The Sun's magnetic field is created by dynamo action in the solar convection zone, probably deep within that layer and in the overshoot region at the top of the radiative interior. The dynamo mechanism is strongly affected by the differential rotation within the convection zone, which itself is largely driven by Reynolds stresses associated with the turbulence. The PI will develop a new simulation of the solar dynamo and the differential rotation within the solar convection zone. For this, he will further develop the turbulent transport theory necessary to explain the mean fluxes of magnetic field, momentum and entropy by the scales of turbulence that are unresolvable in global simulations. To validate and complete the theory, he will perform numerical simulations of convective magneto-turbulence in control volumes representing various depths and latitudes of the solar interior. When a robust parameterization of the turbulence has been obtained, he will use it in a global simulation of the differential rotation and the mean solar magnetic field.
