  Observations of chromospheric and coronal emissions from various solar-type
stars show that the stellar magnetic activity varies with the rotation rates of
the stars. The faster the star rotates, its magnetic activity gets stronger but
activity cycle period does not show a straightforward variation with the
rotation rate. For slowly rotating stars, the cycle period decreases with the
increase of rotation rate, while for the fast rotators dependency of cycle
period on rotation is presently quite complicated. We aim to provide an
explanation of these observational trends of stellar magnetic activity using a
dynamo model. We construct a theoretical dynamo model for stars of mass 1
$M_\odot$ based on the kinematic flux transport dynamo model including radial
pumping near the surface of the stars. The inclusion of this near surface
downward radial pumping is found to be necessary to match the observed surface
magnetic field in case of the Sun. The main ingredients of our dynamo model,
meridional circulation and differential rotation for stars are obtained from a
mean-field hydrodynamic model. Our model shows a decrease of cycle period with
increasing rotation rate in the slowly rotating regime and a slight increase of
cycle period with rotation rate for the rapid rotators. The strength of the
magnetic field is found to be increasing as the rotation rate of the star
increases. We also find that the parity of the stellar magnetic field changes
with rotation. According to our model, the parity flips to quadrupolar from
dipolar if the rotation period of the star is less than 17 days.
