Reynolds stress and heat flux in spherical shell convection

摘要: Context. Turbulent fluxes of angular momentum and enthalpy or heat due to rotationally affected convection play a key role in determining differential rotation stars. Their dependence on latitude depth has been determined the past from simulations Cartesian spherical simulations. Here we perform systematic comparison between two geometries as function rate. Aims. want extend earlier studies by using wedges obtain turbulent transport functions rate stratified convection. We compare results models same parameter regime order study whether restricted geometry introduces artefacts into results. In particular, clarify sharp equatorial profile horizontal Reynolds stress found is also reproduced geometry. Methods. employ direct numerical geometries. alleviate computational cost runs, reach high spatial resolution possible, model only parts longitude. The rotational influence, measured Coriolis number inverse Rossby number, varied zero roughly seven, which that likely be realised solar zone. are performed overlapping regimes. Results. For slow find radial latitudinal directed inward equatorward, respectively. rapid flux changes sign accordance with results, but contradiction theory. remains mostly equatorward develops maximum close equator. this peak can explained strong banana cells. effect case does not appear large. for rotation. Longitudinal always retrograde direction. profiles vary anti-solar (slow equator) intermediate solar-like (fast dominated Taylor-Proudman balance.