Gravitational radiation with 
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Bonga, Béatrice; Bunster, Claudio; Pérez, Alfredo

doi:10.1103/physrevd.108.064039

Cited by 9 publications

(8 citation statements)

References 64 publications

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“…In the case at hand, one can use (55) along with the transformation laws ( 46)-( 49) to separately evaluate the two contributions on the right-hand side of (56). Using again equalities up to integration by parts on the celestial angle, one finds…”

Section: Barnich-troessaert Bracketmentioning

confidence: 99%

“…The effect of cocycle shifts such as ( 62) can be dramatic, possibly even cancelling any field-dependence. To see this, take the initial split (55) and the cocycle (59) as starting points. Then shift the integrable charge (55a) by S ξ = f M − 2EG as in (60).…”

Section: Split Ambiguities Of Charge Algebrasmentioning

confidence: 99%

“…Radiative asymptotic symmetries are thus crucial for quantum gravity and gauge theories as a whole, and for Minkowskian holography in particular [13,[32][33][34][35][36][37][38][39]. Note that similar questions can also be raised in (Anti)-de Sitter [(A)dS] spacetimes, where radiation and holography with porous boundary conditions were recently studied in [40][41][42][43][44][45][46][47][48][49][50][51][52][53][54][55][56][57].…”

Section: Introductionmentioning

confidence: 99%

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Radiative asymptotic symmetries of 3D Einstein-Maxwell theory

Bosma,

Geiller,

Majumdar

et al. 2024

SciPost Phys.

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We study the null asymptotic structure of Einstein-Maxwell theory in three-dimensional (3D) spacetimes. Although devoid of bulk gravitational degrees of freedom, the system admits a massless photon and can therefore accommodate electromagnetic radiation. We derive fall-off conditions for the Maxwell field that contain both Coulombic and radiative modes with non-vanishing news. The latter produces non-integrability and fluxes in the asymptotic surface charges, and gives rise to a non-trivial 3D Bondi mass loss formula. The resulting solution space is thus analogous to a dimensional reduction of 4D pure gravity, with the role of gravitational radiation played by its electromagnetic cousin. We use this simplified setup to investigate choices of charge brackets in detail, and compute in particular the recently introduced Koszul bracket. When the latter is applied to Wald-Zoupas charges, which are conserved in the absence of news, it leads to the field-dependent central extension found earlier in [Class. Quantum Gravity 32, 245001 (2015)]. We also consider (Anti-)de Sitter asymptotics to further exhibit the analogy between this model and 4D gravity with leaky boundary conditions.

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Section: Barnich-troessaert Bracketmentioning

confidence: 99%

Section: Split Ambiguities Of Charge Algebrasmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Radiative asymptotic symmetries of 3D Einstein-Maxwell theory

Bosma,

Geiller,

Majumdar

et al. 2024

SciPost Phys.

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“…The study of the charges at null infinity in the presence of logarithmic terms and violations of peeling has been initiated in [91]. There is also an existing literature on the charges and the flat limit in (A)dS [18,19,[92][93][94][95][96][97], and it would be interesting to study whether the partial Bondi gauge and its extra set of charges could play a role in this context.…”

Section: Perspectivesmentioning

confidence: 99%

The partial Bondi gauge: Further enlarging the asymptotic structure of gravity

Geiller

Zwikel

2022

SciPost Phys.

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We present a detailed analysis of gravity in a partial Bondi gauge, where only the three conditions g_{rr}=0=g_{rA}grr=0=grA are fixed. We relax in particular the so-called determinant condition on the transverse metric, which is only assumed to admit a polyhomogeneous radial expansion. This is sufficient in order to build the solution space, which here includes a cosmological constant, time-dependent sources in the boundary metric, logarithmic branches, and an extra trace mode at subleading order in the transverse metric. The evolution equations are studied using the Newman–Penrose formalism in terms of covariant functionals identified from the Weyl scalars, and we build the explicit dictionary between this formalism and the tensorial Einstein equations. This provides in particular a new derivation of the (A)dS mass loss formula. We then study the holographic renormalisation of the symplectic potential, and the transformation laws under residual asymptotic symmetries. The advantage of the partial Bondi gauge is that it allows to contrast and treat in a unified manner the Bondi–Sachs and Newman–Unti gauges, which can each be reached upon imposing a further specific gauge condition. The differential determinant condition leads to the \LambdaΛ-BMSW gauge, while a differential condition on g_{ur}gur leads to a generalized Newman–Unti gauge. This latter gives access to a new asymptotic symmetry which acts on the asymptotic shear and further extends the \LambdaΛ-BMSW group by an extra abelian radial translation. This generalizes results which we have recently obtained in three dimensions.

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“…In the case of the positive cosmological constant, the Bondi mass has been discussed by various authors. See e.g [62,63]. and references therein.…”

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confidence: 99%

Robinson–Trautman solutions with scalar hair and Ricci flow

Nozawa,

Torii

2024

Class. Quantum Grav.

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The vacuum Robinson-Trautman solution admits a shear-free and twist-free null geodesic congruence. We perform a comprehensive classiﬁcation of solutions exhibiting this property in Einstein's gravity with a massless scalar ﬁeld. We ﬁnd that these solutions can be grouped into three distinct classes: (I-a) a natural extension of the Robinson-Trautman family incorporating a scalar hair satisfying the time derivative of the Ricci ﬂow equation, (I-b) a novel non-asymptotically ﬂat solution characterized by two functions satisfying Perelman's pair of the Ricci ﬂow equations, and (II) a dynamical solution possessing SO(3), ISO(2) or SO(1, 2) symmetry. We provide a complete list of all explicit solutions falling into Petrov type D for classes (I-a) and (I-b). Moreover, leveraging the massless solution in class (I-a), we derive the neutral Robinson-Trautman solution to the N = 2 gauged supergravity with the prepotential F (X) = -iX0X1. By ﬂipping the sign of the kinetic term of the scalar ﬁeld, the Petrov-D class (I-a) solution leads to a time-dependent wormhole with an instantaneous spacetime singularity. Although the general solution is unavailable for class (II), we ﬁnd a new dynamical solution with spherical symmetry from the AdS-Roberts solution via AdS/Ricci-ﬂat correspondence.

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Gravitational radiation with Λ>0

Abstract: The following full text is a publisher's version.For additional information about this publication click this link. https://repository.ubn.ru.nl/handle/2066/297531Please be advised that this information was generated on 2024-05-31 and may be subject to change.

Cited by 9 publications

References 64 publications

Radiative asymptotic symmetries of 3D Einstein-Maxwell theory

Radiative asymptotic symmetries of 3D Einstein-Maxwell theory

The partial Bondi gauge: Further enlarging the asymptotic structure of gravity

Robinson–Trautman solutions with scalar hair and Ricci flow

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