Increasing tidal deformation around a black hole drives bound geodesics through weak chaos, plunging, unbinding, and eventual depletion of all bound motion, with semi-analytic critical amplitudes for each transition.
Mixed citations
Tidal deformation of a slowly rotating black hole
Mixed citation behavior. Most common role is background (60%).
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Pith papers citing it
Background
60% of classified citations
abstract
In the first part of this article I determine the geometry of a slowly rotating black hole deformed by generic tidal forces created by a remote distribution of matter. The metric of the deformed black hole is obtained by integrating the Einstein field equations in a vacuum region of spacetime bounded by r < r_max, with r_max a maximum radius taken to be much smaller than the distance to the remote matter. The tidal forces are assumed to be weak and to vary slowly in time, and the metric is expressed in terms of generic tidal quadrupole moments E_{ab} and B_{ab} that characterize the tidal environment. The metric incorporates couplings between the black hole's spin vector and the tidal moments, and captures all effects associated with the dragging of inertial frames. In the second part of the article I determine the tidal moments by immersing the black hole in a larger post-Newtonian system that includes an external distribution of matter; while the black hole's internal gravity is allowed to be strong, the mutual gravity between the black hole and the external matter is assumed to be weak. The post-Newtonian metric that describes the entire system is valid when r > r_min, where r_min is a minimum distance that must be much larger than the black hole's radius. The black-hole and post-Newtonian metrics provide alternative descriptions of the same gravitational field in an overlap r_min < r < r_max, and matching the metrics determine the tidal moments, which are expressed as post-Newtonian expansions carried out through one-and-a-half post-Newtonian order. Explicit expressions are obtained in the specific case in which the black hole is a member of a post-Newtonian two-body system.
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representative citing papers
Tidal Love numbers of regular black holes are generically nonzero, model-dependent, and can acquire logarithmic scale dependence at higher perturbative orders.
Numerical relativity simulations of equal-mass black holes with initial spins from -0.7 to 0.7 in hyperbolic encounters find maximum spin-up of 0.3 and mass increase of 15%, with spin-up decreasing linearly with initial spin at the threshold angle.
Static fermionic tidal Love numbers are non-vanishing for non-extremal Reissner-Nordström black holes.
A new gauge-invariant effective action computes black hole Love numbers without Regge-Wheeler methods, and these numbers determine leading thermodynamic corrections under external perturbations.
Renormalized dynamical tidal response functions for non-rotating black holes in GR carry inevitable ambiguities from renormalization scheme and flow initial condition, yielding scheme-dependent dynamical tidal Love numbers after MST-worldline EFT matching.
A pedagogical review of Love numbers and tidal responses for black holes and compact objects in general relativity and extensions.
citing papers explorer
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The relativistic restricted three-body problem: geometry and motion around tidally perturbed black holes
Increasing tidal deformation around a black hole drives bound geodesics through weak chaos, plunging, unbinding, and eventual depletion of all bound motion, with semi-analytic critical amplitudes for each transition.
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Tidal Love numbers for regular black holes
Tidal Love numbers of regular black holes are generically nonzero, model-dependent, and can acquire logarithmic scale dependence at higher perturbative orders.
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Spin-up and mass-gain in hyperbolic encounters of spinning black holes
Numerical relativity simulations of equal-mass black holes with initial spins from -0.7 to 0.7 in hyperbolic encounters find maximum spin-up of 0.3 and mass increase of 15%, with spin-up decreasing linearly with initial spin at the threshold angle.
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Fermionic Love number of Reissner-Nordstr\"om black holes
Static fermionic tidal Love numbers are non-vanishing for non-extremal Reissner-Nordström black holes.
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Tidal Response and Thermodynamics of Black Holes
A new gauge-invariant effective action computes black hole Love numbers without Regge-Wheeler methods, and these numbers determine leading thermodynamic corrections under external perturbations.
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Dynamical Tidal Response of Non-rotating Black Holes: Connecting the MST Formalism and Worldline EFT
Renormalized dynamical tidal response functions for non-rotating black holes in GR carry inevitable ambiguities from renormalization scheme and flow initial condition, yielding scheme-dependent dynamical tidal Love numbers after MST-worldline EFT matching.
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Love numbers of black holes and compact objects
A pedagogical review of Love numbers and tidal responses for black holes and compact objects in general relativity and extensions.
- A New Spin on Dissipative Tides: First-Post-Newtonian Effects in Compact Binary Inspirals