  The centrifugal force is often omitted from simulations of stellar convection
either for numerical reasons or because it is assumed to be weak compared to
the gravitational force. However, it might be an important factor in rapidly
rotating stars, such as solar analogs, due to its $\Omega^2$ scaling, where
$\Omega$ is the rotation rate of the star. We study the effects of the
centrifugal force in a set of 21 semi-global stellar dynamo simulations with
varying rotation rates. Included in the set are three control runs aimed at
distinguishing the effects of the centrifugal force from the nonlinear
evolution of the solutions. We decomposed the magnetic field into spherical
harmonics and studied the migration of azimuthal dynamo waves (ADWs), the
energy of different large-scale magnetic modes, and differential rotation. In
the regime with the lowest rotation rates, $\Omega = 5-10\Omega_\odot$, where
$\Omega_\odot$ is the rotation rate of the Sun, we see no marked changes in
either the differential rotation or the magnetic field properties. For
intermediate rotation, $\Omega = 20-25\Omega_\odot$, we identify an increase in
the differential rotation as a function of centrifugal force. The axisymmetric
magnetic energy tends to decrease with centrifugal force, while the
non-axisymmetric one increases. The ADWs are also affected, especially in the
propagation direction. In the most rapidly rotating set with
$\Omega=30\Omega_\odot$, these changes are more pronounced, and in one case the
propagation direction of the ADW changes from prograde to retrograde. The
control runs suggest that the results are a consequence of the centrifugal
force and not due to the details of the initial conditions or the history of
the run. We find that the differential rotation and the ADWs only change as a
function of the centrifugal force when rotation is rapid enough.
