  Precession is observed routinely in solid bodies of Solar system and it has
been invoked to explain number of phenomena observed in pulsars (i.e. Link
2003, Breton et al. 2008). White dwarfs also have been considered as possible
candidates of precessing stellar objects. In slowly rotating compact stars, the
precession period is extremely long and the amplitude of precession is small.
However, in rapid rotating neutron stars and white dwarfs, the precession
period is still within reasonable observational limits and can explain observed
periodicities exceeding spin periods by several times.
