2024/03/11 by И. А. Шапошников, Shaposhnikov, I. A., A. M. Cherepashchuk +5
Physics and Astronomy · #Gamma-ray bursts and supernovae #Stellar, planetary, and galactic studies #Astronomy and Astrophysical Research
paper · pdf · doi:10.48550/arxiv.2403.06473
We aim at searching for secular evolution of the orbital period in the short-period binary system WR 127 (WN3b+O9.5V, P = 9.555d). We performed new low-resolution spectroscopic observations of WR 127 on 2.5-m CMO SAI telescope to construct the radial velocity curves of the components suggesting the component masses MWRsin3(i) = 11.8±1.4 M\odot, MOsin3(i)=17.2±1.4 M\odot. The comparison with archival radial velocity curves enabled us to calculate the (O-C) plot with accuracy sufficient to search for the orbital period change in WR 127. We report on the reliable detection of a secular increase in the orbital period of WR 127 at a rate of P = 0.83±0.14~s~yr-1 corresponding to the dynamical mass-loss rate from the WR star MWR = (2.6±0.5)× 10-5 M\odot yr-1. The mass-loss rate from WR stars in three WR+OB binaries (WR 127, CX Cep and V444 Cyg) as inferred from spectroscopic and photometric measurements suggests a preliminary empirical correlation between the WR star mass and the dynamical mass-loss rate MWR∼ MWR1.8. This relation is important for the understanding of the evolution of massive close binaries with WR stars -- precursors of gravitational-wave binary merging events with neutron stars and black holes.