  Magnetic fields can be created in stably stratified (non-convective) layers
in a differentially rotating star. A magnetic instability in the toroidal field
(wound up by differential rotation) replaces the role of convection in closing
the field amplification loop. Tayler instability is likely to be the most
relevant magnetic instability. A dynamo model is developed from these
ingredients, and applied to the problem of angular momentum transport in
stellar interiors. It produces a prodominantly horizontal field. This dynamo
process might account for the observed pattern of rotation in the solar core.
