BVRI Photometric Observations, Light Curve Solutions and Orbital Period Analysis of BF Pav
Abstract
A new ephemeris, period change analysis and light curve modeling of the W UMatype 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 WilsonDevinney 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 Δ 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 lighttime 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 i' = 90°, a_{3} = 8.04 ± 0.33 AU. The mass of the secondary component was also determined following two different methods which result close to each other.
 Publication:

Research in Astronomy and Astrophysics
 Pub Date:
 October 2021
 DOI:
 10.1088/16744527/21/8/203
 arXiv:
 arXiv:2008.05068
 Bibcode:
 2021RAA....21..203P
 Keywords:

 techniques: photometric;
 binaries: eclipsing;
 stars: individual (BF Pav);
 Astrophysics  Solar and Stellar Astrophysics
 EPrint:
 15 pages, 6 figures, 5 tables, Journal: accepted paper in RAA journal