Covariant Magnetoionic Theory II: Radiative Transfer

Abstract

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.

15 pages, 8 figures, submitted to MNRAS

References in corpus (5)

• Polarimetric Imaging of the Massive Black Hole at the Galactic Center
• Circular polarization from stochastic synchrotron sources
• Covariant Magnetoionic Theory I: Ray Propagation
• The High-Energy Polarization-Limiting Radius of Neutron Star Magnetospheres I -- Slowly Rotating Neutron Stars
• Refraction in a pulsar magnetosphere - the effect of a variable emission height on pulse morphology

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