  We present a combined model for magnetic field generation and transport in
cool stars with outer convection zones. The mean toroidal magnetic field, which
is generated by a cyclic thin-layer alpha-omega dynamo at the bottom of the
convection zone is taken to determine the emergence probability of magnetic
flux tubes in the photosphere. Following the nonlinear rise of the unstable
thin flux tubes, emergence latitudes and tilt angles of bipolar magnetic
regions are determined. These quantities are put into a surface flux transport
model, which simulates the surface evolution of magnetic flux under the effects
of large-scale flows and turbulent diffusion. First results are discussed for
the case of the Sun and for more rapidly rotating solar-type stars.
