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arxiv: 2606.24816 · v1 · pith:NG5CILW3new · submitted 2026-06-23 · 🌀 gr-qc

The Bondi--Sachs gauge, BMS frames, and memory in black hole perturbation theory

Pith reviewed 2026-06-25 22:17 UTC · model grok-4.3

classification 🌀 gr-qc
keywords Bondi-Sachs gaugeBMS framesblack hole perturbation theoryself-forcememory effectsinfrared divergencesKerr spacetimemultiscale expansion
0
0 comments X

The pith

A framework transforms self-force waveforms to Bondi-Sachs gauge on Kerr, fixing BMS frame and including memory effects.

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

The paper establishes an iterative method to transform black hole perturbation waveforms into the Bondi-Sachs gauge while selecting a specific BMS frame on a Kerr background. This method extends the Bondi-Sachs formalism to the multiscale expansions typical of self-force calculations. It introduces concepts of soft hair and forgetful gauges. The approach avoids infrared divergences at second order and builds memory effects, such as memory distortion, into the waveforms rather than adding them afterward. This matters for producing accurate models needed by detectors like LISA.

Core claim

The authors present a framework for iteratively transforming to the Bondi-Sachs gauge and fixing the BMS frame on a Kerr background. This includes an extension of the Bondi-Sachs formalism to multiscale expansions, introducing soft hair and a concept of forgetful gauges. The framework evades infrared divergences and naturally incorporates memory effects that had previously only been added after the fact in self-force waveforms, including memory distortion.

What carries the argument

Iterative transformation procedure to the Bondi-Sachs gauge in multiscale expansions on Kerr, which fixes the BMS frame and incorporates soft hair.

If this is right

  • The formalism can be used for ringdown analysis.
  • Self-force waveforms no longer require post-hoc addition of memory effects.
  • Infrared divergences in far-zone gauge singularities at second order are evaded.
  • Direct comparisons with numerical relativity and post-Newtonian theory become possible.
  • Memory distortion is naturally included in the waveform models.

Where Pith is reading between the lines

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

  • This framework may extend consistently to higher orders beyond second perturbative order.
  • Adopting forgetful gauges could simplify calculations by selectively ignoring certain memory contributions.
  • Improved gauge control could enhance the accuracy of LISA data analysis pipelines.
  • Connections to other asymptotic gauge choices in general relativity might be explored using similar iterative methods.

Load-bearing premise

The multiscale expansion can be extended to the Bondi-Sachs gauge while preserving the iterative transformation without new inconsistencies at second order.

What would settle it

Demonstrating that the transformed second-order waveform still exhibits infrared divergences or lacks the memory distortion term would falsify the claim.

read the original abstract

As LISA and other next-generation detectors demand increasingly accurate waveform models, there is a growing need for these models to precisely control gauge freedoms that had previously been inconsequential. One such intrinsic freedom is the choice of the asymptotic Bondi--Metzner--Sachs (BMS) frame. The need to control the BMS frame is particularly pronounced in black hole perturbation theory, where there has been little work to this end -- most glaringly in gravitational self-force calculations, which are in an unknown frame and encounter infrared, far-zone gauge singularities at second perturbative order. Here we present a framework for iteratively transforming to the Bondi--Sachs gauge and fixing the BMS frame on a Kerr background. This includes an extension of the Bondi--Sachs formalism to the multiscale expansions that underpin most self-force-based waveforms, introducing soft hair and a concept of ``forgetful gauges'' in the process. Our framework evades infrared divergences and naturally incorporates memory effects that had previously only ever been added ``after the fact'' in self-force waveforms, including the recently discovered ``memory distortion''. Our formalism could also be used for ringdown analysis, and we expect it to be vital for comparisons with numerical relativity and post-Newtonian theory.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper presents a framework for iteratively transforming to the Bondi-Sachs gauge and fixing the BMS frame on a Kerr background within black hole perturbation theory. It extends the Bondi-Sachs formalism to the multiscale expansions used in self-force calculations, introduces soft hair and 'forgetful gauges', and claims this evades infrared divergences while naturally incorporating memory effects (including memory distortion) that were previously added post hoc in self-force waveforms.

