Quick Overview of the proposed scientific tasks

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 a, b, and w effects and the emergence of magnetic flux ropes (cf. figure 1).

Task A1: High resolution simulations of the solar convection zone (convective scales) and its associated mean flows. Low magnetic Prandtl number simulations of dynamo action.

Task A2: The role of rotation and magnetism on the dynamics of the solar radiation zone

Task A3: Coupled models of the solar convection and radiation zones and nonlinear interaction between magnetic field generated by dynamo and an inner fossil field. Penetrative convection and pumping of magnetic field. Study of key elements of the solar dynamo puzzle.

Task A4: Flux tubes emergence in convective spherical shells with or without convection and a background magnetic field. Influence of a more realistic atmosphere and of the plasma beta on flux emergence.

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).

Task B1: Convection, differential rotation and magnetism in low mass red giant (RGB) stars

Task B2: Young Suns: magnetism of fastly rotating stars, activity vs rotation scaling law

Task B3: A stars: magnetism in core convection of massive stars and interaction with magnetism in radiative envelope

Task B4: K stars: convection and magnetism in deep convection shell for low mass stars

Task B5: Introduction of averaged profiles and physical quantities deduced from 3-D simulations into 1D stellar evolution models and 2-D mean field stellar dynamo models

Task C: development of STARS² web site and of data handling and analysis tools