Magnetised relativistic accretion disc around a spinning, electrically charged, accelerating black hole: case of C-metric

TL;DR

This study models a magnetised, relativistic accretion disc around a charged, accelerating black hole using the C-metric, revealing potential observational differences from Kerr black holes and providing a framework for numerical simulations.

Contribution

It introduces a new analytical model of a magnetised thick accretion disc around an accelerating, charged black hole using the C-metric, exploring its equilibrium configurations.

Findings

C-metric can be distinguished from Kerr metric by specific disc features

The model demonstrates how magnetic field strength influences disc structure

Provides a testbed for future numerical simulations of accretion discs

Abstract

This paper examines the general relativistic model of a geometrically thick configuration of an accretion disc around an electrically charged black hole in an accelerated motion, as described by the C-metric family. We aim to study the effects of the spacetime background on the magnetised version of the thick disc model via the sequences of figures of equilibrium. While maintaining the assumption of non-selfgravitating (test) fluid, we newly explore the influence of the strength of the large-scale magnetic field with field lines organised over the length-scale of the black hole horizon. We systematically analyze the dependence on a very broad parameter space of the adopted scenario. We demonstrate that the C-metric can, in principle, be distinguished from Kerr black hole metric by resolving specific (albeit rather fine) features of the torus, such as the location of its centre, inner and outer rims, and the overall shape. The analytical setup can serve as a testbed for numerical simulations.