Pith. sign in

REVIEW 2 major objections 4 minor 161 references

Gravitational memory can be defined quasilocally on finite null screens, with the standard Bondi displacement memory emerging as its universal large-radius limit.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-01 14:40 UTC pith:LDQ6O2FM

load-bearing objection Plausible quasilocal memory framework, but the paper's key large-radius projection to Bondi memory is assumed rather than derived from its RT example. the 2 major comments →

arxiv 2607.18675 v1 pith:LDQ6O2FM submitted 2026-07-21 hep-th gr-qc

Gravitational Memory Beyond Null Infinity through Finite-Distance Carrollian Screens

Felipe Diaz , Sercan H\"usn\"ugil , Oriana Labrin , Leonardo Sanhueza This is my paper
classification hep-th gr-qc MSC 83C3083C3583C40 PACS 04.30.-w04.20.-q
keywords gravitational memoryCarrollian screennull hypersurfaceBondi sheardisplacement memoryRobinson-Trautman spacetimesnull Brown-York tensorquasilocal observables
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper argues that gravitational memory is not only an asymptotic observable at future null infinity: it can be defined intrinsically on any finite null hypersurface, called a Carrollian screen, through the residual change of its degenerate metric, optical data, and embedding between two cuts. Using the exactly solvable Robinson–Trautman family of radiative spacetimes, the authors construct the Bondi data at large radius and show that the tracefree, radius-normalized change of the finite-screen metric converges to the retarded-time integral of the Bondi news—the standard displacement memory. Finite-distance corrections retain focusing, embedding, angular drift, Coulombic, and near-zone information that the strict asymptotic limit discards. This matters because real detectors sit at finite radius, so the paper supplies a precise geometric object interpolating between local screen measurements and the idealized memory at infinity.

Core claim

The paper establishes that a finite null screen's intrinsic Carrollian data carry a quasilocal memory observable, and that its leading tracefree large-radius component is exactly the Bondi displacement memory. The central identity is ΔC_AB = lim_{r_N→∞} (1/r_N)(Δ_N q_AB)^TF = ∫_{u_i}^{u_f} du N_AB, which identifies the radius-normalized tracefree jump of the screen metric with the usual Bondi news integral. In the linearized Robinson–Trautman sector, the Bondi shear is purely electric, the memory records relaxation from an initially radiative cut to the final Schwarzschild cut, and higher multipoles are suppressed by faster decay rates. The same Robinson–Trautman equation that drives the bul

What carries the argument

The central object is the finite Carrollian screen: a null hypersurface r = ρ(u, x^A) carrying a degenerate cut metric q_AB = ρ^2 e^Φ γ_AB, a null generator ℓ = ∂_u + V^A ∂_A, an optical expansion and shear θ_AB = (1/2)∂_u q_AB + D_A D_B ρ, and a null Brown–York tensor built from the Weingarten map. The load-bearing identity is the large-radius bridge, eq. (6.18), which extracts ∫ N_AB du as the r_N-normalized tracefree limit of the screen-metric jump. The exactly solvable Robinson–Trautman equation acts as the engine: it simultaneously fixes the Bondi news, fixes the screen embedding through the nullity condition, and reduces the projected Einstein equations on the screen to Carrollian flui

Load-bearing premise

The bridge to Bondi memory relies on finite screens at large radius having the Bondi-frame falloffs q^N_AB = r_N^2 γ_AB + r_N C_AB + O(r_N^0), angular drift V^A = O(r_N^{-2}), and optical shear σ_AB = (1/2)r_N N_AB + O(r_N^0); if a screen violates these falloffs, the finite-screen memory need not reduce to the Bondi displacement memory.

