On the canonical energy of weak gravitational fields with a cosmological constant $$\varLambda \in \mathbb {R}$$

Chruściel, Piotr T.; Hoque, Sk Jahanur; Maliborski, Maciej; Smołka, Tomasz

doi:10.1140/epjc/s10052-021-09350-y

Cited by 10 publications

(4 citation statements)

References 51 publications

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“…The radius is chosen to be the luminosity distance, which amounts to fixing ∂ r det(g AB /r 2 ) = 0. In Bondi-Sachs gauge, the metric can be written as The explicit general expansion of an asymptotically (locally) de Sitter spacetime was derived in [30] (see [56] in the case of axial symmetry and [28,57,58] for subsequent work). The most general class of asymptotically (locally) de Sitter metrics takes the form…”

Section: Bondi Gauge and λ−Bms Symmetriesmentioning

confidence: 99%

“…Going beyond the quadrupolar order is beyond the scope of this paper. Given the mapping between harmonic coordinates and Bondi coordinates achieved in linearized theory around Minkowski spacetime [27] (see also section 4.2 of [28]), our second objective is to similarly map the quadrupolar linear solution in generalized harmonic gauge to Bondi gauge and derive the metric in closed form 6 .…”

Section: Introductionmentioning

confidence: 99%

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Quadrupolar radiation in de Sitter: displacement memory and Bondi metric

Compère,

Hoque,

Kutluk

2024

Class. Quantum Grav.

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We obtain the closed form expression for the metric perturbation around de Sitter spacetime generated by a matter source below Hubble scale both in generalized harmonic gauge and in Bondi gauge up to quadrupolar order in the multipolar expansion, including both parities (i.e. both mass and current quadrupoles). We demonstrate that such a source causes a displacement memory effect close to future infinity that originates, in the even-parity sector, from a Λ-BMS transition between the two non-radiative regions of future infinity.

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Section: Bondi Gauge and λ−Bms Symmetriesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Quadrupolar radiation in de Sitter: displacement memory and Bondi metric

Compère,

Hoque,

Kutluk

2024

Class. Quantum Grav.

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“…• Studies using techniques of exact solutions, analyzing the asymptotic behaviour of the Weyl tensor [49], or the radiation generated by accelerating balck holes [66,42] • Definitions of mass-energy, by using spinorial techniques [82,83], or Newman-Penrose expansions in preferred coordinate systems [74], or on null hypersurfaces [21], or for weak gravitational waves [20,19], or using Hamiltonian techniques [22], or -for the case of a black hole-assuming the existence of a timelike Killing vector [25]. For a review, see [84].…”

Section: Introductionmentioning

confidence: 99%

Gravitational Radiation at Infinity with Non-Negative Cosmological Constant

Senovilla

2022

Universe

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The existence of gravitational radiation arriving at null infinity J+, i.e., escaping from the physical system, is addressed in the presence of a non-negative cosmological constant Λ≥0. The case with vanishing Λ is well understood and relies on the properties of the News tensor field (or the News function) defined at J+. The situation is drastically different when Λ>0, where there is no known notion of `News’ with similar good properties. In this paper, both situations are considered jointly from a tidal point of view, that is, taking into account the strength (or energy) of the curvature tensors. The fundamental object used for this purposes is the asymptotic (radiant) super-momentum, a causal vector defined at infinity with remarkable properties. This leads to a novel characterization of gravitational radiation valid for the general case with Λ≥0, which has been proven to be equivalent when Λ=0 to the standard one based on News. Here, the implications of this result when Λ>0 are analyzed in detail. A general procedure to construct `News tensors’ when Λ>0 is depicted, a proposal for asymptotic symmetries is provided, and an example of a conserved charge that may detect gravitational radiation at J+ is exhibited. A series of illustrative examples is listed as well.

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“…al. [24][25][26] which discuss different approaches for the computation of energy and linear fluxes between null cones in dS, see also [27][28][29][30][31]. A number of other approaches to examining radiative bodies in dS can be found in [32][33][34][35][36][37].…”

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confidence: 99%

Charges, conserved quantities and fluxes in de Sitter spacetime

Poole¹,

Skenderis²,

Taylor³

2021

Preprint

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We discuss the definition of conserved quantities in asymptotically locally de Sitter spacetimes. One may define an analogue of holographic charges at future and past infinity and at other Cauchy surfaces It as integrals over the intersection of timelike surfaces C and the Cauchy surface It. In general, the charges Q t defined on the Cauchy surface It depend on C, but their difference ∆Q t (C1, C2) = Q t (C1) − Q t (C2) is a conserved quantity under time evolution (i.e. independent of the Cauchy surface) if gravitational flux is absent. On the other hand, if there is a net gravitational flux entering or leaving the spacetime region bounded by C1, C2 and two Cauchy surfaces then ∆Q t (C1, C2) changes by the same amount.

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On the canonical energy of weak gravitational fields with a cosmological constant $$\varLambda \in \mathbb {R}$$

Cited by 10 publications

References 51 publications

Quadrupolar radiation in de Sitter: displacement memory and Bondi metric

Quadrupolar radiation in de Sitter: displacement memory and Bondi metric

Gravitational Radiation at Infinity with Non-Negative Cosmological Constant

Charges, conserved quantities and fluxes in de Sitter spacetime

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