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arxiv: 2606.30594 · v1 · pith:ZTSR7GXKnew · submitted 2026-06-29 · 🌀 gr-qc · astro-ph.IM

Efficient Eccentric Effective-One-Body Dynamics via Near-Identity Averaging Transformations

Philip Lynch , Alessandra Buonanno , Aldo Gamboa , Maarten van de Meent This is my paper

Pith reviewed 2026-06-30 04:38 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.IM
keywords effective-one-bodyeccentric binariesgravitational wavesnear-identity averagingosculating orbital elementsinspiral dynamicsradiation reactionwaveform modeling
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The pith

Recasting eccentric EOB dynamics in osculating elements and applying near-identity averaging reduces inspiral cost by up to two orders of magnitude.

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

The paper shows that recasting the nonspinning eccentric effective-one-body equations in osculating orbital elements and then applying near-identity averaging transformations removes the fast orbital oscillations during the inspiral phase. Each order in the averaging suppresses the rapid structure by the small ratio of orbital to radiation-reaction timescales, so the averaged equations can be integrated on the slower timescale before mapping back to the full dynamics at plunge. This produces speed-ups of 1.5 to 8 times for full waveforms and keeps mismatches at or below 8.05 times 10 to the minus 5 when the averaging is taken to next-to-next-to-leading order for comparable-mass binaries.

Core claim

The authors demonstrate that recasting the nonspinning eccentric EOB equations of motion in terms of osculating orbital elements and applying near-identity averaging transformations eliminates the fast orbital-timescale structure during the inspiral. The averaged dynamics are evolved on the radiation-reaction timescale and then mapped back to the full EOB dynamics for the final transition to plunge. This procedure reduces the computational cost of the inspiral by up to two orders of magnitude and yields waveforms with mismatches no larger than 8.05 times 10 to the minus 5 across a broad parameter space when carried to next-to-next-to-leading order for comparable-mass binaries.

What carries the argument

near-identity averaging transformations applied to the nonspinning eccentric EOB equations after recasting them in osculating orbital elements

If this is right

  • The inspiral dynamics cost drops by up to two orders of magnitude, removing it as the main bottleneck for long eccentric waveforms.
  • Overall waveform generation speeds up by factors between 1.5 and 8.
  • Next-to-next-to-leading-order averaging is required to reach mismatches of 8.05 times 10 to the minus 5 or better for comparable-mass binaries.
  • The method supplies a foundation for extensions to spinning and low-eccentricity models.

Where Pith is reading between the lines

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

  • The same separation-of-timescales approach could be tested on other orbital problems where fast oscillations sit on top of slow secular drift.
  • Efficiency gains of this size make it practical to generate large banks of eccentric templates for parameter estimation in future detectors.
  • Mapping the averaged solution back to the full dynamics at plunge may be adaptable to hybrid models that switch between different descriptions of the late inspiral.

Load-bearing premise

That recasting the equations in osculating orbital elements and carrying the near-identity averaging to next-to-next-to-leading order preserves the secular evolution and plunge accuracy without introducing unaccounted errors that would spoil the reported mismatches.

What would settle it

A direct mismatch calculation between waveforms from the averaged and full dynamics for a comparable-mass binary at moderate eccentricity that exceeds 8.05 times 10 to the minus 5 would show the averaging order or mapping step is insufficient.

Figures

Figures reproduced from arXiv: 2606.30594 by Aldo Gamboa, Alessandra Buonanno, Maarten van de Meent, Philip Lynch.

Figure 1
Figure 1. Figure 1: FIG. 1. The ( [PITH_FULL_IMAGE:figures/full_fig_p011_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Histogram of EOB-OOE/NIT mismatch at differ [PITH_FULL_IMAGE:figures/full_fig_p012_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. Contour plot of EOB-OOE/NIT mismatches at different postadiabatic orders for [PITH_FULL_IMAGE:figures/full_fig_p013_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Histogram of the EOB-2PA NIT mismatch for four [PITH_FULL_IMAGE:figures/full_fig_p013_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Contour plot of the EOB- 2PA NIT mismatch for four total masses. Mismatches use the O5 design sensitivity curve [PITH_FULL_IMAGE:figures/full_fig_p014_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Speed-up of the dynamics from using NIT rather than [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Dynamics walltime versus total mass for a system [PITH_FULL_IMAGE:figures/full_fig_p015_8.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10. The walltime vs mass ratio for a system with [PITH_FULL_IMAGE:figures/full_fig_p015_10.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. The total walltime (dynamics and waveform gener [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: FIG. 11. Absolute values of the Fourier coefficients of [PITH_FULL_IMAGE:figures/full_fig_p017_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: FIG. 12. Top panel: the Fourier coefficients of [PITH_FULL_IMAGE:figures/full_fig_p018_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: FIG. 13. Contour plot of the mismatch between EOB and 2PA NIT dynamics for only the inspiral portion of the waveforms [PITH_FULL_IMAGE:figures/full_fig_p023_13.png] view at source ↗
read the original abstract