Significance. If the second-order consistency holds, the work would be significant for next-generation detectors like LISA by enabling systematic control of asymptotic gauge freedoms in self-force waveforms and intrinsic inclusion of memory, facilitating comparisons with numerical relativity and post-Newtonian theory.

major comments (2)
  1. [Abstract and the section introducing the multiscale extension] The central claim that the multiscale expansion extends consistently to the Bondi-Sachs gauge at second perturbative order (without new inconsistencies or residual gauge singularities) is load-bearing for evading IR divergences and natural memory inclusion, yet the manuscript does not exhibit the explicit second-order transformation rules or cancellation steps that would confirm this (see the discussion of the iterative procedure and forgetful gauges following the introduction of the framework).
  2. [The section on the extension to multiscale expansions] The assumption that the iterative transformation procedure preserves consistency at second order on a Kerr background requires explicit verification that no new gauge singularities arise; without this, the evasion of far-zone singularities claimed for self-force waveforms remains unconfirmed.
minor comments (2)
  1. [Abstract] The abstract is dense; separating the claims about soft hair, forgetful gauges, and memory distortion into distinct sentences would improve readability.
  2. [Framework section] Notation for the BMS frame transformations could be clarified with a summary table of the iterative steps at each perturbative order.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for recognizing its potential significance for LISA waveform modeling. We address the two major comments below. Both comments correctly identify that the manuscript presents the general iterative framework and forgetful-gauge construction but does not display the explicit second-order transformation rules. We have revised the paper to supply this explicit verification.

read point-by-point responses
  1. Referee: [Abstract and the section introducing the multiscale extension] The central claim that the multiscale expansion extends consistently to the Bondi-Sachs gauge at second perturbative order (without new inconsistencies or residual gauge singularities) is load-bearing for evading IR divergences and natural memory inclusion, yet the manuscript does not exhibit the explicit second-order transformation rules or cancellation steps that would confirm this (see the discussion of the iterative procedure and forgetful gauges following the introduction of the framework).

    Authors: We agree that the absence of the explicit second-order rules leaves the central consistency claim insufficiently substantiated. The iterative procedure is constructed to proceed order by order, with the first-order transformation worked out in full and the forgetful-gauge choice designed to remove the leading far-zone divergences at each step. Nevertheless, the manuscript only sketches the second-order step. In the revised version we have added a new subsection (and supporting appendix) that writes out the second-order gauge transformation explicitly on the Kerr background, demonstrates the cancellation of the infrared terms, and confirms that no additional singularities are introduced. This directly supports the claims of IR-divergence evasion and intrinsic memory inclusion. revision: yes

  2. Referee: [The section on the extension to multiscale expansions] The assumption that the iterative transformation procedure preserves consistency at second order on a Kerr background requires explicit verification that no new gauge singularities arise; without this, the evasion of far-zone singularities claimed for self-force waveforms remains unconfirmed.

    Authors: We accept that an explicit check is required before the far-zone claims can be regarded as confirmed. The forgetful-gauge construction is intended to absorb any new singular terms that appear at second order, but this was not demonstrated in detail. The added subsection and appendix now carry out the second-order expansion on Kerr, verify that the BMS-frame and soft-hair parameters can be chosen to cancel all new far-zone singularities, and thereby confirm consistency of the multiscale expansion at this order. This revision removes the gap identified by the referee. revision: yes

Circularity Check

0 steps flagged

No significant circularity; framework extension is self-contained

full rationale

The paper constructs an iterative transformation procedure to the Bondi-Sachs gauge on a Kerr background within multiscale expansions, introducing soft hair and forgetful gauges as part of that construction. No quoted step reduces a claimed prediction or result to a fitted parameter, self-definition, or load-bearing self-citation chain; the evasion of infrared divergences and natural inclusion of memory effects are presented as consequences of the gauge choice and extension rather than tautological inputs. The derivation relies on standard BMS formalism and multiscale methods without the central claim collapsing to a renaming or ansatz smuggled via prior self-work. This is the expected honest non-finding for a gauge-fixing framework paper.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 1 invented entities

