Pascale Garaud
12/31/2006 09:00 AM
Applied Mathematics & Statistics
Two distinct classes of magnetic confinement models exist for the solar tachocline. The ``slow tachocline'' models are associated with a large-scale primordial field embedded in the radiative zone. The ``fast tachocline'' models are associated with an overlying dynamo field. I describe the results obtained in each case, their pros and cons, and compare them with existing solar observations. I conclude by discussing new lines of investigation that should be pursued, as well as some means by which these models could be unified or reconciled.
