We consider a conventional $\alpha $
α
–$\Omega $
Ω
-dynamo model with meridional circulation that exhibits typical features of the solar dynamo, including a Hale-cycle period of around 20 years and a reasonable shape of the butterfly diagram. With regard to recent ideas of a tidal synchronization of the solar cycle, we complement this model by an additional time-periodic $\alpha $
α
-term that is localized in the tachocline region. It is shown that amplitudes of some decimeters per second are sufficient for this $\alpha $
α
-term to become capable of entraining the underlying dynamo. We argue that such amplitudes of $\alpha $
α
may indeed be realistic, since velocities in the range of m s−1 are reachable, e.g., for tidally excited magneto–Rossby waves.
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