We present the results of photometric CCD observations of the magnetic cataclysmic variable V405 Aurigae ( RX J0558.0+5353 = 1RXS J055800.7+535358 ) obtained using different instruments .
We analysed variability of the spin period of the white dwarf in the V405 Aur ( RX J0558.0+5353 ) system using our observations and previously published maxima timings .
The spin period of the system in 2010-2012 is P = 545.4558163 ( 94 ) s. As we have gaps in observational data , we present 2 hypotheses of the spin period variability of this system - a cubic ephemeris which may be interpreted by a precession of the magnetic white dwarf or a periodic change with a period of 6.2 years and semi-amplitude of 17.2 \pm 1.8 sec .
The periodic variations may be interpreted by a light-time effect caused by a low-mass star ( M _ { 3 } \geq 0.09 M _ { \odot } ) .
In this case , the system belongs to a rare class of cataclysmic variables with a third body . Key words : stars : binaries : close - stars : novae , cataclysmic variables - stars : individual ( V405 Aurigae ) - stars : binaries : close - accretion disks - novae , cataclysmic variables