Polarized anisotropic synchrotron emission and absorption and its application to Black Hole Imaging

TL;DR

This paper investigates how temperature anisotropy in relativistic plasmas affects polarized synchrotron emission and absorption, with implications for black hole imaging and interpretation of observational data.

Contribution

It provides analytical and numerical models for polarized synchrotron coefficients in anisotropic plasmas and applies these to simulate black hole images, highlighting the impact of anisotropy on observational features.

Findings

Anisotropy significantly alters emission and absorption coefficients depending on viewing angle.

Circular polarization is sensitive to plasma anisotropy, unlike linear polarization.

Temperature anisotropy can change black hole image asymmetry and shadow size by up to a factor of 3.

Abstract

Low-collisionality plasma in a magnetic field generically develops anisotropy in its distribution function with respect to the magnetic field direction. Motivated by the application to radiation from accretion flows and jets, we explore the effect of temperature anisotropy on synchrotron emission. We derive analytically and provide numerical fits for the polarized synchrotron emission and absorption coefficients for a relativistic bi-Maxwellian plasma (we do not consider Faraday conversion/rotation). Temperature anisotropy can significantly change how the synchrotron emission and absorption coefficients depend on observing angle with respect to the magnetic field. The emitted linear polarization fraction does not depend strongly on anisotropy, while the emitted circular polarization does. We apply our results to black hole imaging of Sgr A* and M87* by ray-tracing a GRMHD simulation and assuming that the plasma temperature anisotropy is set by the thresholds of kinetic-scale anisotropy-driven instabilities. We find that the azimuthal asymmetry of the 230 GHz images can change by up to a factor of 3, accentuating ($T_\perp > T_\parallel$) or counteracting ($T_\perp < T_\parallel$) the image asymmetry produced by Doppler beaming. This can change the physical inferences from observations relative to models with an isotropic distribution function, e.g., by allowing for larger inclination between the line of sight and spin direction in Sgr A*. The observed image diameter and the size of the black hole shadow can also vary significantly due to plasma temperature anisotropy. We describe how the anisotropy of the plasma can affect future multi-frequency and photon ring observations. In Appendices we calculate kinetic anisotropy-driven instabilities (mirror, whistler, and firehose) for relativistically hot plasmas.