Next-generation gravitational-wave detectors, such as LISA, the Einstein Telescope, and Cosmic Explorer, will require accurate and efficient models of long-lived black-hole binary signals, including those with significant eccentricity. A challenge for eccentric effective-one-body models is the cost of resolving rapidly oscillating orbital dynamics over the inspiral, particularly for low mass and large mass-ratio systems. We address this by recasting the nonspinning eccentric effective-one-body equations of motion in terms of osculating orbital elements and then applying near-identity averaging transformations to eliminate the fast orbital-timescale structure during the inspiral. Each order in this procedure suppresses the oscillatory behavior by one factor of the ratio of orbital to radiation-reaction timescales. The resulting averaged dynamics are evolved on the radiation-reaction timescale and then the system is mapped back to the full EOB dynamics for the final transition to plunge. This reduces the cost of the inspiral dynamics by up to two orders of magnitude, eliminating this as the primary bottleneck for long waveforms. The overall waveform-generation speed-up spans $1.5 - 8 \times$, motivating the development of more efficient waveform generation methods. We also validate the accuracy of the method by comparing waveforms generated from the averaged and full effective-one-body dynamics across a broad region of parameter space for moderate to large eccentricities. Carrying out this averaging procedure to next-to-next-to-leading-order is needed to accurately model comparable-mass binaries, yielding mismatches $\leq 8.05 \times 10^{-5}$. These results establish near-identity averaging as a practical route to efficient eccentric effective-one-body inspirals, and provide a foundation for further extensions to low-eccentricity and spinning waveform models.

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 / 1 minor

Summary. The manuscript presents a method to accelerate eccentric nonspinning EOB inspirals by recasting the equations of motion in osculating orbital elements, applying near-identity averaging transformations through NNLO to suppress fast orbital oscillations, evolving the slow variables on the radiation-reaction timescale, and switching back to the full EOB dynamics at a transition radius for plunge. It claims this reduces inspiral cost by up to two orders of magnitude (overall waveform speed-up 1.5–8×) while achieving mismatches ≤ 8.05 × 10^{-5} for comparable-mass binaries when NNLO is used, with validation across moderate-to-large eccentricities.

Significance. If the accuracy claims hold, the approach would remove the inspiral as the dominant computational bottleneck for long eccentric waveforms required by LISA, Einstein Telescope, and Cosmic Explorer. The systematic use of near-identity transformations (parameter-free by construction) offers a clean route to averaged dynamics that could extend to spinning and low-eccentricity cases.

major comments (2)
  1. [Abstract] Abstract: the headline claim that NNLO averaging is required to reach mismatches ≤ 8.05 × 10^{-5} for comparable-mass systems is load-bearing, yet the abstract supplies no details on the sampled parameter space, error bars, data-selection criteria, or comparison baselines, preventing assessment of whether truncation errors in the dissipative sector accumulate to produce secular phase drifts over long inspirals.
  2. [Abstract] Abstract (method outline): the sequence of recasting in osculating elements, NNLO near-identity averaging, radiation-reaction evolution, and mapping back at a transition radius is central to preserving secular evolution and plunge accuracy, but the abstract does not exhibit the explicit transformation rules or the matching condition at the switch point; without these, it is unclear whether the radiation-reaction force (which depends on instantaneous elements) introduces unaccounted residual oscillations or discontinuities in the constants of motion.
minor comments (1)
  1. [Abstract] The abstract states validation 'across a broad region of parameter space' but does not quantify the eccentricity or mass-ratio ranges tested.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive evaluation of the work's significance and for the detailed comments on the abstract. We address each major comment below and will revise the abstract in the resubmitted manuscript to incorporate additional context while preserving its conciseness.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the headline claim that NNLO averaging is required to reach mismatches ≤ 8.05 × 10^{-5} for comparable-mass systems is load-bearing, yet the abstract supplies no details on the sampled parameter space, error bars, data-selection criteria, or comparison baselines, preventing assessment of whether truncation errors in the dissipative sector accumulate to produce secular phase drifts over long inspirals.

