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Since its proposal in 1992, the Applegate mechanism has been discussed as apotential intrinsical mechanism to explain transit timing variations in variouskinds of close binary systems. Most analytical arguments presented so farfocused on the energetic feasibility of the mechanism, while applying rathercrude one- or two-zone prescriptions to describe the exchange of angularmomentum within the star. In this paper, we present the most detailed approachto date to describe the physics giving rise to the modulation period fromkinetic and magnetic fluctuations. Assuming moderate levels of stellarparameter fluctuations, we find that the resulting binary period variations areone or two orders of magnitude lower than the observed values in RS-CVn likesystems, supporting the conclusion of existing theoretical work that theApplegate mechanism may not suffice to produce the observed variations in thesesystems. The most promising Applegate candidates are low-masspost-common-envelope binaries (PCEBs) with binary separations $\lesssim1~\mathrm{R}_\odot$ and secondary masses in the range of$0.30~\mathrm{M}_\odot$ and $0.36~\mathrm{M}_\odot$.

The physics of the Applegate mechanism: Eclipsing time variations from magnetic activity