The purpose of task A, is to model as accurately as possible the Sun, its convection and radiation zones, its internal rotation profiles and key elements of the solar dynamo puzzle such as the α, β, and ω effects and the emergence of magnetic flux ropes (cf. figure 1).

Task B: Stellar magnetism across the Hertzsprung-Russell (HR) diagram:

The purpose of task B is to model accurately stars that are either less or more massive than the Sun or younger or more evolved (RGB) in order to map in 3-D stellar magnetism and the HR diagram (cf. figure 2).