Code of Conduct
Emre Isik (Istanbul)
Modelling magnetic flux transport in the Sun and active cool stars
I present an overview of the physical processes thought to underly the observed cyclic magnetic field of the Sun. The turbulent solar convection zone leads to a diversity of effects, which are responsible for the self-organisation of magnetic fields and large-scale flows. I summarise the successes and drawbacks of surface flux transport models, dynamical thin flux tube models, and Babcock-Leighton-type flux transport dynamos, in comparison with observational results. I finish the presentation by discussing our understanding of large-scale magnetism in stars more active than the Sun.