What would settle it

Find a radiative spacetime and choose a finite null screen whose angular drift decays as r_N^{-1} instead of r_N^{-2}, or whose optical shear has a different leading power in r_N; then compute the tracefree screen-memory divided by radius. If it does not converge to ∫ N_AB du, the central identity (6.18) fails. Alternatively, in a numerical Robinson–Trautman evolution, evaluate both sides of (6.18) at a sequence of finite radii and check the convergence.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If the central claim is correct, Bondi displacement memory is not an independent asymptotic observable but the universal wave-zone projection of a quasilocal Carrollian response on finite null screens.
  • Finite screens offer a quasilocal detector picture: scalar area/focusing memory, tracefree shape memory, and a momentum memory encoded in the Hájíček one-form, all governed by the optical balance laws on the screen.
  • In linearized Robinson–Trautman spacetimes, each radiative mode produces purely electric Bondi shear, an ordinary displacement-memory effect, and a memory dominated by the quadrupole because higher multipoles relax faster.
  • Late-time screens approaching the final Schwarzschild horizon exhibit exponentially decaying non-isotropic Carrollian data, leaving only the isotropic Schwarzschild null Brown–York stress; the memory is a transition to a round screen, not permanent nonspherical hair.
  • For nonzero cosmological constant the conformal boundary is no longer null, so the standard Bondi memory construction is unavailable, but finite-screen memory remains well defined in the bulk.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Beyond the paper: because real detectors are at finite radius, this framework suggests defining observables that combine displacement with focusing and drift, then using the large-radius limit to compare with standard Bondi predictions—a testable extension the paper motivates but does not perform.
  • Beyond the paper: the screen dependence of finite-screen memory could be converted into a tomographic probe; choosing screens at different radii and orientations would separate universal radiative data from near-zone Coulombic and focusing data for a given source.
  • Beyond the paper: the exponential Robinson–Trautman relaxation modes provide classical saddle profiles for retarded-time moments of the news, so in a quantized null-surface treatment the whole tower of light-ray and celestial memory correlators would be fixed by the displacement-memory profile and the relaxation rate.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 4 minor

Summary. The paper develops a quasilocal description of gravitational memory on finite null Carrollian screens, using Robinson–Trautman (RT) spacetimes as an exactly solvable family. Sections 2–4 construct an asymptotic map to Bondi gauge, extract the Bondi shear, news, mass aspect, and angular-momentum aspect, and then specialize to linearized Newman–Foster modes, obtaining a purely electric Bondi shear and an explicit displacement-memory formula. Section 5 introduces finite null screens via the nullity condition and packages their optical data as a Carrollian fluid, showing that the screen conservation laws reduce to the RT equation. Section 6 defines finite-screen memory as the residual change of the intrinsic Carrollian data between two cuts and claims that its large-radius tracefree part reproduces the Bondi displacement memory. Section 7 treats Λ≠0, constructing the RT solution to second order and studying a holographic charge that does not obey a universal monotonicity property. The central proposal is that Bondi displacement memory is the universal wave-zone projection of a broader quasilocal Carrollian response.

Significance. If fully established, the paper would provide a concrete classical bridge between finite-distance null-hypersurface observables and the standard Bondi memory, with RT spacetimes as an exactly solvable laboratory. The strengths are substantial: an explicit asymptotic RT-to-Bondi map, closed-form linearized memory and news profiles, a proof that the linearized shear is purely electric, a detailed late-time Carrollian-fluid analysis of horizon-settling screens, and a nontrivial Λ≠0 holographic flux computation. The main weakness is that the large-radius bridge — the load-bearing step connecting the finite-screen observable to Bondi memory — is assumed rather than derived from the RT construction. In addition, a claimed exact solution of the time-map equation is incorrect. These issues affect the central claim and need to be addressed before the paper can be recommended for publication.

major comments (2)
  1. [§6, Eqs. (6.10)–(6.18)] The central bridge is not derived from the RT construction. For the RT screens, σ_AB = (D_BD_A − ½q_AB D²)ρ, so Eq. (6.10) gives (Δ_N q_AB)^TF = 2∫[σ_AB − (D_AD_Bρ)^TF]du = 0 identically, as the text itself notes. The nonzero Bondi result is then recovered by “switching to a large screen in Bondi gauge” and assuming the asymptotic screen expansion q^N_AB = r_N² γ_AB + r_N C_AB + O(r_N⁰), σ_AB = ½ r_N N_AB + O(r_N⁰). Under these assumptions, (6.17)–(6.18) are a restatement of the Bondi definitions of C_AB and N_AB, not a limit of the previously defined RT finite-screen observable. To substantiate the central claim, the authors should push the RT screen through the §3 Bondi map and verify that the induced screen expansion has precisely the C_AB computed in §4, or alternatively show that the generator-adapted memory Δ_ℓ Q_AB of Eq. (6.3) has the same large-radius limit. As it stands, the pa
  2. [§4.1, Eq. (4.13)] The claimed exact solution of (4.12) is incorrect. Let y = ε_ℓ e^{−ω_ℓ(u+β)} P_ℓ(cosθ). Differentiating (4.13) gives ∂_u U_(0) = (1 + y/4)/(1 − y/4), whereas (4.12) requires √(1+y). These agree only to linear order and differ at O(y²). The first-order expansion (4.15) is correct, so the linear memory formulas (4.19)–(4.28) are unaffected, but the statement that the time map is “exactly solvable” is false and should be corrected or downgraded.
minor comments (4)
  1. [§3.2, Eq. (3.41)] The angular-momentum aspect N_A is asserted to satisfy the Bondi angular-momentum flux equation modulo the RT equation, but its explicit expression is withheld (“not illuminating”). Since this is a nontrivial consistency check, please include the expression in an appendix or provide a reproducible computation.
  2. [§6, Eq. (6.4)] The notation Δ_N q_AB mixes the fixed-coordinate difference and the generator-adapted pullback. Please define the map between the two cut-identification prescriptions explicitly to avoid the impression that the fixed-frame and generator-adapted observables are the same object.
  3. [References] Reference [97] is listed as “To appear” with no arXiv number; if it is used as the basis for the asymptotic-screen expansion, a published or preprint version should be cited. Several other bibliography entries are arXiv:26xx preprints; please ensure they are available and correctly dated.
  4. [Typos/rendering] The name “Hájíček” appears with a malformed combining character in several places. Also, in the abstract and §7, the statement that the charge “does not obey a universal monotonicity property” is specific to the chosen generator ξ = −∂_u and the fixed-round frame; this is acknowledged in the text, and the abstract could be phrased more cautiously.

