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State-of-the-art one-dimensional (1D) stellar evolution codes rely onsimplifying assumptions, such as mixing length theory, in order to describesuperadiabatic convection. As a result, 1D stellar structure models do notcorrectly recover the surface layers of the Sun and other stars with convectiveenvelopes. We present a method that overcomes this structural drawback byemploying three-dimensional (3D) hydrodynamic simulations of stellar envelopes:at every time-step of the evolution interpolated 3D envelopes are appended tothe 1D structure and are used to supply realistic boundary conditions for thestellar interior. In contrast to previous attempts, our method includes mean 3Dturbulent pressure. We apply our method to model the present Sun. Thestructural shortcomings of standard stellar models lead to systematic errors inthe stellar oscillation frequencies inferred from the model. We show that ourmethod fully corrects for this error. Furthermore, we show that our realistictreatment of superadiabatic convection alters the predicted evolution of theSun. Our results hence have important implications for the characterization ofstars. This has ramifications for neighbouring fields, such as exoplanetresearch and galactic archaeology, for which accurate stellar models play a keyrole.

Overcoming the structural surface effect with a realistic treatment of turbulent convection in 1D stellar models