Investigation of an eclipsing binary star V1848 Orionis

Abstract

The aim of this research is to study the variation in the orbital period and the physical parameters of the eclipsing binary system V1848 Orionis. The data for this study were observed and collected at the Thai National Observatory (TNO) and the Regional Observatory for Public, Chachoengsao (ROP-CCO) operated by the National Astronomical Research Institute of Thailand (NARIT) in the B, V, R and I bands throughout December 2022. The OC diagram shows the period variation due to the third component. The properties of the third mass were calculated as 0.23±0.02 M⊙ with an orbital radius (a3sini′) of 5.2 ± 0.3 AU and a period variation of 8.7 ± 0.2 years. Our findings indicate that the light curves show asymmetry. The analysis of V1848 Orionis' light curve using the Wilson-Devinney code revealed a mass ratio of 0.756 ± 0.007, an inclination of 76.4°±0.1°, and a 9.28 % degree of contact. Furthermore, we identified a hot spot on the primary component, associated with the O'Connell effect variation. The completeness of the multi-light curves indicates the high reliability of the determined physical parameters. The masses, radii, and luminosities of the primary and secondary components are estimated to be M1 = 0.91±0.10 M⊙, M2 = 0.69±0.07 M⊙, R1 = 0.84±0.03 R⊙, R2 = 0.74±0.03 R⊙, L1 = 0.83±0.06 L⊙, and L2 = 0.54±0.04 L⊙. The evolutionary statuses of both components in the Hertzsprung-Russell diagram show that they are either normal stars or minimally evolved stars.