  Stellar radiative zones are typically assumed to be motionless in standard
models of stellar structure but there is sound theoretical and observational
evidence that this cannot be the case. We investigate by direct numerical
simulations a three-dimensional and time-dependent model of stellar radiation
zones consisting of an electrically-conductive and stably-stratified anelastic
fluid confined to a rotating spherical shell and driven by a baroclinic torque.
As the baroclinic driving is gradually increased a sequence of transitions from
an axisymmetric and equatorially-symmetric time-independent flow to flows with
a strong poloidal component and lesser symmetry are found. It is shown that all
flow regimes characterised with significant non-axisymmetric components are
capable of generating self-sustained magnetic field. As the value of the
Prandtl number is decreased and the value of the Ekman number is decreased
flows become strongly time-dependent with progressively complex spatial
structure and dynamos can be generated at lower values of the magnetic Prandtl
number.
