BVRI photometric observations, light curve solutions and orbital period analysis of BF Pav

• Autores: Poro, Atila; Alicavus, Fahri; Fernandez Lajus, Eduardo Eusebio; Davoudi, Fatemeh; MirshafieKhozani, PegahSadat; Blackford, Mark G.; Budding, Edwin; Jalalabadi, Behjat Zarei; Rahimi, Jabar; Farahani, Farzaneh Ahangarani
• Año de publicación: 2021
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: techniques: photometric; binaries: eclipsing; stars: individual (BF Pav)
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

A new ephemeris, period change analysis and light curve modeling of the W UMa-type eclipsing binary BF Pav are presented in this study. Light curves of the system taken in BVRI filters from two observatories, in Australia and Argentina, were modeled using the Wilson-Devinney code. The results of this analysis demonstrate that BF Pav is a contact binary system with a photometric mass ratio q = 1.460 ± 0.014, a fillout factor f = 12.5%, an inclination of 87.97 ± 0.45 deg and a cold spot on the secondary component. By applying the distance modulus formula, the distance of BF Pav was calculated to be d = 268 ± 18 pc which is in good agreement with the Gaia EDR3 distance. We obtain an orbital period increase at a rate of 0.142 s century−1 due to a quadratic trend in the O − C diagram. Also, an alternative sudden period jump probably occurred which could be interpreted as a rapid mass transfer from the lower mass star to its companion of about ∆M = 2.45×10−6 M. Furthermore, there is an oscillatory behavior with a period of 18.3 ± 0.3 yr. Since BF Pav does not seem to have significant magnetic activity, this behavior could be interpreted as the light-time effect caused by an undetected third body in this system. In this case, the probability for the third body to be a low mass star with M ≥ 0.075 M or a brown dwarf is 5.4% and 94.6% respectively. If we assume i0 = 90◦, a3 = 8.04 ± 0.33 AU. The mass of the secondary component was also determined following two different methods which result close to each other.
Fil: Poro, Atila. The International Occultation Timing Association Middle East section; Irán
Fil: Alicavus, Fahri. Canakkale Onsekiz Mart University; Turquía
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Davoudi, Fatemeh. The International Occultation Timing Association Middle East section; Irán
Fil: MirshafieKhozani, PegahSadat. The International Occultation Timing Association Middle East section; Irán
Fil: Blackford, Mark G.. Congarinni Observatory; Australia
Fil: Budding, Edwin. Université du Québec a Montreal; Canadá
Fil: Jalalabadi, Behjat Zarei. Carter Observatory; Nueva Zelanda
Fil: Rahimi, Jabar. The International Occultation Timing Association Middle; Irán
Fil: Farahani, Farzaneh Ahangarani. The International Occultation Timing Association Middle; Irán