The First Photometric Study of W UMa Binary System V1833 Ori

Abstract

Abstract The first photometric solution in the B, V, R c and I c filters of the short period V1833 Ori eclipsing binary is presented based on new ground-based CCD photometric observations. We analyzed the BVRI photometric light curves of the system, using PHOEBE 0.31a, a binary star modeling program, with the Wilson-Devinney method based on Roche geometry to achieve the best accordance with 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 analyzed 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 × 10−7 days yr−1. The distance of V1833 Ori is 173.7 ± 15.6 pc. From the solutions, we find that V1833 Ori is an A-subtype W UMa overcontact binary with q = 0.701 mass ratio 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 log T eff − log L , logM − logL, logM − logR and log M − log J 0 diagrams.