Testing quantum-corrected black holes with QPOs observations: a study of particle dynamics and accretion flow

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 (Ωr) and vertical (Ωθ) 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 Ωr shows up to 25% deviation for typical b values, underscoring sensitivity to quantum effects. (3) Precession behavior is modified: while Lense-Thirring precession (ΩLT) remains primarily governed by a, periastron precession (ΩP) 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 J1655-40, XTE J1550-564, and H1743-322. 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.