Comparing second-order gravitational self-force and effective one body waveforms from inspiralling, quasicircular and nonspinning black hole binaries. II. The large-mass-ratio case

Albertini, Angelica; Nagar, Alessandro; Pound, Adam; Warburton, Niels; Wardell, Barry; Durkan, Leanne; Miller, Jeremy

doi:10.1103/physrevd.106.084062

Cited by 21 publications

(3 citation statements)

References 67 publications

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“…The self-force expansion on a Schwarzschild background is perhaps the most notable example, due to its significance in the effective-one-body description which accurately describes the two-body problem in general relativity for a (non-spinning) binary system of masses m and M ≫ m [50][51][52][53]. At zeroth-order in the mass ratio m/M, the motion of the probe particle follows a geodesic, and no radiation is emitted.…”

Section: Introductionmentioning

confidence: 99%

Scattering amplitudes for self-force

Adamo,

Cristofoli,

Ilderton

et al. 2024

Class. Quantum Grav.

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The self-force expansion allows the study of deviations from geodesic motion due to the emission of radiation and its consequent back-reaction. We investigate this scheme within the on-shell framework of semiclassical scattering amplitudes for particles emitting photons or gravitons on a static, spherically symmetric background. We ﬁrst present the exact scalar 2-point amplitudes for Coulomb and Schwarzschild, from which one can extract classical observables such as the change in momentum due to geodesic motion. We then present, for the ﬁrst time, the 3-point semiclassical amplitudes for a scalar emitting a photon in Coulomb and a graviton on linearised Schwarzschild, outlining how the latter calculation can be generalized to the fully non-linear Schwarzschild metric. Our results are proper resummations of perturbative amplitudes in vacuum but, notably, are expressed in terms of Hamilton’s principal function for the backgrounds, rather than the radial action.

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Section: Introductionmentioning

confidence: 99%

Scattering amplitudes for self-force

Adamo,

Cristofoli,

Ilderton

et al. 2024

Class. Quantum Grav.

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“…Second, the asymptotic behaviour of the Lorenz gauge MP towards the horizon and infinity is well-understood. Third, the existing Lorenz-gauge set-up has been successfully used in the Schwarzschild case for second-order calculations [21,[59][60][61][62][63]. Fourth, the Lorenz-gauge MP has been computed by other means (e.g.…”

Section: Introductionmentioning

confidence: 99%

Metric perturbations of Kerr spacetime in Lorenz gauge: circular equatorial orbits

Dolan,

Durkan,

Kavanagh

et al. 2024

Class. Quantum Grav.

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We construct the metric perturbation in Lorenz gauge for a compact body on a circular equatorial orbit of a rotating black hole (Kerr) spacetime, using a newly-developed method of separation of variables. The metric perturbation is formed from a linear sum of differential operators acting on Teukolsky mode functions, and certain auxiliary scalars, which are solutions to {\it ordinary} differential equations in the frequency domain. For radiative modes, the solution is uniquely determined by the $s=\pm2$ Weyl scalars, the $s=0$ trace, and $s=0,1$ gauge scalars whose amplitudes are determined by imposing continuity conditions on the metric perturbation at the orbital radius. The static (zero-frequency) part of the metric perturbation, which is handled separately, also includes mass and angular momentum completion pieces. The metric perturbation is validated against the independent results of a 2+1D time domain code, and we demonstrate agreement at the expected level in all components, and the absence of gauge discontinuities. In principle, the new method can be used to determine the Lorenz-gauge metric perturbation at a sufficiently high precision to enable accurate second-order self-force calculations on Kerr spacetime in future. We conclude with a discussion of extensions of the method to eccentric and non-equatorial orbits.

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“…This fact is especially pronounced in the modelling of extreme mass ratio inspirals [16][17][18][19][20][21][22], in which a stellar compact object, like a black hole or a neutron star, inspirals in the background of a supermassive black hole. Even when calibrating the GW waveforms, the starting points are CEOs [23,24]. Hence, in our study we focus on CEOs of an extended test body in pole-dipole-(spin induced) quadrupole approximation around a Kerr black hole.…”

Section: Introductionmentioning

confidence: 99%

Spinning test body orbiting around a Kerr black hole: Comparing spin supplementary conditions for circular equatorial orbits

2022

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This work discusses the motion of extended test bodies as described by the Mathisson-Papapetrou-Dixon (MPD) equations in the pole-dipole-quadrupole approximation. We focus on the case that the quadrupole is solely induced by the spin of the body which is assumed to move on a circular equatorial orbit in a Kerr background. To fix the center of mass of the MPD body we use two different spin supplementary conditions (SSCs): the Tulczyjew-Dixon SSC and the Mathisson-Pirani SSC. We provide the frequencies of the circular equatorial orbits for the pole-dipole-(spin induced) quadrupole approximation of the body for both SSCs. In the process we develop an explicit fourvelocity four-momentum relation for a pole-dipole-quadrupole body under the Mathisson-Pirani SSC.

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Comparing second-order gravitational self-force and effective one body waveforms from inspiralling, quasicircular and nonspinning black hole binaries. II. The large-mass-ratio case

Cited by 21 publications

References 67 publications

Scattering amplitudes for self-force

Scattering amplitudes for self-force

Metric perturbations of Kerr spacetime in Lorenz gauge: circular equatorial orbits

Spinning test body orbiting around a Kerr black hole: Comparing spin supplementary conditions for circular equatorial orbits

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