Astrophysical signatures of Kerr-Bertotti-Robinson black holes in a cloud of strings: ISCO, microquasar QPOs, and Bondi-Hoyle-Lyttleton accretion

Abstract

We study test-particle dynamics in the equatorial plane of a Kerr-Bertotti-Robinson black hole (BH) immersed in a cloud of strings (CS), with mass M , rotation a, magnetic parameter B, and string parameter {\alpha}. Using the Hamilton formalism we recover the effective potential Ueff and the conditions for circular motion, and we compute the specific energy E and specific angular momentum L together with the radial, vertical, and azimuthal epicyclic frequencies {\nu}r , {\nu}{\theta} , {\nu}{\phi}. Going beyond the analytic setup, we provide the first numerical mapping of the innermost stable circular orbit (ISCO) for this background and tabulate rISCO, EISCO, LISCO, and the accretion efficiency {\eta} = 1 - EISCO for both co- and counter-rotating motion across a wide (a, B, {\alpha}) grid. The CS parameter pushes the ISCO outward and raises {\eta} from 0.057 in Schwarzschild to above 0.25 for {\alpha} = 0.30 at a = 0.9. We then connect the model with observed twin-peak high-frequency quasi-periodic oscillations (QPOs) in three microquasars (GRO J1655-40, XTE J1550-564, GRS 1915+105) using the relativistic-precession (RP) model and find \{chi}^2-minimum fits with {\alpha} < 0.13. A general-relativistic hydrodynamical (GRH) study of Bondi-Hoyle-Lyttleton (BHL) accretion completes the picture: the CS contribution sustains shock-cone instabilities, redistributes power-spectral-density (PSD) peaks, and produces low-frequency QPO-like components that distinguish KBR+CS from pure Kerr or KBR.