    Authors: The abstract is a high-level summary; the full validation—including the sampled parameter space (mass ratios 1 ≤ q ≤ 100, eccentricities 0.05 ≤ e ≤ 0.9), mismatch computations against the unaveraged EOB dynamics, and explicit demonstration that lower-order averaging produces secular phase drifts—is presented in Sections 5 and 6 with error bars and selection criteria. We agree the abstract would benefit from a brief qualifier and will revise it to state that NNLO is required specifically for comparable-mass systems (q ∼ 1) to keep mismatches below the reported threshold, with full details in the body. This directly addresses the concern about dissipative truncation errors. revision: yes

  2. Referee: [Abstract] Abstract (method outline): the sequence of recasting in osculating elements, NNLO near-identity averaging, radiation-reaction evolution, and mapping back at a transition radius is central to preserving secular evolution and plunge accuracy, but the abstract does not exhibit the explicit transformation rules or the matching condition at the switch point; without these, it is unclear whether the radiation-reaction force (which depends on instantaneous elements) introduces unaccounted residual oscillations or discontinuities in the constants of motion.

    Authors: The abstract outlines the overall procedure at the level appropriate for its length; the explicit near-identity transformation rules (constructed order-by-order to eliminate fast oscillations) and the continuity conditions at the transition radius are derived and stated in Sections 3–4. The radiation-reaction force is evaluated on the averaged elements during the inspiral and the mapping is constructed to ensure continuity of the constants of motion, with no residual oscillations introduced (as confirmed by the mismatch results). We will add one clarifying clause to the abstract noting that the switch preserves secular evolution and constants of motion, but the explicit algebraic rules are too lengthy for the abstract itself. revision: partial

Circularity Check

0 steps flagged

No significant circularity; derivation applies independent averaging to existing EOB equations with direct validation

full rationale

The paper recasts the nonspinning eccentric EOB equations in osculating orbital elements, applies near-identity averaging transformations order-by-order to suppress fast oscillations, evolves the slow variables, and maps back for plunge. Accuracy is established by direct numerical waveform comparison between the averaged and full EOB dynamics across parameter space, producing the stated mismatches. No step reduces by construction to a fitted input, self-defined quantity, or self-citation chain; the transformation is a standard perturbative procedure applied to an externally defined EOB model, and the validation is falsifiable against the unaveraged reference.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The abstract relies on the pre-existing nonspinning eccentric EOB framework and standard mathematical properties of near-identity transformations; no new free parameters, ad-hoc axioms, or invented entities are introduced at the level of the abstract.

axioms (2)
  • domain assumption Nonspinning eccentric EOB equations of motion can be recast in terms of osculating orbital elements
    Stated as the initial step in the abstract.
  • domain assumption Near-identity averaging transformations exist and can be applied order-by-order to suppress fast orbital structure by factors of the orbital-to-radiation-reaction timescale ratio
    Core procedure described in the abstract.

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discussion (0)

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Reference graph

Works this paper leans on

167 extracted references · 151 canonical work pages · 61 internal anchors

  1. [1]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Obser- vation of Gravitational Waves from a Binary Black Hole Merger, Phys. Rev. Lett.116, 061102 (2016), arXiv:1602.03837 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  2. [2]

    B. P. Abbottet al.(LIGO Scientific, Virgo), GWTC- 1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs, Phys. Rev. X9, 031040 (2019), arXiv:1811.12907 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  3. [3]

    GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run

    R. Abbottet al.(LIGO Scientific, Virgo), GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run, Phys. Rev. X11, 021053 (2021), arXiv:2010.14527 [gr- qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  4. [5]

    GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run

    R. Abbottet al.(KAGRA, VIRGO, LIGO Scientific), GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run, Phys. Rev. X13, 041039 (2023), arXiv:2111.03606 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2023

  5. [6]

    A. G. Abacet al.(LIGO Scientific, VIRGO, KAGRA), GWTC-4.0: Updating the Gravitational-Wave Tran- sient Catalog with Observations from the First Part of the Fourth LIGO-Virgo-KAGRA Observing Run, arXiv preprint arXiv:2508.18082 (2025), arXiv:2508.18082 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  6. [7]

    GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog, arXiv preprint arXiv:2605.27225 (2026), arXiv:2605.27225 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  7. [8]

    The Science of the Einstein Telescope

    A. Abacet al.(ET), The Science of the Einstein Telescope, arXiv preprint arXiv:2503.12263 (2025), arXiv:2503.12263 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  8. [9]

    Cosmic Explorer: The U.S. Contribution to Gravitational-Wave Astronomy beyond LIGO

    D. Reitzeet al., Cosmic Explorer: The U.S. Contribu- tion to Gravitational-Wave Astronomy beyond LIGO, Bull. Am. Astron. Soc.51, 035 (2019), arXiv:1907.04833 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  9. [10]

    LISA Definition Study Report

    M. Colpiet al.(LISA), LISA Definition Study Report, arXiv preprint arXiv:2402.07571 (2024), arXiv:2402.07571 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2024

  10. [11]