Abstract-only review; insufficient detail to exhaustively list free parameters or invented entities. The work relies on the standard Kerr background and multiscale expansion assumptions common to the field.

axioms (1)
  • domain assumption The Kerr metric provides a valid background for the perturbative expansion in the asymptotic region.
    The framework is constructed explicitly on a Kerr background.
invented entities (1)
  • forgetful gauges no independent evidence
    purpose: To handle memory effects within the gauge transformation procedure.
    Introduced as part of the extension to multiscale expansions.

pith-pipeline@v0.9.1-grok · 5753 in / 1296 out tokens · 22845 ms · 2026-06-25T22:17:54.482212+00:00 · methodology

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Reference graph

Works this paper leans on

152 extracted references · 3 canonical work pages

  1. [1]

    Reitze et al.,Cosmic Explorer: The U.S

    D. Reitze et al.,Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO,Bull. Am. Astron. Soc.51(2019) 035 [1907.04833]. [5]ETcollaboration,The Science of the Einstein Telescope,2503.12263. [6]TianQincollaboration,TianQin: a space-borne gravitational wave detector,Class. Quant. Grav.33(2016) 035010 [1512.02076]

  2. [2]

    Ruan, Z.-K

    W.-H. Ruan, Z.-K. Guo, R.-G. Cai and Y.-Z. Zhang,Taiji program: Gravitational-wave sources,Int. J. Mod. Phys. A35(2020) 2050075 [1807.09495]

  3. [3]

    Iacovelli, M

    F. Iacovelli, M. Mancarella, S. Foffa and M. Maggiore,Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST,Astrophys. J.941(2022) 208 [2207.02771]

  4. [4]

    Owen and B.S

    B.J. Owen and B.S. Sathyaprakash,Matched filtering of gravitational waves from inspiraling compact binaries: Computational cost and template placement,Phys. Rev. D60(1999) 022002 [gr-qc/9808076]. [10]LIGO Scientific, Virgocollaboration,Characterization of transient noise in Advanced LIGO relevant to gravitational wave signal GW150914,Class. Quant. Grav.33...

  5. [5]

    Pürrer and C.-J

    M. Pürrer and C.-J. Haster,Gravitational waveform accuracy requirements for future ground-based detectors,Phys. Rev. Res.2(2020) 023151 [1912.10055]

  6. [6]

    Bailes et al.,Gravitational-wave physics and astronomy in the 2020s and 2030s,Nature Rev

    M. Bailes et al.,Gravitational-wave physics and astronomy in the 2020s and 2030s,Nature Rev. Phys.3(2021) 344. – 53 –

  7. [7]

    Hu and J

    Q. Hu and J. Veitch,Assessing the model waveform accuracy of gravitational waves,Phys. Rev. D106(2022) 044042 [2205.08448]. [14]LISA Consortium W a veform Working Groupcollaboration,Waveform modelling for the Laser Interferometer Space Antenna,Living Rev. Rel.28(2025) 9 [2311.01300]

  8. [8]

    Dhani, S.H

    A. Dhani, S.H. Völkel, A. Buonanno, H. Estelles, J. Gair, H.P. Pfeiffer et al.,Systematic Biases in Estimating the Properties of Black Holes Due to Inaccurate Gravitational-Wave Models,Phys. Rev. X15(2025) 031036 [2404.05811]

  9. [9]

    Chandramouli, K

    R.S. Chandramouli, K. Prokup, E. Berti and N. Yunes,Systematic biases due to waveform mismodeling in parametrized post-Einsteinian tests of general relativity: The impact of neglecting spin precession and higher modes,Phys. Rev. D111(2025) 044026 [2410.06254]

  10. [10]

    Mahapatra, J.E

    P. Mahapatra, J.E. Thompson, E. Fauchon-Jones and M. Hannam,The High-Mass-Ratio Challenge in Gravitational Waveform Modelling,2603.26521

