Gansicke, B. T.; Rodriguez-Gil, P.; Marsh, T. R.; de Martino, D.; Nestoras, J.; Szkody, P.; Aungwerojwit, A.; Barros, S. C. C.; Dillon, M.; Araujo-Betancor, S.; Arevalo, M. J.; Casares, J.; Groot, P. J.; Kolb, U.; Lazaro, C.; Hakala, P.; Martinez-Pais, I. G.; Nelemans, G.; Roelofs, G.; Schreiber, M. R.; van den Besselaar, E.; Zurita, C. and Monet, D.
A ZZ Ceti white dwarf in SDSS J133941.11+484727.5.
Monthly Notices of the Royal Astronomical Society, 365(3) pp. 969–976.
We present time-resolved spectroscopy and photometry of the cataclysmic variable (CV) SDSS J133941.11+484727.5 (SDSS 1339) which has been discovered in the Sloan Digital Sky Survey (SDSS) Data Release 4. The orbital period determined from radial velocity studies is 82.524(24) min, close to the observed period minimum. The optical spectrum of SDSS 1339 is dominated to 90 per cent by emission from the white dwarf (WD). The spectrum can be successfully reproduced by a three-component model (white dwarf, disc, secondary) with T-WD=12 500 K for a fixed log g= 8.0, d= 170 pc, and a spectral type of the secondary later than M8. The mass-transfer rate corresponding to the optical luminosity of the accretion disc is very low, similar or equal to 1.7 x 10(-13) M-circle dot yr(-1). Optical photometry reveals a coherent variability at 641 s with an amplitude of 0.025 mag, which we interpret as non-radial pulsations of the white dwarf. In addition, a long-period photometric variation with a period of either 320 or 344 min and an amplitude of 0.025 mag is detected, which bears no apparent relation with the orbital period of the system. Similar long-period photometric signals have been found in the CVs SDSS J123813.73-033933.0, SDSS J204817.85-061044.8, GW Lib and FS Aur, but so far no working model for this behaviour is available.
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