A calibration of mixing length theory based on RHD simulations of solar-type convection

Details A calibration of mixing length theory based on RHD simulations of solar-type convection A calibration of mixing length theory based on RHD simulations of solar-type convection

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997assl..225...59l&link_type=abstract

SCORe'96 : Solar Convection and Oscillations and their Relationship, Proceedings of a workshop, held in Aarhus, Denmark, May 27

Astronomy and Astrophysics

Astrophysics

4

Stellar Convection, Mixing-Length Theory

Scientific paper

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 (alpha c) appropriate to construct global stellar models. The calibration based on our present set of 2D RHD models shows a moderate variation of alpha c across the domain of the HRD investigated so far.

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