Basic physical properties of the low-temperature contact binary system V781 Tau and the near-contact binary system V836 Cyg

YAKUT K., Ulas B., KALOMENI B., GULMEN O.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol.363, no.4, pp.1272-1278, 2005 (SCI-Expanded) identifier identifier

  • Publication Type: Article / Article
  • Volume: 363 Issue: 4
  • Publication Date: 2005
  • Doi Number: 10.1111/j.1365-2966.2005.09534.x
  • Journal Name: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
  • Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus
  • Page Numbers: pp.1272-1278
  • Keywords: techniques : photometric, binaries : eclipsing, stars : fundamental parameters, stars : individual, V781 Tau, stars : individual, V836 Cyg, ECLIPSING BINARIES, MODELS, STARS
  • Çanakkale Onsekiz Mart University Affiliated: Yes

Abstract

We present a detailed photometric study of the low-temperature contact binary V781 Tau, and the near-contact binary V836 Cyg. We have combined the parameters obtained from the light-curve analysis with those found by the spectral studies and we have determined the orbital and physical parameters of the stars. We have collected the times of the mid-eclipses obtained so far and combined with the times obtained in this study. By analysing all these data we determined the mass transfer rate from the massive star to the less massive one for V781 Tau, and from the less massive component to the massive one in the case of V836 Cyg. Finally, we have compared the results obtained for V781 Tau and for V836 Cyg with similar systems.We present a detailed photometric study of the low-temperature contact binary V781 Tau, and the near-contact binary V836 Cyg. We have combined the parameters obtained from the light-curve analysis with those found by the spectral studies and we have determined the orbital and physical parameters of the stars. We have collected the times of the mid-eclipses obtained so far and combined with the times obtained in this study. By analysing all these data we determined the mass transfer rate from the massive star to the less massive one for V781 Tau, and from the less massive component to the massive one in the case of V836 Cyg. Finally, we have compared the results obtained for V781 Tau and for V836 Cyg with similar systems.