Journal of Physical Studies 17(3), Article 3901 [7 pages] (2013) DOI: https://doi.org/10.30970/jps.17.3901 VARIABILITY OF THE SPIN PERIOD OF THE WHITE DWARF IN THE INTERMEDIATE POLAR V405 AUR: LOW-MASS THIRD BODY OR PRECESSION? V. V. Breus{1}, I. L. Andronov{1}, P. Dubovský{2}, S. V. Kolesnikov{3}, E. A. Zhuzhulina{4}, T. Heged&uH;s{5}, P. Beringer{5}, K. Petrík{6}, J. W. Robertson{7}, A. V. Ryabov{3}, I. Kudzej{2}, N. M. Shakhovskoy8 1Department ‟High and Applied Mathematics”, Odessa National Maritime University, Odessa, Ukraine, e-mail: vitaly.breus@gmail.com, tt\_ari@ukr.net 2Vihorlat Astronomical Observatory, Humenne, Slovakia 3Astronomical Observatory, Odessa National University, Odessa, Ukraine 4Department of Astronomy, Odessa National University, Odessa, Ukraine 5Baja Astronomical Observatory, Baja, Hungary 6Astronomical Observatory, Hlohovec, Slovakia 7Arkansas Tech University, Russellville, USA 8Crimean Astrophysical Observatory, Nauchny, Ukraine

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 $17.2\pm1.8$ sec. The periodic variations may be interpreted by a light-time effect caused by a low-mass star ($M_3\ge0.09M_☉$). In this case, the system belongs to a rare class of cataclysmic variables with a third body.

PACS number(s): 97.10.Gz, 97.10.Kc, 97.10.Ld, 97.30.Qt, 97.80.Gm, 97.82.Cp, 98.35.Mp

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