MODELING THE DYNAMICAL COUPLING OF SOLAR CONVECTION WITH THE RADIATIVE INTERIOR

摘要: The global dynamics of a rotating star like the Sun involves coupling highly turbulent convective envelope overlying seemingly benign radiative interior. We use anelastic spherical harmonic code to develop new class three-dimensional models that nonlinearly couple deep stable numerical simulation assumes realistic solar stratification from r = 0.07 up 0.97R (with R radius), thus encompassing part nuclear core through most convection zone. find tachocline naturally establishes itself between differentially and solid body rotation interior, with slow spreading is here diffusively controlled. rapid angular momentum redistribution in leads fast equator poles, conical differential achieved at mid-latitudes, much as has been deduced by helioseismology. motions are able overshoot downward about 0.04R into However, meridional circulation there confined smaller penetration depth directed mostly equatorward base Thermal wind balance established lower zone but departures evident upper Internal gravity waves excited overshooting, yielding complex wave field throughout