Spectral classification of the mass donors in the high-mass X-ray binaries EXO 1722-363 and OAO 1657-415

TL;DR

This study uses near-infrared observations to classify the spectral types of mass donors in two high-mass X-ray binaries, revealing their evolutionary states and implications for their X-ray luminosities and accretion processes.

Contribution

It provides the first detailed spectral classifications of the donors in EXO 1722-363 and OAO 1657-415, linking their properties to evolutionary stages and accretion dynamics.

Findings

EXO 1722-363 is a B0-B1 Ia supergiant at ~8 kpc with a progenitor mass of 30-40 M_Sun.

OAO 1657-415 is classified as Ofpe/WNL, an intermediate evolutionary stage.

OAO 1657-415's wind properties lead to high accretion rates and influence neutron star spin periods.

Abstract

We report near-infrared observations of the mass donors of the eclipsing high-mass X-ray binary (HMXB) systems EXO 1722-363 and OAO 1657-415 in order to derive their accurate spectral classifications. We determined that EXO 1722-363 was of spectral type B0 - B1 Ia, positioned at a distance 8.0 +2.5/-2.0 kpc with a progenitor mass in the range 30 - 40 M_Sun. Luminosity calculations imply that L_X ~ 10^35 - 10^37 erg s^-1 for this distance range. We conclude that EXO 1722-363 shares many of the properties associated with other X-ray binary B-type supergiant donors. We found that OAO 1657-415 correlates closely with the spectra of a class of transitional objects, the Ofpe/WNL, an intermediate evolutionary stage between massive O type stars leaving the main sequence and evolving into Wolf-Rayets. Due to the wide range range in Luminosity displayed by Ofpe/WNL stars, (log L/L_Sun ~ 5.3 - 6.2) distance determinations are problematic. For OAO 1657-415 we report a distance of 4.4 <= d <= 12 kpc, implying an X-ray luminosity of 1.5 x 10^36 <= L_X <= 10^37 erg s^-1. We have used our new classification of OAO 1657-415 to explain the physical processes responsible for its unique position within the Corbet diagram. Ofpe/WNL stars demonstrate a high rate of mass-loss through a dense stellar wind combined with a low terminal velocity. This combination of wind properties leads to a high accretion rate and transfer of angular momentum to the neutron star in this system. We believe this in turn leads to a smaller instantaneous equilibrium spin period with respect to normal OB supergiants.