A different view of wind in X-ray binaries: the accretion disc corona source 2S 0921-630

Accretion disc coronae (ADC) sources are very high inclination neutron star or black hole binaries, where the outer accretion flow blocks a direct view of central source. The weak observed X-ray emission is instead produced mainly by scattering intrinsic radiation from highly ionised gas surrounding source, ADC. However, origin this material still under debate. We use ADC source 2S 0921-630 (V395 Car) to test whether it consistent with thermal-radiative wind illuminating and puffing up disc. This clearly visible in blueshifted absorption lines less inclined systems, seen directly through material. Using phenomenological photoionised plasma model, we first characterise parameter that drives 2S0921 XMM-Newton Chandra data. Following this, run Monte Carlo transfer simulation get scattered/reprocessed emissions wind, density velocity structure obtained previous work. Our model agrees all medium energy grating spectra for an luminosity L > 0.2 LEdd. result strongly favours winds as also show how high-resolution via microcalorimeters can provide definitive detecting lines.