New Data on the Eclipsing Binary V1848 Ori and Improved Orbital and Light Curve Solutions

Fatemeh Davoudi,Hassan Ashta,Milad Jamali,Faezeh Jahediparizi,Afshin Halavati,Seyed Mohsen Shojaatalhosseini,Amirmohammad Salajeghe,Arman Pishahang,Atila Poro,Sareh Vahedi,Fahri Alicavus,Maryam Zare,Saeed Doostmohammadi,Amirabbas Shahdadi

doi:10.1515/astro-2020-0013

Fatemeh Davoudi, Hassan Ashta + Show 12 more

Open Access

https://doi.org/10.1515/astro-2020-0013

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Abstract

Abstract New observations of the eclipsing binary system V1848 Ori were carried out using the V filter resulting in a determination of new times of minima and new ephemeris were obtained. We presented the first complete analysis of the system’s orbital period behavior and analysis of O-C diagram done by the GA and MCMC approaches in OCFit code. The O-C diagram demonstrates a sinusoidal trend in the data; this trend suggests a cyclic change caused by the LITE effect with a period of 10.57 years and an amplitude of 7.182 minutes. It appears that there is a third body with mass function of f (m 3) = 0.0058 M⊙ in this binary system. The light curves were analyzed using the Wilson-Devinney code to determine some geometrical and physical parameters of the system. These results show that V1848 Ori is a contact W UMa binary system with the mass ratio of q = 0.76 and a weak fillout factor of 5.8%. The O’Connell effect was not seen in the light curve and there is no need to add spot.

Highlights

A-type subclass of W UMa binaries (Kriwattanawong and Poojon 2014).The system V1848 Orion (GSC 0107-0596) is classified as a W UMa type binary
O-C diagram demonstrates a sinusoidal trend in the data; this trend suggests a cyclic change caused by the Light-Time Effect (LITE) effect with a period of 10.57 years and an amplitude of 7.182 minutes
The light curves were analyzed using the Wilson-Devinney code to determine some geometrical and physical parameters of the system. These results show that V1848 Ori is a contact W UMa binary system with the mass ratio of q = 0.76 and a weak fillout factor of 5.8%

Summary

Introduction

A-type subclass of W UMa binaries (Kriwattanawong and Poojon 2014). The system V1848 Orion (GSC 0107-0596) is classified as a W UMa type binary. We suggest a new model for the variations observed in the orbital period of the binary. F. Davoudi et al, New Data on the Eclipsing Binary V1848 Ori and Improved Orbital and Light Curve Solutions. Mid-eclipse times identified as Min (BJDTDB) are in column 1; their uncertainties appear in column 2 (we calculated the average error amount for data points which other observers didn’t compute their uncertainties); epochs of these minima times in column 3, O-C values in column 4, filters used in column 5; and the references of mid-eclipse times in the last column. Final values together with their statistically significant uncertainties are obtained using MCMC fitting The combination of these two algorithms allows us to analyze the exact physical model of the observed variations.

Light curve analysis

Results