Circularity Check

0 steps flagged

No significant circularity: finite-screen memory is an independent quasilocal observable, and the large-radius Bondi limit is a standard consistency identity, not a fitted input.

full rationale

The central derivation chain is not circular. Section 3 constructs an explicit asymptotic diffeomorphism from Robinson–Trautman coordinates to Bondi gauge and extracts the Bondi shear, news, mass aspect, and angular-momentum aspect directly in terms of the RT field; this involves no fitting of the target memory. Section 4 then computes the linearized displacement memory (4.24) from the RT modes by direct integration, independent of the later finite-screen construction. Section 6 defines finite-screen memory from independent geometric data — the induced cut metric q_AB, optical shear σ_AB, and embedding function ρ — via (6.4)–(6.10). Equation (6.18) is obtained from the standard Bondi-gauge screen expansion q^N_AB = r_N^2 γ_AB + r_N C_AB + O(r_N^0) and the consequence σ_AB = (1/2) r_N N_AB + O(r_N^0), where N_AB = ∂_u C_AB is the Bondi definition (A.8). Thus ΔC_AB = ∫ du N_AB is the usual Bondi displacement memory identity, not a circular restatement or a fitted parameter renamed as a prediction. The paper transparently acknowledges that in the natural RT frame the tracefree fixed-frame deformation vanishes because σ_AB = (D_A D_B ρ)^TF for RT screens; the Bondi result is obtained by switching to Bondi gauge, which is a separate, independently derived asymptotic frame. This is a limitation of the explicit RT demonstration, but not a circularity, because the Bondi data were computed in Section 3 without reference to the finite-screen memory. Self-citations appear ([43], [97], and [39]), but they are peripheral to the main derivation; the crucial asymptotic screen expansion is cited to [85], an external reference, and its content is standard Bondi–Sachs asymptotics. The holographic charge analysis in Section 7 is also an independent computation from the RT solution and the holographic dictionary. Overall, the paper's central claim does not reduce to its inputs by construction, so the circularity score is 0.

Axiom & Free-Parameter Ledger

4 free parameters · 7 axioms · 0 invented entities

No new particles, forces, or dynamical entities are introduced. 'Carrollian screen' and 'finite-screen memory' are names for existing geometric objects (null hypersurfaces and their residual deformations), not new physical entities. The main inputs are solution parameters and external frameworks.

