The First Photometric Study of W UMa Binary System V1833 Ori

Abstract

The first photometric solution in the B, V, Rc and Ic filters of the short period V1833 Ori eclipsing binary is presented based on new ground-based CCD photometric observations. We analysed the BVRI photometric light curves of the system, using Phoebe0.31a, a binary star modelling program, with the Wilson and Devinney method based on Roche geometry to achieve the best accordance to the photometric observations to determine their absolute parameters from the light curves. We updated the ephemeris of V1833 Ori using two new light curve minima derived by our new observational data from those collected in the literature and analysed the change of the system’s orbital period. The O–C analysis indicates that the variations of the orbital period of V1833 Ori with time are increasing at a rate of 3.03 × 10−7days yr−1. The distance of V1833 Ori are 173.7 ± 15.6 pc. From the solutions, we find that V1833 Ori is A–subtype W UMa over-contact binaries with q = 0.701 mass ratios and f = 1.14 fill–out factor. The HR diagram positions of the eclipsing binary system’s components are discussed. The system’s absolute dimensions were compared to those of similar binaries in the logTef f − logL, logM − logL, logM − logR and logM − logJ0 diagrams.