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We report the results of a twenty-eight-month photometric campaign studyingV1432 Aql, the only known eclipsing, asynchronous polar. Our data show thatboth the residual eclipse flux and eclipse O-C timings vary strongly as afunction of the spin-orbit beat period. Relying upon a new model of the system,we show that cyclical changes in the location of the threading region along theballistic trajectory of the accretion stream could produce both effects. Thismodel predicts that the threading radius is variable, in contrast to previousstudies which have assumed a constant threading radius. Additionally, weidentify a very strong photometric maximum which is only visible for half ofthe beat cycle. The exact cause of this maximum is unclear, but we consider thepossibility that it is the optical counterpart of the third accreting polecapproposed by Rana et al. (2005). Finally, the rate of change of the whitedwarf's spin period is consistent with it being proportional to the differencebetween the spin and orbital periods, implying that the spin period isapproaching the orbital period asymptotically.

Periodic Variations in the Residual Eclipse Flux and Eclipse Timings of Asynchronous Polar V1432 Aql: Evidence of a Shifting Threading Region