Light Curve Analysis of the AP Dor Binary System using Ground-Based and TESS Observations

Abstract

The short-period AP Dor eclipsing binary's first in-depth and multiband photometric solutions are presented. We made use of our eight nights of ground-based at a southern hemisphere observatory, and twelve sectors of TESS observations. We extracted eight and 1322 minima from our observations and TESS, respectively. We suggested a new linear ephemeris based on the trend of orbital period variations using the Markov chain Monte Carlo (MCMC) approach. The PHysics Of Eclipsing BinariEs (PHOEBE) Python code and the MCMC approach were used for the light curve analysis. This system did not require a starspot for the light curve solutions. We calculated the absolute parameters of the system using Gaia DR3 parallax method. The orbital angular momentum (J_0) of the AP Dor indicates that this system is located in a region of contact binaries. According to our results, this system is an overcontact binary system with a mass ratio of 0.584, a fillout factor of 48\%, and an inclination of 53deg. The positions of AP Dor stars on the Hertzsprung-Russell (HR) diagram are represented.

arXiv commentAccepted by the Research in Astronomy and Astrophysics (RAA) journal

References in corpus (8)

• emcee: The MCMC Hammer
• Measuring Reddening with SDSS Stellar Spectra and Recalibrating SFD
• Physics of Eclipsing Binaries. V. General Framework for Solving the Inverse Problem
• Eclipsing binaries in ASAS catalog
• Dynamical evolution of active detached binaries on log Jo - log M diagram and contact binary formation
• Empirical Bolometric Correction Coefficients for Nearby Main-Sequence Stars in Gaia Era
• Eclipsing Binaries in the OGLE Variable Star Catalog.I. W UMa-type Systems as Distance and Population Tracers in Baade's Window
• Investigation of the Orbital Period and Mass Relations for W UMa-type Contact Systems