Poster abstract
The fast solar tachocline
Abstract
Helioseismic measurements indicate that the solar tachocline is very thin. The mechanism
that inhibits differential rotation to propagate from the convective zone to deeper into the radiative zone is not known, though several propositions have been made. One possible scenario for the origin of the solar tachocline, known as the ``fast tachocline'', assumes that the turbulent diffusivity exceeds $ \eta > 10^9$ cm$^2/$s. In this case the dynamics will be governed by the dynamo-generated oscillatory magnetic field on relatively short timescales. Here, we present detailed numerical models for the fast solar tachocline with all components of the magnetic field calculated explicitly.
that inhibits differential rotation to propagate from the convective zone to deeper into the radiative zone is not known, though several propositions have been made. One possible scenario for the origin of the solar tachocline, known as the ``fast tachocline'', assumes that the turbulent diffusivity exceeds $ \eta > 10^9$ cm$^2/$s. In this case the dynamics will be governed by the dynamo-generated oscillatory magnetic field on relatively short timescales. Here, we present detailed numerical models for the fast solar tachocline with all components of the magnetic field calculated explicitly.