A theoretical study of tidal interaction of the eclipsing binary HV 2274 in the Large Magellanic Cloud

About three years ago we did predict, only on the base of theoretical evolutionary models and of the measured apsidal motion rate, the radii and masses for the components of the extragalactic eclipsing binary HV 2274 in the Large Magellanic Cloud. At that time the radial velocity curves were not available and the need of more complete observations to compare with the evolution theory was emphasized. Recently, through ground-based photometry, spectroscopy and spectrophotometry on board the Hubble Space Telescope the absolute dimensions of that system were obtained. In this research note we perform a more complete comparison between observations and theoretical predictions since the light and radial velocity curves are now available. The theoretical radii and apsidal motion rate inferred from models computed for the precise observed masses were found to be in good agreement with observational data. The importance:of the case of HV 2274 lies mainly in the fact that this system is the first extragalactic binary system where it has been possible to investigate its surface astrophysical parameters as well as the tidal interactions using the techniques of apsidal motion.