Allan Sacha Brun,  DSM/DAPNIA/SAp CEA Saclay

We present recent results of 3-D MHD numerical simulation of the bulk of the solar convective envelope in spherical geometry.
In particular we assess the role of the Reynolds and Maxwell stresses in establishing the differential rotation seen in our simulations.
We quantify the respective role of the mean vs fluctuating magnetic fields in our simulated
turbulent dynamo and present a probable scenario for the working of the solar dynamo.