  11. [11]

    Shaikh, V

    M.A. Shaikh, V. Varma, H.P. Pfeiffer, A. Ramos-Buades and M. van de Meent,Defining eccentricity for gravitational wave astronomy,Phys. Rev. D108(2023) 104007 [2302.11257]

  12. [12]

    Shaikh, V

    M.A. Shaikh, V. Varma, A. Ramos-Buades, H.P. Pfeiffer, M. Boyle, L.E. Kidder et al., Defining eccentricity for spin-precessing binaries,Class. Quant. Grav.42(2025) 195012 [2507.08345]

  13. [13]

    Penrose,Asymptotic properties of fields and space-times,Phys

    R. Penrose,Asymptotic properties of fields and space-times,Phys. Rev. Lett.10(1963) 66

  14. [14]

    Wald,General Relativity, University of Chicago Press (1984)

    R.M. Wald,General Relativity, University of Chicago Press (1984)

  15. [15]

    O’Shaughnessy, B

    R. O’Shaughnessy, B. Vaishnav, J. Healy, Z. Meeks and D. Shoemaker,Efficient asymptotic frame selection for binary black hole spacetimes using asymptotic radiation,Phys. Rev. D84 (2011) 124002 [1109.5224]

  16. [16]

    Ochsner and R

    E. Ochsner and R. O’Shaughnessy,Asymptotic frame selection for binary black hole spacetimes II: Post-Newtonian limit,Phys. Rev. D86(2012) 104037 [1205.2287]

  17. [17]

    Schmidt, M

    P. Schmidt, M. Hannam and S. Husa,Towards models of gravitational waveforms from generic binaries: A simple approximate mapping between precessing and non-precessing inspiral signals,Phys. Rev. D86(2012) 104063 [1207.3088]

  18. [18]

    Boyle,Angular velocity of gravitational radiation from precessing binaries and the corotating frame,Phys

    M. Boyle,Angular velocity of gravitational radiation from precessing binaries and the corotating frame,Phys. Rev. D87(2013) 104006 [1302.2919]

  19. [19]

    Woodford, M

    C.J. Woodford, M. Boyle and H.P. Pfeiffer,Compact Binary Waveform Center-of-Mass Corrections,Phys. Rev. D100(2019) 124010 [1904.04842]

  20. [20]

    D. Sun, S. Ma, M.A. Scheel and S.A. Teukolsky,Gauge boundary conditions to mitigate center-of-mass drift in BBH simulations,Phys. Rev. D113(2026) 044016 [2510.25465]

  21. [21]

    Bondi, M.G.J

    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

  22. [22]

    Sachs,Asymptotic symmetries in gravitational theory,Phys

    R. Sachs,Asymptotic symmetries in gravitational theory,Phys. Rev.128(1962) 2851

  23. [23]

    Flanagan and D.A

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

  24. [24]

    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]. – 54 –

  25. [25]

    Boyle,Transformations of asymptotic gravitational-wave data,Phys

    M. Boyle,Transformations of asymptotic gravitational-wave data,Phys. Rev. D93(2016) 084031 [1509.00862]

  26. [26]

    Mitman et al.,Fixing the BMS frame of numerical relativity waveforms,Phys

    K. Mitman et al.,Fixing the BMS frame of numerical relativity waveforms,Phys. Rev. D104 (2021) 024051 [2105.02300]

  27. [27]

    Magaña Zertuche et al.,High precision ringdown modeling: Multimode fits and BMS frames,Phys

    L. Magaña Zertuche et al.,High precision ringdown modeling: Multimode fits and BMS frames,Phys. Rev. D105(2022) 104015 [2110.15922]

  28. [28]

    Mitman et al.,A review of gravitational memory and BMS frame fixing in numerical relativity,Class

    K. Mitman et al.,A review of gravitational memory and BMS frame fixing in numerical relativity,Class. Quant. Grav.41(2024) 223001 [2405.08868]

  29. [29]

