Abstract

In this talk, we will review some aspects of the stellar magnetism and in particular what numerical simulations tell us about the physical processes underlying the observations. In cool Sun-like stars, a convective dynamo is thought to be responsible for the presence and evolution of magnetic fields. One important aspect of stellar dynamos is the possible presence of magnetic cycles, whose caracteristics depend on the stellar parameters. Another question is how magnetic flux is transported from the interior to the surface to produce starspots and whether those spots play a role in the dynamo process. In more evolved stars, i.e. subgiant and giant stars, new asteroseismic results just showed that strong magnetic fields exist in their cores. They may be responsible for an efficient transport of angular momentum that would explain the much-slower-than-expected core rotation of these stars. We will show in this talk that numerical simulations may help us tackle several of the above key questions about stellar magnetism.