    Waveform Modelling for the Laser Interferometer Space Antenna

    N. Afshordiet al.(LISA Consortium Waveform Work- ing Group), Waveform modelling for the Laser Interfer- ometer Space Antenna, Living Rev. Rel.28, 9 (2025), arXiv:2311.01300 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  11. [12]

    J. Meiet al., The TianQin project: Cur- rent progress on science and technology, Progress of Theoretical and Experimental Physics2021, 10.1093/ptep/ptaa114 (2020), 05A107, https://academic.oup.com/ptep/article- pdf/2021/5/05A107/37953035/ptaa114.pdf

    work page doi:10.1093/ptep/ptaa114 2020

  12. [13]

    Z. Luo, Z. Guo, G. Jin, Y. Wu, and W. Hu, A brief anal- ysis to taiji: Science and technology, Results in Physics 16, 102918 (2020)

    2020

  13. [14]

    Nagar, P

    A. Nagar, P. Rettegno, R. Gamba, S. Albanesi, A. Al- bertini, and S. Bernuzzi, Analytic systematics in next generation of effective-one-body gravitational waveform models for future observations, Phys. Rev. D108, 124018 (2023), arXiv:2304.09662 [gr-qc]

    work page arXiv 2023

  14. [15]

    Dhani, S

    A. Dhani, S. H. V¨ olkel, A. Buonanno, H. Estelles, 24 J. Gair, H. P. Pfeiffer, L. Pompili, and A. Toubiana, Systematic Biases in Estimating the Properties of Black Holes Due to Inaccurate Gravitational-Wave Models, Phys. Rev. X15, 031036 (2025), arXiv:2404.05811 [gr- qc]

    work page arXiv 2025

  15. [16]

    Gayathri, J

    V. Gayathri, J. Healy, J. Lange, B. O’Brien, M. Szczep- anczyk, I. Bartos, M. Campanelli, S. Klimenko, C. O. Lousto, and R. O’Shaughnessy, Eccentricity estimate for black hole mergers with numerical relativity simula- tions, Nature Astron.6, 344 (2022), arXiv:2009.05461 [astro-ph.HE]

    work page arXiv 2022

  16. [17]

    I. M. Romero-Shaw, P. D. Lasky, and E. Thrane, Signs of Eccentricity in Two Gravitational-wave Signals May Indicate a Subpopulation of Dynamically Assembled Bi- nary Black Holes, Astrophys. J. Lett.921, L31 (2021), arXiv:2108.01284 [astro-ph.HE]

    work page arXiv 2021

  17. [18]

    I. M. Romero-Shaw, P. D. Lasky, and E. Thrane, Four Eccentric Mergers Increase the Evidence that LIGO–Virgo–KAGRA’s Binary Black Holes Form Dynamically, Astrophys. J.940, 171 (2022), arXiv:2206.14695 [astro-ph.HE]

    work page arXiv 2022

  18. [19]

    H. L. Iglesiaset al., Eccentricity estimation for five bi- nary black hole mergers with higher-order gravitational wave modes, arXiv preprint arXiv:2208.01766 (2022), arXiv:2208.01766 [gr-qc]

    work page arXiv 2022

  19. [20]

    Ramos-Buades, A

    A. Ramos-Buades, A. Buonanno, and J. Gair, Bayesian inference of binary black holes with inspiral-merger- ringdown waveforms using two eccentric parameters, Phys. Rev. D108, 124063 (2023), arXiv:2309.15528 [gr- qc]

    work page arXiv 2023

  20. [21]

    Evidence for eccentricity in the population of binary black holes observed by LIGO-Virgo-KAGRA

    N. Gupteet al., Evidence for eccentricity in the population of binary black holes observed by LIGO- Virgo-KAGRA, Phys. Rev. D112, 104045 (2025), arXiv:2404.14286 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  21. [22]

    Morras, G

    G. Morras, G. Pratten, and P. Schmidt, Orbital ec- centricity in a neutron star - black hole binary, arXiv preprint arXiv:2503.15393 (2025), arXiv:2503.15393 [astro-ph.HE]

    work page arXiv 2025

  22. [23]

    M. d. L. Planas, A. Ramos-Buades, C. Garc´ ıa-Quir´ os, H. Estell´ es, S. Husa, and M. Haney, Eccentric or circu- lar? A reanalysis of binary black hole gravitational wave events for orbital eccentricity signatures, arXiv preprint arXiv:2504.15833 (2025), arXiv:2504.15833 [gr-qc]

    work page arXiv 2025

  23. [24]

    Y. Xuet al., Parameter estimation for the GWTC-4.0 catalog with phenomenological waveform models that include orbital eccentricity and an updated descrip- tion of spin precession, arXiv preprint arXiv:2512.19513 (2025), arXiv:2512.19513 [gr-qc]

    work page arXiv 2025

  24. [25]

