Abstract

Radiation hydrodynamics (RHD) models provide detailed information about the dynamics, thermal structure, and convective efficiency of the superadiabatic region at the top of solar-type convection zones, and allow an extrapolation of the entropy (s ) in their deep, adiabatic layers. For the Sun we find a close agreement between s inferred from our RHD models and an empirical determination of s from helioseismology. In the framework of mixing length theory (MLT), s is translated to an effective mixing-length parameter (α c) appropriate to construct global stellar models. The calibration based on our present set of 2D RHD models shows a moderate variation of α c across the domain of the HRD investigated so far.

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