BO Ari Light Curve Analysis using Ground-Based and TESS Data. (arXiv:2101.06265v1 [astro-ph.SR])
<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:+Zamanpour_S/0/1/0/all/0/1">Shiva Zamanpour</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hashemi_M/0/1/0/all/0/1">Maryam Hashemi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aladag_Y/0/1/0/all/0/1">Yasemin Aladağ</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aksaker_N/0/1/0/all/0/1">Nazim Aksaker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rezaei_S/0/1/0/all/0/1">Samaneh Rezaei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Solmaz_A/0/1/0/all/0/1">Arif Solmaz</a>
We present new BVR band photometric light curves of BO Aries obtained in 2020
and combined them with the Transiting Exoplanet Survey Satellite (TESS) light
curves. We obtained times of minima based on Gaussian and Cauchy distributions
and then applied the Monte Carlo Markov Chain (MCMC) method to measure the
amount of uncertainty from our CCD photometry and TESS data. A new ephemeris of
the binary system was computed employing 204 times of minimum. The light curves
were analyzed using the Wilson-Devinney binary code combined with the Monte
Carlo (MC) simulation. For this light curve solution, we considered a dark spot
on the primary component. We conclude that this binary is an A-type system with
a mass ratio of q=0.2074+-0.0001, an orbital inclination of i=82.18+-0.02 deg,
and a fillout factor of f=75.7+-0.8%. Our results for the a(Rsun) and q
parameters are consistent with the results of the Xu-Dong Zhang and Sheng-Bang
Qian (2020) model. The absolute parameters of the two components were
calculated and the distance estimate of the binary system was found to be
142+-9 pc.
We present new BVR band photometric light curves of BO Aries obtained in 2020
and combined them with the Transiting Exoplanet Survey Satellite (TESS) light
curves. We obtained times of minima based on Gaussian and Cauchy distributions
and then applied the Monte Carlo Markov Chain (MCMC) method to measure the
amount of uncertainty from our CCD photometry and TESS data. A new ephemeris of
the binary system was computed employing 204 times of minimum. The light curves
were analyzed using the Wilson-Devinney binary code combined with the Monte
Carlo (MC) simulation. For this light curve solution, we considered a dark spot
on the primary component. We conclude that this binary is an A-type system with
a mass ratio of q=0.2074+-0.0001, an orbital inclination of i=82.18+-0.02 deg,
and a fillout factor of f=75.7+-0.8%. Our results for the a(Rsun) and q
parameters are consistent with the results of the Xu-Dong Zhang and Sheng-Bang
Qian (2020) model. The absolute parameters of the two components were
calculated and the distance estimate of the binary system was found to be
142+-9 pc.
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