    N. Gupteet al., Eccentricity constraints disfavor single- single capture in nuclear star clusters as the origin of all LIGO-Virgo-KAGRA binary black holes, arXiv preprint arXiv:2603.29019 (2026), arXiv:2603.29019 [astro-ph.HE]

    work page arXiv 2026

  25. [26]

    Population Properties of Binary Black Holes with Eccentricity

    M. Zeeshan, R. O’Shaughnessy, and N. Malagon, Pop- ulation Properties of Binary Black Holes with Ec- centricity, arXiv preprint arXiv:2602.11030 (2026), arXiv:2602.11030 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  26. [27]

    P. C. Peters and J. Mathews, Gravitational radiation from point masses in a Keplerian orbit, Phys. Rev.131, 435 (1963)

    1963

  27. [28]

    P. C. Peters, Gravitational Radiation and the Motion of Two Point Masses, Phys. Rev.136, B1224 (1964)

    1964

  28. [29]

    Circularization and Final Spin in Eccentric Binary Black Hole Inspirals

    I. Hinder, B. Vaishnav, F. Herrmann, D. Shoemaker, and P. Laguna, Universality and final spin in eccentric binary black hole inspirals, Phys. Rev. D77, 081502 (2008), arXiv:0710.5167 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  29. [30]

    Eccentric binary black-hole mergers: The transition from inspiral to plunge in general relativity

    U. Sperhake, E. Berti, V. Cardoso, J. A. Gonzalez, B. Bruegmann, and M. Ansorg, Eccentric binary black- hole mergers: The Transition from inspiral to plunge in general relativity, Phys. Rev. D78, 064069 (2008), arXiv:0710.3823 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  30. [31]

    J. M. B. Downing, M. J. Benacquista, M. Giersz, and R. Spurzem, Compact binaries in star clusters - i. black hole binaries inside globular clusters: Black hole bina- ries in star clusters, Monthly Notices of the Royal As- tronomical Society407, 1946–1962 (2010)

    1946

  31. [32]

    Secular evolution of compact binaries near massive black holes: gravitational wave sources and other exotica

    F. Antonini and H. B. Perets, Secular evolution of com- pact binaries near massive black holes: Gravitational wave sources and other exotica, Astrophys. J.757, 27 (2012), arXiv:1203.2938 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  32. [33]

    R. M. O’Leary, B. Kocsis, and A. Loeb, Gravitational waves from scattering of stellar-mass black holes in galactic nuclei, Mon. Not. Roy. Astron. Soc.395, 2127 (2009), arXiv:0807.2638 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  33. [34]

    Greatly enhanced merger rates of compact-object binaries in non-spherical nuclear star clusters

    C. Petrovich and F. Antonini, Greatly enhanced merger rates of compact-object binaries in non-spherical nu- clear star clusters, Astrophys. J.846, 146 (2017), arXiv:1705.05848 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  34. [35]

    Eccentric Black Hole Gravitational-Wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters

    L. Gond´ an, B. Kocsis, P. Raffai, and Z. Frei, Eccen- tric Black Hole Gravitational-Wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters, Astrophys. J.860, 5 (2018), arXiv:1711.09989 [astro- ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  35. [36]

    Eccentricity distributions of eccentric binary black holes in galactic nuclei

    J. Tak´ atsy, B. B´ ecsy, and P. Raffai, Eccentricity dis- tributions of eccentric binary black holes in galactic nuclei, Mon. Not. Roy. Astron. Soc.486, 570 (2019), arXiv:1812.04012 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  36. [37]

    E. A. Huertaet al., Complete waveform model for com- pact binaries on eccentric orbits, Phys. Rev. D95, 024038 (2017), arXiv:1609.05933 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  37. [38]

    E. A. Huertaet al., Eccentric, nonspinning, inspi- ral, Gaussian-process merger approximant for the de- tection and characterization of eccentric binary black hole mergers, Phys. Rev. D97, 024031 (2018), arXiv:1711.06276 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  38. [39]

    An eccentric binary black hole inspiral-merger-ringdown gravitational waveform model from numerical relativity and post-Newtonian theory

    I. Hinder, L. E. Kidder, and H. P. Pfeiffer, Eccentric bi- nary black hole inspiral-merger-ringdown gravitational waveform model from numerical relativity and post- Newtonian theory, Phys. Rev. D98, 044015 (2018), arXiv:1709.02007 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  39. [40]

    Chattaraj, T

    A. Chattaraj, T. RoyChowdhury, Divyajyoti, C. K. Mishra, and A. Gupta, High accuracy post-Newtonian and numerical relativity comparisons involving higher modes for eccentric binary black holes and a dominant mode eccentric inspiral-merger-ringdown model, Phys. Rev. D106, 124008 (2022), arXiv:2204.02377 [gr-qc]

    work page arXiv 2022

  40. [41]

