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X-ray polarimetric missions planned for this decade will significantlyenhance our knowledge of compact accreting sources. Observations of the X-raypolarization signal from active galactic nuclei (AGNs) or X-ray binary systems(XRBs) will bring new means to study inner accretion flow in these objectsthat, together with currently used spectroscopic and timing techniques, willhelp us to determine better their properties, such as their inclination,orientation, shape, and size of their corona as well as the black hole spin. Inthis work, we present a yet missing piece in the global polarization models ofblack hole accretion discs. We compute the reflected X-ray emission from thedisc in a local co-moving frame using (1) the radiative transfer code TITAN toobtain the ionization structure of the disc and (2) the Monte Carlo code STOKESthat incorporates the physics of absorption, re-emission, and Comptonscattering to produce a complete spectropolarimetric output. We present thefinal Stokes parameters I, Q, and U for a set of photon-indices of the incidentprimary power-law radiation, the disc ionization parameters, incident andemission angles, for three independent polarization states of the incidentcoronal X-ray photons with a sufficient resolution in energy to allow for sharpdiscussion of spectral and polarization properties. We show that the spectralcomponent matches well literature predictions. The polarization degree andangle are in agreement with analytical approximations previously appearing inreflection models and we demonstrate that the polarized reflected X-rayemission can be, locally, quite large in the 2-12 keV band.

Spectral and polarization properties of reflected X-ray emission from black hole accretion discs