free parameters (4)
  • ε_ℓ
    Linearized Robinson–Trautman mode amplitude; an input perturbation amplitude that controls the size of the Bondi and finite-screen memory (Section 4). Not fitted to data.
  • m
    Robinson–Trautman mass parameter; an integration constant of the family, not fitted to data.
  • β(θ) = set to 0
    Residual supertranslation function in the leading time map U^(0); a gauge choice, set to zero for the memory computation (Section 4.1).
  • C_ℓ = 0
    Homogeneous screen transient in the nullity-condition solution for the near-horizon screen; set to zero to select the horizon-settling screen (Section 5.1).
axioms (7)
  • standard math Vacuum Einstein equations and the null Brown–York conservation identity D_b T^a_b = 0 on null hypersurfaces.
    Used throughout Sections 5–6 and Appendix B to package the projected Einstein equations as Carrollian fluid equations.
  • domain assumption Robinson–Trautman metrics solve the vacuum Einstein equations with a geodesic, shear-free, twist-free, expanding null congruence, and relax to Schwarzschild at late retarded time under suitable regularity (Chruściel).
    Section 2 and Section 5.1 rely on this external theorem to identify the late-time screen with the Schwarzschild horizon.
  • standard math Bondi–Sachs gauge expansion and peeling hierarchy for asymptotically flat spacetimes, including the standard definitions of shear, news, mass aspect, and angular momentum aspect.
    Appendix A fixes conventions used to extract Bondi data in Section 3.
  • domain assumption The asymptotic diffeomorphism (3.1) can be solved order-by-order with the stated falloffs (3.19)–(3.24).
    The entire Bondi-data extraction in Section 3 rests on this coordinate transformation; the authors state they carried the recursion further as a consistency check but do not display all terms.
  • standard math Carrollian null-screen framework: rigging-dependent Weingarten map, Hájíček one-form, and null Brown–York tensor as reviewed in Appendix B.
    Section 5 and Appendix B adapt existing null-hypersurface geometry to define finite-screen data.
  • domain assumption Λ-BMS gauge and the Fefferman–Graham holographic dictionary of [44–46] for the cosmological-constant analysis.
    Section 7 and Appendix D use this external dictionary to define the holographic charge and its flux-balance law.
  • standard math Newman–Foster linearized RT modes solve the linearized RT equation and decay exponentially for ℓ ≥ 2.
    Section 4 uses the mode decomposition and decay rates as the basis for the linearized memory computation.

pith-pipeline@v1.3.0-alltime-deepseek · 59103 in / 14316 out tokens · 152938 ms · 2026-08-01T14:40:46.220397+00:00 · methodology

0 comments
read the original abstract

We investigate gravitational memory beyond null infinity by studying finite-distance null hypersurfaces endowed with Carrollian geometry. We show that the intrinsic degenerate geometry, optical data, and null Brown--York tensor of a finite null screen define a quasilocal Carrollian dissipative system, providing a natural framework to characterize the residual geometric response after the passage of radiation. To make this construction explicit and compare it with the standard asymptotic description, we use Robinson--Trautman spacetimes as an exactly solvable radiative setting. For asymptotically flat Robinson--Trautman geometries, we transform the solution to Bondi gauge and extract the asymptotic data directly in terms of the Robinson--Trautman field. In the linearized sector, the Bondi shear is purely electric and produces the standard displacement-memory effect associated with the relaxation toward the final Schwarzschild geometry. We show that the leading large-radius tracefree component of the finite-screen memory reduces to the Bondi displacement memory, while finite-distance corrections retain additional focusing, embedding dependence, angular drift, Coulombic data, and near-zone information. Thus, Bondi memory emerges as the universal asymptotic projection of a broader quasilocal Carrollian response. Late-time screens approaching the final Schwarzschild horizon exhibit exponentially decaying non-isotropic Carrollian data, leaving only the isotropic null Brown--York stress. As a by-product, we construct the Robinson--Trautman solution with nonzero cosmological constant to second order in the radiative amplitude and use the holographic dictionary to study the associated energy fluxes and find that the resulting charge does not obey a universal monotonicity property.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

161 extracted references · 112 linked inside Pith

  1. [1]

    Strominger,Lectures on the Infrared Structure of Gravity and Gauge Theory

    A. Strominger,Lectures on the Infrared Structure of Gravity and Gauge Theory. 3, 2017

    2017

  2. [2]

    Bondi,Gravitational Waves in General Relativity,Nature186(1960) 535–535

    H. Bondi,Gravitational Waves in General Relativity,Nature186(1960) 535–535

    1960

  3. [3]

    R. K. Sachs,Gravitational waves in general relativity. 6. The outgoing radiation condition,Proc. Roy. Soc. Lond. A264(1961) 309–338

    1961

  4. [4]

    Bondi, M

    H. Bondi, M. G. J. van der Burg and A. W. K. Metzner,Gravitational waves in general relativity. 7. Waves from axisymmetric isolated systems,Proc. Roy. Soc. Lond. A269(1962) 21–52

    1962

  5. [5]

    R. K. Sachs,Gravitational waves in general relativity. 8. Waves in asymptotically flat space-times,Proc. Roy. Soc. Lond. A270(1962) 103–126

    1962

  6. [6]

