NEW ASTRONOMY, cilt.96, sa.101848, ss.1-9, 2022 (SCI-Expanded)
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 ± 19.4 𝑝𝑐. 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 𝑙𝑜𝑔𝑇𝑒𝑓 𝑓 −𝑙𝑜𝑔𝐿, 𝑙𝑜𝑔𝑀 −𝑙𝑜𝑔𝐿, 𝑙𝑜𝑔𝑀 −𝑙𝑜𝑔𝑅
and 𝑙𝑜𝑔𝑀 − 𝑙𝑜𝑔𝐽0 diagrams