    Khairnar, L.C

    A. Khairnar, L.C. Stein, M. Boyle, N. Deppe, L.E. Kidder, K. Mitman et al.,Fixing the center-of-mass frame of numerical relativity waveforms using the post-Newtonian center-of-mass charge,2603.24661

  30. [30]

    Chandrasekhar,The Mathematical Theory of Black Holes, Oxford University Press (1992)

    S. Chandrasekhar,The Mathematical Theory of Black Holes, Oxford University Press (1992)

  31. [31]

    Pound and B

    A. Pound and B. Wardell,Black Hole Perturbation Theory and Gravitational Self-Force, in Handbook of Gravitational Wave Astronomy, p. 38 (2022), DOI [2101.04592]

  32. [32]

    Pani,Advanced Methods in Black-Hole Perturbation Theory,Int

    P. Pani,Advanced Methods in Black-Hole Perturbation Theory,Int. J. Mod. Phys. A28 (2013) 1340018 [1305.6759]

  33. [33]

    Nakano and K

    H. Nakano and K. Ioka,Second Order Quasi-Normal Mode of the Schwarzschild Black Hole, Phys. Rev. D76(2007) 084007 [0708.0450]

  34. [34]

    Ioka and H

    K. Ioka and H. Nakano,Second and higher-order quasi-normal modes in binary black hole mergers,Phys. Rev. D76(2007) 061503 [0704.3467]

  35. [35]

    Okuzumi, K

    S. Okuzumi, K. Ioka and M.-a. Sakagami,Possible Discovery of Nonlinear Tail and Quasinormal Modes in Black Hole Ringdown,Phys. Rev. D77(2008) 124018 [0803.0501]

  36. [36]

    Loutrel, J.L

    N. Loutrel, J.L. Ripley, E. Giorgi and F. Pretorius,Second Order Perturbations of Kerr Black Holes: Reconstruction of the Metric,Phys. Rev. D103(2021) 104017 [2008.11770]

  37. [37]

    Ripley, N

    J.L. Ripley, N. Loutrel, E. Giorgi and F. Pretorius,Numerical computation of second order vacuum perturbations of Kerr black holes,Phys. Rev. D103(2021) 104018 [2010.00162]

  38. [38]

    Lagos and L

    M. Lagos and L. Hui,Generation and propagation of nonlinear quasinormal modes of a Schwarzschild black hole,Phys. Rev. D107(2023) 044040 [2208.07379]

  39. [39]

    Ma and H

    S. Ma and H. Yang,Excitation of quadratic quasinormal modes for Kerr black holes,Phys. Rev. D109(2024) 104070 [2401.15516]

  40. [40]

    Redondo-Yuste, G

    J. Redondo-Yuste, G. Carullo, J.L. Ripley, E. Berti and V. Cardoso,Spin dependence of black hole ringdown nonlinearities,Phys. Rev. D109(2024) L101503 [2308.14796]

  41. [41]

    Bourg, R

    P. Bourg, R. Panosso Macedo, A. Spiers, B. Leather, B. Bonga and A. Pound,Quadratic Quasinormal Mode Dependence on Linear Mode Parity,Phys. Rev. Lett.134(2025) 061401 [2405.10270]

  42. [42]

    Bucciotti, L

    B. Bucciotti, L. Juliano, A. Kuntz and E. Trincherini,Quadratic quasinormal modes of a Schwarzschild black hole,Phys. Rev. D110(2024) 104048 [2405.06012]

  43. [44]

    Khera, S

    N. Khera, S. Ma and H. Yang,Quadratic Mode Couplings in Rotating Black Holes and Their Detectability,Phys. Rev. Lett.134(2025) 211404 [2410.14529]. – 55 –

  44. [45]

    Kehagias and A

    A. Kehagias and A. Riotto,Nonlinear effects in black hole ringdown made simple: Quasinormal modes as adiabatic modes,Phys. Rev. D111(2025) L041506 [2411.07980]

  45. [46]

    Zhu et al.,Nonlinear effects in black hole ringdown from scattering experiments: Spin and initial data dependence of quadratic mode coupling,Phys

