Abstract We study the epicyclic oscillations of test particles around rotating quantum-corrected black holes (QCBHs), characterized by mass M , spin a , and the quantum deformation parameter b . By deriving the radial (Ω r ) and vertical (Ω θ ) oscillation frequencies, we explore their dependence on spacetime parameters and show that quantum corrections ( b ≠ 0) significantly modify the dynamics compared to the classical Kerr case. Through numerical modeling of accretion around QCBHs, we further examine how b influences strong-field phenomena, comparing the results with test-particle dynamics and observational data. Our analysis reveals: (1) Quantum corrections shift the ISCOs outward, with b altering the effective potential and conditions for stable circular motion. (2) The curvature of the potential and thus the epicyclic frequencies change Ω r shows up to 25% deviation for typical b values, underscoring sensitivity to quantum effects. (3) Precession behavior is modified: while Lense-Thirring precession (Ω LT ) remains primarily governed by a , periastron precession (Ω P ) is notably affected by b , especially near the black hole. (4) Accretion disk simulations confirm the physical effects of b , which is aligned well with the test particle analysis. In addition, the quasiperiodic oscillation (QPO) frequencies obtained via both approaches agree with the observed low-frequency QPOs from sources like GRS 1915+105, GRO J 1655-40, XTE J 1550-564, and H 1743-322. The distinct frequency profiles and altered ratios offer observational signatures that may distinguish QCBHs from classical black holes. Our findings present testable predictions for X-ray timing and a new avenue to constrain quantum gravity parameters.
Mustafa et al. (Wed,) studied this question.
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