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 microquasars as well as active galactic nuclei (AGNs) 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 microquasars and AGNs 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 of the test particle, mass and rotation of the BH.
Highlights
The motion of a spinning test-body in a fixed gravitational background is a long-standing problem in general relativity [25]
In this article we have studied classical spinning test particle motion around rotating Kerr black hole (BH) and applied spinning particle fundamental frequencies to observe the quasi-periodic oscillations (QPOs) in microquasars as well as AGNs
The position of innermost stable circular orbit (ISCO) is situated close to the horizon when the particle spin is aligned to the z-axis as compared to the case when the spin is anti-aligned
Summary
The motion of a spinning test-body in a fixed gravitational background is a long-standing problem in general relativity [25]. Applying the methods of spectroscopy (frequency distribution of photons) and timing (photon number time dependence) for particular microquasars, one can extract useful information regarding the range of parameters of the system [26] In this connection, the binary systems containing BHs, being compared to neutron star systems, seem to be promising due to the reason that any astrophysical BH is thought to be a Kerr BH (corresponding to the unique solution of general relativity in 4D for uncharged BHs which does not violate the no hair theorem and the weak cosmic censorship conjecture) that is determined by only two parameters: the BH mass M and the BH spin parameter |a/M| ≤ 1. For expressions having astrophysical relevance we use the physical constants explicitly
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