Magnetized particle motion and accretion process with shock cone morphology around a decoupled hairy black holes

TL;DR

This paper explores how hairy black holes affect magnetized particle motion and accretion processes, revealing enhanced energy efficiency and distinctive observational signatures compared to standard black holes.

Contribution

It introduces a new geometric model for decoupled hairy black holes and derives analytical results for accretion dynamics and particle motion, highlighting the impact of hairy parameters.

Findings

Reduced innermost stable circular orbit radius due to hairy parameters

Enhanced energy efficiency and emissivity in accretion processes

Observable signatures in gravitational waves and X-ray emissions

Abstract

Relativistic accretion onto compact objects such as black holes and neutron stars is one of the most efficient known mechanisms for converting gravitational potential energy into radiation. In the case of rapidly spinning black holes, up to $40\%$ of the rest-mass energy of accreting matter can be released, far exceeding the efficiency of nuclear fusion. In this work, we investigate magnetized particle motion and relativistic accretion processes around a decoupled hairy black hole via extended geometric deformation. The developed geometry involves two hairy parameters that preserve the horizon structure with the additional feature of the fulfillment of weak energy conditions outside the event horizon. We provide the foundation with necessary formalism for magnetized particle motion around a decoupled black hole. The effective potential and innermost stable circular orbits are then derived, which demonstrate a significant reduction of the radius of the latter quantity under the hairy parameters for the magnetized particle. Afterwards, we obtain exact analytical expressions for radial velocity profiles, mass accretion rates, and a few others which reveal improved energy efficiency and emissivity as compared to the standard black hole. Furthermore, the decoupling parameter shows strong influence on oscillations, accretion presenting fantastic agreement between analytical predictions and numerical simulations, and thus offering noticeable observational signatures for future gravitational wave and X-ray astronomy.