A small survey for massive stars in the LMC/SMC: binaries and pulsations

Binarity and pulsations are two notable properties that frequently appear together in massive stars. To place constraints on how binarity affects stellar evolution, the exact parameters of massive stars in binary systems must be known. Their exact and accurate masses and radii, which were calculated from binary dynamics, present model-independent restrictions and challenge existing theories of stellar evolution. In this investigation, our goal is to determine the atmospheric characteristics of nine double-lined spectroscopic binaries that are located in the Large Magellanic Cloud and Small Magellanic Cloud. Nine newly discovered double-lined eclipsing binaries with B-type massive components have been studied; these binaries were found using the OGLE variable star catalogues. The absolute physical parameters of each component have been measured with an accuracy of less than or equal to 3 per cent. By analysing through Transiting Exoplanet Survey Satellite data of the systems, we were able to identify five candidates for slowly pulsating B stars in massive binary systems with masses ranging from 2 to 25 M-circle dot. According to the results of the preliminary research, the orbital periods of these binary systems span anywhere from 1.8 to 6.3 d, whereas the pulsating periods range anywhere from 0.3 to 1.5 d. The achievement in identifying a significant number of pulsating eclipsing systems opens the door to the initial sensible approach of constraining the internal physics of a group of massive stars via asteroseismology of eclipsing binaries including such stars.