An extensive photometric study of the recently discovered intermediate polar V647 Aur (1RXS J063631.9+353537)

TL;DR

This extensive photometric study of V647 Aur reveals multiple oscillations indicating the white dwarf's spin and orbital sidebands, and measures a decreasing spin period, providing new insights into its accretion dynamics.

Contribution

First detailed photometric analysis of V647 Aur identifying multiple oscillations and measuring the white dwarf's decreasing spin period.

Findings

Detected three oscillations with specific periods related to spin and orbital sidebands.

Measured the decreasing spin period of the white dwarf in V647 Aur.

Provided oscillation ephemeredes for future confirmation.

Abstract

We report the results of photometry of the intermediate polar V647 Aur. Observations were obtained over 42 nights in 2012 and 2013. The total duration of the observations was 246 h. We clearly detected three oscillations with periods of 932.9123+\-0.0011, 1008.30797+\-0.00038 and 1096.955+\-0.004 s, which may be the white dwarf spin period and two orbital sidebands, accordingly. The oscillation with a period of 932.9123 s has a quasi-sinusoidal pulse profile with a slightly changeable semi-amplitude from 10.9 mmag in 2012 to 12.5 mmag in 2013. The oscillation with a period of 1008.30797 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 (26-77 mmag) and in a time-scale of years (47 mmag in 2012 and 34 mmag in 2013). The oscillation with a period of 1096.955 s has a highly asymmetric pulse profile with a semi-amplitude of about 6 mmag. The three detected oscillations imply an orbital period of 3.46565+\-0.00006 h. By comparing our data with the data of B. T. Gansicke 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+\-0.08) X 10^-10. This important result should be confirmed by future observations. Our oscillation ephemeredes and times of maxima can be useful for this confirmation.