  We present preliminary results of long-term monitoring of the peculiar
cataclysmic variable FS Aurigae conducted during the 2010-2011 observational
season. The multicolor observations revealed, for the first time in photometric
data, the precession period of the white dwarf, previously seen only
spectroscopically. This is best seen in the (B-I) color index and reflects the
spectral energy distribution variability. Analysis of X-ray observations made
with Chandra and Swift, also revealed the existence of both the orbital and
precession periods in the light curve. We also show that the long-term
variability of FS Aur and the character of its outburst activity may be caused
by variations in the mass transfer rate from the secondary star as the result
of eccentricity modulation of a close binary orbit induced by the presence of a
third body on a circumbinary orbit.
