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On the Synchronizability of Tayler–Spruit and Babcock–Leighton Type Dynamos

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Abstract

The solar cycle appears to be remarkably synchronized with the gravitational torques exerted by the tidally dominant planets Venus, Earth and Jupiter. Recently, a possible synchronization mechanism was proposed that relies on the intrinsic helicity oscillation of the current-driven Tayler instability which can be stoked by tidal-like perturbations with a period of 11.07 years. Inserted into a simple \(\alpha \)–\(\Omega \) dynamo model these resonantly excited helicity oscillations led to a 22.14 years dynamo cycle. Here, we assess various alternative mechanisms of synchronization. Specifically we study a simple time-delay model of Babcock–Leighton type dynamos and ask whether periodic changes of either the minimal amplitude for rising toroidal flux tubes or the \(\Omega \) effect could eventually lead to synchronization. In contrast to the easy and robust synchronizability of Tayler–Spruit dynamo models, our answer for those Babcock–Leighton type models is less propitious.

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Notes

  1. The “generous omission” of Mercury, whose tidal effect is nearly the same as that of Earth, but whose 88 days revolution period is often considered as “so short that its influence appears only as an average, non-fluctuating factor…” (Öpik, 1972), might be another argument for skeptics. However, it could also be worthwhile to re-analyze the 50 – 80 years sub-band of the Gleissberg cycle as identified by Ogurtsov et al. (2002) in the light of the 66.4 years period of the four-fold co-alignment of Mercury, Venus, Earth and Jupiter (Verma, 1986).

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Acknowledgements

This work was supported by Helmholtz-Gemeinschaft Deutscher Forschungszentren (HGF) in frame of the Helmholtz alliance LIMTECH.

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  1. Helmholtz-Zentrum Dresden – Rossendorf, Bautzner Landstr. 400, 01328, Dresden, Germany

    F. Stefani, A. Giesecke, N. Weber & T. Weier

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  1. F. Stefani
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Stefani, F., Giesecke, A., Weber, N. et al. On the Synchronizability of Tayler–Spruit and Babcock–Leighton Type Dynamos. Sol Phys 293, 12 (2018). https://doi.org/10.1007/s11207-017-1232-y

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