2006A&A...452..941A

Result. of a CCD study of the variability of the unique magnetic cataclysmic variable V1432 Aql from the Astronomical Observatory of Mallorca are presented. The ``multi-comparison star'' method had been applied for better accuracy estimates. The linear ephemeris based on 76 timings of orbital eclipses for 1993-2004 is HJD<sub>min</sub>=2451492.09876(14)+0.140235812(12)E. For the wide minima due to the spin variability, the quadratic ephemeris HJD<sub>spin</sub>=2449638.327427(74)+0.14062831(23)E -7.81(11)x10<sup>–10</sup>E<sup>2</sup> was determined. The rate of the spin-up of the white dwarf corresponds to the synchronization time-scale determined to be (96.7±1.5) years, in an agreement with theoretical model of the accretion torque. A third type of minima was detected that occur with the spin period. It was interpreted as indicating presence of the second accretion column. For adopted values of mass M<sub>1</sub>=0.9 M<sub>☉</sub> and M<sub>2</sub>=0.3M<sub>☉</sub>, the estimated accretion rate is ∼7x10<sup>–10</sup>M<sub>☉</sub>/yr. Further multi-colour monitoring is needed to study of late stages of the ``spin-orbital'' synchronization and periodic changes of the accretion geometry caused by ``idling'' of the white dwarf.