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Eclipsing time variations (ETVs) are observed in many close binary systems.In particular, for several post-common-envelope binaries (PCEBs) that consistof a white dwarf and a main sequence star, the O-C diagram suggests that realor apparent orbital period variations are driven by Jupiter-mass planets or asa result of magnetic activity, the so-called Applegate mechanism. The latterexplains orbital period variations as a result of changes in the stellarquadrupole moment due to magnetic activity. We explore the feasibility ofdriving ETVs via the Applegate mechanism for a sample of PCEB systems,including a range of different rotations. Using the MESA code we evolve 12stars with different masses and rotation rates. We apply a simple dynamo modelto their radial profiles to investigate on which scale the predicted activitycycle matches the observed modulation period, and quantify the uncertainty, andfurther calculate the required energies to drive que Applegate mechanism. Weshow that the Applegate mechanism is energetically feasible in 5 PCEB systems,and note that these are the systems with the highest rotation rate compared tothe critical rotation rate of the main-sequence star. The results suggest thatthe ratio of physical to critical rotation in the main sequence star is animportant indicator for the feasibility of Applegate's mechanism, but exploringlarger samples will be necessary to probe this hypothesis.

The Applegate mechanism in Post-Common-Envelope Binaries: Investigating the role of rotation