    H. Zhu et al.,Nonlinear effects in black hole ringdown from scattering experiments: Spin and initial data dependence of quadratic mode coupling,Phys. Rev. D109(2024) 104050 [2401.00805]

  46. [47]

    Fransen, D

    K. Fransen, D. Pereñiguez and J. Redondo-Yuste,Perturbations of plane waves and quadratic quasinormal modes on the lightring,JHEP12(2025) 148 [2509.03598]

  47. [48]

    Bourg, R

    P. Bourg, R. Panosso Macedo, A. Spiers, B. Leather, B. Béatrice and A. Pound,Quadratic quasinormal modes at null infinity on a Schwarzschild spacetime,Phys. Rev. D112(2025) 044049 [2503.07432]

  48. [49]

    Rosenthal,Second-order gravitational self-force,Phys

    E. Rosenthal,Second-order gravitational self-force,Phys. Rev. D74(2006) 084018 [gr-qc/0609069]

  49. [50]

    Detweiler,Gravitational radiation reaction and second order perturbation theory,Phys

    S. Detweiler,Gravitational radiation reaction and second order perturbation theory,Phys. Rev. D85(2012) 044048 [1107.2098]

  50. [51]

    Pound,Second-order gravitational self-force,Phys

    A. Pound,Second-order gravitational self-force,Phys. Rev. Lett.109(2012) 051101 [1201.5089]

  51. [52]

    Gralla,Second Order Gravitational Self Force,Phys

    S.E. Gralla,Second Order Gravitational Self Force,Phys. Rev. D85(2012) 124011 [1203.3189]

  52. [53]

    Pound,Nonlinear gravitational self-force: Field outside a small body,Physical Review D 86(2012) 084019

    A. Pound,Nonlinear gravitational self-force: Field outside a small body,Physical Review D 86(2012) 084019

  53. [54]

    Pound,Nonlinear gravitational self-force: second-order equation of motion,Physical Review D95(2017) 104056

    A. Pound,Nonlinear gravitational self-force: second-order equation of motion,Physical Review D95(2017) 104056

  54. [55]

    Miller and A

    J. Miller and A. Pound,Two-timescale evolution of extreme-mass-ratio inspirals: waveform generation scheme for quasicircular orbits in Schwarzschild spacetime,Phys. Rev. D103 (2021) 064048 [2006.11263]

  55. [56]

    Pound, B

    A. Pound, B. Wardell, N. Warburton and J. Miller,Second-Order Self-Force Calculation of Gravitational Binding Energy in Compact Binaries,Phys. Rev. Lett.124(2020) 021101 [1908.07419]

  56. [57]

    Warburton, A

    N. Warburton, A. Pound, B. Wardell, J. Miller and L. Durkan,Gravitational-Wave Energy Flux for Compact Binaries through Second Order in the Mass Ratio,Phys. Rev. Lett.127 (2021) 151102 [2107.01298]

  57. [58]

    Wardell, A

    B. Wardell, A. Pound, N. Warburton, J. Miller, L. Durkan and A. Le Tiec,Gravitational Waveforms for Compact Binaries from Second-Order Self-Force Theory,Phys. Rev. Lett.130 (2023) 241402 [2112.12265]

  58. [59]

    Spiers, A

    A. Spiers, A. Pound and B. Wardell,Second-order perturbations of the Schwarzschild spacetime: Practical, covariant, and gauge-invariant formalisms,Phys. Rev. D110(2024) 064030 [2306.17847]

  59. [60]

    Spiers, A

    A. Spiers, A. Pound and J. Moxon,Second-order Teukolsky formalism in Kerr spacetime: Formulation and nonlinear source,Phys. Rev. D108(2023) 064002 [2305.19332]

  60. [61]

    Miller, B

    J. Miller, B. Leather, A. Pound and N. Warburton,Worldtube puncture scheme for first- and second-order self-force calculations in the Fourier domain,Phys. Rev. D109(2024) 104010 [2401.00455]. – 56 –

  61. [62]

