Optical spectroscopy of the low mass X-ray binary GX9+9

TL;DR

This study uses phase-resolved spectroscopy to identify the donor star's surface in GX9+9, estimating its mass function and revealing accretion stream overflow, with unique Bowen region emission characteristics.

Contribution

First spectroscopic detection of the donor star surface in GX9+9, providing the initial mass function estimate and insights into accretion dynamics.

Findings

Mass function f(M_1) >= 0.22 M_sun

Evidence of stream overflow in accretion disk

CIII dominates Bowen region emission

Abstract

Phase-resolved medium resolution VLT spectroscopy of the low mass X-ray binary GX9+9 has revealed narrow CIII emission lines that move in phase relative to our new estimate of the ephemeris, and show a velocity amplitude of 230+/-35 km/s. We identify the origin of these lines as coming from the surface of the donor star, thereby providing the first estimate of the mass function of f(M_1)>=0.22M_sun. Rotational broadening estimates together with assumptions for the mass donor give 0.07<q<0.35 and 182<K_2<406 km/s. Despite a low mass ratio, there is no evidence for a superhump in our dataset. Doppler maps of GX9+9 show the presence of a stream overflow, either in the form of material flowing downward along the accretion disk rim or in a similar fashion as occurs in high mass transfer rate cataclysmic variables known as the SW Sex stars. Finally we note that the Bowen region in GX9+9 is dominated by CIII instead of NIII emission as has been the case for most other X-ray binaries.