2024A&A...683L..17S

Aims. We aim to determine the secular evolution of the orbital period of the short-period binary system WR 127 (WN3b+O9.5V, P ≈ 9.555^d).
Methods. We performed new low-resolution spectroscopic observations of WR 127 with the 2.5 m CMO SAI telescope to construct the radial velocity curves of the components. Our results suggest component masses of M_WRsin³(i) = 11.8 ± 1.4 M_⊙ and M_Osin³(i) = 17.2 ± 1.4 M_⊙. By comparing these values with archival radial velocity curves we were able to create an (O - C) plot with an accuracy sufficient to search for the orbital period change in WR 127.
Results. We report the reliable detection of a secular increase in the orbital period of WR 127 at a rate of Ṗ = 0.83 ± 0.14 s yr^–1, which corresponds to a dynamical mass-loss rate from the Wolf-Rayet (WR) star of Ė_WR = (2.6 ± 0.5) × 10^–5M_⊙ yr^–1.
Conclusions. The mass-loss rate from WR stars in three Wolf-Rayet+OB binaries (WR 127, CX Cep, and V444 Cyg) as inferred from spectroscopic and photometric measurements suggests a preliminary empirical correlation between a WR star's mass and its dynamical mass-loss rate of $ \dot M_{\mathrm{WR}}\sim M_{\mathrm{WR}}^{1.8} $. This relation is important for the understanding of the evolution of massive close binaries that include WR stars as such an evolution is a precursor of gravitational-wave binary merging events with neutron stars and black holes.