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Published January 1, 2020 | Version v1
Journal article Open

Discovery of a pre-cataclysmic binary with unusual chromaticity of the eclipsed white dwarf by the GPX survey

Creators

  • 1. Ural Fed Univ, Ekaterinburg 620002, Russia
  • 2. Acton Sky Portal Private Observ, Acton, MA 01720 USA
  • 3. Moscow MV Lomonosov State Univ, Sternberg State Astron Inst, Univ Sky Prospect 13, Moscow 119992, Russia
  • 4. Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, Allee 6 Aout 19C, B-4000 Liege, Belgium
  • 5. Queens Univ Belfast, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland
  • 6. Univ Liege, Astrobiol Res Unit, Allee 6 Aout 19C, B-4000 Liege, Belgium
  • 7. Ankara Univ, Fac Sci, Dept Astron & Space Sci, TR-06100 Ankara, Turkey
  • 8. Cadi Ayyad Univ, High Energy Phys & Astrophys Lab, Oukaimeden Observ, Av Abdelkrim Khattabi, Marrakech 40000, Morocco
  • 9. Univ Siena, Astron Observ DSFTA, Via Roma 56, I-53100 Siena, Italy
  • 10. Wild Boar Remote Observ, I-50026 San Casciano In Val Di P, FI, Italy

Description

We report the discovery of a relatively bright eclipsing binary system, which consists of a white dwarf (WD) and a main-sequence K7 star with clear signs of chromospheric and spot activity. The light curve of this system shows similar to 0.2 mag ellipsoidal variability with a period of 0.297549 d and a short total eclipse of the WD. Based on our analysis of the spectral and photometric data, we estimated the parameters of the system. The K7V star is tidally deformed but does not fill its Roche lobe (the filling factor is about 0.86). The orbital inclination is i = 73 degrees.1 +/- 0 degrees.2, and the mass ratio is q = M-2/M-1 approximate to 0.88. The parameters of the K7V star are M-2 approximate to 0.64 M-circle dot, R-2 = 0.645 +/- 0.012R(circle dot), and T-2 approximate to 4070 K. The parameters of the WD are M-1 approximate to 0.72M(circle dot), R-1 = 0.013 +/- 0.003R(circle dot), and T-1 = 8700 +/- 1100 K. Photometric observations in different bands revealed that the maximum depth of the eclipse is in the SDSS r filter, which is unusual for a system of a WD and a late main-sequence star. We suspect that this system is a product of the evolution of a common-envelope binary star, and that the WD accretes the stellar wind from the secondary star (the so-called low-accretion-rate polar, hereafter LARP).

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