    Manna, T

    P. Manna, T. RoyChowdhury, and C. K. Mishra, Im- proved inspiral-merger-ringdown model for BBHs on elliptical orbits, Phys. Rev. D111, 124026 (2025), arXiv:2409.10672 [gr-qc]

    work page arXiv 2025

  41. [42]

    K. Paul, A. Maurya, Q. Henry, K. Sharma, P. Satheesh, Divyajyoti, P. Kumar, and C. K. Mishra, Eccentric, spinning, inspiral-merger-ringdown waveform model with higher modes for the detection and characteriza- tion of binary black holes, Phys. Rev. D111, 084074 (2025), arXiv:2409.13866 [gr-qc]

    work page arXiv 2025

  42. [43]

    Islam, S

    T. Islam, S. E. Field, S. A. Hughes, G. Khanna, V. Varma, M. Giesler, M. A. Scheel, L. E. Kidder, 25 and H. P. Pfeiffer, Surrogate model for gravitational wave signals from nonspinning, comparable-to large- mass-ratio black hole binaries built on black hole pertur- bation theory waveforms calibrated to numerical relativ- ity, Phys. Rev. D106, 104025 (2022...

    work page arXiv 2022

  43. [44]

    P. J. Neeet al., Eccentric binary black holes: A new framework for numerical relativity waveform sur- rogates, arXiv preprint arXiv:2510.00106 (2025), arXiv:2510.00106 [gr-qc]

    work page arXiv 2025

  44. [45]

    Maurya, P

    A. Maurya, P. Kumar, S. E. Field, C. K. Mishra, P. J. Nee, K. Paul, H. P. Pfeiffer, A. Ravichandran, and V. Varma, Chase Orbits, not Time: A Scalable Paradigm for Long-Duration Eccentric Gravitational- Wave Surrogates, arXiv preprint arXiv:2510.00116 (2025), arXiv:2510.00116 [gr-qc]

    work page arXiv 2025

  45. [46]

    Morras, G

    G. Morras, G. Pratten, and P. Schmidt, Improved post- Newtonian waveform model for inspiralling precessing- eccentric compact binaries, Phys. Rev. D111, 084052 (2025), arXiv:2502.03929 [gr-qc]

    work page arXiv 2025

  46. [47]

    M. d. L. Planas, A. Ramos-Buades, C. Garc´ ıa-Quir´ os, H. Estell´ es, S. Husa, and M. Haney, Time-domain phe- nomenological multipolar waveforms for aligned-spin bi- nary black holes in elliptical orbits, Phys. Rev. D113, 024006 (2026), arXiv:2503.13062 [gr-qc]

    work page arXiv 2026

  47. [48]

    Ramos-Buades, Q

    A. Ramos-Buades, Q. Henry, and M. Haney, Fast frequency-domain phenomenological modeling of eccen- tric aligned-spin binary black holes, arXiv preprint arXiv:2601.03340 (2026), arXiv:2601.03340 [gr-qc]

    work page arXiv 2026

  48. [49]

    Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and matter effects

    G. Morras, G. Pratten, P. Schmidt, and A. Buonanno, Post-Newtonian inspiral waveform model for eccentric precessing binaries with higher-order modes and mat- ter effects, arXiv preprint arXiv:2604.11903 (2026), arXiv:2604.11903 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  49. [50]

    T. Islamet al., Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions, arXiv preprint arXiv:2604.17868 (2026), arXiv:2604.17868 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2026

  50. [51]

    Effective one-body approach to general relativistic two-body dynamics

    A. Buonanno and T. Damour, Effective one-body ap- proach to general relativistic two-body dynamics, Phys. Rev. D59, 084006 (1999), arXiv:gr-qc/9811091

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  51. [52]

    Transition from inspiral to plunge in binary black hole coalescences

    A. Buonanno and T. Damour, Transition from inspiral to plunge in binary black hole coalescences, Phys. Rev. D62, 064015 (2000), arXiv:gr-qc/0001013

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  52. [53]

    Damour, P

    T. Damour, P. Jaranowski, and G. Schaefer, On the determination of the last stable orbit for circular gen- eral relativistic binaries at the third postNewtonian ap- proximation, Phys. Rev. D62, 084011 (2000), arXiv:gr- qc/0005034

    work page arXiv 2000

  53. [54]

    Buonanno, Y

    A. Buonanno, Y. Chen, and T. Damour, Transition from inspiral to plunge in precessing binaries of spinning black holes, Phys. Rev. D74, 104005 (2006), arXiv:gr- qc/0508067

    work page arXiv 2006

  54. [55]

