ar X iv : a st ro - p h / 00 11 06 5 v 1 2 N ov 2 00 0 1 RADIATIVE HYDRODYNAMICS IN THE HIGHLY SUPER ADIABATIC LAYER OF STELLAR EVOLUTION MODELS
نویسندگان
چکیده
We present results of three dimensional simulations of the uppermost part of the sun, at 3 stages of its evolution. Each model includes physically realistic radiative-hydrodynamics (the Eddington approximation is used in the optically thin region), varying opacities and a realistic equation of state (full treatment of the ionization of H and He). In each evolution model, we investigate a domain, which starts at the top of the photosphere and ends just inside the convection zone (about 2400 km in the sun model). This includes all of the super-adiabatic layer (SAL). Due to the different positions of the three models in the log(g) vs logT ef f plane, the more evolved models have lower density atmospheres. The reduction in density causes the amount of overshoot into the radiation layer, to be greater in the more evolved models.
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