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 evolu tionary models and of the measured apsidal motion rate, the radii and masse s for the components of the extragalactic eclipsing binary HV 2274 in the L arge Magellanic Cloud. At that time the radial velocity curves were not ava ilable and the need of more complete observations to compare with the evolu tion theory was emphasized. Recently, through ground-based photometry, spec troscopy and spectrophotometry on board the Hubble Space Telescope the abso lute dimensions of that system were obtained. In this research note we perf orm a more complete comparison between observations and theoretical predict ions since the light and radial velocity curves are now available. The theo retical radii and apsidal motion rate inferred from models computed for the precise observed masses were found to be in good agreement with observatio nal data. The importance:of the case of HV 2274 lies mainly in the fact tha t this system is the first extragalactic binary system where it has been po ssible to investigate its surface astrophysical parameters as well as the t idal interactions using the techniques of apsidal motion.