The origin of accretion-disc winds remains disputed. High-inclination, dipping, neutron-star (NS) low-mass X-ray binaries (LMXBs) provide an excellent testbed for studying the launching mechanism of such winds due to them persistently accreting and showing a nearly ubiquitous presence of highly ionised plasmas. We aim to establish or rule out the presence of a wind in the high-inclination LMXB for which a highly ionised plasma has been repeatedly observed in X-ray spectra by Chandra and XMM-Newton, and a thermal--radiative pressure wind is expected. We leveraged the exquisite spectral resolution of the X-ray Imaging and Spectroscopy Mission (to perform phase-resolved spectroscopy of the full binary orbit to characterise the highly ionised plasma at all phases except during absorption dips. An outflow is clearly detected via phase-resolved spectroscopy of the source with and a column density above 10²3 cm^-2. The line profiles are generally narrow, spanning ∼50--100 km s^ Resolve. Based on analysis of the radial-velocity curve, we determine an average velocity of ∼200--320 km s -1 -1, depending on the orbital phase; this points to a low-velocity sheer or turbulence of the highly ionised outflow and a potential increase of turbulence as the absorption dip is approached, likely due to turbulent mixing. The line profiles, together with the derived launching radius and wind velocity, are consistent with a wind being launched from the outskirts of the disc and without stratification, pointing to a thermal-radiative pressure origin.
Trigo et al. (Fri,) studied this question.