Global solar compressible convection simulations on non-Cartesian mappings

Abstract

Modeling the global dynamics of the Sun requires numerical frameworks capable of simulating the highly turbulent convective envelope and its coupling with the stable radiative interior. Simulating such spherical domains in standard Cartesian finite-volume codes presents significant topological challenges. The goal is to extend the Cartesian adaptive mesh refinement (AMR) framework to non-Cartesian geometries in order to perform global solar convection simulations that extend all the way down to the stellar core. Dyablo We introduced a mapped grid approach within the framework to build ( ) code. We implemented a well-balanced α--β scheme to preserve hydrostatic equilibrium. Furthermore, we present a robust methodology to generate fully integrated solar background profiles from r=0 to the surface. Dyablo Dyablo Whole Sun DWS We validated the implementation using standard hydrodynamic tests and ran high-resolution 2D global solar convection simulations on a . Our models successfully capture the turbulent convective broad slow upflows and narrow fast downflows and the excitation of acoustic waves and p modes. The interaction of strong downflowing plumes with the top of the radiative zone successfully excites internal gravity waves in the radiative interior.