Calculates energy fluxes with quadratic-in-spin and quadrupole effects for small-mass-ratio spinning binaries in self-force theory, providing numerical data and sixth-order PN expansions.
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Isolated and dynamical horizons and their applications
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abstract
Over the past three decades, black holes have played an important role in quantum gravity, mathematical physics, numerical relativity and gravitational wave phenomenology. However, conceptual settings and mathematical models used to discuss them have varied considerably from one area to another. Over the last five years a new, quasi-local framework was introduced to analyze diverse facets of black holes in a unified manner. In this framework, evolving black holes are modeled by dynamical horizons and black holes in equilibrium by isolated horizons. We review basic properties of these horizons and summarize applications to mathematical physics, numerical relativity and quantum gravity. This paradigm has led to significant generalizations of several results in black hole physics. Specifically, it has introduced a more physical setting for black hole thermodynamics and for black hole entropy calculations in quantum gravity; suggested a phenomenological model for hairy black holes; provided novel techniques to extract physics from numerical simulations; and led to new laws governing the dynamics of black holes in exact general relativity.
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representative citing papers
All integrable 2D Horndeski theories (and thus many regular black-hole metrics) arise as spherical reductions of pure d≥4 gravities, which the paper terms quasi-topological.
Horizon multipole moments of a Kerr black hole are computed in closed form from two definitions, yielding different values for l >= 1 at nonzero spin and sharing parity and small-spin scaling with field multipoles.
Causal sets can approximate black hole horizons via discrete timelike curves and ladders tracing null geodesics, with a discrete expansion changing sign across the horizon in a 1+1D toy model.
Ultra-relativistic black hole flybys can radiate over 65% of their energy in gravitational waves via irregular waveforms caused by radiation trapping and lensing, without coalescence.
The apparent horizon shape is derived to second order for perturbed evaporating black holes, and an effective classical metric is obtained from quantum expectation values of the reconstructed spacetime.
Numerical study of cusp formation on horizons in head-on non-spinning black hole mergers, with analysis of mass and multipole behavior at the cusp and a proposed phenomenological model.
Black hole horizons in 2+1D are composed of quantized length quanta 8π ℓ_P n, producing entropy near the Bekenstein-Hawking value and a local Hawking spectrum via a length ensemble.
A novel exact solution describes a dynamical black hole dressed with a time-dependent scalar field and immersed in an axisymmetric time-dependent electromagnetic field, where time dependence may cloak curvature singularities.
A spherically symmetric charged black hole evaporating via Hawking radiation can remain regular, with neither a singularity nor a Cauchy horizon, due to electromagnetic repulsion and energy-condition violation.
Extended 1PA self-force waveforms for slowly spinning primary and precessing secondary, with re-summed 1PAT1R variant showing improved accuracy against NR for q ≳ 5 and |χ1| ≲ 0.1.
Vaidya-type dynamical black holes admit homothetic Killing vectors only for linear-in-null-time mass/charge/rotation profiles, and the resulting homothetic Killing horizons carry surface gravities obeying a flux-balance first law.
Quasi-local dynamical horizons admit a first law for finite, far-from-equilibrium processes and a quantitative second law tying area growth to energy fluxes, so black-hole entropy is the area of marginally trapped surfaces.
Interior MOTS in Hayward black holes are located via the b-parameter metric, with self-intersecting pairs identified and positions near the inner horizon given by hypergeometric functions from a singular Sturm-Liouville reduction whose eigenspace is complete but non-discrete and discontinuous.
In f(R) theories, the replica-method gravitational entropy computed on the apparent horizon matches the Hollands-Wald-Zhang dynamical black hole entropy and satisfies the first law, while the event horizon does not; this lets the generalized second law be reinterpreted as matter entanglement across
Bayesian parameter estimation with targeted eccentric numerical-relativity waveforms yields eccentricity estimates of e20 ≈ 0.2 for GW200208_22 and e10 ≈ 0.19 for GW190620, reinforcing the eccentric hypothesis.
In Modified Gravity, a scalar breathing-mode perturbation yields non-thermal radiation and second-order entropy production, while a running MOG parameter α(M) quenches Hawking radiation into a stable remnant.
citing papers explorer
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Quadrupole and quadratic-in-spin effects in quasicircular, spinning, asymmetric binaries
Calculates energy fluxes with quadratic-in-spin and quadrupole effects for small-mass-ratio spinning binaries in self-force theory, providing numerical data and sixth-order PN expansions.
