  The dynamics of stably stratified stellar radiative zones is of considerable
interest due to the availability of increasingly detailed observations of Solar
and stellar interiors. This article reports the first non-axisymmetric and
time-dependent simulations of flows of anelastic fluids driven by baroclinic
torques in stably stratified rotating spherical shells -- a system serving as
an elemental model of a stellar radiative zone. With increasing baroclinicity a
sequence of bifurcations from simpler to more complex flows is found in which
some of the available symmetries of the problem are broken subsequently. The
poloidal component of the flow grows relative to the dominant toroidal
component with increasing baroclinicity. The possibility of magnetic field
generation thus arises and this paper proceeds to provide some indications for
self-sustained dynamo action in baroclinically-driven flows. We speculate that
magnetic fields in stably stratified stellar interiors are thus not necessarily
of fossil origin as it is often assumed.
