2025A&A...702A.274R

Context. The eccentric short-period O-star binary BD+60° 497 is an interesting laboratory in which to study tidal interactions in massive binary systems, notably via the detection and characterisation of apsidal motion.
Aims. The rate of apsidal motion in such systems can help constrain their age and provide insight into the degree of mass concentration in the interior of massive stars.
Methods. We used spectroscopic data collected over two decades to reconstruct the individual spectra of the stars and to establish their epoch-dependent radial velocities. An orbital solution, explicitly accounting for apsidal motion was adjusted to the data. Space-borne photometric time series were analysed with Fourier methods and with binary models.
Results. We derived a rate of apsidal motion of $ \dot{\omega} = (6.15^{+1.05}_{-1.65})\circ $ yr^–1, which suggests an age of $ 4.13^{+0.42}_{-1.37} $ Myr. The disentangled spectra unveiled a curious change in the spectral properties of the secondary star between the epochs 2002-2003 and 2018-2022, with the secondary spectrum appearing to be of an earlier spectral type over recent years. Photometric data show variability at the ∼6 mmag level on the period of the binary system, which is hard to explain in terms of proximity effects.
Conclusions. Whilst the rate of apsidal motion agrees well with theoretical expectations, the changes in the reconstructed secondary spectrum hint at a highly non-uniform surface temperature distribution for this star. Different effects are discussed that could contribute to the photometric variations. The current most-likely explanation is a mix of proximity effects and tidally excited oscillations.