Solar activity cycles, north/south asymmetries, and differential rotation associated with solar spin-orbit variations

Abstract

The possible role of the Sun's planetary-induced spin-orbit dynamics in the generation of various solar oscillations is examined using simple approaches and heuristic models. Theoretically, the 22.5-yr dipole inversion magnetic cycle and the recently described 17-yr neutral line topology cycle can be derived from the non-linear mixing of two oscillations with periods of approximately 20 and 165 years. Oscillations with such periods are observed in two aspects of the Sun's spin-orbit dynamics. The 20-yr oscillation is the fundamental variation in the angular momentum of the solar body with respect to the solar system center-of-mass, while the 165-yr oscillation is the lowest-frequency component of the spin projection variations. It is shown that these two oscillations when mixed non-linearly yield, to a 1st-order approximation, the correct phase and frequency of the observed 17.5- and 22.5-yr magnetic cycles. By allowing an asymmetric shape to the 165-yr oscillation, the frequency modulation inherent in the Hale cycle (and sunspot cycle) is reproduced, yielding a more accurate estimate of solar activity. The asymmetric 165-yr oscillation matches the combination of the two lowest frequency components (165- and 84-yr periods) of the spin projection variations. Hemispheric sunspot asymmetry cycles, north/south differences in convective zone rotational velocities, and meridional flows are also shown to be expected byproducts of classical spin-orbit effects. Finally, the problem of low activity epochs (e.g., Maunder minimum) can be seen as a natural outcome of the interactions among the driving and driven oscillations involved in the conservation of solar system angular momentum.