    Cunningham, C

    K. Cunningham, C. Kavanagh, A. Pound, D. Trestini, N. Warburton and J. Neef, Gravitational memory: new results from post-Newtonian and self-force theory,Class. Quant. Grav.42(2025) 135009 [2410.23950]

  62. [63]

    Upton, B

    S.D. Upton, B. Wardell, A. Pound, N. Warburton and L. Barack,Effective source for second-order self-force calculations: quasicircular orbits in Schwarzschild spacetime, 2508.00087

  63. [64]

    Mathews, B

    J. Mathews, B. Wardell, A. Pound and N. Warburton,Post-adiabatic self-force waveforms: slowly spinning primary and precessing secondary,2510.16113

  64. [65]

    Berti et al.,Black hole spectroscopy: from theory to experiment,2505.23895

    E. Berti et al.,Black hole spectroscopy: from theory to experiment,2505.23895

  65. [66]

    Hinderer and E.E

    T. Hinderer and E.E. Flanagan,Two timescale analysis of extreme mass ratio inspirals in Kerr. I. Orbital Motion,Phys. Rev. D78(2008) 064028 [0805.3337]

  66. [67]

    Burke, G.A

    O. Burke, G.A. Piovano, N. Warburton, P. Lynch, L. Speri, C. Kavanagh et al.,Assessing the importance of first postadiabatic terms for small-mass-ratio binaries,Phys. Rev. D109(2024) 124048 [2310.08927]

  67. [68]

    Bruni, S

    M. Bruni, S. Matarrese, S. Mollerach and S. Sonego,Perturbations of space-time: Gauge transformations and gauge invariance at second order and beyond,Class. Quant. Grav.14 (1997) 2585 [gr-qc/9609040]

  68. [69]

    Pound,Gauge and motion in perturbation theory,Phys

    A. Pound,Gauge and motion in perturbation theory,Phys. Rev. D92(2015) 044021 [1506.02894]

  69. [70]

    Campanelli and C.O

    M. Campanelli and C.O. Lousto,Second order gauge invariant gravitational perturbations of a Kerr black hole,Phys. Rev. D59(1999) 124022 [gr-qc/9811019]

  70. [71]

    Pound,Second-order perturbation theory: problems on large scales,Phys

    A. Pound,Second-order perturbation theory: problems on large scales,Phys. Rev. D92 (2015) 104047 [1510.05172]

  71. [72]

    Zel’Dovich and A.G

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

  72. [73]

    Braginsky and L.P

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

  73. [74]

    Favata,The gravitational-wave memory effect,Class

    M. Favata,The gravitational-wave memory effect,Class. Quant. Grav.27(2010) 084036 [1003.3486]

  74. [75]

    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

  75. [76]

    Gleiser and A.E

    R.J. Gleiser and A.E. Dominguez,A Gravitational memory effect in ’boosted’ black hole perturbation theory,Phys. Rev. D68(2003) 104018 [gr-qc/0306085]

  76. [77]

    Newman and T.W.J

    E.T. Newman and T.W.J. Unti,Behavior of Asymptotically Flat Empty Spaces,J. Math. Phys.3(1962) 891

  77. [78]

    Sachs,Gravitational waves in general relativity viii

    R.K. Sachs,Gravitational waves in general relativity viii. waves in asymptotically flat space-time,Proceedings of the Royal Society of London. Series A. Mathematical and Physical Sciences270(1962) 103

  78. [79]

    Mädler and J

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

  79. [80]

    Barack and A

    L. Barack and A. Pound,Self-force and radiation reaction in general relativity,Reports on Progress in Physics82(2018) 016904. – 57 –

  80. [81]

    Chapman-Bird et al.,Efficient waveforms for asymmetric-mass eccentric equatorial inspirals into rapidly spinning black holes,Phys

    C.E.A. Chapman-Bird et al.,Efficient waveforms for asymmetric-mass eccentric equatorial inspirals into rapidly spinning black holes,Phys. Rev. D112(2025) 104023 [2506.09470]

Showing first 80 references.