Non-thermal processes around accreting galactic black holes

TL;DR

This paper investigates how non-thermal particles in the magnetized coronae of galactic black holes can explain high-energy emissions, predicting a TeV bump detectable by future gamma-ray observatories.

Contribution

It introduces models of non-thermal particle injection in black hole coronae and predicts observable high-energy signatures, including a TeV bump, expanding understanding of accretion physics.

Findings

Non-thermal particles can explain high-energy excess in X-ray sources.

Predicted a TeV energy bump in the spectral energy distribution.

High-energy luminosities around 10^{33} erg s^{-1}.

Abstract

Accreting black holes in galactic X-ray sources are surrounded by hot plasma. The innermost part of these systems is likely a corona with different temperatures for ions and electrons. In the so-called low-hard state, hot electrons Comptonize soft X-ray photons from the disk that partially penetrates the corona, producing emission up to $\sim 150$ keV, well beyond the expectations for an optically thick disk of maximum temperature $\sim 10^{7}$ K. However, sources such as Cygnus X-1 produce steady emission up to a few MeV, which is indicative of a non-thermal contribution to the spectral energy distribution. We study the radiative output produced by the injection of non-thermal (both electron and proton) particles in a magnetized corona around a black hole. Energy losses and maximum energies are estimated for all types of particles in a variety of models, characterized by different kinds of advection and relativistic proton content. Transport equations are solved for primary and secondary particles, and spectral energy distributions are determined and corrected by internal absorption. We show that a local injection of non-thermal particles can account for the high energy excess observed in some sources, and we predict the existence of a high-energy bump at energies above 1 TeV, and typical luminosities of $\sim 10^{33}$ erg s$^{-1}$. High-energy instruments such as the future Cherenkov Telescope Array (CTA) can be used to probe the relativistic particle content of the coronae around galactic black holes.