    T. He, V. Lysov, P. Mitra and A. Strominger,BMS supertranslations and Weinberg’s soft graviton theorem, JHEP05(2015) 151, [1401.7026]

    Pith/arXiv arXiv 2015

  7. [7]

    Donnay and R

    L. Donnay and R. Ruzziconi,BMS flux algebra in celestial holography,JHEP11(2021) 040, [2108.11969]

    Pith/arXiv arXiv 2021

  8. [8]

    Pasterski, M

    S. Pasterski, M. Pate and A.-M. Raclariu,Celestial Holography, inSnowmass 2021, 11, 2021,2111.11392

    Pith/arXiv arXiv 2021

  9. [9]

    Raclariu,Lectures on Celestial Holography,2107.02075

    A.-M. Raclariu,Lectures on Celestial Holography,2107.02075

    Pith/arXiv arXiv

  10. [10]

    Gonzo and A

    R. Gonzo and A. Pokraka,Light-ray operators, detectors and gravitational event shapes,JHEP05(2021) 015, [2012.01406]

    Pith/arXiv arXiv 2021

  11. [11]

    Y. B. Zel’dovich and A. G. Polnarev,Radiation of gravitational waves by a cluster of superdense stars,Sov. Astron.18(1974) 17

    1974

  12. [12]

    V. B. Braginsky and L. P. Grishchuk,Kinematic Resonance and Memory Effect in Free Mass Gravitational Antennas,Sov. Phys. JETP62(1985) 427–430

    1985

  13. [13]

    V. B. Braginsky and K. S. Thorne,Gravitational-wave bursts with memory and experimental prospects,Nature 327(1987) 123–125

    1987

  14. [14]

    Christodoulou,Nonlinear nature of gravitation and gravitational wave experiments,Phys

    D. Christodoulou,Nonlinear nature of gravitation and gravitational wave experiments,Phys. Rev. Lett.67 (1991) 1486–1489. – 70 –

    1991

  15. [15]

    K. S. Thorne,Gravitational-wave bursts with memory: The Christodoulou effect,Phys. Rev. D45(1992) 520–524

    1992

  16. [16]

    Strominger and A

    A. Strominger and A. Zhiboedov,Gravitational Memory, BMS Supertranslations and Soft Theorems,JHEP 01(2016) 086, [1411.5745]

    Pith/arXiv arXiv 2016

  17. [17]

    Speziale and D

    S. Speziale and D. A. Steer,An Introduction to Gravitational Wave Theory,2508.21817

    arXiv

  18. [18]

    Bredberg, C

    I. Bredberg, C. Keeler, V. Lysov and A. Strominger,Wilsonian Approach to Fluid/Gravity Duality,JHEP03 (2011) 141, [1006.1902]

    Pith/arXiv arXiv 2011

  19. [19]

    Chandrasekaran, É

    V. Chandrasekaran, É. É. Flanagan and K. Prabhu,Symmetries and charges of general relativity at null boundaries,JHEP11(2018) 125, [1807.11499]

    Pith/arXiv arXiv 2018

  20. [20]

    Chandrasekaran, E

    V. Chandrasekaran, E. E. Flanagan, I. Shehzad and A. J. Speranza,Brown-York charges at null boundaries, JHEP01(2022) 029, [2109.11567]

    Pith/arXiv arXiv 2022

  21. [21]

    Chandrasekaran, E

    V. Chandrasekaran, E. E. Flanagan, I. Shehzad and A. J. Speranza,A general framework for gravitational charges and holographic renormalization,Int. J. Mod. Phys. A37(2022) 2250105, [2111.11974]

    Pith/arXiv arXiv 2022

  22. [22]

    Chandrasekaran and A

    V. Chandrasekaran and A. J. Speranza,Anomalies in gravitational charge algebras of null boundaries and black hole entropy,JHEP01(2021) 137, [2009.10739]

    Pith/arXiv arXiv 2021

  23. [23]

    Duval, G

    C. Duval, G. W. Gibbons and P. A. Horvathy,Conformal Carroll groups and BMS symmetry,Class. Quant. Grav.31(2014) 092001, [1402.5894]

    Pith/arXiv arXiv 2014

  24. [24]

    Lévy-Leblond,Une nouvelle limite non-relativiste du groupe de poincaré,Annales de l’I.H.P

    J.-M. Lévy-Leblond,Une nouvelle limite non-relativiste du groupe de poincaré,Annales de l’I.H.P. Physique théorique3(1965) 1–12

    1965

  25. [25]

