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, cilt.363, sa.4, ss.1272-1278, 2005 (SCI-Expanded) identifier identifier

  • Yayın Türü: Makale / Tam Makale
  • Cilt numarası: 363 Sayı: 4
  • Basım Tarihi: 2005
  • Doi Numarası: 10.1111/j.1365-2966.2005.09534.x
  • Dergi Adı: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
  • Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus
  • Sayfa Sayıları: ss.1272-1278
  • Anahtar Kelimeler: techniques : photometric, binaries : eclipsing, stars : fundamental parameters, stars : individual, V781 Tau, stars : individual, V836 Cyg, ECLIPSING BINARIES, MODELS, STARS
  • Çanakkale Onsekiz Mart Üniversitesi Adresli: Evet

Özet

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.