The detached eclipsing binary TX Her revisited


Erdem A. , Aliçavuş F. , Soydugan F. , Dogru S. S. , Soydugan F. , Çiçek C., ...Daha Fazla

NEW ASTRONOMY, cilt.16, ss.498-502, 2011 (SCI İndekslerine Giren Dergi) identifier identifier

Özet

This paper presents new CCD Bessell BVRI light curves and photometric analysis of the Algol-type binary star TX Her. The CCD observations were carried out at Canakkale Onsekiz Mart University Observatory in 2010. New BVRI light curves from this study and radial velocity curves from Popper (1970) were solved simultaneously using modern light and radial velocity curves synthesis methods. The general results show that TX Her is a well-detached eclipsing binary, however, both component stars fill at least half of their Roche lobes. A significant third light contribution to the total light of the system could not be determined. Using O-C residuals formed by the updated minima times, an orbital period study of the system was performed. It was confirmed that the tilted sinusoidal O-C variation corresponds to an apparent period variation caused by the light travel time effect due to an unseen third body. The following absolute parameters of the components were derived: M(1) = 1.62 +/- 0.04 M(circle dot), M(2) = 1.45 +/- 0.03 M(circle dot), R(1) = 1.69 +/- 0.03 R(circle dot), R(2) = 1.43 +/- 0.03 R(circle dot), L(1) = 8.21 +/- 0.90 L(circle dot), and L(2) = 3.64 +/- 0.60 L(circle dot). The distance to TX Her was calculated as 155 +/- 10 pc, taking into account interstellar extinction. The position of the components of TX Her in the HR diagram are also discussed. The components are young stars with an age of similar to 500 Myr. (C) 2011 Elsevier B.V. All rights reserved.
This paper presents new CCD Bessell BVRI light curves and photometric analysis of the Algol-type binary star TX Her. The CCD observations were carried out at Çanakkale Onsekiz Mart University Observatory in 2010. New BVRI light curves from this study and radial velocity curves from Popper (1970) were solved simultaneously using modern light and radial velocity curves synthesis methods. The general results show that TX Her is a well-detached eclipsing binary, however, both component stars fill at least half of their Roche lobes. A significant third light contribution to the total light of the system could not be determined. Using O-C residuals formed by the updated minima times, an orbital period study of the system was performed. It was confirmed that the tilted sinusoidal O-C variation corresponds to an apparent period variation caused by the light travel time effect due to an unseen third body. The following absolute parameters of the components were derived: M1 = 1.62 ± 0.04 Msun, M2 = 1.45 ± 0.03 Msun, R1 = 1.69 ± 0.03 Rsun, R2 = 1.43 ± 0.03 Rsun, L1 = 8.21 ± 0.90 Lsun and L2 = 3.64 ± 0.60 Lsun. The distance to TX Her was calculated as 155 ± 10 pc, taking into account interstellar extinction. The position of the components of TX Her in the HR diagram are also discussed. The components are young stars with an age of ˜500 Myr.