Monitoring the Period Variation of KR Cyg Eclipsing Binary

TL;DR

This paper investigates the period variation of the near-contact eclipsing binary KR Cyg, analyzing historical and new data to identify long-term and cyclical changes possibly caused by a tertiary component.

Contribution

The study provides updated eclipse timings and (O-C) analysis of KR Cyg, suggesting a tertiary companion influencing the system's period variations.

Findings

Detection of long-term period trends

Identification of cyclical oscillations in the (O-C) diagram

Evidence supporting a tertiary component affecting the system

Abstract

This study examines the period variation of the eclipsing binary system KR Cyg, a near-contact binary characterized by its short orbital period and significant stellar interactions. The precise orbital parameters of the system have been determined through light curve data collected periodically since 1999 and were published in our previous studies. Additionally, minimum light observations have been continuously monitored to analyze the period variation of the system. In our earlier work, the masses of the primary and secondary components were determined as $2.88\pm0.20 M_{\odot}$ and $1.26\pm 0.07 M_{\odot}$, with corresponding radii of $2.59\pm 0.06 R_{\odot}$ and $1.80\pm 0.04 R_{\odot}$. The bolometric albedo and effective temperature of the less massive star were also investigated, and deviations caused by mutual illumination effects were identified. These results provide valuable insights into the evolutionary status of KR Cyg and shed light on the dynamic processes that occur in near-contact binary systems. Using updated eclipse timings, an (O-C) diagram was constructed, revealing both long-term trends and periodic oscillations. These cyclical variations are thought to indicate the presence of a tertiary component affecting the system via the light-time effect. Additional observations and modeling are recommended to confirm the tertiary hypothesis and further refine the parameters of the system.