RVs of 5 binaries with fast-rotating OB stars

We aim to characterize these binary systems in order to understand the causes behind their markedly different spectral line widths, providing observational clues as to the physical mechanisms at play. We used new and archival multi-epoch high-resolution optical spectra for the radial velocity analysis and determined the spectroscopic orbits of both components in five systems: HD 57236, HD 93028, HD 101413, HD 151003, and HD 153426.

The physical properties of the individual stellar components were determined through quantitative analysis. Using evolutionary models, we estimated the age of the systems and explored their tidal evolution. The systems consist of O+O or O+B stars, with minimum masses ranging from ~6M_{sun}_ to 21M_{sun}_, in young, wide, and fairly eccentric orbits (periods from approximately 22 to 977d and eccentricities of e>0.14).