  Accretion onto compact objects plays a central role in high energy
astrophysics. In these environments, both general relativistic and plasma
effects may have significant impacts upon the spectral and polarimetric
properties of the accretion flow. In paper I we presented a fully general
relativistic magnetoionic theory, capable of tracing rays in the geometric
optics approximation through a magnetised plasma in the vicinity of a compact
object. In this paper we discuss how to perform polarised radiative transfer
along these rays. In addition we apply the formalism to a barotropic thick disk
model, appropriate for low luminosity active galactic nuclei. We find that it
is possible to generate large fractional polarisations over the innermost
portions of the accretion flow, even when the emission mechanism is
unpolarised. This has implications for accreting systems ranging from pulsars
and X-ray binaries to AGN.
