Several solar-like stars exhibit magnetic activity similar to the Sun. Wewant to understand the rotational dependency of these activity cycle periods.We use three dimensional magnetohydrodynamical simulations of global convectivedynamo models of solar-like stars to investigate the rotational dependency ofdynamos. We further apply the test-field method to determine the $\alpha$effect in these simulations. We find dynamo with clear oscillating meanmagnetic fields for moderately and rapidly rotating runs. For slower rotation,the field is constant or exhibit irregular cycles. In the moderately andrapidly rotating regime the cycle periods increase weakly with rotation. Thisbehavior can be well explained with a Parker-Yoshimura dynamo wave travelingequatorward. Even though the $\alpha$ effect becomes stronger for increasingrotation, the shear decreases steeper, causing this weak dependence onrotation. Similar as other numerical studies, we find no indication of activitybranches as suggested by Brandenburg et al. (1998). However, our simulationseems to agree more with the transitional branch suggested by Distefano 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.
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