Radiation reaction for spinning black-hole scattering

Alessio, Francesco; Di Vecchia, Paolo

doi:10.48550/arxiv.2203.13272

Cited by 4 publications

(6 citation statements)

References 76 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Moreover, to the leading 3PM order, Eq. (4.14) has been explicitly shown to hold also if the colliding objects carry spin, for generic spin alignments [64]. Via unitarity, analyticity and crossing symmetry, the 3PM divergent part of Im 2δ immediately provides the radiationreaction corrections to the 3PM deflection [18,55].…”

Section: Zfl (And Im 2δ) At Arbitrary Velocitiesmentioning

confidence: 94%

The eikonal operator at arbitrary velocities I: the soft-radiation limit

Vecchia¹,

Heissenberg²,

Russo³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

Observables related to the real part of the gravitational eikonal, such as the deflection angle and time delay, have been found so far to have a smooth post-Minkowskian (PM) expansion whose validity extends from the non-relativistic to the most extreme ultra-relativistic (UR) regime, which smoothly connects with massless particle collisions. To describe gravitational radiation, the eikonal phase has to be promoted to a unitary operator for which we motivate a proposal and start discussing properties in the softradiation limit. A convergent PM expansion is found to only hold below an UR bound (discussed in the GR literature in the seventies) above which a different expansion is instead needed implying, in general, some non-analyticity in Newton's constant. In this extreme UR regime soft radiative observables receive contributions only from gravitons and are therefore universal. This generalises the pattern discussed in [1] beyond the elastic case.

show abstract

Section: Zfl (And Im 2δ) At Arbitrary Velocitiesmentioning

confidence: 94%

The eikonal operator at arbitrary velocities I: the soft-radiation limit

Vecchia¹,

Heissenberg²,

Russo³

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

show abstract

“…Analogous results, obtained independently through various worldline effective field theory (EFT) approaches, followed shortly thereafter [42][43][44][45][46][47]. These results were later extended to include tidal deformation [48][49][50][51][52][53][54][55] and spin effects [56][57][58][59][60][61][62][63][64][65][66][67].…”

mentioning

confidence: 70%

“…(See also Refs. [66,67,[73][74][75][76][77][78][79][80][81][82][83][84][85][86][87] for related works on radiative effects.) Notably absent from the literature, however, is the inclusion of spins in the radiated observables at 3PM.…”

mentioning

confidence: 99%

Gravitational bremsstrahlung from spinning binaries in the post-Minkowskian expansion

Riva,

Vernizzi,

Wong

2022

Preprint

View full text Add to dashboard Cite

We present a novel calculation of the four-momentum that is radiated into gravitational waves during the scattering of two arbitrarily spinning bodies. Our result, which is accurate to leading order in 𝐺, to quadratic order in the spins, and to all orders in the velocity, is derived by using a Routhian-based worldline effective field theory formalism in concert with a battery of analytic techniques for evaluating loop integrals. While nonspinning binaries radiate momentum only along the direction of their relative velocity, we show that the inclusion of spins generically allows for momentum loss in all three spatial directions. We also verify that our expression for the radiated energy agrees with the overlapping terms from state-of-the-art calculations in post-Newtonian theory.

show abstract

“…Several approaches have been taken to remedy these unphysicalities [51,[59][60][61][62]. Results including spin at 3PM have also begun to emerge [63,64]. Recently, refs.…”

mentioning

confidence: 99%

“…Observables related to classical scattering involving a spinning object can be derived from amplitudes using a variety of methods [10,11,14,43]. One approach passes through the eikonal phase [43,46,56,60,64,[66][67][68], which we present for aligned-spin scattering.…”

mentioning

confidence: 99%

Classical gravitational spinning-spinless scattering at $\mathcal{O}(G^{2} S^{\infty})$

Aoude,

Haddad,

Helset

2022

Preprint

View full text Add to dashboard Cite

Making use of the recently-derived, all-spin, opposite-helicity Compton amplitude, we calculate the classical gravitational scattering amplitude for one spinning and one spinless object at O(G 2 ) and all orders in spin. By construction, this amplitude exhibits the spin structure that has been conjectured to describe Kerr black holes. This spin structure alone is not enough to fix all deformations of the Compton amplitude by contact terms, but when combined with considerations of the ultrarelativistic limit we can uniquely assign values to the parameters remaining in the even-in-spin sector. Once these parameters are determined, much of the spin dependence of the amplitude resums into hypergeometric functions. Finally, we derive the eikonal phase for aligned-spin scattering. I. INTRODUCTIONRecent years have seen a large mobilization within the scattering amplitudes community towards describing the gravitational coalescence of compact objects. This stems from the necessity for ever-more precise gravitational wave templates in current and upcoming gravitational wave observatories [1-7], and because scattering amplitudes are eminently suited to calculating classical observables in the post-Minkowskian (PM) expansion [8][9][10][11][12][13][14][15][16]. This huge effort has led to unprecedented precision in the PM description of spinless scattering [17][18][19][20][21][22][23][24][25][26][27][28][29][30], tidal effects [31][32][33][34][35][36][37], and radiation [23][24][25][38][39][40][41]].Yet another pertinent property affecting the motion of the constituents of a binary is their individual rotational angular momenta. The connection between classical rotational angular momentum and quantum spin appearing in scattering amplitudes is by now well understood [11,[42][43][44]. Classical scattering at 1PM is known to all orders in the spin vectors for Kerr black holes [45][46][47][48][49] and general spinning bodies [44]. Dynamics at 2PM have been understood up to quartic order in spin [37,43,46,[50][51][52][53][54][55][56][57]. Until recently, progress past quartic order at 2PM has been restricted owing partly to the absence of a physical opposite-helicity Compton amplitude above this spin order [58]. Several approaches have been taken to remedy these unphysicalities [51,[59][60][61][62]. Results including spin at 3PM have also begun to emerge [63,64]. Recently, refs. [62,65] have pushed the state-of-theart in the scattering of spinning objects at 2PM past the fourth order in spin. In the former work, we applied the

show abstract

Radiation reaction for spinning black-hole scattering

Cited by 4 publications

References 76 publications

The eikonal operator at arbitrary velocities I: the soft-radiation limit

The eikonal operator at arbitrary velocities I: the soft-radiation limit

Gravitational bremsstrahlung from spinning binaries in the post-Minkowskian expansion

Classical gravitational spinning-spinless scattering at $\mathcal{O}(G^{2} S^{\infty})$

Contact Info

Product

Resources

About