THE SOLAR INTERNAL MAGNETISM: PUTTING TOGETHER MORE PIECES OF THE PUZZLE

摘要

We discuss recent advances made in modelling in three dimensions the internal magnetohydrodynamical processes present in the Sun with the anelastic spherical harmonic (ASH) code. The intense magnetism of the Sun is most likely linked to dynamo action in the turbulent convective envelope and at its base, but the detailed description of the relevant physical processes have yet to be modeled self-consistently and non linearly. We here focus our study on how dynamical processes in unstable conducting convective zones, nonlinearly interact to establish the solar differential rotation, meridional circulation and generate strong magnetic field, and how toroidal (flux tube like) magnetic structures could emerge at the solar surface as active regions from the base of the convection zone in such a turbulent media.