replace the simplified atmosphere normally used. Ourimplementation also contains a non-constant mixing-length parameter, whichvaries as a function of the stellar surface gravity and temperature -- alsoderived from the 3D simulations. We give a detailed account of our fullyconsistent implementation and compare to earlier works, and also provide afreely available MESA-module. The evolution of low-mass stars with differentmasses is investigated, and we present for the first time an asteroseismicanalysis of a standard solar model utilising calibrated convection andtemperature stratification from 3D simulations. We show that the inclusion of3D results have an almost insignificant impact on the evolution and structureof stellar models -- the largest effect are changes in effective temperature oforder 30 K seen in the pre-main sequence and in the red-giant branch. However,this work provides the first step for producing self-consistent evolutionarycalculations using fully incorporated 3D atmospheres from on-the-flyinterpolation in grids of simulations.

Stellar models with calibrated convection and temperature stratification from 3D hydrodynamics simulations