2026/01/02 by Marta Cocco, G. Grignani, Gianluca Grignani +5 · 2 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black Holes and Theoretical Physics #Black hole (networking) #Circular orbit #Hamiltonian (control theory) #Kerr metric #Mass ratio #Perturbation (astronomy) #Pulsars and Gravitational Waves Research #Rotating black hole #Spacetime #Tidal force
paper · pdf · open access · doi:10.1088/1361-6382/ae80b6
published in Classical and Quantum Gravity 43(14), 145005 (IOP Publishing)
openalex publication_date 2026/06/23 · openalex created_date 2026/06/24 · openalex updated_date 2026/08/05
Abstract We determine the metric of a Kerr black hole subject to external tidal fields using metric reconstruction techniques. Working within the Newman–Penrose formalism, we solve the Teukolsky master equation for static, quadrupolar modes associated with a slowly varying tidal environment, and reconstruct the corresponding metric perturbation in the outgoing radiation gauge. As an application, we derive the secular Hamiltonian governing the motion of a test particle in the tidally deformed Kerr spacetime and investigate long-term tidal effects relevant to extreme-mass-ratio inspirals. In particular, we compute tidal-induced shifts of the innermost stable circular orbit and the light ring. We find that these tidal corrections are strongly spin dependent, with significantly larger effects for retrograde orbits around rapidly rotating black holes. Our results provide a fully analytic framework for studying tidal interactions and secular dynamics in rotating black-hole spacetimes, with direct applications to gravitational-wave modeling and tests of gravity in the strong-field regime.