Emergence of magnetic flux and organisation on the surface of the Sun
On the solar surface there is a continual emergence of magnetic flux, distributed over various spatial scales; this can lead to the formation of active regions, of ephemeral regions, be added to the intranet work magnetic field or be distributed over even smaller scales, not resolved with present instruments. In order to contribute to the understanding of these problems, a series of coordinated observational campaigns are necessary, making use of both ground-based (IBIS at the DSR/NSO or the Goettingen Fabry-Perot at the VTT in Tenerife or the CRISP at the SST in La Palma) and satellite-based (SOHO-MDI, HINODE, SDO) instruments, so as to gain information on the various layers of the solar atmosphere and the magnetic configuration of the regions observed.
Also, the understanding of the predicted phenomena could be achieved by studying the emergence of magnetic flux tubes from the convection zone to the solar surface, via the development of 3D, numerical, MHD simulations, using appropriate codes with Adaptive Mesh Refinement.
