Recent years have seen an increased interest in the question of whether the gravitational action of planets could have an influence on the solar dynamo. Without discussing the observational validity of the claimed correlations, we ask for a possible physical mechanism that might link the weak planetary forces with solar dynamo action. We focus on the helicity oscillations that were recently found in simulations of the current-driven, kink-type Tayler instability, which is characterized by an m = 1 azimuthal dependence. We show how these helicity oscillations can be resonantly excited by some m = 2 perturbation that reflects a tidal oscillation. Specifically, we speculate that the 11.07 years tidal oscillation induced by the Venus-Earth-Jupiter system may lead to a 1:1 resonant excitation of the oscillation of the α-effect. Finally, in the framework of a reduced, zero-dimensional α-Ω dynamo model we recover a 22.14-year cycle of the solar dynamo.Roughly, we can distinguish between four different interpretations of the toroidal-to-poloidal field transformation. Mean-field dynamo theory, focusing on helical twisting of toroidal field lines in the turbulent convective zone, can be traced back to heuristic arguments by Parker (1955) and was later corroborated in mathematical detail by Steenbeck, Krause, and Rädler (1966); see also Krause and Rädler (1980). The theory starts by expressing the flow U = U + u and the magnetic field B = B + b as the sum of their mean parts (denoted by an overbar) and their fluctuating parts (denoted by lower-case letters). The interaction of the fluctuating flow and magnetic-field components produces an additional electromotive force term in the induction equation which, in its simplest form, can be written as E = u × b = αB − β∇ × B (but see Krause and Rädler (1980) and Rädler and Stepanov (2006) for significant extensions).Despite various conceptual problems (Proctor, 2006), regarding e.g. the catastrophic quenching of α (Vainshtein and Cattaneo, 1992), or the questionable relationship between helicity and α and the non-convergence of α for large magnetic Reynolds numbers (Courvoisier, Hughes, and Tobias, 2012), meanfield theory has served for decades as the standard model of the solar dynamo, which provided a natural explanation for the periodicity and the equator-ward sunspot propagation of the solar cycle (Steenbeck and Krause, 1969;Stix, 1972). A first blow to this model came when helioseismology mapped the differential rotation in the solar interior (Brown et al., 1989), in particular the positive radial shear in a ±30 • strip around the Equator, resulting in a serious problem with the Parker-Yoshimura sign rule which requires α∂Ω/∂r < 0 in the northern hemisphere for the correct equator-ward propagation of sun spots (Parker, 1955;Yoshimura, 1975). A second issue was raised by D' Silva and Choudhuri (1993) who noticed that the rather strong toroidal field at the bottom of the convection zone, which is needed to explain the variation of the tilts of bipolar sunspot pairs with lati...