Absolute Dimensions and Apsidal Motion of the Eccentric Binary V731 Cephei
V. Bakis, M. Zejda, I. Bulut, M. Wolf, S. Bilir, H. Bakis, O., Demircan, J. W. Lee, M. Slechta, B. Kucerova

TL;DR
This paper provides a comprehensive analysis of the eccentric binary V731 Cephei, determining its physical parameters, apsidal motion, internal structure, and evolutionary status, suggesting a possible origin from the nearby open cluster NGC 7762.
Contribution
The study offers new spectroscopic and photometric data, precise measurements of stellar and orbital parameters, and insights into the system's internal structure and evolution, including apsidal motion analysis.
Findings
Masses: M1=2.577 M☉, M2=2.017 M☉
Apsidal motion period: ~10,000 years
Relativistic contribution to apsidal motion: 76%
Abstract
A detailed analysis of new and existing photometric, spectroscopic and spatial distribution data of the eccentric binary V731 Cep was performed. Spectroscopic orbital elements of the system were obtained by means of cross-correlation technique. According to the solution of radial velocities with UBVRcIc light curves, V731 Cep consists of two main-sequence stars with masses M=2.577 (0.098) M, M=2.017 (0.084) M, radii R=1.823 (0.030) R, R=1.717 (0.025) R, and temperatures T=10700 (200) K, T=9265 (220) K separated from each other by a=23.27 (0.29) R in an orbit with inclination of 88.70 (0.03). Analysis of the O--C residuals yielded a rather long apsidal motion period of U=10000(2500) yr compared to the observational history of the system. The relativistic contribution to the observed…
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