We report the results of photometry of the intermediate polar V647Â Aur .
Observations were obtained over 42 nights in 2012 and 2013 .
The total duration of the observations was 246Â h. We clearly detected three oscillations with periods of 932.9123 \pm 0.0011 , 1008.307 97 \pm 0.000 38 and 1096.955 \pm 0.004 Â s , which may be the white dwarf spin period and two orbital sidebands , accordingly .
The oscillation with a period of 932.9123Â s has a quasi-sinusoidal pulse profile with a slightly changeable semi-amplitude from 10.9Â mmag in 2012 to 12.5Â mmag in 2013 .
The oscillation with a period of 1008.307 97Â s has a slightly asymmetric pulse profile with a remarkable small hump on the ascending part .
The semi-amplitude of this oscillation is highly changeable both in a time-scale of days ( 26–77Â mmag ) and in a time-scale of years ( 47Â mmag in 2012 and 34Â mmag in 2013 ) .
The oscillation with a period of 1096.955Â s has a highly asymmetric pulse profile with a semi-amplitude of about 6Â mmag .
The three detected oscillations imply an orbital period of 3.46565 \pm 0.00006  h. By comparing our data with the data of B. T. Gänsicke et al. , which were obtained 8 years ago , we discovered that the spin period of the white dwarf in V647 Aur decreases with dP / dt = ( -1.36 \pm 0.08 ) \times 10 ^ { -10 } .
This important result should be confirmed by future observations .
Our oscillation ephemeredes and times of maxima can be useful for this confirmation .