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All $2D$ generalised dilaton theories from $d\geq 4$ gravities
All integrable 2D Horndeski theories (and thus many regular black-hole metrics) arise as spherical reductions of pure d≥4 gravities, which the paper terms quasi-topological.
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Horizon Multipole Moments of a Kerr Black Hole
Horizon multipole moments of a Kerr black hole are computed in closed form from two definitions, yielding different values for l >= 1 at nonzero spin and sharing parity and small-spin scaling with field multipoles.
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Towards black-hole horizons and geodesic focusing in causal sets
Causal sets can approximate black hole horizons via discrete timelike curves and ladders tracing null geodesics, with a discrete expansion changing sign across the horizon in a 1+1D toy model.
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Trapping, Irregular Waveforms, and Efficient Radiation in Ultra-relativistic Black Hole Encounters
Ultra-relativistic black hole flybys can radiate over 65% of their energy in gravitational waves via irregular waveforms caused by radiation trapping and lensing, without coalescence.
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Quantum Field Theory of Black Hole Perturbations with Backreaction VI. Apparent Horizons, Quasi-Local Mass and Effective Classical Metrics
The apparent horizon shape is derived to second order for perturbed evaporating black holes, and an effective classical metric is obtained from quantum expectation values of the reconstructed spacetime.
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Cusp Formation in Merging Black Hole Horizons
Numerical study of cusp formation on horizons in head-on non-spinning black hole mergers, with analysis of mass and multipole behavior at the cusp and a proposed phenomenological model.
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Hawking radiation from black holes in 2+1 dimensions
Black hole horizons in 2+1D are composed of quantized length quanta 8π ℓ_P n, producing entropy near the Bekenstein-Hawking value and a local Hawking spectrum via a length ensemble.
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Magnetized dynamical black holes
A novel exact solution describes a dynamical black hole dressed with a time-dependent scalar field and immersed in an axisymmetric time-dependent electromagnetic field, where time dependence may cloak curvature singularities.
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Radiating black holes in general relativity need not be singular
A spherically symmetric charged black hole evaporating via Hawking radiation can remain regular, with neither a singularity nor a Cauchy horizon, due to electromagnetic repulsion and energy-condition violation.
-
Post-adiabatic self-force waveforms: slowly spinning primary and precessing secondary
Extended 1PA self-force waveforms for slowly spinning primary and precessing secondary, with re-summed 1PAT1R variant showing improved accuracy against NR for q ≳ 5 and |χ1| ≲ 0.1.
-
Homothetic Killing horizons in generic Vaidya spacetimes
Vaidya-type dynamical black holes admit homothetic Killing vectors only for linear-in-null-time mass/charge/rotation profiles, and the resulting homothetic Killing horizons carry surface gravities obeying a flux-balance first law.
-
Thermodynamics of dynamical black holes beyond perturbation theory
Quasi-local dynamical horizons admit a first law for finite, far-from-equilibrium processes and a quantitative second law tying area growth to energy fluxes, so black-hole entropy is the area of marginally trapped surfaces.
-
Interior marginally outer trapped surfaces in Hayward black holes
Interior MOTS in Hayward black holes are located via the b-parameter metric, with self-intersecting pairs identified and positions near the inner horizon given by hypergeometric functions from a singular Sturm-Liouville reduction whose eigenspace is complete but non-discrete and discontinuous.
-
Entanglement Entropy and Thermodynamics of Dynamical Black Holes
In f(R) theories, the replica-method gravitational entropy computed on the apparent horizon matches the Hollands-Wald-Zhang dynamical black hole entropy and satisfies the first law, while the event horizon does not; this lets the generalized second law be reinterpreted as matter entanglement across
-
Parameter Estimation with Targeted Eccentric Numerical-Relativity Simulations for GW200208_22 and GW190620
Bayesian parameter estimation with targeted eccentric numerical-relativity waveforms yields eccentricity estimates of e20 ≈ 0.2 for GW200208_22 and e10 ≈ 0.19 for GW190620, reinforcing the eccentric hypothesis.
-
Dynamical Black Hole Thermodynamics in Modified Gravity
In Modified Gravity, a scalar breathing-mode perturbation yields non-thermal radiation and second-order entropy production, while a running MOG parameter α(M) quenches Hawking radiation into a stable remnant.
- Primordial Black Holes: A Review of Formation and Evolution