  Several solar-like stars exhibit cyclic magnetic activity similar to the Sun
as found in photospheric and chromospheric emission. We want to understand the
physical mechanism involved in rotational dependence of these activity cycle
periods. We use three-dimensional magnetohydrodynamical simulations of global
convective dynamos models of solar-like stars to investigate the rotational
dependency of dynamos. We further apply the test-field method to determine the
$\alpha$ effect in these simulations. We find dynamo with clear oscillating
mean magnetic fields for moderately and rapidly rotating runs. For slower
rotation, the field is constant or exhibit irregular cycles. In the moderately
and rapidly rotating regime the cycle periods increase weakly with rotation.
This behavior can be well explained with a Parker-Yoshimura dynamo wave
traveling equatorward. Even though the $\alpha$ effect becomes stronger for
increasing rotation, the shear decreases steeper, causing this weak dependence
on rotation. Similar as other numerical studies, we find no indication of
activity branches as suggested by Brandenburg et al. (1998). However, our
simulation seems to agree more with the transitional branch suggested by
Distefano et al. (2017) and Olspert et al. (2017). If the Sun exhibit a dynamo
wave similar as we find in our simulations, it would operate deep inside the
convection zone.

Solar and Stellar Astrophysics