Determination of the axial rotation rate using apsidal motion for early-type eclipsing binaries

Because the modern theory of stellar structure and evolution has a sound observational basis, we can consider that the apsidal parameters k 2 computed in terms of this theory correctly reflect the radial density distribution in stars of different masses and spectral types. This allows us to address the problem of apsidal motion in close binary systems in a new way. Unlike the traditional approach, in this paper we use the observed apsidal periods U obs to estimate the angular axial velocities of components, r , at fixed model values of k 2 . We use this approach to analyse the observational data for 28 eclipsing systems with known U obs and early-type primaries (M 1.6 M or T e 6000 K). We measure the age of the system in units of the synchronization time, t/t syn .

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