The First Light Curve Solutions and Period Study of BQ Ari. (arXiv:2006.00528v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Poro_A/0/1/0/all/0/1">A. Poro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davoudi_F/0/1/0/all/0/1">F. Davoudi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basturk_O/0/1/0/all/0/1">O Basturk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Esmer_E/0/1/0/all/0/1">E. M. Esmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aksaker_N/0/1/0/all/0/1">N. Aksaker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akyuz_A/0/1/0/all/0/1">A. Akyüz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aladag_Y/0/1/0/all/0/1">Y. Aladağ</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rahimi_J/0/1/0/all/0/1">J. Rahimi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lashgari_E/0/1/0/all/0/1">E. Lashgari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ghanbarzadehchaleshtori_M/0/1/0/all/0/1">M. Ghanbarzadehchaleshtori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Modarres_S/0/1/0/all/0/1">S. Modarres</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sojoudizadeh_A/0/1/0/all/0/1">A. Sojoudizadeh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boudesh_A/0/1/0/all/0/1">A. Boudesh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Solmaz_A/0/1/0/all/0/1">A. Solmaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tekes_M/0/1/0/all/0/1">M. Tekeş</a>
The first complete analysis of the photometric observation of the W UMa type
binary system BQ Ari was performed using the Wilson-Devinney code to determine
its photometric and geometric elements. These results show that BQ Ari is a
contact W UMa binary system with a photometric mass ratio q = 0.91, and the
fillout factor equal to 34 percent. We calculated the distance of BQ Ari to be
146.24 pm 15 parsec. In this study, we suggested a new linear ephemeris for BQ
Ari, combining our new mid-eclipse times and the previous observations. We
present the first complete analysis of the system’s orbital period behavior and
analysis of the O-C diagram using the Genetic Algorithm (GA) and the Monte
Carlo Markov Chain (MCMC) approaches in OCFit code. We applied two approaches
to analyze the sinusoidal trend in the O-C diagram. This may suggest a periodic
change caused by the Light-Time Effect (LiTE) effect with a period of 4.60
years and an amplitude of 6.212 minutes. On the other hand, the sinusoidal
trend may indicate the existence of magnetic activity in this system. The
period of magnetic activity was calculated to be 4.16 years and changes of
period induced by magnetic activity obtained as DeltaP/P=4.36x 10^(-7). It was
concluded that magnetic activity is more likely to be the causal agent as
opposed to the LiTE signals.
The first complete analysis of the photometric observation of the W UMa type
binary system BQ Ari was performed using the Wilson-Devinney code to determine
its photometric and geometric elements. These results show that BQ Ari is a
contact W UMa binary system with a photometric mass ratio q = 0.91, and the
fillout factor equal to 34 percent. We calculated the distance of BQ Ari to be
146.24 pm 15 parsec. In this study, we suggested a new linear ephemeris for BQ
Ari, combining our new mid-eclipse times and the previous observations. We
present the first complete analysis of the system’s orbital period behavior and
analysis of the O-C diagram using the Genetic Algorithm (GA) and the Monte
Carlo Markov Chain (MCMC) approaches in OCFit code. We applied two approaches
to analyze the sinusoidal trend in the O-C diagram. This may suggest a periodic
change caused by the Light-Time Effect (LiTE) effect with a period of 4.60
years and an amplitude of 6.212 minutes. On the other hand, the sinusoidal
trend may indicate the existence of magnetic activity in this system. The
period of magnetic activity was calculated to be 4.16 years and changes of
period induced by magnetic activity obtained as DeltaP/P=4.36x 10^(-7). It was
concluded that magnetic activity is more likely to be the causal agent as
opposed to the LiTE signals.
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