Epicyclic oscillations in spinning particle motion around Kerr black hole applied in models fitting the quasi-periodic oscillations observed in quasars and microquasars

TL;DR

This paper investigates how epicyclic oscillations of spinning particles around Kerr black holes can model the observed quasi-periodic oscillations in quasars and microquasars, providing insights into strong gravity phenomena.

Contribution

It introduces a modified geodesic model incorporating spinning test particles to explain QPOs, extending previous models and fitting observational data with specific parameter constraints.

Findings

Modified geodesic models can explain some QPO data

Successful fitting of high-frequency QPOs using resonance and precession models

Constraints on particle spin, black hole mass, and spin derived from data

Abstract

The study of the quasi-periodic oscillations (QPOs) of X-ray flux observed in the stellar-mass black hole (BH) binaries or quasars can provide a powerful tool for testing the phenomena occurring in strong gravity regime. We thus fit the data of QPOs observed in the well known quasars as well as microquasars in the framework of the model of geodesic oscillations of Keplerian disks modified for the epicyclic oscillations of spinning test particles orbiting Kerr BHs. We show that the modified geodesic models of QPOs can explain the observational fixed data from the quasars and microquasars but not for all sources. We perform a successful fitting of the high frequency QPOs models of epicyclic resonance and its variants, relativistic precession and its variants, tidal disruption, as well as warped disc models, and discuss the corresponding constraints of parameters of the model, which are the spin $S$ of the test particle, mass $M$ and spin $a$ of the BH.