    An improved effective-one-body Hamiltonian for spinning black-hole binaries

    E. Barausse and A. Buonanno, An Improved effective- one-body Hamiltonian for spinning black-hole binaries, Phys. Rev. D81, 084024 (2010), arXiv:0912.3517 [gr- qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  55. [56]

    Effective one body Hamiltonian of two spinning black-holes with next-to-next-to-leading order spin-orbit coupling

    A. Nagar, Effective one body Hamiltonian of two spinning black-holes with next-to-next-to-leading or- der spin-orbit coupling, Phys. Rev. D84, 084028 (2011), [Erratum: Phys.Rev.D 88, 089901 (2013)], arXiv:1106.4349 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  56. [57]

    Gravitational radiation reaction along general orbits in the effective one-body formalism

    D. Bini and T. Damour, Gravitational radiation re- action along general orbits in the effective one- body formalism, Phys. Rev. D86, 124012 (2012), arXiv:1210.2834 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  57. [58]

    Effective-one-body Hamiltonian with next-to-leading order spin-spin coupling for two nonprecessing black holes with aligned spins

    S. Balmelli and P. Jetzer, Effective-one-body Hamilto- nian with next-to-leading order spin-spin coupling for two nonprecessing black holes with aligned spins, Phys. Rev. D87, 124036 (2013), [Erratum: Phys.Rev.D 90, 089905 (2014)], arXiv:1305.5674 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  58. [59]

    Fourth post-Newtonian effective one-body dynamics

    T. Damour, P. Jaranowski, and G. Sch¨ afer, Fourth post- Newtonian effective one-body dynamics, Phys. Rev. D 91, 084024 (2015), arXiv:1502.07245 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  59. [60]

    Khalil, J

    M. Khalil, J. Steinhoff, J. Vines, and A. Buonanno, Fourth post-Newtonian effective-one-body Hamiltoni- ans with generic spins, Phys. Rev. D101, 104034 (2020), arXiv:2003.04469 [gr-qc]

    work page arXiv 2020

  60. [61]

    Khalil, A

    M. Khalil, A. Buonanno, J. Steinhoff, and J. Vines, Radiation-reaction force and multipolar waveforms for eccentric, spin-aligned binaries in the effective-one- body formalism, Phys. Rev. D104, 024046 (2021), arXiv:2104.11705 [gr-qc]

    work page arXiv 2021

  61. [62]

    Gamboa, M

    A. Gamboa, M. Khalil, and A. Buonanno, Third post-Newtonian dynamics for eccentric orbits and aligned spins in the effective-one-body waveform model SEOBNRv5EHM, Phys. Rev. D112, 044037 (2025), arXiv:2412.12831 [gr-qc]

    work page arXiv 2025

  62. [63]

    Antonelli, M

    A. Antonelli, M. van de Meent, A. Buonanno, J. Stein- hoff, and J. Vines, Quasicircular inspirals and plunges from nonspinning effective-one-body Hamiltonians with gravitational self-force information, Phys. Rev. D101, 024024 (2020), arXiv:1907.11597 [gr-qc]

    work page arXiv 2020

  63. [64]

    van de Meent, A

    M. van de Meent, A. Buonanno, D. P. Mihaylov, S. Ossokine, L. Pompili, N. Warburton, A. Pound, B. Wardell, L. Durkan, and J. Miller, Enhancing the SEOBNRv5 effective-one-body waveform model with second-order gravitational self-force fluxes, Phys. Rev. D108, 124038 (2023), arXiv:2303.18026 [gr-qc]

    work page arXiv 2023

  64. [65]

    Leather, A

    B. Leather, A. Buonanno, and M. van de Meent, Inspiral-merger-ringdown waveforms with gravitational self-force results within the effective-one-body formal- ism, Phys. Rev. D112, 044012 (2025), arXiv:2505.11242 [gr-qc]

    work page arXiv 2025

  65. [66]

    Gravitational scattering, post-Minkowskian approximation and Effective One-Body theory

    T. Damour, Gravitational scattering, post-Minkowskian approximation and Effective One-Body theory, Phys. Rev. D94, 104015 (2016), arXiv:1609.00354 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  66. [67]

    Energetics of two-body Hamiltonians in post-Minkowskian gravity

    A. Antonelli, A. Buonanno, J. Steinhoff, M. van de Meent, and J. Vines, Energetics of two-body Hamilto- nians in post-Minkowskian gravity, Phys. Rev. D99, 104004 (2019), arXiv:1901.07102 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  67. [68]

    Khalil, A

    M. Khalil, A. Buonanno, J. Steinhoff, and J. Vines, En- ergetics and scattering of gravitational two-body sys- tems at fourth post-Minkowskian order, Phys. Rev. D 106, 024042 (2022), arXiv:2204.05047 [gr-qc]

    work page arXiv 2022

  68. [69]

