Phase resolved X-ray spectroscopy of HDE228766: Probing the wind of an extreme Of+/WNLha star

TL;DR

This study uses phase-resolved X-ray spectroscopy and optical data to analyze the wind interactions in the massive binary system HDE228766, revealing wind properties, orbital inclination, and the nature of the wind collision zone.

Contribution

First detailed phase-resolved X-ray spectral analysis of HDE228766, constraining stellar wind parameters and orbital inclination in a massive binary system.

Findings

Wind-wind collision causes observable X-ray absorption variations.

Orbital inclination constrained to 54-61 degrees.

Secondary wind momentum exceeds primary by at least a factor of 5.

Abstract

HDE228766 is a very massive binary system hosting a secondary component, which is probably in an intermediate evolutionary stage between an Of supergiant and an WN star. The wind of this star collides with the wind of its O8 II companion, leading to relatively strong X-ray emission. Measuring the orbital variations of the line-of-sight absorption toward the X-ray emission from the wind-wind interaction zone yields information on the wind densities of both stars. X-ray spectra have been collected at three key orbital phases to probe the winds of both stars. Optical photometry has been gathered to set constraints on the orbital inclination of the system. The X-ray spectra reveal prominent variations of the intervening column density toward the X-ray emission zone, which are in line with the expectations for a wind-wind collision. We use a toy model to set constraints on the stellar wind parameters by attempting to reproduce the observed variations of the relative fluxes and wind optical depths at 1 keV. The lack of strong optical eclipses sets an upper limit of about 68 degrees on the orbital inclination. The analysis of the variations of the X-ray spectra suggests an inclination in the range 54 - 61 degrees and indicates that the secondary wind momentum ratio exceeds that of the primary by at least a factor 5. Our models further suggest that the bulk of the X-ray emission arises from the innermost region of the wind interaction zone, which is from a region whose outer radius, as measured from the secondary star, lies between 0.5 and 1.5 times the orbital separation.