BVRI Photometric Observations, Light Curve Solutions and Orbital Period Analysis of BF Pav. (arXiv:2008.05068v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Poro_A/0/1/0/all/0/1">Atila Poro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blackford_M/0/1/0/all/0/1">Mark G. Blackford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alicavus_F/0/1/0/all/0/1">Fahri Alicavus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davoudi_F/0/1/0/all/0/1">Fatemeh Davoudi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MirshafieKhozani_P/0/1/0/all/0/1">PegahSadat MirshafieKhozani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandez_Lajus_E/0/1/0/all/0/1">Eduardo Fern&#xe1;ndez-Laj&#xfa;s</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rahimi_J/0/1/0/all/0/1">Jabar Rahimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jalalabadi_B/0/1/0/all/0/1">Behjat Zarei Jalalabadi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Farahani_F/0/1/0/all/0/1">Farzaneh Ahangarani Farahani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Budding_E/0/1/0/all/0/1">Edwin Budding</a>

The new ephemeris and light curve analysis by synthesizing our mid-eclipse
times and the former observations of BF Pav, that is classified as a W UMa-type
eclipsing binary, are presented in this study. We also obtain this binary
system’s period changes using the Wilson-Devinney code after eight nights of
observation in BVRI filters from two observatories in Australia and Argentina.
Our results demonstrate that BF Pav is a contact binary system with a
photometric mass ratio q=1.459(20), a fillout factor f=9.9%, and an inclination
of 89.31 when in the light curve solutions we have a cold spot. We also
calculated the distance of BF Pav d=240+-21 pc from the distance modulus
formula, which is in good agreement with the distance obtained from this binary
system’s parallax in Gaia DR2. From our O-C analysis, we found a continuous
period increase at a rate of 0.3079288 . (10)^(-7) days/year which corresponds
to a period increase of 0.266 s (century)^(-1). We determined the mass of the
primary component of this binary system using two different methods.

The new ephemeris and light curve analysis by synthesizing our mid-eclipse
times and the former observations of BF Pav, that is classified as a W UMa-type
eclipsing binary, are presented in this study. We also obtain this binary
system’s period changes using the Wilson-Devinney code after eight nights of
observation in BVRI filters from two observatories in Australia and Argentina.
Our results demonstrate that BF Pav is a contact binary system with a
photometric mass ratio q=1.459(20), a fillout factor f=9.9%, and an inclination
of 89.31 when in the light curve solutions we have a cold spot. We also
calculated the distance of BF Pav d=240+-21 pc from the distance modulus
formula, which is in good agreement with the distance obtained from this binary
system’s parallax in Gaia DR2. From our O-C analysis, we found a continuous
period increase at a rate of 0.3079288 . (10)^(-7) days/year which corresponds
to a period increase of 0.266 s (century)^(-1). We determined the mass of the
primary component of this binary system using two different methods.

http://arxiv.org/icons/sfx.gif