  Cataclysmic Variables (CV) are close binary systems, in which the primary,
the more massive star, is a white dwarf. CVs usually exhibit a number of
periodicities, most of which are now understood. However, recently, a new
phenomenon was discovered that does not fit the standard picture. Two objects
have been discovered to show periods that are much longer than orbital, and
have no relation to it, either in light curves or in radial velocity (RV)
variations measured from spectroscopy. Here, we show that the precession of the
fast rotating magnetically accreting white dwarf can successfully explain these
phenomena. The theory of compact objects predicts certain relations between the
spin and precession periods, and our finding provides a good test for the
theory and establishes a qualitative model to be explored both theoretically
and observationally. Detection of precession can become a powerful tool in
searching for the internal properties of compact stars, which would be
otherwise inaccessible for us.
