Dynamics, Ringdown, and Accretion-Driven Multiple Quasi-Periodic Oscillations of Kerr-Bertotti-Robinson Black Holes

TL;DR

This paper investigates the dynamics of test particles around Kerr-Bertotti-Robinson black holes, analyzing orbital frequencies, quasi-periodic oscillations, quasinormal modes, and accretion structures, revealing how black hole parameters influence observable phenomena.

Contribution

It provides analytical expressions for particle orbits, studies quasinormal modes in magnetic fields, and models accretion structures, offering new insights into black hole physics and QPO origins.

Findings

Particle motion is strongly influenced by black hole parameters.

Magnetic fields increase damping of quasinormal modes.

Accretion structures produce observable QPOs in X-ray binaries.

Abstract

We study the motion of test particles around Kerr--Bertotti--Robinson (KBR) black hole (BH) and explore how the three defining parameters the mass $M$, rotation parameter $a$, and magnetic parameter $B$ influence their dynamics. We derive analytical expressions for the energy and angular momentum of stable equatorial circular orbits, along with the corresponding radial and latitudinal oscillation frequencies, as functions of $M$, $a$, and $B$. We also examine the key features of the quasi-periodic oscillations of test particles near stable circular orbits, including the precession effects such as periastron precession and the Lense-Thirring effect. Finally, we compare our results with those corresponding to the Kerr BH. We find that particle motion is strongly shaped by the BH parameters. Using a WKB approach, we also study scalar quasinormal modes of a rotating KBR BH in an external magnetic field and show that the magnetic field increases damping, while rotation and angular momentum mainly set the oscillation frequencies. Alternatively, general relativistic modelling of Bondi-Hoyle-Lyttleton (BHL) accretion onto a rapidly rotating KBR BH shows that two distinct physical structures emerge and cyclically transform into one another over time. These processes produce either a strongly oscillating flip-flop shock cone or a nearly stationary toroidal structure, with their formation governed by the black hole spin and magnetic curvature. Power spectral analysis shows that these configurations give rise to low and high-frequency quasi-periodic oscillations, offering a unified explanation for the multiple quasi-periodic oscillations observed in rapidly spinning X--ray binaries.