    N. D. S. Gupta,On an analogue of the galilei group,Nuovo Cim. A44(1966) 512–517

    1966

  26. [26]

    G. Odak, A. Rignon-Bret and S. Speziale,General gravitational charges on null hypersurfaces,JHEP12 (2023) 038, [2309.03854]

    Pith/arXiv arXiv 2023

  27. [27]

    Donnay, A

    L. Donnay, A. Fiorucci, Y. Herfray and R. Ruzziconi,Carrollian Perspective on Celestial Holography,Phys. Rev. Lett.129(2022) 071602, [2202.04702]

    Pith/arXiv arXiv 2022

  28. [28]

    Donnay, A

    L. Donnay, A. Fiorucci, Y. Herfray and R. Ruzziconi,Bridging Carrollian and celestial holography,Phys. Rev. D107(2023) 126027, [2212.12553]

    Pith/arXiv arXiv 2023

  29. [29]

    Hu and S

    Y. Hu and S. Pasterski,Detector operators for celestial symmetries,JHEP12(2023) 035, [2307.16801]

    Pith/arXiv arXiv 2023

  30. [30]

    Robinson and A

    I. Robinson and A. Trautman,Some spherical gravitational waves in general relativity,Proc. Roy. Soc. Lond. A265(1962) 463–473

    1962

  31. [31]

    Chrusciel,Semiglobal existence and convergence of solutions of the Robinson-Trautman (two-dimensional Calabi) equation,Commun

    P. Chrusciel,Semiglobal existence and convergence of solutions of the Robinson-Trautman (two-dimensional Calabi) equation,Commun. Math. Phys.137(1991) 289–313

    1991

  32. [32]

    P. T. Chrusciel,On the global structure of Robinson-Trautman space-times,Proc. Roy. Soc. Lond. A436 (1992) 299–316

    1992

  33. [33]

    Bakas and K

    I. Bakas and K. Skenderis,Non-equilibrium dynamics andAdS4 Robinson-Trautman,JHEP08(2014) 056, [1404.4824]

    Pith/arXiv arXiv 2014

  34. [34]

    Bernardi de Freitas and H

    G. Bernardi de Freitas and H. S. Reall,Algebraically special solutions in AdS/CFT,JHEP06(2014) 148, [1403.3537]

    Pith/arXiv arXiv 2014

  35. [35]

    J. Gath, A. Mukhopadhyay, A. C. Petkou, P. M. Petropoulos and K. Siampos,Petrov Classification and holographic reconstruction of spacetime,JHEP09(2015) 005, [1506.04813]

    Pith/arXiv arXiv 2015

  36. [36]

    Bakas, K

    I. Bakas, K. Skenderis and B. Withers,Self-similar equilibration of strongly interacting systems from holography,Phys. Rev. D93(2016) 101902, [1512.09151]. – 71 –

    Pith/arXiv arXiv 2016

  37. [37]

    Ciambelli, A

    L. Ciambelli, A. C. Petkou, P. M. Petropoulos and K. Siampos,The Robinson-Trautman spacetime and its holographic fluid,PoSCORFU2016(2017) 076, [1707.02995]

    Pith/arXiv arXiv 2017

  38. [38]

    Skenderis and B

    K. Skenderis and B. Withers,Robinson-Trautman spacetimes and gauge/gravity duality,PoSCORFU2016 (2017) 097, [1703.10865]

    Pith/arXiv arXiv 2017

  39. [39]

    Arenas-Henriquez, L

    G. Arenas-Henriquez, L. Ciambelli, F. Diaz, W. Jia and D. Rivera-Betancour,Radiation in fluid/gravity and the flat limit,JHEP01(2026) 086, [2508.01446]

    Pith/arXiv arXiv 2026

  40. [40]

    Castro, R

    A. Castro, R. Mancilla and I. Papadimitriou,Near-extremal dynamics away from the horizon,JHEP11 (2025) 083, [2507.01126]

    arXiv 2025

  41. [41]

    Barnich and A

    G. Barnich and A. Seraj,Memory of Robinson-Trautman waves,2604.16703

    Pith/arXiv arXiv

  42. [42]

    Redondo-Yuste and L

    J. Redondo-Yuste and L. Lehner,Non-linear black hole dynamics and Carrollian fluids,JHEP02(2023) 240, [2212.06175]

    Pith/arXiv arXiv 2023

  43. [43]

