BSN: Photometric Light Curve Analysis of Two Contact Binary Systems LS Del and V997 Cyg

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Poro A., Tanriver M., Sarvari E., Zavvarei S., Azarara H., Corp L., ...More

Research in Astronomy and Astrophysics, vol.24, no.4, 2024 (SCI-Expanded) identifier identifier

  • Publication Type: Article / Article
  • Volume: 24 Issue: 4
  • Publication Date: 2024
  • Doi Number: 10.1088/1674-4527/ad30b2
  • Journal Name: Research in Astronomy and Astrophysics
  • Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Aerospace Database, INSPEC
  • Keywords: (stars:) binaries: eclipsing, methods: observational, stars: individual (LS Del and V997 Cyg)
  • Çanakkale Onsekiz Mart University Affiliated: Yes


The light curve analyses and orbital period variations for two contact binary stars, LS Del and V997 Cyg, are presented in this work which was conducted in the frame of the Binary Systems of South and North project. Ground-based photometric observations were performed at two observatories in France. We used the Transiting Exoplanet Survey Satellite (TESS) data for extracting times of minima and light curve analysis of the target systems. The O − C diagram for both systems displays a parabolic trend. LS Del and V997 Cyg’s orbital periods are increasing at rates of dP/dt = 7.20 × 10−08 days yr−1 and dP/dt = 2.54 × 10−08 days yr−1, respectively. Therefore, it can be concluded that mass is being transferred from the less massive star to the more massive component with a rate of dM/dt = -1.96 × 10−7 M ⊙ yr−1 for the LS Del system, and dM/dt =-3.83 × 10−7 M ⊙ yr−1 for V997 Cyg. The parameters of a third possible object in the system are also considered. The PHysics Of Eclipsing BinariEs Python code was used to analyze the light curves. The light curve solutions needed a cold starspot due to the asymmetry in the LS Del system’s light curve maxima. The mass ratio, fill-out factor, and star temperature all indicate that both systems are contact binary types in this investigation. Two methods were applied to estimate the absolute parameters of the systems: one method relied on the parallax of Gaia DR3, and the other used a P − M relationship. The positions of the systems are also depicted on the M − L, M − R, q − L ratio, and log M tot − logJ 0 diagrams. We recommend that further observations and investigations be done on the existence of a fourth body in this system.