  The operation of an interface dynamo (as has been suggested for the Sun and
other stars with convective envelopes) relies crucially upon the effective
transport of magnetic flux between two spatially disjoint generation regions.
In the simplest models communication between the two regions is achieved solely
by diffusion. Here we incorporate a highly simplified anisotropic transport
mechanism in order to model the net effect of flux conveyance by magnetic
pumping and by magnetic buoyancy. We investigate the influence of this
mechanism on the efficiency of kinematic dynamo action. It is found that the
effect of flux transport on the efficiency of the dynamo is dependent upon the
spatial profile of the transport. Typically, transport hinders the onset of
dynamo action and increases the frequency of the dynamo waves. However, in
certain cases there exists a preferred magnitude of transport for which dynamo
action is most efficient. Furthermore, we demonstrate the importance of the
imposition of boundary conditions in drawing conclusions on the role of
transport.