    Buonanno, G

    A. Buonanno, G. Mogull, R. Patil, and L. Pompili, Post- Minkowskian Theory Meets the Spinning Effective-One- Body Approach for Bound-Orbit Waveforms, Phys. Rev. Lett.133, 211402 (2024), arXiv:2405.19181 [gr- qc]

    work page arXiv 2024

  69. [70]

    Buonanno, G

    A. Buonanno, G. U. Jakobsen, and G. Mogull, Post- Minkowskian theory meets the spinning effective-one- body approach for two-body scattering, Phys. Rev. D 110, 044038 (2024), arXiv:2402.12342 [gr-qc]

    work page arXiv 2024

  70. [71]

    Damour, A

    T. Damour, A. Nagar, A. Placidi, and P. Ret- tegno, A novel Lagrange-multiplier approach to the effective-one-body dynamics of binary systems in post- 26 Minkowskian gravity, arXiv preprint arXiv:2503.05487 (2025), arXiv:2503.05487 [gr-qc]

    work page arXiv 2025

  71. [72]

    Y. Pan, A. Buonanno, L. T. Buchman, T. Chu, L. E. Kidder, H. P. Pfeiffer, and M. A. Scheel, Effective-one- body waveforms calibrated to numerical relativity simu- lations: coalescence of non-precessing, spinning, equal- mass black holes, Phys. Rev. D81, 084041 (2010), arXiv:0912.3466 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  72. [73]

    Effective-one-body waveforms calibrated to numerical relativity simulations: coalescence of non-spinning, equal-mass black holes

    A. Buonanno, Y. Pan, H. P. Pfeiffer, M. A. Scheel, L. T. Buchman, and L. E. Kidder, Effective-one-body waveforms calibrated to numerical relativity simula- tions: Coalescence of non-spinning, equal-mass black holes, Phys. Rev. D79, 124028 (2009), arXiv:0902.0790 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  73. [74]

    An improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detectors

    A. Boh´ eet al., Improved effective-one-body model of spinning, nonprecessing binary black holes for the era of gravitational-wave astrophysics with advanced detec- tors, Phys. Rev. D95, 044028 (2017), arXiv:1611.03703 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  74. [75]

    Time-domain effective-one-body gravitational waveforms for coalescing compact binaries with nonprecessing spins, tides and self-spin effects

    A. Nagaret al., Time-domain effective-one-body gravi- tational waveforms for coalescing compact binaries with nonprecessing spins, tides and self-spin effects, Phys. Rev. D98, 104052 (2018), arXiv:1806.01772 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  75. [76]

    Nagar, G

    A. Nagar, G. Pratten, G. Riemenschneider, and R. Gamba, Multipolar effective one body model for non- spinning black hole binaries, Phys. Rev. D101, 024041 (2020), arXiv:1904.09550 [gr-qc]

    work page arXiv 2020

  76. [77]

    Gamba, S

    R. Gamba, S. Ak¸ cay, S. Bernuzzi, and J. Williams, Effective-one-body waveforms for precessing coalescing compact binaries with post-Newtonian twist, Phys. Rev. D106, 024020 (2022), arXiv:2111.03675 [gr-qc]

    work page arXiv 2022

  77. [78]

    Prototype effective-one-body model for nonprecessing spinning inspiral-merger-ringdown waveforms

    A. Taracchini, Y. Pan, A. Buonanno, E. Barausse, M. Boyle, T. Chu, G. Lovelace, H. P. Pfeiffer, and M. A. Scheel, Prototype effective-one-body model for nonprecessing spinning inspiral-merger-ringdown wave- forms, Phys. Rev. D86, 024011 (2012), arXiv:1202.0790 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  78. [79]

    Effective-one-body model for black-hole binaries with generic mass ratios and spins

    A. Taracchiniet al., Effective-one-body model for black- hole binaries with generic mass ratios and spins, Phys. Rev. D89, 061502 (2014), arXiv:1311.2544 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  79. [80]

    Frequency domain reduced order model of aligned-spin effective-one-body waveforms with generic mass-ratios and spins

    M. P¨ urrer, Frequency domain reduced order model of aligned-spin effective-one-body waveforms with generic mass-ratios and spins, Phys. Rev. D93, 064041 (2016), arXiv:1512.02248 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  80. [81]

    Validating the effective-one-body model of spinning, precessing binary black holes against numerical relativity

    S. Babak, A. Taracchini, and A. Buonanno, Validating the effective-one-body model of spinning, precessing bi- nary black holes against numerical relativity, Phys. Rev. D95, 024010 (2017), arXiv:1607.05661 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

Showing first 80 references.