Reviewing solar magnetic field generation in the light of helioseismology

Helioseismic observations, in recent years, have vastly improved our understanding of solar interior dynamics. This has challenged theorists to come up with up-to-date models for the origin and evolution of magnetic fields in the Sun - which on the one hand has to be consistent with these new results from the solar interior and on the other hand, has to correctly reproduce magnetic features that have been observed on the Sun since the advent of telescopes and magnetograms. We report here results from such dynamo simulations and address the following questions: Where in the Sun are the strong "sunspot-forming" toroidal magnetic field and the much weaker poloidal field generated? What is the role and nature of the unobserved meridional counterflow? We also discuss possible future helioseismic inputs that may usefully constrain the exact nature of the solar dynamo.