From Scattering in Black Hole Backgrounds to Higher-Spin Amplitudes: Part I

Bautista, Yilber Fabian; Guevara, Alfredo; Kavanagh, Chris; Vines, Justin

doi:10.48550/arxiv.2107.10179

Cited by 23 publications

(55 citation statements)

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“…Here the retarded time u : t − r is fixed and now corresponds to the celestial sphere. As in [83], this translates directly into our starting data (37), see also appendix I.…”

Section: Four-point Amplitudes: Radiative Momentsmentioning

confidence: 99%

“…In this case, our equation (10) is nothing but a (free) bulk field reconstructed from its radiative data ψ, by inverting the retarded propagation. Now, quite remarkably, it has been argued that the modes of ψ(u), being purely on-shell, are given by a coherent-classical limit of scattering amplitudes [81][82][83][84].…”

Section: Analytic Continuation and Reconstructionmentioning

confidence: 99%

“…The extension to Gravitational Waves is straightforward. The QFT description of such processes in terms of a four-point S-Matrix in (1, 3) was recently studied in [83,99].…”

Section: Four-point Amplitudes: Radiative Momentsmentioning

confidence: 99%

“…In (1,3) signature, this is radiative because the massive source is accelerated by an incoming wave. Identifying the source with a linearized black hole, it was found in [83] that the Regge-Wheeler amplitudes j(k) = M 4 (k) solely depend on the direction of k µ = ω µ in the longwavelength regime. Thus they can be easily written in terms of spherical harmonics, see appendix III,…”

Section: Four-point Amplitudes: Radiative Momentsmentioning

confidence: 99%

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Reconstructing Classical Spacetimes from the S-Matrix in Twistor Space

Guevara¹

2021

Preprint

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We present a holographic construction of solutions to the gravitational wave equation starting from QFT scattering amplitudes. The construction amounts to a change of basis from momentum to (2, 2) twistor space, together with a recently introduced analytic continuation between (2, 2) and (1, 3) spacetimes. We test the transform for three and four-point amplitudes in a classical limit, recovering both stationary and dynamical solutions in GR as parametrized by their tower of multipole moments, including the Kerr black hole. As a corollary, this provides a link between the Kerr-Schild classical double copy and the QFT double copy.

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“…Here the retarded time u : t − r is fixed and now corresponds to the celestial sphere. As in [83], this translates directly into our starting data (37), see also appendix I.…”

Section: Four-point Amplitudes: Radiative Momentsmentioning

confidence: 99%

Section: Analytic Continuation and Reconstructionmentioning

confidence: 99%

“…The extension to Gravitational Waves is straightforward. The QFT description of such processes in terms of a four-point S-Matrix in (1, 3) was recently studied in [83,99].…”

Section: Four-point Amplitudes: Radiative Momentsmentioning

confidence: 99%

Section: Four-point Amplitudes: Radiative Momentsmentioning

confidence: 99%

See 2 more Smart Citations

Reconstructing Classical Spacetimes from the S-Matrix in Twistor Space

Guevara¹

2021

Preprint

Self Cite

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“…Spin effects were included in PM expansions using all these approaches in Refs. [75][76][77][78][79][80][81][82][83][84][85][86][87][88], and radiative contributions in Refs. [89][90][91][92][93].…”

Section: Introductionmentioning

confidence: 99%

Gravitational spin-orbit dynamics at the fifth-and-a-half post-Newtonian order

Khalil

2021

Preprint

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Accurate waveform models are crucial for gravitational-wave data analysis, and since spin has a significant effect on the binary dynamics, it is important to improve the spin description in these models. In this paper, we derive the spin-orbit (SO) coupling at the fifth-and-a-half post-Newtonian (5.5PN) order. The method we use splits the conservative dynamics into local and nonlocal-in-time parts, then relates the local-in-time part to gravitational self-force results by exploiting the simple mass-ratio dependence of the post-Minkowskian expansion of the scattering angle. We calculate the nonlocal contribution to the 5.5PN SO dynamics to eighth order in the small-eccentricity expansion for bound orbits, and to leading order in the large-eccentricity expansion for unbound orbits. For the local contribution, we obtain all the 5.5PN SO coefficients from first-order self-force results for the redshift and spin-precession invariants, except for one unknown that could be fixed in the future by second-order self-force results. However, by incorporating our 5.5PN results in the effective-onebody formalism and comparing its binding energy to numerical relativity, we find that the remaining unknown has a small effect on the SO dynamics, demonstrating an improvement in accuracy at that order.

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The ultrarelativistic limit of Kerr

Adamo

Cristofoli

Tourkine

2023

J. High Energ. Phys.

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The massless (or ultrarelativistic) limit of a Schwarzschild black hole with fixed energy was determined long ago in the form of the Aichelburg-Sexl shockwave, but the status of the same limit for a Kerr black hole is less clear. In this paper, we explore the ultrarelativistic limit of Kerr in the class of Kerr-Schild impulsive pp-waves by exploiting a relation between the metric profile and the eikonal phase associated with scattering between a scalar and the source of the metric. This gives a map between candidate metrics and tree-level, 4-point scattering amplitudes. At large distances from the source, we find that all candidates for the massless limit of Kerr in this class do not have spin effects. This includes the metric corresponding to the massless limit of the amplitude for gravitational scattering between a scalar and a massive particle of infinite spin. One metric, discovered by Balasin and Nachbagauer, does have spin and finite size effects at short distances, leading to a remarkably compact scattering amplitude with many interesting properties. We also discuss the classical single copy of the ultrarelativistic limit of Kerr in electromagnetism.

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From Scattering in Black Hole Backgrounds to Higher-Spin Amplitudes: Part I

Cited by 23 publications

References 0 publications

Reconstructing Classical Spacetimes from the S-Matrix in Twistor Space

Reconstructing Classical Spacetimes from the S-Matrix in Twistor Space

Gravitational spin-orbit dynamics at the fifth-and-a-half post-Newtonian order

The ultrarelativistic limit of Kerr

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