The first photometric analysis study of the GW Psc binary system

Abstract

The first photometric solution in the B,V,Rc and Ic filters of the short period GW Psc 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 (Wilson and Devinney (1971); Wilson (1979) method based on Roche geometry to achieve the best accordance to the photometric observations to estimate their absolute parameters from the light curves. We updated the ephemeris of GW Psc 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 plot suggests the presence of a companion. The distance of GW Psc are 318.4±19.4pc. From the solutions, we find that GW Psc is A–subtype W UMa over-contact binaries with q=0.399 mass ratios and f=0.21 fill–out factor. The likely HR diagram positions of the eclipsing binary system’s components are discussed. The system’s estimated absolute dimensions were compared to those of similar binaries in the logTeff−logL, logM−logL, logM−logR and logM−logJ0 diagrams.