The first study of the light-travel time effect in massive LMC eclipsing binaries

TL;DR

This study investigates period changes in LMC eclipsing binaries using light-travel time effect analysis, revealing third bodies with orbital periods of 3.6 to 11.3 years and eccentricities up to 0.64, based solely on photometric data.

Contribution

First analysis of light-travel time effect in extragalactic eclipsing binaries, identifying third bodies and their orbital parameters using photometric observations.

Findings

Detected third bodies with orbital periods from 3.6 to 11.3 years.

Found high eccentricities up to 0.64 in some systems.

Identified systems with high mass functions and peculiar light curve variability.

Abstract

Aims: New CCD observations for semidetached and detached eclipsing binaries from the Large Magellanic Cloud were carried out using the Danish 1.54-m telescope located at the La Silla Observatory in Chile. The selected systems were monitored for their times of minima, which were required to be able to study the period changes taking place in them. In addition, many new times of minima were derived from the photometric surveys OGLE-II, OGLE-III, and MACHO. Methods: The O-C diagrams of minima timings were analysed using the hypothesis of the light-travel time effect, i.e. assuming the orbital motion around a common barycenter with the distant component. Moreover, the light curves of these systems were also analysed using the program PHOEBE, which provided the physical parameters of the stars. Results: For the first time, in this study we derived the relatively short periods of modulation in these systems, which relates to third bodies. The orbital periods resulted from 3.6 to 11.3 yr and the eccentricities were found to be up to 0.64. This is the first time that this kind of analysis for the set of extragalactic sources has been performed. The Wolf-Rayet system OGLE-LMC-ECL-08823 is the most mysterious one, owing to the resultant high mass function. Another system, OGLE-LMC-ECL-19996, was found to contain a third body with a very high mass (M3,min = 26M0). One system (OGLE-LMC-ECL-09971) is suspicious because of its eccentricity, and another one (OGLE-LMC-ECL-20162) shows some light curve variability, with a possible flare-like or microlensing-like event. Conclusions: All of these results came only from the photometric observations of the systems and can be considered as a good starting point for future dedicated observations.