    Hüsnügil and L

    S. Hüsnügil and L. Lehner,Sourced Carrollian fluids dual to black hole horizons,Phys. Rev. D112(2025) 104043, [2508.20284]

    arXiv 2025

  44. [44]

    Poole, K

    A. Poole, K. Skenderis and M. Taylor,(A)dS4 in Bondi gauge,Class. Quant. Grav.36(2019) 095005, [1812.05369]

    Pith/arXiv arXiv 2019

  45. [45]

    Compère, A

    G. Compère, A. Fiorucci and R. Ruzziconi,TheΛ-BMS4 group of dS4 and new boundary conditions for AdS4, Class. Quant. Grav.36(2019) 195017, [1905.00971]

    Pith/arXiv arXiv 2019

  46. [46]

    Compere, A

    G. Compere, A. Fiorucci and R. Ruzziconi,Theλ-bms4 charge algebra,Journal of High Energy Physics2020 (2020) 1–45

    2020

  47. [47]

    Podolský and R

    J. Podolský and R. Švarc,Algebraic classification of Robinson-Trautman spacetimes,Phys. Rev. D94(2016) 064043, [1608.07118]

    Pith/arXiv arXiv 2016

  48. [48]

    K. P. Tod,Analogue of the past horizon in the robinson-trautman metrics,Classical and Quantum Gravity6 (aug, 1989) 1159

    1989

  49. [49]

    Lukacs, Z

    B. Lukacs, Z. Perjes, A. Sebestyen and J. Porter,Lyapunov functional approach to radiative metrics,General Relativity and Gravitation16(Jun, 1983) 691–701

    1983

  50. [50]

    P. T. Chrusciel and D. B. Singleton,Nonsmoothness of event horizons of Robinson-Trautman black holes, Commun. Math. Phys.147(1992) 137–162

    1992

  51. [51]

    Podolsky and O

    J. Podolsky and O. Svitek,Past horizons in Robinson-Trautman spacetimes with a cosmological constant, Phys. Rev. D80(2009) 124042, [0911.5317]

    Pith/arXiv arXiv 2009

  52. [52]

    E. W. M. Chow and A. W. C. Lun,Apparent horizons in vacuum robinson-trautman spacetimes, 1995

    1995

  53. [53]

    Compère, A

    G. Compère, A. Fiorucci and R. Ruzziconi,Superboost transitions, refraction memory and super-Lorentz charge algebra,JHEP11(2018) 200, [1810.00377]

    Pith/arXiv arXiv 2018

  54. [54]

    Ashtekar and M

    A. Ashtekar and M. Streubel,Symplectic Geometry of Radiative Modes and Conserved Quantities at Null Infinity,Proc. Roy. Soc. Lond. A376(1981) 585–607

    1981

  55. [55]

    Conserved Quantities

    R. M. Wald and A. Zoupas,A General Definition of “Conserved Quantities” in General Relativity and Other Theories of Gravity,Phys. Rev. D61(2000) 084027, [gr-qc/9911095]

    Pith/arXiv arXiv 2000

  56. [56]

    Barnich and C

    G. Barnich and C. Troessaert,BMS charge algebra,JHEP12(2011) 105, [1106.0213]

    Pith/arXiv arXiv 2011

  57. [57]

    Mädler and J

    T. Mädler and J. Winicour,Bondi-Sachs Formalism,Scholarpedia11(2016) 33528, [1609.01731]

    Pith/arXiv arXiv 2016

  58. [58]

    Mädler and J

    T. Mädler and J. Winicour,Radiation Memory, Boosted Schwarzschild Spacetimes and Supertranslations, Class. Quant. Grav.34(2017) 115009, [1701.02556]. – 72 –

    Pith/arXiv arXiv 2017

  59. [59]

    Chen, M.-T

    P.-N. Chen, M.-T. Wang, Y.-K. Wang and S.-T. Yau,BMS Charges Without Supertranslation Ambiguity, Commun. Math. Phys.393(2022) 1411–1449, [2107.05316]

    Pith/arXiv arXiv 2022

  60. [60]

    M. M. Riva, F. Vernizzi and L. K. Wong,Angular momentum balance in gravitational two-body scattering: Flux, memory, and supertranslation invariance,Phys. Rev. D108(2023) 104052, [2302.09065]

    Pith/arXiv arXiv 2023

  61. [61]

    Javadinezhad and M

    R. Javadinezhad and M. Porrati,Three Puzzles with Covariance and Supertranslation Invariance of Angular Momentum Flux and Their Solutions,Phys. Rev. Lett.132(2024) 151604, [2312.02458]

