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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Analytic black hole perturbation approach to gravitational radiation
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abstract
We review analytic methods to perform the post-Newtonian expansion of gravitational waves induced by a particle orbiting a massive compact body, based on the black hole perturbation theory. There exist two different methods of the post-Newtonian expansion. Both are based the Teukolsky equation. In one method, the Teukolsky equation is transformed into a Regge-Wheeler type equation that reduces to the standard Klein-Gordon equation in the flat space limit, while in the other method, which were introduced by Mano, Suzuki and Takasugi relatively recently, the Teukolsky equation is directly used in its original form. The former has an advantage that it is intuitively easy to understand how various curved space effects come into play. However, it becomes increasingly complicated when one goes on to higher and higher post-Newtonian orders. In contrast, the latter has an advantage that a systematic calculation to higher post-Newtonian orders is relatively easily implementable, but otherwise so mathematical that it is hard to understand the interplay of higher order terms. In this paper, we review both methods so that their pros and cons may be clearly seen. We also review some results of calculations of gravitational radiation emitted by a particle orbiting a black hole.
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Generalizes ⟨Φ̂²⟩_ren and flux computations to non-minimal ξ near Kerr inner horizon along axis, finding per-mode ringdown (frequencies twice classical QNMs) then r_*^{-2ℓ-3} tails approaching finite value.
All redshift-mode contributions to Schwarzschild black-hole ringdown waveforms vanish exactly because causality forces the source-integrated Green function to vanish on the light cone.
Retarded correlators of bulk scalars and Wilson-line displacement operators exhibit bouncing singularities at t_c=β/2(1+i) with matching WKB and asymptotic OPE data, implying a universal high-frequency factorization.
Gravitational Compton amplitude computed to third post-Minkowskian order via worldline EFT with infrared and forward divergences regulated to connect to black hole perturbation theory.
A universal anomalous dimension for multipole moments in GR is derived via two EFT methods and applied to resum short-distance logarithmic tails in binary gravitational waveforms.
Dynamical tidal Love numbers for Kerr black holes are obtained to linear frequency order by matching EFT worldline couplings to black-hole perturbation solutions, including spin-induced mode mixing.
Computation of the quadrupolar bremsstrahlung waveform for two-body scattering at 3.5PN order, including frequency-domain evaluation up to O(G^4) and nonlinear memory effects.
Closed-form Sommerfeld factor via EFT connection matrix with analytic O(G^10) magnitude and phase for l=0,1,2 waves, plus a new RG equation for radiative multipole moments that improves waveform resummation beyond tail logarithms.
Kerr QNM anomalies near algebraically special frequencies arise from avoided crossings with resonant excitation and pole skipping due to quasinormal-Matsubara pole-zero cancellations.
WKB analysis of the Teukolsky equation establishes a quasinormal-mode to greybody-factor correspondence for Kerr black holes that holds in the eikonal limit for gravitational perturbations and matches numerics at high angular momentum.
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.
The prompt response is ~1.2 times stronger than quasinormal mode excitation during inspiral and enables 99% accurate reconstruction of the full inspiral-merger-ringdown waveform when combined with other components.
Presents cavity-based effective descriptions for scalar radiation from black holes and modified models, linking them to wave profiles and accumulated phase shifts for detecting small deviations from classical behavior.
Quasinormal modes are eigenmodes of dissipative gravitational systems whose spectra encode near-equilibrium transport coefficients in dual quantum field theories and enable tests of general relativity through gravitational wave observations.
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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.