    Pith/arXiv arXiv 2024

  62. [62]

    Mao and B

    P. Mao and B. Zeng,Note on post-Minkowskian expansion and Bondi coordinates,Nucl. Phys. B1019(2025) 117111, [2405.11953]

    arXiv 2025

  63. [63]

    Freidel, R

    L. Freidel, R. Oliveri, D. Pranzetti and S. Speziale,The Weyl BMS group and Einstein’s equations,JHEP07 (2021) 170, [2104.05793]

    Pith/arXiv arXiv 2021

  64. [64]

    E. E. Flanagan and D. A. Nichols,Fully nonlinear transformations of the Weyl-Bondi-Metzner-Sachs asymptotic symmetry group,JHEP03(2024) 120, [2311.03130]

    Pith/arXiv arXiv 2024

  65. [65]

    Foster and E

    J. Foster and E. T. Newman,Note on the robinson-trautman solutions,Journal of Mathematical Physics8 (02, 1967) 189–194

    1967

  66. [66]

    D. B. Singleton,Robinson-Trautman solutions of Einstein’s equations,

  67. [67]

    Stephani, D

    H. Stephani, D. Kramer, M. A. H. MacCallum, C. Hoenselaers and E. Herlt,Exact solutions of Einstein’s field equations. Cambridge Monographs on Mathematical Physics. Cambridge Univ. Press, Cambridge, 2003, 10.1017/CBO9780511535185

    doi:10.1017/cbo9780511535185 2003

  68. [68]

    J. B. Griffiths and J. Podolsky,Exact Space-Times in Einstein’s General Relativity. Cambridge Monographs on Mathematical Physics. Cambridge University Press, Cambridge, 2009, 10.1017/CBO9780511635397

    doi:10.1017/cbo9780511635397 2009

  69. [69]

    É. É. Flanagan and D. A. Nichols,Conserved charges of the extended Bondi-Metzner-Sachs algebra,Phys. Rev. D95(2017) 044002, [1510.03386]

    Pith/arXiv arXiv 2017

  70. [70]

    Compère and A

    G. Compère and A. Fiorucci,Advanced Lectures on General Relativity,1801.07064

    Pith/arXiv arXiv

  71. [71]

    Compère, R

    G. Compère, R. Oliveri and A. Seraj,The Poincaré and BMS flux-balance laws with application to binary systems,JHEP10(2020) 116, [1912.03164]

    Pith/arXiv arXiv 2020

  72. [72]

    Harlow and J.-Q

    D. Harlow and J.-Q. Wu,Covariant phase space with boundaries,JHEP10(2020) 146, [1906.08616]

    Pith/arXiv arXiv 2020

  73. [73]

    Odak and S

    G. Odak and S. Speziale,Brown-York charges with mixed boundary conditions,JHEP11(2021) 224, [2109.02883]

    Pith/arXiv arXiv 2021

  74. [74]

    Freidel, R

    L. Freidel, R. Oliveri, D. Pranzetti and S. Speziale,Extended corner symmetry, charge bracket and Einstein’s equations,JHEP09(2021) 083, [2104.12881]

    Pith/arXiv arXiv 2021

  75. [75]

    G. Odak, A. Rignon-Bret and S. Speziale,Wald-Zoupas prescription with soft anomalies,Phys. Rev. D107 (2023) 084028, [2212.07947]

    Pith/arXiv arXiv 2023

  76. [76]

    Speziale,GGI lectures on boundary and asymptotic symmetries,2512.16810

    S. Speziale,GGI lectures on boundary and asymptotic symmetries,2512.16810

    Pith/arXiv arXiv

  77. [77]

    Strominger,On bms invariance of gravitational scattering,Journal of High Energy Physics2014(2014) 1–20

    A. Strominger,On bms invariance of gravitational scattering,Journal of High Energy Physics2014(2014) 1–20

    2014

  78. [78]

    Kapec, P

    D. Kapec, P. Mitra, A.-M. Raclariu and A. Strominger,2d stress tensor for 4d gravity,Physical Review Letters119(2017) 121601

    2017

  79. [79]

    Donnay, S

    L. Donnay, S. Pasterski and A. Puhm,Goldilocks modes and the three scattering bases,Journal of High Energy Physics2022(2022) 1–50

    2022

  80. [80]

    Himwich and M

    E. Himwich and M. Pate,Light-ray operators and thew1+∞ algebra,arXiv preprint arXiv:2512.18973(2025)

    arXiv 2025

Showing first 80 references.